International VLBI Service for Geodesy and Astrometry

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Front cover:

The development and use of new technology continues to advance within IVS. The front cover shows four selected examples of design and development work described 

in this year’s Annual Report (in clockwise direction): [top right] broadband phase calibration system (breadboard model) at Svetloe Observatory; [bottom right] 

experimental wide-band feed elements for Arrayed Travel Wave Antenna studies developed at NICT and cooperating Japanese institutions; [bottom left] prototype of 

a Balun-fed Eleven feed with a linear taper developed at Chalmers University; and [top left] QRFH broadband feed at the Westford 18-m antenna. More details about 

the displayed technology are available in the Technology Development (TD) Center reports of IAA (p. 287ff), NICT (p. 291ff), Onsala Space Observatory (p. 295ff) and 

Haystack Observatory (p. 283ff), respectively. Photos are courtesy of these TD Centers and their collaborators at other institutions.
NASA/TP—201–21

 

International VLBI Service for Geodesy 

and Astrometry 2011 Annual Report 

.DUHQ'%DYHU(ed.)

NVI, Inc., Greenbelt, Maryland 

 

Dirk Behrend (ed.)

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National Aeronautics and 

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June 2012
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Preface

This volume of reports is the 2011 Annual Report of the International VLBI Service for Geodesy

and Astrometry (IVS). The individual reports were contributed by VLBI groups in the international geodetic and astrometric community who constitute the permanent components of IVS.

The IVS 2011 Annual Report documents the work of the IVS components for the calendar year

2011, our thirteenth year of existence. The reports describe changes, activities, and progress of

the IVS. Many thanks to all IVS components who contributed to this Annual Report.

The contents of this Annual Report also appear on the IVS Web site at

http://ivscc.gsfc.nasa.gov/publications/ar2011

This book and the Web site are organized as follows:

• The first section contains general information about IVS, a map showing the location of the

components, information about the Directing Board members, and the annual report of the

IVS Chair.

• The second section holds a special report about the IVS Retreat at Hohe Wand, Austria

including a reproduction of the retreat’s final declaration. A major focus of the retreat was

a review and update of the IVS Terms of Reference (ToR). The updated ToR can be found

in the last section (see below).

• The next seven sections hold the reports from the Coordinators and the reports from the IVS

Permanent Components: Network Stations, Operation Centers, Correlators, Data Centers,

Analysis Centers, and Technology Development Centers.

• The next section contains a compilation of publications in the field of geodetic and astrometric

VLBI during 2011.

• The last section includes reference information about IVS: the Terms of Reference, the lists of

Member and Affiliated organizations, the IVS Associate Member list, a complete list of IVS

components, the list of institutions that contributed to this report, and a list of acronyms.

iii

Table of Contents

Preface . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . iii

About IVS . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 1

IVS Organization . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 2

IVS Component Map . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 4

IVS Directing Board . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 6

IVS Chair’s Report . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 8

Special Reports . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 11

Hohe Wand Declaration . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 13

IVS Coordination . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 15

Coordinating Center Report . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 17

Analysis Coordinator Report . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 21

Network Coordinator Report . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 24

IVS Technology Coordinator Report . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . .28

Network Stations . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 33

Badary Radio Astronomical Observatory . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 35

Fortaleza Station Report for 2011 . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 39

Goddard Geophysical and Astronomical Observatory . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 42

Hartebeesthoek Radio Astronomy Observatory (HartRAO) . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 46

AuScope VLBI Project and Hobart 26-m Antenna . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 50

Kashima 34-m Radio Telescope . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . .54

Kashima and Koganei 11-m VLBI Stations . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 58

Kokee Park Geophysical Observatory . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 62

Matera CGS VLBI Station . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 66

The Medicina Station Status Report . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 70

VERA Geodetic Activities . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 72

Noto Station Status Report . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 76

Ny- ̊Alesund 20-meter Antenna . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 80

German Antarctic Receiving Station (GARS) O’Higgins . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 84

Onsala Space Observatory – IVS Network Station . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 88

Parkes 2011 IVS Report . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 92

Sheshan VLBI Station Report for 2011 . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 93

Geodetic and Astrophysical Study at the Simeiz VLBI Station . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . .95

Svetloe Radio Astronomical Observatory . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 99

JARE Syowa Station 11-m Antenna, Antarctica . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 103

Status and Developments at TIGO Concepci ́on . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 107

Tsukuba 32-m VLBI Station . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 111

Nanshan VLBI Station Report for 2011 . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 115

Warkworth 12-m VLBI Station: WARK12M . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 119

Westford Antenna . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 123

Geodetic Observatory Wettzell - 20-m Radio Telescope and Twin Telescope . . . . . . . . . . . . . . . . . . . . . . . . . 127

Instituto Geogr ́afico Nacional of Spain . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 131

Zelenchukskaya Radio Astronomical Observatory . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 135

v
Operation Centers . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 139

The Bonn Geodetic VLBI Operation Center . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 141

CORE Operation Center Report . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 143

NEOS Operation Center . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 147

Correlators . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 149

The Bonn Astro/Geo Correlator . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 151

Haystack Observatory VLBI Correlator . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 155

IAA Correlator Center . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 159

VLBI Correlators in Kashima . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 161

Tsukuba VLBI Correlator . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 165

Washington Correlator . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 169

Data Centers . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 173

BKG Data Center . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 175

CDDIS Data Center Summary for the IVS 2011 Annual Report . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 177

Italy INAF Data Center Report . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 180

Data Center at NICT . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 181

Paris Observatory (OPAR) Data Center . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 185

Analysis Centers . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 189

Analysis Center of Saint Petersburg University . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 191

Geoscience Australia Analysis Center . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 193

Report for 2011 from the Bordeaux IVS Analysis Center . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 197

BKG/DGFI Combination Center Annual Report 2011 . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 201

Matera CGS VLBI Analysis Center . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 204

DGFI Analysis Center Annual Report 2011 . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 206

FFI Analysis Center . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 208

The BKG/IGGB VLBI Analysis Center . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 209

GSFC VLBI Analysis Center . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 213

IAA VLBI Analysis Center Report 2011 . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 217

Vienna IGG Special Analysis Center Annual Report 2011 . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 220

Italy INAF Analysis Center Report . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 224

JPL VLBI Analysis Center Report for 2011 . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 226

KASI Combination Center Report . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 230

KTU-GEOD IVS Analysis Center Annual Report 2011 . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 234

IVS Analysis Center at Main Astronomical Observatory of National Academy of Sciences of Ukraine 236

Analysis Center at National Institute of Information and Communications Technology . . . . . . . . . . . . . . . 238

NMA Analysis Center . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 242

Paris Observatory Analysis Center OPAR: Report on Activities, January - December 2011 . . . . . . . . . . 245

Onsala Space Observatory – IVS Analysis Center . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . .249

PMD Analysis Center Report for 2011 . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 252

Pulkovo IVS Analysis Center (PUL) 2011 Annual Report . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . .256

SAI VLBI Analysis Center Report 2011 . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 259

SHAO Analysis Center 2011 Annual Report . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 261

Tsukuba VLBI Analysis Center . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 264

U.S. Naval Observatory VLBI Analysis Center . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 268

USNO Analysis Center for Source Structure Report . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 272

vi
Technology Development Centers . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 275

Canadian VLBI Technology Development Center . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 277

FFI Technology Development Center - Software Development . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 278

GSFC Technology Development Center Report . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 280

Haystack Observatory Technology Development Center . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 283

IAA Technology Development Center Report 2011 . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 287

Technology Development Center at NICT . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 291

Onsala Space Observatory – IVS Technology Development Center . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 295

Bibliography . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 299

Bibliography . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 301

IVS Information . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 315

IVS Terms of Reference . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 317

IVS Member Organizations . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 327

IVS Affiliated Organizations . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 329

IVS Associate Members . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 330

IVS Permanent Components . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 340

Addresses of Institutions of Authors Contributing to this Report . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 344

List of Acronyms . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . .351

vii

About IVS

About IVS
2

IVS Organization

Objectives

IVS is an international collaboration of organizations which 

operate or support Very Long Baseline Interferometry 

(VLBI) components. The goals are:

1. To provide a service to support geodetic, geophysical 

and astrometric research and operational activities.

2. To promote research and development activities in 

all aspects of the geodetic and astrometric VLBI 

technique.

3. To interact with the community of users of VLBI 

products and to integrate VLBI into a global Earth 

observing system.

The IVS

• Interacts closely with the IERS, which is tasked by 

IAU and IUGG with maintaining the international 

celestial and terrestrial reference frames (ICRF

and ITRF),

• coordinates VLBI observing programs, 

• sets performance standards for the observing stations, 

• establishes conventions for data formats and products, 

• issues recommendations for analysis software,

• sets standards for analysis documentation,

• institutes appropriate product delivery methods in 

order to insure suitable product quality and timeliness.

Realization And Status Of IVS

IVS consists of

• 31 Network Stations, acquiring high performance 

VLBI data,

• 3 Operation Centers, coordinating the activities of a 

network of Network Stations,

• 6 Correlators, processing the acquired data, providing feedback to the stations and providing processed 

data to analysts,

• 6 Data Centers, distributing products to users, 

providing storage and archiving functions,

• 27 Analysis Centers, analyzing the data and producing 

the results and products,

• 7 Technology Development Centers, developing new 

VLBI technology,

• 1 Coordinating Center, coordinating daily and long 

term activities.

Altogether

• 81 Permanent Components, representing 41 institutions in 20 countries,

• ~280 Associate Members.

In addition the IVS has:

• Directing Board, determining policies, standards and 

goals; the board is composed of 15 members (elected 

and ex officio), including

• Coordinators for the network, analysis and technology.

ORGANIZATION OF INTERNATIONAL VLBI SERVICE

performance feedback

data bases

Coordinating

Center

Analysis

Centers

Analysis

Coordinator

Network

Stations

Operation

Centers

Technology

Development

Centers

Users

Network

Coordinator

Technology

Coordinator

• Publications

• Web Site

• Master Schedule

raw data 10-20Gb/s

(disks, ftp)

performance feedback

correlated data bases

analyzed results and products

schedules

products for EOP, TRF, CRF

Data

Centers

Correlators

IAG IAU IVS Directing

Board
3

IVS Affiliated Organizations

The following organizations cooperate with IVS on issues 

of common interest, but do not support an IVS component. 

Affiliated Organizations express an interest in establishing 

and maintaining a strong working association with IVS to 

mutual benefit. Listed alphabetically by country. 

Products

The VLBI technique contributes uniquely to

• Definition and realization of the International Celestial 

Reference Frame (ICRF)

• Monitoring of Universal Time (UT1) and length of day 

(LOD)

• Monitoring the coordinates of the celestial pole (nutation and precession)

Further significant products are

• All components of Earth Orientation Parameters at 

regular intervals

• Station coordinates and velocity vectors for the realization and maintenance of the International Terrestrial 

Reference Frame (ITRF)

All VLBI data and results in appropriate formats are archived in data centers and publicly available for research 

in related areas of geodesy, geophysics and astrometry.

IVS Member Organizations

The following organizations contribute to IVS by supporting 

one or more IVS components. They are considered IVS 

Members. Listed alphabetically by country.

Organization Country

Geoscience Australia Australia

University of Tasmania Australia

CSIRO Australia

Vienna University of Technology Austria

Centro de Rádio Astronomia e Aplicações 

Espaciais

Brazil

Geodetic Survey Division, Natural 

Resources Canada

Canada

Dominion Radio Astrophysical 

Observatory

Canada

Universidad de Concepción Chile

Instituto Geográfico Militar Chile

Chinese Academy of Sciences China

Observatoire de Paris France

Observatoire de Bordeaux France

Deutsches Geodätisches 

Forschungsinstitut

Germany

Bundesamt für Kartographie und Geodäsie Germany

Institut für Geodäsie und Geoinformation 

der Universität Bonn

Germany

Forschungseinrichtung Satellitengeodäsie, 

TU-Munich

Germany

Max-Planck-Institut für Radioastronomie Germany

Istituto di Radioastronomia INAF Italy

Agenzia Spaziale Italiana Italy

Politecnico di Milano DIIAR Italy

Geospatial Information Authority of Japan Japan

National Institute of Information and 

Communications Technology

Japan

National Astronomical Observatory of 

Japan

Japan

National Institute of Polar Research Japan

Auckland University of Technology New 

Zealand

Norwegian Defence Research 

Establishment

Norway

Norwegian Mapping Authority Norway

Astronomical Institute of St.-Petersburg 

University

Russia

Institute of Applied Astronomy Russia

Pulkovo Observatory Russia

Sternberg Astronomical Institute of 

Moscow State University

Russia

Organization Country

Hartebeesthoek Radio Astronomy 

Observatory

South 

Africa

Korea Astronomy and Space Science 

Institute

South 

Korea

Instituto Geográfico Nacional Spain

Chalmers University of Technology Sweden

Karadeniz Technical University Turkey

Main Astronomical Observatory, 

National Academy of Sciences, Kiev

Ukraine

Laboratory of Radioastronomy of Crimean 

Astrophysical Observatory

Ukraine

NASA Goddard Space Flight Center USA

U. S. Naval Observatory USA

Jet Propulsion Laboratory USA

Organization Country

Australian National University Australia

University of New Brunswick Canada

FÖMI Satellite Geodetic Observatory Hungary

Joint Institute for VLBI in Europe (JIVE) Netherlands

Westerbork Observatory Netherlands

National Radio Astronomy Observatory USA
4

IVS Component Map

IVS Components by Country

Country Qty.

Australia 3

Austria 1

Brazil 1

Canada 1

Chile 1

China 3

France 3

Germany 8

Italy 8

Japan 13

New Zealand 1

Norway 4

Russia 9

South Africa 1

South Korea 1

Spain 1

Sweden 3

Turkey 1

Ukraine 2

USA 16

Total 81

A complete list of IVS Permanent

Components is in the IVS Information

section of this volume.

O'Higgins

NEOS

GGAO

Canadian VLBI

Haystack

USNO

GSFC

JPL

Kokee Park

O'Higgins

Fortaleza

NEOS

GGAO

Canadian VLBI

Haystack

USNO

GSFC

JPL

Kokee Park

TIGO Network Station

Former Station

Operation Center

Correlator

Data Center

Analysis Center

Technology Development Center

Coordinating Center

Network Station

Former Station

Operation Center

Correlator

Data Center

Analysis Center

Technology Development Center

Coordinating Center

Gilmore Creek

Yellowknife

Algonquin
5

Syowa

Hartebeesthoek

Seshan

Nanshan

Shanghai

Kashima 11

Koganei

Tsukuba

NICT

Mizusawa

Kashima34

TU Vienna

Yebes

Noto

Wettzell

Simeiz

DGFI

INAF

Matera

BKG

Svetloe

IAA

MAO

AIStPbU

Bordeaux

Paris

FGS(BKG,IGGB)

IGGB

FFI Onsala

Ny Ålesund

Seshan

Nanshan

Badary

Shanghai

Kashima 11

Koganei

Tsukuba

NICT

Mizusawa

GA

Kashima34

Medicina

TU Vienna

Yebes

Noto

DGFI Wettzell

INAF

Matera

BKG

Svetloe

IAA

MAO

KTU

AIStPbU

Bordeaux

Paris

FGS(BKG,IGGB)

IGGB

FFI

NMA

PMD

Onsala

Ny Ålesund

Syowa

Hartebeesthoek

Simeiz

Hobart

Zelenchukskaya

KASI

PUL

SAI

Warkworth

Parkes

GSI

Yarragadee Yarragadee

Katherine
6

IVS Directing Board

NAME: Hayo Hase

AFFILIATION: Bundesamt für 

Kartographie und Geodäsie/

TIGO, Germany/Chile

POSITION: Networks 

Representative

TERM: Feb 2011 to Feb 2015

NAME: Rüdiger Haas

AFFILIATION: Chalmers 

University of Technology, 

Sweden

POSITION: Technology Development Centers Representative

TERM: Feb 2009 to Feb 2013

NAME: Dirk Behrend

AFFILIATION: NVI, Inc./Goddard 

Space Flight Center, USA

POSITION: Coordinating Center 

Director

TERM: ex officio

NAME: Harald Schuh

AFFILIATION: Vienna University 

of Technology, Austria

POSITION: Acting Chair and IAG 

Representative

TERM: ex officio

NAME: Jesús Gómez González

AFFILIATION: National 

Geographic Institute of Spain

POSITION: At Large Member

TERM: Feb 2011 to Feb 2013

NAME: Patrick Charlot

AFFILIATION: Bordeaux 

Observatory, France

POSITION: IAU Representative

TERM: ex officio

NAME: Alessandra Bertarini

AFFILIATION: University 

of Bonn, Germany

POSITION: Correlators

and Operation Centers

Representative

TERM: Feb 2011 to Feb 2015
7

NAME: Shinobu Kurihara

AFFILIATION: Geographical 

Survey Institute, Japan

POSITION: At Large Member

TERM: (Feb 2011) to Feb 2013

NAME: Gino Tuccari

AFFILIATION: Istituto di

Radioastronomia, Italy

POSITION: Networks

Representative

TERM: Feb 2009 to Feb 2013

NAME: Axel Nothnagel

AFFILIATION: University 

of Bonn, Germany

POSITION: Analysis

Coordinator

TERM: permanent

NAME: Chopo Ma

AFFILIATION: NASA Goddard 

Space Flight Center, USA

POSITION: IERS Representative

TERM: ex officio

NAME: Fengchun Shu

AFFILIATION: Shanghai 

Astronomical Observatory, 

China

POSITION: At Large Member

TERM: Feb 2011 to Feb 2013

NAME: Alan Whitney

AFFILIATION: Haystack

Observatory, USA

POSITION: Technology

Coordinator

TERM: permanent

NAME: Oleg Titov

AFFILIATION: Geoscience 

Australia, Australia

POSITION: Analysis and 

Data Centers Representative

TERM: Feb 2009 to Feb 2013

NAME: Ed Himwich

AFFILIATION: NVI, Inc./Goddard 

Space Flight Center, USA

POSITION: Network

Coordinator

TERM: permanent
8

IVS Chair’s Report

Harald Schuh

Institute of Geodesy and Geophysics, Vienna University 

of Technology, Austria

With the 2011 Annual Report the IVS components report 

about their progress and activities which were conducted 

during the service’s thirteenth year of existence. I would 

like to thank all IVS Associate Members for their contributions over the course of the year, in particular for 

providing their reports in time. Timely appearance of the 

Annual Report is always an ambitious goal and is highly 

appreciated for maintaining this volume as a real information exchange tool for the community and related groups. 

I thank the editors for the timely release.

In 2011 IVS observing activities remained at the same 

high level as in previous years, testament to the optimized coordination by the Coordinating Center and 

strong support from all components despite the limited 

resources and failures at a few aging radio telescopes. I 

would like to thank the staff of the Coordinating Center 

who bear much responsibility and carry a heavy burden 

for the entire service activities. Day-to-day work is done 

continuously by the Network Stations, the Correlators, 

the Data Centers, and the Analysis Centers and is the 

basis for the regular provision of precise and reliable IVS 

products. Here I would like to emphasize those activities 

performed in 2011 that go beyond the normal work load.

IVS Contribution to the Global Geodetic 

Observing System (GGOS)

In 2005 the intergovernmental Group on Earth Observations (GEO) was formed. This group initiated the creation 

of a Global Earth Observing System of Systems (GEOSS) 

for monitoring and understanding global change. The International Association of Geodesy (IAG) contributes to 

this multi-national and multi-institutional effort with the 

Global Geodetic Observing System (GGOS). Based on 

the well-established, international space-geodetic services GGOS will provide the most precise terrestrial and 

celestial reference frames that are needed as a stable 

reference to monitor any kind of changes on Earth and 

in space. 

Integration and combination in the framework of GGOS 

is the main challenge for the international geodesy in 

this decade. GGOS goes beyond the integration of the 

geometric techniques (VLBI, SLR, GNSS, DORIS) as it 

includes also techniques measuring terrestrial gravity, the 

global Earth gravity field, sea level, and also the magnetic 

field. Thus, a consistent combination of all geometric and 

physical techniques will be required. GGOS plays an essential role in helping to solve environmental and societal 

problems. Many tasks such as establishing a unified global 

height system or open questions related to global change, 

sea level rise, or the prevention of natural hazards need 

precise reference frames and exact geodetic measurements. VLBI can give a critical contribution to GGOS by 

its relation to a quasi-inertial celestial reference frame and 

its unique ability to measure long-term UT1-UTC and precession/nutation. One of the IVS main tasks in 2011 was 

to continue its contribution as an efficient partner within 

GGOS. Several GGOS events were attended in 2011 

with presentations about the IVS and its next generation 

VLBI2010 system; the IVS is well represented in the GGOS 

Steering Committee. Since August 2011 GGOS itself has 

been subject to a re-organization with new entities formed 

(GGOS Consortium, GGOS Coordinating Board)—this 

process is still ongoing and the IVS is actively contributing.

VLBI2010 Committee (V2C) and VLBI2010 

Project Executive Group (V2PEG)

In recent years the IVS has developed the concept and 

specifications of a next generation VLBI system called 

VLBI2010. The goals of the new system are to achieve 

(on scales up to the size of the Earth): 

• 1 mm position accuracy,

• 0.1 mm/yr velocity accuracy,

• continuous observations, and

• results available in near real-time. 

The VLBI2010 Committee (V2C), chaired by Bill Petrachenko, was established in 2005. It is tasked with promoting the goals set by the VLBI2010 Report released by 

the IVS Working Group 3 “VLBI2010: Current and Future 

Requirements for Geodetic VLBI Systems.” All results 

have been summarized in the excellent VLBI2010 Progress Report with recommendations that can be used as 

benchmark for new VLBI systems. Since the VLBI2010 

Progress Report was finalized in spring 2009 and put 

on the IVS Web site (ftp://ivscc.gsfc.nasa.gov/pub/

misc/V2C/TM-2009-214180.pdf ) the V2C activities have 

continued with a lot of further simulations and technical 

studies. I would like to thank all members of the V2C for 

taking over the responsible leading role in the realization 

of the VLBI2010 visions.

VLBI2010 is supposed to develop not only the visions but 

also very detailed specifications for future VLBI systems. 

Now, the task for the IVS is the realization of the VLBI2010 

concept. To support the implementation of VLBI2010 and 
9

experiments in application to planetary and space 

science missions.

2. To determine areas of VLBI support of planetary and 

space science missions where experiments conducted by the IVS (possibly together with other VLBI 

networks) can be mutually beneficial.

3. To investigate desirability and feasibility of establishing 

a mission-specific liaison between IVS and appropriate space agencies and organizations involved in 

planetary and space science missions.

Due to cancellations or postponement of several relevant 

space missions the work of WG5 was also delayed, but it 

is anticipated that a first report of WG5 will be published 

in 2012.

IVS Working Group 6 on “VLBI Education 

and Training” 

The IVS Directing Board established in March 2009 the 

Working Group 6 on “Education and Training” chaired by 

Rüdiger Haas. The general aim of IVS WG6 is to support 

education and training in the field of geodetic and astrometric VLBI, in order to maintain and pass on the expertise 

in this field to the next generations.

The Terms of Reference of IVS WG6 are:

1. To establish contacts to education institutions in geodesy and geosciences worldwide with the aim to raise 

interest in geodetic VLBI among students.

2. To develop ideas for education material that can be 

distributed to education institutions.

3. To seek funding to organize training in form of, for 

instance, IVS summer schools for Master and PhD 

students.

Proposals for a VLBI summer school were submitted in 

2011 which hopefully can be organized in the near future.

Events and Highlights in 2011

From March 29 to 31, 2011 the 20th European VLBI for 

Geodesy and Astrometry (EVGA) Working Meeting and 

an IVS Analysis Workshop were held at Max-PlanckInstitute for Radio Astronomy (MPIfR) in Bonn, Germany. 

The scientific organization of the meetings was performed 

in close collaboration with the IVS Analysis Coordinator and Chair of the EVGA, Axel Nothnagel. The local 

organizing committee was led by Walter Alef from MaxPlanck-Institute who was supported by his colleagues 

from MPIfR together with the VLBI group of the Institute 

of Geodesy and Geoinformation (IGG) of Bonn University. It was extremely interesting to listen to the talk about 

to actively contact governmental entities and funding organizations the VLBI2010 Project Executive Group (V2PEG) 

under the leadership of Hayo Hase continued its activities 

in 2011. Several letters of support were sent to government bodies and funding agencies all over the world and 

an update of the so-called station survey was requested 

from the IVS network stations in December 2011. Based 

on this questionnaire very useful information was obtained 

about the status of the planning process concerning the 

transition to VLBI2010 at the various observing stations. 

Right now several countries have already decided to 

develop or purchase new VLBI systems. We highly appreciate that the following agencies got approval of 

new VLBI2010-type radio telescopes in 2011: National 

Geographic Information Institute (NGII), South Korea; 

Geospatial Information Authority of Japan (GSI); Finnish 

Geodetic Institute (FGI); University of Kazan, Russia; 

and Norwegian Mapping Authority (NMA). I would like 

to congratulate them on the ambitious projects and wish 

them success for the realization in the next years. Thus, 

already thirteen VLBI2010 antennas have been approved 

with more proposals under consideration or already in 

review in countries like China, France, Saudi Arabia, and 

Sweden (while writing this report in March 2012 further 

proposals for new radio telescopes got approved, for 

instance, in Sweden and China). With new antennas the 

global coverage of geodetic VLBI is getting better; but it is 

still far from being optimal, in particular more VLBI sites in 

the southern hemisphere would be more than welcome. 

IVS Working Group 4 on “VLBI Data 

Structures”

The IVS Working Group on “VLBI Data Structures” chaired 

by John Gipson was established in September 2007 as a 

response to the strong need of new, common VLBI data 

structures. This Working Group examines the data structure currently used in VLBI data processing and develops 

the data structure needed in the future. WG4 is now close 

to realize all its goals and to provide the new data format 

strongly required by the IVS Analysis Centers.

IVS Working Group 5 on “Space Science Applications” 

The current mandate of the WG5, chaired by Leonid Gurvits, comprises the following tasks: 

1. To investigate synergies in scientific and technological areas between the IVS core activities and VLBI 
10

IVS Chair’s Report Continued

‘EVGA - Looking back at the early beginnings’ delivered 

by James Campbell who had been leading the European 

VLBI activities over decades and for sure is the person 

who knows best about the history of European geodetic 

VLBI. It should also be mentioned here that the Proceedings of the 20th EVGA Working Meeting have been printed 

already in July 2011 (http://www.mpifr-bonn.mpg.de/

div/meetings/20thEVGA/pdf-files/EVGA-proceedings.

pdf) proving the efficiency of the local organizers.

Another highlight in 2011 certainly was the continuous 

VLBI session CONT11 that took place in the second half 

of September 2011 and was observed on a network of 

13 stations. Remote-control of several radio telescopes 

allowed unattended operation (e.g., during nights). Due to 

the high number of baselines to be correlated the correlation was just finished recently (as of March 2012) but as 

the CONT sessions have always shown the best possible 

performance of international VLBI and provided the most 

interesting and valuable results we expect another bunch 

of extremely useful VLBI data. 

On 21–22 October 2011, the first IVS Retreat and on 23 

October 2011, the 26th IVS Directing Board Meeting were 

held at Hohe Wand, a table mountain 60 kilometers southwest of Vienna. For the Retreat the Board was augmented 

by invited guests, namely, Johannes Böhm, Thomas Hobiger, Jim Lovell, and Arthur Niell. The focus of the Retreat 

was placed on a review and update of the IVS Terms of 

Reference (ToR). Periodic reviews of the IVS organization 

and its mandate, functions, and components are actually 

a requirement according to the ToR. The conclusions of 

a thorough final discussion about the IVS strategic goals 

and tasks were summarized in the ‘Hohe Wand Declaration’ shown just after the Chair’s Report in this volume. 

One new Operational Analysis Center (GSI, Tsukuba, 

Japan) and two new IVS Associate Analysis Centers 

(Norwegian Mapping Agency (NMA), and Politecnico di 

Milano, Italy) were approved in 2011. One ‘Special Analysis 

Center for Specific Observing Sessions’ SAC-SOS (Institute of Geodesy and Geophysics, Vienna, Austria), and 

one Observing Station (Parkes CSIRO Radio Telescope, 

Australia) were also accepted as new IVS components. 

Summary information about all IVS events and activities 

is available on the IVS homepage http://ivscc.gsfc.

nasa.gov and in the IVS Newsletters 29, 30, and 31. The 

Newsletter is an excellent means to transfer information 

to everybody. The editor team, Dirk Behrend, Hayo Hase, 

and Heidi Johnson, presented interesting and up-to-date 

information. They once again did an excellent job, which 

is highly appreciated. 

Another feature should be mentioned here which 

provides excellent information about on-going VLBI 

sessions: it is the IVS live-stream set up by the VLBI 

group of Bordeaux Observatory that can be watched 

under http://ivslive.obs.u-bordeaux1.fr/.

Finally it should be recognized that in a special issue 

of Journal of Geodesy (2011, Volume 85, Number 7) 

six valuable scientific manuscripts were published 

that concentrate on using VLBI observations from the 

CONT08 campaign which took place in August 2008. 

Such an intensive VLBI campaign provides excellent 

data to investigate geodetic and geophysical phenomena of the same period employing meteorological or 

other space-geodetic observations. All authors and in 

particular the guest editors of this special issue, Axel 

Nothnagel, Urs Hugentobler, and David Salstein shall 

be acknowledged here.

The Directing Board in 2011

In February 2011, the Directing Board welcomed the 

two new elected representative members for the term 

2011 to 2015; namely, Hayo Hase (Germany/Chile) as 

re-elected Networks representative and Alessandra 

Bertarini (Germany) as Correlators and Operations 

Centers representative. In addition, Shinobu Kurihara 

(Geospatial Information Authority of Japan), Fengchun 

Shu (Shanghai Astronomical Observatory, China), and 

Jesús Gómez-González (National Geographical Institute of Spain) commenced their terms (2011 to 2013) 

as the new at-large members of the Board. I am very 

pleased that the IVS Directing Board is well balanced 

in its composition with respect to global coverage, with 

respect to component representation, and with respect 

to a good mixture of experienced and young members.

IVS Events in the Coming Year 2012

In the week of March 4, 2011, the 7th IVS General 

Meeting will be held in Madrid, Spain; i.e., in the country 

where presently the planning and establishment of four 

new VLBI radio telescopes is taking place in the frame 

of the Spanish/Portuguese RAEGE project. 
Special Reports

Special Reports

IVS Retreat at Hohe Wand

Hohe Wand Declaration

From 21–22 September 2011 the IVS held a retreat in the Gutenstein Alps in Lower Austria,

a good hour’s drive southwest of Vienna. The venue was an Alpengasthof (‘alpine guesthouse’)

within the Hohe Wand nature park. For the retreat, the IVS Directing Board was augmented

by several invited guests: Johannes B ̈ohm, Thomas Hobiger, Jim Lovell, and Arthur Niell (see

Figure 1), resulting in an overall group strength of 18 participants.

Figure 1. Participants of the IVS retreat at Hohe Wand, Austria.

The focus of the retreat was placed on a review and update of the IVS Terms of Reference

(ToR). Periodic reviews of the IVS organization and its mandate, functions, and components are

actually a requirement according to the ToR. The retreat participants went through the existing

ToR sentence by sentence and discussed the continued validity of the contents. When needed, the

ToR were rephrased or the formulations were simplified. In addition, a few minor additions and

deletions were done. None of the changes were critical or controversial in nature. The additions

were mostly with respect to the Global Geodetic Observing System (GGOS); perhaps the only

major update was the addition of a second Analysis Center representative on the Board. The

revised ToR were approved by the Board in the subsequent Board meeting and then officially

ratified by the International Association of Geodesy (IAG) in December. The revised ToR can be

found in the IVS information section of this volume.

A second major discussion block dealt with focus areas for future IVS work and activities. The

participants felt that emphasis should be put on improving quality control, internal and external

outreach, VLBI2010 infrastructure, real-time observation and product creation (including automation), and expanding research and research fields. The results of the discussion were compiled into

a declaration that was subsequently approved by the Board. Please peruse the reproduction of the

declaration below.

IVS 2011 Annual Report 13
IVS Retreat at Hohe Wand

Declaration of the Participants of the IVS Retreat at

Hohe Wand, Austria from 21–22 September 2011

We, the eighteen participants of the International VLBI Service for Geodesy and Astrometry (IVS)

Retreat at Hohe Wand, Austria, met on 21–22 September 2011 to review the IVS organization and

its mandate, functions, and components, as well as to define focus areas for future IVS work and

activities. We

recognize

• that the global framework for geodetic activities has evolved since the inception of the service

through the establishment of the Global Geodetic Observing System (GGOS);

• that the IVS data and products are also GGOS data and products;

• that the increased requirements, as mandated by GGOS, for position accuracy of 1 mm

and velocity accuracy of 0.1 mm/year by the year 2020 can only be achieved by the nextgeneration VLBI system (VLBI2010); and

• that the IVS organization, mandate, functions, and components as outlined in the IVS Terms

of Reference (ToR) continue to fulfill the requirements of the global geodetic/astrometric

VLBI science and the associated user communities;

recommend

• that the development of the next generation VLBI system be vigorously advanced, and that

the corresponding VLBI2010 infrastructure be established on a global basis;

• that the quality control of VLBI data and products be improved;

• that internal and external outreach activities be enhanced;

• that real-time observation and product creation (including automation) be advanced to an

operational state; and

• that both research activities and research fields-of-interest be expanded.

Hohe Wand, Austria

22 September 2011

14 IVS 2011 Annual Report
IVS Coordination

IVS Coordination

NASA Goddard Space Flight Center IVS Coordinating Center

Coordinating Center Report

Dirk Behrend

Abstract

This report summarizes the activities of the IVS Coordinating Center during the year 2011 and

forecasts activities planned for the year 2012.

1. Coordinating Center Operation

The IVS Coordinating Center is based at the Goddard Space Flight Center and is operated by

NEOS (National Earth Orientation Service), a joint effort for VLBI by the U.S. Naval Observatory

and the NASA Goddard Space Flight Center.

The mission of the Coordinating Center is to provide communications and information for

the IVS community and the greater scientific community and to coordinate the day-to-day and

long-term activities of IVS.

The Web server for the Coordinating Center is provided by Goddard. The address is

http://ivscc.gsfc.nasa.gov

2. Activities during 2011

During the period from January through December 2011, the Coordinating Center supported

the following IVS activities:

• Directing Board support: Coordinated, with local committees, two IVS Directing Board

meetings, in Bonn, Germany (April 2011) and Hohe Wand, Austria (September 2011). Notes

from each meeting were published on the IVS Web site.

• Communications support: Maintained the Web pages, e-mail lists, and Web-based mail

archive files. Generated analysis reports and included them into the 24-hour session Web

pages. Maintained Intensive session Web pages.

• Publications: Published the 2010 Annual Report in spring 2011. Published three editions

of the IVS Newsletter in April, August, and December 2011. All publications are available

electronically as well as in print form.

• Observing Program Committee (OPC): Coordinated meetings of the OPC to monitor the

observing program, review problems and issues, and discuss changes.

• 2011 Master Schedule: Generated and maintained the master observing schedule for 2011.

Coordinated VLBI resources for observing time, correlator usage, and disk modules. Coordinated the usage of Mark 5 systems at IVS stations and efficient deployment of disk modules.

Coordinated the continuous VLBI campaign 2011 (CONT11).

• 2012 Master Schedule: Generated the proposed master schedule for 2012 and received approval from the Observing Program Committee.

• VLBI2010: Supported the activities of the VLBI2010 Committee (V2C) and the VLBI2010

Project Executive Group (V2PEG). Worked with the Local Committee and the Program

IVS 2011 Annual Report 17
IVS Coordinating Center NASA Goddard Space Flight Center

Committee to prepare the VLBI2010 Workshop on Technical Specifications to be held in

Bad K ̈otzting, Germany in March 2012.

• Meetings: Coordinated, with the Local Committee, the sixth IVS Technical Operations

Workshop, held at Haystack Observatory in May 2011. Chaired the Program Committee for

the meeting.

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Figure 1. Logo (left) and participants (right) of the sixth IVS Technical Operations Workshop held at MIT

Haystack Observatory in May 2011. More information about the workshop can be found on the IVS Web

site at http://ivscc.gsfc.nasa.gov/meetings/tow2011/.

Coordinated, with the Local Committee, the seventh IVS General Meeting, to be held in

Madrid, Spain in March 2012. Chaired the Program Committee for the meeting.

3. CONT11 Campaign

The Continuous VLBI Campaign 2011 (CONT11) was successfully observed in late summer to

early fall. Thirteen IVS stations (see Figure 2) observed for 15 consecutive days at a rate of 512

Mbps in the time frame of September 15-29, 2011. The observing was done on the basis of UT

days with each CONT11 day running from 0 UT to 24 UT. UT day observing is needed to make

the most accurate combination and comparison of results from other techniques.

The Coordinating Center, in collaboration with the OPC, was responsible for:

• the overall planning and coordination of the campaign,

• the media usage and shipment schedule, and

• the preparation of the detailed observing schedules and notes.

As was done with the CONT08 campaign, all CONT11 data are being correlated at the Washington Correlator. The release of the correlated data is expected for early 2012. Performing the

correlation at a single place significantly eased the logistics involved with module handling at the

correlators and the stations.

The staggered station check times that were successfully introduced with the CONT08 campaign were also repeated: the daily station checks were decoupled from the change of schedules

and were instead introduced at convenient and well-coordinated times for the stations (i.e., different daily check times for each station) avoiding observational gaps overall. Such gaps existed

18 IVS 2011 Annual Report
NASA Goddard Space Flight Center IVS Coordinating Center

Figure 2. Geographical distribution of the 13 CONT11 stations. From the original 14 stations, Warkworth

had to drop out because of technical problems.

in pre-CONT08 continuous campaigns (usually a 30-minute break between individual observing

days) and resulted in unrealistic peaks in the sub-daily EOP time series derived from the CONT

data.

More information about the CONT11 campaign can be found on the IVS Web site under the

URL http://ivscc.gsfc.nasa.gov/program/cont11.

4. Staff

The staff of the Coordinating Center is drawn from individuals who work at Goddard. The

staff and their responsibilities are listed in Table 1.

Table 1. IVS Coordinating Center staff.

Name Title Responsibilities

Dirk Behrend Director Web site and e-mail system maintenance, Directing Board support, meetings, publications, session Web page monitoring

Cynthia Thomas Operation Manager Master schedules (current year), resource management and monitoring, meeting and travel support, special sessions

Frank Gomez Web Manager Web server administration, mail system maintenance, Data Center support, session processing

scripts, mirror site liaison

Karen Baver General Programmer

and Editor

Publication processing programs, LaTeX support and editing, session Web page support and

scripts

IVS 2011 Annual Report 19
IVS Coordinating Center NASA Goddard Space Flight Center

5. Plans for 2012

The Coordinating Center plans for 2012 include the following:

• Maintain IVS Web site and e-mail system.

• Publish the 2011 Annual Report (this volume).

• Coordinate, with the local committee, the VLBI2010 Workshop on Technical Specifications

to be held in Bad K ̈otzting, Germany in March 2012.

• Coordinate, with the local committee, the seventh IVS General Meeting to be held in Madrid,

Spain in March 2012.

• Support Directing Board meetings in 2012.

• Coordinate the 2012 master observing schedules and IVS resources.

• Publish Newsletter issues in April, August, and December.

• Support the VLBI2010 activities of the V2C and V2PEG.

20 IVS 2011 Annual Report
Institut f ̈ur Geod ̈asie und Geoinformation der Universit ̈at Bonn IVS Analysis Coordinator

Analysis Coordinator Report

A. Nothnagel, T. Artz

Abstract

IVS analysis coordination issues in 2011 are reported here. Routine Earth orientation parameter

combinations on the basis of datum-free normal equations are being carried out by the IVS Combination

Center at BKG, Frankfurt a.M., Germany. The IVS Analysis Coordinator is responsible for consistency

of the input data and requires strict adherence to models and conventions.

1. General Issues

The “Twelfth IVS Analysis Workshop” was hosted by the Max-Planck-Institute for Radio

Astronomy in Bonn, Germany, on March 31, 2011, in connection with the 20th Meeting of the

European VLBI Group for Geodesy and Astrometry (EVGA). The coordination of IVS routine

data analysis was discussed as well as developments for improving geodetic and astrometric data

analysis in general.

The timeliness of the submission of the SINEX files from the operational IVS Analysis Centers

(ACs) to the IVS Data Centers has improved considerably since the last report, although individual

analysis centers still attract attention by not providing input according to their initial proposals.

With more operational analysis centers coming online, the less reliable ACs may be subject to a

more rigorous assessment.

It is well known that the treatment of the sub-daily tidal Earth rotation parameter variations

and the introduction of harmonic site position variations may generate alias effects in the daily

EOP time series. During the Analysis Workshop, Thomas Artz presented an empirical sub-daily

EOP model combined from VLBI and GPS observations [1]. This model comprises the strengths

of both techniques and compensates at least some of the deficits which are inherent to empirical

models. The model should be tested by the IVS ACs for use in routine IVS data analysis.

The attendants of the meeting discussed the impact of the IERS Conventions 2010 [5] on IVS

analyses. The main issues are the new mean pole model, the S1/S2 tides, the Earth’s libration,

and the ocean pole tide. These effects are already included in the Calc/Solve analysis package and

should also be incorporated into the other independent packages.

Concerning atmospheric gradient modelling, there are two models available, the so-called

Macmillan model [3] and the Chen and Herring model [2]. They are very similar in formulation and in the results, but a consistent use of one of these two models throughout the IVS should

be achieved. For the decision, it should be taken into account that the IGS uses the Chen and

Herring model and that for combination of VLBI results with GPS the models should be identical.

It was agreed that it would be advisable to use the Chen and Herring model as the IVS conventional model but that tests will have to be done on the impact of such a move. The results should

be discussed at the next IVS Analysis Workshop in Madrid in 2012.

The decision on the a priori gradients was less critical. All participants agreed unanimously

that the Goddard Data Assimilation Office (DAO) results should be used as the conventional IVS

a priori gradient model. Nothing has happened concerning the reference pressure for atmospheric

loading, which is under the responsibility of the Special Bureau of Loading of the International

Earth Rotation and Reference Systems Service (IERS).

IVS 2011 Annual Report 21
IVS Analysis Coordinator Institut f ̈ur Geod ̈asie und Geoinformation der Universit ̈at Bonn

2. IVS Operational Data Analysis and Combination

Since October 1, 2009, the operational combination has been carried out by the IVS Combination Center at the German Bundesamt f ̈ur Kartographie und Geod ̈asie (BKG) in Frankfurt a.M.

(see separate report by BKG/DGFI). The input to these combinations are datum-free (constraintfree) normal equation systems in SINEX format (Solution Independent Exchange format). The

nutation representation in the IAU2000 paradigm, dX and dY , is now the standard. For users of

the old system, a separate table is generated through a transformation.

At the 12th IVS Analysis Workshop it was also agreed by all participants that the SINEX files

reported to the Combination Center have to include the elements of the normal equation system

for the positions of the radio sources. So far, this is done routinely only by three IVS ACs but

others will follow step by step. Investigations are being carried out to determine how this affects

the combination and what benefits can be drawn from this additional information in the normal

equation systems.

At present, the combination product is still dominated by input from the Calc/Solve software.

For good combination products it is, however, important that results from many different software

packages be contributed. If the same analysis software is used, it is important that the analyses

are independent and that the analysts create their solutions with their own approach. The IVS

Analysis Coordinator has, therefore, established a new template for the analysis description that

accompanies the solutions. This template gives a deeper insight into the genuine nature of each

contribution.

Further details of radio telecopes have been collected in the antenna information file under

http://vlbi.geod.uni-bonn.de/IVS-AC/Conventions. The background of the thermal expansion

models is described in [4].

3. Personnel

Table 1. Personnel at the IVS Analysis Coordinator’s office

Axel Nothnagel +49-228-733574 nothnagel@uni-bonn.de

Thomas Artz +49-228-733563 thomas.artz@uni-bonn.de

References

[1] T. Artz, L. Bernhard, A. Nothnagel, P. Steigenberger, and S. Tesmer (2011). Methodology for the combination of sub-daily Earth rotation from GPS and VLBI observations. J Geod. DOI: 10.1007/s00190-

011-0512-9.

[2] G. Chen, and T.A. Herring (1997) Effects of atmospheric azimuthal asymmetry on the analysis of space

geodetic data. J Geophys Res, Vol. 102, No. B9, pp. 20489-20502, doi: 10.1029/ 97JB01739

[3] D. S. MacMillan (1995) Atmospheric gradients from very long baseline interferometry observations.

Geoph Res Letters, Vol. 22, No. 9, pp. 1041-1044, doi: 10.1029/95GL00887

[4] Nothnagel A. (2009) Conventions on thermal expansion modelling of radio telescopes for geodetic and

astrometric VLBI. J. Geod 83(8):787–792, doi:10.1007/s00190-008-0284-z

22 IVS 2011 Annual Report
Institut f ̈ur Geod ̈asie und Geoinformation der Universit ̈at Bonn IVS Analysis Coordinator

[5] IERS Conventions (2010) G ́erard Petit and Brian Luzum (eds.). (IERS Technical Note 36) Verlag des

Bundesamts f ̈ur Kartographie und Geod ̈asie, Frankfurt am Main, 2010. ISBN 3-89888-989-6

IVS 2011 Annual Report 23
Network Coordinator NVI, Inc./GSFC

Network Coordinator Report

Ed Himwich

Abstract

A brief report on network performance is presented. Most of network operations went well. Some

positive developments are identified. There were a few significant problems, mostly with antennas and

receivers. New antennas in Australia and New Zealand started observing. New antennas are under

development in the USA. There are prospects for Korea, India, and Saudi Arabia to start contributing

to IVS. Other activities of the Network Coordinator are summarized.

1. Network Performance

The overall network performance was for the most part good. As occurred last year, this year’s

report does not include the usual detailed assessment of overall network performance (but we hope

to include it again next year). However, the usual average single station loss of 10-20% probably

occurred again this year.

One of the positive developments this year is the increased use of e-transfer with data from Ny-

 ̊Alesund, Fortaleza, AuScope, and Warkworth now being largely e-transferred. This speeds data

transfer and reduces shipping costs. Another positive development is that Mark 5B recorders were

installed at several stations. This improves correlator efficiency. A third development is that digital

back-ends are starting to be used at more stations for operations. The DBBC developed by the

EVN is being used at Hobart, Katherine, Yarragadee, and Warkworth (which is another positive

development—the latter three stations just started observing this year). The Haystack/NRAOdeveloped RDBE is nearing readiness for observations and is expected to start being used in 2012.

Overall, while the network operated well for the most part, there are a few notable issues (in

alphabetical order), while some situations improved from the previous year:

• Badary, Svetloe, and Zelenchukskaya had intermittent antenna problems that caused occasional data losses.

• Fortaleza started observing again after being off the air for more than a year. Its SEFDs are

now a little higher than before. This may be related to increases in local RFI.

• Hobart, Katherine, and Yarragadee have timing issues with the DBBC back-ends. These

cause occasional clock breaks and data gaps when they occur. The manufacturer is investigating this issue.

• Kokee Park’s damaged gearbox was repaired and was re-installed. This improved the antenna’s pointing and its SEFDs but did not return them to their normal levels. There are

still problems with both azimuth gearboxes that will need to be repaired.

• Matera repaired its X-band cryogenic system.

• The receiver at Medicina warmed up in November 2011. It is not clear when it will be

repaired.

• Noto is repairing its bearing and is expected to return to operations in the spring of 2012.

• Ny- ̊Alesund has had higher than normal SEFDs since about May 2010. The cause of this

was found and repaired.

24 IVS 2011 Annual Report
NVI, Inc./GSFC Network Coordinator

• Ny- ̊Alesund’s receiver communications has failed. A back-up system is being used to control

the noise diode for system temperature measurements until the receiver can be repaired.

Otherwise this is not currently impacting operations.

• TIGO has shown higher than normal SEFDs for several years. There has been no success in

resolving this issue.

2. New Stations

There are prospects for new stations on several fronts. These include (in approximate order of

how soon they will start regular observations):

• At Wettzell in Germany, construction of the new Twin Telescope Wettzell (TTW) for

VLBI2010 is underway.

• At GSFC in the USA, a new 12-m antenna has been erected and is undergoing testing. While

this antenna is primarily for use in the development of the VLBI2010 systems, it is expected

that it will eventually join the network for regular observing.

• At Arecibo in Puerto Rico a new 12-m antenna has been erected and is expected to be used

for geodetic observing.

• In Spain/Portugal, the RAEGE (Atlantic Network of Geodynamical and Space Stations)

project aims to establish a network of four fundamental geodetic stations including radio

telescopes that will fulfill the VLBI2010 specifications: Yebes (1), Canary Islands (1), and

Azores (2).

• In Norway, the Norwegian Mapping Authority (NMA) has received initial funding for a

project to establish a fundamental station at Ny- ̊Alesund, which will include a twin telescope

of the Wettzell type.

• Onsala has applied for funds for a twin telescope system.

• In Russia, an effort is underway to get 12-m VLBI2010 antennas at some of the QUASAR

network sites.

• Korea is planning to build one antenna primarily for geodesy (Korea VLBI system for

Geodesy, KVG) at Sejong. There is also interest in geodetic use of the Korean VLBI Network

(KVN), which will consist of three stations intended primarily for astronomy.

• There is interest in India in building a network of four telescopes that would be useful for

geodesy.

• Saudi Arabia is investigating having a combined geodetic observatory, which would presumably include a VLBI antenna.

• Colombia is investigating having a combined geodetic observatory, which would presumably

include a VLBI antenna.

Many of these antennas may become available for use in the next few years. Efforts are being

made to ensure that these antennas will be compatible with VLBI2010.

IVS 2011 Annual Report 25
Network Coordinator NVI, Inc./GSFC

3. Network Coordination Activities

Network coodination involved dealing with various network and data issues. These included:

• Reviewing all experiment “ops” messages, correlator reports, and analysis reports for problems and working with stations to resolve them

• Responding to requests from stations for assistance

• Identifying network station issues and working with the Coordinating Center and stations to

get them resolved. This year these included:

– Dealing with Mark 5 recording problems

– Adjusting procedures for correct monitoring of Mark 5 timing

– Implementing strong passwords for Mark 5 systems

– Identifying incorrect resistors on Mark 5 motherboards

– Preparing Mark 5 modules for use and correcting VSN problems

– Checking Mark 5 modules for correct alignment

– Maintaining FS PC kernel

• Planning for possible USA government shutdowns and providing alternate servers for operational data and messages

• Collecting information for RFI protection of sites

• Participating in development of the new VEX2 schedule file standard

• Helping to coordinate Mark 5B transitions at Kokee, Ny- ̊Alesund, TIGO, Matera, and HartRAO

• Developing a database of Mark 5 recorder version information to help identify station capabilities and which stations need upgrades to be compliant

• Assisting with Warkworth antenna calibration

• Preparations and support for CONT11, including:

– Preparing plans for handling cable wrap issues at schedule change and break times.

These can be avoided in the future if schedules are built continuously across day changes

and if the tag-along observations during station breaks are built into the original schedule instead of being added afterwards.

– Identifying stations unable to support SATA modules and developing work-arounds so

all scheduled data can be recorded on available modules.

– Preparing station test procedures and reviewing results from stations.

– Assisting with problems during experiments.

• Updating RDV experiment VEX files to allow proper operation with the VLBA correlator,

updating the notes file to reflect equipment set-up at different stations, and encouraging

timely shipping of data.

• Installing software to support a MET3 instrument at Westford.

26 IVS 2011 Annual Report
NVI, Inc./GSFC Network Coordinator

4. Future Activities

Network coordination activities are expected to continue next year. The activities will largely

be a continuation of the previous year’s activities:

• Reviewing all experiment “ops” messages, correlator reports, and analysis reports for problems and working with stations to resolve them

• Responding to requests from stations for assistance

• Identifying network station issues and working with the Coordinating Center and the stations

to get them resolved.

• Updating Network Station configuration files.

• Other activities as needed.

IVS 2011 Annual Report 27
IVS Technology Coordinator Report MIT Haystack Observatory

IVS Technology Coordinator Report

Alan Whitney

Abstract

The efforts of the Technology Coordinator in 2011 include the following areas: 1) support of work

to implement the new VLBI2010 system, 2) e-VLBI development, 3) continuing development of global

VLBI standards, 4) DiFX software correlator for geodetic-VLBI, and 5) creation of a new VLBI technical resources webpage. We will briefly describe each of these activities.

1. VLBI2010 Progress

Progress continues towards the goal of a next-generation VLBI2010 system. Much more detailed

information about VLBI2010 development is presented elsewhere in this report; here we briefly

report some of the highlights:

1.1. Development of the VLBI2010 Broadband System

The VLBI2010 system continues to develop at several locations:

1. A pair of VLBI2010 13-m ‘twin-telescopes’ has been installed at Wettzell and is currently

under test. RMS surface accuracy is better than 60 micrometers, and the antenna and

subreflector are aligned. A tri-band feed will be installed soon, followed by measurements

of G/T and pointing tests. A new broadband “Eleven” feed and accompanying receiver and

recording systems will be installed in the latter half of 2012.

2. Development of firmware for the FILA10G board for the dBBC continues at MPIfR and

Metsahovi. This board is installed in the dBBC, developed by Gino Tuccari, to support bidirectional data-format conversions between VSI-H data format and 10GigE VDIF format.

3. The broadband ‘QRFH’ broadband feed from Caltech has been successfully tested on the

VLBI2010 prototype antenna at NASA/GGAO and will soon also be installed on the Westford antenna. Experimental results for beam patterns and efficiencies closely match theoretical predictions. The QRFH feed can be easily re-designed to accommodate a wide variety

of antenna geometries.

4. RDBE development continues at Haystack Observatory: The current working version accepts two 512 MHz IFs, channelizes each into fifteen adjacent 32 MHz-wide channels using

polyphase filter band (PFB) technology; the user can choose any 16 of these channels to be

sent to a 10GigE data link at an aggregate rate of 2 Gbps, which is then recorded on a Mark

5C data system in Mark 5B+ data format. A new ‘quad-band’ version under development

will accept up to four 512 MHz IFs, for an aggregate output rate of 4 Gbps. Support for Tsys

calibration has been completed and has been verified by tests at NRAO. A comprehensive set

of tests comparing the RDBE performance against an exact software model has been highly

successful, giving considerable confidence in its proper function.

5. Mark 5C VLBI data system: Mark 5C is now used routinely at 2 Gbps to a single 8-disk

module and will enter service at 4 Gbps in early 2012. A 16 Gbps COTS-based Mark 6 system

28 IVS 2011 Annual Report
MIT Haystack Observatory IVS Technology Coordinator Report

is under development at Haystack Observatory; a successful 16 Gbps VLBI experiment using

an early Mark 6 development system was conducted in November 2011. The Mark 6 is

projected to enter service in mid/late 2012.

6. A number of VLBI2010 data-taking sessions between Westford and NASA/GSFC were undertaken during 2011. Most were recorded onto four Mark 5C units at each station using

RDBE backend units as data sources, at an aggregate data rate of 8 Gbps/station. More of

the processing of VLBI2010 data continues to be moved from the Mark IV correlator to the

DiFX correlator at Haystack Observatory.

7. DiFX correlators at MPI, Haystack Observatory, and U.S. Naval Observatory continue to be

developed and used for processing geodetic-VLBI data.

2. e-VLBI Development

2.1. Continuing Expansion and Development of Routine e-VLBI Data Transfers

MPI continues regular e-VLBI transfers of data for which the Bonn correlator is the correlation

target. This includes data from Japan, Onsala, Ny- ̊Alesund, and Wettzell. All data recorded on

K5 system at Tsukuba and Kashima are transferred either to MPI or Haystack depending on the

target correlator. Syowa K5 data are physically shipped to Japan and electronically transferred

to Haystack or MPI. UT1 Intensive data from Wettzell, Japan, and Ny- ̊Alesund are transferred to

either MPI or the Washington correlator.

The Kokee station network connection is being upgraded from 100 Mbps to ∼600 Mbps to

enhance turnaround for daily UT1 observations. Haystack Observatory has recently upgraded its

network connection to 10 Gbps.

2.2. 10th International e-VLBI Workshop Held at South Africa

Participants in the 10th International e-VLBI Workshop (13-16 November 2011) were hosted

by our South African colleagues at a beautiful and remote conference several kilometers from the

Hartebeesthoek Radio Astronomy Observatory. The workshop was attended by 55 participants

from 19 countries, including five countries in Africa.

The theme of the meeting was “Towards Global Real-Time e-VLBI”. Within this context,

e-VLBI has a lot to offer as a pathfinder technology for the proposed SKA telescope, and the

presentations from both the e-VLBI and the SKA communities made for a particularly interesting

forum. The workshop was three days in duration, with the first two days dedicated to scientific and

technical presentations. The third day we were transported to the HartRAO observatory for tours

and more presentations, focusing heavily on establishing VLBI on the greater African continent.

A most enjoyable and useful meeting for all!

Presentations from the workshop are available on-line at http://www.hartrao.ac.za/e-vlbi2011/evlbi2011.html.

The 11th International e-VLBI Workshop will be held at MIT Haystack Observatory in Q3

2011.

IVS 2011 Annual Report 29
IVS Technology Coordinator Report MIT Haystack Observatory

Figure 1. Attendees of the 2011 International e-VLBI Workshop held at Amanzingwe Conference Center,

South Africa.

3. Global VLBI Standards

3.1. VLBI Standards Website Continues to Expand

http://www.vlbi.org has been established as a one-stop shop for access to global VLBI standards.

These include VEX, VSI-H, VSI-S, VDIF, and standardized VLBI file-naming conventions, plus a

brand new VLBI technical resources page. As new standards and technical VLBI resources emerge,

they will be included in this website.

3.2. VDIF Data Format

Adoption of the VLBI Data Interchange Format (VDIF), ratified in 2008 at the Madrid eVLBI workshop, continues to expand. The VLBI2010 project has adopted VDIF as the standard

data format, and work is proceeding to fully implement it. Several other data systems now in

development are also supporting the VDIF format, and VDIF is now moving strongly into the

astronomical world as well. Broad adoption of VDIF across various VLBI disciplines will allow for

more standardization and inter-operational capabilities that will benefit all of VLBI.

A VDIF2 data format is nearing completion to meet new demands, including the accommodation of arbitrary sample rates, including those that do not have an integral number of samples in a

single second. Such ‘non-standard’ sample rates are being designed into some of the SKA-related

systems that would like to participate in global VLBI. The new VDIF2 standard will also relax the

constraint of an integral number of filled data packets per second and allow much more flexibility

in the choice of packet lengths. This work should be completed by mid-2012.

3.3. VTP

A VLBI Transport Protocol (VTP) Task Force, led by Chris Phillips of ATNF, has developed

a proposed standard which is now under review and is expected to be ratified early in 2012.

3.4. VEX2 Task Force Continues Work

The VEX file format is a standardized method to prescribe a complete description of a VLBI

experiment, including setup, scheduling, data-taking and correlation, independent of any particular VLBI data-acquisition system or correlator. VEX has gained broad acceptance and is used to

30 IVS 2011 Annual Report
MIT Haystack Observatory IVS Technology Coordinator Report

support a large fraction of global VLBI observations, but it needs updating as new technologies

and equipment become available. The VEX2 Task Force was created in late 2009 to undertake

this job. The members of the VEX2 Task Force are Walter Brisken (NRAO, chair), Ed Himwich

(NASA/GSFC), Mark Kettenis (JIVE), Cormac Reynolds (Curtin University), and Alan Whitney

(MIT Haystack). This group continues working to craft the needed VEX updates and to incorporate them into several VLBI-support software packages. Again, the target for completion of this

work is sometime in 2012.

4. DiFX Software Correlator for Geodetic VLBI

The so-called DiFX software correlator was originally developed at Swinburne University in

Australia by Adam Deller, primarily for astronomical VLBI use. The development of an economical

and powerful software correlator, a dream less than a decade ago, has been made possible by the

relentless march of Moore’s Law to provide powerful inexpensive clustered PCs with high-speed

data interconnections that can distribute and correlate VLBI data in an efficient manner. Since

the original DiFX development several years ago, the use of the DiFX correlator has spread, and

a global DiFX user group has been formed to coordinate continued improvements and additions.

Several institutions that support geodetic-VLBI correlation processing now have DiFX correlators

(MPIfR, USNO, Haystack Observatory) and have been working to augment the core DiFX software

to meet the needs of geodetic-VLBI. This includes the integration of much of the Mark IV-correlator

software involving data-management, output data formats, fringe finding and delay estimates, and

editing/quality-assurance software. In addition, a substantial amount of work has been done to

integrate accurate multi-tone phase-calibration processing into the DiFX correlator, a task that is

often not important for astronomical VLBI.

Progress towards developing the necessary additions and improvements to DiFX for geodetic

VLBI has been rapid, allowing the DiFX correlator to take over the job of current hardware

correlators. MPIfR closed its Mark IV hardware correlator at the end of CY2010. Haystack

Observatory is planning to phase out its Mark IV correlator by the end of 2011, with USNO likely

to follow soon thereafter.

5. VLBI Technical Resources Web Page

A new webpage with links to many on-line VLBI technical resources is now available at

http://vlbi.org/resources.html. Presently 15 institutions worldwide have contributed to this webpage, and more are expected. If you are looking for technical information on a particular VLBI

system or subsystem, check here first!

IVS 2011 Annual Report 31

Network Stations

Network Stations

Institute of Applied Astronomy of Russian Academy of Sciences Badary Station

Badary Radio Astronomical Observatory

Sergey Smolentsev, Valery Olifirov

Abstract

This report provides information about the Badary network station: general information, facilities,

staff, present status, and outlook.

1. General Information

The Badary Radio Astronomical Observatory (Figure 1) was founded by the Institute of Applied Astronomy (IAA) as one of three stations of the Russian VLBI network QUASAR [1]. The

sponsoring organization of the project is the Russian Academy of Sciences (RAS). The Badary

Radio Astronomical Observatory is situated in the Republic Buryatia (East Siberia) about 130 km

east of Baikal Lake (see Table 1). The geographic location of the observatory is shown on the IAA

RAS Web site (http://www.ipa.nw.ru/PAGE/rusipa.htm). The basic instruments of the observatory are a 32-m radio telescope equipped with special technical systems for VLBI observations,

GPS/GLONASS/Galileo receivers, a DORIS antenna, and an SLR system installed in 2011.

Figure 1. Badary observatory.

Table 1. Badary Observatory location and address.

Longitude 102◦14

′

Latitude 51◦46

′

Badary Observatory

Republic Buryatia

671021, Russia

oper@badary.ipa.stbur.ru

IVS 2011 Annual Report 35
Badary Station Institute of Applied Astronomy of Russian Academy of Sciences

2. Technical Staff

Vladimir Shpilevsky — observatory chief,

Nicolay Mutovin — FS, pointing system control,

Roman Sergeev — main engineer,

Roman Kuptsov — main engineer.

3. Technical and Scientific Information

Characteristics of the radio telescope are presented in Table 2. The electrical part of the gear

and pointing system of the radio telescope was upgraded in 2008 — 2010. A new DAS R1002M

designed at the IAA [2, 3] has been used in all kinds of VLBI observational programs since October

2011.

Table 2. Technical parameters of the radio telescope.

Year of construction 2005

Mount AZEL

Azimuth range ±270◦(from south)

Elevation range from −5

◦

to 95◦

Maximum azimuth

- velocity 1.5

◦/s

- tracking velocity 1.5

′/s

- acceleration 0.2

◦/s2

Maximum elevation

- velocity 0.8

◦/s

- tracking velocity 1.0

′/s

- acceleration 0.2

◦/s2

Pointing accuracy better than 10′′

Configuration Cassegrain

(with asymmetrical subreflector)

Main reflector diameter 32 m

Subreflector diameter 4 m

Focal length 11.4 m

Main reflector shape quasi-paraboloid

Subreflector shape quasi-hyperboloid

Main reflector surface accuracy ± 0.5 mm

Frequency range 1.4–22 GHz

Axis offset 2.5 ± 0.5 mm

36 IVS 2011 Annual Report
Institute of Applied Astronomy of Russian Academy of Sciences Badary Station

4. Co-location of VLBI, GPS/GLONASS, DORIS and SLR System

The Topcon GPS/GLONASS/Galileo receiver with automatic meteorological station WXT-510

was tested and put into operation (Figure 2).

Figure 2. Topcon GPS/GLONASS/Galileo receiver at the Badary observatory.

The SLR system “Sazhen-TM” (Figure 3) was mounted in July 2011. The “Sazhen-TM” SLR

system was manufactured by Open Joint-stock Research-and-Production Corporation “Precision

Systems and Instruments”. Technical parameters of the system are presented in Table 3.

Figure 3. “Sazhen-TM” SLR system at Badary observatory.

IVS 2011 Annual Report 37
Badary Station Institute of Applied Astronomy of Russian Academy of Sciences

Table 3. Technical parameters of the SLR system “Sazhen-TM”.

Ranging distance, day 400-6000 km

Ranging distance, night 400-23000 km

Aperture 25 cm

Wavelength 532 nm

Beam divergence 12′′

Laser pulse frequency 300 Hz

Pulse energy 2.5 mJ

Mass 170 kg

Normal points precision 1 cm

Angular precision 1-2′′

5. Current Status and Activities

Badary observatory participates in IVS and domestic VLBI observational programs. During

2011 Badary station participated in 44 diurnal IVS sessions — IVS-R1, IVS-R4, IVS-T2, EURO,

and IVS-CONT11.

Badary participated in 49 diurnal sessions in the frame of the domestic Ru-E program for

determination of all Earth orientation parameters, and in 55 one-hour Ru-U sessions for obtaining

Universal Time using e-VLBI data transfer.

6. Outlook

Our plans for the coming year are the following:

• To participate in IVS observations

• To carry out domestic observational programs for obtaining Universal Time with e-VLBI

data transfer and Earth orientation parameters once a week

• To carry out SLR observations of geodetic and navigation satellites

• To participate in EVN and RADIOASTRON observational sessions

• To continue geodetic monitoring of the antenna parameters.

References

[1] Finkelstein A., Ipatov A., Smolentsev S. The Network “Quasar”: 2008 — 2011 // “Measuring the

future”, Proc. of the Fifth IVS General Meeting, A. Finkelstein, D. Behrend (eds.), St. Petersburg,

“Nauka”, 2008. pp. 39–46.

[2] Grenkov S. A., Nosov E. V., Fedotov L. V., Koltsov N. E. A Digital Radio Interferometric Signal

Conversion System // Instruments and Experimental Techniques, 2010. Vol. 53, No. 5. pp. 675–681.

[3] Nosov E. Next-Generation DAS for the Russian VLBI-Network. // 20th EVGA Meeting. MPIfR, Bonn.

2011. pp. 41–43.

38 IVS 2011 Annual Report
CRAAM, Universidade Presbiteriana Mackenzie, S ̃ao Paulo Fortaleza

Fortaleza Station Report for 2011

Pierre Kaufmann, A. Mac ́ılio Pereira de Lucena, Adeildo Sombra da Silva

Abstract

This is a brief report about the activities carried out at the Fortaleza geodetic VLBI station (ROEN:

R ́adio Observat ́orio Espacial do Nordeste), located in Eus ́ebio, CE, Brazil, during the period from January until December 2011. The observing activities were resumed in May after the major maintenance

that comprised the azimuth bearing replacement. The total observational experiments consisted of

73 VLBI sessions and continuous GPS monitoring recordings. Fortaleza station participated in the

CONT11 campaign. Around 90% of the VLBI data has been transferred to the correlators through a

high speed network.

1. General Information

The R ́adio Observat ́orio Espacial do Nordeste, ROEN, located at INPE facilities in Eus ́ebio,

nearly 30 km east of Fortaleza, Cear ́a State, Brazil, began operations in 1993. Geodetic VLBI

and GPS observations are carried out regularly, as contributions to international programs and

networks. ROEN is part of the Brazilian space geodesy program, which was initially conducted by

CRAAE (a consortium of the Brazilian institutions Mackenzie, INPE, USP, and UNICAMP) in the

early 1990s. The program began with antenna and instrumental facility installations, with activities sponsored by the U.S. agency NOAA and the Brazilian Ministry of Science and Technology’s

FINEP agency. ROEN is currently coordinated by CRAAM, Center of Radio Astronomy and Astrophysics, Engineering School, Mackenzie Presbyterian University, S ̃ao Paulo, in agreement with

the Brazilian National Space Research Institute, INPE. The activities were later carried out under an Agreement of Cooperation signed between NASA—representing research interests of NOAA

and USNO—and the Brazilian Space Agency, AEB. This Agreement has been extended until 2021.

Under the auspices of this NASA-AEB Agreement, contracts have been signed between NASA and

CRAAM, Mackenzie Presbyterian Institute and University to partially support the activities at

ROEN. The present contract holds until 2014. The counterpart of the operational costs, staff, and

support of infrastructure are provided by INPE and by Mackenzie.

2. Main Instruments

The largest instrument at ROEN is the 14.2-m radio telescope, on an alt-azimuth positioner. It

is operated at S- and X-bands, using cryogenic radiometers. The system is controlled by the Field

System, Version 9.10.4. Observations are recorded with a Mark 5 system. One Sigma-Tau hydrogen

maser clock standard is operated at ROEN. GPS monitoring is performed within a cooperative

program with NOAA (USA). There is a Leica System 1200 installed at the station that operates

continuously. The collected data are provided to the NOAA/IGS center and to the Brazilian IBGE

center. ROEN has all basic infrastructures for mechanical, electrical, and electronic maintenance

of the facilities.

IVS 2011 Annual Report 39
Fortaleza CRAAM, Universidade Presbiteriana Mackenzie, S ̃ao Paulo

Figure 1. Receiver box being removed for maintenance.

3. Staff

The Brazilian space geodesy program is coordinated by one of the authors (PK), who is Brazil’s

AEB representative in the NASA-AEB Agreement. The coordination receives support from the

S ̃ao Paulo office at CRAAM/Instituto and Universidade Presbiteriana Mackenzie, with administrative support given by Valdomiro S. Pereira and Luc ́ıola Russo. The Fortaleza Station facilities and geodetic VLBI and GPS operations are managed on site by Dr. A. M. P. de Lucena

(CRAAE/INPE), assisted by Eng. Adeildo Sombra da Silva (CRAAE/Mackenzie), and the technicians Avicena Filho (CRAAE/INPE) and Karlos Daniel Menezes (CRAAE/Mackenzie).

4. Current Status and Activities

4.1. VLBI Observations

In the year 2011, Fortaleza carried out geodetic VLBI experiments as listed in Table 1.

Table 1. 2011 session participation.

Experiment Number of Sessions

IVS-R1 15

IVS-R4 27

IVS-T2 02

IVS-R&D 02

IVS-RDV 04

IVS-CRF 02

IVS-CONT11 15

IVS-CRMS 01

IVS-OHIG 03

40 IVS 2011 Annual Report
CRAAM, Universidade Presbiteriana Mackenzie, S ̃ao Paulo Fortaleza

4.2. Operational and Maintenance Activities

The summary of activities performed in the period is listed below:

1) Supervision of azimuth bearing replacement and antenna painting service;

2) Installation of the new cryogenic system;

3) Re-installation of the receiver box;

4) Repair and maintenance of the following equipment: shaft encoder, FS computer, temperature controller and IF distributor, Mark IV formatter;

5) Maintenance and adjustment of DC azimuth and elevation motors;

6) Re-making of the antenna pointing model;

7) Tests of the antenna, receiver electronics, data acquisition and recording systems for the

CONT11 campaign;

8) Installation and tests of the Mark IV decoder;

9) Operation and maintenance of geodetic GPS (NOAA within the scope of NASA contract);

10) Operation and maintenance of power supply equipment at the observatory (main and diesel

driven standby);

11) Maintenance of the Web site (http://www.roen.inpe.br) and the local server computer.

4.3. GPS Operations

The IGS network GPS receiver operated regularly at all times during 2011. Data were collected

and uploaded to an IGS/NOAA computer.

5. Future Plans

Plans for the immediate future consist of the continuation of geodetic VLBI regular observations and the support of GPS receiver operations. Further progress is expected to expand data

transmission via high speed national and international networks.

Acknowledgements

The activities have received partial support from NASA, within an agreement with the Brazilian

Space Agency (AEB) and a NASA contract with Mackenzie. They are part of an agreement

between Mackenzie and INPE.

IVS 2011 Annual Report 41
Goddard Geophysical and Astronomical Observatory NASA Goddard Space Flight Center

Goddard Geophysical and Astronomical Observatory

Ricardo Figueroa, Wendy Avelar

Abstract

This report summarizes the technical parameters and the technical staff of the VLBI system at

the fundamental station GGAO. It also gives an overview about the VLBI activities during the report

year.

Figure 1. Goddard Geophysical and Astronomical Observatory.

1. GGAO at Goddard

The Goddard Geophysical and Astronomical Observatory (GGAO) consists of a 5-meter radio

telescope for VLBI, a new 12-meter radio telescope for VLBI2010 development, a 1-meter reference

antenna for microwave holography development, an SLR site that includes MOBLAS-7, the NGSLR

development system, and a 48′′ telescope for developmental two-color Satellite Laser Ranging, a

GPS timing and development lab, a DORIS system, meteorological sensors, and a hydrogen maser.

In addition, we are a fiducial IGS site with several IGS/IGSX receivers.

GGAO is located on the east coast of the United States in Maryland. It is approximately 15

miles NNE of Washington, D.C. in Greenbelt, Maryland (Table 1).

42 IVS 2011 Annual Report
NASA Goddard Space Flight Center Goddard Geophysical and Astronomical Observatory

Table 1. Location and addresses of GGAO at Goddard.

Longitude 76.4935◦ W

Latitude 39.0118◦ N

MV3

Code 299.0

Goddard Space Flight Center (GSFC)

Greenbelt, Maryland 20771

http://cddisa.gsfc.nasa.gov/ggao/vlbi.html

2. Technical Parameters of the VLBI Radio Telescopes at GGAO

The 5-m radio telescope for VLBI (MV3) was originally built as a transportable station; however, it was moved to GGAO in 1991 and has been used as a fixed station. In the winter of 2002

the antenna was taken off its trailer and permanently installed at GGAO.

In October 2010, construction of the new 12-meter VLBI2010 developmental antenna was

completed. This antenna features all electric drives and a Cassegrain feed system. Integration of

the broadband receiver and the associated sub-systems is underway as a joint effort between ITT

Exelis and the MIT Haystack Observatory.

The technical parameters of the radio telescopes are summarized in Table 2.

Table 2. Technical parameters of the radio telescopes at GGAO.

Parameter 5m 12m

Owner and operating agency NASA NASA

Year of construction 1982 2010

Diameter of main reflector d 5m 12m

Azimuth range ±270◦ ±270◦

Azimuth velocity 3

◦/s 5◦/s

Azimuth acceleration 1

◦/s2 1◦/s2

Elevation range ±90

◦ 5 − 88◦

Elevation velocity 3

◦/s 1.25◦/s(Avg.)

Elevation acceleration 1

◦/s2 1◦/s2

Receiver System

Focus Cassegrain Cassegrain

Receive Frequency 2 − 14GHz 2 − 14GHz

Tsys 100 K 50 K(Theoretical)

Bandwidth 512MHz, 4 bands 512MHz, 4 bands

G/T 26 dB/K 43 dB/K

VLBI terminal type VLBI2010 VLBI2010

Recording media Mark 5C Mark 5C

IVS 2011 Annual Report 43
Goddard Geophysical and Astronomical Observatory NASA Goddard Space Flight Center

3. Technical Staff of the VLBI Facility at GGAO

GGAO is a NASA R&D and data collection facility. On April 9, 2011 the NENS contract

transitioned to the SCNS contract operated by ITT Exelis Information Systems. Wendy Avelar

conducts VLBI operations and maintenance at GGAO with the support of Ricardo Figueroa, Katie

Pazamickas, and Charles Kodak.

4. Status of MV3 at GGAO

MV3 continues on a full time basis to be a major component in the program to demonstrate

the feasibility of the VLBI2010 broadband delay concept. Working under the guidance of the MIT

Haystack Observatory, MV3 has played a critical role in the advancement of the VLBI2010 project.

MV3 is configured with the prototype VLBI2010 broadband receiver originally installed in 2009.

The 5-m antenna is primarily used to support the holography effort.

Much of the 2011 activities at GGAO have been focused on the performance testing of the

VLBI2010 antenna. There were some other activities worth noting:

• Wideband system testing and characterization of the 5-m antenna.

• Procurement of new test equipment for characterization of the wideband RF hardware.

• Broadband Phase Cal unit was installed and under test on the 12-m antenna.

• Testing of three different feed designs for future Broadband use.

• Elevation creep monitoring and prevention.

• Use of Mark 6 recorders to demonstrate 16 Gigabit per second with Westford.

• QRFH feed installed.

• Antenna efficiency significantly improved by adjustment of subreflector and feed positions.

• System temperature, efficiency, and SEFD exceeded nominal values.

• Proof of concept/value of high frequency optical fiber link.

• Refinement of maintenance procedures/schedules for the antenna system.

The holographic imaging capability, which is being developed by the MIT Haystack Observatory

with support from ITT Exelis, was suspended during 2011. Activity will begin early in 2012 in order

to understand antenna deformations that could potentially dilute the accuracy of the VLBI2010

system. Initially holographic data collections were performed using the 5-m dish as the antenna to

be tested and a 1-m satellite receiving dish as the phase reference. Preliminary results from 2010

data collection show that the imaging technique was able to faithfully reconstruct deformations in

the aperture of the primary reflector. These deformations included GPS antennas mounted on the

rim of the dish, an RF absorbing block, the offset feed Water Vapor Radiometer (WVR) cover,

and the subreflector in the center of the primary as shown in Figure 2.

5. Outlook

GGAO will continue to support VLBI2010, e-VLBI, and other developmental activities during

the upcoming year. Tentative plans for 2012 include:

44 IVS 2011 Annual Report
NASA Goddard Space Flight Center Goddard Geophysical and Astronomical Observatory

Figure 2. Holographic imaging of the 5-m antenna.

• Install the new VLBI2010 broadband receiver system onto the 12-m antenna.

• Short baseline ties between the 5-m and 12-m antennas.

• Continue testing of the new broadband phase calibrator for the VLBI2010 system.

• Continue holographic imaging of the 5-m and 12-m antennas.

• Continue broadband observations and testing of the VLBI2010 system.

• Continue integration of the RDBEs and Mark 5Cs to replace DBE1s and Mark 5B+s.

• Install newly designed positioner for Dewar and Post-Dewar electronics.

• Test new capabilities of the RDBE digital back end: noise diode switches control and synchronous power measurements for system temperature; use of sign-bit for phase cal monitoring and system diagnosis.

• Implement and use new Mark 6 recorder.

• Use holography to check the position and alignment of the 12-m subreflector.

• Measure the baseline between the 5-m and the 12-m antennas for position tie for the reference

frame.

• Continue to monitor elevation creep and evaluate solutions.

• Investigate/resolve problems encountered with cold weather related performance of the 5-m

and 12-m elevation axis controller.

IVS 2011 Annual Report 45
Hartebeesthoek Radio Astronomy Observatory (HartRAO) HartRAO, NRF

Hartebeesthoek Radio Astronomy Observatory (HartRAO)

Marisa Nickola, Jonathan Quick, Ludwig Combrinck, Mike Gaylard

Abstract

HartRAO provides the only fiducial geodetic site in Africa, and it participates in global networks

for VLBI, GNSS, SLR, and DORIS (located at the adjoining South African National Space Agency

Earth Observation (SANSA EO)). This report provides an overview of the geodetic VLBI activities

and HartRAO’s 50th anniversary during 2011.

1. Geodetic VLBI at HartRAO

Hartebeesthoek is located 65 kilometers northwest of Johannesburg, just inside the provincial

boundary of Gauteng, South Africa. The nearest town, Krugersdorp, is 32 km distant. The

telescope is situated in an isolated valley which affords protection from terrestrial radio frequency

interference. HartRAO currently uses a 26-meter equatorially mounted Cassegrain radio telescope

built by Blaw Knox in 1961. The telescope was part of the NASA deep space tracking network

until 1974 when the facility was converted to an astronomical observatory. The telescope is colocated with an ILRS SLR station (MOBLAS-6), an IGS GNSS station (HRAO), and an IDS

DORIS station (HBMB) at the adjoining South African National Space Agency Earth Observation

(SANSA EO) site. HartRAO became a full member of the EVN on the 11th of May 2011.

Figure 1. The 26-m antenna and 15-m KAT-prototype antenna, IGS GPS antenna, NASA Moblas-6 SLR

and LLR under development. (Credit: L. Combrinck)

46 IVS 2011 Annual Report
HartRAO, NRF Hartebeesthoek Radio Astronomy Observatory (HartRAO)

2. Technical Parameters of the 26-m Telescope of HartRAO

Table 1 contains the technical parameters of the HartRAO 26-m radio telescope and the 15-m

Karoo Array Telescope (KAT) prototype antenna, while Table 2 contains technical parameters of

the HartRAO 26-m radio telescope’s receivers. The current data acquisition system consists of a

Mark 5 terminal and a Mark 5B recorder.

Table 1. Antenna parameters.

Parameter HartRAO 26-m HartRAO 15-m

Owner and operating agency HartRAO HartRAO

Year of construction 1961 2007

Radio telescope mount Offset equatorial Az-El

Receiving feed Cassegrain Prime focus

Diameter of main reflector d 25.914 m 15 m

Focal length f 10.886 m 7.5 m

Focal ratio f/d 0.424 0.5

Surface error of reflector (RMS) 0.5 mm ∼ 2.5 mm

Short wavelength limit 1.3 cm 2 cm

Pointing resolution 0.001◦ 0.001◦

Pointing repeatability 0.004◦ not tested

Slew rate on each axis HA: 0.5

◦

s

−1 Az: 2◦

s

−1

Dec: 0.5

◦

s

−1 El: 1◦

s

−1

Table 2. 26-m receiver parameters with dichroic reflector (DR), used for simultaneous S-X VLBI, off or on.

Parameter X-band S-band

Feeds dual CP conical dual CP conical

Amplifier type cryo HEMT cryo HEMT

Tsys (DR off) (K) 60 44

Tsys (DR on) (K) 70 50

SSEF D (DR off) (Jy) 684 422

SSEF D (DR on) (Jy) 1330 1350

Point source sensitivity (DR off) (Jy/K) 11.4 9.6

Point source sensitivity (DR on) (Jy/K) 19 27

3 dB beamwidth (◦) 0.092 0.332

3. Current Status

A bearing replacement before age 50 did not hamper the performance of the HartRAO 26-m

radio telescope. Position time series solutions indicate that the repair of the 26-m’s south polar

bearing did not cause any noticeable shift in the telescope’s position. During September 2011,

shortly after celebrating its 50th birthday on the 1st of July 2011, the 26-m successfully participated

IVS 2011 Annual Report 47
Hartebeesthoek Radio Astronomy Observatory (HartRAO) HartRAO, NRF

in the CONT11 campaign, needing to make use of only one of the scheduled maintenance periods.

Earlier the data acquisition system was upgraded with a Mark 5 (VSI-4) sampler and the recorder

upgraded to Mark 5B, with the first experiment following the upgrade taking place on the 11th of

July. Another first was the commencement of e-transfers of geodetic VLBI data starting on the

21st of February 2011 with R1 data destined for the Bonn correlator. Telescope time allocation for

geodetic VLBI was increased to 63 24-hour experiments in 2011 to include the CONT11 campaign

(Table 3). Table 4 lists the HartRAO station staff who are involved in geodetic VLBI. Jonathan

Quick (VLBI friend) provides technical support for the Field System as well as for hardware

problems. Further progress was made with the conversion of the 15-m KAT prototype to a geodetic

VLBI capable antenna with the new co-axial dual circular polarization S/X (2.3 and 8.4 GHz)

prime-focus cryogenic receiver now successfully calibrated in laboratory tests, showing average

system temperatures of ∼32K at S and ∼29K at X. In preparation for the installation of the S/X

receiver, the original XDM (eXperimental Design Model) multi-feed receiver system “Stargate”

and its parallactic rotation stage have been removed from the 15-m’s prime focus, and installation

of helium and vacuum lines is in process.

Table 3. Geodetic VLBI experiments HartRAO

participated in during 2011.

Experiment Number of Sessions

R1 26

CONT11 15

CRDS 6

RDV 5

RD 4

OHIG 3

CRF 2

T2 2

Total 63

Table 4. Staff supporting geodetic VLBI at

HartRAO.

Name Function Program

L. Combrinck Program Geodesy

Leader

J. Quick Hardware/ Astronomy

Software

R. Botha Operator Geodesy

J. Grobler Operator Technical

L. Masongwa Operator Technical

R. Myataza Operator Technical

M. Nickola Logistics/ Geodesy

Operations

P.Stronkhorst Operator Technical

4. Future Plans

Conversion of the 15-m KAT prototype antenna for use in geodetic VLBI experiments should

hopefully be completed during early 2012. Two DBBC back-ends have recently arrived at HartRAO

and are undergoing acceptance testing. A spare Mark 5B+ recorder has also been procured with

a third recorder (for electronic data shipment) on order. The Lunar Laser Ranger (LLR) housing

has been completed, and refurbishment of the telescope and design of other LLR subsystems will

proceed during 2012.

48 IVS 2011 Annual Report
HartRAO, NRF Hartebeesthoek Radio Astronomy Observatory (HartRAO)

Figure 2. 15-m XDM’s S/X receiver package looking at sky during noise temperature tests. (Credit

K. Jones)

Figure 3. S/X receiver with integral feed to be installed at XDM prime focus. (Credit M. Nickola)

Figure 4. A coin minted in 1961 indicates the year

the foundation for the 26-m was laid. (Credit: M.

Gaylard)

Figure 5. Mechanical supervisor, Andr ́e van der

Merwe, inspects the LLR telescope and its housing.

(Credit: L. Combrinck)

Acknowledgements

The Space Geodesy Programme is an integrated program, combining VLBI, SLR, and GNSS,

and it is active in several collaborative projects with GSFC, JPL, and GFZ (Potsdam) as well as

numerous local institutes. Collaboration also includes CNES/GRGS/OCA and the ILRS community in a Lunar Laser Ranger (LLR) project with local support from the University of Pretoria

and the National Laser Centre (CSIR), among others. General information as well as news and

progress on geodesy and related activities can be found at http://geodesy.hartrao.ac.za/.

IVS 2011 Annual Report 49
Hobart 12-m and 26-m, Katherine and Yarragadee University of Tasmania

AuScope VLBI Project and Hobart 26-m Antenna

Jim Lovell, John Dickey, Brett Reid, Jamie McCallum, Stas Shabala, Simon Ellingsen

Abstract

This is a report on the activities carried out at the three AuScope VLBI observatories and the

Hobart 26-m antenna. In 2011 the AuScope 12-m antenna at Hobart (Hb) completed its first full

year of operations while the Katherine (Ke) and Yarragadee (Yg) antennas were commissioned and

commenced operation. The Hobart 26-m antenna (Ho) continued to make a contribution to IVS,

providing overlap with the Hb time series. The Hobart 12-m also participated in the 15-day CONT11

campaign in September. In total the AuScope antennas and the Hobart 26-m observed for 171 antenna

days in 2011.

1. Introduction

In 2006 the National Collaborative Research Infrastructure Strategy (NCRIS) initiated program

5.13, “Structure and Evolution of the Australian Continent”, which is funded by the Australian

Federal Government’s Department of Innovation, Industry, Science and Research (DIISR) and

managed by AuScope Ltd. (www.auscope.org.au). A major component of this project was the establishment of a national geospatial framework to provide an integrated spatial positioning system

spanning the whole continent. Total federal funding for this undertaking is AUD$15.8M, together

with AUD$21M from universities, state governments and Geoscience Australia. The infrastructure

that was funded to achieve this improvement to the geospatial framework included:

• three 12-meter radio telescopes and a software correlator

• approximately 100 GNSS receivers

• an upgrade of existing SLR facilities

• an absolute gravimeter and three tidal gravimeters

• improved computing facilities

2. VLBI Facilities

As part of this effort, the University of Tasmania (UTAS) has constructed three new radio telescopes, located near Hobart (Tasmania), Yarragadee (Western Australia), and Katherine (Northern

Territory). UTAS is responsible for construction and operation of these new VLBI sites (Figure 1).

The AuScope telescopes closely follow the International VLBI Service VLBI2010 specification for

the next generation of telescopes for geodesy (Petrachenko et al., 2009) or provide an upgrade path

to meet the specification where it is not currently possible to do so.

The new Hobart telescope (Hb) is co-located with the existing 26-m telescope (Ho) to preserve

the more than 20 year VLBI time series at the site. Midway between the 26-m and 12-m telescopes

is the HOB2 GNSS installation which has been a core site of the International GNSS Service (IGS)

since its conception. A hut capable of housing a mobile gravimeter is also co-located on the site.

The Yarragadee telescope (Yg) provides a far western point on the continent and is co-located with

multiple existing geodetic techniques including SLR, GNSS, DORIS and gravity. The Katherine

50 IVS 2011 Annual Report
University of Tasmania Hobart 12-m and 26-m, Katherine and Yarragadee

Figure 1. The geographical distribution of VLBI and GNSS infrastructure for AuScope. From west to east,

the new VLBI stations are at Yarragadee, Katherine, and Hobart. An additional ∼100 GNSS receivers will

be distributed across the continent.

IVS 2011 Annual Report 51
Hobart 12-m and 26-m, Katherine and Yarragadee University of Tasmania

site (Ke) is new and provides a central longitude, northern site. The telescope at Katherine is

co-located with a new GNSS site that forms part of the AuScope GNSS network.

Each AuScope VLBI observatory is equipped with a 12.1-m diameter main reflector designed

and constructed by COBHAM Satcom, Patriot Products division. The telescope specifications

include: 0.3 mm of surface precision (RMS), fast slewing rates (5 deg/s in azimuth and 1.25 deg/s

in elevation), and acceleration (1.3 deg/s/s). All three sites are equipped with dual polarization Sand X-band feeds from COBHAM with room temperature receivers, developed at UTAS by Prof.

Peter McCulloch. The receiver systems cover 2.2 to 2.4 GHz at S-band and 8.1 to 9.1 GHz at Xband. System Equivalent Flux Densities (SEFDs) are 3500 Jy in both bands. Data digitization and

formatting is managed by the Digital Base Band Converter (DBBC) system from HAT-Lab, and

data are recorded using the Conduant Mark 5B+ system. Each site is equipped with VCH-1005A

Hydrogen maser time and frequency standards from Vremya-CH.

All three observatories were designed and constructed to be remotely controlled and monitored

to keep operating costs at a minimum. Operation of the AuScope VLBI array is being carried out

from a dedicated operations room on the Sandy Bay campus of the University of Tasmania.

3. Staff

Staff at UTAS consist of academics, Prof. John Dickey (director), Dr. Simon Ellingsen, and

Prof. Peter McCulloch. Dr. Jim Lovell is Project Manager for the AuScope VLBI project. Dr.

Jamie McCallum and Dr. Stas Shabala are Australian Research Council Super-Science Fellows who

are carrying out research aimed at improving geodetic VLBI solutions in the southern hemisphere.

Mr. Brett Reid is the Observatory Manager whose position is funded by the university. In addition

we have an electronics technical officer, Mr. Eric Baynes. For operation of the observatories during

geodetic observations we rely heavily on support from astronomy PhD and post graduate students.

Logistical and maintenance support at Katherine is provided by Mr. Martin Ephgrave and at

Yarragadee by Mr. Vince Noyes and team at the MOBLAS5 SLR station.

4. AuScope VLBI Project Status

Construction of the first AuScope telescope at Hobart was completed in 2009 and officially

opened at the IVS General Meeting on February 9, 2010. Following a period of commissioning,

testing and debugging, the Hobart telescope made its first successful IVS observation in October

2010. Construction and commissioning at the other two sites continued in parallel. Yarragadee

made its first successful IVS observation in May 2011, and all three telescopes participated in an

IVS observation for the first time on June 16, 2011.

At present, the AuScope VLBI facility has sufficient operational funds for ∼70 observing days

per year, usually consisting of two AuScope telescopes observing as part of the IVS network. The

Hobart 26-m antenna will continue to participate in IVS observations at the level of one session

per month to provide continuity in the Hobart time series.

5. Geodetic VLBI Observations

In 2011 the AuScope and Hobart 26-m antennas participated in 102 IVS sessions for a total

of 171 antenna days of observing. This included the Hobart 12-m participating in the 15-day

52 IVS 2011 Annual Report
University of Tasmania Hobart 12-m and 26-m, Katherine and Yarragadee

CONT11 campaign. A summary of the observations is presented in Table 1

Table 1. AuScope and Hobart 26-m antenna participation (number of days) in IVS sessions in 2011.

Session Antenna

Ho Hb Ke Yg

AUSTRAL 2 2 2

CONT11 15

CRDS 5 4 3

CRF 3

OHIG 1 2

R1 11 27 9 8

R4 12 29 11 11

RD 2 1 1

RDV 1

T2 3 4 1 1

Total 27 90 28 26

6. References

Petrachenko, B. et al., 2009, “Design Aspects of the VLBI2010 System. Progress Report of the

IVS VLBI2010 Committee.”. NASA/TM-2009-214180, June 2009.

IVS 2011 Annual Report 53
Kashima 34-m Radio Telescope Kashima Space Research Center, NICT

Kashima 34-m Radio Telescope

Ryuichi Ichikawa, Eiji Kawai, Mamoru Sekido

Abstract

The Kashima 34-m radio telescope has been continuously operated and maintained by the National

Institute of Information and Communications Technology (NICT) as a facility of the Kashima Space

Research Center (KSRC) in Japan. This brief report summarizes the status of this telescope, the staff,

and activities during 2011. In particular, we describe antenna damage due to the Mw 9.0 megaquake

which occurred on March 11th, 2011.

1. General Information

The Kashima 34-m radio telescope (Figure 1, left) was constructed as a main station of the

“Western Pacific VLBI Network Project” in 1988. After that project’s termination, the telescope

has been used not only for geodetic experiments but also for astronomy and other purposes [1].

The station is located about 100 km east of Tokyo, Japan and is co-located with the 11-m radio

telescope and the International GNSS Service station (KSMV) (Figure 1, right). The station is

maintained within the Space-Time Measurement Project of the Space-Time Standards Group,

NICT.

The Kashima 34-m radio telescope with new logo

design of NICT.

34-m radio

Kashima Station

11-m radio

telescope

telescope

GEONET Station

IGS Station

Facilities at Kashima.

Figure 1. The Kashima Station.

2. Component Description

The receiver equipment of the Kashima 34-m radio telescope is summarized in Table 1 and

Table 2. In particular the high-temperature superconductor (HTS) band-pass filter is equipped at

the S-band receiver for RFI mitigation [3]. We also installed a band-pass filter on July 15, 2008 to

cut out signals between 1405 MHz and 1435 MHz for L-band RFI mitigation.

54 IVS 2011 Annual Report
Kashima Space Research Center, NICT Kashima 34-m Radio Telescope

Table 1. Main specifications of the 34-m radio telescope.

Main reflector aperture 34.073 m

Latitude N 35◦ 57’ 21.78”

Longitude E 140◦ 39’ 36.32”

Height of AZ/EL intersection above sea level 43.4 m

Height of azimuth rail above sea level 26.6 m

Antenna design Modified Cassegrain

Mount type AZ-EL mount

Drive range azimuth North ±270◦

Drive range elevation 7

◦

-90◦

Maximum speed azimuth 0.8

◦/sec

Maximum speed elevation 0.64◦/sec

Maximum operation wind speed 13 m/s

Panel surface accuracy r.m.s. 0.17 mm

Table 2. The receiver specifications of the 34-m radio telescope.

Band frequency (MHz) Trx (K) Tsys (K) Efficiency SEFD (Jy) Polarization

L 1350-1750⋆ 18 45 0.68 200 L/R

S 2193-2350 19 72 0.65 340 L/R

C 4600-5100 100 127 0.70 550 L(R)

X-n 8180-9080∗ 41 48 0.68 210 L/R

X-wL 8180-9080# 41 67 0.68 300 L/R

X-wH 7860-8360# - 67 0.68 300 L/R

K 22000-24000 105 141 0.5 850 L(R)

Ka 31700-33700 85 150 0.4 1100 R(L)

Q 42300-44900 180 350 0.3 3500 L(R)

∗ : 8 GHz LNA narrow band use. # : 8 GHz LNA wide band use.

⋆ : Narrow bandwidth filter, 1405 – 1435 MHz, is used generally to mitigate RFI.

3. Staff

The engineering and technical staff of the Kashima 34-m radio telescope are listed in Table 3.

Dr. Sekido returned to KSRC in March 2011, and he is now continuing the development of the K5

system.

4. Current Status and Activities

The Mw 9.0 megaquake hit the 34-m antenna on March 11th, 2011. We suffered from strong

ground motion, and a 5.2-m high tsunami attacked the Kashima port as shown in Figure 2. In

addition, we were facing serious restrictions due to the Fukushima nuclear accident. Fortunately,

we have no staff casualties in KSRC/NICT. Coseismic crustal deformations measured by our GPS

station near the 34-m antenna showed movements of up to 749 mm in the horizontal (eastward) and

IVS 2011 Annual Report 55
Kashima 34-m Radio Telescope Kashima Space Research Center, NICT

Table 3. The engineering and technical staff of the Kashima 34-m radio telescope.

Name Main Responsibilities

KAWAI Eiji responsible for operations and maintenance

SEKIDO Mamoru technical development for time and frequency (T&F) transfer

TAKEFUJI Kazuhiro T&F experiments using VLBI facilities

HASEGAWA Shingo K5 operation and data transfer

ICHIKAWA Ryuichi responsible for the project

KONDO Tetsuro software correlator development and e-VLBI

-245 mm in the vertical. Moreover, post-seismic deformations following the main shock reached

values of over 270 mm in the horizontal and about 100 mm in the vertical component as recorded

until the end of July.

We carried out an operational repair of the antenna (i.e., repainting of the main dish and rustproofing of the antenna structure) starting on the first of January, 2011. The repair was supposed

to be finished by the end of March. However, the repair was stopped due to the earthquake.

The repair was restarted in April, and it was finished at the end of June. After the repair, we

investigated earthquake damage carefully. Unfortunately, the gear reducers, the power and helium

plumbing, the azimuth track wear strips, and one azimuth wheel were damaged by the strong motion which exceeded 650 gal as recorded around the Kashima region. In 2011, the operation time

of our 34-m antenna was only 364 hours in total. About 60% of the operation time was used for

earthquake damage investigation. The other facilities at KSRC/NICT (e.g., the main building, the

guest room building, and the outreach building) are also partly damaged. Thus, these buildings

are currently under repair.

5. Future Plans

First, we have to fix damage of the 34-m radio telescope due to the earthquake as soon as

possible. Though the damage is severe, we are going to repair them by the end of the next fiscal

year. In addition, we have a plan to install new AZ/EL driving units into the antenna in this fiscal

year.

References

[1] Kawai, E., M. Sekido, R. Ichikawa, Kashima 34-m Radio Telescope, International VLBI Service for

Geodesy and Astrometry 2008 Annual Report, NASA/TP–2009-214183, D. Behrend and K. D. Baver

(eds.), pp. 114–117, 2008.

[2] “Koho Kashima (Kashima public relations, http://city.kashima.ibaraki.jp/20kouhou/data/

20110401/0401 all ver2.eps (in Japanese))”, No. 393, April 1st, 2011.

[3] Kawai, E., J. Nakajima, H. Takeuchi, H. Kuboki, T. Kondo, M. Suzuki, K. Saito, RFI mitigation at a

2 GHz band by using a wide-band high-temperature superconductor filter, J. Geod. Soc. Jpn., Vol. 54,

No. 1, pp. 31–37, 2008.

56 IVS 2011 Annual Report
Kashima Space Research Center, NICT Kashima 34-m Radio Telescope

Figure 2. Earthquake damage in Kashima city. (a) A tsunami struck the Kashima port and surrounding

area [2], (b) train rail bent by powerful ground motion, (c) cargo containers thrown around by the tsunami

in Kashima, (d) Kashima port hit by the tsunami, (e) ripple mark of 34-m antenna azimuth rail caused by

strong motion, (f) broken road in front of the KSRC/NICT main building (photos (b) and (f) were taken

by Dr. Kondo).

IVS 2011 Annual Report 57
Kashima and Koganei 11-m VLBI Stations Kashima Space Technology Center, NICT

Kashima and Koganei 11-m VLBI Stations

Mamoru Sekido, Ryuichi Ichikawa

Abstract

Two 11-m VLBI antennas at Kashima and Koganei are continuously operated and maintained

by the National Institute of Information and Communications Technology (NICT). This brief report

summarizes the status of these antennas, the staff, and the activities during 2011.

1. Introduction

Figure 1. 11-m VLBI antennas at Kashima (left) and Koganei (right).

Koganei Kashima

Miura

Tateyama

Tomakomai

Gifu

145 E 135 E 140 E

35 N

40 N

Figure 2. Geographic locations of four KSP VLBI

stations and two stations at Tomakomai and Gifu.

Two 11-m VLBI antennas at Kashima and

Koganei (Figure 1) used to be stations of the

Key Stone Project (KSP) VLBI Network. The

network consisted of four VLBI stations at

Kashima, Koganei, Miura, and Tateyama (Figure 2). These 11-m antennas and other VLBI

facilities at the Miura and Tateyama stations

have been transported to the Tomakomai Experimental Forest of the Hokkaido University

and to the campus of Gifu University, respectively. As a consequence, two 11-m stations at

Kashima and Koganei remain as IVS Network

Stations.

The KSP was a research and development

project of the National Institute of Information

58 IVS 2011 Annual Report
Kashima Space Technology Center, NICT Kashima and Koganei 11-m VLBI Stations

and Communications Technology (NICT, formerly Communications Research Laboratory) [1]. After the regular VLBI sessions with the KSP VLBI Network terminated in 2001, the 11-m VLBI

stations at Kashima and Koganei have mainly been used for the purposes of technical developments

and miscellaneous observations.

2. Current Status

The main specifications of the antennas are summarized in Table 1. Both antennas can observe

S- and X-band. The original specifications of these antennas were the same. The frequency of the

first local oscillator of X-H band at the Kashima 11-m station was changed by 80 MHz, so that

the observation frequency range became the same as the range of the Kashima 34-m station. The

band-pass filter for S-band was replaced for RFI mitigation at both stations in 2010.

The optical loop-back controlled reference signal transmission system has been installed between the second building of NICT-HQ and the Koganei VLBI station operation building since

2009. That provides the reference signal (5MHz/1PPS) of UTC(NICT) to the Koganei 11-m

station [2].

The reference signal (5MHz/1PPS) of the Kashima 11-m station has been provided by the

H-maser atomic standard at the Kashima 34-m station via a long distance (about 500 m) co-axial

cable. In November 2011, a mobile hydrogen maser atomic time standard was installed at the

Kashima 11-m station, and its reference signal became independent from the reference signal of

the Kashima 34-m station. A precise temperature control box, which was installed in the Kashima

11-m observation room in 2010, is keeping the temperature inside the box within a few tenths of

degrees of Kelvin. Reference signal distribution units are placed inside this box.

Both stations are using phase calibration signal (P-cal) unit of 5-MHz interval instead of 1-MHz

interval.

Table 1. The specifications of the KSP 11-m antennas.

Kashima Koganei

Antenna Type Cassegrain type

Diameter of the Main Reflector 11 m

Mount Style Az El mount

Latitude N 35◦ 57’ 20.12” N 35◦ 42’ 38.01”

Longitude E 140◦ 39’ 26.93” E 139◦ 29’ 17.10”

Height of Az/El intersection above sea level 62.4 m 125.4 m

S band 2212 ∼ 2360 2212 ∼ 2360

Input Frequency (MHz) X Low band 7700 ∼ 8200 7700 ∼ 8200

X High band 8180 ∼ 8680 8100 ∼ 8600

S band 3000 3000

Local Frequency (MHz) X Low band 7200 7200

X High band 7680 7600

IVS 2011 Annual Report 59
Kashima and Koganei 11-m VLBI Stations Kashima Space Technology Center, NICT

Figure 3. Displacement of the Kashima 11-m station’s global coordinates obtained from R1 sessions (left).

Horizontal displacement vector of the Kashima 11-m and Koganei 11-m stations derived from the JD1109

session (right).

3. Activities in 2011























$SU -XQ -XO $XJ 'HF

Az offset

Title to Az=0

Title to AZ=90

Observation Date

Angle (deg.)

Figure 4. Changes of azimuthal axis tilting and

azimuth angle offset were found after the earthquake on 11 March 2011.

The Kashima region was widely affected by the

big earthquake that occurred on 11 March 2011 in

the north east of Japan, although fortunately the

Kashima 11-m and Koganei 11-m stations were not

seriously damaged. We have performed antenna

pointing parameter observations with the Kashima

11-m station several times (8 June, 4 July, 29 August, and 28 December) for monitoring of particular changes of pointing parameters caused by the

earthquake and after-shocks. In a comparison of the

pointing model parameters with those obtained in

2008, there were permanent changes to the Az-axis

tilting angle and the Az-offset parameters in these

observations (Figure 4).

Since the earthquake was so big, crustal deformation around the north east area of Japan is

still continuing. For the purpose of monitoring the baseline changes on the Kashima — Koganei

baseline, a series of VLBI observations have been conducted since 7 May. The time series of the

baseline length changes, and a general list of experiments processed by the correlator at Kashima,

is indicated in Figure 2 and Table 2, respectively, in the correlator report of Kashima in this

volume.

Apart from the VLBI sessions, the Space Weather and Environment Informatics Laboratory of

NICT is using the 11-m antenna at Koganei to download data from the STEREO spacecrafts. Two

STEREO spacecrafts were launched by NASA in October 2006 to investigate the solar terrestrial

environment and to provide 3D images of the Sun and solar storms. The Koganei 11-m antenna

60 IVS 2011 Annual Report
Kashima Space Technology Center, NICT Kashima and Koganei 11-m VLBI Stations

is most of the time operated for this purpose, as long as VLBI sessions are not scheduled.

4. Staff Members

The 11-m antenna stations at Kashima and Koganei are operated and maintained by the members of the Space-Time Standards Laboratory at the Kashima Space Technology Center (KSTC)

and headquarters of NICT. The staff members of the group are listed in Table 2. The operation and

maintenance of the 11-m VLBI station at Koganei is also greatly supported by the Space Weather

and Environment Informatics Laboratory and the Space Communication Systems Laboratory at

the Koganei Headquarters of NICT.

Table 2. Staff members of the Space-Time Standards Laboratory, KSTC, NICT.

Name Main Responsibilities

KAWAI Eiji Antenna Systems

ICHIKAWA Ryuichi Meteorological Sensors, IGS Receivers

AMAGAI Jun Antenna System and Timing Systems

at Koganei 11-m station

SEKIDO Mamoru Antenna System, Field System,

Calibration and Frequency Standard Systems

HASEGAWA Shingo Computer System

5. Future Plans

In 2012, we plan to continue VLBI experiments for precise time and frequency transfer and

crustal deformation monitoring. In 2012, the Kashima and Koganei 11-m stations will also participate in IVS-T2 sessions.

References

[1] Special issue for the Key Stone Project, J. Commun. Res. Lab., Vol. 46, No. 1, March 1999.

[2] Fujieda, M., M. Kumagai, S. Nagano, and T. Gotoh UTC(NICT) signal transfer system using optical

fibers, IVS NICT-TDC News, No. 31, 17-20, 2010.

[3] Sekido, M., R. Ichikawa, VLBI Correlators in Kashima, International VLBI Service for Geodesy and

Astrometry 2011 Annual Report, this volume, 2012.

IVS 2011 Annual Report 61
Kokee Park Geophysical Observatory USNO and NASA GSFC

Kokee Park Geophysical Observatory

Ron Curtis

Abstract

This report summarizes the technical parameters and the staff of the VLBI system at Kokee Park

on the island of Kauai.

1. KPGO

The Kokee Park Geophysical Observatory (KPGO) is located in the Kokee State Park on the

island of Kauai in Hawaii at an elevation of 1,100 meters near the Waimea Canyon, often referred

to as the Grand Canyon of the Pacific.

Table 1. Location and address of Kokee Park Geophysical Observatory.

Longitude 159.665◦ W

Latitude 22.126◦ N

Kokee Park Geophysical Observatory

P.O. Box 538 Waimea, Hawaii 96796

USA

2. Technical Parameters of the VLBI System at KPGO

The receiver is of NRAO (Green Bank) design (dual polarization feed using cooled 15 K HEMT

amplifiers). The DAR rack and tape drive were supplied through Green Bank. The antenna is

of the same design and manufacture as those used at Green Bank and Ny- ̊Alesund. We presently

employ a Mark 5B+ recorder for all of our data recording.

The technical parameters of the radio telescope are summarized in Table 2.

Timing and frequency is provided by a Sigma Tau Maser with a NASA NR Maser providing

backup. Monitoring of the station frequency standard performance is provided by a CNS (GPS)

Receiver/Computer system. The Sigma Tau performance is also monitored via the IGS Network.

3. Staff of the VLBI System at KPGO

The staff at Kokee Park from January 1 through April 8, 2011 consisted of five people employed

by Honeywell Technology Solutions, Inc. under the NENS contract to NASA for the operation and

maintenance of the observatory. Matt Harms, Chris Coughlin, and Ron Curtis conducted VLBI

operations and maintenance. Ben Domingo was responsible for antenna maintenance, with Amorita

Apilado providing administrative, logistical, and numerous other support functions. Kelly Kim of

Caelum Research Corporation also supported VLBI operations and maintenance during 24-hour

experiments and as backup support.

On April 9, 2011 the NENS contract transitioned to the SCNS contract operated by ITT

62 IVS 2011 Annual Report
USNO and NASA GSFC Kokee Park Geophysical Observatory

Table 2. Technical parameters of the radio telescope at KPGO.

Parameter Kokee Park

owner and operating agency USNO-NASA

year of construction 1993

radio telescope system Az-El

receiving feed primary focus

diameter of main reflector d 20m

focal length f 8.58m

f /d 0.43

surface contour of reflector 0.020inchesrms

azimuth range 0 . . . 540◦

azimuth velocity 2

◦/s

azimuth acceleration 1

◦/s2

elevation range 0 . . . 90◦

elevation velocity 2

◦/s

elevation acceleration 1

◦/s2

X-band

(reference ν = 8.4GHz, λ = 0.0357m)

8.1 − 8.9 GHz

Tsys 40 K

SSEF D(CASA) 900 Jy

G/T 45.05 dB/K

η 0.406

S-band

(reference ν = 2.3GHz, λ = 0.1304m)

2.2 − 2.4GHz

Tsys 40 K

SSEF D(CASA) 665 Jy

G/T 35.15 dB/K

η 0.539

VLBI terminal type VLBA/VLBA4-Mark 5

Field System version 9.7.6

Information Systems. The staff at Kokee Park consisted of six people under the new contract to

NASA. Matt Harms retired, and Kiah Imai and Lawrence Chang were added to the Kokee Park

staff to conduct VLBI operations and maintenance.

4. Status of KPGO

Kokee Park has participated in many VLBI experiments since 1984. We started observing with

GAPE, continued with NEOS and CORE, and are now in IVS R4 and R1. We also participate

in the RDV experiments. We averaged 1.5 experiments per week during calendar year 2000 and

increased to an average of two experiments of 24 hours each week, with daily Intensive experiments

starting in year 2002 and continuing into 2011. After the earthquake in Japan in March 2011,

IVS 2011 Annual Report 63
Kokee Park Geophysical Observatory USNO and NASA GSFC

KPGO supported weekend Intensive experiments for the rest of the year while data from the

Tsukuba VLBI station was being analyzed for supporting weekend Intensive experiments.

Kokee Park also hosts other systems, including a 7-m PEACESAT command and receive antenna, a DORIS beacon, a QZSS monitoring station, a TWSTFT relay station, and a Turbo-Rogue

GPS receiver. Kokee Park is an IGS station.

In October 2007, Japanese interests, along with representatives from NASA, USNO, and the

State Department, held a meeting at KPGO to explore the possible installation of a project called

Quasi-Zenith Satellite System (QZSS). In 2008, further investigation continued towards making

the QZSS project a part of KPGO. NASA sent an engineering team to investigate the support

requirements that would be needed to implement the QZSS project here, and an engineering

team from Japan surveyed the site for the hardware that would be installed. The aging KPGO

infrastructure was upgraded in stages as the project progressed. In October 2009, the power at

KPGO was upgraded to support the QZSS and Two-Way Satellite Time and Frequency Transfer

(TWSTFT) requirements. In March 2010 the construction of the antenna base for the project

was completed, and all components were installed and tested. In July 2010 the TWSTFT for the

project was operationally configured by USNO and NICT.

In June 2010, the remote control capability for the DORIS beacon was installed at KPGO.

In October 2010, two members of the Ny- ̊Alesund VLBI team visited KPGO for the sharing

of processes and procedures on operations and maintenance.

Also, in 2008, advances were made for making real-time VLBI data from KPGO a reality.

The agencies that will be responsible for the wideband pipes leading from the site entered into a

service agreement late in 2008. The coordination with the parties involved in the communication

infrastructure upgrades continued through 2010. While work continues towards implementing

the final architecture, an interim configuration has permitted some successful testing. Initially,

the daily Intensive experiments are being targeted so that correlation back at the Washington

Correlator can happen days earlier than it previously did. 24-hour experiment data flow will

hopefully follow when the final architecture is implemented. The testing of the new communication

infrastructure progressed slowly in 2011 but looks more promising in 2012.

5. Outlook

KPGO will be undergoing incremental changes and upgrades in the coming year to replace

aging components as well as preparing to support VLBI2010 technical specifications. Plans are in

progress to upgrade the KPGO backend to use the RDBE architecture in 2012. The Mark 5B+

data recorders will be upgraded to a Mark 5C. There are plans to migrate the e-transfer data

connection to dedicated fiber supporting 1 Gbit/s or higher data rates. Plans are in progress for

developing a new receiver box and feed for the 20-m antenna to support VLBI2010 specifications.

Discussions are also in progress that may bring to KPGO a new 12-m antenna capable of supporting

VLBI2010 specifications, including the faster slew rates.

KPGO’s support of the PEACESAT mission will end in 2012 as the project comes to an end.

CNES has reached out to NASA on the possibility of upgrading KPGO to be part of their

REGINA Network.

64 IVS 2011 Annual Report
USNO and NASA GSFC Kokee Park Geophysical Observatory

Figure 1. KPGO VLBI 20-m antenna (right) with

the old NASA USB 9-m antenna in the background.

Figure 2. TWSTFT antennas.

Figure 3. DORIS remote control (left foreground)

and beacon (right foreground).

Figure 4. QZSS/TWSTFT equipment racks.

IVS 2011 Annual Report 65
Matera CGS VLBI Station Agenzia Spaziale Italiana

Matera CGS VLBI Station

Giuseppe Bianco, Giuseppe Colucci, Francesco Schiavone

Abstract

This report describes the status of the Matera VLBI station. Also, an overview of the station, some

technical characteristics of the system, and staff addresses are given.

1. General

Figure 1. The Matera “Centro di Geodesia Spaziale” (CGS).

The Matera VLBI station is located at the Italian Space Agency’s ‘Centro di Geodesia Spaziale

G. Colombo’ (CGS) near Matera, a small town in the south of Italy. The CGS came into operation

in 1983 when the Satellite Laser Ranging SAO-1 System was installed at CGS. Fully integrated into

the worldwide network, SAO-1 was in continuous operation from 1983 up to 2000, providing high

precision ranging observations of several satellites. The new Matera Laser Ranging Observatory

(MLRO), one of the most advanced Satellite and Lunar Laser Ranging facilities in the world, was

66 IVS 2011 Annual Report
Agenzia Spaziale Italiana Matera CGS VLBI Station

installed in 2002 and replaced the old SLR system. CGS also hosted mobile SLR systems MTLRS

(Holland/Germany) and TLRS-1 (NASA).

In May 1990 the CGS extended its capabilities to Very Long Baseline Interferometry (VLBI),

installing a 20-m radio telescope. Since then, Matera has performed in 824 sessions up through

December 2011.

In 1991 we started GPS activities, participating in the GIG 91 experiment and installing

at Matera a permanent GPS Rogue receiver. In 1994 six TurboRogue SNR 8100 receivers were

purchased in order to create the Italian Space Agency GPS fiducial network (IGFN). At the moment

12 stations are part of the IGFN, and all data from these stations, together with 24 other stations in

Italy, are archived and made available by the CGS Web server GeoDAF (http://geodaf.mt.asi.it).

In 2000 we started activities with an Absolute Gravimeter (FG5 Micro-G Solutions). The

gravimeter operates routinely at CGS, and it is available for external campaigns on request.

Figure 2. MLRO in action, photo courtesy of Francesco Ambrico.

Thanks to the co-location of all precise positioning space based techniques (VLBI, SLR, LLR,

and GPS) and the Absolute Gravimeter, CGS is one of the few “fundamental” stations in the world.

With the objective of exploiting the maximum integration in the field of Earth observations, in

the late 1980s ASI extended CGS’ involvement also to remote sensing activities for present and

future missions (ERS-1, ERS-2, X-SAR/SIR-C, SRTM, ENVISAT, and COSMO-SkyMed).

2. Technical/Scientific Overview

The Matera VLBI antenna is a 20-meter dish with a Cassegrain configuration and an AZ-EL

mount. The AZ axis has ±270 degrees of available motion. The slewing velocity is 2 deg/sec for

both the AZ and the EL axes.

IVS 2011 Annual Report 67
Matera CGS VLBI Station Agenzia Spaziale Italiana

The technical parameters of the Matera VLBI antenna are summarized in Table 1.

The Matera time and frequency system consists of three frequency sources (two Cesium beam

and one H-maser standard) and three independent clock chains. The EFOS-8 H-maser from

Oscilloquartz is used as a frequency source for VLBI.

Table 1. Matera VLBI Antenna Technical Specifications.

Input frequencies S/X 2210−2450 MHz / 8180−8980 MHz

Noise temperature at dewar flange S/X <20 K

IF output frequencies S/X 190−430 MHz / 100−900 MHz

IF Output Power (300 K at inp. flange) S/X 0.0 dBm to +8.0 dBm

Gain compression S/X <1 dB at +8 dBm output level

Image rejection S/X >45 dB within the IF passband

Inter modulation products S/X At least 30 dB below each of 2 carriers

at an IF output level of 0 dBm per carrier

Tsys S/X 55/65 K

SEFD S/X 800/900 Jy

3. Staff

The list of the VLBI staff members of the Matera VLBI station is provided in Table 2.

Table 2. Matera VLBI staff members.

Name Agency Activity E-Mail

Dr. Giuseppe Bianco ASI Space Geodesy Manager giuseppe.bianco@asi.it

Francesco Schiavone e-geos Operations Manager francesco.schiavone@e-geos.it

Giuseppe Colucci e-geos VLBI contact giuseppe.colucci@e-geos.it

4. Status

In 2011, 59 sessions were observed. Figure 3 shows a summary of the total acquisitions per

year, starting in 1990.

In 2004, in order to fix the existing rail problems, a complete rail replacement had been planned.

In 2005, due to financial difficulties, it was instead decided that only the concrete pedestal under

the existing rail would be repaired. From then on, no rail movements have been noted [1]-[3].

5. Outlook

In order to plan the eventual building of a VLBI2010 system, the fund raising investigation

process has been started. At this moment it is not clear when the budget for starting the project

will be ready.

68 IVS 2011 Annual Report
Agenzia Spaziale Italiana Matera CGS VLBI Station

Figure 3. Acquisitions per year.

The replacement of two azimuth wheels is planned for 2012. The other two were replaced in

2008 and 2009 respectively.

The process of purchasing a new H-Maser has been already started. The delivery of the new

unit is planned for 2013.

References

[1] M. Mannarella “Relazione sulle misure effettuate sulla rotaia dell’antenna VLBI”, Telespazio doc. OTSPA-SM REL 180010 1140 0222, 21/01/2004.

[2] M. Mannarella “Misure sugli spostamenti indotti sulle piastre e sulla rotaia dell’antenna VLBI”,

Telespazio doc. OT-SPA-SM REL 180010 1320 0661, 06/04/2005.

[3] M. Mannarella “Relazione sull’esito dei lavori di ripristino delle parti ammalorate della fondazione

dell’antenna VLBI”, Telespazio Doc. OT-SPA-SM REL 180010 1320 0732, 27/06/2005.

IVS 2011 Annual Report 69
Medicina Network Station Istituto di Radioastronomia, Medicina

The Medicina Station Status Report

Alessandro Orfei, Andrea Orlati, Giuseppe Maccaferri

Abstract

General information about the Medicina Radio Astronomy Station, the 32-m antenna status, and

the staff in charge of VLBI observations is provided. In 2011 the data from geodetic VLBI observations

were acquired using the Mark 5A recording system with good results. Updates of the hardware have

been performed and are briefly described.

1. The Medicina 32-m Antenna: General Information

The Medicina 32-m antenna is located at the Medicina Radio Astronomy Station. The station is

run by the Istituto di Radioastronomia and is located about 33 km east of Bologna. The Consiglio

Nazionale delle Ricerche was the funding agency of the Istituto di Radioastronomia until the end

of 2004. Since January 1, 2005 the funding agency has been the Istituto Nazionale di Astrofisica

(INAF).

The antenna, inaugurated in 1983, has regularly taken part in IVS observations since 1985 and

is an element of the European VLBI network. A permanent GPS station (MEDI), which is part

of the IGS network, is installed in the vicinity. Another GPS system is installed near the VLBI

telescope (MSEL) and is part of the EUREF network.

2. Antenna Description

The Medicina antenna has Cassegrain optics, consisting of a primary mirror of 32-m in diameter,

and a secondary mirror, called the subreflector, of convex shape and about 3-m in diameter. The

subreflector, mounted on a quadrupode, is placed opposite the primary mirror and focuses the

radio waves at its center, where the receiver system is located. For some observing frequencies, a

simplified optical system is enough. The subreflector is therefore shifted from its normal position,

and the receiving system is placed at the primary focus. This is the case for the S-X observations.

The antenna can operate in the range between 327 MHz and 22 GHz.

The receivers are cooled with cryogenic techniques to improve the system sensitivity. The antenna’s operative receiver is easily changed; only a few minutes are needed to change the observing

frequency. A recent picture of the antenna is shown in Figure 1.

3. The Staff

Many scientists and technicians take care of the observations. However, a limited number

are dedicated to maintaining and improving the reliability of the antenna during the observations:

Alessandro Orfei is the Chief Engineer, expert in microwave receivers; and Andrea Orlati, Software

Engineer, takes care of the observing schedules and regularly implements SKED, DRUDG, and the

Field System. At the end of 2010 Giuseppe Maccaferri took a one-year sabbatical period. Marco

Bartolini and Simona Righini have been temporarily included in the staff helping Andrea Orlati

for the VLBI preparation and observation.

70 IVS 2011 Annual Report
Istituto di Radioastronomia, Medicina Medicina Network Station

Figure 1. View of the Medicina 32-m dish taken during geodetic VLBI observations. Note that the subreflector is shifted to allow the use of the S/X receiver located in the primary focus of the radio telescope.

4. Current Status and Activities

The board to upgrade our version of Mark 5 to Mark 5C has been purchased. At the same time

an order has been placed to buy a DBBC equipped with ADB2 and CORE2 boards. An added

FILA10G Ethernet interface will allow the use of it with Mark 5C.

The antenna will be provided with a new Helium pipeline and cryo compressors. The cold head

will be substituted in the receivers.

A plan for heavy and extraordinary maintenance is in progress. The first step is to provide

materials and contracts. The H-Maser is near the end of its life; it has been decided to buy a new

one.

The upgrade to 10 Gb/s is still in progress, as is the creation of a 10 Gb/s POP center at

Bologna Headquarters.

5. Geodetic VLBI Observations

In 2011 Medicina took part in 23 (24-hour) routine geodetic sessions (namely 2 IVS-T2, 18

IVS-R4, 2 EUROPE, and 1 R&D experiments).

IVS 2011 Annual Report 71
National Astronomical Observatory of Japan Mizusawa VLBI Observatory, NAOJ

VERA Geodetic Activities

Takaaki Jike, Seiji Manabe, Yoshiaki Tamura, Makoto Shizugami, VERA group

Abstract

The geodetic activities of VERA in the year 2011 are briefly described. The regular geodetic

observations are carried out both in K- and S/X-bands. The frequency of regular observations are

three times a month—twice for the VERA internal observations in K-band. The networks of the S/X

sessions are JADE of GSI and IVS-T2. The raw data of the T2 and JADE sessions are electronically

transferred to the Bonn, Haystack, and GSI correlators via Internet.

Gravimetric observations are carried out at the VERA stations. The superconducting gravimeter

previously installed at Esashi Earth Tides Station was moved to Mizusawa and placed in the vicinity

of the VERA antenna in order to monitor vertical displacement at the end of 2008, and the observation

continued throughout the year.

The 2011 earthquake off the Pacific coast of Tohoku generated step-like and creeping-like movements

to the VERAMZSW position.

1. General Description

VERA is a Japanese domestic VLBI network consisting of the Mizusawa, Iriki, Ogasawara, and

Ishigakijima stations. Each station is equipped with a 20-m radio telescope and a VLBI backend.

The VERA-Mizusawa antenna and the Mizusawa 10-m antenna are shown in Figure 1. In this

figure, the antenna in the front is the Mizusawa 10-m antenna, and the one in the back is the

VERA-Mizusawa antenna. The VERA array is controlled from the Array Operation Center at

Mizusawa via Internet.

The primary scientific goal of VERA is to reveal the structure and the dynamics of our galaxy

by determining 3-dimensional force field and mass distribution. Galactic maser sources are used as

dynamical probes, the positions and velocities of which can be precisely determined by phase referenced VLBI relative to extragalactic radio sources. The distance is measured as a classical annual

trigonometric parallax. The observing frequency bands of VERA are S and X, K (22 GHz), and

Q (43 GHz). Geodetic observations are made in S/X- and K-bands. Q-band is currently not used

for geodesy. Only a single beam is used even in K-band in geodetic observations, although VERA

can observe two closely separated (0.2

◦ < separation angle < 2.2◦

) radio sources simultaneously by

using the dual beam platforms.

General information about the VERA stations is summarized in Table 1, and the geographic

locations are shown in Figure 2. Lengths of baselines range from 1000 km to 2272 km. The skyline

at Ogasawara station ranges from 7◦to 18◦ because it is located at the bottom of an old volcanic

crater. The north-east sky at Ishigakijima station is blocked by a nearby high mountain. However,

the majority of the skyline is below 9◦. The skylines at Mizusawa and Iriki are low enough to

observe sources with low elevation. Since Ogasawara and Ishigakijima are small islands in the

open sea and their climate is subtropical, the humidity in the summer is very high. This brings

about high system temperatures in the summer, in particular in K and Q bands. Iriki station as

well as these stations are frequently hit by strong typhoons. The wind speed sometimes reaches

up to 60–70 m/s.

72 IVS 2011 Annual Report
Mizusawa VLBI Observatory, NAOJ National Astronomical Observatory of Japan

Figure 1. VERA-Mizusawa antenna and Mizusawa

10-m antenna. Figure 2. Location of the VERA stations.

Table 1. General information.

Sponsoring agency Mizusawa VLBI Observatory,

National Astronomical Observatory of Japan

Contributing type Network observing station

Location

Mizusawa 141◦ 07’ 57”.199 E, 39◦ 08’ 00”.726 N, 75.7 m(sea level)

Iriki 130◦ 26’ 23”.593 E, 31◦ 44’ 52”.437 N, 541.6 m(sea level)

Ogasawara 142◦ 12’ 59”.809 E, 27◦ 05’ 30”.487 N, 223.0 m(sea level)

Ishigakijima 124◦ 10’ 15”.578 E, 24◦ 24’ 43”.834 N, 38.5 m(sea level)

2. Technical Parameters

Parameters of the antennas and front- and back-ends are summarized in Tables 2 and 3,

respectively. Two observing modes are used in geodetic observations. One is the VERA internal

observation in K-band with the recording rate of 1 Gbps. The other is the conventional S/Xband observation with K5-VSSP. JADE, which is GSI’s domestic observation project, and IVS-T2

sessions belong to this class. Only Mizusawa and Ishigakijima participated in these sessions.

Table 2. Antenna parameters.

Diameter 20m Slew Azimuth Elevation

Mount Az-El range -90◦ – 450◦ 5

◦ – 85◦

Surface accuracy 0.2mm(rms) speed 2.1◦/sec 2.1◦/sec

Pointing accuracy <12”(rms) acceleration 2.1◦/sec2 2.1◦/sec2

S X K

HPBW 1550” 400” 150”

Aperture efficiency 0.25 0.4 0.47

IVS 2011 Annual Report 73
National Astronomical Observatory of Japan Mizusawa VLBI Observatory, NAOJ

Table 3. Front-end and back-end parameters.

Front-end

Frequency Frequency Receiver Polarization Receiver Feed

band range(GHz) temperature type

S 2.18–2.36 100◦K RHC HEMT Helical array

X 8.18–8.60 100◦K RHC HEMT Helical array

K 21.5–24.5 39±8

◦K LHC HEMT(cooled) Horn

Back-end

Type channels BW/channel Filter Recorder Deployed

station

VERA 16 16MHz Digital DIR2000 4 VERA

K5-VSSP 16 4MHz VC HDD Mizusawa

Ishigakijima

3. Current Status and Activities

3.1. VLBI

VERA observes seven days a week except for the maintenance period in the summer. The

nominal frequency of geodetic observations is three days a month. Among these three, VERA

internal geodetic observations in K-band are performed twice a month, and Mizusawa and Ishigakijima participate in JADE by GSI or IVS-T2 sessions in S/X-band on a once-a-month basis. The

main purpose of the VERA internal geodetic observations is to determine relative positions of the

VERA antennas accurate enough for astrometric requirements. The purpose of the S/X sessions

is to make the VERA coordinates refer to the IVS reference frame. The reason for the shift of the

observing frequency band from S/X-band to K-band is to avoid the strong radio interference by

cellular phone in S-band, particularly at Mizusawa. The interfering signal which has line spectra

is filtered out. However, this filtering considerably degrades the system noise temperature. It is

likely that the S-band observation will become impossible in the near future. On the other hand,

VERA has the highest sensitivity in K-band as shown in Table 3. Thanks to the high sensitivity

in this band the maximum number of scans in K-band is 800/station/24-hours, while that in S/Xband is 500 at most. It has been confirmed that the K-band observations are far more precise,

although the ionospheric delay is not corrected for. In fact, standard deviations of the individual

determinations of the antenna positions in K-band are less than half of those in S/X-band.

In order to link the VERA network to the international reference frame, VERA continues

participation in the IVS-T2 sessions by using the Mizusawa and Ishigakijima stations. In 2011, we

participated in seven T2 sessions and in three JADE sessions. VERA internal geodetic observations

were carried out 18 times. The final estimation of the geodetic parameters are derived by using

the software developed by the VERA team.

74 IVS 2011 Annual Report
Mizusawa VLBI Observatory, NAOJ National Astronomical Observatory of Japan

3.2. Other Activities

Continuous GPS observations were carried out at each VERA station throughout the year. The

superconducting gravimeter (SCG) was moved from the Esashi Earth Tides Station to Mizusawa

in order to accurately monitor gravity change for the purpose of monitoring height change at the

VERA Mizusawa station. Four water table gauges surrounding the SCG were used for monitoring

the water table height. SCG was installed also in the VERA Ishigakijima station in January 2012.

The preliminary results show that gravity variation due to the variation of the water table can be

corrected as accurately as the 1μgal level.

4. The 2011 Earthquake Off the Pacific Coast of Tohoku

The strong quakes by the 2011 earthquake off the Pacific coast of Tohoku (Mw=9.0) [Epoch=11

March 2011, 14:16:18 JST] damaged the VERA-Mizusawa 20-m antenna. Operations of the VERAMizusawa antenna stopped five weeks after the earthquake and for ten weeks of the repair period.

VERAMZSW was displaced by co-seismic crustal movement and post-seismic creeping. These

movements are clearly detected from VERA internal geodetic VLBI observations and continuous

GPS observations. During the approximately three minutes of seismic motion, VERAMZSW was

displaced 3.4 m at the maximum and shifted 2.4 m in the direction of east-northeast eventually.

The co-seismic steps are X=-1.924 m, Y=-1.227 m, and Z=-1.062 m in the geocentric Cartesian

coordinate system. The direction of the creeping is well agreed with the direction of co-seismic

slip (Figure 3). Total length of the movement by the post-seismic creeping is 40.6 cm between 12

March and 31 December, 2011. This creeping is gradually decreasing but still continues.

Figure 3. Movements of VERAMZSW after the 2011 earthquake.

5. Staff Members

The Mizusawa VERA Observatory of NAOJ was reorganized as the Mizusawa VLBI Observatory in April 2009. VERA and VSOP-2 were integrated into a unified project. Noriyuki Kawaguchi

was inaugurated as Director in April 2010. The geodesy group consists of S. Manabe (scientist),

Y. Tamura (scientist), T. Jike (scientist), and M. Shizugami (software technician).

IVS 2011 Annual Report 75
Noto VLBI Station Istituto di Radioastronomia INAF, Stazione VLBI di Noto

Noto Station Status Report

G. Tuccari, F. Schillir ́o, P. Cassaro, S. Buttaccio, C. Contavalle, F. Giacalone,

N. Lombardo, G. Nicotra, L. Nicotra, C. Nocita, L. Papaleo, M. Patern ́o, P.R. Platania

Abstract

The year 2011 for the Noto station has been one of great renovation and of important improvements

for its observational capabilities. In particular we are able to mention four key projects that were

completed or under way.

1. Repairs of Azimuthal Axis of Rotation

In recent years, there has been a tangible and sensible decrease of the mechanical performance

of the antenna, mainly due to mechanical wear of components of the system, in particular related to

the system of the azimuth rotation axis of the telescope and all subparts that compose it: rail track,

base metal plates, wheels, reducer gears, and especially the grout. The slow action of wear and tear

of time and weather has gradually deteriorated the state of these components and their assembly,

affecting not only the antenna observational parameters (pointing accuracy, tracking speed and

accuracy, camber angle of the wheels, and the proper angle of the rotation axes (affecting the geo

antenna point)), but also the stiffness of the antenna, so that in March 2010 a structural failure of

a wheel bearing stopped the antenna activity and caused the necessity of completely repairing the

azimuth rotation axis. During 2011 the station activities have been focused on the organization

of this repair work; in particular the search for funding—about 700K Euro fully funded by the

Ministry of Research (of which INAF is part), the execution of preparatory paperwork and project

design, drafting the implementation of the projects, and the actual activity. This last phase took

about 13 weeks; it was completely performed by a highly qualified Italian company, Galbiati Srl,

and it can be described in three main parts:

1) a. Dismantling of the mechanical parts and anchorages to the main azimuth bearing (see

Figure 1);

b. plucking up of the rail track, metal plates and grout that capture and support the rail;

c. performing of reference measurements;

2) Installation and grouting of the support plates, including the maturation phase of the grout

(28 days) (see Figure 2);

3) a. Installation of new mechanical parts such as rails, bolts and gears (see Figure 3).

b. Performing of new reference measurements.

The work was completed with the phases of protection and painting of the antenna base,

cleaning of reflective surfaces (especially primary optics) and the alignment of the telescope and

pointing systems reprogramming (see Figure 4). Radio telescope parameters have been restored

like the original ones by project, in particular for the correction of the camber angle of the wheels

(average 9’ over 2◦ 52’), and the orthogonal offset recovery (about 10”) of both elevation and

azimuth axis.

76 IVS 2011 Annual Report
Istituto di Radioastronomia INAF, Stazione VLBI di Noto Noto VLBI Station

Figure 1. a) Rail track removal b) Grout removal, metal plates visible

Figure 2. a) Continuous metal plate installation and b) grouting phase

IVS 2011 Annual Report 77
Noto VLBI Station Istituto di Radioastronomia INAF, Stazione VLBI di Noto

Figure 3. a) New wheels b) Wheel, support and reducer gear coupling

Figure 4. It’s the end of the work!!!

78 IVS 2011 Annual Report
Istituto di Radioastronomia INAF, Stazione VLBI di Noto Noto VLBI Station

2. Fiber Optics Connection

A fiber optics link for e-VLBI activities has been financed by GARR (Italian Academic and

Research Network) and it is now ready to start with a 1 Gbps data rate starting in March 2012,

and 10 Gbps probably starting in September 2012.

3. Frequency Agility

A frequency agility system is now in the design phase. This system will install a set of receivers

in the antenna secondary focus, so that the receivers will automatically be available within a few

minutes. The primary focus will receive a revised version of the SXL receiver that was developed

some years ago but was never used due to the difficult mechanical operations required to implement

it for regular observing. This project has been funded, and the activities will start in summer 2012.

4. DBBC2010 for VLBI2010 Observations

The Noto station will participate in VLBI observing with the legacy antenna. This will require

the adoption of a wide band receiver and a dedicated back-end. The first will be assembled as

soon as the feed becomes available, following the VLBI2010 Committee recommendations, while

the back-end will be upgraded during 2012. This requires the installation of four additional IFs in

the existing DBBC system, as well as a number of additional boards, which will make the system

compatible with the required specifications. In particular the FILA10G network board will be

adopted to support the high output data rate. A Mark 6 recorder will be supported at 32 Gbps.

At the same time the DBBC3 Project has been financed by Radionet and will formally start in

July 2012. Such a new back-end will provide the entire two polarization 14 GHz band coverage in

full digital fashion, including support for the data process and multiple 100G network capability.

IVS 2011 Annual Report 79
Ny- ̊Alesund 20-Meter Antenna Geodetic Institute, Norwegian Mapping Cadastre Authority

Ny- ̊Alesund 20-meter Antenna

Carl Petter Nielsen

Abstract

In 2011, the 20-meter VLBI antenna at the Geodetic Observatory, Ny- ̊Alesund, has participated in

VLBI experiments, observing 115 of 115 scheduled 24-hour experiments, 35 of 41 scheduled Intensives

and the CONT in September. Reasons for the lost Intensive experiments were cancellations due to the

disabling of the Tsukuba antenna by the earthquake in Japan. In 2011, Ny- ̊Alesund was manned by

four employees dividing three positions between them—Carl Petter Nielsen as base commander and

Geir Mathiassen, Moritz Sieber, and Lars Karvonen as engineers, all working 75%. In November Lars

Karvonen was replaced by  ̊Asmund Skjæveland. In connection with our VLBI2010 application, the

Norwegian Mapping Authority (NMA) was granted 219 million NOK from the Norwegian Government.

1. General Information

The Geodetic Observatory of the NMA is situated at 78.9 N and 11.87 W in Ny- ̊Alesund,

in Kings Bay, at the west side of the island of Spitsbergen. This is the biggest island in the

Svalbard archipelago. In 2011, Ny- ̊Alesund was scheduled for 115 24-hour VLBI experiments,

including R1, R4, EURO, RD, T2, and RDV sessions, and 41 1-hour Intensives within the Int1/Int3

program. Five Intensive experiments were cancelled due to the earthquake in Japan that disabled

the Tsukuba antenna. One Intensive had to be cancelled because of station problems. The rest of

the 150 experiments were run as planned. Ny- ̊Alesund also participated successfully in the CONT

in September.

In addition to the 20-meter VLBI antenna, the Geodetic Observatory has two GPS antennas in

the IGS system and a Super Conducting Gravimeter in the Global Geodynamics Project (GGP)

installed at the site. There is also a SATREF (dGPS) installation at the station. At the French

research station in Ny- ̊Alesund, there is a DORIS station. In October 2004 a GISTM (GPS Ionospheric Scintillation and TEC Monitor) receiver was installed at the Mapping Authority structure

in the frame of ISACCO, an Italian research project on ionospheric scintillation observations, led

by Giorgiana De Franceschi of the Italian Institute of Geophysics and Volcanology (INGV).

2. Component Description

The antenna is intended for geodetic use and is designed for receiving in S-band and X-band.

Ny- ̊Alesund is located so far north that the sun is below the horizon from the 23rd of October

until the 22nd of February and has midnight sun from the 20th of April to the 27th of August.

The station is situated under the auroral circle during the daytime, giving some extra disturbance

in the ionosphere, but generally the polar atmosphere is calmer than the atmosphere closer to the

equator.

80 IVS 2011 Annual Report
Geodetic Institute, Norwegian Mapping Cadastre Authority Ny- ̊Alesund 20-Meter Antenna

Figure 1. Ny- ̊Alesund antenna.

3. Staff

Table 1. Staff related to VLBI operations at Ny- ̊Alesund.

Hønefoss: Section manager: Line Langkaas

Station responsible at Hønefoss: Line Langkaas

Ny- ̊Alesund: Station commander: Carl Petter Nielsen

Engineer Geir Mathiassen

Engineer Moritz Sieber

Engineer Lars Karvonen until 2011.10.01

Engineer  ̊Asmund Skjæveland since 2011.11.15

Carl Petter Nielsen has a three-year contract as base commander, ending 2012.12.31. Geir

Mathiassen and Moritz Sieber have two-year contracts as engineers ending 2012.09.01 and

2013.07.31, respectively. Lars Karvonen terminated his contract on 2011.10.01 and was replaced

by Asmund Skjæveland on 2011.11.15. When Carl Petter Nielsen is off, one of the others step in

as base commander.

IVS 2011 Annual Report 81
Ny- ̊Alesund 20-Meter Antenna Geodetic Institute, Norwegian Mapping Cadastre Authority

4. Current Status and Activities

Ny- ̊Alesund participated in the scheduled VLBI experiments. During 2011 e-transfer was

extended to transfer all experiments from Ny- ̊Alesund to the different correlators. The fibercable between Longyearbyen and Ny- ̊Alesund was postponed until 2013/2014. The new cable will

enable us to take part in real time correlation as opposed to our present radiolink, which is 100

Mbit/s.

The Super Conducting Gravimeter (SCG) placed on the same foundation as IGS-GPS NYA1

has been running without problems. The yearly service on the system was performed by the staff

in September. There were some problems in transporting the liquid helium (LHe) to Ny- ̊Alesund.

Due to the 2–3 weeks it takes to transport the LHe to Ny- ̊Alesund, most of it might turn into

gas on the journey, especially if the ship experiences bad weather. We also experienced increasing

problems transferring LHe from the transport container to the gravimeter. As a result we had three

shipments of LHe in 2011. To reduce the running cost of the gravimeter the NMA is applying for

a new gravimeter with a built-in regenerating LHe system. National Astronomical Observatory of

Japan, Mizusawa VERA Observatory, which owns the SCG, lent this equipment to NMA starting

2007.04.01, to continue the scientific measurement series.

NMA plans to take part in VLBI2010 and was granted 219 million NOK from the Norwegian

Government for two new antennas and SLR. Ny- ̊Alesund is an Arctic research village, and the

scientific community (organized in NySMAC) would like to keep the surroundings as pristine and

unaffected by human activity as possible. Therefore NMA has initiated an extensive Enviromental

Impact Assessment (EIA) involving the different interested parties. This work is soon to be finished

enabling us to complete the planning of the project. Our hope is that everybody involved will find

that the VLBI2010 project is acceptable for the ongoing research in Ny- ̊Alesund.

The Mark IV formatter was replaced with a Mark 5 sampler. Mark 5B is now used as the

recorder, and Mark 5A is used for transferring data to correlators. In early May the receivermonitorsystem broke down, and we are in the process of replacing it with an alternative PLCsystem.

In order to improve the skills of the staff some measures were taken. In March, Geir Mathiassen

and Lars Karvonen visited Wettzell. Lars Karvonen and Moritz Sieber attended the Technical

Operations Workshop (TOW) in early May, and Moritz Sieber attended the ILRS workshop in

Wettzell in the middle of May. Carl Petter Nielsen and Moritz Sieber visited Wettzell in June. A

climbing and safety course was held in November. In November Moritz Sieber studied the SLR at

Wettzell, and during that period Kent Roskifte substituted for him in Ny- ̊Alesund.

During August the roof was insulated against the arctic cold, and two heat-pumps were installed

to improve our energy budget. The lift was treated for rust and repainted. A new car was bought

in October, and the oldest car was sold.

Our present antenna is scheduled to observe until 2022, when it will be taken down due to

airport safety. A representative for Vertex inspected the antenna in August and produced a list of

measures that need to be carried out in order to keep our old lady alive.

5. Future Plans

Ny- ̊Alesund will continue to participate in the 123 regular and 46 Intensive experiments. Our

aim is to use e-transfer for all transfers of data. A new system for monitoring the receiver will be

82 IVS 2011 Annual Report
Geodetic Institute, Norwegian Mapping Cadastre Authority Ny- ̊Alesund 20-Meter Antenna

implemented.

During 2012 competitive tendering for the different parts of the VLBI2010 project will be

carried out. Hopefully work on the infrastructure can start in late 2012. The new fiber-cable

between Longyearbyen and Ny- ̊Alesund has been delayed. Depending on the availability and price

of cable-ships the fiber-cable will be laid during the summer of 2012 or 2013.

IVS 2011 Annual Report 83
German Antarctic Receiving Station (GARS) O’Higgins Bundesamt f ̈ur Kartographie und Geod ̈asie (BKG)

German Antarctic Receiving Station (GARS) O’Higgins

Christian Pl ̈otz, Thomas Kl ̈ugel, Alexander Neidhardt

Abstract

In 2011 the German Antarctic Receiving Station (GARS) O’Higgins contributed to the IVS observing program with four observation sessions. Maintenance and upgrades were made. A new replacement

dewar is under construction.

1. General Information

The German Antarctic Receiving Station (GARS) is jointly operated by the German Aerospace

Center (DLR) and the Federal Agency for Cartography and Geodesy (BKG, belongs to the duties of the Geodetic Observatory Wettzell (GOW)). The Institute for Antarctic Research Chile

(INACH) coordinates the activities and logistics. The 9-m radio telescope at O’Higgins is used

for geodetic VLBI and for downloading of remote sensing data from satellites like ERS-2 (mission

ended in September 2011) and TanDEM-X as well as for commanding and monitoring of spacecraft

telemetry. In 2011 the station was manned by DLR staff the entire year and by BKG staff only

in January and February for the VLBI observations. The VLBI campaign in November-December

2011 had to be cancelled due to logistical circumstances. Besides engineers and operators from

DLR and BKG, a team for maintaining the infrastructure (e.g., power and freshwater generation)

was present all over the year.

Over the last years, special flights using “Hercules C-130” aircraft and small “Twin Otter

DHC-6” aircraft as well as transportation by ship were organized by INACH in close collaboration

with the Chilean Army, Navy, and Airforce and with the Brazilian and Uruguayan Airforce in

order to transport staff, technical material, and food for the entire campaign from Punta Arenas

via Base Frei on King George Island to O’Higgins on the Antarctic Peninsula. Due to the fact

that the conditions for landing aircraft on the glacier are strongly weather dependent and involve

an increasing risk, the usage of ships for transportation becomes more and more important. In

general, transport of personnel and cargo is always a challenging task. Arrival and departure times

strongly depend on the weather conditions and on the logistical circumstances.

After the long Antarctic winter the VLBI equipment at the station has to be initialized. Damages resulting from the winter conditions or strong storms have to be identified and repaired.

Shipment of each kind of material like spare parts or upgrade kits has to be carefully prepared in

advance.

Beside the 9-m radio telescope for VLBI, the following instruments are operated:

• a H-Maser, an atomic Cs-clock, a GPS time receiver and a Total Accurate Clock (TAC) offer

time and frequency.

• two GNSS receivers both operating in the frame of the IGS network, while one receiver is

additionally part of the Galileo CONGO network. The receivers worked without failure in

2011.

• a meteorological station providing pressure, temperature and humidity and wind information,

as long as the temporarily extreme conditions did not disturb the sensors.

84 IVS 2011 Annual Report
Bundesamt f ̈ur Kartographie und Geod ̈asie (BKG) German Antarctic Receiving Station (GARS) O’Higgins

• a radar tide gauge which was installed in 2011. The radar sensor itself is space referenced

by a GPS-antenna mounted on top and Earth referenced via the local survey network. The

radar gauge is operated only during the Antarctic summer.

• an underwater sea level gauge for permanent monitoring of water pressure, temperature, and

salinity, which was replaced in 2011.

The 9-m radio telescope is designed for dual purpose:

• performing geodetic VLBI and

• receiving data from and sending commands to remote sensing satellites, mainly ERS-2 and

TanDEM-X.

Figure 1. The 9-m radio telescope of GARS O’Higgins.

2. Technical Staff

The members of staff for operation, maintenance, and upgrade of the VLBI system and other

geodetic devices are summarized in Table 1.

Table 1. Staff members

Name Affiliation Function Working for

Johannes Ihde BKG interim head of the GOW (until February 2011) GOW

Ulrich Schreiber BKG head of the GOW (since March 2011) GOW

Christian Pl ̈otz BKG electronic engineer O’Higgins (responsible), RTW

Reiner Wojdziak BKG software engineer O’Higgins, IVS Data Center

Leipzig

Thomas Kl ̈ugel BKG geologist administration for O’Higgins,

laser gyro and local systems

Wettzell

Rudolf Stoeger BKG geodesist logistics for O’Higgins

Alexander Neidhardt FESG head of the RTW group and VLBI station chief RTW, TTW (partly O’Higgins,

laser ranging)

Gerhard Kronschnabl BKG electronic engineer RTW, TTW (partly TIGO

and O’Higgins)

IVS 2011 Annual Report 85
German Antarctic Receiving Station (GARS) O’Higgins Bundesamt f ̈ur Kartographie und Geod ̈asie (BKG)

3. Observations in 2011

GARS participated in the following sessions of the IVS observing program during the Antarctic

summer campaign (January-February 2011)

• IVS-T2074 February 01.-02., 2011

• IVS-OHIG70 February 02.-03., 2011

• IVS-OHIG71 February 08.-09., 2011

• IVS-OHIG72 February 09.-10., 2011

The observations were recorded with Mark 5A. The related data modules were carried from

O’Higgins to Punta Arenas by the staff on their way back. From Punta Arenas the disk units were

shipped by regular air freight back to Wettzell and then to the correlator in Bonn, Germany.

4. Maintenance

The extreme environment conditions in the Antarctic require special attention to the GARS

telescope and the infrastructure. Corrosion frequently results in problems with connectors and

capacitors. Defective equipment needs to be detected and replaced. The antenna, the S/X-band

receiver, the cooling system, and the data acquisition system have to be activated properly.

The construction of the new dewar is in progress in order to replace the original O’Higgins

dewar. This one has to be evacuated permanently by a turbo molecular pump to maintain the

required vacuum due to a leakage. Besides this the IF-Distributor was shipped to Wettzell to

be repaired. The board for the communication with the NASA Field System bailed out and was

replaced by a new one, and all damaged components were replaced. This turned out to be a

difficult task, as some components as well as technical information are barely available anymore.

Figure 2. The new radar tide gauge which was installed in 2011.

5. Technical Improvements

A new backup system was installed which allows the copying of the VLBI data to a local disk

in order to keep a copy of the raw data on site. The system has a capacity to store the data

86 IVS 2011 Annual Report
Bundesamt f ̈ur Kartographie und Geod ̈asie (BKG) German Antarctic Receiving Station (GARS) O’Higgins

of observation campaigns from one year. Data access and administration is possible via network

communication.

The remote control of complete VLBI sessions could be extended. Using the newly developed

Wettzell software, the O’Higgins Field System can be controlled over a secure Internet connection

from Wettzell. This is a key feature to extend the operation periods in GARS O’Higgins.

6. Upgrade Plans for 2012

The replacement dewar will be completed. A dedicated plan should offer a shared, interleaved

observation of satellites (DLR) and VLBI sources (BKG) during the whole year. Some antenna

motors must be replaced, and a gear needs to be inspected. There are further plans to replace

the receiver with a more suitable, smaller, and more maintainable system, similar to the TWIN

tri-band-receiver. This needs to be planned and designed.

IVS 2011 Annual Report 87
Onsala Space Observatory (OSO) Onsala Space Observatory (OSO)

Onsala Space Observatory – IVS Network Station

R ̈udiger Haas, Gunnar Elgered, Johan L ̈ofgren, Tong Ning, Hans-Georg Scherneck

Abstract

During 2011 we contributed to 38 IVS sessions, including the CONT11 campaign. We used the

majority of the sessions that involved both Onsala and Tsukuba to do ultra-rapid dUT1 observations

together with our colleagues in Tsukuba. In particular, the whole CONT11 campaign was operated in

ultra-rapid mode. Furthermore, we observed one additional one-baseline ultra-rapid dUT1 session, a

three-station ultra-rapid EOP-session, the Venus Express space probe, and the RadioAstron satellite.

1. General Information

The Onsala Space Observatory is a fundamental geodetic station with equipment for geodetic

VLBI, GNSS, a superconducting gravimeter, and several radiometers for atmospheric measurements. Figure 1 shows an aerial photo taken on October 13, 2011.

The staff associated with the IVS Network Station at Onsala remained the same as reported

in last year’s report. Contact information is found on www.chalmers.se/rss/oso-en/.

Figure 1. The radome enclosed 20-m radio telescope used for geodetic/astrometric VLBI (1), the IGS

antenna (2), a new GNSS-monument erected in 2011 (3), the water vapor radiometers Astrid (4) and

Konrad (5), the old laboratory for visiting gravimeters (6), and the new gravimeter laboratory (7).

88 IVS 2011 Annual Report
Onsala Space Observatory (OSO) Onsala Space Observatory (OSO)

2. VLBI Observations for Geodesy and Space Navigation

Onsala was involved in the four IVS observing series EUROPE, R1, T2, and RD and participated in the CONT11 campaign, see Table 1. Observations were acquired during 38 IVS sessions.

All experiments were recorded with our Mark IV VLBI-rack and recorded on the Mark 5A unit.

Most of the experiments whose data were correlated at the Bonn correlator were recorded in parallel on the PCEVN-computer that is daisy-chained to the Mark 5A unit. The observed data of

these experiments were then e-transferred off-line using the Tsunami protocol, and no Mark 5

modules were actually sent to Bonn. The data to be correlated at the Haystack correlator were

shipped on Mark 5 modules. However, the data of the last RD-session in 2011 were e-transferred

off-line to the Haystack correlator, and no modules were shipped. The observational data of the

CONT11 campaign were shipped on Mark 5 modules to the Washington correlator.

We used the majority of the sessions involving both Onsala and Tsukuba to perform ultrarapid dUT1 observations. This was done for many of the R1- and RD-sessions, and all of the

CONT11-sessions. In these cases the Onsala data were e-transferred in real-time to the Tsukuba

correlator using the Tsunami protocol. The data were correlated with the corresponding data from

the Tsukuba station in near real-time, followed by a near real-time analysis to determine dUT1.

Using this automated strategy, dUT1 results were already determined during the ongoing VLBI

observations using a “sliding window” approach. This strategy worked very well and produced a

continuous dataset of dUT1 values for the whole 15-day-long campaign. Only during CONT11.07

was it not possible to derive dUT1 values since the Tsukuba telescope had to be stowed because

of a typhoon.

In the second half of the year, a DBBC was installed at Onsala. In order to gain experience

with the new digital system, we performed several parallel recordings with Mark IV/Mark 5A and

DBBC/Mark 5B+. First fringes on all 14 S/X-channels were found by the Tsukuba correlator

using Onsala DBBC/Mark 5B+ data and Tsukuba K5 data for RD.11.04 observed on June 21.

In collaboration with our colleagues in Tsukuba we observed a 12-hour long one-baseline dUT1-

experiment in January. In November we observed the first three-station ultra-rapid EOP experiment, together with Tsukuba and Hobart. The observational data from Onsala and Hobart were

e-transferred in real-time to the Tsukuba correlator, where the data of the three baselines were

correlated and analyzed in near real-time. Again, a sliding window approach was used, and polar

motion and dUT1 were determined in ultra-rapid mode, i.e. during the ongoing session.

We also participated with X-band observations in several campaigns for spacecraft navigation.

We observed four sessions for the determination of the orbit of the Venus Express spacecraft and

participated in one session to determine the orbit of the RadioAstron satellite.

Radio interference due to UMTS mobile telephone signals continued to be a disturbing factor

for the S-band observations.

3. Monitoring Activities in 2011

We continued with the monitoring activities as described in previous annual reports:

Vertical height changes of the telescope tower

We continued to monitor the vertical height changes of the telescope tower using the invar rod

system at the 20-m telescope. The measurements are available at wx.oso.chalmers.se/pisa/.

IVS 2011 Annual Report 89
Onsala Space Observatory (OSO) Onsala Space Observatory (OSO)

Table 1. VLBI observations for geodesy and space navigation at Onsala during 2011: information is given on

whether the data were e-transferred in real-time (RT) and/or off-line (OL) and to which correlator, whether

modules were shipped to a correlator, and whether ultra-rapid dUT1 (UR-dUT1) results were produced.

Exper. Date E-transfer Module UR- General remarks from the observations

RT OL ship. dUT1 and the final correlation

R1-464 01.03 – Bonn – – OK

EUR-109 01.17 – Bonn – – OK

R1-466 01.18 – Bonn – – OK

UR-11.019 01.19 Tsuk – – yes OK, 12 h of ultra-rapid dUT1

R1-477 02.21 – Bonn – – OK, PCal problems for about 6 h

RD-11.01 02.22 Tsuk – Hays yes OK, four scans lost due to Mark 5 problems

EUR-110 03.23 – Bonn – – OK

VEX-03.25 03.25 – JIVE – – OK, Venus Express observations, 2 h

VEX-03.28 03.28 – JIVE – – OK, Venus Express observations, 2 h 45 min

VEX-03.31 03.31 – JIVE – – OK, Venus Express observations, 2 h

R1-476 03.28 – Bonn – – OK

RD-11.02 03.29 – – Hays – OK, several scans missed due to Mark 5 problems

R1-477 04.04 Tsuk Bonn – yes OK, phase-cal problems for 5 h

T2-076 05.03 – Bonn – – OK

R1-484 05.23 – Bonn – – OK, some scans lost due to Mark 5 problems

EUR-111 05.24 – Bonn – – OK, some scans lost due to Mark 5 problems

R1-488 06.20 Tsuk Bonn – yes OK

RD-11.04 06.21 Tsuk – Hays yes OK

R1-496 08.16 Tsuk Bonn – yes OK

R1-497 08.22 Tsuk Bonn – yes OK

T2-077 08.23 Tsuk – Hays yes no correlation report yet

R1-498 08.29 – Bonn – – OK

R1-500 09.12 Tsuk – Wash yes OK

C11-01 09.15 Tsuk – Wash yes OK, spurious signal in PCal for X-band Ch-2

C11-02 09.16 Tsuk – Wash yes no correlation report yet

C11-03 09.17 Tsuk – Wash yes no correlation report yet

C11-04 09.18 Tsuk – Wash yes no correlation report yet

C11-05 09.19 Tsuk – Wash yes OK, spurious signal in PCal for X-band Ch-2

C11-06 09.20 Tsuk – Wash yes no correlation report yet

C11-07 09.21 Tsuk – Wash – no correlation report yet

C11-08 09.22 Tsuk – Wash yes no correlation report yet

C11-09 09.23 Tsuk – Wash yes no correlation report yet

C11-10 09.24 Tsuk – Wash yes no correlation report yet

C11-11 09.25 Tsuk – Wash yes no correlation report yet

C11-12 09.26 Tsuk – Wash yes OK, spurious signal in PCal for X-band Ch-2

C11-13 09.27 Tsuk – Wash yes no correlation report yet

C11-14 09.28 Tsuk – Wash yes no correlation report yet

C11-15 09.29 Tsuk – Wash yes OK, spurious signal in PCal for X-band Ch-2

R1-501 10.03 Tsuk Bonn – yes OK

VEX-11.14 11.14 – JIVE – – OK, Venus Express observations, 2 h 20 min

RA-11.15 11.15 – JIVE – – OK, RadioAstron observations, 1 h 10 min

R1-509 11.28 – Bonn – – receiver/antenna problems, session lost

RD-11.06 11.29 Tsuk Bonn – yes no correlation report yet

UREOP.01 11.30 Tsuk – – yes OK, ultra-rapid EOP Onsala-Tsukuba-Hobart

RD-11.07 12.06 Tsuk Hays – yes no correlation report yet

90 IVS 2011 Annual Report
Onsala Space Observatory (OSO) Onsala Space Observatory (OSO)

Microwave radiometry

The water vapor radiometer Astrid was in operation continuously during 2011, mainly observing in a so-called sky-mapping mode. However, after the first week of the CONT11 campaign the

azimuth drive of the instrument failed, and it could only be operated in tip-curve mode. The second

water vapor radiometer Konrad was successfully upgraded and is in operation again since CONT11.

Calibration of pressure sensor

We continued to calibrate the Onsala pressure sensor using a Vaisala barometer borrowed from

the Swedish Meteorological and Hydrological Institute (SMHI). This instrument was installed at

Onsala in late 2002 and has been calibrated at SMHI’s main facility in Norrk ̈oping every 1–2 years

since then. The latest calibration was on October 11, 2011. Since the installation of a new VLBI

pressure sensor in 2008 the agreement between the Onsala pressure sensor and the SMHI pressure

sensor has been on the level of ±0.1 hPa.

Sea level monitoring

We continued to operate the GNSS-based tide gauge at the coastline at the observatory to

monitor the local sea level. The tidal analysis of the sea level variations clearly shows the dominant ocean tides in the Kattegatt. In August 2011 the GNSS-based tide gauge was moved to a

new location at the observatory, where it was installed semi-permanently. The new installation

has a number of advantages, e.g., that the instrumentation can be mounted at different heights,

in steps of 25 cm, between approximately 1.5 m and 3.5 m above the mean sea level.

Superconducting gravimetry

The superconducting gravimeter (SCG) operated continuously during 2011 and produced a

highly precise record of gravity variations. Of course it recorded earthquakes and free oscillations

of the earth, e.g. in connection to the Sendai 2011 earthquake. Further information on the SCG

and its observations is available at froste.oso.chalmers.se/hgs/SCG/. Measurements of the

auxiliary sensors for monitoring, e.g., bedrock temperature below the gravimeter house are available at wx.oso.chalmers.se/gravimeter/.

Absolute gravimetry

We supported visiting absolute gravity measurement campaigns by the University of Hannover

(Germany) and Lantm ̈ateriet, the Swedish mapping, cadastral and land registration authority.

Seismological observations

The three-axis seismometer provided by Uppsala University and the Swedish National Seismic

Network (SNSN) has been operated continuously on the lower level of the gravimeter laboratory

during 2011. The recorded data are valuable auxiliary observations for the analysis of absolute

gravity measurements.

4. Outlook

The Onsala Space Observatory will continue to operate as an IVS Network Station and to

participate in the IVS observation series. For 2012 we plan to participate in 40 IVS sessions, and

we hope that we eventually can switch over to using the digital backend in operational mode. We

also plan to continue our ultra-rapid project with our Japanese colleagues.

A proposal to construct a VLBI2010 twin-telescope at Onsala was submitted in 2011 to the

Wallenberg foundation. A decision concerning this proposal is expected in 2012. Regardless of the

outcome, we will strive to make the station fully VLBI2010-compatible in the coming years.

IVS 2011 Annual Report 91
Parkes Network Station CSIRO Astronomy and Space Science

Parkes 2011 IVS Report

John Reynolds, Tasso Tzioumis

Abstract

This report presents the status of the Parkes Observatory in 2011, as well as our future plans.

1. Status

In the second full year of IVS membership the Parkes Observatory participated in six 24-hour

IVS sessions, compared to just two in the previous year. These sessions were generally successful,

although one session (CRDS55) was lost to an unusual recorder problem. (This problem has since

resulted in an advisory circular to all stations from the Network Coordinator, headed ‘Mark 5B/B+

“,E” scan check problem’, 20th March 2012).

In August 2011 the Parkes S/X receiver was modified to double the available bandwidth at Xband, in order to support sessions requiring an “IF3” observing configuration. In the first of these

three sessions the improvised IF3 system proved only partially successful, but it was subsequently

improved for the R1507 session in November.

Parkes also continues to support a program led by Leonid Petrov (ADNET Systems/GSFC)

of hybrid astronomy/geodesy observations, refining the locations of several southern hemisphere

radio stations that are equipped with neither dual S/X receiving systems nor IVS-compatible

recording systems. This program also aims to identify additional calibrator sources in the Southern

Hemisphere for “densification” of the ICRF in the south.

2. Future Plans

The outlook for 2012 is a little uncertain owing to possible scheduling constraints arising from

proposed changes to the Parkes Operations model that could impact the availability of the dual S/X

receiver (see http://www.atnf.csiro.au/management/atuc/2012feb/docs/carretti ATUC 1202.pdf

for details). In 2011 these restrictions led to the participation of Parkes in IVS sessions being

confined to just two blocks of time (August and November, each comprising 3 x 24hr sessions). We

are working with our Australian colleagues to ensure that the S/X receiver will continue to remain

available and that the active participation of Parkes in IVS observing programs will continue to

be both valued and supported.

92 IVS 2011 Annual Report
Shanghai Astronomical Observatory, CAS Sheshan

Sheshan VLBI Station Report for 2011

Bo Xia, Zhiqiang Shen, Xiaoyu Hong, Qingyuan Fan

Abstract

The Sheshan VLBI station (also named SESHAN25 in the geodetic community) is located at Sheshan, about 30 km west of Shanghai. A 25-meter radio telescope is in operation at 1.3, 3.6/13, 5, 6,

and 18-cm wavelengths. The Sheshan VLBI station is a member of the IVS and EVN. The SESHAN25

telescope takes part in international VLBI experiments for astrometric, geodetic, and astrophysical

research. Apart from its international VLBI activities, the telescope spent a large amount of time on

the Chinese Lunar Project, including the testing before the launch of the Chang’E-2 satellite and the

tracking campaign after the launch of Chang’E-2.

1. General Information

The Sheshan VLBI station (‘SESHAN25’) is located at Sheshan, 30 km west of Shanghai

downtown. It is hosted by the Shanghai Astronomical Observatory (SHAO), Chinese Academy

of Sciences (CAS). A 25-meter radio telescope is in operation at 1.3, 3.6/13, 5, 6, and 18 cm

wavelengths. The Sheshan VLBI station is a full member of the IVS and EVN. The SESHAN25

telescope takes part in international VLBI experiments in astrometric, geodetic, and astrophysics

research. Apart from its international VLBI activities, the telescope spent a large amount of

time on the Chinese Lunar Project, including testing observations and the tracking campaign of

Chang’E-2.

2. VLBI Observations in 2011

In 2011, SESHAN25 participated in 30 IVS sessions (including six INT3 Intensive sessions).

SESHAN25 also participated in the EVN sessions in February, June, and October. We missed the

IVS session T2077 because of an antenna motor problem. In order to participate in the Chinese

Chang’E-2 Lunar Project, SESHAN25 has observed the Chang’E-2 satellite with long term routine

VLBI tracking model for two or three days per week. We also missed the IVS sessions of RD1103

and R1479 during the Chang’E-2 tracking task.

3. Development and Maintenance of Sheshan Telescope in 2011

A new analog VLBA Terminal, which included a VLBA sampler and a VSI-C card together

with a Mark 5B recorder, worked normally in our station. We solved the sampling status problems

of 1 bit and 2 bit sampling respectively. After upgrading, we successfully participated in the EVN

session 3 and two IVS sessions (R1512 and R1513).

We have upgraded the Mark 5A Firmware Version to 12.13 (APT 10.07, SDK 8.2). We also

upgraded the Mark 5B Firmware Version to 12.06 (APT 10.07, SDK 8.2).

We also performed routine maintenance of our antenna in May of 2012.

IVS 2011 Annual Report 93
Sheshan Shanghai Astronomical Observatory, CAS

4. The Staff of the Sheshan VLBI Station

Table 1 lists the group members of the Sheshan VLBI Station. The staff are involved in the

VLBI program at the station with various responsibilities.

Table 1. The staff of the Sheshan VLBI Station.

Name Background Position & Duty Contact

Xiaoyu Hong Astrophysics Director, Astrophysics xhong@shao.ac.cn

Qingyuan Fan Ant. control Chief Engineer, Antenna qyfan@shao.ac.cn

Zhiqiang Shen Astrophysics Head of VLBI Division zshen@shao.ac.cn

Zhuhe Xue Software Professor, FS zhxue@shao.ac.cn

Quanbao Ling Electronics Senior Engineer,VLBI terminal qling@shao.ac.cn

Bin Li Microwave Technical friend, receiver bing@shao.ac.cn

Tao An Astrophysics Astrophysics antao@shao.ac.cn

Bo Xia Electronics VLBI friend,VLBI terminal bxia@shao.ac.cn

Hong Yu Ant. control Associated Professor, Antenna yuhong@shao.ac.cn

Li Fu Ant. mechanics Engineer, Antenna fuli@shao.ac.cn

Jinqing Wang Electronics Engineer, Antenna jqwang@shao.ac.cn

Lingling Wang Software Engineer, VLBI terminal llwang@shao.ac.cn

Rongbing Zhao Software Engineer, VLBI terminal rbzhao@shao.ac.cn

Weiye Zhong Microwave Engineer, Receiver wyzhong@shao.ac.cn

Wei Gou Electronics Engineer gouwei@shao.ac.cn

Linfeng Yu Electronics Engineer lfyu@shao.ac.cn

Yongbin Jiang Electronics Engineer jyb@shao.ac.cn

Yunxia Sun HVAC Engineer, Refrigeration sunyunxia@shao.ac.cn

Xiaocong Wu Electronics Engineer wuxc@shao.ac.cn

Wen Guo Electronics Engineer gw@shao.ac.cn

Jian Dong Ant. Control Engineer dongjian@shao.ac.cn

5. Outlook

In 2012 the Sheshan radio telescope will take part in 13 IVS sessions and 2 EVN sessions. The

telescope will regularly monitor the Chang’E-2 satellite in its lunar orbit for 2-3 days per week in

2012.

94 IVS 2011 Annual Report
Radio Astronomy Lab of Crimean Astrophysical Observatory Simeiz station

Geodetic and Astrophysical Study at the Simeiz VLBI Station

A.E. Volvach

Abstract

This report gives an overview about the geodetic and astrophysical activities at 22-m radio telescope

RT-22 (Simeiz). We summarize briefly the status of Simeiz station as an IVS Network Station.

1. General Information

The Simeiz VLBI Station (also known as CRIMEA in the geodetic community), operated by

Radio Astronomy Laboratory of Crimean Astrophysical Observatory of the Ministry of Education

and Sciences of Ukraine, is situated on the coast of the Black Sea near the village of Simeiz 20 km

west of the city of Yalta in Ukraine.

RT-22, the 22-meter radio telescope, which was put into operation in 1966, is among the 10

most efficient telescopes in the world. Various observations in the centimeter and millimeter wave

ranges have been performed with this telescope and will be performed in the near future. First

VLBI observations were performed in 1969 on the Simeiz (RT-22) to Green Bank (RT-43, USA)

intercontinental baseline. RT-22 is equipped with radiometers at the 92 cm, 18 cm, 13 cm, 6 cm,

3.5 cm, 2.8 cm, 2.3 cm, 2.0 cm, 13.5 mm, and 8 mm wavelengths.

Figure 1. Simeiz VLBI station, 22-m radio telescope RT-22.

RT-22 is a fully steerable paraboloid, 22 m in diameter, with a focal length of 9.525 m. The

rms surface accuracy is 0.15 mm. The horizontal axis is shifted by −1.8 ± 0.2 mm relative to the

IVS 2011 Annual Report 95
Simeiz station Radio Astronomy Lab of Crimean Astrophysical Observatory

azimuthal axis. The operating ranges of turning angles are -210◦to 210◦in azimuth and -3◦to

90◦in elevation. The maximum slew rate of the antenna is 1.5◦/sec.

RT-22 is used for multifrequency regular monitoring of active galactic nuclei; for the exploration

of solar and stellar activity; for VLBI observations within the frames of international astrophysical,

geophysical, and radar programs; for the exploration of water vapor, hydroxyl, methanol, and SiO

cosmic masers; as well as for spectral observations in the range of frequencies from 85 GHz to 115

GHz; i.e., it is used to study the most challenging problems of modern astrophysics and natural

history.

2. Effective Area of the Antenna of the 22-m Radio Telescope RT-22

Forty years of intensive observations with the 22-m radio telescope RT-22 CrAO and studying

its characteristics at millimeter wavelengths demonstrated a fairly high quality of the instrument.

Based on the results of calibrator observations at 13.5 mm and 8.2 mm wavelengths in 1985 and

2010, the dependence of the effective area of the RT-22 CrAO antenna on ambient temperature

and elevation was determined. The obtained results confirm a high quality of the RT-22 antenna

at millimeter wavelengths. A high accuracy of the reflector surface makes it possible to observe

at millimeter wavelengths right to 2 mm. At 8.2 mm wavelength, the effective area changes by no

more than 5% when the antenna is moved from zenith to 15◦elevation angle. The effective area

of the RT-22 antenna decreases by ∼ 7% when the ambient temperature deviates by 10◦C from

the value T0 = 17.5◦C. Large antennas, intended to operate at maximum frequencies, should be

built either taking into account the climatic conditions of the antenna sites or taking measures to

provide thermal stability of the antenna.

3. Current Status and Activities

During 2011 the Space Geodesy and Geodynamics stations regularly participated in the following international network programs: IVS, the International GNS Service (IGS), and the International Laser Ranging Service (ILRS).

From 1 January through 31 December 2011, Simeiz VLBI station participated in twelve 24-

hour geodetic sessions. Simeiz regularly participated in the EUROPE and T2 series of geodetic

sessions.

The results for the RT-22 Simeiz coordinates were compared with the monthly averages of

the long-term measurements of the Black Sea tide gauge stations, located in Odessa, Ochakov,

Sevastopol, Yalta, and Katsively. All items of sea level measuring have a different water flow,

which gives the opportunity to explore global geodynamic processes and their dependence on solar

activity cycle. The spectrum of sea level variations in different points indicates the presence of

periods of one to eleven and twenty-two years. Using wavelet analysis the periods for each tide

gauge station are estimated separately.

Use of the Simeiz antenna is shared with the “Radioastron” program:

1. The catalog of sources for flight program “Radioastron”.

Observations of sample sources from the preliminary “Radioastron” catalog were obtained at 22.2

and 36.8 GHz with the RT-22 radio telescope of the Crimean Astrophysical Observatory. We

have determined the distribution of the source spectral indices between these frequencies [1]. The

96 IVS 2011 Annual Report
Radio Astronomy Lab of Crimean Astrophysical Observatory Simeiz station

distributions of the spectral indices of the RT-22 sample have more important dispersion of the

distribution than in the WMAP catalog (between 23 and 33 GHz) due to input parameters of

sample sources from the “Radioastron” catalog. We have plotted the log(10∆N/N0) − logS dependence down to the flux levels of about 0.1 Jy using the survey data near 22 GHz. There is

a reduction in the density of cosmological sources in relation to non-evolving Euclidean universe

(Figure 2). The variability of individual sources in connection with flare activity is considered.

0,6

0,7

0,8

0,9

1

1,1

1,2

0,1 1 10 100

log(10∆N/∆No)

S, Jy

Figure 2. The differential statistical dependency logN-logS.

2. The RT-22 of CrAO: scientific program elaboration and performance of groundbased VLBI test experiments within the framework of the project “Radioastron”.

The Earth-space science program “Radioastron” includes high-resolution (microseconds of arc)

studies of the morphology and dynamics of the circumnuclear regions of sources of powerful energy. In accordance with the scientific cooperation between Ukraine and Russia, the study is

carried out using the 22-m radio telescope RT-22 of the Crimean Astrophysical Observatory. The

research program provides the investigation with highly sensitive radiometers at frequencies of 22

GHz and 36 GHz. This makes it possible to obtain spectral characteristics of the sources near 22

GHz, which is the fundamental frequency of the experiment “Radioastron”. To realize the project,

the scientific program is developed, a substantial part of which is the study of compact structures

in extragalactic sources, and groundbased VLBI test experiments are conducted [2].

3. The testing of the ground-based segment of the “Radioastron” mission. The Simeiz

- Pushchino interferometer at wavelengths of 6 and 1.35 cm.

In accordance with the scientific cooperation between Ukraine and Russia a series of studies was

done for the preparation of the operation of the ground segment of the “Radioastron” mission. Using the 22-m radio telescope RT-22 (Crimean Astrophysical Observatory) the scientific program of

measurements was prepared, a substantial part of which is the study of the compact structures in

the extragalactic sources, as well as the structure and spatial distribution of H2O galactic masers.

For testing the model of the ground segment of “Radioastron”, RT-22 of Crimean Astrophysical

Observatory in Simeiz and RT-22 of the PRAO in Pushchino jointly conducted groundbased VLBI

test experiments. As a result of data processing using the ASC LPI correlator the amplitude and

phase of the cross-correlation functions were obtained and calibrated, and the available coherence

time was estimated [3]. The results of the experiment demonstrate readiness of RT-22 (CrAO)

to participate in further joint radiointerferometric sessions, including those of the “Radioastron”

project. The modernization of the Simeiz station was opened up by the possibility of beginning

IVS 2011 Annual Report 97
Simeiz station Radio Astronomy Lab of Crimean Astrophysical Observatory

research of systematic and complex polarization of star forming regions.

4. The testing of the ground-based segment of the “Radioastron” mission. The Simeiz

- Evpatoria interferometer at wavelengths of 6 and 18 cm.

In accordance with the scientific cooperation between Ukraine and Russia a series of studies was

performed for the preparation of the operation of the ground segment of the “Radioastron” mission.

Using the 22-m radio telescope RT-22 the scientific program of measurements was prepared, a

substantial part of which is the study of the compact structures of the extragalactic sources.

For testing the model of the ground segment of “Radioastron”, RT-22 of Crimean Astrophysical

Observatory in Simeiz and RT-70 (P-2500) in Evpatoria jointly conducted groundbased VLBI test

experiments at 6 cm and 18 cm [4]. As a result of data processing using the ASC LPI correlator

the amplitude and phase of the cross-correlation functions were obtained and calibrated, and the

available coherence time was estimated (Figure 3).

-3e-005 -2e-005 -1e-005 0 1e-005 2e-005 3e-005

Delay, sec

0

0.005

0.01

0.015

0.02

0.025

Corr. amplitude

a

-2e-005 -1e-005 0 1e-005 2e-005

Delay, sec

0

0.01

0.02

0.03

Corr. amplitude

b

Figure 3. Simeiz-Evpatoria, 6 cm. a) 3C279, t=300 sec, S/N > 400 sec; b) 3C286, t=180 sec, S/N = 440

sec.

The results of the experiment demonstrate the readiness of RT-22 and RT-70 to participate in

space-ground Very Long Baseline Interferometer sessions of the “Radioastron” project.

4. Future Plans

Our plans for 2012 are the following: to put into operation the VLBI Data Acquisition System

DBBC, upgrade the laser of SLR Simeiz-1873 station, and set up a new GPS station near Simeiz

VLBI station.

References

[1] A. E. Volvach // Space Science and Technology. 2009. T.15. N.5. P.8297.

[2] A. E.Volvach, N. S. Kardashev, M. G. Larionov // Space Science and Technology. 2011. T.17. N.1.

P.70–75.

[3] A. E. Volvach, V. I. Kostenko, M. G. Larionov, L. N. Volvach // Space Science and Technology. 2011.

T.17. N.2. P.45–50.

[4] Volvach A. E., Kostenko V. I., Larionov M. G., Volvach L. N., et al. // Bulletin of the Crimean

Astrophysical Observatory. 2012. T.108. N.1. P.1–7.

98 IVS 2011 Annual Report
Institute of Applied Astronomy of Russian Academy of Sciences Svetloe Station

Svetloe Radio Astronomical Observatory

Sergey Smolentsev, Ismail Rahimov

Abstract

This report summarizes information on recent activities at the Svetloe Radio Astronomical Observatory in 2011. During the previous year a number of changes were carried out at the observatory to

improve some technical parameters and upgrade some units to the required status. The report also

provides an overview of current geodetic VLBI activities and gives an outlook for the next year.

1. General Information

Svetloe Radio Astronomical Observatory (Figure 1) was founded by the Institute of Applied

Astronomy (IAA) as the first station of the Russian VLBI network QUASAR [1].

The sponsoring organization of the project is the Russian Academy of Sciences (RAS). The

Svetloe Radio Astronomical Observatory is situated near Svetloe village in the Priozersky district

of the Leningrad region (Table 1). The geographic location of the observatory is shown on the

IAA RAS Web site: http://www.ipa.nw.ru/PAGE/rusipa.htm. The basic instruments of the observatory are a 32-m radio telescope equipped with special technical systems for VLBI observations,

GPS/GLONASS/Galileo receivers, and an SLR system installed in 2011.

Figure 1. Svetloe observatory.

Table 1. Svetloe Observatory location and address.

Longitude 29◦47

′

Latitude 60◦32

′

Svetloe Observatory

Leningrad region, Priozerski district

188833 Russia

rahimov@osvtl.spb.ru

IVS 2011 Annual Report 99
Svetloe Station Institute of Applied Astronomy of Russian Academy of Sciences

2. Technical Staff

Ismail Rahimov — observatory chief,

Tatiana Andreeva — main operator,

Andrey Mikhailov — FS, pointing system control.

3. Technical and Scientific Information

Table 2. Technical parameters of the radio telescope.

Year of construction 2000

Mount AZEL

Azimuth range ±270◦(from south)

Elevation range from −5

◦

to 95◦

Maximum azimuth

- velocity 1.5

◦/s

- tracking velocity 1.5

′/s

- acceleration 0.2

◦/s2

Maximum elevation

- velocity 0.8

◦/s

- tracking velocity 1.0

′/s

- acceleration 0.2

◦/s2

Pointing accuracy better than 10′′

Configuration Cassegrain

(with asymmetrical subreflector)

Main reflector diameter 32 m

Subreflector diameter 4 m

Focal length 11.4 m

Main reflector shape quasi-paraboloid

Subreflector shape quasi-hyperboloid

Main reflector surface accuracy ± 0.5 mm

Frequency range 1.4–22 GHz

Axis offset −3.0 ± 1.5 mm

The electrical part of the gear and pointing system of the radio telescope was upgraded in 2008

— 2010. A new DAS R1002M designed at the IAA [2, 3] has been used in all kinds of VLBI

observational programs since October 2011. The DAS R1002M is suited to work with Mark 5B

and Mark 5B+ recording systems.

4. Co-location of VLBI, GPS/GLONASS and SLR System

The Topcon GPS/GLONASS/Galileo receiver with meteo station WXT-510 was tested and

put into operation (Figure 2).

100 IVS 2011 Annual Report
Institute of Applied Astronomy of Russian Academy of Sciences Svetloe Station

Figure 2. Topcon GPS/GLONASS/Galileo receiver at Svetloe observatory.

The SLR system “Sazhen-TM” (Figure 3) was mounted in October 2011. The “SazhenTM” SLR system was manufactured by Open Joint-stock Research-and-Production Corporation

“Precision Systems and Instruments”. The technical parameters of the system are presented in

Table 3.

Figure 3. “Sazhen-TM” SLR system at Svetloe observatory.

5. Current Status and Activities

The Svetloe observatory participates in IVS and domestic VLBI observational programs. During 2011 Svetloe station participated in 27 diurnal IVS-R1, IVS-R4, IVS-T2, and EURO sessions

and in 17 IVS Intensive sessions.

Svetloe participated in 49 diurnal sessions in the frame of the domestic Ru-E program for

determination of all Earth orientation parameters, and in 5 one-hour Ru-U sessions for obtaining

Universal Time using e-VLBI data transfer.

IVS 2011 Annual Report 101
Svetloe Station Institute of Applied Astronomy of Russian Academy of Sciences

Table 3. Technical parameters of the SLR system “Sazhen-TM”.

Ranging distance, day 400-6000 km

Ranging distance, night 400-23000 km

Aperture 25 cm

Wavelength 532 nm

Beam divergence 12′′

Laser pulse frequency 300 Hz

Pulse energy 2.5 mJ

Mass 170 kg

Normal points precision 1 cm

Angular precision 1-2′′

6. Outlook

Our plans for the coming year are the following:

• To participate in IVS observations

• To carry out domestic observational programs for obtaining Universal Time with e-VLBI

data transfer and Earth orientation parameters once a week

• To carry out SLR observations of geodetic and navigation satellites

• To participate in EVN and RADIOASTRON observational sessions

• To continue geodetic monitoring of the antenna parameters.

References

[1] Finkelstein A., Ipatov A., Smolentsev S. The Network “Quasar”: 2008-2011 // “Measuring the future”,

Proc. of the Fifth IVS General Meeting, A. Finkelstein, D. Behrend (eds.), St. Petersburg, “Nauka”,

2008. pp. 39–46.

[2] Grenkov S. A., Nosov E. V., Fedotov L. V., Koltsov N. E. A Digital Radio Interferometric Signal

Conversion System // Instruments and Experimental Techniques, 2010. Vol. 53, No. 5. pp. 675–681.

[3] Nosov E. Next-Generation DAS for the Russian VLBI-Network. // 20th EVGA Meeting. MPIfR, Bonn.

2011. pp. 41–43.

102 IVS 2011 Annual Report
National Institute of Polar Research JARE Syowa Station 11-m antenna

JARE Syowa Station 11-m Antenna, Antarctica

Yuichi Aoyama, Koichiro Doi, Kazuo Shibuya

Abstract

In 2011, the 51st and the 52nd Japanese Antarctic Research Expeditions (hereinafter, referred to as

JARE–51 and JARE–52, respectively) participated in six OHIG sessions, OHIG70, 71, 72, 73, 74, and

75. These data were recorded on hard disks through the K5 terminal. The hard disks for the former

three sessions were brought back from Syowa Station to Japan in April 2011, by the icebreaker, Shirase,

while those for the latter three sessions are scheduled to arrive in April 2012. The data obtained from

the OHIG70, OHIG71, and OHIG72 sessions by JARE–51 and JARE–52 have been transferred to the

Bonn Correlator via the NICT’s servers. At Syowa Station, JARE–52 and JARE–53 will participate

in six OHIG sessions in 2012.

1. General Information

With the objective of conducting studies of polar science, the National Institute of Polar

Research (NIPR) is managing the Japanese Antarctic Research Expeditions (JAREs). The 30

members of JARE–52 overwintered at Syowa Station, East Ongul Island, East Antarctica in 2011.

Syowa Station has become one of the key observation sites in the Southern Hemisphere’s geodetic network, as reported in [1]. As part of these geodetic measurements, the JAREs have been

operating the 11-m S/X–band antenna at Syowa Station (69.0◦S, 39.6◦E) for geodetic VLBI experiments since February 1998. A cumulative total of 97 quasi-regular geodetic VLBI experiments

had been observed by the end of 2011.

2. Component Description

For VLBI, the Syowa antenna is registered as IERS Domes Number 66006S004 and as CDP

Number 7342. The basic configuration of the Syowa VLBI front-end system has not changed from

the description in [2]. A K5 recording system was introduced at Syowa Station in September 2004.

Syowa’s K4 recording terminal had been fully replaced by K5 simultaneously with the termination

of the SYW session at the end of 2004. Syowa has participated in the OHIG sessions in the austral

summer season since 1999. Data transfer through an Intelsat satellite link from Syowa Station to

NIPR has been available since 2004. However, its maximum transfer speed is about 200 kB/sec,

which is too slow to be practical for the transfer of the amount of VLBI data.

3. Staff of the JARE Syowa Station 11-m Antenna

The 11–m S/X–band antenna at Syowa Station is operated and maintained by JARE and

NIPR. The staff members are listed in Table 1. OHIG sessions in 2011 were performed primarily

by the staff of JARE–52 as shown in Figure 1. The staff of JARE–51 greatly supported JARE–52

during OHIG70 – OHIG72, in order to hand the operation and maintenance of the 11–m antenna

over to their successor (JARE–52).

IVS 2011 Annual Report 103
JARE Syowa Station 11-m antenna National Institute of Polar Research

Table 1. Staff members

Name Affiliation Function

Kazuo SHIBUYA NIPR Project coordinator

Koichiro DOI NIPR Liaison officer

Yuichi AOYAMA NIPR Liaison officer

Iuko TSUWA University of Tokyo Chief operator of JARE–51

Yoshinao KINJYO NEC Antenna engineer for JARE–51

Syunsuke IWANAMI Tomakomai National College Chief operator of JARE–52

of Technology

Shinobu TAKAHIRA NEC Antenna engineer for JARE–52

JARE–51: February 2010 – January 2011

JARE–52: February 2011 – January 2012

Figure 1. Syowa VLBI staff of JARE–52, S. Iwanami (left) and S. Takahira (right).

4. Current Status and Activities

4.1. Notes on System Maintenance

The hydrogen maser (Anritsu RH401A; HM–1002C) was transported to Japan by the icebreaker

Shirase in April 2011, because of the trouble with the 10 MHz output unit that occurred in

December 2010. The HM–1002C was repaired and overhauled by technical experts of Anritsu

and was loaded again on the Shirase in the middle of October 2011. We planned to re-install the

HM–1002C at Syowa Station as the backup system. However, it was impossible to transport the

HM–1002C from the Shirase to the Syowa Station, because the Shirase could not approach the

Syowa Station in this austral summer season due to dense and thick sea ice. The HM–1002C will

104 IVS 2011 Annual Report
National Institute of Polar Research JARE Syowa Station 11-m antenna

be back in Japan in April 2012 and will be deployed at the Syowa Station again in the next austral

summer.

Another hydrogen maser (Anritsu RH401A; HM–1001C) has been used for VLBI observations

since January 2011. On 11 March 2011, its ion pump was interrupted by instability in both voltage

and frequency of the generator for power supplies at Syowa Station. In addition, an uninterruptible

power supply (UPS) for the HM–1002C broke down simultaneously. Due to a low vacuum inside

the HM–1001C, the hydrogen maser oscillator was stopped. In July 2011, the staff of JARE–52

restored its high vacuum and confirmed the hydrogen maser generation. We immediately compared

1 PPS and 10 MHz signals of the HM–1001C with those of GPS using an oscilloscope, and we

observed no apparent differences between the HM–1001C and GPS. The HM–1001C kept stable

after its restarting.

A significant clock offset of the Syowa system was found in the correlation procedure for the

OHIG68 session. This offset also appeared in the correlation procedures for the OHIG69, 70,

71, and 72 sessions, although the hydrogen maser was replaced before the OHIG70 session. We

pinpointed the cause of the clock offset during preparation for the OHIG74 session. Although

we had believed that the 1 PPS signal of the HM–1001C, which was synchronized with GPS 1

PPS, was being directly used as the reference of the K5 recording system, in actuality, the K5

system was referred to 1 PPS signals of the SONY DFC-1100. The DFC-1100 internally generates

1 PPS by synchronizing to HM–1001C’s 1 PPS, which was the external reference. The staff of

JARE-53 found a warning of this synchronization system of DFC-1100 on November 8, 2011.

The synchronization system had probably failed since February 2010. The clock delay of DFC1100’s 1 PPS in comparison with GPS was about 700 msec measured with the oscilloscope. After

resetting the synchronization system, the clock delay became insignificant. However, we changed

an arrangement of 1 PPS signal cables on November 8 as follows: 1 PPS signal cables from HM–

1001C were connected to DFC-1100 and directly to K5 system; 1 PPS signal cable from DFC-1100

was connected to the HP universal counter for checking the clock offset in comparison with GPS.

4.2. Session Status

Table 2 summarizes the status of processing as of December 2011 for the sessions after 2008.

The OHIG sessions involved Fortaleza (Ft), O’Higgins (Oh), Kokee Park (Kk), Parkes (Pa), TIGO

Concepci ́on (Tc), Hobart 26-m antenna (Ho), Hobart 12-m antenna (Hb), HartRAO (Hh), Warkworth (Ww), and Syowa (Sy). In 2005, Syowa joined the CRD sessions, but after 2006, Syowa

participated only in OHIG sessions. Syowa took part in six OHIG sessions in 2011.

Until 2004, K4 tapes containing the OHIG sessions’ data from Syowa Station were copied to

Mark IV tapes at GSI, and the Mark IV tapes were sent to the Mark IV Correlator for final

correlation. Since the introduction of the K5 system, K5 hard disk data brought back from Syowa

Station have been transferred by ftp to the MIT Haystack Observatory or the Bonn Correlator

through a NICT server and converted to the Mark 5 format there.

4.3. Analysis Results

As of December 2011, Syowa had contributed 88 sessions from May 1999. Among them, 77

sessions up to February 2011 had been analyzed with the software CALC/SOLVE developed by

NASA/GSFC. According to the result analyzed by the BKG IVS Analysis Center, the length of

the Syowa–Hobart baseline is increasing with a rate of 55.0 ± 0.8 mm/yr. The Syowa–HartRAO

IVS 2011 Annual Report 105
JARE Syowa Station 11-m antenna National Institute of Polar Research

Table 2. Status of OHIG sessions as of December 2011.

Code Date Station Hour Correlation Solution Notes

OHIG62 2009/Feb/04 Ft, Ho, Kk, Oh, Tc 24 h Yes Yes J50

OHIG63 2009/Feb/10 Ft, Ho, Kk, Oh, Tc 24 h Yes Yes

OHIG64 2009/Feb/11 Ft, Ho, Kk, Oh, Tc 24 h Yes Yes

OHIG65 2009/Nov/10 Ho, Kk, Oh, Tc 24 h Yes Yes

OHIG66 2009/Nov/11 Ho, Kk, Oh, Tc 24 h Yes Yes

OHIG67 2010/Feb/03 Ft, Kk, Oh, Tc 24 h Yes Yes J51

OHIG68 2010/Feb/09 Ft, Ho, Kk, Oh, Tc, Hb 24 h Yes Yes

OHIG69 2010/Feb/10 Ft, Ho, Kk, Oh, Tc, Hb 24 h Yes Yes

OHIG70 2011/Feb/02 Hb, Hh, Ho, Kk, Oh, Tc 24 h Yes Yes J52

OHIG71 2011/Feb/08 Hb, Hh, Kk, Oh, Tc 24 h Yes Yes

OHIG72 2011/Feb/09 Hh, Kk, Oh, Tc 24 h No No

OHIG73 2011/Nov/01 Ft, Kk, Ww 24 h – –

OHIG74 2011/Nov/08 Ft, Kk, Tc, Ww 24 h – –

OHIG75 2011/Nov/09 Ft, Kk, Tc, Ww 24 h – –

J50: JARE–50, op Y. Murakami eng Y. Yamaguchi J51: JARE–51, op I. Tsuwa eng Y. Kinjyo

J52: JARE–52, op S. Iwanami eng S. Takahira

baseline shows a slight increase in its length with a rate of 11.1 ± 0.9 mm/yr. These results agree

approximately with those of GPS. The Syowa–O’Higgins baseline also shows a slight increase,

although its rate is only 2.1 ± 1.0 mm/yr. Detailed results from the data until the end of 2003 as

well as comparisons with those from other space geodetic techniques were reported in [3].

5. Future Plans

NIPR has already started to discuss how to remove the Syowa VLBI antenna during December

2015 – February 2016. Therefore, we must make a concrete plan and obtain a budget for replacing

the Syowa antenna within a few years.

References

[1] Shibuya, K., Doi, K., and Aoki, S. (2003): Ten years’ progress of Syowa Station, Antarctica, as a

global geodesy network site. Polar Geoscience, 16, 29-52.

[2] Shibuya, K., Doi, K., and Aoki, S. (2002): JARE Syowa Station 11-m Antenna, Antarctica, in

International VLBI Service for Geodesy and Astrometry 2002 Annual Report, 149-152, NASA/TP2003-211619, ed. by N. R. Vandenberg and K. D. Baver.

[3] Fukuzaki, Y., Shibuya, K. Doi, K., Ozawa, T., Nothnagel, A., Jike, T., Iwano, S., Jauncey, D.L.,

Nicolson, G.D., and McCulloch, P.M. (2005): Results of the VLBI experiments conducted with

Syowa Station, Antarctica. J. Geod., 79, 379-388.

106 IVS 2011 Annual Report
Bundesamt f ̈ur Kartographie und Geod ̈asie - TIGO TIGO

Status and Developments at TIGO Concepci ́on

Cristian Herrera, Felipe Pedreros, Octavio Zapata, Hayo Hase

Abstract

The main activities at the TIGO VLBI station during 2011 have been the successful observation of

121 VLBI sessions enabling post-earthquake monitoring, the development of a VLBI control software

for smartphones, encoder replacement, and beamsize analysis measurements.

1. General Information

The operation of TIGO is based on an agreement between the Republic of Chile and the Federal

Republic of Germany. The following three institutions are responsible for the actual activities:

Universidad de Concepci ́on (UdeC, Chile), Instituto Geogr ́afico Militar (Chile), and Bundesamt

f ̈ur Kartographie und Geod ̈asie (BKG, Germany). TIGO is located on a tract of land of UdeC

(73.025◦W, 36.843◦S) in Concepci ́on, Chile. Due to financial problems of UdeC, the TIGO project

was threatened with termination by the end of 2011. A temporary financial aid from BKG allows

for the continued operation in 2012.

2. Component Description

The IVS Network Station TIGOCONC constitutes the VLBI part of the Geodetic Observatory

TIGO, which was designed as a fundamental station for geodesy. Hence, the VLBI radio telescope

is co-located with an SLR telescope (ILRS site), a GPS/Glonass receiver (IGS site), and other

instruments such as a seismometer, a superconducting gravimeter, and an absolute gravity meter.

The atomic clock ensemble of TIGO consists of three hydrogen masers, three cesium clocks, and

four GPS time receivers realizing the Chilean contribution to the Universal Time scale (Circular T,

BIPM). The technical parameters of the TIGO radio telescope published in [1] have not changed.

3. Staff

The 2011 VLBI staff consisted of four persons (see Table 1). At the beginning of 2011, three

Table 1. TIGO VLBI staff in 2011. Email addresses are firstname.lastname@tigo.cl for individuals and

vlbistaff@tigo.cl for all VLBI operators.

Staff Function

Hayo Hase Head

Cristian Herrera Informatic Engineer

Felipe Pedreros Telecommunications Engineer

Octavio Zapata Telecommunications Engineer

(from left) Herrera, Zapata, Pedreros, and Hase.

IVS 2011 Annual Report 107
TIGO Bundesamt f ̈ur Kartographie und Geod ̈asie - TIGO

former staff members (Sergio Sobarzo, Eric O ̃nate, and Pedro Zaror) left; their positions could not

be refilled due to financial problems at UdeC.

4. Current Status and Activities

During 2011 TIGO was scheduled to participate in 124 regular IVS sessions plus 15 additional

sessions of the CONT11 campaign. Twelve 24-hour experiments were carried out within the

TANAMI project [2]. Table 2 gives an overview of the participation of TIGOCONC in 2011. Out

of the 136 requested observation days, 121 could be observed successfully, reaching an efficiency of

89%. The main reason for the experiment failures was a technical problem in the vacuum system

of the dewar in April 2011. The replacement of the waveguide window and the vacuum valve

became necessary. The lack of these spare parts at TIGO and the delay for delivery caused the

loss of several experiments.

Table 2. TIGO’s IVS observation statistics for 2011.

Name R1xxx R4xxx OHIGxx T2 RD TANAMI CONT11 Total IVS

# of Exp. 48 48 5 2 6 12 15 136

Success 42 40 5 2 5 12 15 121

Failure 6 8 0 0 1 0 0 15

4.1. Post-earthquake Monitoring

Two years after the M8.8 earthquake, the TIGOCONC coordinates still show post-seismic

activity. Figure 1 depicts the coordinate time series for TIGOCONC (relative to the first session)

for the period 2002–2012; the insets display the post-earthquake coordinate behavior. The postseismic velocity vector points to the West, while the pre-seismic velocity vector pointed to the

North-East.

2002 2004 2006 2008 2010 2012

−2000

−1500

−1000

−500

0

500

1000

Year

North [mm]

North component

2010.5 2011 2011.5 2012

−550

−500

−450

2002 2004 2006 2008 2010 2012

−4000

−3000

−2000

−1000

0

1000

2000

Year

East [mm]

East component

2010.5 2011 2011.5 2012

−3050

−3000

−2950

−2900

−2850

−2800

2002 2004 2006 2008 2010 2012

−2000

−1500

−1000

−500

0

500

1000

Year

Height [mm]

Height component

2010.5 2011 2011.5 2012

−200

−100

0

100

Figure 1. TIGOCONC coordinate time series showing pre- and post-earthquake displacements in the North,

East and Up components. The biggest change is still active in the East component. (Time series courtesy

of Gerald Engelhardt, BKG.)

108 IVS 2011 Annual Report
Bundesamt f ̈ur Kartographie und Geod ̈asie - TIGO TIGO

4.2. Elevation Encoder Replacement

During 2011 the elevation servo control showed small jumps in the elevation axis of the telescope without causing an emergency stop. Several warning

messages about this behavior appeared

in the log files. Since the amplitude of

these periodical jumps were only on the

order of 0.01 degrees, the observations

were not affected by significant pointing errors. After ruling out many potential error sources through tests, the

problem was identified as missing bits

in the elevation encoder. Consequently,

Figure 2. Screen shots from the diagnosis computer of the

elevation encoder signal during tracking before (left) and after

(right) the encoder replacement.

the encoder was replaced by a spare which resolved the problem. Figure 2 presents screen shots

from the diagnosis computer showing the elevation encoder signal during tracking before and after

the exchange of the encoder.

4.3. Beam Pattern and Sidelobe Detection Measurements

In collaboration with undergraduate students of UdeC, work was done to characterize the beam

pattern of the 6-m telescope [3]. For the first part of the investigation two RF sources (2.3 GHz

−100 −80 −60 −40 −20 0 20 40 60 80

−2

−1

0

1

2

3

4

Amplitude [dB]

Azimuth [o]

X−Band Near Field beam pattern

−3 −2 −1 0 1 2 3

0

5

10

15

Amplitude [dB]

Azimuth [o]

X−Band Near Field main lobe beam

θ

3dB = 0.8o

−80 −60 −40 −20 0 20 40 60 80

0

5

10

15

20

Amplitude [dB]

Azimuth [o]

X−Band Far Field beam pattern

−3 −2 −1 0 1 2 3

0

5

10

15

20

25

Amplitude [dB]

Azimuth [o]

X−Band Far Field main lobe beam

θ

3dB = 0.48 Sidelobe o

Figure 3. Beam patterns in the near field (left) and far field (right) measured at 8.4 GHz.

and 8.4 GHz) were placed at a distance of 115 m from the telescope. Using a raster scan technique,

the variation of the received power was measured at the square law detectors in the two baseband

converters. Then the background noise was measured (with the RF sources off) and subtracted

from the data. Figure 3 (left) shows the main beam and a wide scan beam pattern, looking for

sidelobes in X band. However, the results obtained are not a true representation of the beam,

since the distance between the source and the receiver is in the near field of the telescope and very

likely affected by ground reflections. In the second part of the investigation, the RF source was

IVS 2011 Annual Report 109
TIGO Bundesamt f ̈ur Kartographie und Geod ̈asie - TIGO

located beyond the Rayleigh distance for X band (∼2 km). The geography allowed placement of

the RF source at an elevated height (20 m above the observatory level) at a distance of 2.84 km.

The direct line of sight crossed a valley therefore reducing ground reflections. The same previous

scanning and acquisition strategy was used. Figure 3 (right) shows the far field main beam and

the wide beam pattern for X band. The main beam was fitted with a Gaussian function. Results

show that the measured 3dB beamwidth θ3dB = 0.48◦is larger than the theoretical value for an

X-band 6-m aperture antenna (0.36◦). In addition a sidelobe near 1.5◦from the center has been

detected at a level of ∼15dB below the maximum.

4.4. Smartphone Monitor Application

Figure 4. (left) A screen shot of the smartphone software with Antenna Control Unit

and the current schedule. (right) Webcam

of the radio telescope in the interface of the

smartphone software for VLBI experiments.

Due to a shortage of operators it was necessary to control the running of VLBI sessions from elsewhere. For

the remote control and monitoring of VLBI operations

a software optimized for smartphones was developed

by Cristian Herrera. This is a new tool based on a

client-server architecture with a Web interface optimized for smartphone screens and cellphone networks.

The server uses variables of the Field System and its

station specific parameters stored in shared memory.

The client running on the smartphone by a Web interface analyzes and visualizes the current status of the

radio telescope, receiver, schedule, and recorder. In

addition, it allows the sending of commands remotely

to the Field System computer and displays the log

entries. The software also integrates a webcam interface. It was tested successfully in many sessions during

2011, and it can be adapted to other VLBI stations.

5. Future Plans

The VLBI activities in 2012 will focus on the execution of the IVS observation program,

upgrading from the Mark 5A recorder to Mark 5B+, and tests of e-VLBI transfer.

References

[1] Vandenberg, N. R.: International VLBI Service for Geodesy and Astrometry 2000 Annual Report,

NASA/TP–1999-209243, 1999.

[2] M. Kadler, R. Ojha, S. Tingay and J. Lovell, The TANAMI Program: Southern-Hemisphere VLBI

Monitoring of Relativistic Jets in Active Galaxies, American Astronomical Society, AAS Meeting #211,

#04.13; Bulletin of the American Astronomical Society, Vol. 39, p. 732.

[3] F. Pedreros, H. Pacheco, H. Hase, Beam pattern characterization of the 6 m TIGO telescope, Poster

presented at the 7th IVS General Meeting, Madrid, Spain, 2012.

110 IVS 2011 Annual Report
Geospatial Information Authority of Japan Tsukuba 32-m VLBI Station

Tsukuba 32-m VLBI Station

Ryoji Kawabata, Shinobu Kurihara, Kensuke Kokado, Yoshihiro Fukuzaki, Jiro Kuroda,

Misao Ishihara, Yasuko Mukai, Takashi Nishikawa

Abstract

The Tsukuba 32-m VLBI station is operated by the Geospatial Information Authority of Japan

(hereafter GSI). This report summarizes the activities of the Tsukuba 32-m VLBI station in 2011.

Over 200 sessions were observed with the Tsukuba 32-m and other GSI antennas in accordance

with the IVS Master Schedule of 2011. The Tsukuba 32-m could not participate in the IVS sessions

for nearly one month due to the 2011 earthquake that occured off the Pacific Coast of Tohoku and the

following aftershocks which occurred in March. Fortunately, the Tsukuba 32-m had no serious damage

and came back to IVS observing on April 4.

1. General Information

The Tsukuba 32-m VLBI station is located at GSI in Tsukuba Science City which is about

50 km to the northeast of the capital Tokyo (Figure 1). GSI has three regional stations besides

TSUKUB32: SINTOTU3, CHICHI10, and AIRA, which form the Geodetic VLBI network in Japan

covering the whole country (Figure 2).

GSI has carried out the domestic VLBI session series called “JADE (JApanese Dynamic Earth

observation by VLBI)”. The main purposes of the JADE series are to define the reference frame

of Japan and to monitor the plate motions for the advanced study of crustal deformations. Additionally, Mizusawa (VERAMZSW) and Ishigakijima (VERAISGK), which are part of the VERA

network of the National Astronomical Observatory of Japan (NAOJ), have also participated in the

JADE sessions.

Figure 1. Tsukuba 32-m VLBI station.

120 ̊

120 ̊

130 ̊

130 ̊

140 ̊

140 ̊

150 ̊

150 ̊

20 ̊ 20 ̊

30 ̊

30 ̊

40 ̊

40 ̊

50 ̊

50 ̊

CHICHI10

TSUKUB32

VERAISGK

VERAMZSW

AIRA

SINTOTU3

Figure 2. Geodetic VLBI network in Japan.

IVS 2011 Annual Report 111
Tsukuba 32-m VLBI Station Geospatial Information Authority of Japan

2. Component Description

The specifications of the Tsukuba 32-m antenna are summarized in Table 1.

Table 1. Tsukuba 32-m antenna specifications.

Owner and operating agency Geospatial Information Authority of Japan

Year of construction 1998

Radio telescope system Az-El

Antenna design Cassegrain

Diameter of main reflector 32 m

Azimuth range 10 – 710◦

Elevation range 5 – 88◦

Az/El drive velocity 3

◦/sec

Tsys at zenith (X/S) 50 K / 75 K

SEFD (X/S) 320 Jy / 360 Jy

RF range (X1) 7780 – 8280 MHz

RF range (X2) 8180 – 8680 MHz

RF range (X3) 8580 – 8980 MHz

RF range (S with BPF) 2215 – 2369 MHz

Recording terminal K5/VSSP32, ADS3000+ with DBBC

3. Staff

Table 2 lists the regular operating staff belonging to the GSI VLBI observation group. In

December 2011, Yoshihiro Fukuzaki re-joined our group in order to investigate and determine the

specifications of the new station for VLBI2010, which will be installed near Tsukuba as mentioned

in Section 5.

Routine operations were mainly performed under contract with Advanced Engineering Service

Co., Ltd. (AES). Daisuke Tanimoto resigned from our group at the end of March. To replace him,

Takashi Nishikawa became a new member in June.

Table 2. Staff list of the GSI VLBI group.

Name Position/Company Function

Misao ISHIHARA Director of Space Geodesy Div. Supervisor

Jiro KURODA Deputy Director of Space Geodesy Div. Management, Co-location

Yoshihiro FUKUZAKI Technical Officer Specification of VLBI2010 system

Shinobu KURIHARA Chief of Very Long Baseline Sec. Responsible official, IVS DB member

Kensuke KOKADO Chief of Baseline Analysis Sec. Correlation, Analysis, Data transfer

Ryoji KAWABATA Very Long Baseline Sec. VLBI operation, miscellaneous work

Kazuhiro TAKASHIMA Chief Researcher of Space Geodesy Research Div. Research

Yasuko MUKAI AES, Co., Ltd. Observation

Takashi NISHIKAWA AES, Co., Ltd. Observation and Correlation

Toshio NAKAJIMA I-JUSE System engineer

112 IVS 2011 Annual Report
Geospatial Information Authority of Japan Tsukuba 32-m VLBI Station

4. Current Status and Activities

4.1. Geodetic VLBI Observations

The regular sessions in the IVS Master Schedule carried out by GSI antennas are shown in

Table 3. TSUKUB32 participated in 88 domestic and international 24-hr VLBI sessions and 116

Intensive 1-hr sessions for dUT1 measurement in this year. SINTOTU3, CHICHI10, and AIRA

participated not only in domestic sessions but also in some international sessions.

Table 3. The number of regular sessions carried out by GSI antennas in 2011. The numbers in parentheses

show those of canceled sessions listed in the IVS Master Schedule.

Sessions TSUKUB32 SINTOTU3 CHICHI10 AIRA

IVS-R1 44(3) – – –

IVS-T2 6(1) – 6(1) 5(2)

APSG 2 2 2 0(2)

VLBA 6 – – –

IVS-R&D 6(1) – – –

CONT 15 – – –

JADE 8 7 4 3(2)

JAXA 1 – 1 1

IVS-INT2 79(1) – – –

IVS-INT3 37(1) – – –

Total 204(7) 9 13(1) 9(6)

4.2. The 2011 Earthquake Off the Pacific Coast of Tohoku

On March 11, a massive earthquake with a moment magnitude of 9.0 hit Japan, and we

experienced a severe shake in Tsukuba. The elevation drive gear of the Tsukuba 32-m shook

from side to side due to the earthquake. Nevertheless, the antenna and other observation devices

had no serious damage, though some computer displays fell from the desks in the building of the

observatory.

Many aftershocks following the main earthquake continued for nearly one month. Therefore we

decided to stop the observation of the Tsukuba 32-m until the beginning of April, since we were

afraid that the antenna might have serious damage caused by the aftershocks. The Tsukuba 32-m

returned to IVS observing on April 4. These sessions enabled us to determine the new position of

the Tsukuba 32-m, and we found large co- and post-seismic displacements of Tsukuba.

4.3. Ultra Rapid dUT1 Experiments in CONT11

The Tsukuba 32-m participated in the CONT11 campaign from September 15 to 29. We

transferred the data of the Tsukuba 32-m to the Tsukuba correlator via high-speed network. The

data of the Onsala Space Observatory in Sweden was also transferred via high-speed network

to the Tsukuba correlator and converted to the K5 data format in near real-time. Then both

data sets were correlated and analyzed automatically. This was the first success for us to obtain

continuous ultra rapid dUT1 values during 15 days, though the observation of the Tsukuba 32

meter was interrupted for nearly one day due to a typhoon which struck Tsukuba during the

CONT11 campaign. The details of the results are shown in the annual report of the Tsukuba

IVS 2011 Annual Report 113
Tsukuba 32-m VLBI Station Geospatial Information Authority of Japan

analysis center.

4.4. Co-location Survey of the Tsukuba 32-m

From June through July, we performed field surveys in order to measure the relative vector

of the reference points of the Tsukuba 32-m and TSKB, which is the IGS point in Tsukuba. We

needed 10 intermediate points in order to determine the relative vector of the Tsukuba 32-m and

TSKB, since the distance between the two points is approximately 300 m. We determined the

relative vector of two points with precisions of 3.0 mm horizontally and 0.9 mm vertically as a

preliminary result. Further analysis is in progress.

5. VLBI2010 Project in GSI

We obtained a budget for surveys of the RFI environment and the underground condition at

the candidate sites for a VLBI2010 station. We checked the radio interference in two candidate

sites and will survey the underground condition by March 2012.

Moreover we obtained a special budget for the installation of a VLBI2010 station, which includes antenna, feed, receiver, data recorder, hydrogen masers, and operation building. Our group

has investigated and discussed the specifications of the new system for VLBI2010 and prepared

some documents for the installation of the new station. Construction of the new station will be

completed by the end of March 2013.

114 IVS 2011 Annual Report
Xinjiang Astronomical Observatory, NAO–CAS Nanshan Station

Nanshan VLBI Station Report for 2011

Aili Yusup, Xiang Liu, Zhang Ming

Abstract

The Nanshan 25-meter radio telescope is operated by Xinjiang Astronomical Observatory. This

report describes the activities and the status of the Nanshan VLBI station as an IVS network station

in 2011.

1. Introduction

The Nanshan VLBI station is located 70 km south of Urumqi, the capital city of the Xinjiang

Uygur Autonomous Region of China. The station is affiliated with the Xinjiang Astronomical

Observatory of the National Astronomical Observatories of CAS. In 2011, we participated in a

total of 230 domestic and international VLBI sessions and contributed to IVS in geodetic VLBI

observations. The Nanshan VLBI station has participated in domestic VLBI experiments as one

of the VLBI ground stations tracking the Chinese Chang’E satellite. In addition, a GPS station,

as a part of the IGS network, is located near the VLBI telescope.

Figure 1. The Nanshan station, Xinjiang Astronomical Observatory, NAOC, CAS.

IVS 2011 Annual Report 115
Nanshan Station Xinjiang Astronomical Observatory, NAO–CAS

2. Telescope Status

2.1. Antenna

• Diameter: 25-meter

• Antenna type: Modified Cassegrain

• Seat-rack type: Azimuth-pitching ring

• Main surface precision: 0.40 mm (rms)

• Pointing precision: 15′′ (rms)

• Rolling range: Azimuth: ±270◦; Elevation: 5◦to 88◦

• Maximum rolling speed: Azimuth: 1.0◦/sec; Elevation: 0.5◦/sec

Figure 2. The 25-m, modified Cassegrain radio telescope of the Xinjiang Astronomical Observatory.

2.2. Receivers

The basic specifications of the receivers and the antenna sensitivities are given in Table 1. The

new 1.3 cm dual cooling receiver was installed in 2011.

116 IVS 2011 Annual Report
Xinjiang Astronomical Observatory, NAO–CAS Nanshan Station

Table 1. Specifications of receivers.

Parameters Freq. Range

(MHz)

1.3 cm dual Tsys= 45K DPFU=0.08 22000–24200

3.6 cm RCP Tsys= 60K DPFU=0.093 8100–8900

6 cm dual Tsys= 22K DPFU=0.11 4700–5110

13 cm RCP Tsys= 50K DPFU=0.096 2150–2450

18 cm dual Tsys= 24K DPFU=0.088 1400–1720

30 cm LCP Tsys=160K DPFU=0.06 800–1200

2.3. Recording Systems

The recording systems available at the Nanshan VLBI station are Mark 5B, Mark IV, Mark

II, and K5. The performance of the observing system was improved in the report year. The Field

System has been upgraded to version 9.10.4, and it works well. The DBBC system, which was

built at Shanghai Observatory (SHAO), was installed at Urumqi for domestic VLBI observations

with the Mark 5B recorder. The traditional BBC system is still being used for international VLBI

observations together with the Mark 5B recorder.

2.4. Time and Frequency System

There are three H-masers at the Nanshan Station: the MHM2010 imported from Symmetricom

company of the U. S. plus the No. 13 and No. 90 H-masers made in Shanghai. The time and

frequency comparison system operates continuously.

3. IVS Observations in 2011

Seven IVS sessions were scheduled for the Nanshan VLBI station in 2011. We participated in

all seven of these sessions. The details are listed in Table 2.

Table 2. IVS sessions scheduled for the Nanshan VLBI station in 2011.

Experiment Date Remarks (problems)

T2075 03.22 Observed

T2076 05.05 Observed, no problems

APSG28 07.28 Observed, no problems

APSG29 08.17 Observed, no problems

T2077 08.23 Observed, began 22:17 (UT)

T2078 10.11 Observed, no problems

T2079 11.28 Observed, no problems

IVS 2011 Annual Report 117
Nanshan Station Xinjiang Astronomical Observatory, NAO–CAS

4. Personnel

The main staff of the Nanshan VLBI station is compiled in Table 3.

Table 3. The main staff of the Nanshan VLBI station.

Name Position Working area e-mail

Na Wang Professor Station chief na.wang@uao.ac.cn

Aili Yusup Professor Chief engineer aliyu@uao.ac.cn

Xiang Liu Professor VLBI friend liux@uao.ac.cn

Maozheng Chen Senior engineer Receiver mzchen@uao.ac.cn

Ming Zhang Scientist Astronomy zhangming@uao.ac.cn

Wenjun Yang Engineer Terminal yangwj@uao.ac.cn

Shiqiang Wang Engineer Antenna Wangshq@uao.ac.cn

Hua Zhang Engineer Terminal, Time and Freq. zhangh@uao.ac.cn

Guanghui Li Engineer Network, Computer ligh@uao.ac.cn

Jun Ma Engineer Receiver majun@uao.ac.cn

Chenyu Chen Engineer Antenna chency@uao.ac.cn

Jun Nie Scientist Network, Computer niejun@uao.ac.cn

Mingshuai Li Engineer Time and Freq. limingsh@uao.ac.cn

118 IVS 2011 Annual Report
Institute for Radio Astronomy and Space Research, Auckland University of Technology Warkworth Observatory

Warkworth 12-m VLBI Station: WARK12M

Stuart Weston, Hiroshi Takiguchi, Tim Natusch, Sergei Gulyaev

Abstract

The Warkworth 12-m Radio Telescope is operated by the Institute for Radio Astronomy and Space

Research (IRASR) at AUT University, Auckland, New Zealand. This report briefly reviews the characteristics of the 12-m VLBI station. We report on a number of technical developments; integration of the

station DBBC with the Field System pointing algorithm, installation of a MET4 weather sensor and

an experimental phase calibration system. We discuss work being done to improve the determination

of ocean tide loading effects for the site and report on efforts to develop the capability to participate

in EOP experiments.

Figure 1. Warkworth 12-m (left) and Warkworth 30-m (right) antennas at the AUT’s Warkworth Radio

Astronomical Observatory. Photo: Sergei Gulyaev.

1. Station Equipment and Characteristics

The WARK12M radio telescope is located some 60 km north of the city of Auckland, near the

township of Warkworth (Figure 1) [1]. Specifications of the Warkworth 12-m antenna are provided

in Table 1. The radio telescope is equipped with an S/X dual-band dual-circular polarization feed.

Backend data digitizing is handled by a digital base band converter (DBBC) developed by the

Italian Institute of Radio Astronomy. The station frequency standard is a Symmetricom Active

Hydrogen Maser MHM-2010 (75001-114). Mark 5B+ and Mark 5C data recorders are used for

data storage and streaming of recorded data off site by computer network. The radio telescope

is directly connected to the regional network KAREN (Kiwi Advanced Research and Education

Network) via a 1 Gbps fiber link to the site [2].

2. Technical Developments

2.1. DBBC Integration with Field System

Software has been written that allows the Field System pointing routines (fivept, onoff, and

acquire) to access power measurements from the DBBC. The TCP socket interface to the DBBC

IVS 2011 Annual Report 119
Warkworth Observatory Institute for Radio Astronomy and Space Research, Auckland University of Technology

Table 1. Specifications of the Warkworth 12-m antenna.

Antenna type Dual-shaped Cassegrain

Manufacturer Cobham/Patriot, USA

Main dish Diam. 12.1 m

Secondary refl. Diam. 1.8 m

Focal length 4.538 m

Surface accuracy 0.35 mm

Pointing accuracy 18′′

Frequency range 1.4—43 GHz

Mount alt-azimuth

Azimuth axis range 90◦ ± 270◦

Elevation axis range 4.5

◦

to 88◦

Azimuth axis max speed 5◦/s

Elevation axis max speed 1◦/s

Main dish F/D ratio: 0.375

control program is used for this inter-device communication. With this new capability we have

been able to dramatically improve the pointing of Wark12M and finally obtain reasonable results

in X band. Further work in this area is planned that will result in the determination of SEFD,

Tsys, and Gain curves for the telescope.

2.2. MET4 Meteorological Sensor

Properly calibrated data on local atmospheric conditions is now available following the installation of a MET4 sensor at the telescope site. At present the MET4 directly connects to the station

Field System computer via an RS 232 physical interface. With optimization of the measurements

in mind an RS 485 interface is currently being investigated that would allow the sensor to be

positioned in closer proximity to the antenna and further away from the influence of buildings and

other structures. Data from the MET4 is continuously monitored and automatically written into

the Field System log for IVS experiments. It is anticipated that this data will be used to improve

the compensation for atmospheric effects at the station.

2.3. E-transfer

We have made extensive use of our connection via KAREN (Kiwi Academic Research Education

Network) to international research networks for data transfers to correlators. In the last year only

one diskpack, bound for Haystack, was physically shipped. Considerable savings on shipping costs

have been realized as a result of this capability. We have used Tsunami, gridFTP, and UDT

protocols as appropriate for the requirements of the correlator site to which we are sending data

[3, 4].

120 IVS 2011 Annual Report
Institute for Radio Astronomy and Space Research, Auckland University of Technology Warkworth Observatory

2.4. Experimental Phase Calibration System

Figure 2. Experimental phase

calibration system.

By kind offer from the National Institute of Information and

Communications Technology, Kashima Space Research Center, we

installed an experimental phase calibration system which was assembled by NICT on the 12-m antenna. The unit is fed a 5 MHz

signal from the station Maser, and its output is coupled into the

antenna feed by 30 dB loop couplers located immediately prior to

the LNA in both S and X band paths (Figure 2).

After considerable engineering effort it has been possible to adjust the phase calibration signal level observed at the backend of

the receivers to suitable levels. Phase calibration signals have been

detected in both S and X band channels using K5 software [5].

We have carried out fringe tests on the WARK12M-KASHIM11 baseline several times, finally

obtaining fringes and succeeding with bandwidth synthesis and analysis of the data (Figure 3).

∆τ

S band X band 

2bit 16MHz sampling, Source: 3C454.3 

2269.99MHz 8214.99MHz 

∆τ

∆τ ∆τ

. . 

Warkworth 12m Kashima 11m 

Figure 3. Warkworth 12-m (left) and Kashima 11-m (right) baseline. The fringes of this baseline for both

S and X band are presented.

2.5. Improving the Determination of Ocean Tide Loading Effects

We are preparing appropriate models for our station to use in geodetic analysis. Firstly we

checked the ocean tide loading effects and determined that the coastline data used by the Ocean

IVS 2011 Annual Report 121
Warkworth Observatory Institute for Radio Astronomy and Space Research, Auckland University of Technology

Tide Loading Provider [6] is not sufficiently accurate for our station. Therefore, we have constructed a more accurate coastline model from SRTM (the Shuttle Radar Topography Mission) [7]

data sets. We calculated the site-dependent tidal coefficients of the 11 main tides by using GOTIC2

software [8] with this new coastline data. To compare the result we obtained the standard tidal

coefficients from the Ocean Tidal Loading provider. The differences of the ocean tidal loading

displacement at Warkworth calculated from both site-dependent tidal coefficients were about ±1

mm in the horizontal components and ±2 mm in the vertical component, respectively (Figure 4).

These differences are large compared with our aim of 1 mm accuracy for baseline measurements.

As a next step we are going to apply this result to geodetic analysis and evaluate the effect.

-40

-30

-20

-10

 0

 10

 20

 30

 40

2011/01 2011/02 2011/03 2011/04

Onsala

GOTIC2

-2

-1

 0

 1

 2

2011/01 2011/02 2011/03 2011/04

Vertical Displacement Difference 

mm mm 

Figure 4. The ocean tidal loading displacement (vertical) at Warkworth in millimeters (left) and the

difference between two OTL models (right).

References

[1] Takiguchi, H., S. Gulyaev, T. Natusch, S. Weston, and L. Woodburn, Towards Synergy of VLBI and

GNSS Geodetic Techniques in Geologically Dynamic New Zealand, Advances in Geosciences, 2012.

(in press)

[2] Weston, S., Natusch, T., Gulyaev, S., Radio Astronomy and e-VLBI using KAREN. In Proceedings of

the 17th Electronics New Zealand Conference, 2010. Preprint arXiv:1011.0227.

[3] Wagner, J., Tsunami UDP Protocol. Available online: http://tsunami-udp.sourceforge.net

[4] Gu, Y., UDT: A High Performance Data Transport Protocol (Unpublished doctoral dissertation).

University of Illinois, Chicago, USA, 2005. See also http://udt.sourceforge.net/doc/udt-2009.ppt

[5] Kondo. T., Y. Koyama, R. Ichikawa, M. Sekido, E. Kawai, and M. Kimura, Development of the

K5/VSSP System, J. Geodetic Soc. Japan, 54(4), 233-248, 2008.

[6] http://froste.oso.chalmers.se/loading/index.html

[7] Farr, T. G., et al., The Shuttle Radar Topography Mission, Rev. Geophys., 45, RG2004,

doi:10.1029/2005RG000183, 2007.

[8] Matsumoto, K., T. Sato, T. Takanezawa, and M. Ooe, GOTIC2: A Program for Computation of

Oceanic Tidal Loading Effect, J. Geod. Soc. Japan, 47, 243-248, 2001.

122 IVS 2011 Annual Report
MIT Haystack Observatory Westford Antenna

Westford Antenna

Mike Poirier

Abstract

Technical information is provided about the antenna and VLBI equipment at the Westford site of

the Haystack Observatory and about changes to the systems since the IVS 2010 Annual Report.

1. Westford Antenna at Haystack Observatory

Since 1981 the Westford antenna has been one of the primary geodetic VLBI sites in the world.

Located ∼70 km northwest of Boston, Massachusetts, the antenna is part of the MIT Haystack

Observatory complex.

Figure 1. The radome of the Westford antenna.

Table 1. Location and addresses of the Westford antenna.

Longitude 71.49

◦ W

Latitude 42.61

◦ N

Height above m.s.l. 116 m

MIT Haystack Observatory

Off Route 40

Westford, MA 01886-1299 U.S.A.

http://www.haystack.mit.edu

The Westford antenna was constructed in 1961 as part of the Lincoln Laboratory Project West

Ford that demonstrated the feasibility of long-distance communication by bouncing radio signals

off a spacecraft-deployed belt of copper dipoles at an altitude of 3600 km. In 1981 the antenna was

converted to geodetic use as one of the first two VLBI stations of the National Geodetic Survey

Project POLARIS. Westford has continued to perform geodetic VLBI observations on a regular

IVS 2011 Annual Report 123
Westford Antenna MIT Haystack Observatory

basis since 1981. Westford has also served as a test bed in the development of new equipment and

techniques now employed in geodetic VLBI worldwide. Funding for geodetic VLBI at Westford is

provided by the NASA Space Geodesy Program.

2. Technical Parameters of the Westford Antenna and Equipment

The technical parameters of the Westford antenna, which is shown in Figure 2, are summarized

in Table 2.

Figure 2. Wide-angle view of the Westford antenna inside the radome. The VLBI S/X receiver is located at

the prime focus. The subreflector in front of the receiver is installed when observing with the TAL receiver

(see Section 4), which is located at the Cassegrain focus.

The antenna is enclosed in a 28-meter diameter air-inflated radome made of 1.2 mm thick

Teflon-coated fiberglass—see Figure 1. When the radome is wet, system temperatures increase by

10–20 K at X-band and by a smaller amount at S-band. The major components of the VLBI data

acquisition system are a Mark IV electronics rack, a Mark 5B recording system, and a Pentiumclass PC running PC Field System version 9.10.2. The primary frequency and time standard is

the NR-4 hydrogen maser. A CNS Clock GPS receiver system provides a 1 pps reference clock to

which the maser 1 pps is compared.

Westford also hosts the WES2 GPS site of the IGS network. A Dorne-Margolin chokering

antenna is located on top of a tower ∼60 meters from the VLBI antenna, and a LEICA GRX1200

Reference Station receiver acquires the GPS data.

124 IVS 2011 Annual Report
MIT Haystack Observatory Westford Antenna

Table 2. Technical parameters of the Westford antenna for geodetic VLBI.

Parameter Westford

primary reflector shape symmetric paraboloid

primary reflector diameter 18.3 meters

primary reflector material aluminum honeycomb

S/X feed location primary focus

focal length 5.5 meters

antenna mount elevation over azimuth

antenna drives electric (DC) motors

azimuth range 90◦ − 470◦

elevation range 4

◦ − 87◦

azimuth slew speed 3

◦

s

−1

elevation slew speed 2

◦

s

−1

X-band system S-band system

frequency range 8180-8980 MHz 2210-2450 MHz

Tsys at zenith 50–55 K 70–75 K

aperture efficiency 0.40 0.55

SEFD at zenith 1400 Jy 1400 Jy

3. Westford Staff

The personnel associated with the geodetic VLBI program at Westford and their primary

responsibilities are:

Chris Beaudoin broadband development

Joe Carter antenna controls

Brian Corey VLBI technical support

Kevin Dudevoir pointing system software

Dave Fields technician, observer

Glenn Millson observer

Arthur Niell principal investigator

Michael Poirier site manager

Alan Whitney site director

4. Standard Operations

From January 1, 2011 through December 31, 2011, Westford participated in 46 standard 24-

hour sessions and in the 15 day CONT geodetic session. Westford regularly participated in IVS-R1,

IVS-R&D, and RD-VLBA observations.

Use of the Westford antenna is shared with the Terrestrial Air Link (TAL) Program operated

by the MIT Lincoln Laboratory. In this project Westford serves as the receiving end on a 42-km

long terrestrial air link designed to study atmospheric effects on the propagation of wideband

communications signals at 20 GHz.

IVS 2011 Annual Report 125
Westford Antenna MIT Haystack Observatory

5. Research and Development

In its role as a test bed for VLBI developments, the Westford antenna was implemented several

times during the year with the VLBI2010 broadband feed assembly and used successfully as the

second element of the interferometer with the GGAO 12-m VLBI2010 system.

The antenna was also equipped with the Mark 6 prototype data recorder for a demonstration

of 16 Gbps recording capability. The equipment has been left in place for additional Mark 6 testing

and development.

6. Outlook

Westford is expected to participate in 61 24-hour sessions in 2012. We also plan to have the

flexibility to support occasional fringe tests, e-VLBI experiments, and the continuing VLBI2010

broadband development program.

126 IVS 2011 Annual Report
FESG TU Munich, BKG Geodetic Observatory Wettzell - 20-m radio telescope and Twin telescope

Geodetic Observatory Wettzell - 20-m Radio Telescope and Twin

Telescope

Alexander Neidhardt, Gerhard Kronschnabl, Raimund Schatz

Abstract

In 2011 the 20-m radio telescope at the Geodetic Observatory Wettzell, Germany contributed again

very successfully to the IVS observing program. Technical changes, developments, improvements, and

upgrades have been made to increase the reliability of the entire VLBI observing system. In parallel

the mechanical assembly of the new Twin radio telescope (TTW) was finished while the HF-receiving

system was constructed.

1. General Information

The 20-m radio telescope in Wettzell (RTW) is an essential component of the Geodetic Observatory Wettzell (GOW) and is jointly operated by Bundesamt f ̈ur Kartographie und Geod ̈asie (BKG)

and Forschungseinrichtung Satellitengeod ̈asie (FESG) of the Technische Universit ̈at M ̈unchen

(Technical University Munich). In addition to the RTW, GOW also operates an ILRS laser ranging system, several IGS GPS permanent stations, a large laser gyroscope G (ringlaser), and the

associated local techniques such as time and frequency, meteorology and super conducting gravity

meter. Currently also the first fully VLBI2010-compliant Twin telescope is being built on location.

It should extend the observation possibilities according to the new technical suggestions of the IVS

Working Group 3 (WG3).

Within the responsibility of the GOW are also the TIGO system in Concepci ́on, Chile, operated

mainly together with the Universidad de Concepci ́on (see separate report about TIGO), and the

German Antarctic Receiving Station (GARS) O’Higgins in Antarctica, operated together with

the German Space Center (DLR) and the Institute for Antarctic Research Chile (INACH) (see

separate report about O’Higgins).

2. Staff

The staff of the GOW consists in total of 34 members (excluding students) for operations,

maintenance, repair work, and the improvement and development of the systems. The staff operating RTW are in Table 1. One additional engineer is on a position which is funded by the

“Novel EXploration Pushing Robust e-VLBI Services” (NEXPReS) project in cooperation with

the Max-Planck-Institute for Radioastronomy (MPIfR), Bonn. It was also possible to support the

student operators to work within development projects and internships.

3. Observations in 2011

The 20-m RTW has supported the geodetic VLBI activities of the IVS and partly those of

other partners, such as the EVN, for over 25 years. All successfully observed sessions in the year

2011 are summarized in Table 2. After the repair of the bearings the RTW once again observes

in all sessions and, except for some problems with the gears and the servo system, which are also

dated, the telescope is in a very good and stable state. The main priority for operations was

IVS 2011 Annual Report 127
Geodetic Observatory Wettzell - 20-m radio telescope and Twin telescope FESG TU Munich, BKG

Table 1. Staff members of RTW.

Name Affiliation Function Mainly working for

Johannes Ihde BKG interim head of the GOW (until February 2011) GOW

Ullrich Schreiber BKG head of the GOW (since March 2011) GOW

Alexander Neidhardt FESG head of the RTW group and VLBI station chief RTW, TTW (partly O’Higgins,

laser ranging)

Erhard Bauernfeind FESG mechanical engineer RTW

Ewald Bielmeier FESG technician RTW

Gerhard Kronschnabl BKG electronic engineer RTW, TTW (partly TIGO

and O’Higgins)

Christian Pl ̈otz BKG electronic engineer O’Higgins, RTW

Raimund Schatz FESG software engineer RTW

Walter Schwarz BKG electronic engineer RTW (partly O’Higgins

and WVR)

Reinhard Zeitlh ̈ofler FESG electronic engineer RTW

Martin Ettl FESG/MPIfR IT and computer scientist NEXPReS

Thomas Guggeis FESG/BKG student (January to September 2011) RTW, project work, WLRS

Yvonne Klingl FESG/BKG student (May to December 2011) WLRS, RTW, project work

Daniel Prexler FESG/BKG student (May to December 2011) WLRS, RTW, project work

Martin Riederer FESG/BKG student (January to March 2011) RTW, project work

Johannes Vogl FESG/BKG student (January to December 2011) RTW, project work, WLRS

the participation in all daily one-hour INTENSIVE sessions (INT) in order to determine UT1-

UTC. For these sessions the complete data transfer is done electronically (e-transfer). RTW now

routinely uses the increased Internet connection capacities of 1 Gbit/sec for the e-transfers to

Bonn, Tsukuba, and Haystack. Following the implementation of a Field System extension for

remote control, weekend INTENSIVEs were partly done in the new observation modes of remote

attendance, remote control from students at the laser ranging system (WLRS), or completely

unattended.

In addition to the standard sessions, RTW also observed fifteen CONT11 sessions of the IVS

within a network of thirteen stations in September 2011. During the CONT11 campaign all stations

ran observations continuously over a period of fifteen days. Within these days the RTW had only

dropouts of a few minutes. The data were saved on Mark 5A (standard) and as backup on Mark

5B+ or EVN PC hard drive. In addition, the RTW staff also operated the TIGO VLBI telescope

remotely during the Chilean night shifts, using the e-RemoteCtrl software from Wettzell. Other

special observations were done for Digital Baseband Converter (DBBC) tests and for spacecraft

tracking. Within these additional one-hour observations the ESA Venus Express and Mars express

spacecraft were observed at X-band with the Wettzell radio telescope using a framework of the

assessment study for possible contributions in the European VLBI network to the upcoming ESA

deep space missions.

4. Technical Improvements and Maintenance

During the report period usual maintenance work had to be done. Regularly, tasks and maintenance days (obtaining replacements for the hardware, 8-pack repair, gear maintenance, Field

System updates, cryo system maintenance, servo replacements, and improvements by using EVNPCs for e-VLBI issues) were scheduled for this work. Especially the exchange of motors in elevation

and azimuth after reaching their lifetime must be mentioned. Another very important work was to

128 IVS 2011 Annual Report
FESG TU Munich, BKG Geodetic Observatory Wettzell - 20-m radio telescope and Twin telescope

Table 2. RTW observations in 2011.

program number of program number of

24h-sessions 1h-sessions

IVS R1 50 INT1(Kokee-RTW) 229

IVS R4 49 INT2/K(Tsukuba-RTW) 153

IVS T2 7 INT3/K(Tsukuba-RTW-NyAl) 40

IVS R&D 7 total (in hours) 422

RDV/VLBA 5

EUROPE 6 special program in hours

CONT11 15 VENUS Express /

total 139 MARS Express 9

total (in hours) 3336 total (in hours) 18

derust, prime, and paint the metal parts of the cabin, the feed cone, and the legs of the subreflector

support. The work was done during observation gaps and the final cleanup of the large repair of

the bearings. After several problems with the servo system, it became necessary to work on some

relays and to clean up the gear motor and the break adapter. The components of the servo system

are dated and not available on the market anymore. Similar changes had to be done to the Mark

IV data acquisition rack.

A first change from Mark 5A to Mark 5B and Mark 5B+ was possible, by changing the Mark

IV formatter to support the new VSI-interface. Within a student project, a Mark IV VSI version

of the formatter was programmed, developing VHDL for a Xilinx-FPGA using the Xilinx-Software

“ISE”. The developed software runs on a specially designed VSI-formatter board. It was tested

during integration tests and CONT11. Parallel to this development all Mark 5 systems were

upgraded and updated.

The usage of the EVN-PC for e-transfer was continuously extended. In addition, the installation

and test usage of the new Digital Baseband Converters (DBBC) were advanced. They should

replace the existing analog video converters and formatter of the Mark IV-rack. They should

provide the basis for a higher data rate with better data quality in a fully digital way, in particular

for the VLBI2010 system. Wettzell is one of the main test sites for the DBBC. In cooperation with

the developers at HATLab, MPIfR and INAF, new DBBC components were tested, calibrated,

and adjusted. Several test data were correlated at the Bonn Correlator to check the functionality

and quality. The development is still under way.

The remote control software “e-RemoteCtrl” was also extended mainly by the TUM. In close

cooperation with the developers of the NASA Field System and with other test sites, new features

were established. Some sites (e.g., the new AuScope network in Australia) already use the software

routinely. During CONT11 the software was used to control the TIGO VLBI telescope remotely

by the night shifts. The development is funded in Task 3 of Work Package 5 of the NEXPReS

Project and is performed in cooperation with MPIfR. An appropriate authentication, a dedicated

role management for different user types, different remote access states to shared telescopes, system

monitoring, and sophisticated graphical user interfaces are under development.

5. The TWIN Radio Telescope Wettzell (TTW)

The Twin Telescope Wettzell project is Wettzell’s realization of a fully VLBI2010-compliant

radio telescope. With the design and construction being the main focus, the buildings could be

IVS 2011 Annual Report 129
Geodetic Observatory Wettzell - 20-m radio telescope and Twin telescope FESG TU Munich, BKG

Figure 1. The telescopes of Wettzell: the 20-m radio telescope during CONT11 and the new TWIN radio

Telescope Wettzell (TTW).

finished in 2011. Therefore, at the beginning of 2011 a lot of factory approvals were made (e.g., of

the sub-reflector and servo systems). Also the construction of the control building was completed

(coordinated with the Staatliche Bauamt Regensburg).

In detail the following items were performed:

• A photogrammetric survey of the reflector surface was made in June. It included the adjustment of the sub-reflector at an elevation of 58 degrees. The adjusting optimizes the

wavelength error.

• The TWIN is now in the geodetic survey of the observatory.

• All mechanical installations and assemblies were finished successfully in August. Therefore

the telescopes are now fully maneuverable.

• An optimization of the servo system was started according to the local conditions.

• The construction of the multiband coaxial horn for S-, X-, and Ka-band and the corresponding dewar is in the final stage at the companies Mirad (feed) and Callisto (dewar). The

second feed of the Eleven feed type for 2 to 14 GHz is under development at the company

Omnisys.

• The computer and server room was populated with water cooled racks.

• The development of the new receivers is in progress in Wettzell. Several student projects to

implement single parts of them were carried out very successfully.

6. Plans for 2012

For 2012, dedicated plans are:

• Regular usage of the digital baseband converters (DBBC)

• Continue NEXPReS

• Develop the front end parts of the Twin telescopes

• Finalize one of the Twin telescopes

130 IVS 2011 Annual Report
Instituto Geogr ́afico Nacional Instituto Geogr ́afico Nacional – Yebes

Instituto Geogr ́afico Nacional of Spain

Francisco Colomer, Susana Garc ́ıa–Espada, Jes ́us G ́omez–Gonz ́alez,

Jos ́e Antonio L ́opez–Fern ́andez, Pablo de Vicente

Abstract

This report updates the description of the space geodesy facilities of the Spanish National Geographic Institute (IGN). The current 40-m radio telescope at Yebes, a network station for IVS, has

performed geodetic VLBI observations regularly since September 2008. In addition to this, the project

to establish an Atlantic Network of Geodynamical and Space Stations (RAEGE) is progressing with

the construction of the first antenna, to be erected in Yebes in 2012.

1. General Information: the IGN Facilities at Yebes

Yebes Observatory, a department of the Instituto Geogr ́afico Nacional (IGN, Ministerio de

Fomento), holds two radio telescopes: the new 40-m which is a network station for IVS, and the

old 14-m used between 1995 and 2003. Yebes Observatory is also the reference station for the

Spanish GNSS network and holds permanent facilities for gravimetry. The RAEGE project will

provide a new VLBI2010-type antenna in Yebes as soon as 2012. An SLR system in a new control

building will also be built in the near future.

2. IGN Staff Working on VLBI Projects

Table 1 lists the IGN staff who are involved in space geodesy studies and operations. The

VLBI activities are also supported by other staff such as receiver engineers, computer managers,

secretaries, and students. In 2011, the process of hiring dedicated telescope operators was finally concluded, increasing the operational efficiency of the instrument also for its participation in

geodetic VLBI campaigns.

Table 1. Staff in the IGN VLBI group (e-mail: vlbitech@oan.es).

Name Background Role Address∗

Francisco Colomer Astronomer VLBI Project coordinator IGN

Susana Garc ́ıa–Espada Engineer geoVLBI expert CAY

Jes ́us G ́omez–Gonz ́alez Astronomer Deputy Director for IGN

Astronomy, Geodesy and Geophysics

Jos ́e Antonio L ́opez–Fdez Engineer Yebes site manager CAY

Javier L ́opez–Ramasco Geodesist Geodesist CAY

Alvaro Santamar ́ıa Geodesist Geodesist CAY

Pablo de Vicente Astronomer VLBI technical coordinator CAY

Addresses:

IGN: Instituto Geogr ́afico Nacional. Calle General Iba ̃nez de Ibero 3, E–28003 Madrid, Spain.

CAY: Centro Astron ́omico de Yebes. Apartado 148, E–19080 Guadalajara, Spain.

IVS 2011 Annual Report 131
Instituto Geogr ́afico Nacional – Yebes Instituto Geogr ́afico Nacional

Figure 1. Geometric approach to determine the location of the Invariant Reference Point of the 40-m radio

telescope at Yebes observatory.

3. Status of Geodetic VLBI Activities at IGN

The 40-m radio telescope has participated in 21 sessions of the EURO, R4, and T2 series as

well as in the whole CONT11 campaign on September 15-30, 2011.

The studies of the tropospheric effect caused by neutral atmosphere continues in cooperation

with the geodesy group at Onsala Space Observatory in Sweden, by using the HIRLAM 3D-VAR

numerical weather prediction model; the slant delay caused by the neutral atmosphere is calculated

via ray-tracing (see Garc ́ıa–Espada, Haas and Colomer 2011).

A simulation has been produced to assess to what extent an automatic system based on robotic

total stations could be properly configured to continuously monitor the Invariant Reference Point

of the 40-m radio telescope at the Yebes observatory, using a geometric model that improves the

classical 3D circle fitting methods. This approach is able not only to accurately estimate the IRP

coordinates and other parameters (e.g., eccentricity and non-orthogonality of the axes), but also

it allows monitoring of its temporal behavior, thus providing fundamental information about the

radio telescope deformation. Indeed, one robotic total station would allow reliable estimation of

the IRP coordinates in 24h observation batches, provided that the precision of the observed target

coordinates is better than 1 cm (see Santamar ́ıa-G ́omez and Garc ́ıa–Espada 2011).

A new high-speed Internet connection has been built to connect Yebes to GEANT. Running at  ́

1 Gbps since April 2009, the new dark fiber will allow data transfer of 10 Gbps starting in 2012.

Figure 2 shows the new gravimeter pavillion, which permanently holds an absolute gravimeter

and a GWR superconducting gravimeter installed in May 2010.

132 IVS 2011 Annual Report
Instituto Geogr ́afico Nacional Instituto Geogr ́afico Nacional – Yebes

Figure 2. The A10 absolute and GWR superconducting gravimeters installed in a dedicated building in

Yebes. (Figure courtesy of Carlos Albo Casta ̃no, IGN).

4. Project RAEGE

As mentioned in the previous report, IGN (together with the Portuguese colleagues in DSCIG)

is constructing a network of four new Fundamental Geodynamical and Space Stations in Spain

and Portugal (Azores Islands). The project, named RAEGE (after “Red Atl ́antica de Estaciones

Geodin ́amicas y Espaciales”), consists of the erection of one radio telescope of VLBI2010 class

(i.e., of 13.2-m diameter, having a high slew rate, and capable of operating in the 2-14 GHz

bands but also up to 90 GHz), a permanent GNSS receiver, and a gravimeter in Yebes, Tenerife

(Canary Islands), Santa Mar ́ıa and Flores (Azores Islands), and an SLR station in Yebes (see e.g.

G ́omez-Gonz ́alez et al. 2011).

The construction of three antennas, to be installed in Yebes, Azores (Santa Mar ́ıa), and Canary

Islands, and contracted to MT Mechatronics (Germany), has started (see Figure 3). The first

antenna will be erected in Yebes in 2012, shortly followed by the antenna in Santa Mar ́ıa.

Radio frequency interference (RFI) has been monitored at Yebes and the other chosen sites,

demonstrating that in the latter cases the spectrum in the bands of interest is very clean.

Meanwhile, preliminary studies, concerning the installation of a Satellite Laser Ranging system

in Yebes, have started (see Vaquero Jim ́enez and L ́opez Fern ́andez 2011).

IVS 2011 Annual Report 133
Instituto Geogr ́afico Nacional – Yebes Instituto Geogr ́afico Nacional

Figure 3. RAEGE telescopes under construction in Spain. Left: receiver cabins. Right: antenna counterweights.

References

[1] Garc ́ıa–Espada S., Haas R., Colomer F. “Application of ray-tracing through the high resolution numerical weather model HIRLAM for the analysis of European VLBI data”. In Procs. 20th European

VLBI working meeting for Geodesy and Astrometry (EVGA). Bonn (Germany), 2011.

[2] G ́omez-Gonz ́alez J., Assis M. C. S., Colomer F., J. A., L ́opez Fern ́andez J. A. “An

Atlantic Network of Geodynamical and Space Stations (Project RAEGE)”. In Procs.

European Geosciences Union General Assembly 2011. Vienna (Austria), 2011 (see

http://meetingorganizer.copernicus.org/EGU2011/EGU2011-8026.pdf).

[3] Santamar ́ıa-G ́omez A., Garc ́ıa–Espada S. “Simulating the estimation of the 40-m radio telescope Invariant Reference Point at the Yebes Observatory”. Informe T ́ecnico OAN 2011-9 (see

http://www1.oan.es/informes/archivos/IT-OAN-2011-9.pdf).

[4] Vaquero Jim ́enez B., L ́opez Fern ́andez J. A. “CYLAR Specifications (CDT Yebes Laser Ranging)”. Informe T ́ecnico OAN 2011-11 (see http://www1.oan.es/informes/archivos/IT-OAN-2011-11.pdf).

[5] de Vicente P., Garc ́ıa–Espada S. “Testing the VLBI system prior to the CONT11 campaign”. Informe

T ́ecnico OAN 2011-6 (see http://www1.oan.es/informes/archivos/IT-OAN-2011-6.pdf).

[6] de Vicente P., Bola ̃no R., Almendros C. “DBBC installation and tests at the 40-m radio telescope”.

Informe T ́ecnico OAN 2011-8 (see http://www1.oan.es/informes/archivos/IT-OAN-2011-8.pdf).

134 IVS 2011 Annual Report
Institute of Applied Astronomy of Russian Academy of Sciences Zelenchukskaya Station

Zelenchukskaya Radio Astronomical Observatory

Sergey Smolentsev, Andrei Dyakov

Abstract

This report summarizes information on recent activities at the Zelenchukskaya Radio Astronomical

Observatory in 2011. During the previous year a number of changes were carried out at the observatory

to improve some technical parameters and upgrade some units to required status. The report also

provides an overview of current geodetic VLBI activities and gives an outlook for the next year.

1. General Information

Zelenchukskaya Radio Astronomical Observatory (Figure 1) was founded by the Institute

of Applied Astronomy (IAA) as one of three stations of the Russian VLBI network QUASAR

[1]. The sponsoring organization of the project is the Russian Academy of Sciences (RAS).

The Zelenchukskaya Radio Astronomical Observatory is situated in Karachaevo-Cherkesskaya

Republic (the North Caucasus) about 70 km south of Cherkessk, near to the Zelenchukskaya

village. The geographic location of the observatory is shown on the IAA RAS Web site:

http://www.ipa.nw.ru/PAGE/rusipa.htm (Table 1). The basic instruments of the observatory

are a 32-m radio telescope equipped with special technical systems for VLBI observations,

GPS/GLONASS/Galileo receivers, and an SLR system installed in 2011.

Figure 1. Zelenchukskaya observatory.

2. Technical Staff

Andrei Dyakov — observatory chief,

Dmitry Dzuba — FS, pointing system control,

Anatoly Mishurinsky — front end and receiver support.

IVS 2011 Annual Report 135
Zelenchukskaya Station Institute of Applied Astronomy of Russian Academy of Sciences

Table 1. Zelenchukskaya Observatory location and address.

Longitude 41◦34

′

Latitude 43◦47

′

Zelenchukskaya Observatory

Karachaevo-Cherkesskaya Republic

369140, Russia

ipazel@mail.svkchr.ru

3. Technical and Scientific Information

Table 2. Technical parameters of the radio telescope.

Year of construction 2000

Mount AZEL

Azimuth range ±270◦(from south)

Elevation range from −5

◦

to 95◦

Maximum azimuth

- velocity 1.5

◦/s

- tracking velocity 1.5

′/s

- acceleration 0.2

◦/s2

Maximum elevation

- velocity 0.8

◦/s

- tracking velocity 1.0

′/s

- acceleration 0.2

◦/s2

Pointing accuracy better than 10′′

Configuration Cassegrain

(with asymmetrical subreflector)

Main reflector diameter 32 m

Subreflector diameter 4 m

Focal length 11.4 m

Main reflector shape quasi-paraboloid

Subreflector shape quasi-hyperboloid

Main reflector surface accuracy ± 0.5 mm

Frequency range 1.4–22 GHz

Axis offset −3.0 ± 1.5 mm

The electrical part of the gear and pointing system of the radio telescope was upgraded in 2008

— 2010. A new DAS R1002M designed at the IAA [2, 3] has been used in all kinds of VLBI

observational programs since October 2011. The DAS R1002M is suited to work with Mark 5B

and Mark 5B+ recording systems.

136 IVS 2011 Annual Report
Institute of Applied Astronomy of Russian Academy of Sciences Zelenchukskaya Station

4. Co-location of VLBI, GPS/GLONASS and SLR System

The Topcon GPS/GLONASS/Galileo receiver with meteo station WXT-510 was tested and

put into operation (Figure 2).

Figure 2. Topcon GPS/GLONASS/Galileo receiver at the Zelenchukskaya observatory.

The SLR system “Sazhen-TM” (Figure 3) was mounted in May 2011. The “Sazhen-TM” SLR

system was manufactured by Open Joint-stock Research-and-Production Corporation “Precision

Systems and Instruments”. The technical parameters of the system are presented in Table 3.

Figure 3. “Sazhen-TM” SLR system at Zelenchukskaya observatory.

IVS 2011 Annual Report 137
Zelenchukskaya Station Institute of Applied Astronomy of Russian Academy of Sciences

Table 3. Technical parameters of the SLR system “Sazhen-TM”.

Ranging distance, day 400-6000 km

Ranging distance, night 400-23000 km

Aperture 25 cm

Wavelength 532 nm

Beam divergence 12′′

Laser pulse frequency 300 Hz

Pulse energy 2.5 mJ

Mass 170 kg

Normal points precision 1 cm

Angular precision 1-2′′

5. Current Status and Activities

The Zelenchukskaya observatory participates in IVS and domestic VLBI observational programs. During 2011 Zelenchukskaya station participated in 49 diurnal IVS sessions — IVS-R1,

IVS-R4, IVS-T2, IVS-R&D, EURO, and CONT11.

Zelenchukskaya participated in 49 diurnal sessions in the frame of the domestic Ru-E program for determination of all Earth orientation parameters and in 55 one-hour Ru-U sessions for

obtaining Universal Time using e-VLBI data transfer.

6. Outlook

Our plans for the coming year are the following:

• To participate in IVS observations

• To carry out domestic observational programs for obtaining Universal Time with e-VLBI

data transfer and Earth orientation parameters once a week

• To carry out SLR observations of geodetic and navigation satellites

• To participate in EVN and RADIOASTRON observational sessions

• To continue geodetic monitoring of the antenna parameters.

References

[1] Finkelstein A., Ipatov A., Smolentsev S. The Network “Quasar” : 2008-2011 // “Measuring the future”,

Proc. of the Fifth IVS General Meeting, A. Finkelstein, D. Behrend (eds.), St. Petersburg, “Nauka”,

2008. pp. 39–46.

[2] Grenkov S. A., Nosov E. V., Fedotov L. V., Koltsov N. E. A Digital Radio Interferometric Signal

Conversion System // Instruments and Experimental Techniques, 2010. Vol. 53, No. 5. pp. 675–681.

[3] Nosov E. Next-Generation DAS for the Russian VLBI-Network. // 20th EVGA Meeting. MPIfR, Bonn.

2011. pp. 41–43.

138 IVS 2011 Annual Report
Operation Centers

Operation Centers

Institut f ̈ur Geod ̈asie und Geoinformation der Universit ̈at Bonn IGGB Operation Center

The Bonn Geodetic VLBI Operation Center

A. Nothnagel, A. M ̈uskens

Abstract

The IGGB Operation Center has continued to organize and schedule the IVS-T2, IVS-OHIG, IVSINT3, and EUROPE sessions.

1. Center Activities

The IGGB VLBI Operation Center is located at the Institute of Geodesy und Geoinformation

of the University of Bonn, Nussallee 17, D-53115 Bonn, Germany. It has been organizing and

scheduling VLBI observing sessions for more than twenty years. The observing series organized

and scheduled in 2011 are the same as in 2010.

• Measurement of Vertical Crustal Motion in Europe by VLBI (EUROPE)

In Europe, a series of special sessions has been scheduled for the determination of precise

station coordinates and for long term stability tests. This year, six sessions with Ny- ̊Alesund,

Onsala, Metsahovi, Svetloe, Zelenchukskaya, Badary, Effelsberg, Wettzell, Simeiz, Madrid

(DSS65A), Medicina, Matera, Noto and Yebes (YEBES40M) were scheduled employing the

frequency setup of 16 channels and 4 MHz bandwidth in fan-out mode (identical to the setup

of the IVS-T2 sessions).

• IVS-T2 series

This series has been observed roughly every second month (seven sessions in 2011) primarily

for maintenance and stabilization of the VLBI terrestrial reference frame as well as for Earth

rotation monitoring as a by-product. Each station of the global geodetic VLBI network is

planned to participate at least once per year in the T2 sessions. In view of the limitations in

station days, priority was given to stronger and more robust networks with many sites over

more observing sessions. Therefore, 12 to 15 stations have been scheduled in each session

requiring multiple passes on the IVS correlators. The scheduling of these sessions has to

take into account that a sufficient number of observations must be planned for each baseline

of these global networks. The recording frequency setup is 16 channels and 4 MHz channel

bandwidth.

• Southern Hemisphere and Antarctica Series (OHIG):

In February 2011, three sessions of the Southern Hemisphere and Antarctica Series with the

Antarctic stations Syowa (Japanese) and O’Higgins (German) plus Fortaleza, Hobart, Kokee,

and DSS45 have been organized. Furthermore, OHIGGINS was also included successfully

in the T2074 session. The (southern) winter O’Higgins burst was again canceled for various

reasons. The purpose of these sessions is the maintenance of the VLBI TRF and monitoring

of Earth rotation as a by-product. The recording frequency setup is 16 channels and 4 MHz

channel bandwidth. Due to the fact that Syowa is not able to deliver the recorded data for

nearly one year after the observations, the correlation and the generation of the databases

will be delayed considerably.

IVS 2011 Annual Report 141
IGGB Operation Center Institut f ̈ur Geod ̈asie und Geoinformation der Universit ̈at Bonn

• UT1 determination with near-real-time e-VLBI (INT3):

The so-called INT3 sessions included the telescopes of Ny- ̊Alesund, Tsukuba, and Wettzell

for weekly UT1 determinations with rapid processing time. Since August 2007 these sessions

have been scheduled to start every Monday morning at 7:00 a.m. UT.

The operations of the INT3 series is directly linked to data transmission and correlation

since the raw VLBI observation data of the three sites is directly transferred to the Bonn

Correlator by Internet connections to speed up delivery of the results. The transmission rate

is about 100 Mb/s for Ny- ̊Alesund (limited due to the use of a radio link for the first part

of the distance) and 400 Mb/s from Tsukuba and Wettzell. The correlation is solely carried

out with the new DiFX software correlator.

In 2011, 50 sessions were observed and transmitted successfully. 90% of the sessions were

correlated and the databases delivered within the first eight hours after the end of the observations. A further 5% were completed within 10 hours. The rest took between 10 and 24

hours due to difficulties with networking hardware.

2. Staff

Table 1. Personnel at IGGB Operation Center

Arno M ̈uskens +49-228-525264 mueskens@mpifr.de

Axel Nothnagel +49-228-733574 nothnagel@uni-bonn.de

142 IVS 2011 Annual Report
NASA Goddard Space Flight Center CORE Operation Center

CORE Operation Center Report

Cynthia C. Thomas, Daniel MacMillan

Abstract

This report gives a synopsis of the activities of the CORE Operation Center from January 2011 to

December 2011. The report forecasts activities planned for the year 2012.

1. Changes to the CORE Operation Center’s Program

The Earth orientation parameter goal of the IVS program is to attain precision at least as good

as 3.5 μs for UT1 and 100 μas for pole position.

The IVS program, which started in 2002, used the Mark IV recording mode for each session.

The IVS program began using the Mark 5 recording mode in mid-2003. By the end of 2007, all

stations were upgraded to Mark 5. Due to the efficient Mark 5 correlator, the program continues

to be dependent on station time and media. The following are the network configurations for the

sessions for which the CORE Operation Center was responsible in 2011:

IVS-R1: 50 sessions, scheduled weekly and mainly on Mondays, six to eleven station networks

RDV: Six sessions, scheduled evenly throughout the year, 13 to 19 station networks

IVS-R&D: Seven sessions, scheduled monthly, eight to eleven station networks

2. IVS Sessions from January 2011 to December 2011

This section displays the purpose of the IVS sessions for which the CORE Operation Center is

responsible.

• IVS-R1: In 2011, the IVS-R1s were scheduled weekly with six to eleven station networks.

During the year, 21 different stations participated in the IVS-R1 network, but there were

only eight stations that participated in at least half of the scheduled sessions—Wettzell (50),

Ny- ̊Alesund (45), Tsukuba (44), Tigo (42), Westford (36), Hobart-12m (27), Kokee (27), and

HartRAO (26). Several new stations were added to the IVS-R1s during 2011, Katherine (9),

Kashima-11m (9), Warkworth (9), and Yarragadee (8).

The purpose of the IVS-R1 sessions is to provide weekly EOP results on a timely basis.

These sessions provide continuity with the previous CORE series. The “R” stands for rapid

turnaround because the stations, correlators, and analysts have a commitment to make the

time delay from the end of recording to the results as short as possible. The time delay goal

is a maximum of 15 days. Participating stations are requested to ship disks to the correlator

as rapidly as possible or to transfer the data electronically to the correlator using e-VLBI.

The “1” indicates that the sessions are mainly on Mondays.

• RDV: There are six bi-monthly coordinated astrometric/geodetic experiments each year that

use the full 10-station VLBA plus up to nine geodetic stations.

These sessions are being coordinated by the geodetic VLBI programs of three agencies: 1.

USNO performs repeated imaging and correction for source structure; 2. NASA analyzes

IVS 2011 Annual Report 143
CORE Operation Center NASA Goddard Space Flight Center

this data to determine a high accuracy terrestrial reference frame; and 3. NRAO uses these

sessions to provide a service to users who require high quality positions for a small number of

sources. NASA (the CORE Operation Center) prepares the schedules for the RDV sessions.

• R&D: The purpose of the seven R&D sessions in 2011, as decided by the IVS Observing

Program Committee, was to test the 512 Mbps recording mode for CONT11 for the first five

sessions. The purpose of the last two sessions was to support observations close to the Sun.

3. Current Analysis of the CORE Operation Center’s IVS Sessions

Table 1 gives the average formal errors for the R1, R4, RDV, and T2 sessions from 2011.

The R1 session formal uncertainties are not significantly different from the 2009-2010 errors. The

R4 uncertainties for 2011 sessions are better than for 2010. This improvement is likely due to

the improved network geometry since several stations were not available in 2010. Specifically,

Fortaleza, Katherine, and Yarragadee were not available in 2010. RDV uncertainties are not

significantly different among the three years from 2009 to 2011. Clearly the RDV formal errors

are significantly better than any of the other experiment series. This is due to the larger number

of RDV stations as well as better global geometry.

Table 2 shows the EOP differences with respect to the IGS series for the R1, R4, RDV, and T2

series. The WRMS differences were computed after removing a bias, but estimating rates did not

affect the residual WRMS significantly. Both the R1 and R4 series show worse WRMS agreement

in x-pole and y-pole for 2011 than for the R1 and R4 series since 2000. This is consistent with the

formal error trend for the R4s, but it is not clear why the agreement is worse for the R1s. There

are some significant biases greater than 100 μas between the VLBI and GPS series that should

be investigated. Formal uncertainties of the bias estimates are not shown, but the polar motion

biases are all several sigma. Of all the series, the RDV series has the best WRMS agreement of

x-pole and y-pole with IGS in 2011 as well as for all sessions since 2000. However, there are really

too few RDV and T2 sessions to give significance to the WRMS differences for 2011 compared

with the full series from 2000-2011.

Table 1. Average EOP Formal Uncertainties for 2011.

Session Num X-pole Y-pole UT1 DPSI DEPS

Type (μas) (μas) (μs) (μas) (μas)

R1 51 65(60,61) 64(58,61) 3.0(3.0,2.4) 112(116,128) 45(47,51)

R4 5l 85(96,72) 76(84,77) 3.2(3.2,2.9) 163(172,189) 66(71,72)

RDV 3 42(42,40) 44(43,40) 2.0(2.0,1.7) 71(68,68) 26(28,27)

T2 3 113(93,79) 125(100,89) 5.5(5.2,4.1) 255(192,171) 90(75,69)

Values in parentheses are for 2010 and then 2009.

144 IVS 2011 Annual Report
NASA Goddard Space Flight Center CORE Operation Center

Table 2. Offset and WRMS Differences (2011) Relative to the IGS Combined Series.

X-pole Y-pole LOD

Session Type Num Offset WRMS Offset WRMS Offset WRMS

(μas) (μas) (μas) (μas) (μs/d) (μs/d)

R1 51(510) -102(-43) 108(95) 105(67) 109(87) 0.6(0.2) 17(17)

R4 51(507) -92(-77) 128(112) 85(62) 129(112) 0.4(1.5) 16(18)

RDV 3(69) -96(12) 92(78) 127(68) 8(70) -5.1(-0.3) 9(15)

T2 3(76) -85(-44) 100(140) 139(47) 253(124) 21.2(1.4) 23(20)

Values in parentheses are for the entire series (since 2000) for each session type

4. The CORE Operations Staff

Table 3 lists the key technical personnel and their responsibilities so that everyone reading this

report will know whom to contact about their particular question.

Table 3. Key Technical Staff of the CORE Operations Center.

Name Responsibility Agency

Dirk Behrend Organizer of CORE program NVI, Inc./GSFC

Brian Corey Analysis Haystack

Ricky Figueroa Receiver maintenance ITT Exelis

John Gipson SKED program support and development NVI, Inc./GSFC

Frank Gomez Software engineer for the Web site Raytheon/GSFC

David Gordon Analysis NVI, Inc./GSFC

Ed Himwich Network Coordinator NVI, Inc./GSFC

Dan MacMillan Analysis NVI, Inc./GSFC

Katie Pazamickas Maser maintenance ITT Exelis

David Rubincam Procurement of materials necessary for CORE

operations

GSFC/NASA

Braulio Sanchez Procurement of materials necessary for CORE

operations

GSFC/NASA

Dan Smythe Tape recorder maintenance Haystack

Cynthia Thomas Coordination of master observing schedule

and preparation of observing schedules

NVI, Inc./GSFC

5. Planned Activities during 2012

The CORE Operation Center will continue to be responsible for the following IVS sessions

during 2012.

• The IVS-R1 sessions will be observed weekly and recorded in a Mark 5 mode.

IVS 2011 Annual Report 145
CORE Operation Center NASA Goddard Space Flight Center

• The IVS-R&D sessions will be observed ten times during the year.

• The RDV sessions will be observed six times during the year.

146 IVS 2011 Annual Report
U.S. Naval Observatory NEOS Operation Center at USNO

NEOS Operation Center

Kerry Kingham, M.S. Carter

Abstract

This report covers the activities of the NEOS Operation Center at USNO for 2011. The Operation

Center schedules IVS-R4 and the INT1 Intensive experiments.

1. VLBI Operations

NEOS operations in the period covered consisted, each week, of one 24-hour duration IVS-R4

observing session (on Thursday-Friday) for Earth Orientation and five daily one-hour duration

“Intensives” for UT1 determination (Monday through Friday). In 2011, the operational IVSR4 network included VLBI stations at Kokee Park (Hawaii), Wettzell (Germany), Ny- ̊Alesund

(Norway), TIGO (Chile), Svetloe, Badary and Zelenchukskaya (Russia), Hobart (Australia), Yebes

(Spain), and Matera and Medicina (Italy). A typical IVS R4 consisted of eight to twelve stations.

The regular stations for the weekday IVS Intensives were Kokee Park and Wettzell. Intensives

including Kokee Park, Wettzell, and Svetloe were occasionally scheduled in order to characterize

the Kokee Park — Svetloe baseline so that Svetloe can be used as an alternate for Wettzell should

it be needed. Odd-day Intensives were scheduled with the scheduling technique used since 2000;

even-day Intensives were scheduled with a new, experimental scheduling technique.

The Operation Center updated the version of sked as updates became available.

All sessions are correlated at the Washington Correlator, which is located at USNO and is run

by NEOS.

Table 1. Experiments scheduled during 2011.

experiment type # sessions

IVS-R4 49

Intensives 230

2. Staff

K. A. Kingham and M. S. Carter are the only staff members of the NEOS Operation Center.

Kingham is responsible for the overall management, and Carter makes the schedules. M. S. Carter

is located at the USNO Flagstaff Station (NOFS).

IVS 2011 Annual Report 147

Correlators

Correlators

Institut f ̈ur Geod ̈asie und Geoinformation der Universit ̈at Bonn Bonn MPIfR/BKG Correlator

The Bonn Astro/Geo Correlator

Laura La Porta, Walter Alef, Simone Bernhart, Alessandra Bertarini, Arno M ̈uskens,

Helge Rottmann, Alan Roy

Abstract

The Bonn Distributed FX (DiFX) correlator is a software correlator operated jointly by the MPIfR

and the IGG in Bonn and the BKG in Frankfurt.

1. Introduction

The Bonn correlator is hosted at the Max-Planck-Institut f ̈ur Radioastronomie (MPIfR)1in

Bonn, Germany. It is operated jointly by the MPIfR and the Bundesamt f ̈ur Kartographie und

Geod ̈asie (BKG)2in cooperation with the Institut f ̈ur Geod ̈asie und Geoinformation der Universit ̈at

Bonn (IGG)3. It is a major correlator for geodetic observations and astronomical projects, for

instance those involving pulsar gating, millimeter wavelengths, and astrometry.

2. Present Correlator Capabilities

The Distributed FX correlator4 was developed at Swinburne University in Melbourne, Australia by Adam Deller (and collaborators) and adapted to the VLBA operational environment by

Walter Brisken and NRAO staff. DiFX in Bonn is installed and running on a High Performance

Compute Cluster (HPC cluster – see Figure 1).

Features of the software correlator cluster are:

• 60 nodes (8 compute cores each)

• 4 TFlops in the Linpack benchmark test

• 20 Gbps Infiniband interconnection

• 10 RAIDs (about 380 TBs storage capacity)

• one control node for correlation (fxmanager)

• two computers (called frontend and frontend2) for executing parallelized jobs on the cluster,

e.g., post-correlation applications

• one control computer (appliance) for installing and monitoring the cluster

• closed loop rack cooling

The correlator cluster is connected via 2 × 1 Gb Ethernet to 14 Mark 5 units5 used for playing

back the data. If more than 14 playback units are required, and in the case of e-VLBI, data are

1

http://www.mpifr.de/div/vlbicor

2

http://www.bkg.bund.de/

3

http://www.gib.uni-bonn.de/

4DiFX: A Software Correlator for Very Long Baseline Interferometry using Multiprocessor Computing Environments, 2007, PASP, 119, 318

5http://www.haystack.mit.edu/tech/vlbi/mark5/

IVS 2011 Annual Report 151
Bonn MPIfR/BKG Correlator Institut f ̈ur Geod ̈asie und Geoinformation der Universit ̈at Bonn

Figure 1. From the left: the first and second racks contain the storage RAIDs and frontend2; the third and

fourth racks contain the cluster nodes, fxmanager and frontend.

copied to the raid systems prior to correlation. All Mark 5 can play back all types of Mark 5

data (A/B/C). The disk-modules in the Mark 5 are controlled via NRAO’s mk5daemon program.

The available functionality includes all necessary functions such as recording the directories of the

modules, resetting and rebooting the units, and module conditioning.

A summary of the capabilities of the DiFX software correlator is presented in Table 1.

3. Staff

The people in the geodetic group at the Bonn correlator are

Arno M ̈uskens - group leader, scheduling of T2, OHIG, EURO, INT3.

Simone Bernhart - e-VLBI supervision and operations, experiment setup and evaluation of correlated data, media shipping.

Alessandra Bertarini - experiment setup and evaluation of correlated data for both astronomy

and geodesy, digital baseband converter (DBBC) testing (APEX fringe test). Friend of the correlator.

Laura La Porta - experiment setup and evaluation of correlated data, DBBC testing.

Fr ́ed ́eric Jaron - phasecal extraction for software correlator, software support, and Web page

maintenance.

Two student operators for the night shifts and the weekends.

The people in the astronomical group at the Bonn correlator are

Walter Alef - head of the VLBI technical department, computer systems and cluster administration.

Alan Roy - deputy group leader, support scientist (water vapor radiometer, technical assistance,

development of FPGA firmware for linear to circular polarization conversion, project manager for

equipping APEX for millimeter VLBI).

152 IVS 2011 Annual Report
Institut f ̈ur Geod ̈asie und Geoinformation der Universit ̈at Bonn Bonn MPIfR/BKG Correlator

Table 1. Correlator capabilities.

Playback Units

Number available 14 Mark 5 (4 Mark 5A, 2 Mark 5B, 8 Mark 5C)

Playback speed 1.6 Gbps

Formats Mark 5A, Mark 5B, LBA, VDIF

Sampling 1 bit,2 bits

Fan-out (Mark 5A) 1:1, 1:2, 1:4

Nr channels ≤ 16 USB and/or LSB

Bandwidth/channel (2, 4, 6, 8, 32) MHz

Signal Single-, dual-frequency; all four Stokes parameters

for circular and linear polarization

Correlation

Geometric model CALC 9

Phase cal Phase-cal extraction of all tones in a sub-band simultaneously

Pre-average time Milliseconds to seconds

Spectral channels Max no. of FFT tested 218

Export FITS export. Interface to Mk IV data format which enables the use of

geodetic analysis software and Haystack fringe fitting program.

Pulsar Pulsar gating possible

Helge Rottmann - software engineer for correlator development and operation, cluster administration. DBBC and RDBE control software, Field System.

Heinz Fuchs - correlator operator, responsible for the correlator operator schedule, daily operations and media shipping.

Hermann Sturm - correlator operator, correlator support software, media shipping, and Web

page development.

Rolf M ̈artens - technician maintaining cluster hardware and Mark 5 playbacks.

Gino Tuccari - guest scientist from INAF, DBBC development, DBBC project leader.

Michael Wunderlich - engineer, development and testing of DBBC components.

Jan Wagner - PhD student, support scientist for APEX, DBBC development, DiFX developer.

David Graham - consultant (technical development, DBBC development and testing).

4. Status

Experiments: In 2011 the Bonn group correlated sixty-five R1, six EURO, seven T2, six

OHIG, forty INT3, and about twenty astronomical experiments.

e-VLBI: e-transfers to Bonn are performed on a regular basis from Tsukuba, Ny- ̊Alesund,

Onsala, Fortaleza, Hartebeesthoek, Mets ̈ahovi, Wettzell, Kashima (including data of the antarctic

Syowa station), Aira, Chichijima, Japanese VERA stations Ishigakijima (all from Tsukuba) and

Mizusawa (from Mitaka), Medicina, Yebes, Hobart and Warkworth. E-transfer reduces the time

between observation and correlation since no shipment is required. The achieved data rates range

from 100 Mb/s with Ny- ̊Alesund (limited by radio link) to 600 Mb/s with peaks up to 800 Mb/s

IVS 2011 Annual Report 153
Bonn MPIfR/BKG Correlator Institut f ̈ur Geod ̈asie und Geoinformation der Universit ̈at Bonn

(with Mets ̈ahovi). The transfers are done using the UDP-based Tsunami protocol. The total disk

space available for e-VLBI data storage at the correlator is currently about 70 TB. A webpage

has been developed (http://www.mpifr-bonn.mpg.de/cgi-bin/showtransfers.cgi), which shows currently active (Tsunami) e-transfers and helps to coordinate transfer times and rates on a first

come-first served base.

DiFX software correlator: A graphical user interface was installed on the DiFX control

computer, which simplifies the use of the software correlator.

A new graphical user interface (comedia) has been implemented to replace the old tape library

administration software. Comedia permits the operator to monitor the modules from the time

they arrive at the correlator to the moment they are sent back to the stations. In particular, it

allows one to trace whether a module can be released, a feature that was not present in the old

tape library. All experiment and module related metadata are stored in a relational database.

The DiFX software correlator has been operated at Bonn since 2009 and has been continuously updated and improved. Thanks to the possibility of performing pulsar gating, the DiFX

correlator in Bonn became a top center for the correlation of EVN pulsar experiments. Significant

improvements have been made to adapt the DiFX correlator to the geodetic export path via Mark

IV format and fourfit, although some issues are left that will probably soon be resolved. This

requires at present some work-arounds sometimes causing delays in the submission of experiment

databases.

A branch version of the DiFX software correlator for RFI mitigation is being developed as part

of a PhD project.

DBBC: The Bonn group is involved in the development of the DBBC for the European VLBI

Network (EVN) and geodesy. The DBBC is designed as a full replacement for the existing analog BBCs. The following stations have already bought one or more DBBCs: APEX, AuScope

(Australia), Effelsberg, Onsala, Pico Veleta, Yebes, Wettzell, and Warkworth. The functionality of these DBBCs is currently being tested. The AuScope and Effelsberg stations already use

the DBBC in their regular observations. A test at 2 Gbps was successfully performed using the

Effelsberg and Onsala DBBCs in July 2011.

APEX: The Bonn VLBI group is equipping the APEX telescope for VLBI observations at

1 mm. The first fringe tests were performed in March 2011 (results pending).

5. Outlook for 2012

DiFX Correlator: Continue testing the DiFX software and ancilliary programs to match the

geodetic needs.

e-VLBI: Tests of e-VLBI transfer with other antennas are planned or ongoing. In order to

meet the requirements of the higher observing rate foreseen within VLBI2010, it is planned to

upgrade the Internet connection from 1 Gbps to 2 Gbps. However, there are some issues concering

funding and technical implementation.

DBBC: Continue DBBC testing in the EVN stations that recently acquired DBBCs. Wide

bandwidth modes are also under test. First observations at 2 Gbps are planned for 2012.

APEX Further fringe tests will take place at APEX in March 2012.

Phasing up ALMA The group is involved in an international project to add array phasing

capability to ALMA. This will enable its use as an extremely sensitive station in 1 mm VLBI

experiments.

154 IVS 2011 Annual Report
MIT Haystack Observatory Haystack Correlator

Haystack Observatory VLBI Correlator

Mike Titus, Roger Cappallo, Brian Corey, Kevin Dudevoir, Arthur Niell, Alan Whitney

Abstract

This report summarizes the activities of the Haystack Correlator during 2011. Highlights include

acquisition of new hardware for a DiFX cluster, development and improvement of tools to facilitate

DiFX production, more u-VLBI Galactic Center observations, Mark 6 recording system testing, and

various other continuing projects. Non-real-time e-VLBI transfers and engineering support of other

correlators continued.

1. Introduction

The Mark IV and DiFX VLBI correlators of the MIT Haystack Observatory, located in Westford, Massachusetts, are supported by the NASA Space Geodesy Program and the National Science

Foundation. They are dedicated mainly to the pursuits of the IVS, with a smaller fraction of time

allocated to processing radio astronomy observations for the Ultra High Sensitivity VLBI (u-VLBI)

project. The Haystack correlators serve as a development system for testing new correlation modes,

for hardware improvements such as the Mark 6 system, and in the case of the Mark IV, for diagnosing correlator problems encountered at Haystack and at the identical correlator at the U.S. Naval

Observatory. This flexibility is made possible by the presence on-site of the team that designed the

Mark IV correlator hardware and software. Some software support is provided to the Max Planck

Institute for Radioastronomy (MPI) in Bonn, Germany for DiFX processing of IVS experiments.

2. Summary of Activities

2.1. DiFX Cluster Acquisition

Commissioning of the DiFX correlator has accelerated. Acquisition of cluster hardware began

in mid-2011. This included the purchase of six Supermicro server machines with 12-core Intel

CPUs, an infiniband switch, and infiniband cards for each server and some of the capable Mark 5

units. Configuration and testing of the cluster and new hardware are in progress. The transition

to all-DiFX correlation is expected in the first half of 2012 but will be coupled with hardware

correlator comparison tests. Some comparison tests of many experiment types have already been

done with the existing setup. The annual DiFX developers’ meeting, which was held at Haystack

in 2011, resulted in much progress adapting some of the other sites’ tools, such as the database

system developed at MPI and a GUI developed at USNO. Other tools will be adapted by mid-2012.

2.2. DiFX Software Support

Meanwhile, the development of the tools to support conversion of DiFX output to Mark IV

format has continued, such as the difx2mark4 utility for converting DIFX correlator output and

an export package of HOPS tools to facilitate post-processing data analysis at other institutions.

Some of these tools have been installed at Goddard and used to process geodetic experiments.

IVS 2011 Annual Report 155
Haystack Correlator MIT Haystack Observatory

2.3. Broadband Delay

Although Broadband Delay “production” observing has been light this year, one major milestone was reached in seeing first fringes to the Patriot 12-meter antenna which was recently completed at the GGAO site. Two fringe tests were conducted over the last year, one in March and

another in June.

2.4. Galactic Center Observations

Further u-VLBI observations of the Galactic Center were conducted and correlated. The lessons

from 2010’s engineering test of a phased-array processor system to combine the collecting area of

interferometer elements on Mauna Kea were applied to the interferometer elements at the CARMA

site.

2.5. WACO Support

Similar to 2009, the Haystack correlator was used during the Technical Operations Workshop

(TOW) held at Haystack in May to process Kokee-Wettzell Intensive sessions, with the data then

being sent down to WACO for cleanup and export. This demonstrated that Haystack can serve

as a backup correlation site in the event of down time at WACO. Another experiment, an APSG,

was correlated at Haystack to reduce WACO’s processing backlog. The raw correlator output was

fourfited and exported by WACO. This correlation was also done to fulfill contractual requirements

to USNO.

2.6. Bonn Support

A significant amount of support for difx2mark4 and HOPS issues was provided to the Bonn

DiFX correlator to facilitate geodetic operations. Also, the Haystack Correlator gave support

related to the SgrA* Galactic Center observations conducted in April to facilitate fringe searches

for two newly participating MPI-sponsored antennas.

2.7. Special IYA Export

A special export of the IYA-2009 data was made for Arnaud Collioud of Bordeaux Observatory

to allow imaging of sources in the AIPS software package (one of the goals of the IYA session).

Assistance was also provided for the HOPS software package so that the data could be prepped

for reading into AIPS through the MPI-developed mk4in method.

2.8. RDV Fourfiting

With NRAO converted to DiFX correlation, the option of processing RDV experiments through

the HOPS/Mark IV data path, as opposed to the AIPS path, has opened. In order to test the

viability of this path, RDV85 through RDV89 were converted to the Mark IV data structure with

difx2mark4 and then fourfited. It was concluded that the Mark IV data path is preferable, so we

are developing a procedure to turn Mark IV conversion and fringing into the default method.

156 IVS 2011 Annual Report
MIT Haystack Observatory Haystack Correlator

2.9. Mark 6 Testing

A live demonstration of 16 Gb/sec recording with RDBEs and Mark 6 data recorders was performed at the TOW meeting in May. Another test was conducted in October between GGAO and

Westford, where fringes were obtained using RDBE digital back ends and Mark 6 data recorders.

A description of the Mark 6 system and those demonstrations can be found at:

http://www.haystack.mit.edu/tech/vlbi/mark6/mark6 memo/04-2011.12.05 Mark6 data system

-DiFX mtg-Haystack.pdf

2.10. e-VLBI

Non-real-time transfers have continued. Data from thirty-two experiments were transferred to

Haystack this year from nine stations (eight in Japan, and one in Sweden): Kashima34, Kashima11,

Koganei, Tsukuba, Chichijima, Ishigaki, Aira, Mizusawa, and Onsala. e-VLBI transfers will significantly increase this coming year due to an upgrade of Haystack’s connectivity to the Internet,

which enables higher data transfer rates.

2.11. Experiments Correlated

Production processing using the Mark IV correlator continues amidst all the DiFX development.

In 2011, twenty-nine geodetic VLBI experiments were processed, at least in part, on the Haystack

Mark IV correlator, consisting of six R&Ds, six T2s, an AUST experiment, an APSG, and the

Intensives during the TOW for USNO as mentioned before. The remainder were various tests. The

R&Ds were especially important this year as they were preparatory tests for the CONT campaign

which ran in September. This pre-testing was designed to ensure that the CONT campaign

collected the highest quality data possible. The other test experiments included the broadband

fringe tests and an assortment of other projects, some of which were touched on in the summary

above. As usual, there were smaller tests that are not included in the above count because they

were too small to warrant individual experiment numbers.

3. Current/Future Hardware and Capabilities

As of the end of 2011, the Mark IV correlator was comprised of seven Mark 5A units, seven

station units, seven Mark 5B units (DOMs) with their associated correlator interface boards (CIBs),

16 operational correlator boards, two crates, and miscellaneous other support hardware. We have

the capacity to process all baselines for 11 stations simultaneously in the standard geodetic modes,

provided the aggregate recordings match the above hardware matrix. Note that all experiments

up to 15 stations have been done in one pass due to the ability to share playback units between

stations which do not co-observe. A subset of the playback units is accessible to the DiFX cluster.

In 2012 we hope to transition to the software correlator, only keeping the hardware correlator

alive in support of USNO until their transition to a software correlator, which is expected in late

2012.

IVS 2011 Annual Report 157
Haystack Correlator MIT Haystack Observatory

4. Staff

Staff who participated in aspects of Mark IV, DiFX, Mark 5/6, and e-VLBI development and

operations include:

4.1. Software Development Team

• John Ball - Mark 5A/5B; e-VLBI

• Roger Cappallo - real-time correlator software and troubleshooting; system integration; postprocessing; Mark 5B/5C/6; Linux conversion; e-VLBI; DiFX correlator development

• Geoff Crew - DiFX correlator development, post-processing software; Mark 6

• Kevin Dudevoir - correlation; maintenance/support; Mark 5A/5B/5C; e-VLBI; Linux

conversion; correlator software and build system development; computer system support/development; DiFX correlator development

• Jason SooHoo - e-VLBI; Mark 5A/5B/5C/6; computer system support

• Chester Ruszczyk - e-VLBI; Mark 5A/5B/5C

• Alan Whitney - system architecture; Mark 5A/5B/5C/6; e-VLBI

4.2. Operations Team:

• Peter Bolis - correlator maintenance

• Brian Corey - experiment correlation oversight; station evaluation; technique development

• Dave Fields - playback drive maintenance; Mark 5 installation and maintenance; general

technical support

• Glenn Millson - correlator operator

• Arthur Niell - technique development

• Don Sousa - correlator operator; experiment setup; tape library and shipping

• Mike Titus - correlator operations oversight; experiment setup; computer services; software

and hardware testing

• Ken Wilson - correlator maintenance; playback drive maintenance; general technical support

5. Conclusion/Outlook

A full transition to the DiFX software correlator is expected by mid-2012. Testing of a complete

VLBI2010 system comprised of new front and back end hardware at a station is expected to start

in early 2012. Testing and implementation of new digital back ends and recording systems will

continue.

158 IVS 2011 Annual Report
IAA RAS IAA Correlator Center

IAA Correlator Center

Igor Surkis, Voitsekh Ken, Alexey Melnikov, Vladimir Mishin, Nadezda Sokolova,

Violet Shantyr, Vladimir Zimovsky

Abstract

The activities of the six-station IAA RAS correlator include regular processing of national geodetic

VLBI programs Ru-E, Ru-U, and Ru-F. The Ru-U sessions transferred in e-VLBI mode and correlated

in the IAA Correlator Center automatically since 2011.

1. Introduction

The IAA Correlator Center is located at and staffed by the Institute of Applied Astronomy in

St.-Petersburg, Russia.

The IAA Correlator Center is devoted to processing geodetic, astrometric, and astrophysical

observations made with the Russian national VLBI network Quasar.

Figure 1. View of the six-station ARC correlator, showing four racks containing (left to right) signal

distribution and synchronization system (SDSS) and three Mark 5B playback units, two correlator crates

and KVM, three correlator crates, and one more cabinet with SDSS and three Mark 5B playback units.

IVS 2011 Annual Report 159
IAA Correlator Center IAA RAS

2. Component Description

The ARC (Astrometric Radiointerferometric Correlator) (Figure 1) was the main data processing device in the IAA Correlator Center in 2011. The ARC was designed and built in the IAA

RAS in 2007 - 2009. The correlator has XF design and is based on FPGA technology.

The ARC is a six-station, 15-baseline correlator. It is able to process up to 16 frequency

channels on each baseline, for a total of 240 channels. The correlator accesses two-bit VLBI

signals with 32 MHz maximal clock frequency. The maximal data range from each station is

1 Gbit per second. The correlator requires VSI-H input VLBI signals, and it is equipped with

Mark 5B playback terminals.

In 2011 the correlator control software was improved to obtain almost fully automatic data

transfer and processing in e-VLBI mode. Special software corrections were made due to the use of

R1002M DAS at Quasar stations.

The ARC was used for processing all of the national geodetic VLBI observations in the IAA

Correlator Center in 2011.

In 2011 the DiFX software correlator was installed in the IAA on a Sun Fire X4450 Server.

The DiFX works as a virtual machine under the VMware, and it is used in some astrophysical

experiments.

3. Staff

• Voitsekh Ken — hardware developer;

• Alexey Melnikov — software developer, scheduler of the Ru-sessions;

• Vladimir Mishin — software developer, data processing;

• Nadezda Sokolova — software developer;

• Violet Shantyr — software developer, post processing;

• Igor Surkis — leading investigator, software developer;

• Vladimir Zimovsky — hardware developer, data processing;

• Ekaterina Medvedeva — data processing.

160 IVS 2011 Annual Report
National Institute of Information and Communications Technology VLBI Correlators in Kashima

VLBI Correlators in Kashima

Mamoru Sekido, Ryuichi Ichikawa

Abstract

K5 VLBI data acquisition and processing systems developed at the Kashima Space Technology

Center have been used for R&D VLBI experiments. Correlation tasks processed in 2011 were mainly

for crustal deformation monitoring between the Kashima 11-m and Koganei 11-m stations after the

big earthquake that occurred on 11 March 2011.

1. General Information

Figure 1. Locations of NICT Headquarters and KSTC.

The VLBI group of the Kashima

Space Technology Center (KSTC) of

the National Institute of Information and Communications Technology (NICT: Figure 1) has been contributing to the VLBI community by

developing the K5 VLBI data acquisition system (DAS) and correlation

systems.

The multi-channel DAS named

K5/VSSP32 [1] has been used for

geodetic and radio science observations. A corresponding software correlation package for the K5/VSSP32

DAS has been developed and maintained by Dr. T. Kondo. Another

high speed software correlator called

“GICO3” [2], has been developed by

M. Kimura.

The K5/VSSP32 system is a multi-channel data acquisition system with four channels input

per unit. One unit has the sampling capability in the range of 40 kHz to 64 MHz at 1, 2, 4, and 8

bits quantization within the limit of output data rate up to 256 Mbps. A geodetic K5 DAS system

is composed of four K5/VSSP32 units. The K5/VSSP software package contains a variety of

VLBI data manipulation utilities from data acquisition with the K5/VSSP32 in accordance with

the observation schedule file and data checking of K5 and Mark 5 data, to conversion between

K5/VSSP32 format and the Mark IV, Mark 5, and VLBA data formats. This DAS and the

software correlator package have been widely used for geodesy operationally. e-VLBI experiments

for rapid UT1 measurements have been performed by using the K5 software correlator for the

Onsala, Mets ̈ahovi, Tsukuba, and Kashima stations [3, 4].

Another K5 system (K5/VSI) is the name of the recording system with a VSI-H interface.

NICT has developed three kinds of samplers with a VSI-H interface [5] (see Table 1). Thus a

variety of combinations of sampling rate and number of output channels is possible. And the

K5/VSI can be connected with not only NICT’s ADS samplers, but also any sampler with a VSIH compliant data interface. A good example is the combination use of the K5/VSI and Mark 5B

IVS 2011 Annual Report 161
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Table 1. Three VLBI samplers with VSI-H interface developed by NICT

ADS1000 ADS2000 ADS3000Plus

Pictures

Sampling rate 1024Msps 64Msps ∼ 4Gsps

No. of inputs 1 16 4

No. of channels 1 16 Programmable

Max. Data Rate 2048Mbps 2048Mbps 8192Mbps

sampler at Wettzell, which has routinely been used for real-time data transfer in the INT2 sessions.

The VSI-H output data stream from the Mark 5B sampler is captured by the K5/VSI. Then it is

transfered to the Tsukuba station and recorded in K5/VSSP32 format in real-time for ultra-rapid

UT1 measurements on the Wettzell—Tsukuba baseline.

2. Staff

The mega-earthquake that occurred on 11 March 2011 caused destruction of roads and some

parts of KSTC’s buildings. Fortunately there were no personal injuries in our laboratory.

The names of the staff members who contribute to the Correlation Center at NICT/Kashima

and their tasks are listed below in alphabetical order.

• HASEGAWA Shingo: in charge of maintenance and troubleshooting of K5 system computers,

operation of the 34-m antenna for IVS sessions.

• HOBIGER Thomas: working at Koganei Headquarters in Tokyo for development of a new

VLBI database system that uses NetCDF, research on atmospheric delay calibration with

the ray tracing technique, and development of a software receiver for GNSS.

• ICHIKAWA Ryuichi: VLBI Project Manager at Kashima, in charge of research on the small

size antenna with wide band receiver system named MARBLE project [6] and on atmospheric

delay with ray tracing.

• KAWAI Eiji: in charge of maintenance of the 34-m and 11-m telescopes, operation of the

telescopes for IVS sessions.

• KIMURA Moritaka: developer of the high speed Gigabit software correlator “GICO3” and

the K5/VSI DAS. He left from KSTC at the end of March 2011.

• KONDO Tetsuro: continuing development and maintenance of the software correlator package of the K5/VSSP32.

• SEKIDO Mamoru: e-VLBI development, Time and Frequency transfer experiments, and

maintenance of the 34-m and 11-m antennas.

• TAKEFUJI Kazuhiro: correlation processing operation with GICO software correlator, development of MARBLE antenna, and its application for Time and Frequency transfer.

• TSUTSUMI Masanori: maintenance of K5 system computers and network environment.

162 IVS 2011 Annual Report
National Institute of Information and Communications Technology VLBI Correlators in Kashima

3. Component Description

-5

 0

 5

 10

 15

 20

 25

 30

 35

 40

01 May 01 Jun. 01 Jul. 01 Aug. 01 Sep. 01 Oct. 01 Nov.

Baseline Length - 109100165 (mm)

Dates in 2011

Kashim11-Koganei Baseline Length

Figure 2. Post-seismic baseline length changes of Kashima11 –

Koganei11 from sessions that were correlated at NICT and are

listed in Table 2, as well as APSG29 and T2077 (which were

correlated at GSI/Tsukuba and are omitted from Table 2).

The APSG29 and T2077 points have the largest error bars.

After the big earthquake occurred

on 11 March 2011 in the north

east region of Japan, post-seismic

crustal deformation monitoring with

the Kashima-Koganei VLBI baseline

was regularly conducted from 7 May

2011 until October with a 20 day interval (Figure 2). Correlation processing

of these data were performed by using

Multi-core PC (e.g., CPU Intel Core i7

920 2.67 GHz cache 8192KB, Processor 4 (Hyper Threading Total Core8),

Memory 12 GB) and cluster of PCs,

which are used for data recording of

K5/VSSP32. Table 2 shows a list of

experiments processed at Kashima.

Table 2. Major correlation tasks processed at Kashima in 2011. The first eight sessions (K11127 through

K111279) are also shown in Figure 2. R&D experiment D11292 is not shown in that figure.

Project Exp code Date Stations baseline x scans Data rate

(Mbps)

Geodesy K11127 7 May K1, Kg 1 x 1085 256

Geodesy K11146 26 May K1, Kg 1 x 1379 256

Geodesy K11167 16 Jun. K1, Kg 1 x 1338 512

Geodesy K11188 07 Jul. K1, Kg 1 x 1192 512

Geodesy K11208 27 Jul. K1, Kg 1 x 1256 512

Geodesy K11227 15 Aug. K1, Kg 1 x 1264 512

Geodesy K11256 13 Sep. K1, Kg 1 x 1278 512

Geodesy K11279 6 Oct. K1, Kg 1 x 1278 512

Direct Sampling D11292 19 Oct. K1, Ts 1 x 928 1024

Ts:Tsukuba-32m, K1:Kashima-11m, Kg:Koganei-11m

4. Development and Future Plans

4.1. Direct Sampling Experiment

A geodetic VLBI experiment with the Radio Frequency Direct Sampling system was conducted

on 19 October, and its data were processed with the GICO3 software correlator. That system

samples joined S-band and X-band radio frequency signals simultaneously with 1024 MHz-2bit

quantization. It uses an aliasing effect to record the signal outside of the Nyquist frequency range

of the sampling rate. A total of 1.5 GHz of frequency range of X-band was recorded with 1024

MHz sampling. Reversely folded frequency signals of X-band and S-band were processed separately

IVS 2011 Annual Report 163
VLBI Correlators in Kashima National Institute of Information and Communications Technology

with different RF correlation parameters in accordance with the observation. Since only a single

sampler is used for dual band observation, a sampling clock offset between S and X-band could

be avoided. Thus it has the potential to be a key technology for utilizing phase delay observables

across the wide frequency band. More details are described in “Technology Development Center

at NICT” in this volume [7].

References

[1] T. Kondo, et al.: Development of a New VLBI Sampler Unit (K5/VSSP32) Equipped with a USB

2.0 Interface, IVS 2006 General Meeting Proceedings, edited by Dirk Behrend and Karen Baver,

NASA/CP-2006-214140, pp.195-199, 2006.

[2] M. Kimura, et al.: High Speed VLBI Software Correlator, Submitted to Pub. Astr. Soc. Pacific, 2010.

[3] Sekido. M., H. Takiguchi, Y. Koyama, T. Kondo, R. Haas, J. Wagner, J. Ritakari, S. Kurihara,

K. Kokado: Ultra-rapid UT1 measurement by e-VLBI, Earth Planets and Space, 60, pp.865-870,

2008.

[4] Matsuzaka S., S. Kurihara, M. Sekido, T. Hobiger, R. Haas, J. Ritakari, J. Wagner: Ultra-rapid dUT1

Measurements on Japan-Fennoscandian Baselines - Application to 24-hour Sessions, IVS 2010 General

Meeting Proceedings, pp.143-147, 2010.

[5] Whitney, A. R.: VLBI Standard Hardware Interface Specification -VSI-H Rev. 1.01, 2000.

[6] Ichikawa, R., et al.: Present Status and Outlook of Compact VLBI System Development for Providing

over 10km Baseline Calibration, IVS NICT-TDC News 2, 30, pp. 22-25, 2009.

[7] K. Takefuji et al.,: Technology Development Center at NICT, International VLBI Service for Geodesy

and Astrometry 2011 Annual Report, edited by D. Behrend and K. D. Baver, this volume, 2012.

1http://www.vlbi.org/vsi/

2http://www2.nict.go.jp/aeri/sts/stmg/ivstdc/news-index.html

164 IVS 2011 Annual Report
Geospatial Information Authority of Japan Tsukuba VLBI Correlator

Tsukuba VLBI Correlator

Kensuke Kokado, Shinobu Kurihara, Ryoji Kawabata, Kentaro Nozawa

Abstract

This report briefly summarizes activities at the Tsukuba VLBI Correlator in 2011. The Tsukuba

VLBI Correlator processed 145 IVS Intensive sessions and eight Japanese domestic sessions via the

K5/VSSP correlation system, which includes some K5/VSSP kernel software. We improved a software

correlation system and succeeded in shortening the latency of VLBI sessions. All of the sessions

performed after the improvement were correlated by the software correlation system.

Figure 1. Tsukuba VLBI Correlator.

1. Introduction

The Tsukuba VLBI Correlator is a part of VLBI facilities operated by the Geospatial Information Authority of Japan (GSI) as well as the Tsukuba 32-m VLBI station (TSUKUB32). A

principal component of our correlation system is the K5/VSSP correlation software package developed by the National Institute of Information and Communications Technology (NICT). We

can install the software on commercially-based computers operated by CentOS (Linux OS). We

have processed IVS-INT2 sessions and domestic VLBI sessions (JADE sessions) with a number

of computers on which the K5/VSSP software package was installed. The sessions we processed

in 2011 are described in Section 4. The number of processed sessions was dramatically increased

because additional INT2 sessions on the baseline between the Kokee and Wettzell stations were

implemented after the 2011 earthquake off the Pacific coast of Tohoku.

IVS 2011 Annual Report 165
Tsukuba VLBI Correlator Geospatial Information Authority of Japan

2. Component Description

The system components of the Tsukuba VLBI correlator are described in Table 1. We have

two systems to process the observed data from international sessions or domestic sessions.

System 1 is an old correlation system which was used for correlation of JADE sessions and

JAXA sessions. It is operated by a management application “PARNASSUS” (Processing Application in Reference to NICT’s Advanced Set of Software Usable for Synchronization) designed for

distributed correlation processing.

System 2 is a new correlation system which is mainly used for correlation of INT2 sessions. We

introduced distributed processing programs written in Perl script into the system. The programs

have been developed by GSI since 2009 and routinely used since 2010. The framework of the

programs is shown in Figure 2. We can correlate the VLBI data automatically with the new

distributed processing programs. MK3TOOLS is a program to create Mark III databases from the

output files of bandwidth synthesis program for K5/VSSP.

All of the hardware consists of commercially-based products operated on CentOS version 5.4

or 5.5. Now all of the servers work well.

For the INT2 sessions, we have transferred the data from the Wettzell or the Kokee station to

the Tsukuba correlator via high-speed network. The Tsukuba Correlator has been connected to

high-speed network “SINET4 (Science Information NETwork4)” operated by the National Institute

of Informatics (NII). The effective network bandwidth was increased from 1 Gbps to 10 Gbps in

October 2011. The network enables us to perform a real-time data transfer from the Wettzell or

the Onsala station to the Tsukuba correlator.

1st scan

1st scan

Cout file

2nd scan 3rd scan 4th scan 5th scan 6th scan 7th scan 8th scan

2nd scan 3rd scan 4th scan 5th scan 6th scan 7th scan 8th scan

Cout file

Cout file

Cout file

Cout file

Cout file

Cout file

Cout file Data flow

TCP/IP control

rapid_cor.pl

Cor_srv2.pl Cor_srv2.pl Cor_srv2.pl Cor_srv2.pl Cor_srv2.pl Cor_srv2.pl Cor_srv2.pl Cor_srv2.pl

Management server

Correla#on servers

Figure 2. The framework of new distributed processing programs.

166 IVS 2011 Annual Report
Geospatial Information Authority of Japan Tsukuba VLBI Correlator

Table 1. Specifications of the K5/VSSP correlation system components.

System 1 System 2

Management Server 1 server 2 servers

(CPU) (Intel Pentium 4, 3.0 GHz) (Intel Xeon 3.4 GHz dual CPU)

Correlation Servers 16 servers 8 servers

(CPU) (Intel Xeon 3.06 GHz dual CPU) (Intel Xeon 3.4 GHz dual CPU)

Data Servers 24 servers 8 servers

(CPU) (Intel Pentium 4, 3.0 GHz) (Intel Xeon 3.07 GHz quad CPU)

File system NFS Luster File System

Main application PARNASSUS 1.3 Perl Programs

Operating System CentOS version 5.4, version 5.5

Processing Sessions JADE sessions IVS-INT2 sessions

Additional domestic sessions JADE sessions

( until July, 2011 ) JAXA sessions

3. Staff

The technical and engineering staff of the Tsukuba VLBI Correlator is as follows. Most of

our staff members are subcontract engineers from private companies, the Advanced Engineering

Service Co., Ltd (AES) and the Institute of Japanese Union of Scientists and Engineers (I-JUSE).

• Kensuke Kokado (GSI): Correlation Chief, Management of overall activity

• Kentaro Nozawa (AES): Main operator of the correlation work

• Takashi Nishikawa (AES): Sub-operator of the correlation work

• Toshio Nakajima (I-JUSE): System Engineer for computers and network

4. Current Status and Activities

4.1. Processing of JADE Sessions

JADE sessions are domestic 24-hour VLBI sessions scheduled by GSI. The participating stations

in the session are four GSI stations (TSUKUB32, SINTOTU3, CHICHI10, and AIRA) and two

VERA stations (VERAMZSW and VERAISGK) of the National Astronomical Observatory of

Japan (NAOJ). The TSUKUB32 and VERAISGK stations are connected to broad-band network,

so we can transfer the data via network. However, the other stations’ network transfer rates are

too slow to transfer the data to the correlator. Therefore, we have to send the data by shipment

of hard disk. We have more than 100 hard disks for shipment, because we need more than four

disks per station for each JADE session.

The JADE and JAXA sessions processed at the Tsukuba correlator in 2011 are described in

Table 2. The JAXA series was registered by IVS in March 2011, and we submitted all of the

databases that had been observed since 2006. The processing factor of each session is described

in the rightmost column of Table 2. Although the processing times depend on the number or

the performance of the correlation servers, we succeeded in shortening the processing times by

installing the “Lustre File System” and the new distributed processing programs. As a result, the

processing factor per baseline of sessions after September 2011 is smaller than that of the sessions

before that.

IVS 2011 Annual Report 167
Tsukuba VLBI Correlator Geospatial Information Authority of Japan

Table 2. JADE sessions processed in 2011.

Session Stations Processed Baseline # Processing Factor

JADE-1101 TsAiCcVmVs 10 4.00

JAXA-1101 TsAiCcUd 6 1.61

JADE-1104 TsAiCcS3 4 1.68

JADE-1105 TsS3 1 0.59

JADE-1106 TsAiCcS3Vm 4 0.77

JADE-1109 TsK1KgCcS3VmVs 16 3.38

JADE-1110 TsS3 1 0.42

JADE-1111 TsS3 1 0.07

JADE-1112 TsS3 1 0.06

Ts:TSUKUB32, Ai:AIRA, S3:SINTOTU3, Cc:CHICHI10, Vm:VERAMZSW

Vs:VERAISGK, Ud:USUDA, K1:KASHIM11, Kg:KOGANEI

4.2. Processing of IVS-INT2 Sessions

The Tsukuba correlator also processes the data of IVS-INT2/INT3 sessions. Usually, the INT2

sessions are observed on the Tsukuba-Wettzell baseline twice a week (Saturday and Sunday).

However, a number of additional INT2 sessions on the Kokee-Wettzell baseline were implemented

after the 2011 earthquake off the Pacific coast of Tohoku, so the number of INT2 sessions processed

by the Tsukuba correlator was dramatically increased. The number of the processed sessions is

shown in Table 3.

We have transferred all of the data via high-speed network. Especially, the data observed at

Wettzell station is transferred and converted from VDIF to K5 format in real-time (during the

observing session). For the data transfer for the Kokee station, we transferred the data with UDPbased protocol “TSUNAMI” after the observing sessions. The average achieved rate of the data

transfer was up to 300 Mbps. As most of the INT2 sessions on the Tsukuba-Wettzell baseline are

processed in real-time, the processing factors of the session are about 1.00. If we process all of the

data with the new processing programs on the Lustre File System after the observing session, the

processing factor could be under 0.2.

Table 3. IVS-INT2/INT3 sessions processed in 2011.

Session Stations Processed session # AVG. Processing Factor

IVS-INT2(K) Ts-Wz 78 0.73

IVS-INT2(I) Kk-Wz 66 0.54

IVS-INT3(K) Ts-Wz-Ny 1 1.5

Ts:TSUKUB32, Wz:WETTZELL, Kk:KOKEE, Ny:NYALES20

5. Plans for 2012

The Tsukuba VLBI correlator will process eight JADE sessions, 112 IVS-INT2 sessions and one

IVS-INT3 session. We plan to correlate all of the INT2 and INT3 sessions on the Tsukuba-Wettzell

baseline with the real-time correlation system.

168 IVS 2011 Annual Report
U. S. Naval Observatory Washington Correlator

Washington Correlator

Kerry A. Kingham, David M. Hall

Abstract

This report summarizes the activities of the Washington Correlator for the year 2011. The Washington Correlator provides up to 80 hours of attended processing per week plus up to 40 hours of

unattended operation, primarily supporting Earth Orientation and astrometric observations. In 2011

the major programs supported include the IVS-R4, IVS-INT, CONT11, APSG, and CRF observing

sessions.

1. Introduction

The Washington Correlator (WACO) is located at and staffed by the U.S. Naval Observatory (USNO) in Washington, DC, USA. The correlator is sponsored and funded by the National

Earth Orientation Service (NEOS), which is a joint effort of the USNO and NASA. Dedicated to

processing geodetic and astrometric VLBI observations, the facility spent 100 percent of its time

on these sessions. All of the weekly IVS-R4 sessions, all of the IVS-INT01 Intensives, the entire

CONT11, and the APSG and CRF sessions were processed at WACO. The facility houses a Mark

IV Correlator.

Figure 1. The e-transfer corner. A Storage Area Network (large unit) and three Mark 5B+s (far left) collect

data over the high-speed networks and write the data out to Mark 5 diskpacks.

IVS 2011 Annual Report 169
Washington Correlator U. S. Naval Observatory

2. Correlator Operations

- The Washington Correlator continues to operate 80 hours per week with an operator on

duty. The correlator has continued to function well unattended, allowing another 40 hours

per week, on average, of extra processing. This has also decreased the time it takes to process

an R4 or other 24-hour sessions by one day.

- The correlator staff continues the testing and repair of Mark 5 modules. Not only were failed

disks replaced, but some modules were upgraded by the replacement of lower capacity disks

with higher capacity disks.

- A combination of three new Mark 5B playback units and conversions of existing Mark 5A

units to Mark 5B now brings the correlator complement to ten Mark 5Bs and five Mark

5As. Additional Mark 5B+s are used for transfers. The 15 available Mark 5 units allowed

processing of CONT11 in a single pass.

- The correlator processed the entire CONT11 session. In addition to the increase in the

playback complement, a Storage Area Network (SAN) was added to assist in handling the

large volume of electronically transferred observations.

- Intensive observations from Kokee Park and Wettzell were routinely transferred via e-VLBI

during 2011. 24-hour sessions from both Hobart antennas, Warkworth, Ny- ̊Alesund, Fortaleza, Tsukuba, Aira, Kashima, Chichijima, and Sintotu were also transferred by high-speed

networks.

- Correlator time was also spent processing test observations connected with the commissioning

of the 12-m antennas at Katherine, Yarragadee, and Warkworth.

- Table 1 lists the experiments processed during 2011.

Table 1. Experiments processed during 2011.

49 IVS-R4 sessions

6 CRF (Celestial Reference Frame)

3 APSG

230 Intensives

15 CONT11

3. Staff

The Washington Correlator is under the management and scientific direction of the Earth

Orientation Department of the U.S. Naval Observatory. USNO personnel continue to be responsible

for overseeing scheduling and processing. During the period covered by this report, a private

contractor, NVI, Inc., supplied a contract manager and correlator operators. Table 2 lists staff

and their duties.

It is with sadness that we report the death of long-time operator Kenneth Potts on December

27, 2011.

170 IVS 2011 Annual Report
U. S. Naval Observatory Washington Correlator

Table 2. Staff.

Staff Duties

Dr. Kerry Kingham (USNO) Chief VLBI Operations Division

and Correlator Project Scientist

David Hall (USNO) VLBI Correlator Project Manager

Bruce Thornton (NVI) Operations Manager

Harvis Macon (NVI) Lead Correlator Operator

Roxanne Inniss (NVI) Media Librarian

Kenneth Potts (NVI) Correlator Operator

4. Outlook

Due to a change in policy by the U.S. Navy, the NVI contract was ended. We are presently

trying to move the contracted jobs to Naval Observatory positions. By the end of 2011, the

correlator staff had been reduced to three positions, and the backlog of processing and analyis was

growing. We hope to eventually add three more people to bring the staffing up to the original

level.

During 2012, the processing load should be transferred from the present Mark IV hardware

correlator to a DiFX software correlator.

IVS 2011 Annual Report 171

Data Centers

Data Centers

Bundesamt f ̈ur Kartographie und Geod ̈asie BKG Data Center

BKG Data Center

Volkmar Thorandt, Reiner Wojdziak

Abstract

This report summarizes the activities and background information of the IVS Data Center for the

year 2011. Included are information about functions, structure, technical equipment, and staff members

of the BKG Data Center.

1. BKG Data Center Functions

The BKG (Federal Agency for Cartography and Geodesy) Data Center is one of the three

IVS Primary Data Centers. It archives all VLBI related data of IVS components and provides

public access for the community. The BKG Data Center is connected to the OPAR and GSFC

CDDIS Data Centers by mirroring the OPAR and the CDDIS file stocks several times per day.

The following sketch shows the principle of mirroring:

Figure 1. Principle of mirroring

IVS components can choose one of these Data Centers to put their data into the IVS network

by using its incoming area, which each of them has at its disposal. The BKG incoming area is

protected, and users need to obtain the username and password to get access.

An incoming script is watching the incoming area and checking the syntax of the files sent by

IVS components. If it is o.k., the script moves the files into the Data Center directories. Otherwise

the files will be sent to a badfile area. Furthermore, the incoming script informs the responsible

staff at the Data Center by sending e-mails about its activities. The incoming script is part of the

technological unit which is responsible for managing the IVS and the Operational Data Center,

and for carrying out the first analysis steps in an automatic manner. All activities are monitored

to guarantee data consistency and to control all analysis steps from data arrival to delivery of

analysis products to IVS.

Public access to the BKG Data Center is available through FTP and HTTP:

IVS 2011 Annual Report 175
BKG Data Center Bundesamt f ̈ur Kartographie und Geod ̈asie

FTP: ftp://ivs.bkg.bund.de/pub/vlbi/

HTTP: http://ivs.bkg.bund.de/vlbi/

Structure of the BKG IVS Data Center:

vlbi/ : root directory

ivs-special/ : special CRF investigations

ivscontrol/ : control files for the data center

ivsdata/ : VLBI observation files

ivsdocuments/ : IVS documents

ivs-iers/ : old IERS solutions

ivsproducts/ : analysis products

crf/ : celestial frames

trf/ : terrestrial frames

eops/ : earth orientation (24h sessions)

eopi/ : earth orientation (Intensive sessions)

daily_sinex/ : daily sinex files (24h sessions)

int_sinex/ : daily sinex files (Intensive sessions)

trop/ : troposphere

2. Technical Equipment

DELL Server (SUSE Linux operating system)

disk space: 500 GBytes (Raid system)

backup: automatic tape library

3. Staff Members

Volkmar Thorandt (coordination, data analysis, data center, volkmar.thorandt@bkg.bund.de)

Reiner Wojdziak (data center, Web design, reiner.wojdziak@bkg.bund.de)

Dieter Ullrich (data analysis, data center, dieter.ullrich@bkg.bund.de)

Gerald Engelhardt (data analysis, gerald.engelhardt@bkg.bund.de)

176 IVS 2011 Annual Report
NASA Goddard Space Flight Center CDDIS Data Center

CDDIS Data Center Summary for the IVS 2011 Annual Report

Carey Noll

Abstract

This report summarizes activities during the year 2011 and future plans of the Crustal Dynamics

Data Information System (CDDIS) with respect to the International VLBI Service for Geodesy and

Astrometry (IVS). Included in this report are background information about the CDDIS, the computer

architecture, staff supporting the system, archive contents, and future plans for the CDDIS within the

IVS.

1. Introduction

The Crustal Dynamics Data Information System (CDDIS) has supported the archiving and

distribution of Very Long Baseline Interferometry (VLBI) data since its inception in 1982. The

CDDIS is a central facility providing users access to data and derived products to facilitate scientific investigation. The CDDIS archives of GNSS (GPS and GLONASS), laser ranging, VLBI, and

DORIS data are stored on-line for remote access. Information about the system is available via

the Web at the URL http://cddis.gsfc.nasa.gov. In addition to the IVS, the CDDIS actively supports other IAG services including the International GNSS Service (IGS), the International Laser

Ranging Service (ILRS), the International DORIS Service (IDS), the International Earth Rotation

and Reference Systems Service (IERS), and the Global Geodetic Observing System (GGOS) of

the IAG. The current and future plans for the system’s support of the IVS are discussed below.

2. System Description

The CDDIS archive of VLBI data and products is accessible to the public through anonymous

ftp.

2.1. Computer Architecture

The CDDIS is operational on a dedicated server, cddis.gsfc.nasa.gov. The system has over 8

Tbytes of on-line disk storage; at this time, over 140 Gbytes are devoted to VLBI activities. The

CDDIS is located at NASA GSFC and is accessible to users 24 hours per day, seven days per week.

2.2. Staffing

Currently, a staff consisting of one NASA civil service employee and five (one full-time, four

part-time) contractor employees supports all CDDIS activities (see Table 1 below).

3. Archive Content

The CDDIS has supported GSFC VLBI coordination and analysis activities for the past several

years through an on-line archive of schedule files, experiment logs, and data bases in several formats.

This archive has been expanded for the IVS archiving requirements.

The IVS Data Center content and structure is shown in Table 2 below. (A figure illustrating

IVS 2011 Annual Report 177
CDDIS Data Center NASA Goddard Space Flight Center

Table 1. CDDIS Staff

Name Position

Ms. Carey Noll CDDIS Manager

Dr. Patrick Michael System Engineer (part-time)

Dr. Maurice Dube Senior programmer

Mr. Nathan Pollack Programmer (part-time)

Ms. Lori Tyahla Programmer (part-time)

Ms. Lisa Lee Web developer (part-time)

the flow of information, data, and products between the various IVS components was presented

in the CDDIS submission to the IVS 2000 Annual Report.) In brief, an incoming data area has

been established on the CDDIS host computer, cddis.gsfc.nasa.gov. Using specified file names,

operation and analysis centers deposit data files and analyzed results to appropriate directories

within this filesystem. Automated archiving routines, developed by GSFC VLBI staff, peruse the

directories and move any new data to the appropriate public disk area. These routines migrate

the data based on the file name to the appropriate directory as described in Table 2. Index files

in the main sub-directories under ftp://cddis.gsfc.nasa.gov/pub/vlbi are updated to reflect data

archived in the filesystem. Furthermore, mirroring software has been installed on the CDDIS host

computer, as well as at all other IVS data centers, to facilitate equalization of data and product

holdings among these data centers. At this time, mirroring is performed between the IVS data

centers located at the CDDIS, the Bundesamt f ̈ur Kartographie und Geod ̈asie in Leipzig, and the

Observatoire de Paris.

The public filesystem in Table 2 on the CDDIS computer, accessible via anonymous ftp, consists

of a data area, which includes auxiliary files (e.g., experiment schedule information, session logs)

and VLBI data (in both database and NGS card image formats). A products disk area has also

been established to house analysis products from the individual IVS analysis centers as well as

the official combined IVS products. A documents disk area contains format, software, and other

descriptive files.

4. Data Access

During 2011, over 1600 distinct hosts accessed the CDDIS on a regular basis to retrieve VLBI

related files. These users, which include other IVS data centers, successfully downloaded over 80

Gbytes of data and products (1.2 M files) from the CDDIS VLBI archive last year.

5. Future Plans

In early 2012, the CDDIS will move operations to a new distributed, redundant server environment. Users and suppliers of data and product files will see little difference in operations but

the system will provide a more secure and stable system for CDDIS operations. The structure of

the VLBI data and product archive remained unchanged in this new system configuration.

The CDDIS staff will continue to work closely with the IVS Coordinating Center staff to ensure

that our system is an active and successful participant in the IVS archiving effort.

178 IVS 2011 Annual Report
NASA Goddard Space Flight Center CDDIS Data Center

Table 2. IVS Data and Product Directory Structure

Directory Description

Data Directories

vlbi/ivsdata/db/yyyy VLBI database files for year yyyy

vlbi/ivsdata/ngs/yyyy VLBI data files in NGS card image format for year

yyyy

vlbi/ivsdata/aux/yyyy/ssssss Auxiliary files for year yyyy and session ssssss; these

files include: log files, wx files, cable files, schedule

files, correlator notes

vlbi/raw Raw VLBI data

Product Directories

vlbi/ivsproducts/crf CRF solutions

vlbi/ivsproducts/eopi EOP-I solutions

vlbi/ivsproducts/eops EOP-S solutions

vlbi/ivsproducts/daily sinex Daily SINEX solutions

vlbi/ivsproducts/int sinex Intensive SINEX solutions

vlbi/ivsproducts/trf TRF solutions

vlbi/ivsproducts/trop Troposphere solutions

Project Directories

vlbi/ivs-iers IVS contributions to the IERS

vlbi/ivs-pilot2000 IVS Analysis Center pilot project (2000)

vlbi/ivs-pilot2001 IVS Analysis Center pilot project (2001)

vlbi/ivs-pilotbl IVS Analysis Center pilot project (baseline)

vlbi/ivs-pilottro IVS Analysis Center pilot project (troposphere)

vlbi/ivs-special IVS special analysis solutions

Other Directories

vlbi/ivscontrol IVS control files (master schedule, etc.)

vlbi/ivsdocuments IVS document files (solution descriptions, etc.)

vlbi/dserver dserver software and incoming files

IVS 2011 Annual Report 179
Italy INAF Data Center Istituto di Radioastronomia–Bologna

Italy INAF Data Center Report

M. Negusini, P. Sarti

Abstract

This report summarizes the activities of the Italian INAF VLBI Data Center. Our Data Center is

located in Bologna, Italy and belongs to the Institute of Radioastronomy, which is part of the National

Institute of Astrophysics.

1. Introduction

The main analysis activity and storage is concentrated in Bologna, where we store and analyze

single databases, using CALC/SOLVE software.

The IRA started to store geodetic VLBI databases in 1989, but the databases archived in

Bologna mostly contain data including European antennas from 1987 onward. In particular most

of the databases available here have VLBI data with at least three European stations. However,

we also store all the databases with the Ny- ̊Alesund antenna observations. In 2002 we decided to

store the complete set of databases available on the IVS data centers, although we limited the time

span to the observations performed from 1999 onwards. All the databases have been processed

and saved with the best selection of parameters for the final arc solutions. In order to perform

global solutions, we have computed and stored the superfiles for all the databases.

In some cases we have introduced GPS-derived wet delays into the European databases (1998

and 1999 EUROPE experiments, for the time being) as if they were produced by a WVR. These

databases are available and stored with a different code from the original databases. In order to

produce these databases, we have modified DBCAL, and this new version is available to external

users.

2. Computer Availability and Routing Access

To date, the main computer is a Linux workstation, on which Mark 5 Calc/Solve version 10

was installed and to which all VLBI data analysis was migrated. The Internet address of this

computer is sarip.ira.inaf.it. Since 2011 a new server with a storage capacity of 5 TB has been

available, and, therefore, all experiments performed in the previous years were downloaded and

archived, thus completing the catalog. The older experiments will be analyzed in order to perform

global long term analysis. At present, the databases are stored in the following directories:

1 = /data2/dbase2

2 = /geo1/dbase1

3 = /geo1/dbase

4 = /geo1/dbase3

The superfiles are stored in:

/data1/super1

The list of superfiles is stored in the file /data2/mk5/save files/SUPCAT. The username for

accessing the databases is geo. The password may be requested by sending an e-mail to negusini@ira.inaf.it.

180 IVS 2011 Annual Report
Kashima Space Research Center, NICT Data Center at NICT

Data Center at NICT

Ryuichi Ichikawa, Mamoru Sekido

Abstract

The Data Center at the National Institute of Information and Communications Technology (NICT)

archives and releases the databases and analysis results processed at the Correlation Center and the

Analysis Center at NICT. Regular VLBI sessions of the Key Stone Project VLBI Network were the

primary objective of the Data Center. These regular sessions continued until the end of November

2001. In addition to the Key Stone Project VLBI sessions, NICT has been conducting geodetic VLBI

sessions for various purposes, and these data are also archived and released by the Data Center.

1. Introduction

The IVS Data Center at National Institute of Information and Communications Technology

(NICT) archives and releases the databases and analysis results processed by the Correlation

Center and the Analysis Center at NICT. Major parts of the data are from the Key Stone Project

(KSP) VLBI sessions [1], but other regional and international VLBI sessions conducted by NICT

are also archived and released. Since routine observations of the KSP network terminated at the

end of November 2001, there have been no additional data from the KSP regular sessions since

2002. In 2009 and 2010, a series of geodetic VLBI sessions were carried out by using the Kashima

34-m, Kashima 11-m, and Koganei 11-m stations to demonstrate precise time comparison. Another

series of astronomical VLBI sessions were carried out between the Kashima 34-m and Koganei 11-

m stations to monitor the flux densities of radio variable stars using real-time e-VLBI data transfer

and processing. In addition, seven geodetic experiments using the two compact VLBI systems with

a 1.6-m antenna were also carried out in 2010 [2]. These data sets are also held by our database

archives.

The analysis results in SINEX (Solution INdependent EXchange) format, as well as in other

formats, are available on the WWW server. Database files of non-KSP sessions, i.e., other domestic

and international geodetic VLBI sessions, are also available on the WWW server. Table 1 lists the

WWW server locations maintained by the NICT Data Center. In the past, an FTP server was

used to provide data files, but it was decided to terminate the FTP service because of the security

risks of maintaining an anonymous FTP server. Instead, the www3.nict.go.jp WWW server was

prepared to provide large size data files.

Table 1. URL of the WWW server systems.

Service URL

KSP WWW pages http://ksp.nict.go.jp/

IVS WWW mirror pages http://ivs.nict.go.jp/mirror/

Database files http://www3.nict.go.jp/aeri/sts/stmg/database/

e-VLBI Sessions http://www2.nict.go.jp/aeri/sts/stmg/research/e-VLBI/UT1/

Hayabusa Sessions http://www2.nict.go.jp/aeri/sts/stmg/research/Navi/HAYABUSA/

The responsibilities for the maintenance of these server machines were moved from the VLBI

IVS 2011 Annual Report 181
Data Center at NICT Kashima Space Research Center, NICT

research group of NICT to the common division for the institutional network service of the laboratory in 2001 to improve the network security of these systems.

2. Data Products

2.1. KSP VLBI Sessions

The KSP VLBI sessions were performed with four KSP IVS Network Stations at Kashima,

Koganei, Miura, and Tateyama on a daily or bi-daily basis until May 1999. The high-speed ATM

(Asynchronous Transfer Mode) network line to the Miura station became unavailable in May

1999, and real-time VLBI observations with the Miura station became impossible. Thereafter,

the real-time VLBI sessions were performed with the three other stations. Once every six days

(every third session), the observed data were recorded to the K4 data recorders at three stations,

and the Miura station participated in the sessions with the tape-based VLBI technique. In this

case, the observed data at the three stations other than the Miura station were processed in realtime, and the analysis results were released promptly after the observations completed. A day

later, the observed tapes were transported from the Kashima, Miura, and Tateyama stations to

the Koganei station for tape-based correlation processing with all six baselines. After the tapebased correlation processing was completed, the data set produced with the real-time VLBI data

processing was replaced by the new data set.

In July 2000, unusual site motion of the Tateyama station was detected from the KSP VLBI

data series, and the frequency of the sessions was increased from bi-daily to daily on July 22, 2000.

The daily sessions were continued until November 11, 2000, and the site motions of the Tateyama

and Miura stations were monitored in detail. During the period, it was found that the Tateyama

station moved about 5 cm in the northeast direction. The Miura station also moved about 3 cm

to the north. The unusual site motions of these two stations gradually settled, and the current

site velocities seem to be almost the same as the site velocities before June 2000. By investigating

the time series of the site positions, the unusual site motion started sometime between the end

of June 2000 and the beginning of July 2000. At the same time, volcanic and seismic activities

near the Miyakejima and Kozushima Islands began. These activities are believed to have caused

the regional crustal deformation in the area, explaining the unusual site motions at Tateyama and

Miura.

2.2. Other VLBI Sessions

In addition to the KSP regular VLBI sessions, domestic and international geodetic and astronomical VLBI sessions were conducted by NICT in cooperation with the Geospatial Information

Authority of Japan (GSI), the National Astronomical Observatory (NAO), and other organizations. These sessions are listed in Table 2. The recent observed data of these sessions were mainly

processed by using the K5 software correlator at NICT either at Koganei or at Kashima or by

using a real-time hardware correlator developed by NAO.

In 2011, the operation time of our 34-m antenna was only 364 hours in total. We repaired and

maintained several parts of the antenna (i.e., repainting of the main dish and rustproofing of the

antenna structure) since the first of January, 2011. The repair was supposed to be finished by the

end of March. However, since the Mw 9.0 megaquake hit our antenna on March 11th, 2011, the

repair was stopped. The repair was restarted in April, and it was finished at the end of June. After

182 IVS 2011 Annual Report
Kashima Space Research Center, NICT Data Center at NICT

Table 2. Geodetic VLBI sessions conducted by NICT (since 2005).

Year exp. names sessions

2005 Geodetic c0505 (CONT05, partial participation),

GEX13

Hayabusa 14 sessions

2006 Geodetic GEX14, viepr2, CARAVAN (3 sessions)

Spacecraft Geotail : 1 session

Pulsar 1 session

2007 Ultra Rapid e-VLBI 15 times, 29 sessions

Time Transfer 4 sessions, 12 days in total

Cs-Gas-Cell 1 session

Spacecraft Hayabusa: 1 session

2008 Ultra Rapid e-VLBI 8 times, 33 sessions

Time Transfer 26 sessions

Variable Star e-VLBI 31 sessions

2009 e-VLBI 15 sessions, 90.5 hours in total

IVS 12 sessions, 332 hours in total

Time Transfer 9 sessions, 72 hours in total

VERA 16 sessions, 149 hours in total

Survey 26 sessions, 276 hours in total

2010 IVS 38 sessions, 442 hours in total

Radio astronomy 34 sessions, 324 hours in total

Spacecraft (IKAROS, UNITEC-1, QZSS) 33 sessions, 259 hours in total

domestic geodetic 13 sessions, 94 hours in total

Time Transfer 9 sessions, 86 hours in total

e-VLBI 9 sessions, 27 hours in total

2011 IVS 2 sessions, 48 hours in total

Radio astronomy 100 hours in total

earthquake damage investigation 216 hours in total

the repair, we investigated the earthquake damage carefully. Unfortunately, the gear reducers, the

power and helium plumbing, the azimuth track wear strips, and one azimuth wheel were damaged.

We are going to fix them as soon as possible in this fiscal year.

3. Staff Members

The Data Center at NICT is operated and maintained by the Space-Time Standards Group at

the Kashima Space Research Center, NICT. The staff members are listed in Table 3.

IVS 2011 Annual Report 183
Data Center at NICT Kashima Space Research Center, NICT

Table 3. Staff members of the Space-Time Measurements Group, KSRC, NICT.

Name Main Responsibilities

ICHIKAWA Ryuichi Frequency and Time Transfer using compact VLBI system

SEKIDO Mamoru Responsible for e-VLBI sessions

HASEGAWA Shingo System Engineer

4. Future Plans

The IVS Data Center at NICT will continue its service and will archive and release the analysis

results accumulated by the Correlation Center and the Analysis Center at NICT. In addition, a

number of VLBI sessions will be conducted for the purposes of various technology developments.

References

[1] Special issue for the Key Stone Project, J. Commun. Res. Lab., Vol. 46, No. 1, March 1999.

[2] Hobiger T., Takiguchi H., Ichikawa R., Sekido M., Koyama Y., and Kondo T., Analysis Center at NICT,

International VLBI Service for Geodesy and Astrometry 2010 Annual Report, pp. 229-232, C2011.

184 IVS 2011 Annual Report
Observatoire de Paris, SYRTE/UMR 8630 Paris Observatory (OPAR) Data Center

Paris Observatory (OPAR) Data Center

Christophe Barache, S ́ebastien Lambert

Abstract

This report summarizes the OPAR Data Center activities in 2011. Included is information about

functions, architecture, status, future plans, and staff members of OPAR Data Center.

1. OPAR Data Center Functions

The Paris Observatory (OPAR) has provided a Data Center for the International VLBI Service

for Geodesy and Astrometry (IVS) since 1999. The OPAR, as well as CDDIS and BKG, is one of

the three IVS Primary Data Centers. Their activities are done in close collaboration for collecting

files (data and analysis files) and making them available to the community as soon as they are

submitted.

The three data centers have a common protocol and each of them:

• has the same directory structure (with the same control file),

• has the same script,

• is able to receive all IVS files (auxilliary, database, products, documents),

• mirrors the other ones every three hours,

• gives free FTP access to the files.

Figure 1. Mirroring among the primary IVS Data Centers.

IVS 2011 Annual Report 185
Paris Observatory (OPAR) Data Center Observatoire de Paris, SYRTE/UMR 8630

This protocol gives the IVS community transparent access to a data center through the same

directory structure and permanent access to files in case of a data center breakdown.

2. Architecture

To be able to put a file into a data center, operational and analysis centers have to be registered

by the IVS Coordinating Center. The file names have to conform to the naming convention.

A script checks the file and puts it into the right directory. The script undergoes permanent

improvement and takes into account the IVS components’ requests.

The structure of IVS Data Centers is:

ivscontrol/ : provides the control files needed by the data center

(session code, station code, solution code...)

ivscontrol_new/ : temporary test directory

ivscontrol_old/ : temporary test directory

ivsdocuments/ : provides documents and descriptions about IVS products

ivsdata/ : provides files related to the observations:

aux/ : auxilliary files (schedule, log...)

db/ : observation files in data-base CALC format

ngs/ : observation files in NGS format

sinex/ : observation files in SINEX format

ivsproducts/ : provides results from Analysis Center:

eopi/ : Earth Orientation Parameters, Intensive sessions

eops/ : Earth Orientation Parameters, 24-hour sessions

crf/ : Celestial Reference Frame

trf/ : Terrestrial Reference Frame

daily_sinex/ : Time series solutions in SINEX format of Earth

orientation and site positions

int_sinex/ : Daily Intensive solution in SINEX format, mainly

designed for combination

trop/ : Tropospheric time series (starting July 2003)

ivs-iers/ : provides products for IERS Annual Report

ivs-pilot2000/ : provides products of 2000 for special investigations

ivs-pilot2001/ : provides products of 2001 for special investigations

ivs-pilottro/ : provides tropospheric time series for Pilot Project

(until June 2003)

ivs-pilotbl/ : provides baseline files

ivs-special/ : specific studies

raw/ : original data (not writable at OPAR Data Center)

3. Current Status

The OPAR Data Center is operated currently on a PC Server (PowerEdge 2800 - Xeron 3.0

GHz) located at Paris Observatory running the Fedora Linux operating system.

To make all IVS products available on-line, the disk storage capacity was significantly increased.

The server is now equipped with a RAID 3-TB disk extensible up to 4.7 TB.

186 IVS 2011 Annual Report
Observatoire de Paris, SYRTE/UMR 8630 Paris Observatory (OPAR) Data Center

Figure 2. Monthly access of the OPAR Data Center during 2011. For each month listed in column 1,

columns 2 through 6 show the number of different visitors, the total number of visits, the number of pages

viewed, the number of hits, and the downloaded bandwidth in Megabytes (Mo) or Gigabytes (Go).

The OPAR server is accessible 24 hours per day, seven days per week through Internet connection with 2Mbit/s rate. Users can get the IVS products by using the FTP protocol. Access to

this server is free for users.

FTP access:

ivsopar.obspm.fr

username: anonymous

password: your e-mail

cd vlbi (IVS directory)

In 2011, 25 different users regularly put and got data on the FTP OPAR ivsincoming. There

were also 3273 distinct users of the Web OPAR server.

4. Future Plans

The OPAR staff will continue to work with the IVS community and closely collaborate with

the two other Primary Data Centers in order to provide public access to all VLBI-related data.

To obtain information about the OPAR Data Center please contact: ivs.opa@obspm.fr

IVS 2011 Annual Report 187

Analysis Centers

Analysis Centers

Sobolev Astronomical Institute of Saint Petersburg University Analysis Center of Saint Petersburg University

Analysis Center of Saint Petersburg University

Dmitriy Trofimov, Veniamin Vityazev

Abstract

This report briefly summarizes the activities of the Analysis Center of Saint Petersburg University

during 2011. Changes which happened, as well as our future plans, are described.

1. Introduction

The Analysis Center of Saint Petersburg University (SPU AC) was established in the Sobolev

Astronomical Institute of the SPb University in 1998. The main activity of the SPU AC for

the International VLBI Service before 2007 consisted of routine processing of 24-hour and 1-hour

observational sessions for obtaining Earth Orientation Parameters (EOP) and rapid UT1-UTC

values, respectively. Due to staff changes in 2007 we had a gap in our submissions to IVS. In 2008

we resumed submitting results of 24-hour session processing. During 2011 the activities of the

SPU AC continued unchanged.

2. Staff

The lecturer in astronomy of Saint Petersburg University, Dmitriy Trofimov, was in charge

of the routine processing of the VLBI observations. General coordination and support for the

activities of the SPU AC at the Astronomical Institute was performed by Prof. Veniamin Vityazev.

3. Activities in 2011

• In 2011 we continued the work resumed in 2008. There were breaks in the work due to

technical reasons. The routine estimation of the five Earth Orientation Parameters was

performed. The OCCAM software package (version 6 2) was used for current processing of

VLBI data [1]. The time series is named spu00004.eops. It includes data obtained by the

IRIS-A, NEOS-A, R1, and R4 observing programs, and it covers 24 years of observations

(from January 2, 1989 until the end of 2011). The total number of processed experiments

is about 1730, of which 90 VLBI sessions were processed in 2011. Our experience and the

equipment of the Analysis Center was used for giving lectures and practical work on the

basics of radio interferometry for the university students. In 2011, with the purpose of giving

students education in practical applications, we published a training manual on modern

astrometry, in which the VLBI technique is considered [2].

In 2011, the work of the SPU AC was supported by the project “Kinematic and Dynamic

Astronomy” (a grant of the President of the Russian Federation for leading scientific schools)

as well as by the project “Acquisition and analysis of time-series in astronomy and the study

of astronomical catalogs” (an SPU grant for fundamental research) and “GLONASS, GPS

and VLBI observations as the basis of astronomical, gravimetric and geodynamic studies”

(an SPU grant for fundamental research).

• All parameters were adjusted using the Kalman filter technique. For all stations (except the

reference station), the wet delay, clock offsets, clock rates, and troposphere gradients were

IVS 2011 Annual Report 191
Analysis Center of Saint Petersburg University Sobolev Astronomical Institute of Saint Petersburg University

estimated. Troposphere wet delay and clock offsets were modeled as a stochastic process

such as a random walk. The clock rates and the troposphere gradients were considered to

be the constant parameters.

• The main details of the preparation of the EOP time series spu00004.eops are summarized

below:

– Data span: 1989.01–2011.12

– CRF: fixed to ICRF-Ext.2

– TRF: VTRF2005 was used as an a priori TRF

– Estimated parameters:

1. EOP: x, y, UT1 − UT C, dψ, dε;

2. troposphere: troposphere gradients were estimated as constant parameters, and wet

troposphere delays were modeled as a random walk process;

3. station clocks were treated as follows: offset as a random walk process, rate as a

constant.

– nutation model: IAU 1980

– mapping function: VMF1

– technique: Kalman filter

– software: OCCAM v.6 2

4. Future Plans

In 2012 we are going to continue our regular processing of the results of the VLBI sessions as well

as giving lectures and the practical work for the students within a special course on radio astrometry

which is included in the systematic curriculum of astronomical education at SPb University.

References

[1] O. Titov, V. Tesmer, J. Boehm, OCCAM v. 6. 0 Software for VLBI Data Analysis, In International

VLBI Service for Geodesy and Astrometry 2004 General Meeting Proceedings, N. R. Vandenberg and

K. D. Baver (eds.), NASA/CP-2004-212255, pp.267-271, 2004.

[2] V.Vityazev, I.Guseva, V.Kiyaev, M.Mishchenko, O. Titov, A.Tsvetkov. Celestial and Terrestrial Coordinates (In Russian), Manual on Astrometry, 301 p., SPb University, 2011.

192 IVS 2011 Annual Report
Geoscience Australia Geoscience Australia Analysis Center

Geoscience Australia Analysis Center

Oleg Titov, Laura Stanford

Abstract

This report gives an overview of the activities of the Geoscience Australia IVS Analysis Center

during 2011.

1. General Information

The Geoscience Australia (GA) IVS Analysis Center is located in Canberra. The Geodesy

group operates as a part of the Mineral and Natural Hazard Division (MNHD).

2. Component Description

Currently the GA IVS Analysis Center contributes nutation offsets, EOP, and EOP rates on a

regular basis for IVS-R1 and IVS-R4 networks and their predecessors (IRIS-A and NEOS-A). The

EOP time series are available for 1983 to 2011. The CRF catalogs using a global set of VLBI data

since 1979 are regularly submitted to the IVS archives.

3. Staff

• Dr. Oleg Titov - project manager

• Dr. Laura Stanford - VLBI scientist

4. Current Status and Activities

Several CRF solutions have been prepared using the OCCAM 6.2 software. The last solution

was uploaded in January 2011. VLBI data comprising 4,109 daily sessions from 25-Nov-1979 to

10-Oct-2011 have been used to compute several global solutions with different sets of reference

radio sources. This includes 5,257,804 observational delays from 2,881 radio sources observed by

60 VLBI stations [1].

Station coordinates were also estimated using NNR and NNT constraints. The long-term time

series of the station coordinates have been established to estimate the corresponding velocities

for each station. The tectonic motion for the Gilcreek VLBI site after the Denali earthquake was

modelled using an exponential function typical of post-seismic deformation [2]. The tectonic motion

of the Tigoconc (2010 year) and Tsukub32 (2011 year) VLBI sites after the strong earthquakes is

currently under study.

The adjustment was made by least squares collocation [3], which considers the clock offsets, wet

troposphere delays, and tropospheric gradients as stochastic parameters with apriori covariance

functions. The gradient covariance functions were estimated from GPS hourly values [4].

A paper on the secular aberration drift has been prepared in collaboration with colleagues

from the IVS Analysis Center of Paris Observatory [5]. A dipole systematic effect, with magnitude

6.4 ± 1.5 μas/yr, was found using the individual proper motions of the 555 reference radio sources

IVS 2011 Annual Report 193
Geoscience Australia Analysis Center Geoscience Australia

with the CALC/SOLVE software. This corresponds to the Galactocentric acceleration of (3.2 ±

0.7) × 10−13 km/s2, in good agreement with the theoretical predictions.

5. Geodetic Activity of the Australian Radio Telescopes

During 2011, three Australian radio telescopes – Hobart26, Hobart12 operated by the University of Tasmania (UTAS) and Parkes, operated by the Australia Telescope National Facility

(ATNF) – started regular geodetic VLBI observations for different IVS programs.

The Parkes 64-meter telescope participated in six geodetic VLBI sessions in 2011 for improvement of the ITRF and the ICRF in the Southern Hemisphere. This program is undertaken in

cooperation with ATNF and UTAS.

6. Optical Spectroscopic Observations of the Reference Radio Sources

A program for optical identification and spectroscopy of the reference radio sources has continued [6]. During 2011, five large optical facilities were used for observing optical spectra of the reference radio sources to determine their red shifts. This list comprises two 8-meter Gemini telescopes

in Chile (projects GS-2011A-Q-89 and GS-2011B-Q-94) and Hawaii (project GN-2011B-Q-109),

a 6-meter telescope in Russia operated by the Special Astrophysical Observatory, a 3.58-meter

New Technology Telescope (NTT) in Chile, operated by the European Space Observatory (project

088.A-0021(A)), and a 2-meter Nordic Optical Telescope (NOT). The goal of this work is to identify the radio sources regularly observed for the geodetic and astrometric VLBI programs. An

international team of scientists participated in this program. A paper describing the new set of

red shifts is in preparation.

During the new five-night observing run, several faint quasars were completely resolved from

the obscuring bright star due to a more stable atmosphere (0905-202, 1123-356, 2300-307). Figures

1 and 2 show a sky field around the 2300-307 source observed at NTT in August 2010 and December

2011. The bright star in the image center in Figure 1 has a size of 4 arcseconds obscuring the

quasar separated by 4 arcseconds from the star. Under better sky conditions the visible disk of

the bright star in the image center has a smaller size in Figure 2 (about 2 arcseconds). Therefore,

the faint quasar in Figure 2 is becoming clearly visible.

7. New Staff Member

Dr Laura Stanford joined the geodetic group of Geoscience Australia in October 2011.

Acknowledgements

Two observers (Oleg Titov from GA and David Jauncey from ATNF) were supported by a

travel grant from the Access to Major Research Facilities Program (AMRFP) to travel to Russia

to the 6-meter telescope in August 2011.

This report has been published with the permission of the CEO, Geoscience Australia.

194 IVS 2011 Annual Report
Geoscience Australia Geoscience Australia Analysis Center

Figure 1. NTT image of the sky field around the quasar 2300-307 made in August 2010 at a visual field of

about 2 arcseconds. The bright star in the image center completely obscures the quasar due to the large

size of the visible disk (4 arcseconds).

Figure 2. NTT image of the sky field around the quasar 2300-307 made in December 2011 at a visual field

of about 0.5 arcseconds. The bright star in the image center has a visible disk two times smaller than in

Figure 1, disclosing the faint quasar (22nd magnitude) separated by 4 arcseconds from the star.

IVS 2011 Annual Report 195
Geoscience Australia Analysis Center Geoscience Australia

References

[1] Titov, O., Systematic effects in the radio source proper motion, in: Proceedings of the 19th European

VLBI for Geodesy and Astrometry Meeting, Bordeaux, G. Bourda, P. Charlot, and A. Collioud (eds.),

14–18, 2009.

[2] Titov, O., P. Tregoning, Post-seismic motion of the Gilcreek geodetic sites following the November,

2002 Denali Earthquake, in: International VLBI Service for Geodesy and Astrometry 2004 General

Meeting Proceedings, NASA/CP–2004-212255, N. R. Vandenberg and K. D. Baver (eds.), 496–500,

2004.

[3] Titov, O., Estimation of subdiurnal tidal terms in UT1-UTC from VLBI data analysis, in: IERS

Technical Notes 28, B. Kolaczek, H. Schuh, and D. Gambis (eds.), 11–14, 2000.

[4] Haas, R., private communication.

[5] Titov, O, S. Lambert, A.-M. Gontier, VLBI measurement of secular aberration drift. AA, 529, A91,

2011.

[6] Titov, O., D. Jauncey, H. Johnston, R. Hunstead and L. Christensen, Optical Spectra of the southern

hemisphere flat-spectrum ICRF radio sources, AJ, 142, 165, 2011.

196 IVS 2011 Annual Report
Laboratoire d’Astrophysique de Bordeaux Bordeaux IVS Analysis Center

Report for 2011 from the Bordeaux IVS Analysis Center

Patrick Charlot, Antoine Bellanger, G ́eraldine Bourda, Arnaud Collioud, Alain Baudry

Abstract

This report summarizes the activities of the Bordeaux IVS Analysis Center during the year 2011.

The work focused on (i) regular analysis of the IVS-R1 and IVS-R4 sessions with the GINS software

package; (ii) systematic VLBI imaging of the RDV sessions and calculation of the corresponding source

structure index and compactness values; (iii) imaging of the sources observed during the 2009 International Year of Astronomy IVS observing session; and (iv) continuation of our VLBI observational

program to identify optically-bright radio sources suitable for the link with the future Gaia frame. Also

of importance is the enhancement of the IVS Live Web site which now comprises all IVS sessions back to

2003, allowing one to search past observations for session-specific information (e.g. sources or stations).

1. General Information

The “Laboratoire d’Astrophysique de Bordeaux” (LAB), formerly Bordeaux Observatory, is

located in Floirac, near Bordeaux, in the southwest of France. It is funded by the University of Bordeaux and the CNRS (“Centre National de la Recherche Scientifique”). VLBI activities are primarily developed within the M2A team (“M ́etrologie de l’espace, Astrodynamique, Astrophysique”).

The contribution of the Bordeaux group to the IVS has been mostly concerned with the maintenance, extension, and improvement of the International Celestial Reference Frame (ICRF). This

includes regular imaging of the ICRF sources and evaluation of their astrometric suitability, as

well as developing specific VLBI observing programs for enhancing the celestial reference frame.

In addition, the group is in charge of the VLBI component in the multi-technique GINS software package [1] as part of a collaborative effort within the French “Groupe de Recherches de

G ́eod ́esie Spatiale” (GRGS) to combine VLBI and space geodetic data (SLR, GPS, DORIS) at the

observation level. This effort also involves space geodesy groups in Toulouse, Grasse, and Paris.

2. Description of the Analysis Center

The Bordeaux IVS group routinely analyzes the weekly IVS-R1 and IVS-R4 sessions with the

GINS software package. During the past year, weekly normal equations for all such sessions in

2011 (with 6-hour EOP resolution) have been produced and integrated in the multi-technique

solutions derived by the GRGS within the framework of the “Combination at the Observation

Level” (COL) Working Group. The CONT08 session was also reanalyzed in the same way. Specific

studies were conducted to compare different analysis strategies for the EOP determination and to

test the impact on the analysis of new stations and of stations displaced by earthquakes. Finally,

a pipeline was developed to characterize the observing sessions in a graphical form.

The group is also focused on imaging the ICRF sources on a regular basis by systematic analysis

of the data from the RDV sessions which are conducted six times a year. This analysis is carried out

with the AIPS and DIFMAP software packages. The aim of such regular imaging is to characterize

the astrometric suitability of the sources based on the so-called “structure index”, and to compare

source structural evolution and positional instabilities. Such studies are essential for identifying

sources of high astrometric quality, for example for the ICRF2 [2] or the future Gaia link.

IVS 2011 Annual Report 197
Bordeaux IVS Analysis Center Laboratoire d’Astrophysique de Bordeaux

3. Scientific Staff

During the past year, there were no changes in the IVS staff. In all, five individuals contributed

to IVS analysis and research activities during 2011. A description of what each person worked on,

along with the time spent on these activities, is given below.

• Patrick Charlot (20%): overall responsibility for Analysis Center work and data processing.

His research interests include the ICRF densification, extension, and link to the Gaia frame,

studies of source structure effects in astrometric VLBI data, and astrophysical interpretation.

• Antoine Bellanger (80%): engineer with background in statistics and computer science. His

tasks are to process VLBI data with GINS and to develop procedures and analysis tools to

automate such processing. He is also the Web master for the M2A group.

• G ́eraldine Bourda (50%): astronomer in charge of developing the VLBI part of GINS and

responsible for the analysis results derived from GINS. She also leads a VLBI observational

program for linking the ICRF and the future Gaia frame.

• Arnaud Collioud (100%): engineer with background in astronomy and interferometry. His

tasks are to image the sources in the RDV sessions using AIPS and DIFMAP, to develop the

Bordeaux VLBI Image Database and IVS Live tool, and to conduct VLBI2010 simulations.

• Alain Baudry (10%): radioastronomy expert with specific interest in radio source imaging

and astrometric VLBI. Professor Emeritus and with a part-time ESO contract.

4. Analysis and Research Activities during 2011

As noted above, a major activity of the Bordeaux group consists of imaging the sources observed

during the RDV sessions on a systematic basis. During 2011, three such sessions were processed

(RDV80, RDV82, and RDV84), resulting in 532 VLBI images at either X or S band for 213 different

sources. The imaging work load has been shared with USNO since 2007 (starting with RDV61):

the USNO group processes the odd-numbered RDV sessions while the Bordeaux group processes

the even-numbered ones. The VLBI images are used in a second stage to derive structure correction

maps and visibility maps along with values for structure indices and source compactness (see [3,

4] for a definition of these quantities) in order to assess astrometric source quality. All such

information is made available through the Bordeaux VLBI Image Database (BVID)1. At present,

the BVID comprises a total of 3181 VLBI images for 1075 different sources (with links to an

additional 7851 VLBI images from the Radio Reference Frame Image Database of USNO at either

S, X, K, or Q band) along with 11,032 structure correction maps and as many visibility maps.

Another major piece of work that took place during the past year was the analysis of the

International Year of Astronomy 2009 (IYA2009) specific IVS session [5] with the aim of imaging

the sources. This session, which was conducted on 18 November 2009, was remarkable in that it

used a 32-station network and observed 243 of the 295 ICRF2 defining sources. Analysis of such

a large data set required modifications of the AIPS software package so that it can handle that

many stations. In all, 232 sources were successfully imaged, a sample of which is shown in Figure 1.

Most of the images show very compact structures, as expected for defining sources. This property

will be assessed in a more quantitative way in the future by calculating source structure indices.

1The BVID may be accessed at http://www.obs.u-bordeaux1.fr/BVID

198 IVS 2011 Annual Report
Laboratoire d’Astrophysique de Bordeaux Bordeaux IVS Analysis Center

Figure 1. VLBI images at X band for six ICRF2 defining sources with declination ranging from −40◦to

+70◦(0133+476, 0420−014, 0657+172, 0716+714, 0727−115, and 1144−379). These sources were observed

during the IYA2009 session organized by IVS on 18 November 2009 with a 32-station VLBI network.

On the observational side, the group leads a project to identify and characterize appropriate

radio sources to align the ICRF and the future Gaia optical frame. To this end, dedicated VLBI

imaging observations of a sample of 395 optically-bright radio sources have been conducted, beginning in 2008 [6, 7]. The last set of sources (75 sources) was observed in March 2011 during a

38-hour long experiment combining 15 stations from the European VLBI Network (EVN) and the

Very Long Baseline Array (VLBA) (as for previous experiments). All data sets have been analyzed,

the results of which will be presented at the upcoming IVS General Meeting. In all, 250 sources

have been successfully imaged, and roughly half of them show the required properties in terms of

astrometric suitability. Additionally, we are examining the ICRF2 to identify those sources that

also meet the criteria for the alignment. Preliminary results indicate that about 200 of them are

in this case [8]. Hence, we anticipate that ultimately there should be more than 300 sources to

align the two frames, a similar number to the number of defining sources in the ICRF2.

5. Dissemination and Outreach

During the past year, the IVS Live Web site [9] was updated on a regular basis and enhanced.

In particular, all IVS sessions back to 2003 have been added to the database. With this addition,

there is now a total of 4,834 IVS sessions available. These sessions involved 63 stations and observed

1,633 sources. As described in [9], IVS Live allows one to monitor IVS sessions in real time and view

IVS 2011 Annual Report 199
Bordeaux IVS Analysis Center Laboratoire d’Astrophysique de Bordeaux

source images but also to search for specific information about sources and stations in past IVS

sessions. Monitoring of the connections showed that there were about 1,500 visits from around the

world during 2011, with at least half of them coming from different individuals. Locally, the Web

site was presented to the public during an open day session at the Observatory on 15 May 2011.

6. Outlook

Our plans for the coming year are focused on moving towards operational analysis of the

IVS-R1 and IVS-R4 sessions with the GINS software package. Additionally, we are considering a

specific analysis for estimating time series of radio source positions. Imaging of the RDV sessions

and evaluation of the astrometric suitability of the sources will continue along the same lines. On

the observational side, dedicated astrometric observations of the ∼125 sources that are deemed

to be suitable for the Gaia link (see Section 4) will be considered. A proposal will be submitted

to the EVN and the VLBA to this end. Furthermore, we plan to make a complete assessment of

all 3,400 ICRF2 sources for the same purpose. The list of targets for the Gaia link will then be

finalized, and we will ask IVS to strengthen observations of these sources. Finally, we will also

prepare plans for monitoring such sources during the Gaia mission, which will be launched the

year after (in 2013).

References

[1] Bourda, G., Charlot, P., Biancale, R.: 2007, GINS: A New Tool for VLBI Geodesy and Astrometry,

18th EVGA Working Meeting, Eds. J. B ̈ohm, A. Pany and H. Schuh, IGG Vienna, p. 59–63.

[2] IERS Technical Note 35: 2009, The Second Realization of the International Celestial Reference Frame

by Very Long Baseline Interferometry, Eds. A. L. Fey, D. Gordon and C. S. Jacobs, Frankfurt am Main:

Verlag des Bundesamts f ̈ur Kartographie und Geod ̈asie, 204 pages.

[3] Fey, A. L., Charlot, P.: 1997, VLBA Observations of Radio Reference Frame Sources. II. Astrometric

Suitability Based on Observed Structure, ApJS, 111, pp.95–142.

[4] Charlot, P.: 2008, Astrophysical Stability of Radio Sources and Implication for the Realization of the

Next ICRF, 5th IVS General Meeting, St Petersburg, Eds. A. Finkelstein and D. Behrend, p. 345–354.

[5] Charlot, P., Bellanger, A., Bourda, G., Collioud, A., Zhang, M., Baudry, A.: 2010, Report for 2009

from the Bordeaux IVS Analysis Center, IVS 2009 Annual Report, Eds. D. Behrend and K. D. Baver,

NASA/TP-2010-215860, p. 213–216.

[6] Charlot, P., Bellanger, A., Bourda, G., Collioud, A., Zhang, M., Baudry, A.: 2009, Bordeaux Observatory Analysis Center Report, IVS 2008 Annual Report, Eds. D. Behrend and K. D. Baver, NASA/TP2009-214183, p 246–249.

[7] Charlot, P., Bellanger, A., Bourda, G., Collioud, A., Zhang, M., Baudry, A.: 2011, Report for 2010

from the Bordeaux IVS Analysis Center, IVS 2010 Annual Report, Eds. D. Behrend and K. D. Baver,

NASA/TP-2011-215880, p. 179–182.

[8] Bourda, G., Charlot, P.: 2011, Plans for an accurate alignment of the VLBI frame and the future Gaia

frame, Journ ́ees Syst`emes de r ́ef ́erence spatio-temporels 2011, Eds. H. Schuh, S. B ̈ohm, T. Nilsson and

N. Capitaine (in press).

[9] Collioud, A.: 2011, IVS Live: All IVS on your deskstop, Proceedings of the 20th Meeting of the

European VLBI Group for Geodesy and Astronomy, Eds. W. Alef, S. Bernhart and A. Nothnagel,

Universit ̈at Bonn, Institut f ̈ur Geod ̈asie und Geoinformation, Schriftenreihe 22, p. 14–18.

200 IVS 2011 Annual Report
BKG and DGFI BKG/DGFI Combination Center

BKG/DGFI Combination Center Annual Report 2011

Sabine Bachmann, Michael L ̈osler, Robert Heinkelmann, Michael Gerstl

Abstract

This report summarizes the activities of the BKG/DGFI Combination Center in 2011 and outlines

the planned activities for the year 2012. The main focus was to stabilize outlier detection and to update

the Web presentation of the combined products.

1. General Information

The BKG/DGFI Combination Center was established in October 2008 as a joint effort of the

Federal Agency for Cartography and Geodesy (Bundesamt f ̈ur Kartographie und Geod ̈asie, BKG)

and the German Geodetic Research Institute (Deutsches Geod ̈atisches Forschungsinstitut, DGFI).

The participating institutions, as well as the tasks and the structure of the IVS Combination

Center, have been described in [5]. The tasks comprise quality control and a timely combination of

the session-based intermediate results of the IVS Analysis Centers into a final combination product

(e.g., Earth Orientation Parameters (EOP)). In coordination with the IVS Analysis Coordinator,

the combination results will be released as official IVS products. The Combination Center is also

expected to contribute to the generation of the official IVS input to any ITRF activities. These

tasks are performed on an operational basis.

2. Component Description

The BKG/DGFI Combination Center performs a combination of session-based results of the

IVS Analysis Centers on an operational basis. The strategy for the combination has been adopted

from the combination process developed and performed by the IVS Analysis Coordinator (cf. [3],

[4]).

At BKG Combination Center (BKG CC) the following tasks are performed:

• Ensuring quality control of the Analysis Center results: checking the format of the results

and their suitability for combination, performing identification and reduction of outliers,

comparing the Analysis Centers’ results with each other, and comparing the results w.r.t.

external time series, e.g. from IERS or IGS.

• Providing feedback to the Analysis Centers: quality control results will be available at the

BKG IVS Combination Center Web page [8].

• Creating high quality combination products and performing timely archiving and distribution: combination products will be created using the DGFI DOGS software package [7].

• Submitting official IVS combination products to the IERS: the produced official IVS combination products will be submitted to the responsible IERS components as requested by the

IERS. This will be supported by the staff of the IERS Central Bureau at BKG.

• Placing final results in IVS Data Centers: final results will be placed in the BKG Data

Center. This will be assisted by the staff of the BKG Data Center in Leipzig.

IVS 2011 Annual Report 201
BKG/DGFI Combination Center BKG and DGFI

• Generating official IVS input to the ITRF: official IVS input to the ITRF will be created as

combined quarterly solutions in SINEX format.

DGFI is in charge of the following Combination Center functions:

• Developing state-of-the-art combination procedures: state-of-the-art combination procedures

will be developed mainly at DGFI. This work, as well as the following item, is also related

to DGFI’s efforts within the IERS WG on the Combination on Observation Level (COL).

• Performing software development and documentation: at DGFI the DOGS software package

will be continuously updated by implementing the developed state-of-the-art combination

procedures.

• Adhering to IERS Conventions: the DGFI DOGS software package is continuously updated

to be in accordance with the IERS Conventions.

3. Staff

In the beginning of 2011 Michael L ̈osler replaced Alexander Lothhammer for the hardware

maintenance and for the maintenance of the IVS combination Web pages at BKG. The list of the

staff members of the BKG/DGFI Combination Center in 2011 is given in Table 1.

Table 1. Staff members of the BKG/DGFI Combination Center.

Name Affiliation Function E-Mail

Michael Gerstl DGFI Software gerstl@dgfi.badw.de

maintenance

Robert Heinkelmann DGFI Combination heinkelmann@dgfi.badw.de

strategies

Sabine Bachmann BKG Combination sabine.bachmann@bkg.bund.de

Michael L ̈osler BKG Hardware/Web site michael.loesler@bkg.bund.de

maintenance

4. Current Status and Activities

The combination of the IVS Rapid EOP series (R1 and R4 sessions), which started in 2009

at BKG, has been continued routinely in 2011. In 2011, six IVS Analysis Centers (BKG, DGFI,

GSFC, IAA, OPA, and USNO) contributed to the IVS combined product (see [4]). Potential new

ACs are AUS, CGS, NMA, and TUW. The rapid solutions contain only R1 and R4 sessions, and

new data points are added twice a week as soon as the SINEX files of at least four IVS Analysis

Centers are available. The results of the combination process are placed in the BKG Data Center

in Leipzig. The combined rapid EOP series, as well as the results of the quality control of the

Analysis Center results, are also available directly at the BKG/DGFI Combination Center Web

page [8] or via the IVS Analysis Coordinator Web site [6]. The inclusion of new Analysis Centers

has continued, and new Web-based analysis possibilities of combined products have been made

available.

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BKG and DGFI BKG/DGFI Combination Center

5. Plans for 2012

In 2012 the work of the BKG/DGFI Combination Center will focus on the following:

• Including three new Analysis Center solutions: one based on the GEOSAT software and provided by Halfdan Pascal Kierulf from the Geodetic Institute, Norwegian Mapping Authority

(NMA), Hønefoss, Norway; another one based on the OCCAM software and provided by

Oleg Titov from Geoscience Australia (AUS), Canberra, Australia; and a third one based

on VieVS (Vienna VLBI Software) provided by the Vienna VLBI Group from the Technical

University of Vienna, Austria.

• Inclusion of source coordinates in the routine combination process as soon as enough Analysis

Centers provide source parameters in their SINEX files.

• Extending the Web-based data analysis feature on the IVS Combination Center Web pages

([8]).

• Providing more products and information resulting from the combination process.

References

[1] Heinkelmann, R., B ̈ohm J., Bolotin S., Engelhardt G., Haas R., Lanotte R., MacMillan D.S.,

Negusini M., Skurikhina E., Titov O., Schuh H., VLBI-derived troposphere parameters during

CONT08, J Geod, SI CONT08, submitted.

[2] Kutterer, H., Kr ̈ugel M., Tesmer V., Towards an improved assessment of the quality of terrestrial reference frames, in: Drewes H. (ed.) Geodetic Reference Frames, IAG Symposia 143, doi:

10.1007/978-3-642-00860-3 10, Springer-Verlag Berlin Heidelberg, 2009.

[3] Nothnagel, A., B ̈ockmann, S., Artz, T., Analysis Coordinator Report, in: International VLBI

Service for Geodesy and Astrometry 2007 Annual Report, NASA/TP-2008-214162, D. Behrend

and K. D. Baver (eds.), 16–17, 2008.

[4] Nothnagel, A., B ̈ockmann, S., Artz, T., Analysis Coordinator Report, in: International VLBI

Service for Geodesy and Astrometry Annual Report 2009, NASA/TP-2010-215860, D. Behrend

and K. D. Baver (eds.), 45–47, 2010.

[5] Schwegmann, W., Gerstl, M., Heinkelmann, R., BKG/DGFI Combination Center Annual Report 2008, in: International VLBI Service for Geodesy and Astrometry Annual Report 2008,

NASA/TP-2009-214183, D. Behrend and K. D. Baver (eds.), 250–252, 2009.

[6] http://vlbi.geod.uni-bonn.de/IVS-AC/index.html

BKG/DGFI Combination Center results at Analysis Coordinator’s Web page.

[7] http://ilrs.dgfi.badw.de/fileadmin/dogs/cs manual.ps

DOGS CS software manual (German version only).

[8] http://ida.bkg.bund.de/IVS/

BKG Combination Center Web page.

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Matera CGS VLBI Analysis Center Centro di Geodesia Spaziale (CGS) - e-geos SpA

Matera CGS VLBI Analysis Center

Roberto Lanotte

Abstract

This paper reports the VLBI data analysis activities at the Space Geodesy Center (CGS), Matera,

from January 2011 through December 2011 and the contributions that the CGS intends to provide for

the future as an IVS Analysis Center.

1. General Information

The Matera VLBI station became operational at the Space Geodesy Center (CGS) of the Italian

Space Agency (ASI) in May 1990. Since then, it has been active in the framework of the most

important international programs. The CGS, operated by e-geos (a Telespazio/ASI company)

on behalf of ASI, provides full scientific and operational support using the main space geodetic

techniques: VLBI, SLR, and GPS.

2. Staff at CGS contributing to the IVS Analysis Center

- Dr. Giuseppe Bianco, responsible for CGS/ASI (primary scientific/technical contact).

- Dr. Rosa Pacione, responsible for scientific activities, e-geos.

- Dr. Roberto Lanotte, geodynamics data analyst, e-geos.

3. Current Status and Activities

3.1. Global VLBI Solution cgs2010a

The main VLBI data analysis activities at the CGS in the year 2011 were directed towards

the realization of a global VLBI solution, named cgs2010a, using the CALC/SOLVE software

(developed at GSFC). The solution activities, started at the end of 2010, ended in March 2011,

when the solution sections (crf, trf, and eop) were published in the IVS archives. The main, final,

characteristics of this solution are:

• Data span:

1979.08.03 - 2010.12.29 (3924 sessions)

• Estimated Parameters:

– Celestial Frame:

Right ascension and declination as global parameters for 839 sources

– Terrestrial Frame:

Coordinates and velocities for 81 stations as global parameters

– Earth Orientation:

Unconstrained X pole, Y pole, UT1, Xp rate, Yp rate, UT1 rate, dpsi and deps.

204 IVS 2011 Annual Report
Centro di Geodesia Spaziale (CGS) - e-geos SpA Matera CGS VLBI Analysis Center

3.2. IVS Tropospheric Products

Regular submission of tropospheric parameters (wet and total zenith path delays, and east

and north horizontal gradients) for all VLBI stations observing in the IVS R1 and R4 sessions

continued during 2011. At present 1056 sessions have been analyzed and submitted, covering the

period from 2002 to 2011. The results are available at the IVS products ftp site.

3.3. IVS Product “Time Series of Baseline Lengths”

Regular submission of station coordinate estimates, in SINEX files, continued during 2011 for

the IVS product “Time Series of Baseline Lengths”. This is composed of 3693 sessions, from 1979

to 2011.

3.4. CGS Contribution to IERS EOP Operational Series

Since 2008, CGS has been delivering IERS R1 and R4 session EOP estimates as a regular

contribution to the IERS EOP operational series. The whole cgs2007a solution, available when

the contribution started, has been delivered to IERS as a reference series updated by the periodic

EOP solution submission.

4. Future Plans

• Continue and improve the realization of our global VLBI solution, providing its regular

update on time.

• Continue to participate in IVS analysis projects, providing the datum-free normal equations.

IVS 2011 Annual Report 205
DGFI Analysis Center DGFI, Deutsches Geod ̈atisches Forschungsinstitut

DGFI Analysis Center Annual Report 2011

Robert Heinkelmann, Michael Gerstl, Julian Andres Mora-Diaz, Manuela Seitz

Abstract

This report summarizes the activities of the DGFI Analysis Center in 2011 and outlines the planned

activities for 2012.

1. General Information and Component Description

The German Geodetic Research Institute (Deutsches Geod ̈atisches Forschungsinstitut, DGFI,

http://www.dgfi.badw.de) is an autonomous and independent research institute hosted at the

Bavarian Academy of Sciences (BAdW), Munich. It is run by the Free State of Bavaria. The research covers all fields of geodesy and includes participation in national and international projects

as well as functions in international bodies. Since October 2010 the scientific geodetic institutions in

Munich and Bavaria — namely the Institute of Astronomical and Physical Geodesy (IAPG) and the

Forschungseinrichtung Satellitengeod ̈asie (FESG) including the personnel at the Geodetic Observatory Wettzell (both at Technical University Munich (TUM)), the Bayerische Kommission f ̈ur die internationale Erdmessung (BEK) and the Deutsches Geod ̈atisches Forschungsinsitut of the Deutsche

Geod ̈atische Kommission (both at the Bavarian Academy of Sciences) — have worked together in

a cooperation called Center for Geodetic Earth system research (Centrum f ̈ur Geod ̈atische Erdsystemforschung, CGE; http://www.iapg.bv.tum.de/2791632- -∼iapg∼forschung∼boards∼cge.html).

In 2011 the BEK and the Kommission f ̈ur Glaziologie together founded the Kommission f ̈ur

Erdmessung und Glaziologie (KEG), while the geodetic part of this commission remains a part of

CGE.

2. Staff

The DGFI IVS AC (http://www.dgfi.badw.de/index.php?id=126&L=2) is operated by Robert

Heinkelmann and Manuela Seitz. In addition, Michael Gerstl works on development and numerical optimizations of the VLBI analysis software DOGS-RI (Radio Interferometry). Julian Andres

Mora-Diaz (Figure 1) joined our VLBI group in March 2011. With his background (BSc in Physics,

MSc in Astronomy), he is most of all interested in AGNs, astrometry, geodetic VLBI, and astrophysics. We are happy to welcome him onboard.

Figure 1. Our new team member: Julian Andres Mora-Diaz.

206 IVS 2011 Annual Report
DGFI, Deutsches Geod ̈atisches Forschungsinstitut DGFI Analysis Center

3. Current Status and Activities

• Rearrangement of the VLBI software used and developed at DGFI

The VLBI analysis software used at DGFI is currently rearranged and will be part of the

DGFI Orbit and Geodetic Parameter Estimation Software DOGS (Heinkelmann and Gerstl,

2010), named DOGS-RI (Radio Interferometry).

• IVS Operational Analysis Center at DGFI

DGFI routinely processes the standard IVS sessions (currently the two IVS rapid turnaround

sessions IVS-R1 and -R4) and additional sessions of the geodetic and astrometric program

run by IVS and delivers datum free normal equations in SINEX format. For the operational

analysis and for the preparation of normal equations in SINEX format, OCCAM and DOGSCS are used. The operational processes now completely run on DGFI-owned hardware under

the Linux OS.

• Atmosphere research

In 2011 our main scientific work focussed on the atmosphere: we found very good agreement

of VLBI VTEC with other space geodetic techniques during CONT08 (Dettmering et al.,

2011a) and included VLBI-derived VTEC into a regional multi-level model over the South

American continent (Dettmering et al., 2011b). The tropospheric estimates during CONT08

were compared among the techniques (Teke et al., 2011), and some new insights and conclusions could be drawn from intra-technique comparison and combination (Heinkelmann et

al., 2011).

4. Future Plans

At DGFI IVS AC we want to continue our investigations concerning the atmosphere. The new

VLBI analysis software DOGS-RI and DGFI’s OCCAM version will be developed in parallel for a

while. In 2012 we plan to switch all VLBI analysis to DOGS-RI.

References

[1] Dettmering D., R. Heinkelmann, and M. Schmidt: Systematic differences between VTEC obtained by

different space-geodetic techniques during CONT08, J Geod, DOI 10.1007/s00190-011-0473-z, 2011a

[2] Dettmering D., M. Schmidt, R. Heinkelmann, and M. Seitz: Combination of different space-geodetic

observations for regional ionosphere modeling, J Geod, DOI 10.1007/s00190-010-0423-1, 2011b

[3] Heinkelmann R. & M. Gerstl: OCCAM - LSM for Linux: new developments at DGFI (poster). 6th

International VLBI Service for Geodesy and Astrometry General Meeting, 7-13 February 2010, Hobart,

Australia, 2010

[4] Heinkelmann R., J. B ̈ohm, S. Bolotin, G. Engelhardt, R. Haas, R. Lanotte, D. S. MacMillan, M. Negusini, E. Skurikhina, O. Titov, and H. Schuh: VLBI-derived troposphere parameters during CONT08,

J Geod, DOI 10.1007/s00190-011-0459-x, 2011

[5] Teke K., J. B ̈ohm, T. Nilsson, H. Schuh, P. Steigenberger, R. Dach, R. Heinkelmann, P. Willis, R. Haas,

S. Garc ́ia-Espada, T. Hobiger, R. Ichikawa, and S. Shimizu: Multi-technique comparison of troposphere

zenith delays and gradients during CONT08, J Geod, DOI 10.1007/s00190-010-0434-y, 2011

IVS 2011 Annual Report 207
FFI Analysis Center Forsvarets forskningsinstitutt (FFI) (Norwegian Defence Research Establishment)

FFI Analysis Center

Per Helge Andersen

Abstract

This report discusses the current status of the FFI Associate Analysis Center as well as upcoming

changes.

1. Status and Future Changes

The Norwegian Mapping Authority (NMA) and FFI have for the last few years had a close

cooperation in the analysis of space geodetic data using the GEOSAT software. NMA has recently

been given the status of an Associate Analysis Center of IVS (28 October 2010). The plan is that

FFI will end this formal role in 2012. The future GEOSAT activities at both institutions will be

coordinated by NMA.

All VLBI analysis activities in 2011 have been performed within NMA where Dr. Per Helge

Andersen has been an external contributor paid by NMA. Therefore, the reader should consult the

NMA AAC report for further information.

2. Staff

Dr. Per Helge Andersen - Research Professor of Forsvarets forskningsinstitutt (FFI and NMA).

Dr. Halfdan Pascal Kierulf - Research geodesist of the Norwegian Mapping Authority (NMA).

208 IVS 2011 Annual Report
Bundesamt f ̈ur Kartographie und Geod ̈asie BKG/IGGB Analysis Center

The BKG/IGGB VLBI Analysis Center

Volkmar Thorandt, Axel Nothnagel, Gerald Engelhardt, Dieter Ullrich, Thomas Artz,

Judith Leek, Christoph Holst

Abstract

In 2011, the activities of the BKG/IGGB VLBI Analysis Center, as in previous years, consisted of

routine computations of Earth orientation parameter (EOP) time series and of a number of research

topics in geodetic VLBI. The VLBI group at BKG continued its regular submissions of time series of

tropospheric parameters and the generation of daily SINEX (Solution INdependent EXchange format)

files. Quarterly updated solutions have been computed to produce terrestrial reference frame (TRF)

and celestial reference frame (CRF) realizations. Routine computations of the UT1–UTC Intensive

observations include all sessions of the Kokee–Wettzell and Tsukuba–Wettzell baselines and the networks Kokee–Svetloe–Wettzell and Ny- ̊Alesund–Tsukuba–Wettzell. After a big earthquake on March

11th, 2011 near the Tsukuba station, no IVS products including Tsukuba Intensive observations could

be delivered. At IGGB, the emphasis has been placed on individual research topics.

1. General Information

The BKG/IGGB VLBI Analysis Center has been established jointly by the analysis groups of

the Federal Agency for Cartography and Geodesy (BKG), Leipzig, and the Institute of Geodesy

and Geoinformation of the University of Bonn (IGGB). Both institutions cooperate intensely in the

field of geodetic VLBI. The responsibilities include both data analysis for generating IVS products

and special investigations with the goal of increasing accuracy and reliability. BKG is responsible

for the computation of time series of EOP and tropospheric parameters, for the generation of

SINEX files for 24-hour VLBI sessions and 1-hour Intensive sessions, and for the generation of

quarterly updated global solutions for TRF and CRF realizations. Besides data analysis, the BKG

group is also responsible for writing schedules for the Tsukuba-Wettzell INT2 UT1-UTC observing

sessions. In addition to this, schedules for observing the Kokee-Wettzell baseline on weekends were

made after the Japan earthquake in March 2011. IGGB continues to host the office of the IVS

Analysis Coordinator and carries out special investigations within the technique of geodetic and

astrometric VLBI. Details of the research topics of IGGB are listed in Section 3.

2. Data Analysis at BKG

At BKG, the Mark 5 VLBI data analysis software system Calc/Solve, release 2010.05.21 [3], has

been used for VLBI data processing. It is running on a Linux operating system. As in the previous

releases, the Vienna Mapping Function (VMF1) has been implemented in a separate Solve version.

This modified version was used for all data analysis. The VMF1 data were downloaded daily

from the server of the Vienna University of Technology. Additionally, the technological software

environment for Calc/Solve has been refined to link the Data Center management with the preand post-interactive parts of the EOP series production and to monitor all Analysis and Data

Center activities.

• Processing of correlator output

The BKG group continued the generation of calibrated databases for the sessions correlated at

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the MPIfR/BKG Astro/Geo Correlator at Bonn (e.g., EURO, OHIG, and T2) and submitted

them to the IVS Data Centers.

• Scheduling

BKG continued scheduling the INT2 Intensive sessions, which are observed on the TSUKUBAWETTZELL baseline. Due to the earthquake in Japan on March 11th, 2011, scheduling at

BKG was extended for the INT1 Intensive sessions on the KOKEE-WETTZELL baseline on

weekends. Altogether 153 schedule files were created in 2011.

• BKG EOP time series

The BKG EOP time series bkg00013 was continued. The main features of this solution

were not changed. Nevertheless, slight changes in modeling of the TSUKUB32 station from

globally estimated station coordinates to locally estimated coordinates in all respective sessions were made. Furthermore three new VLBI stations in the southern hemisphere could

be included successfully in data processing.

Each time after the preprocessing of any new VLBI session (correlator output database

version 1), a new global solution with 24-hour sessions since 1984 was computed, and the

EOP time series bkg00013 was extracted including the coordinates of those stations for which

components were estimated for each session. Altogether 4246 sessions were processed. The

main parameter types in this solution are globally estimated station coordinates and velocities

together with radio source positions. The datum definition was realized by applying no-netrotation and no-net-translation conditions for 26 selected station positions and velocities with

respect to VTRF2008a and a no-net-rotation condition for 295 defining sources with respect

to ICRF2. The station coordinates of the telescopes AIRA (Japan), CHICHI10 (Japan),

CTVASTJ (Canada), DSS13 (USA), HOBART12 (Australia), PT REYES (USA), SEST

(Chile), SINTOTU3 (Japan), TIGOCONC (Chile), TSUKUB32 (Japan), WIDE85 3 (USA),

VERAISGK (Japan), VERAMZSW (Japan), and YEBES40M (Spain) were estimated as

local parameters in each session. The three new VLBI stations KATH12M (Australia),

WARK12M (New Zealand), and YARRA12M (Australia) were modeled in the same way.

Regular analysis of the UT1-UTC Intensive time series bkgint09 was continued. Reporting

was extended to also list the a priori UT1-UTC values as well as the stations participating

in each session. The series bkgint09 was generated with fixed TRF (VTRF2008a) and fixed

ICRF2. The a priori EOP were taken from finals USNO series [7]. The estimated parameter types were only UT1-TAI, station clock, and zenith troposphere. Observations of the

two baselines KOKEE-WETTZELL and TSUKUBA-WETTZELL and also of the networks

KOKEE-SVETLOE-WETTZELL and NYALES20-TSUKUBA-WETTZELL were processed

regularly. But no time series of Intensive sessions with station TSUKUBA were delivered

to IVS after the Japan earthquake. The analysis of the INT3 sessions processed at the

Bonn correlator every Monday after transferring the raw observations by e-transfer could

be finished almost always on the same day. Maximal delays of one day appeared because

of problems in data transfer. A total of 3803 UT1 Intensive sessions were analyzed for the

period from 1999.01.01 to 2011.12.31.

• Quarterly updated solutions for submission to IVS

In 2011, one quarterly updated solution was computed for the IVS products TRF and CRF.

There are no differences in the solution strategy compared to the continuously computed

EOP time series bkg00013. The results of the radio source positions were submitted to

210 IVS 2011 Annual Report
Bundesamt f ̈ur Kartographie und Geod ̈asie BKG/IGGB Analysis Center

IVS in IERS format. The TRF solution is available in SINEX format, version 2.1, and

includes station coordinates, station velocities, and radio source coordinates together with

the covariance matrix, information about constraints, and the decomposed normal matrix

and vector.

• Tropospheric parameters

The VLBI group of BKG continued regular submissions of long time series of tropospheric

parameters to the IVS (wet and total zenith delays and horizontal gradients) for all VLBI

sessions since 1984. The tropospheric parameters were extracted from the standard global

solution bkg00013 and transformed into SINEX format.

• Daily SINEX files

The VLBI group of BKG also continued regular submissions of daily SINEX files for all available 24-hour sessions for the IVS combined products and for the IVS time series of baseline

lengths. In addition to the global solutions, independent session solutions were computed

for the station coordinates, radio source coordinates, and EOP parameters including the

X,Y-nutation parameters. The a priori datum for TRF is defined by the VTRF2008a, and

ICRF2 is used for the a priori CRF information.

• SINEX files for Intensive sessions

The parameter types are station coordinates, pole coordinates and their rates, and UT1-TAI

and its rate. But only the normal equations stored in the SINEX files are important for

further intra-technique combination or combination with other space geodetic techniques.

3. Research Topics at IGGB

• Determination of sub-daily tidal ERP models

To overcome deficiencies of the official IERS model for tidal Earth Rotation Parameter (ERP)

variations with periods around one day and below [5], empirical models estimated from

space geodetic techniques might be used. At IGGB, a method based on transformations of

normal equation systems has been developed to estimate such a model [2]. This method has

also been successfully applied to estimate combined sub-daily ERPs from GPS and VLBI

observations [1]. Within this combination no constraints on the ERPs are necessary as

geometric instabilities of the techniques are cross-wise compensated. The final combined

model as published in [1] was distributed to the different services to be validated.

• Automatic scheduling based on Singular Value Decomposition

An automatic scheduling process for VLBI Intensive sessions based on singular value decomposition has been developed [6]. Based on a simple starting configuration, the observations

are selected successively by analyzing the Jacobian matrix. Indicators on the geometry of

the measurement derived from the singular value decomposition are used for the selection

of the sources to be observed with the purpose of improving the dUT1 determination. The

formal errors of dUT1 deduced from the normal equation serve as an assessment criterion of

the scheduling method. The new scheduling method shows promise for improvements of the

dUT1 determination by IVS Intensive observing sessions.

• Gravitational deformation of the Effelsberg radio telescope

Due to gravitation, the main reflector of a radio telescope undergoes a deformation, which

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BKG/IGGB Analysis Center Bundesamt f ̈ur Kartographie und Geod ̈asie

causes a change in focal length depending on the elevation angle of the telescope. In order to

estimate these focal length variations of the 100-m radio telescope at Effelsberg, Germany,

the main reflector was scanned at seven different elevation angles by a laser scanner mounted

near the primary focus. A three-step adjustment procedure based on an alteration of the

orthogonal distance regression and several outlier eliminations is then used to determine the

variations of the elevation-dependent focal lengths [4]. The estimated focal length decreases

by a maximum of 12.6 mm when tilting the reflector from 90◦to 7.5◦elevation angle. The

post-fit discrepancies between the best-fit paraboloid and the reflector’s surface are Gaussian

distributed within the accuracy of the measurements, which supports the assumption of a

homologous deformation of the main reflector.

4. Personnel

Table 1. Personnel at BKG/IGGB Analysis Center

Thomas Artz IGGB +49-228-733563 thomas.artz@uni-bonn.de

Gerald Engelhardt BKG +49-341-5634438 gerald.engelhardt@bkg.bund.de

Christoph Holst IGGB +49-228-733570 holst@igg.uni-bonn.de

Axel Nothnagel IGGB +49-228-733574 nothnagel@uni-bonn.de

Judith Leek IGGB +49-228-733565 judith.leek@igg.uni-bonn.de

Volkmar Thorandt BKG +49-341-5634285 volkmar.thorandt@bkg.bund.de

Dieter Ullrich BKG +49-341-5634328 dieter.ullrich@bkg.bund.de

Reiner Wojdziak BKG +49-341-5634286 reiner.wojdziak@bkg.bund.de

References

[1] T. Artz, L. Bernhard, A. Nothnagel, P. Steigenberger, and S. Tesmer. Methodology for the combination

of sub-daily Earth rotation from GPS and VLBI observations. J Geod, 86(3):565 – 585, 2012.

[2] T. Artz, S. Tesmer, and A. Nothnagel. Assessment of Periodic Sub-diurnal Earth Orientation Parameter Variations at Tidal Frequencies via Transformation of VLBI Normal Equation Systems. J Geod,

85(9):221 – 239, 2011.

[3] GSFC, NASA (2010): Release of Mark 5 VLBI Analysis Software Calc/Solve from May 21, 2010 (Web

reference: http://gemini.gsfc.nasa.gov/solve).

[4] C. Holst, P. Zeimetz, A. Nothnagel, W. Schauerte, and H. Kuhlmann. Estimation of Focal Length

Variations of a 100 m Radio Telescope’s Main Reflector by Laser Scanner Measurements. Journal of

Surveying Engineering, 2012 (accepted)

[5] G. Petit and B. Luzum. IERS Conventions 2010. IERS Technical Note 35, Verlag des Bundesamtes

f ̈ur Kartographie und Geod ̈asie, Frankfurt am Main, July 2010. ISSN: 1019-4568, in print (available

electronically at http://www.iers.org/IERS/EN/Publications/TechnicalNotes/tn36.html).

[6] J. Pietzner and A. Nothnagel. Geodetic VLBI Intensive Scheduling based on Singular Value Decomposition. In W. Alef, S. Bernhart, and A. Nothnagel (eds), Proceedings of the 20th European VLBI for

Geodesy and Astrometry Working Meeting, pages 9 – 13. Schriftenreihe des Instituts f ̈ur Geod ̈asie und

Geoinformation der Rheinischen-Friedrich-Wilhelms Universit ̈at Bonn, No. 22

[7] USNO (2011): Earth orientation parameters series from finals USNO series 2011, (Web reference:

http://gemini.gsfc.nasa.gov/500/oper/solve apriori files/usno finals.erp).

212 IVS 2011 Annual Report
NASA Goddard Space Flight Center GSFC Analysis Center

GSFC VLBI Analysis Center

David Gordon, Chopo Ma, Dan MacMillan, John Gipson, Karen Baver, Sergei Bolotin,

Karine Le Bail, Johanna Juhl, David Eriksson

Abstract

This report presents the activities of the GSFC VLBI Analysis Center during 2011. The GSFC

VLBI Analysis Center analyzes all IVS sessions, makes regular IVS submissions of data and analysis

products, and performs research and software development aimed at improving the VLBI technique.

1. Introduction

The GSFC VLBI Analysis Center is located at NASA’s Goddard Space Flight Center in Greenbelt, Maryland. It is part of a larger VLBI group which also includes the IVS Coordinating Center,

the CORE Operation Center, a Technology Development Center, and a Network Station. The

Analysis Center participates in all phases of geodetic and astrometric VLBI analysis, software development, and research. We maintain a Web site at http://lupus.gsfc.nasa.gov. We also provide

a pressure loading service to the geodetic community at http://gemini.gsfc.nasa.gov/results/aplo.

Figure 1. Members of the GSFC VLBI Analysis Center.

2. Activities

2.1. Analysis Activities

The GSFC VLBI Analysis Center analyzes all IVS sessions, using the Calc/Solve system, and

performs the fringe fitting and Calc/Solve analysis of the VLBA-correlated RDV sessions. The

group submits the analyzed databases to IVS for all R1, RDV, R&D, APSG, CONT11, INT01,

and INT03 sessions. During 2011, GSFC analyzed 153 24-hour (52 R1, 49 R4, 5 CONT11, 6 RDV,

5 R&D, 6 EURO, 7 T2, 3 APSG, 3 OHIG, 3 CRF, 3 CRDS, 1 AUST, 4 JADE, and 6 JAXA)

sessions, and 406 1-hour UT1 (280 INT01, 88 INT02, and 38 INT03) sessions, and we submitted

IVS 2011 Annual Report 213
GSFC Analysis Center NASA Goddard Space Flight Center

updated EOP and daily Sinex files to IVS immediately following analysis. Two updates were made

in 2011 of our 24-hr and Intensive EOP series. Also, as part of the RDV program, we observed 24

requested sources for the astronomical community.

2.2. Research Activities

• Intensive Scheduling: We continued studying the alternative INT01 scheduling strategy that

we proposed in 2009 and tested in several 2009 and 2010 R&D sessions. This strategy consists

of using all mutually visible geodetic sources, and it is now called the Uniform Sky Strategy

(USS). It was used in INT01 sessions on alternating days continuously since Dec. 2010. An

analysis of the first five months showed that while it improves the sky coverage, it also yields

higher UT1 formal errors and session fits, indicating a need for further analysis. With the

first full year of continuous data now available, we will begin this analysis in early 2012.

• Fourfit Processing of RDV Sessions: A transition from AIPS post-correlation processing

of RDV sessions to Fourfit processing was begun. An RDV session was fourfit processed

at both Haystack and USNO and was compared to an AIPS version. The fourfit processing was shown to result in greater sensitivity, better detection of weak sources, and fewer

subambiguity errors. All new RDVs will now be fourfit processed at GSFC.

• Meteorological Data Analysis: The geodetic VLBI data set is known to have many cases of

missing, biased, and inaccurate meteorological data that impacts the quality of the VLBI

processing. We developed statistical tools to detect bad and missing met data, and we

compared the met data to other sources. To homogenize the met data, we used pressure and

temperature time series derived from the ECMWF model, interpolated and extrapolated

to the VLBI stations. For this purpose, we modified Solve to allow use of an external

meteorological time series. Use of our ECMWF derived time series instead of the database

met values showed noticeable improvements in the solutions. We also implemented an option

that uses a time lag in the thermal deformation model that can be chosen by the user.

• Analysis of LOD Time Series with the SSA: We studied the length-of-day time series derived

from the GSFC 2011a solution with the Singular Spectrum Analysis (SSA) tool. This allowed

us to extract different significant components and to compare them with the Multivariate

ENSO Index (MEI). We first studied the time series with the long-term tendency removed.

The time-varying amplitudes of the annual and semi-annual components, as well as a secondary tendency extracted by the SSA, show a very strong correlation with the MEI time

series. In a second study, we removed the long-term tendency, and annual and semi-annual

signals at constant amplitude with time. A correlation study of the principal component of

the remaining signal of the LOD with the MEI showed that they correlate strongly with each

other for a time delay of 31 days, which is in agreement with other studies.

• Source Monitoring: Together with USNO we continued our program of monitoring all ICRF2

defining sources. Our goal is to observe geodetic sources at least 12 times and non-geodetic

sources at least 3 times during a 12 month period. The R1, R4, and RDV sessions participate

in the monitoring program.

• VLBI2010 Systematic Errors: We investigated the level of error of VLBI2010 geodetic measurements by simulating the effect of tropospheric turbulence, clock error, observation noise,

hydrostatic troposphere mapping function error, antenna gravitational deformation, and site

214 IVS 2011 Annual Report
NASA Goddard Space Flight Center GSFC Analysis Center

pressure error. Biases at the 1-2 mm level in vertical site position estimates can be caused

by troposphere mapping function error, gravitational antenna deformation, or site pressure

errors. Errors due to tropospheric turbulence decrease with latitude, leading to 1-3 mm RMS

site vertical error but no significant bias. Given the precision and stability of high quality

meteorological sensors, vertical bias errors due to pressure (used to compute hydrostatic delay) and temperature (used to compute antenna thermal deformation) errors should be much

less than 1 mm.

• Tsukuba Postseismic Motion: The observed motion of the TSUKUB32 antenna after the

Tohoku earthquake was nonlinear following a coseismic displacement of about 700 mm, primarily in the eastward direction. Six months after the earthquake, the eastward displacement

rate was about 15 cm/yr greater than the long term rate before the earthquake. Analysis of

the single baseline Tsukuba-Wettzell Intensive sessions requires very accurate site positions

since they cannot be estimated along with UT1. We used GPS post-earthquake positions

from the co-located GPS antenna TSKB to correct the TSUKUB32 positions after the earthquake. After correction, the Tsukuba-Wettzell and Kokee-Wettzell UT1 estimates agree with

the USNO UT1 combination solution with the same level of WRMS and bias error.

• Hydrology Loading: Continental hydrology loading causes peak-to-peak vertical site displacements of 3-8 mm that are strongly seasonal. We have computed the hydrological loading

using both the GSFC GLDAS hydrology model data and GRACE data. Applying either

loading series in Calc/Solve analysis reduces the UEN site position and baseline length scatter. We are working on starting a hydrology loading service to provide site loading series to

the VLBI user community.

• Astronomical Source Catalog and Source Time Series: A new astronomical source catalog,

gsf2011a astro, was generated. This catalog contains positions of 3671 total sources, of which

3522 are X/S sources, 123 are X/GPS-ionosphere sources, and 26 are X-only sources. A new

source time series, gsf2011a ts, was also generated. It contains single session positions of

1366 sources in the ICRF2 time series format. Both files will be updated regularly and are

available at http://lupus.gsfc.nasa.gov/dataresults main.htm.

2.3. Software Development

The GSFC VLBI Analysis Center develops and maintains the Calc/Solve analysis system, a

package of approximately 120 programs and 1.2 million lines of code. A new version of Calc/Solve

was released in April 2011.

Also, we continued refining the new data structure which stores VLBI data in netCDF files

organized by an ASCII ‘wrapper’ file. We wrote software to convert from the Mark III database

format into this new format. The software converts around 80% of the data included in a database,

including all of the data currently contained in NGS cards. We are in the process of modifying

Calc/Solve to use this new format and successfully ran a large global solution, producing results

essentially identical to the standard processing.

We also continued work on a new software system. A replacement for the interactive part

of Solve, νSolve, is being developed using C++. νSolve is currently able to read in a pair of

X/S databases, resolve ambiguities, deal with clock breaks, evaluate ionospheric corrections, and

edit outliers. It performs analysis of VLBI sessions using the Square Root Information Filter

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GSFC Analysis Center NASA Goddard Space Flight Center

and can treat estimated parameters as local (one value for a session), arc (multiple values for a

session), piece-wise linear, and stochastic. It can write out a processed session in Mark III database

format and can work either in a standalone mode or interacting with the Mark III catalog system.

Currently we are making comparisons of νSolve and Solve analysis. We expect to make the first

public release of this software in early 2012.

3. Staff

The Analysis Center staff consists of one GSFC civil servant, Dr. Chopo Ma, six NVI Inc.

employees who work under contract to GSFC, and two student interns from Chalmers University of Technology. Dr. Ma oversees the GSFC VLBI project for GSFC and is also the IVS

co-representative to the IERS and the current chair of the IERS Directing Board. Dr. John Gipson is the GSFC VLBI Project Manager and also the chair of IVS Working Group 4 on VLBI Data

Structures. Table 1 lists the staff members and their main areas of activity.

Table 1. Staff members and their main areas of activity.

Ms. Karen Baver Intensive analysis, monitoring, and improvement; software development; Web site development; quarterly nuvel updates.

Dr. Sergei Bolotin Database analysis, νSolve development.

Dr. John Gipson Source monitoring, high frequency EOP, parameter estimation, new

data structure, station dependent noise.

Dr. David Gordon Database analysis, RDV analysis, ICRF2 and astronomical catalogs,

K/Q reference frame, Calc development, quarterly ITRF updates.

Dr. Karine Le Bail Time series statistical analysis (EOP, nutation, source positions),

database meteorological data analysis.

Dr. Chopo Ma ICRF2, CRF/TRF/EOP, K/Q reference frame.

Dr. Daniel MacMillan CRF/TRF/EOP, mass loading, antenna deformation, apparent

proper motion, VLBI2010 simulations, VLBI/SLR/GPS combinations.

Ms. Johanna Juhl Meteorological data analysis, ray tracing.

Mr. David Eriksson Hydrology loading, topographic errors in pressure loading.

4. Future Plans

Plans for the next year include: ICRF2 maintenance, astronomical catalog expansion, participation in VLBI2010 development, continued development of the new VLBI data structure and the

new analysis software, upgrade of program Calc, creation of a hydrology loading service, creation of

a pressure and temperature service using ECMWF data, and further research aimed at improving

the VLBI technique.

216 IVS 2011 Annual Report
Institute of Applied Astronomy of Russian Academy of Sciences (IAA) IAA Analysis Center

IAA VLBI Analysis Center Report 2011

Elena Skurikhina, Sergey Kurdubov, Vadim Gubanov

Abstract

This report presents an overview of IAA VLBI Analysis Center activities during 2011 and the plans

for the coming year.

1. General Information

The IAA IVS Analysis Center (IAA AC) is located at the Institute of Applied Astronomy

of the Russian Academy of Sciences in St. Petersburg, Russia. The IAA AC contributes to IVS

products, such as daily SINEX files, TRF, CRF, rapid and long-term series of EOP, baseline

lengths, and tropospheric parameters. EOP, UT1, and station positions were estimated from

domestic observation programs Ru-E and Ru-U. The IAA AC generates NGS files.

2. Component Description

The IAA AC performs data processing of all kinds of VLBI observation sessions. For VLBI

data analysis we use the QUASAR and the OCCAM/GROSS software packages. All reductions

are performed in agreement with IERS Conventions (2010). Both packages use NGS files as input

data.

The IAA AC submits to the IVS Data Center all kinds of products: daily SINEX files for

EOP and EOP-rates and station position estimates, TRF, CRF, baseline length, and tropospheric

parameters.

The QUASAR and the OCCAM/GROSS software packages are supported and developed.

IVS NGS files are generated in automatic mode on a regular basis.

3. Staff

– Vadim Gubanov, Prof.: development of the QUASAR software and development of the

methods of stochastic parameter estimation.

– Sergey Kurdubov, Dr.: scientific researcher: development of the QUASAR software, global

solution, and DSNX file calculation.

– Elena Skurikhina, Dr.: team coordinator, VLBI data processing, and OCCAM/GROSS

software development.

4. Current Status and Activities

• Software Development for VLBI Processing

The QUASAR software is capable of calculating all types of IVS products. A new release of

the QUASAR software was developed in 2011 by S. Kurdubov with the ability to estimate a

generous amount of new parameters (tidal waves, for example).

• Routine Analysis

IVS 2011 Annual Report 217
IAA Analysis Center Institute of Applied Astronomy of Russian Academy of Sciences (IAA)

During 2011 the IAA AC continued to submit daily SINEX files for the IVS-R1 and IVS-R4

sessions as rapid solution (iaa2010a.snx) and SINEX files based on all 24-hour experiments

for the quarterly solution.

A new global solution was calculated.

The routine data processing was performed with the OCCAM/GROSS software using a

Kalman Filter. The IAA AC operationally processed the “24h” and Intensive VLBI sessions

and submitted the results to the IERS and IVS on a regular basis. Processing of the Intensive sessions is fully automated. The EOP series iaa2007a.eops and iaa2005a.eopi, baseline

lengths iaa2007a.bl, and troposphere parameters iaa2007a.trl were continued. Long-time series of station coordinates, baseline lengths, and tropospheric parameters (ZTD, gradients)

were computed with the station position catalog ITRF2005.

• EOP Parameter Calculation from Domestic QUASAR Network Observations

Regular determinations of Earth orientation parameters with the QUASAR VLBI Network

Svetloe-Zelenchukskaya-Badary and single baseline 1-hour observations for UT1 with e-VLBI

transfer were performed weekly. Correlation is performed at the IAA correlator ARC. For

2011 the mean RMS EOP deviations from the IERS 08 C04 series in the Ru-E program

were 1.0 mas for Pole position, 35 μs for UT1-UTC, and 0.37 mas for Celestial Pole position

for 38 Ru-E sessions. The RMS deviation of the Universal Time values from the IERS C04

series for 58 sessions of the Ru-U program was 53 μs. We used station positions from the

QUASAR global solution in our calculations.

• Tidal Deformation of the Earth from VLBI Data Analysis

In a study by V. S. Gubanov and S. L. Kurdubov, statistically significant corrections to

the parameters of the lunar-solar tides as the complex Love/Shida numbers were obtained

from the analysis of VLBI observations carried out in 1985 – 2010 by international geodetic

programs on global networks. The new nominal (independent of frequency) values of these

parameters (in 10−4) are the following:

– for total tide h

(0) = (6113 ± 3) − (33 ± 2)i, l(0) = (843 ± 1) − (5 ± 2)i,

– for diurnal tides h

(0) = (6106 ± 3) − (10 ± 6)i, l(0) = (843 ± 1) − (8 ± 1)i,

– for semi-diurnal tides h

(0) = (6106 ± 3) − (24 ± 3)i, l(0) = (843 ± 1) + (3 ± 1)i.

The frequency-dependent effects of resonances in the diurnal tides could not be evaluated

because of the existence of close frequencies in their harmonic expansion. In the future, for

this purpose it is proposed to involve positional data GPS-measurements. But for 50 VLBI

stations we have discovered a new effect of the asymmetry of the horizontal tidal displacement

in the direction of tectonic movements of these stations.

• TSUKUBA station position

TSUKUB32 station positions and velocities were estimated. After the Tohoku Earthquake

we estimated the station position and velocity using a linear approach for two time steps;

results are presented in Table 1.

218 IVS 2011 Annual Report
Institute of Applied Astronomy of Russian Academy of Sciences (IAA) IAA Analysis Center

Table 1. Station positions and velocities for TSUKUB32, epoch 2000.0, in ITRF2005.

Time span Station Position, m Velocity, mm/year

(MJD) X Y Z Vx Vy Vz

until 55631 -3957408.757 3310229.3920 3737494.782 -0.0022 0.0049 -.0053

± 0.001 ± 0.001 ± 0.002 ± 0.0002 ± 0.0001 ± 0.0002

55632 -3957405.798 3310231.506 3737495.661 -0.2987 -0.2332 -0.0861

to 55767 ± 0.327 ± 0.292 ± 0.397 ± 0.0287 ± 0.0256 ± 0.0348

55768 -3957408.0631 33310229.231 3737494.3503 -0.1020 -0.0363 0.0266

to present ± 0.117 ± 0.101 ± 0.121 ± 0.0099 ± 0.0085 ± 0.0102

5. Future Plans

• We plan to continue to submit all types of IVS product contributions.

• Continue investigations of VLBI estimation of EOP, station coordinates, and troposphere

parameters, and comparison with satellite techniques.

• Further improve algorithms and software for processing VLBI observations.

References

[1] A. Finkelstein, E. Skurikhina, I. Surkis, A. Ipatov, I. Rahimov, S. Smolentsev, “QUASAR National

Programs of EOP Determinations”, Measuring the future, Proceedings of the Fifth IVS General Meeting,

ed. A. Finkelstein, D. Behrend, St-Petersburg, “Nauka”, 2008, p. 319–323.

[2] A. Finkelstein, A. Salnikov, A. Ipatov, S. Smolentsev, I. Surkis, I. Gayazov, I. Rahimov, A. Dyakov, R.

Sergeev, E. Skurikhina, S. Kurdubov, EOP determination from observations of Russian VLBI-network

QUASAR, in Proceedings of the 20th Meeting of the European VLBI Group for Geodesy and Astronomy,

Ed. by W. Alef, S. Bernhart, A. Nothnagel, 2011, IGG, Germany, p. 49–51.

IVS 2011 Annual Report 219
IGG Analysis Center Institute of Geodesy and Geophysics/University of Technology, Vienna

Vienna IGG Special Analysis Center Annual Report 2011

Harald Schuh, Johannes B ̈ohm, Sigrid B ̈ohm, Matthias Madzak, Vahab Nafisi,

Tobias Nilsson, Andrea Pany, Lucia Plank, Benedikt Soja, Hana Spicakova, Jing Sun,

Claudia Tierno Ros

Abstract

The main activities of the VLBI group at the Institute of Geodesy and Geophysics (IGG) of the

Vienna University of Technology in 2011 were related to the development of the Vienna VLBI Software

VieVS (http://vievs.hg.tuwien.ac.at/). The number of external VieVS users further increased to about

twenty, and some of them took part in the second VieVS User Workshop which was held at our institute

in September 2011. In the last year, the tools for the VLBI global solutions were further refined

and extended, and investigations on scheduling as well as on spacecraft and satellite tracking have

been intensified. Furthermore, studies on VLBI2010 simulations, Earth rotation, and geodynamical

parameters from VLBI have been continued.

1. General Information

The Institute of Geodesy and Geophysics (IGG) is part of the Faculty of Mathematics and

Geoinformation of the Vienna University of Technology. It is divided into three research units,

one of them focusing on advanced geodesy (mathematical and physical geodesy, space geodesy).

Within this research unit, one group (out of three) is dealing with geodetic VLBI.

Figure 1. Members of the VLBI group participating in the EVGA meeting in Bonn: Hana Spicakova, Tobias

Nilsson, Harald Schuh, Johannes B ̈ohm, Lucia Plank, Jing Sun, and Claudia Tierno Ros in front of the radio

telescope in Effelsberg.

220 IVS 2011 Annual Report
Institute of Geodesy and Geophysics/University of Technology, Vienna IGG Analysis Center

2. Staff

Personnel at IGG associated with the IVS Special Analysis Center in Vienna are Harald Schuh

(Head of IGG, Chair of the IVS Directing Board), and eleven scientific staff members. Their main

research fields are summarized in Table 1.

Table 1. Staff members ordered by their main focus of research.

Johannes B ̈ohm VLBI2010, atmospheric effects

Jing Sun VLBI2010, scheduling of VLBI observations

Tobias Nilsson VLBI2010, turbulence, Earth orientation

Andrea Pany (until 07/2011) VLBI2010, simulation

Sigrid B ̈ohm Earth orientation, tidal influences

Lucia Plank Spacecraft and satellite tracking with VLBI

Benedikt Soja Relativistic effects of solar system bodies

Matthias Madzak Ray-tracing, VieVS graphical user interfaces

Hana Spicakova Global solution, geodynamical parameters

Vahab Nafisi (until 09/2011) Ray-traced delays for VLBI

Claudia Tierno Ros External ionospheric delays

3. Current Status and Activities

• Vienna VLBI Software VieVS

Most of the activities were related to the development of the Vienna VLBI Software (VieVS,

http://vievs.hg.tuwien.ac.at/). For example, tools for the VLBI global solutions were updated in the latest release (Version 1d), and investigations into spacecraft and satellite tracking have been continued. Furthermore, studies on VLBI2010 simulations, scheduling, Earth

rotation, and geodynamical parameters from VLBI were carried out, and the second VieVS

User Workshop was held in September 2011.

• Complex demodulation

By applying the so-called complex demodulation, high-frequency variations in a time series

can be shifted to low frequencies, preserving thereby the original amplitudes. This enables

the estimation of diurnal and subdiurnal variations with merely diurnal parameter sampling.

The features of the complex demodulation were used in an extended parameterization of

polar motion and universal time which was implemented in a dedicated version of VieVS. The

functionality of the approach was evaluated by comparing amplitudes and phases of harmonic

variations at tidal periods (diurnal/semidiurnal) as derived from demodulated Earth rotation

parameters (ERP) to the terms of the conventional model for ocean tidal effects in Earth

rotation (see B ̈ohm et al., 2012 [1]).

• External ionospheric delays in VieVS

A new module that allows the use of external ionospheric delay corrections calculated from

Global Navigation Satellite Systems (GNSS) maps of Total Electron Content (TEC) has been

implemented in VieVS. It has been shown that the use of GNSS TEC maps is certainly useful

IVS 2011 Annual Report 221
IGG Analysis Center Institute of Geodesy and Geophysics/University of Technology, Vienna

in the case of single-frequency VLBI observations or when lacking ionospheric information

due to measurement errors.

• Global solutions with VieVS

VieVS allows a global adjustment of normal equations from single sessions in a separate module called vie glob. It allows the estimation of terrestrial reference frames (station positions

and velocities assuming linear motion of stations), celestial reference frames (source positions) and Earth orientation parameters. We analyzed all 24-hour IVS sessions from 1984.0

to 2011.0 and estimated our new terrestrial and celestial reference frames (VieTRF10a and

VieCRF10a; see Spicakova et al. (2012, [4])). Furthermore, we examined the effect of tropospheric delay modeling on the estimated reference frames (see Figure 2).

−180 ̊ −120 ̊ −60 ̊ 0 ̊ 60 ̊ 120 ̊ 180 ̊

−90 ̊

−45 ̊

0 ̊

45 ̊

90 ̊

−0.2

−0.1

0.0

0.1

0.2

cm

1 mm 

Figure 2. Influence of a priori gradients on station coordinates at epoch 2000.0. In both cases, tropospheric

gradients were estimated as piecewise linear offsets every six hours with 1 mm absolute and 0.5 mm relative

constraints. We show the differences in the sense DAO apriori gradients minus zero a priori gradients.

Horizontal position changes are shown as arrows, vertical changes by color-coded triangles pointing in the

direction of change (from Spicakova et al. (2012, [4]).

• VLBI for space applications

The efforts of implementing the processing of VLBI observations of artificial sources within

the solar system into VieVS have been continued. Same-beam differential VLBI observations of the Japanese lunar mission SELENE were analyzed with VieVS, and the results

were successfully verified by comparison with those obtained by the National Astronomical

Observatory (NAOJ), Mizusawa. Additionally, investigations regarding atmospheric effects,

as well as the estimation of spacecraft coordinates, were performed. More recently the focus

was put on VLBI tracking of satellites orbiting the Earth. This covers delay solutions of

GNSS satellites in single mode, GNSS satellites in differential mode with a close-by quasar,

and studies of simulated GNSS observations with a four station network.

• General relativistic delay in VLBI observations

In terms of the accuracy requirements for the VLBI delay model nowadays and for VLBI2010,

the significance of the relativistic effect due to the major celestial bodies was investigated.

Therefore, the gravitational time delay for the Earth, the Sun, the Moon, and the planets

was calculated for the observational configurations of all R1 and R4 sessions from 2002-2010.

222 IVS 2011 Annual Report
Institute of Geodesy and Geophysics/University of Technology, Vienna IGG Analysis Center

According to our results, besides the Sun and the Earth, we recommend including the effects

of Saturn, the Moon, and possibly also Venus in the delay modeling.

• Scheduling with VieVS

The module vie sched is the part of VieVS which designs the new scheduling algorithms to

fully exploit the possibilities of the future VLBI2010 system. It considers a more uniform

network and fast moving antennas. To support the development of vie sched, it is directly

connected to VieVS to provide feedback on the quality of the schedules by thorough and

realistic simulations (see Sun et al., 2011 [3]).

• Combination with ringlaser

We have combined data from the “G” ring laser gyroscope in Wettzell with VLBI observations

in order to estimate Earth orientation parameters with hourly resolution. The details about

the combination procedure and the results were summarized by Nilsson et al. (2012, [2]).

Since the accuracy of the ring laser currently is about one order of magnitude worse than that

of VLBI, the ring laser data normally do not contribute significantly to the combination, and

the results are not improved compared to using only VLBI data. However, the combination

with ring laser data would significantly improve the results if the accuracy of the ring laser

was higher and/or data from more than one ring laser was used.

4. Future Plans

In 2012 we will continue the development of VieVS, with special focus on spacecraft tracking

and scheduling. Additionally, we will contribute to the ongoing activities within VLBI2010 and

Earth orientation, and reference system studies will be carried out. Other goals are to organize a

third VieVS User Workshop and to equip VieVS with a Kalman filter solution.

Acknowledgements

We are very grateful to the Austrian Science Fund (FWF) for supporting our work by projects

P21049 (‘SCHED2010’), P22203 (‘MDION’) and P23143 (‘Integrated VLBI’). We also acknowledge

the German Research foundation (DFG) for funding project SPEED2 (SCHU 1103/3-2).

References

[1] B ̈ohm, S., Brzezinski, A., Schuh, H., Complex demodulation in VLBI estimation of high frequency

Earth rotation components, Journal of Geodynamics, published online, doi: 10.1016/j.jog.2011.10.002,

2012.

[2] Nilsson, T., B ̈ohm, J., Schuh, H., Schreiber, U., Gebauer, A., Kl ̈ugel, T., Combining VLBI and ringlaser

observations for determination of high frequency earth rotation variation, J. Geodyn., submitted 2012.

[3] Sun, J., Pany, A., Nilsson, T., B ̈ohm, J., Schuh, H., Status and future plans for the VieVS scheduling

package, in: W. Alef, S. Bernhart, A. Nothnagel (eds.) Proceedings of the 20th Meeting of EVGA, pp.

44-48, 2011.

[4] Spicakova, H., B ̈ohm, J., Plank, L., Nilsson, T., Schuh, H., Atmospheric Effects on VLBI-derived

Terrestrial and Celestial Reference Frames, in: P. Willis (ed.) Proceedings of the IAG Symposium

2011, Melbourne, submitted 2012.

IVS 2011 Annual Report 223
Italy INAF Analysis Center Istituto di Radioastronomia–Bologna

Italy INAF Analysis Center Report

M. Negusini, P. Sarti

Abstract

This report summarizes the activity of the Italian INAF VLBI Analysis Center. Our Analysis

Center is located in Bologna, Italy and belongs to the Institute of Radioastronomy, which is part of the

National Institute of Astrophysics. IRA runs the observatories of Medicina and Noto, where two 32-m

VLBI AZ-EL telescopes are situated. This report contains the AC’s VLBI data analysis activities and

shortly outlines the investigations into the co-location of space geodetic instruments.

1. Current Status and Activity

Investigations into VLBI local tie surveying and antenna deformation continued in 2011. The

impact of different contributing effects on the tie vector estimate has been simulated and evaluated.

In particular, different local ground control network geometries, a varying number and distribution

of ground pillars, the impact of the observing scheme adopted during the terrestrial survey, the

impact of the redundancy of observations, the contribution of thermal and gravitational deformations of the space geodetic instrument structure were introduced into the tie vector computation,

and their effects on the tie vector estimate were precisely evaluated [1]. In addition, a thorough

investigation of the local stability of the geodetic monuments at the Medicina site and the determination of local, intra-site motions are currently in process. The starting data sets are those

acquired during the terrestrial surveys of the GPS-VLBI tie vector during the period 2001 - 2010.

The results derived by the analysis of the terrestrial data have been cross-checked against those obtained by the analysis of the GPS data acquired by the two permanent EUREF [2] stations MEDI

and MSEL over the period 2004 - 2010. The results show a non-negligible, statistically significant

motion of the local ground control network pillars, especially in the horizontal components, and

are being summarized in a paper that has been almost finalized and is about to be submitted.

2. Data Analysis and Results

The IRA started to analyze VLBI geodetic databases in 1989, using a CALC/SOLVE package

on the HP1000 at the Medicina station. In subsequent years, the same software was installed

first on an HP360 workstation and later on an HP715/50 workstation. In more recent years,

two HP785/B2600 workstations and an HP282 workstation were used. In 2007, a new Linux

workstation was set up for the migration of all the VLBI data analysis, and Mark 5 Calc/Solve

was installed. During 2011, we stored all the 1999 - 2011 databases available on the IVS Data

Centers. All the databases were processed and saved with the best selection of parameters for the

final arc solutions. The most recent IRA solution for crustal deformation comprises all Europe

sessions analyzed at IRA from 1987 to 2009; the estimated horizontal and vertical velocities are

presented in [3].

Our Analysis Center has participated in the IVS TROP Project on Tropospheric Parameters

since the beginning of the activities. Tropospheric parameters (wet and total zenith delay and

horizontal gradients) of all IVS-R1 and IVS-R4 24-hour VLBI sessions were regularly submitted in

the form of SINEX files. INAF solutions for the CONT08 campaign were used for intra-technique

combination and the results published in [4]. In 2011 we regularly submitted our results to IVS.

224 IVS 2011 Annual Report
Istituto di Radioastronomia–Bologna Italy INAF Analysis Center

3. Outlook

We will continue with the regular submission of INAF tropospheric parameters to the IVS

Data Centers, also studying the impact of the Vienna Mapping Function on the geodetic results.

We will submit a long time series of troposphere parameters using all VLBI sessions available in

our catalog in order to estimate the variations over time of the content of water vapor in the

atmosphere.

References

[1] Abbondanza, C. and Sarti, P. (2012). Impact of network geometry, observation schemes and telescope

structure deformations on local ties: simulations applied to Sardinia Radio Telescope. J Geodesy, doi:

10.1007/s00190-011-0507-6.

[2] Bruyninx, C. (2004). The EUREF Permanent Network; a Multidisciplinary Network Serving Surveyors

as well as Scientists. GEOInformatics 7(5), 32-35.

[3] Sarti, P., M. Negusini, C. Abbondanza. (2010) Improved geodetic European very-long-baseline interferometry solution using models of antenna gravitational deformation. Ann Geophys 53(5-6) doi

10.4401/ag-4739.

[4] Heinkelmann, R., J. Boehm, S. Bolotin, G. Engelhardt, R. Haas, R. Lanotte, D. Macmillan, M. Negusini, E. Skurikhina, O. Titov, H. Schuh. (2011) Vlbi-Derived Troposphere Parameters During Cont08.

J. Geodesy 85(7); 377-393, Issn: 0949-7714, Doi: 10.1007/S00190-011-0459-X

IVS 2011 Annual Report 225
JPL Analysis Center Jet Propulsion Laboratory, California Institute of Technology

JPL VLBI Analysis Center Report for 2011

Chris Jacobs

Abstract

This report describes the activities of the JPL VLBI Analysis Center for the year 2011. We continue

to do celestial reference frame, terrestrial reference frame, earth orientation, and spacecraft navigation

work using the VLBI technique. In 2011 we continued to collect reference frame data at 448 Mbps.

Our work to build a reference at X/Ka-bands (8.4/32 GHz) is close to ppb accuracy. We supported

several missions with VLBI navigation measurements. We continue to study ways to improve spacecraft

tracking using VLBI techniques.

1. General Information

The Jet Propulsion Laboratory (JPL) Analysis Center is in Pasadena, California. Like the rest

of JPL, the center is operated by the California Institute of Technology under contract to NASA.

JPL has done VLBI analysis since about 1970. We focus on spacecraft navigation, including:

1. Celestial Reference Frame (CRF) and Terrestrial Reference Frame (TRF) are efforts which

provide infrastructure to support spacecraft navigation and Earth orientation measurements.

2. Time and Earth Motion Precision Observations (TEMPO) measures Earth orientation parameters based on single baseline semi-monthly measurements. These VLBI measurements

are then combined with daily GPS measurements as well as other sources of Earth orientation

information. The combined product provides Earth orientation for spacecraft navigation.

3. Delta differenced one-way range (∆DOR) is a differential VLBI technique which measures

the angle between a spacecraft and an angularly nearby extragalactic radio source. This

technique thus complements the radial information from spacecraft doppler and range measurements by providing plane-of-sky information for the spacecraft trajectory.

4. ∆VLBI phase referencing uses the VLBA to measure spacecraft positions.

2. Technical Capabilities

The JPL Analysis Center acquires its own data and supplements it with data from other

centers. The data we acquire are taken using NASA’s Deep Space Network (DSN).

1. Antennas: Most of our work uses 34-m antennas located near Goldstone (California, USA),

Madrid (Spain), and Tidbinbilla (Australia). These include the following Deep Space Stations

(DSS): the “High Efficiency” subnet comprised of DSS 15, DSS 45, and DSS 65 (see Figure

1) which has been the most often used set of antennas for VLBI. More recently, we have used

the DSN’s beam waveguide (BWG) antennas: DSS 13, DSS 24, DSS 25, DSS 26, DSS 34,

DSS 54, and DSS 55. Less frequent use is made of the DSN’s 70-m network (DSS 14, DSS

43, DSS 63). Typical X-band system temperatures are 35K on the HEF antennas. The 70-m

and BWGs are about 20K. Antenna efficiencies are typically well above 50% at X-band.

226 IVS 2011 Annual Report
Jet Propulsion Laboratory, California Institute of Technology JPL Analysis Center

Figure 1. The three ‘high-efficiency’ DSN antennas: Goldstone (center); Robledo, Spain (lower left); and

Tidbinbilla, Australia (lower right). These antennas were completed before 1986 for the Voyager Uranus

encounter. In the 1990s, Ka-band (32 GHz) BWG antennas (not shown) were added.

2. Data acquisition: We use the Mark 5A VLBI data acquisition systems. In addition, we

have JPL-unique systems called the VLBI Science Recorder (VSR) and the Wideband VSRs

(WVSR) which have digital baseband converters and record directly to hard disk. The data

are later transferred via network to JPL for processing with our software correlator.

3. Correlators: JPL VLBI Correlator has been exclusively based on the SOFTC software, which

handles the ∆DOR, TEMPO, and CRF correlations as well as tests of antenna arraying.

4. Solution types: We run several different types of solutions. For ∆DOR spacecraft tracking

we make narrow field (≈ 10◦) differential solutions. The TEMPO solutions typically have a

highly constrained terrestrial (TRF) and celestial frame (CRF) as a foundation for estimating

Earth orientation parameters. These reference frames are produced from global solutions

which then provide the framework needed for use by TEMPO and ∆DOR.

3. Staff

Our staff are listed below along with areas of concentration. Note that not all of the staff listed

work on VLBI exclusively, as our group is involved in a number of projects in addition to VLBI.

• Durgadas Bagri: VLBI instrumental calibrations and TEMPO.

• Jim Border: ∆DOR spacecraft tracking.

• Cristina Garcia-Miro: Field support of VLBI experiments at Madrid.

• Shinji Horiuchi: Field support of VLBI experiments at Canberra.

• Chris Jacobs: S/X, K, Q, X/Ka CRFs, and TRF.

IVS 2011 Annual Report 227
JPL Analysis Center Jet Propulsion Laboratory, California Institute of Technology

• Peter Kroger: ∆DOR spacecraft tracking.

• Gabor Lanyi: VLBA phase referencing, ∆DOR, WVR, K-Q CRF, and TRF.

• Steve Lowe: Software correlator, fringe fitting software, ∆DOR.

• Walid Majid: ∆DOR, VLBA phase referencing.

• Chuck Naudet: WVR, Mark 5A support, and K-Q CRF.

• Andres Romero-Wolf: ∆DOR, CRF, and TRF. Maintains MODEST analysis code.

• Lawrence Snedeker: Field support of VLBI experiments at Goldstone.

• Ioana Sotuela: Field support of VLBI experiments and antenna calibration at Madrid.

• Ojars Sovers: S/X, K, Q, and X/Ka CRFs and TRF. Maintains MODEST analysis code.

• Alan Steppe: TEMPO and TRF.

4. Current Status and Activities

X/Ka-band (8.4/32 GHz) CRF work continues along with S/X CRF and TEMPO EOP work.

VLBI spacecraft tracking continues to provide measurements of angular position in support of

mission navigation and planetary ephemeris development. The ESA mission Rosetta was supported

for its deep space maneuver in February. The Messenger spacecraft was guided into orbit about

Mercury in March. Dawn was guided to a rendezvous with asteroid Vesta in May. Delta-DOR

measurements of the Deep Impact spacecraft were taken in conjunction with ranging to verify that

the DSN can uplink a ranging signal from one complex and then receive it at a second complex.

This scenario is needed for later New Horizons support, when the round trip light time will be

so great that a ranging signal transmitted by one complex cannot return before the complex has

rotated out of view. The New Horizons trajectory toward Pluto was verified in June. The JAXA

mission Planet-C was supported during its engine checkout in October – November. Monthly

measurements of MRO and Mars Odyssey continue to improve the ephemeris of Mars. Juno and

MSL were launched in late 2011 and will be heavily supported with Delta-DOR in 2012.

5. Future Plans

In 2012, we hope to improve TEMPO and reference frame VLBI by increasing data rates to 2048

Mbps. Operational Ka-band phase calibrators have been built and are planned for deployment in

2012. Work on the Digital Back End (DBE) continues. Our next generation fringe fitting program

is also expected to come online. We anticipate refereed publications on our X/Ka celestial reference

frame work. On the spacecraft front, we plan to continue supporting a number of operational

missions while further improving techniques for using VLBI for spacecraft tracking.

Acknowledgements

The work described here was in part performed at the Jet Propulsion Laboratory, California

Institute of Technology, under contract with the NASA. Copyright 
c 2012 California Institute of

Technology. Government sponsorship acknowledged. This report is dedicated to Lyle J. Skjerve,

who died in 2011. He supported Goldstone VLBI during four decades. He is missed.

228 IVS 2011 Annual Report
Jet Propulsion Laboratory, California Institute of Technology JPL Analysis Center

References

[1] Bourda, G., P. Charlot, and C. S. Jacobs, ‘Future Radio Reference Frames & Implications for Gaia

Link,’ Proc. ELSA Conf.: Gaia at the Frontiers of Astrometry, Sevres, France, 7–11 June 2010. eds. C.

Turon, F. Meynadier, and F. Arenou, EAS Publications Series, 45 (2010) pp. 377–380, 15 Feb 2011.

http://ftphip.obspm.fr/gaia2010/IMG/pdf/Poster Bourda.pdf

[2] Heflin, M. B., C. S. Jacobs, O. J. Sovers, A. Moore, and S. Owen, ‘Use of Reference Frames for

Interplanetary Navigation at JPL,’ REFAG-2010 Conference, Marne-La-Vallee, France, Oct 2010.

http://iag.ign.fr/abstract/pdf/Heflin REFAG2010.pdf

[3] Jacobs, C. S., J. E. Clark, C. Garcia-Miro, M. B. Heflin, S. Horiuchi, V. E. Moll, L. J. Skjerve, and

O. J. Sovers, ‘Celestial Reference Frame at X/Ka-Band,’ REFAG-2010, Marne-La-Vallee, France, Oct

2010.

http://iag.ign.fr/abstract/pdf/Jacobs REFAG2010.pdf

[4] Jacobs, C. S., J. E. Clark, C. Garcia-Miro, S. Horiuchi, L. J. Skjerve, and O. J. Sovers ‘Celestial

Reference Frame at X/Ka-Band,’ Proc. 20th EVGA, Bonn, Germany, S. Bernhart, ed., 29–31 Mar

2011.

http://www.mpifr-bonn.mpg.de/div/meetings/20thEVGA/EVGA-Talks/Jacobs XKa 110330.pdf

[5] Jacobs, C. S., J. E. Clark, C. Garcia-Miro, S. Horiuchi, I. Sotuela, ‘The Contribution of X/Ka-band

VLBI to Multi-wavelength Celestial Frame Studies,’ Journees: Earth rotation, reference systems and

celestial mechanics: Synergies of geodesy and astronomy” Vienna, Austria, 19-21 Sep 2011.

http://info.tuwien.ac.at/hg/meetings/journees11/abstracts.php

[6] Jacobs, C., U. Bach, F. Colomer, P. de Vincente, C. Garcia-Miro, J. Gomez-Gonzalez, S. Gulyaev,

S. Horiuchi, R. Ichikawa, A. Kraus, G. Kronschnabl, J. Lopez-Fernandez, J. Lovell, W. Majid, T.

Natusch, A. Neidhardt, C. Phillips, R. Porcas, A. Romero-Wolf, L. Saldana, U. Schreiber, I. Sotuela,

H. Takeuchi, J. Trinh, A. Tzioumis, and V. Zharov, ‘The Potential for a Ka-band Worldwide VLBI

Network,’ Journees Systemes de reference spatio-temporels, Vienna, Austria, 19-21 Sep 2011.

http://info.tuwien.ac.at/hg/meetings/journees11/Pres/S2/S2 07 Jacobs.pdf

[7] Jacobs, C. S., J. E. Clark, C. Garcia-Miro, S. Horiuchi, I. Sotuela, ‘A Ka-band Celestial Reference

Frame with Applications to Deep Space Navigation,’ Ka and Broadband Communications: Navigation

and Earth Observation Conference, Palermo, Italy, 3 Oct 2011. http://www.kaconf.org/

[8] Lanyi, G., ‘Quadruply Differenced One-Way Ranging: QDOR, IPN PR 42-186, pp. 1-15, 2011.

http://tmo.jpl.nasa.gov/progress report/42-186/186A.pdf

[9] Lowe, S. T., ‘A Measurement of X-Band Front-End Phase Dispersion for Delta-Differenced One-Way

Range (DDOR) Experiments,‘ IPN PR 42-184, pp. 1-15, 2011.

http://tmo.jpl.nasa.gov/progress report/42-184/184B.pdf

[10] Ma, C., A. Andrei, G. Bourda, and C.S. Jacobs, ‘Celestial Frames at Multiple Wavelengths,’ JENAM,

St. Petersburg, Russia, 4–8 July 2011. http://jenam2011.org/c4onf/

[11] Navarro, R., S. Rogstad, J. Trinh, C. Jacobs, ‘Implementation Issues and Choices for VLBI Data

Acquisition System in DSN,’ 9th U.S. VLBI Technical Meeting, Socorro, NM, 01 Nov 2011.

http://www.aoc.nrao.edu/ jromney/9th US VLBI/navarro JPL

[12] Sotuela, I., C. S. Jacobs, J. E. Clark, C. Garcia-Miro, S. Horiuchi, O. J. Sovers, ‘Contribution of X/Kaband VLBI to Multi-wavelength Celestial Frame Studies,’ GREAT-ESF, Porto, Portugal, June 2011.

http://www.fc.up.pt/great-ws-porto/Ioana Sotuela.pdf

[13] Romero-Wolf, A. and C. S. Jacobs, ‘Correlated Noise processing of VLBI data,’ Journees: Systemes

de reference spatio-temporels: Earth rotation, reference systems and celestial mechanics: Synergies of

geodesy and astronomy” Vienna, Austria, 19-21 Sep 2011.

http://info.tuwien.ac.at/hg/meetings/journees11/Pres/S2/S2 09 Romero-Wolf.pdf

IVS 2011 Annual Report 229
KASI Combination Center Korea Astronomy and Space Science Institute

KASI Combination Center Report

Younghee Kwak, Jungho Cho

Abstract

This report introduces the activities of the Korea Astronomy and Space Science Institute (KASI)

as an IVS Combination Center and shows the current status of the combination work. It also outlines

the intended tasks for 2012.

1. General Information

KASI was accepted as an IVS Combination Center in October 2008 and has prepared for regular combination operation. The KASI Combination Center combines the sessionwise products of

the IVS Analysis Centers (ACs) into a final combination product.

2. Component Description

The missions of the KASI Combination Center are to create high quality combination products,

to verify the combination solution of the BKG/DGFI Combination Center through cross-checking,

to control the quality of the ACs’ results, to provide feedback to the Analysis Centers, and to

adhere to the IERS Conventions. We combine the products of individual IVS ACs at the normal

equation level using the Bernese GPS Software (S/W) Version 5.0. Since the software has been

developed for GPS data processing and analysis by the Astronomical Institute, University of Bern

(AIUB), we have modified the software to deal with IVS analysis products properly.

3. Staff

The staff members of the KASI Combination Center are listed below.

Table 1. Personnel of the KASI Combination Center.

Jungho Cho +82-42-865-3234 jojh@kasi.re.kr

Younghee Kwak +82-42-865-2031 bgirl02@kasi.re.kr

4. Current Status and Activities

The Bernese S/W provides the functions of stacking Normal Equations (N.E.) and estimating

parameters. The inputs to the Bernese S/W are the N.E. matrices and the N.E. vectors from the

daily SINEX files of the individual ACs. The outputs are daily SINEX files including combined

station coordinates and Earth Orientation Parameters (EOPs).

In order to validate the modified Bernese S/W, we reanalyzed solutions of BKG, GSFC, and

OPA (Table 2) that use identical analysis software, Calc/Solve, and combined them. As a prepara230 IVS 2011 Annual Report
Korea Astronomy and Space Science Institute KASI Combination Center

tory combination analysis, we also combined IVS analysis products of six ACs — BKG, DGFI,

GSFC, IAA, OPA, and USNO (Table 2) — and then compared the residuals of individual solutions

with respect to the combination solution.

Table 2. Products of individual ACs for the combination.

AC BKG DGFI GSFC IAA OPA USNO

Solution bkg2010a dgf2009a gsf2010a iaa2010a opa2010a usn2007b

(1) Test combination with 3ACs

The solutions of 144 sessions, especially XA and XE code sessions, in 2008 were combined.

The outliers were not excluded in this combination. We solely compared X-pole, Y-pole, UT1,

and their rates of individual solutions with respect to those of combined solutions. The residuals

between individual solutions and the combined solution are shown in Figure 1. The Root-MeanSquares (RMS) and biases of the residuals are shown in Table 3. As all three ACs use Calc/Solve,

the combined solution agrees well with individual solutions except for the rates of polar motion.

There are systematic variations between individual and combined solutions. We expect that they

are caused by inappropriate apriori values or nutation definition.

(2) Full combination with 6ACs

We combined six main AC solutions. Figure 2 shows the residuals between individual solutions

and the combined solution, and Table 4 shows their RMS and biases. In the combination, we

excluded severe outliers. The RMS of the residuals are around 300 microarcseconds (μas) for

polar motion, 10 microseconds (μs) for UT1, 300 microarcseconds/day (μas/d) for polar motion

rates, and 20 μs for LOD. This accuracy level still is inferior to that of current BKG/DGFI

Combination Center[1]. The systematic variation patterns of polar motion rates are similar with

3ACs combination.

5. Future Work for 2012

Our future work in 2012 is as follows:

• Weighting the individual solutions

• Combining whole period IVS products (1984-present)

• Comparing with BKG/DGFI Combination Center, IERS 08C04, and IGS solutions

• Providing IVS EOP format solutions (Rapid and Quarterly)

References

[1] http://ida.bkg.bund.de/IVS/index.html

BKG/DGFI Combination Center Web page.

IVS 2011 Annual Report 231
KASI Combination Center Korea Astronomy and Space Science Institute

Figure 1. Internal comparison between individual solutions and KASI combination solution (Individual

solutions - Combined solution). + : BKG, × : GSFC, N : OPA.

Table 3. RMS and offset of the residuals between individual solutions and the combined solution.

RMS X-Pole Y-Pole UT1 X-Pole rate Y-Pole rate LOD

/Offset (mas) (mas) (ms) (mas/d) (mas/d) (ms)

BKGKAS 0.193 0.329 0.018 0.335 0.702 0.035

−COMKAS /-0.025 /0.055 /-0.002 /-0.049 /0.069 /0.003

GSFKAS 0.163 0.432 0.013 0.308 0.481 0.025

−COMKAS /-0.008 /0.011 /-0.001 /-0.066 /0.086 /0.001

OPAKAS 0.263 0.236 0.016 0.345 0.592 0.032

−COMKAS /-0.019 /0.007 /0.000 /-0.015 /0.068 /0.001

232 IVS 2011 Annual Report
Korea Astronomy and Space Science Institute KASI Combination Center

Figure 2. Internal comparison between individual solutions and KASI combination solution (Individual

solutions - Combined solution). + : BKG, ⋄ : DGFI, × : GSFC,  : IAA, N : OPA, 
 : USNO

Table 4. RMS and offset of the residuals between individual solutions and the combined solution.

RMS X-Pole Y-Pole UT1 X-Pole rate Y-Pole rate LOD

/Offset (mas) (mas) (ms) (mas/d) (mas/d) (ms)

BKGKAS 0.325 0.350 0.010 0.323 0.290 0.021

−COMKAS /-0.034 /0.130 /0.002 /-0.054 /0.072 /-0.003

GSFKAS 0.282 0.340 0.010 0.308 0.373 0.021

−COMKAS /-0.012 /0.124 /0.001 /-0.034 /0.118 /-0.003

OPAKAS 0.291 0.331 0.011 0.320 0.361 0.023

−COMKAS /-0.046 /0.119 /0.001 /-0.010 /0.129 /-0.002

DGFKAS 0.276 0.312 0.011 0.334 0.320 0.021

−COMKAS /-0.029 /0.077 /0.000 /-0.045 /0.112 /0.000

IAAKAS 0.283 0.380 0.011 0.372 0.360 0.022

−COMKAS /0.014 /0.160 /-0.001 /-0.039 /0.135 /0.003

USNKAS 0.264 0.294 0.008 0.334 0.335 0.016

−COMKAS /0.031 /0.024 /-0.001 /-0.162 /0.000 /0.003

IVS 2011 Annual Report 233
KTU-GEOD IVS Analysis Center Karadeniz Technical University, Department of Geomatics Engineering

KTU-GEOD IVS Analysis Center Annual Report 2011

Emine Tanır Kayık ̧cı, Kamil Teke

Abstract

This report summarizes the activities of the KTU-GEOD IVS Analysis Center (AC) in 2011 and

outlines the planned activities for the year 2012. Analysis of the EUROPE sessions is one of our specific

interests. Combination of different AC solutions for continuous VLBI sessions, e.g., CONT11 sessions,

will be investigated.

1. General Information

The KTU-GEOD IVS Analysis Center (AC) is located at the Department of Geomatics Engineering, Karadeniz Technical University, Trabzon, Turkey.

2. Staff at KTU-GEOD Contributing to the IVS Analysis Center

Members who are contributing to research of the KTU-GEOD IVS Analysis Center (AC) in

2011 are listed in Table 1 (in alphabetical order) by their main focus of research and working

location:

Table 1. Staff members.

Name and Email Working Location Main Focus of Research

Emine Tanır Kayık ̧cı Karadeniz Technical University, responsibility for

etanir@ktu.edu.tr Department of Geomatics Analysis Center work and

Engineering, data processing

Trabzon, Turkey

Kamil Teke Hacettepe University, data processing

kteke@hacettepe.edu.tr Department of Geodesy and

Photogrammetry Engineering,

Ankara, Turkey

3. Current Status and Activities

During 2011 we focused on things outside IVS. In 2012 we plan to return to IVS activities.

4. Future Plans

We will continue to analyze VLBI sessions with different parameterizations, focusing on the

EUROPE sessions by using VieVS software. In 2012, combination of different AC solutions for

continuous VLBI sessions, e.g., CONT11 sessions, will be investigated.

234 IVS 2011 Annual Report
Karadeniz Technical University, Department of Geomatics Engineering KTU-GEOD IVS Analysis Center

Acknowledgements

We are thankful to all the governing board of IVS. We are grateful to Karadeniz Technical

University for their financial support of KTU-GEOD IVS AC research activities.

IVS 2011 Annual Report 235
Analysis Center at MAO Main Astronomical Observatory, National Academy of Sciences of Ukraine

IVS Analysis Center at Main Astronomical Observatory of

National Academy of Sciences of Ukraine

Yaroslav Yatskiv

Abstract

This report summarizes the activities of the VLBI Analysis Center at the Main Astronomical

Observatory of the National Academy of Sciences of Ukraine in 2011.

1. Introduction

The VLBI Analysis Center was established in 1994 by the Main Astronomical Observatory

(MAO) of the National Academy of Sciences of Ukraine (NASU) as a working group of the Department of Space Geodynamics of the MAO. In 1998 the group started its IVS membership as an

IVS Analysis Center. The MAO AC is located at the office building of the observatory in Kiev.

2. Technical Description

VLBI data analysis at the center is performed on two computers: an Intel Core 2 Duo 3.1 GHz

box with 4 GB RAM and a 1 TB HDD, and a Pentium-4 3.4 GHz box with 1 GB RAM and two

200 GB HDDs. Both computers are running under the Linux/GNU Operating System.

For data analysis we use the SteelBreeze software which was developed at the MAO NASU.

The SteelBreeze software is written in the C++ programming language and uses the Qt 2.x widget library. SteelBreeze makes Least Squares estimation of different geodynamical parameters

with the Square Root Information Filter (SRIF) algorithm (see [1]).

The software analyzes VLBI data (time delays) of a single session or a set of multiple sessions.

The time delay is modeled according to the IERS Conventions (2003) [2], as well as by using

additional models (tectonic plate motion, nutation models, wet and hydrostatic zenith delays,

mapping functions, etc.). The following parameters are estimated: Earth orientation parameters,

coordinates and velocities of a selected set of stations, coordinates of a selected set of radio sources,

clock function, and wet zenith delay.

3. Staff

The VLBI Analysis Center at Main Astronomical Observatory consists of the following members:

Yaroslav Yatskiv: Head of the Department of Space Geodynamics; general coordination and

support of activity of the Center.

Sergei Bolotin: Scientific consultant on VLBI software development.

4. Current Status and Activities in 2011

In 2011 we performed regular VLBI data analysis to determine Earth orientation parameters.

“Operational” solutions were produced and submitted to the IVS on a weekly basis. The IERS

236 IVS 2011 Annual Report
Main Astronomical Observatory, National Academy of Sciences of Ukraine Analysis Center at MAO

Conventions (2003) [2] models were applied in the analysis. In the solutions, station coordinates

and Earth orientation parameters were estimated.

Also, this year we continued to participate in the IVS Tropospheric Parameters project. Estimated wet and total zenith delays for each station were submitted to IVS. The analysis procedure

was similar to the one used for the operational solutions.

5. Plans for 2012

The MAO Analysis Center will continue to participate in operational EOP determination,

as well as in updating the TRF and CRF solutions from VLBI analysis of the full data set of

observations.

Acknowledgements

The work of our Analysis Center would be impossible without the activities of other components

of IVS. We are grateful to all contributors from the Service.

References

[1] Biermann, G.J., 1977, Factorization Methods for Discrete Sequential Estimation, V128, Mathematics

in Science and Engineering Series, Academic Press.

[2] IERS Conventions (2003), IERS Technical Note 32, eds. D.D. McCarthy and G. Petit, Bundesamt f ̈ur

Kartographie und Geod ̈asie, Frankfurt am Main.

IVS 2011 Annual Report 237
NICT Analysis Center Kashima Space Research Center, NICT

Analysis Center at National Institute of Information and

Communications Technology

Thomas Hobiger, Ryuichi Ichikawa, Mamoru Sekido, Yasuhiro Koyama, Tetsuro Kondo

Abstract

This report summarizes the activities of the Analysis Center at the National Institute of Information

and Communications Technology (NICT) for the year 2011.

1. General Information

The NICT Analysis Center is operated by the space-time standards group of NICT and is

located in Kashima, Ibaraki, Japan as well as at the headquarters in Koganei, Tokyo. In April

2011 the space-time standards group, to which the VLBI group belongs, was re-organized under the

Applied Electromagnetic Research Institute of NICT. Analysis of VLBI experiments and related

study fields at our group are mainly concentrated on experimental campaigns for developing new

techniques such as time and frequency transfer, e-VLBI for real-time EOP determination, analysis

software development, prototyping of a compact VLBI system, and atmospheric path delay studies.

2. Staff

Members who are contributing to the Analysis Center at the NICT are listed below (in alphabetical order, with their working locations in parentheses):

• HOBIGER Thomas (Koganei, Tokyo): Analysis software development, time and frequency

transfer, and atmospheric research

• ICHIKAWA Ryuichi (Kashima): Compact VLBI system and atmospheric modeling

• KONDO Tetsuro (Kashima): Software correlator

• KOYAMA Yasuhiro (Koganei, Tokyo): e-VLBI

• SEKIDO Mamoru (Kashima): International e-VLBI and VLBI for spacecraft navigation

3. Current Status and Activities

After the big earthquake on 11 March 2011, post-seismic crustal deformation has been regularly

monitored by the Kashima (11 m) - Koganei (11 m) baseline since 7 May 2011. More details about

these monitoring observations are described in [3].

3.1. Ultra-rapid EOP Experiments

In cooperation with Geospatial Information Authority of Japan (GSI), Onsala Space Observatory, and University of Tasmania, several ultra-rapid UT1 and EOP experiments were carried

out. Since the single baseline between Onsala and Tsukuba only allows the determination of UT1

in real-time, first tests with a three-station network including Hobart were made in order to test

the potential of obtaining all three Earth orientation parameters in near-real time. Therefore, the

238 IVS 2011 Annual Report
Kashima Space Research Center, NICT NICT Analysis Center

automated analysis software (see section 3.3) needed to be adopted to handle automated ambiguity resolution of multi-baseline sessions and to allow for a robust estimation of the three EOP

components. In addition to the dedicated ultra-rapid experiments, GSI regularly automatically

submits c5++ processed UT1 results (see [2] for details on the processing strategy) from INT2

sessions to the IERS for test purposes.

3.2. Time and Frequency Transfer via VLBI

 1e-16

 1e-15

 1e-14

 1e-13

102103104105

Allan deviation

averaging time [sec]

VLBI2010 simulations

simulation avg.

10-15 at 1 day

10-16 at 1 day

Figure 1. Frequency transfer performance over an 18

station global network of VLBI2010-like stations using

a combination of 3 m and 10 m dishes. Simulated observations were kindly provided by the Vienna University

of Technology.

Space geodetic techniques like GNSS have

been proven to be a useful tool for time and

frequency transfer purposes. Besides SLR,

which is currently tested under the name

T2L2, VLBI could be another space geodetic

technique that can be utilized for time and

frequency transfer. Unlike GNSS, VLBI does

not require any orbital information, as it directly refers to an inertial reference frame defined by the location of the quasi stellar objects. As summarized in [5], current VLBI

systems can provide a frequency link stability of about 2 x 10-15 @ 1d (ADEV). But due

to the fact that geodetic VLBI networks do

not observe for more than 24h continuously,

no statement about long-term stability can be

made. Moreover, as VLBI only provides one

observation per epoch, troposphere and station clocks need to be de-correlated in space

geodetic analysis by estimating these parameters from a batch of several scans. Thus,

VLBI can only contribute to frequency transfer with clock estimates made every 30 minutes or longer. In order to overcome this drawback, NICT’s Space-Time Standards Laboratory has

started to work on the realization of a time and frequency transfer system based on the principles of

VLBI, whereas developments from the upcoming geodetic VLBI2010 system are expected to help

to reach these goals. VLBI2010 is designed to provide observables with a few picoseconds of uncertainty, and once a global station network is deployed, it is expected to operate 24h/7d which would

allow to access long-term frequency stability on intercontinental links. The VLBI2010 short-term

frequency transfer limitation is thought to be overcome when VLBI is combined with GNSS (or

TWSTFT) in the analysis processing. Based on simulation data (see Figure 1) we have started to

evaluate the frequency transfer performance of the future VLBI2010 network. In parallel, system

development has started at the Kashima Space Research Center facility.

IVS 2011 Annual Report 239
NICT Analysis Center Kashima Space Research Center, NICT

3.3. Development of a Multi-technique Space-geodetic Analysis Software Package

c5++, which is a space-geodetic analysis software that includes SLR, GNSS and VLBI, has

undergone several modifications and updates in the year 2011. First of all, the software has been

made compatible with the IERS Conventions 2010 (see [4]), and its processing speed was improved.

In addition, a SINEX interface has been added in order to output data for inter-comparison

and submission of results. This interface can also be used to read a priori information (TRF,

CRF, EOPs, etc.) which are also given in SINEX format. The VLBI module has been extended

to handle unattended multi-station experiments, whereas a new simple and robust ambiguity

resolution method has been implemented in order to ensure automated processing. This feature

has been tested with three-station EOP experiments (see Section 3.1) and is currently undergoing

an evaluation using large global VLBI networks. Further software updates include new features

for real-time UT1 experiments [2] as well as a support for VMF1. In addition to the currently

used least-squares estimation method, a Kalman filter is being implemented in c5++. Moreover,

Figure 2. S-band (top) and X-band (bottom) residuals after the first (left) and second (right) iteration using

the automated ambiguity resolution strategy applied to data from a three-station experiment (Onsala,

Tsukuba, and Metsahovi) on September 4, 2007. For this example one can see that all ambiguities are

resolved properly after two iterations.

240 IVS 2011 Annual Report
Kashima Space Research Center, NICT NICT Analysis Center

dedicated time and frequency transfer and spacecraft navigation modules are being developed in

order to support the research activities of NICT’s VLBI project.

3.4. Ray-traced Troposphere Slant Delay Correction for Space Geodesy

A software package, called Kashima Ray-tracing Tools (KARAT), has been developed, and it is

capable of transforming numerical weather model data sets to geodetic reference frames, computing

fast and accurate ray-traced slant delays, and correcting geodetic data on the observation level.

A thorough comparison of ray-traced troposphere delays with results from other space-geodetic

techniques during CONT08 has been made by Teke et al. (2011, [6]). KARAT has been extended

to support frequency dependency of the refractivity following the Liebe model [1] with the goal of

finding out whether modern space-geodetic microwave techniques (including VLBI2010 and higher

dual-frequency VLBI configurations) should be corrected for dispersive troposphere delays.

4. Future Plans

For the year 2012 the plans of the Analysis Center at NICT include:

• Time and frequency transfer simulations and experiments by VLBI and combination with

other techniques like GPS or TWSTFT

• Further improvement of the multi-technique space-geodetic analysis c5++ software

• Experiments and analysis of multi-baseline network which allows the determination of all

three EOPs in real-time

• Usage of multi-processors/multi-core processing platforms for the acceleration of space geodetic applications

• VLBI experiments for spacecraft tracking and its analysis

References

[1] Liebe, H.J., MPM-An atmospheric millimeter-wave propagation model, Int. J. Infrared and Millimeter

Waves, 10, 631-650, 1989.

[2] Hobiger T., T. Otsubo, M. Sekido, T. Gotoh, T. Kubooka and H. Takiguchi, Fully automated VLBI

analysis with c5++ for ultra-rapid determination of UT1, Earth, Planets, Space, 45, 2, 75–79, 2010.

[3] Ichikawa R. and M. Sekido, Kashima and Koganei 11-m VLBI Stations, this issue, 2012.

[4] Petit G. and B. Luzum, IERS Conventions, IERS Technical Note, 36, 179 pp., 2010.

[5] Rieck C., R. Haas, R.T.K. Jaldehag, and J.M. Johansson, VLBI time-transfer using CONT08 data,

Proceedings of the 6th IVS General Meeting, 365-369, 2010.

[6] Teke K., J. Boehm, T. Nilsson, H. Schuh, P. Steigenberger, R. Dach, R. Heinkelmann, P. Willis, R.

Haas, S. G. Espada, T. Hobiger, R. Ichikawa and S. Shimizu, Multi-technique comparison of troposphere

zenith delays and gradients during CONT08, Journal of Geodesy, 85, 7, 395-413, 2011..

IVS 2011 Annual Report 241
NMA Associate Analysis Center Norwegian Mapping Authority (NMA)

NMA Analysis Center

Halfdan Pascal Kierulf and Per Helge Andersen

Abstract

The Norwegian Mapping Authority (NMA) has during the last few years had a close cooperation

with FFI in the analysis of space geodetic data using the GEOSAT software. NMA has recently been

given the status of an Associate Analysis Center of IVS (28 October 2010). The future GEOSAT

activities at both institutions will be coordinated by NMA. This also implies that FFI will end being

an IVS Associate Analysis Center in 2012. NMA’s and FFI’s contributions to the IVS as Analysis

Centers focus primarily on 1) routine production of session-by-session unconstrained and consistent

normal equations by GEOSAT as input to the IVS combined solution, and 2) a combined analysis at

the observation level of data from VLBI, GPS (ground-based and LEO), SLR, DORIS, altimetry, accelerometry, and GRACE KBR. After the recent improvements, we expect that VLBI results produced

with GEOSAT will be consistent with results from the other VLBI Analysis Centers to a satisfactory

level.

1. Introduction

A number of co-located stations with more than one observation technique have been established. In principle, all instruments at a given co-located station move with the same velocity, and

it should be possible to determine one set of coordinates and velocities for each co-located site.

In addition, a constant eccentricity vector from the reference point of the co-located station to

each of the individual phase centers of the co-located antennas is estimated using constraints in

accordance with a priori information given by the ground surveys. One set of Earth orientation

parameters (EOP) and geocenter coordinates can be estimated from all involved data types. The

present dominating error source of VLBI is the water content of the atmosphere, which must be

estimated. The introduction of GPS data with a common VLBI and GPS parameterization of

the zenith wet delay and atmospheric gradients will strengthen the solution for the atmospheric

parameters. The inclusion of SLR data, which is nearly independent of water vapor, gives new

information which will help in the de-correlation of atmospheric and other solve-for parameters

and lead to more accurate parameter estimates. These, and many more advantages with the combination of independent and complementary space geodetic data at the observation level, are fully

provided by the GEOSAT software developed by FFI [1, 2].

2. The GEOSAT Software and Analysis Activities in 2011

The Norwegian Mapping Authority (NMA) and FFI have started a close cooperation in the

analysis of space geodetic data using the GEOSAT software. NMA has recently been given the

status of an Associate Analysis Center of IVS. The GEOSAT software is to be used in the analysis

of VLBI data. In addition, there is a lot of activity going on at NMA and FFI to further develop

the multi-technique software GEOSAT (see the FFI TDC 2011 annual report).

The NMA has in collaboration with FFI made a large effort to make the GEOSAT software

compatible with other VLBI analysis software. The software is also in full compliance with the

IERS 2010 Conventions [6].

One of the first challenges that had to be solved was how to extract an unconstrained SINEX

solution from the Upper-Diagonal UD Kalman filter solution produced by GEOSAT. A first test

242 IVS 2011 Annual Report
Norwegian Mapping Authority (NMA) NMA Associate Analysis Center

solution was sent to the IVS Combination Center in autumn 2009. During 2010 several solutions

covering all VLBI sessions with at least four stations from the start of 1994 to the end of 2009

were submitted to the IVS Combination Center. The first solution was presented at the 6th IVS

General Meeting, in Hobart, Australia [5]. The overall agreement between the NMA-GEOSAT

solution and the solutions from the other ACs was satisfactory for this first comparison. However,

some discrepancies were found. There were some systematic differences in the nutation parameters,

which in our latest comparisons seem to have vanished. A misinterpretation of the NGS-format

led to systematic differences in UT1-UTC. Systematic differences in station heights have also

disappeared in the latest comparison mostly due to the use of the VMF1 [4] model instead of 3D

ray tracing. We also noticed more noise in the GEOSAT-derived EOP compared to results from

the other software packages. The largest “EOP-outliers” disappeared after some manual editing of

the observations. Some other “EOP-outliers” were removed after a manual introduction of clock

breaks in the analysis.

Our plan is to go through the VLBI data from the start of 1994 to the present and perform a

detailed manual editing of outliers. We expect that this will contribute to a reduction of the EOP

“noise level”. When the editing is completed, a new set of normal equations will be submitted to

IVS for a test combination. We hope (and expect) that the results then will be at the level of the

other IVS ACs.

As soon as the GEOSAT solution is in satisfactory agreement with the other solutions, NMA

will start to deliver unconstrained normal equations in the SINEX format to the IVS Combination

Center on a routine basis. Tests of different models are also planned, for instance, a comparison

of results using VMF1 and 3D ray tracing.

To produce VLBI solutions for IVS [3] is the first part of a larger strategic plan from NMA. The

next step is to include other geometric geodetic techniques (GNSS, SLR, and DORIS) in a common

solution where the different techniques are combined at the observation level. The long-term goal

of this large effort is to also include data from the gravity satellites GRACE and GOCE and from

altimeter satellites.

3. Staff

Dr. Halfdan Pascal Kierulf - Research geodesist of the Norwegian Mapping Authority (NMA).

Dr. Per Helge Andersen - Research Professor of Forsvarets forskningsinstitutt (FFI and NMA).

Dr. Oddgeir Kristiansen - Section Manager at the Norwegian Mapping Authority (NMA).

References

[1] Andersen, P. H., 1995. High-precision station positioning and satellite orbit determination. PhD Thesis,

NDRE/Publication 95/01094

[2] Andersen, P. H., 2000. Multi-level arc combination with stochastic parameters. Journal of Geodesy 74:

531-551 (doi: 10.1007/s001900000115)

[3] B ̈ockmann, S., Artz, T., and Nothnagel, A. 2009, VLBI terrestrial reference contribution to ITRF2008.

Journal of Geodesy, 84, 201-219 (doi: 10.1007/s00190-009-0357-7)

[4] Boehm, J., Werl, B., and Schuh, H. 2006, Troposphere mapping functions for GPS and very long baseline interferometry from European Center for Medium-Range Weather Forecasts operational analysis

data. Journal of Geophysical Research, 111, B02406, (doi:10.1029/2005JB003629)

IVS 2011 Annual Report 243
NMA Associate Analysis Center Norwegian Mapping Authority (NMA)

[5] Kierulf, H.P., Andersen, P.-H., Boeckmann, S., and Kristiansen, O. 2010, VLBI analysis with the

multi-technique software GEOSAT. IVS 2010 General Meeting Proceedings, Edited by Dirk Behrend

and Karen D. Baver (NASA/CP-2010-215864)

[6] Petit, G., and Luzum, B. (eds.), 2010. IERS Conventions (2010). (IERS Technical Note; 36) Frankfurt

am Main: Verlag des Bundesamts f ̈ur Kartographie und Geod ̈asie. 179 pp., paperback, in print

[7] Petrov, L., and Boy, J.-P. 2004. Study of the atmospheric pressure loading signal in VLBI observations,

Journal of Geophysical Research, (doi: 10.1029/2003JB002500)

244 IVS 2011 Annual Report
Observatoire de Paris, SYRTE, CNRS/UMR8630 Paris Observatory Analysis Center (OPAR)

Paris Observatory Analysis Center OPAR: Report on Activities,

January - December 2011

S ́ebastien B. Lambert

Abstract

We report on activities of the Paris Observatory VLBI Analysis Center (OPAR) for calendar year

2011 concerning the development of operational tasks and the Web site.

1. Operational Activities

1.1. 2011a Base Solution

A reanalysis of the complete 24-hour session database was done (2011a) and resulting EOP

series and radio source catalogs were sent to the IVS. This solution estimated EOP and rates

as session parameters, station coordinates and velocities as global parameters, and most of the

sources’ coordinates as global parameters. Troposphere and clock parameters were estimated every

20 min and 60 min, respectively, and gradients were estimated every six hours except for a list

of 105 stations having a non-sufficient observational history. Axis offsets were estimated as global

parameters for a list of 77 stations. We used up-to-date geophysical and astronomical modeling

to compute the theoretical delay and partials, including the IAU 2006 nutation and precession,

the Vienna mapping functions 1, the FES 2004 ocean loading model, and the antenna thermal

deformations as provided by A. Nothnagel (2009, J. Geod., 83, 787). Since the solution was released

after the 11 March 2011 earthquake in Japan, the displacement of the 32-m antenna at Tsukuba

was modeled by splines, as done earlier for Fairbanks and the TIGO antenna at Concepci ́on. We

used the latest version of the Calc/Solve geodetic VLBI analysis software package. More details

can be found at

http://ivsopar.obspm.fr/earth/glo

1.2. Station and Radio Souce Coordinate Time Series

Station and radio source coordinate time series were also produced. For each source, a page

displays plots of original and smoothed time series and provides links to source information of

various external databases (e.g., the French Virtual Observatory software package Aladin that

permits someone to get the optical counterpart of the VLBI quasars, or the Bordeaux VLBI Image

Database that gives the VLBI structure).

1.3. Operational Solutions

24-hour sessions were analyzed routinely within 24 hours after the version 4 database was

submitted to the IVS. The operational solution was aligned to the 2011a global solution. Unconstrained normal equations relevant to EOP, rates, and station and source coordinates were sent

to the IVS in SINEX format for combination in the framework of the IVS Analysis Coordinator’s

task.

Two operational solutions (2011i and 2011j) analyzing Intensive sessions after 2006 were also

submitted to the IVS together with corresponding SINEX files. The solution 2011i processed

IVS 2011 Annual Report 245
Paris Observatory Analysis Center (OPAR) Observatoire de Paris, SYRTE, CNRS/UMR8630

Intensive sessions in order to produce UT1 consistent with VTRF 2008a, ICRF2, and C04 Earth

orientation data. The solution 2011j processed Intensive sessions in order to produce UT1 but is

overparameterized (station coordinates and troposphere delays are also estimated together with

UT1) and produces postfit rms delays as low as for the 24-hr sessions, i.e., lower than 2011i by

a factor of two. In both solutions, due to the 11 March, 2011 earthquake in Japan, data points

obtained from the analysis of the Tsukuba-Wettzell baseline should not be used.

All the above products, except SINEX files, were also published on the OPAR Web site. SINEX

files were only sent to the data centers.

2. Follow-up of Various Phenomena

2.1. Free Core Nutation

The free core nutation (FCN) is a free oscillation of the Earth’s figure axis in space due to the

presence of a liquid core rotation inside the viscoelastic mantle. Its period is close to 430 days and

is retrograde. Understanding the excitation of the FCN and its amplitude and phase variations is

still an open question, although the community generally believes that the key resides in improved

atmospheric and oceanic circulation modeling at diurnal and subdiurnal frequencies. At OPAR,

we maintain an FCN model directly fitted to routinely estimated nutation offsets (Figure 1).

In addition to the FCN, amplitudes and phases of a set of 42 prograde and retrograde tidal

waves are also fitted to the data. These tidal terms are interpreted as small deficiencies of the

IAU 2000A nutation model. More explanations and material can be found at

http://ivsopar.obspm.fr/earth/geo

1980 1985 1990 1995 2000 2005 2010

−0.5

0

0.5

dX (mas)

1980 1985 1990 1995 2000 2005 2010

−0.5

0

0.5

dY (mas)

Figure 1. The free core nutation fitted to opa2010d nutation offsets with respect to the IAU 2006 nutation

and precession models.

246 IVS 2011 Annual Report
Observatoire de Paris, SYRTE, CNRS/UMR8630 Paris Observatory Analysis Center (OPAR)

2.2. Displacement of TIGO at Concepci ́on and of the Tsukuba Radio Telescope

Still using the routinely analyzed 24-hour sessions, we monitored the displacements of the

station of TIGO at Concepci ́on after the 27 February 2010 earthquake and of the radio telescope

at Tsukuba after the 11 March 2011 earthquake. Figure 2 displays the UEN coordinates of the two

sites with respect to the mean position as given in the VTRF 2008a. The monitoring is continued

at

http://ivsopar.obspm.fr/earth/tigo

http://ivsopar.obspm.fr/earth/tsukuba

3. Staff Members

Staff members who contributed to the OPAR analysis and data centers in 2011 are listed below:

• S ́ebastien Lambert, Analysis Center manager, responsible for data analysis, development of

GLORIA analysis software,

• Christophe Barache, Data Center manager, data analysis,

• Daniel Gambis, responsible for the IERS Earth Orientation Center, interface with IERS

activities.

IVS 2011 Annual Report 247
Paris Observatory Analysis Center (OPAR) Observatoire de Paris, SYRTE, CNRS/UMR8630

2010 2010.5 2011 2011.5 2012 2012.5

−20

0

20

Up (cm)

TIGOCONC

2010 2010.5 2011 2011.5 2012 2012.5

−300

−200

−100

0

East (cm)

2010 2010.5 2011 2011.5 2012 2012.5

−100

−50

0

North (cm)

2011 2011.5 2012 2012.5

−20

−10

0

10

Up (cm)

TSUKUB32

2011 2011.5 2012 2012.5

0

50

100

East (cm)

2011 2011.5 2012 2012.5

−20

0

20

North (cm)

Figure 2. The UEN coordinates of TIGOCONC and TSUKUB32 antennas with respect to the VTRF 2008a

solution.

248 IVS 2011 Annual Report
Onsala Space Observatory (OSO) Onsala Space Observatory (OSO) Analysis Center

Onsala Space Observatory – IVS Analysis Center

R ̈udiger Haas, Tong Ning, Gunnar Elgered, Johan L ̈ofgren, Hans-Georg Scherneck

Abstract

This report briefly summarizes the activities of the IVS Analysis Center at the Onsala Space

Observatory during 2011 and gives examples of results of ongoing work.

1. Introduction

We concentrate on a number of research topics that are relevant for space geodesy and geosciences. These research topics are addressed in connection to data observed with geodetic VLBI

and complementing techniques.

2. Assessment of Ultra-rapid dUT1-sessions

Since 2007, Onsala and Tsukuba have cooperated in a project to perform so-called ultra-rapid

dUT1-sessions. For these sessions, real-time data transfer, near real-time correlation, and an

automated near real-time data analysis allows the determination of dUT1 results with very low

latency. In the beginning of the project, these sessions were dedicated Intensive-style sessions

on one baseline for about 1 hour. Since 2009, normal 24-hour-long IVS sessions have also been

observed in ultra-rapid mode. We performed a preliminary assessment of the dUT1 results derived

in ultra-rapid mode [1]. The agreement between the ultra-rapid dUT1 results and the IERS final

results is about 30 msec, i.e. approximately on the same level as the agreement between the IERS

rapid results and the IERS final results. However, the ultra-rapid dUT1 results have a much lower

latency and are, for example, available already during ongoing 24-hour IVS sessions.

3. Multi-technique Comparisons of Zenith Wet Delay Estimates

We compared 10-year-long time series of atmospheric zenith wet delay data [2]. These data

were derived from VLBI, GPS, and ground-based radiometry at the Onsala Space Observatory,

radiosondes from Landvetter airport, at a distance of about 37 km from Onsala, and the reanalysis product from the European Center for Medium-Range Weather Forecast. This comparison

significantly extends previous work focussing on VLBI CONT-sessions only, see e.g. [3]. The best

agreement over the 10 year period is seen between GPS and VLBI with a mean bias of −3.4 mm

and a standard deviation of 5.1 mm. The ECMWF product shows a positive bias of about 7 mm

with respect to the other techniques.

4. Trends in the Amount of Integrated Atmospheric Water Vapor

We also compared long term trends in the amount of integrated atmospheric water vapor

derived from four different techniques [4]. The four techniques are VLBI, GPS, ground-based radiometry at the Onsala Space Observatory, and radiosondes from Landvetter airport, at a distance

of about 37 km from Onsala. The time series cover up to 30 years of data, and the four techniques

detect individual positive trends in the integrated water vapor (IWV) on the order of 0.3 to 0.6

IVS 2011 Annual Report 249
Onsala Space Observatory (OSO) Analysis Center Onsala Space Observatory (OSO)

kg/m2 per decade. The IWV data derived from the techniques agree with correlation coefficients

on the order of 0.95 and better and root mean-square differences of less than 2 kg/m2.

5. Raytracing through the High Resolution Numerical Weather Model HIRLAM

We used the conformal theory of refraction to perform raytracing through data of the High

Resolution Numerical Weather Model HIRLAM, and we computed slant delays for 15 European

geodetic VLBI sessions between 2005 and 2007 [5]. Compared to our previous raytracing approaches, the new approach enables us to include atmospheric inhomogenities.

6. Ocean Tides at Onsala

We used data recorded with the GNSS-based tide-gauge at Onsala [6] to determine ocean tidal

constituents and compared these to theoretical models. The results indicate that the accuracy of

global ocean models is restricted in the Skagerrak and Kattegat, and refined regional ocean tide

models are necessary [7, 8].

7. Ocean Tide Loading

The automatic ocean tide loading provider [9] was maintained during 2011. Three new ocean

tide models, DTU10 [10, 11] from the Danish University of Technology, EOT11a (which is an

updated version of ET08a [12]) from DGFI Munich, and HAMTIDE [13] from the Institute of

Oceanography at Hamburg University, were included.

8. VLBI Observations of GLONASS Satellite Signals

We continued to work on the analysis of VLBI observations of GLONASS satellite signals

observed on the baseline Onsala – Medicina [14]. Fringes were successfully found with two different

and independent software correlators.

9. Outlook

The IVS Analysis Center at the Onsala Space Observatory will continue its efforts to work on

specific topics relevant to space geodesy and geosciences. During 2012 we plan to intensify our

activities, in particular concerning VLBI data analysis.

250 IVS 2011 Annual Report
Onsala Space Observatory (OSO) Onsala Space Observatory (OSO) Analysis Center

References

[1] Haas R, Hobiger T, Sekido M, Koyama Y, Kondo T, Takiguchi H, Kurihara S, Kokado K, Tanimoto D,

Nozawa K, Wagner J, Ritakari J, Mujunen A, Uunila M (2011) Near real-time monitoring of UT1 with

geodetic VLBI. In: W. Alef, S. Bernhart, A. Nothnagel (eds.): Proc. 20th Meeting of the European

VLBI Group for Geodesy and Astrometry, 64–66.

[2] Ning T, Haas R, Elgered G, Will ́en U (2011) Multi-technique comparisons of 10 years of wet delay

estimates on the west coast of Sweden. Journal of Geodesy, online published November 22, 2011,

doi:10.1007/s00190-011-0527-2

[3] Teke K, B ̈ohm J., Nilsson T, Schuh H, Steigenberger P, Dach R, Heinkelmann R, Willis P, Haas R,

Garcia-Espada S, Hobiger T, Ichikawa R, Shimizu S (2011) Multi-technique comparison of troposphere

zenith delays and gradients during CONT08. Journal of Geodesy, 85(7), 395–413, doi:10.1007/s00190-

010-0434-y

[4] Haas R, Ning T, Elgered G (2011) Long-Term Trends in the Amount of Atmospheric Water Vapour

Derived From Space Geodetic and Remote Sensing Techniques. ESA Proceedings WPP 326 : Proc. 3rd

Int. Colloquium – Scientific and Fundamental Aspects of the Galileo Programme

[5] Garc ́ıa-Espada S, Haas R, Colomer-Sanmartin F (2011) Application of ray-tracing through the high resolution numerical weather model HIRLAM applying the Conformal Theory of Refraction. In: W. Alef,

S. Bernhart, A. Nothnagel (eds.): Proc. 20th Meeting of the European VLBI Group for Geodesy and

Astrometry, 133–137.

[6] L ̈ofgren J, Haas R, Johansson J M (2011) Monitoring coastal sea level using reflected GNSS signals. J.

Advances in Space Research, 47(2), 213–229, doi:10.1016/j.asr.2010.08.015

[7] L ̈ofgren J, Haas R, Scherneck H-G (2011) Three months of local sea-level derived from reflected GNSS

signals. Radio Science, 46, (RS0C05), doi:10.1029/2011RS004693

[8] L ̈ofgren J, Haas R, Scherneck H-G (2011) Sea-Level Analysis Using 100 Days of Reflected GNSS Signals.

ESA Proceedings WPP 326 : Proc. 3rd Int. Colloquium – Scientific and Fundamental Aspects of the

Galileo Programme

[9] Scherneck H.-G., Bos M. (2002) Ocean Tide and Atmospheric Loading. In: IVS 2002 General Meeting

Proceedings, N.R. Vandenberg and K.D. Baver (eds.), NASA/CP-2002-210002, 205–214.

[10] Andersen OB, Knudsen P (2009) The DNSC08 mean sea surface and mean dynamic topography. J.

Geophys. Res., 114, C11, doi:10.1029/2008JC005179

[11] Andersen OB (2010) The DTU10 Gravity field and Mean sea surface. Second international symposium

of the gravity field of the Earth (IGFS2), Fairbanks, Alaska.

[12] Savcenko R, Bosch W (2008) EOT08a - empirical ocean tide model from multi-mission satellite altimetry. DGFI Report 81, Deutsches Geod ̈atisches Forschungsinstitut (DGFI), M ̈unchen.

[13] Taguchi E, Stammer D, Zahel W (2010) Estimation of deep ocean tidal energy dissipation based on

the high-resolution data-assimilative HAMTIDE model. (to be submitted to J. Geophys. Res.).

[14] Tornatore V, Haas R, Duev D, Pogrebenko S, Casey S, Molera-Calves G, Keimpema A (2011) Single

baseline GLONASS observations with VLBI: data processing and first results. In: W. Alef, S. Bernhart,

A. Nothnagel (eds.): Proc. 20th Meeting of the European VLBI Group for Geodesy and Astrometry,

162–165.

IVS 2011 Annual Report 251
PMD Analysis Center Politecnico di Milano, DIIAR

PMD Analysis Center Report for 2011

Vincenza Tornatore, Letizia Cannizzaro

Abstract

This report gives an overview of the “Politecnico di Milano” (PMD) VLBI Analysis Center activities

during 2011 and briefly outlines the plans for 2012. The PMD AC processes IVS EUROPE sessions

for baseline length variation computation and determination of time series coordinates of VLBI antennas. The AC performs also research and software development aimed to improve time series analysis.

This work was developed within the context of comparison of VLBI and GPS (Global Positioning System) techniques and with respect to the geophysical models available in the European area. Another

important task concerns the observational part; in particular several tests have been carried out to

demonstrate the possibility of detecting GNSS satellite signals using the VLBI technique.

1. General Infomation

During 2011 the PMD AC did not significantly change its principal characteristics, e.g., the

hardware and software components, location, sponsorship agency and staff described in the 2010

report. Three of the main fields of interest to PMD during 2011 are briefly highlighted in this

report. They can be summarized here:

• Space co-location (VLBI—GNSS)

• Processing of EUROPE VLBI sessions

• Establishing procedures for VLBI and GPS time series analysis.

The current status of these activities, the principal results achieved, and foreseen further developments for next year are described in the following.

2. Space Co-location (VLBI—GNSS)

Many efforts dedicated to continue the observation activity of GNSS signals started already

in 2009 [1]. International cooperation with other universities and research centers with similar

interests was strongly supported. Thanks to the availability of different instruments, software,

and interdisciplinary capabilities, several tests were performed to establish procedures for making

possible the observation of GNSS signals with VLBI antennas. This is a very challenging task,

since the use of the same optics (including gravitational and thermal deformations), electronics, and

processing pipelines as for natural radio sources, observed with the VLBI technique, ensures the

cross-calibration of two frames. GLONASS (GLObal NAvigation Satellite System) data observed

during an experiment in 2010 with the Medicina and Onsala VLBI antennas were processed with

two different correlation software packages, giving promising results; see [2] for more details on

the experiment. The plans of PMD in this field are to continue with observing tests, using more

than two stations, longer observing time intervals, and different designs that can foresee the use of

natural calibrators near the satellite orbits for effectively reducing the contribution of uncalibrated

errors in VLBI delay measurements such as station clock offsets, instrumental errors, and effects

due to signal propagation in the ionosphere and the troposphere.

252 IVS 2011 Annual Report
Politecnico di Milano, DIIAR PMD Analysis Center

3. Processing of EUROPE VLBI Sessions

All the European sessions available since 1990 through the end of 2010 have been processed

under the same modeling conditions and analogous parameterizations. The software used was

VieVS (Vienna VLBI Software) [3] developed by the members of the VLBI group of the Institute

of Geodesy and Geophysics (IGG), Vienna University of Technology (TU Wien) under the Matlab

programming language. The configuration of the European geodetic VLBI network, that started

with a core of six radio telescopes observing with an average of six sessions per year, reaches today a

number of fourteen participating radio telescopes observing as regularly as possible with the same

duty cycle. European site coordinates and baseline lengths with respective variance-covariance

matrices have been estimated with VieVS to study their temporal evolution. The adjustments

were performed both using single session and global approaches. Analyses of different solutions

are in progress. In 2012, we plan to investigate in more detail the obtained results and to study

also the influence of different datum definitions on European network parameter estimations.

4. Establishing Procedures for Time Series Analysis

In the framework of algorithm development for improving time series analysis of VLBI data

and comparing them with GPS results, the goal was to develop tools that were common as much

as possible to both techniques. Some members of the group working at the ‘Surveying Section’ of

DIIAR gained a lot of experience on the Continuous GPS (CGPS) time series analysis field in the

last years. This experience was considered as a starting point to develop/adapt such algorithms

to VLBI time series analysis. It is well known that GPS solutions are daily or weekly solutions,

generally quite regular for any GPS station; in contrast, VLBI solutions are usually carried out

not as frequently. Then it often happens that, due to hardware or software problems at a VLBI

station, this station will not take part in all the planned. European sessions. In particular the

work at PMD during 2011 was devoted to refining tools for CGPS coordinate time series analysis

for geodynamic applications. In the last two decades the issues of CGPS time series analysis for

geophysical applications were of great interest among the scientific community; different approaches

have been developed, and several works have been published by different authors, e.g., [4], [5], [6].

The PMD DIIAR team faced the issue of GPS time series analysis in the context of the Seismic

Information System for Monitoring and Alert Project (S.I.S.M.A. project) which was a three-year

pilot project funded by the Italian Space Agency (ASI) starting in February 2007 [7], [8] with the

aim to integrate Earth Observation data: SAR (Synthetic Aperture Radar) and GPS techniques

and new advanced methods in seismological and geophysical data analysis for time-dependent

seismic hazard assessment. The procedure implemented at PMD estimates a certain number of

parameters by least squares adjustment. The most interesting parameters, from the geophysical

point of view, are the velocity displacements and their errors. As scientific literature proved, the

observations are temporally correlated and the adopted method estimates the proper deterministic

and stochastic models. Here we briefly illustrate the analysis procedure that can be divided into

five steps.

Step 1: removal of outliers and known discontinuities (see, e.g., Figure 1) due to

• technical equipment changes (e.g., GPS antennas/receivers)

• discontinuities due, e.g., to non-straight alignment of Reference Frame parameters

IVS 2011 Annual Report 253
PMD Analysis Center Politecnico di Milano, DIIAR

• co-seismic effect

Step 2: linear and periodic parameter estimations by least squares adjustment

Step 3: KPSS test [9] on residuals for assessment of stationary behavior

Step 4: study of coordinate time series correlations

• stationary residuals: estimate of the Empirical Covariance Function

• non-stationary residuals: simplified White Noise + Flicker Noise model [5]

Step 5: linear and periodic parameter re-estimations by least squares adjustment, applying the

correct stochastic model.

Figure 1. Coordinate time series for the GPS station of Novara.

254 IVS 2011 Annual Report
Politecnico di Milano, DIIAR PMD Analysis Center

The dots are North (mm), East (mm), and Up (mm) daily coordinate time series of the NOVA

CGPS station (located in the town of Novara) and belonging to the Italian GPS fiducial network

managed by the ASI – Italian Spatial Agency. Vertical lines represent the date of known discontinuities due to the Reference System and GPS antenna/receiver changes (the discontinuities have

been removed in the figure). Continuous lines represent the final estimated deterministic models

superimposed on the time series: the linear parameters stand for the velocity displacement of

NOVA coordinate components.

The described procedure was applied to several Italian GPS stations. Due to the success of

the method on GPS data which proved to have more reliable results, we plan for next year to

adapt the developed algorithms from Fortran to the Matlab programming language and to VLBI

time series studies. The final goal of such a task is to set up a statistical method common to both

techniques, to reveal possible differences in estimated deformations of the European plate, and to

compare the results with geophysical models.

References

[1] Tornatore V., Haas R., (2009), Considerations on the observation of GNSS-signals with the VLBI2010

system. In: G. Bourda, P. Charlot, A. Collioud (eds.): Proc. 19th Meeting of the European VLBI Group

for Geodesy and Astrometry pp. 151-155.

[2] Tornatore V., Haas R., Duev D., Pogrebenko S., Casey S., Molera-Calves G., Keimpema A., (2011)

Single baseline GLONASS observations with VLBI: data processing and first results. In: W. Alef,

S. Bernhart, A. Nothnagel (eds.): Proc. 20th Meeting of the European VLBI Group for Geodesy and

Astrometry, 162–165.

[3] Nilsson T., Boehm J., Boehm S., Madzak M., Nafisi V., Plank L., Spicakova H., Sun J., Tierno Ros J.,

Schuh H. (2011) Status and future plans for the Vienna VLBI Software VieVS, In: W. Alef, S. Bernhart,

A. Nothnagel (eds.): Proc. 20th Meeting of the European VLBI Group for Geodesy and Astrometry,

93-96.

[4] Nikolaidis R. (2002) Observation of Geodetic and Seismic Deformation with the Global Positioning

System, PhD. Thesis, University of California, San Diego.

[5] Williams SDP (2003) The effect of coloured noise on the uncertainties of rates estimated from geodetic

time series, Journal of Geodesy, 76, pp. 483-494.

[6] Amiri-Simkooei AR, Tiberius CCJM, Teunissen PJG (2007) Assessment of noise in GPS coordinate

time series: Methodology and results, Journal of Geophysical Research, 112, B07413, pp. 19.

[7] Barzaghi R., Borghi A., Cannizzaro L., Chersich M., Fermi M., Osmo M. (2009) Role of GPS data

analysis in seismic hazard assessment in the frame of SISMA project, ENC-GNSS 2009, May 3-6,

Naples, Italy.

[8] Panza G.F., Peresan A., Magrin A., Sabadini R., Crippa B., Barzaghi R., Borghi A., Cannizzaro L., Amodio A., Zoffoli S. (2011) The SISMA prototype system: integrating Geophysical Modeling and Earth Observation for time dependent seismic hazard assessment, Natural Hazards, DOI:

10.1007/s11069-011-9981-7.

[9] Hobijn B., Franses P.H., Ooms M., (2004) Generalization of the KPSS-test for stationarity, Statistica

Neerlandica, 58, 4, 483-502.

IVS 2011 Annual Report 255
PUL Analysis Center Pulkovo Observatory

Pulkovo IVS Analysis Center (PUL) 2011 Annual Report

Zinovy Malkin

Abstract

This report briefly presents the PUL IVS Analysis Center activities during 2011 and plans for the

coming year. The main topics of the investigations of the PUL staff in that period were ICRF related

studies, computation and analysis of EOP series, celestial pole offset (CPO) modelling, and VLBI2010

related issues.

1. General Information

The PUL IVS Analysis Center (AC) was organized in September 2006 and is located at and

sponsored by the Pulkovo Observatory of the Russian Academy of Sciences. It is a part of the

Pulkovo EOP and Reference Systems Analysis Center (PERSAC) [1]. The main topics of our IVS

related activities are:

• Improvement of the International Celestial Reference Frame (ICRF).

• Computation and analysis of the Earth orientation parameters (EOP) from Intensives and

24-hour IVS sessions.

• Modelling of the celestial pole offset (CPO) and free core nutation (FCN).

• Comparison of VLBI products, primarily as Earth orientation parameters (EOP), with results

of other space geodesy techniques.

• Computation and analysis of observation statistics.

The PUL AC’s Web page [2] is supported. It contains the following sections:

• General Information on the PUL AC. Includes brief history, activity overview, and scientific

staff list.

• VLBI data analysis. Includes results of VLBI data analysis, such as CPO/FCN series, UT1

Intensives series, and mean Pole coordinates. Data are updated daily.

• OCARS catalog. Includes the latest version of the catalog of optical characteristics of astrometric radio sources (OCARS) [3]. The catalog is continually updated as new information

becomes available.

• Approaches and occultations. Includes tables for forthcoming mutual events of planets and

astrometric radio sources, such as close angular approaches and occultations for the period

until 2050 [4].

• PUL members’ publications and presentations.

• VLBI technology overview.

• Links to the VLBI World. Includes links to (primarily geodetic and astrometric) VLBI

coordinating bodies, stations, analysis centers, software, etc.

• Contact information.

256 IVS 2011 Annual Report
Pulkovo Observatory PUL Analysis Center

2. Scientific Staff

In 2011 the following persons contributed to the PUL activity:

1. Zinovy Malkin (70%) — PUL coordinator, EOP and CRF analysis

2. Natalia Miller (10%) — EOP analysis

3. Julia Sokolova (10%) — CRF analysis

3. Activities and Results

The main activities and results of the PUL IVS Analysis Center during 2011 included:

• Operational processing of the IVS Intensive sessions in automated mode and submission of

results to IVS was continued.

• ICRF related research was continued. The main directions of this activity were comparison

and combination of radio source catalogs, and investigation of their stochastic and systematic

errors.

• The work on the OCARS catalog [3] was continued. The current basic statistics of the catalog

is the following:

OCARS ICRF2 ICRF2 def.

Sources 6431 3414 295

Sources with known redshift 3167 (49.2%) 2072 (60.7%) 253 (85.8%)

Sources with known optical magnitude 4132 (64.3%) 2541 (74.4%) 284 (96.3%)

• A catalog of approaches of planets to radio sources and occultations of astrometric radio

sources by planets through the year 2050 was updated [4].

• Investigations of CPO modelling and its impact on data processing were continued. The

main activities and results in 2011 are the following:

– The PUL CPO and FCN series are updated daily.

– The results of comparing the CPO and FCN models were published [5]. In this paper,

several publicly available empirical models of the celestial pole offset (CPO) and free

core nutation (FCN), including those developed by the author, were investigated and

compared to each other from different points of view, such as representation of the

observational data, FCN parameter variation, and prediction accuracy. Based on this

study, some practical recommendations were proposed.

– The impact of celestial pole offset modelling on VLBI UT1 Intensive results was studied

[6]. In this study, three CPO models currently available for users were tested and the

differences between UT1 estimates obtained with those models were investigated. It was

shown that neglecting CPO modelling during VLBI UT1 Intensive processing causes

systematic errors in UT1 series of up to 20 μas. It was also found that using different

CPO models causes differences in UT1 estimates reaching 10 μas. The obtained results

are applicable to the satellite data processing as well.

IVS 2011 Annual Report 257
PUL Analysis Center Pulkovo Observatory

• A preliminary study of the impact of the Galactic aberration on VLBI-derived precession

parameters has begun [7]. It has been shown by comparison of the linear trends in the

coordinates of the celestial pole obtained with and without taking into account the Galactic

aberration that this effect can reach 20 μas/cy. It is also shown that correcting for the

Galactic aberration influences the derived parameters of low-frequency nutation terms. It is

therefore necessary to correct for Galactic aberration in the reduction of modern astrometric

observations.

• The PUL archive of VLBI data and products is supported. At present, all available databases

and corresponding NGS cards for 1979 – 2011 have been stored (about 9.4 million observations) along with the main IVS and IERS products. These archives are continually updated

as new databases become available.

• The development of algorithms and software for data processing and analysis was continued.

• PUL staff members participated in the activities of several IERS, IAG, and IVS projects,

committees, and working groups.

4. Outlook

Plans for the coming year include:

• Continue VLBI related studies.

• Continue UT1 Intensive processing.

• Continue OCARS catalog support.

• Continue development of algorithms and software for data processing.

• Continue support of the PUL archives of data and products.

References

[1] http://www.gao.spb.ru/english/as/persac/index.htm

[2] http://www.gao.spb.ru/english/as/ac vlbi/

[3] http://www.gao.spb.ru/english/as/ac vlbi/ocars.txt

[4] http://www.gao.spb.ru/english/as/ac vlbi/occultations approaches.pdf

[5] Malkin Z. M. Comparison of CPO and FCN empirical models. In: Proc. Journees 2010: New challenges

for reference systems and numerical standards in astronomy, Paris, France, 20-22 Sep 2010, ed. N.

Capitaine, Paris, 2011, pp. 172–175

[6] Malkin Z. The impact of celestial pole offset modelling on VLBI UT1 intensive results. J. of Geodesy,

2011, v. 85, No. 9, 617-622. DOI 10.1007/s00190-011-0468-9

[7] Malkin Z. M. The Influence of Galactic Aberration on Precession Parameters Determined from VLBI

Observations. Astronomy Reports, 2011, Vol. 55, No. 9, 810–815. DOI: 10.1134/S1063772911090058

258 IVS 2011 Annual Report
Sternberg State Astronomical Institute (SAI) of Lomonosov Moscow State University SAI Analysis Center

SAI VLBI Analysis Center Report 2011

Vladimir Zharov

Abstract

This report presents an overview of the SAI VLBI Analysis Center activities during 2011 and

the plans for 2012. The AC SAI analyzes all IVS sessions for computations of the Earth orientation

parameters (EOP), time series of source positions at the scope of new realizations of the ICRF, and

performs research and software development aimed at improving the VLBI technique.

1. General Information

The SAI VLBI Analysis Center is located at Sternberg State Astronomical Institute of

Lomonosov Moscow State University in Moscow, Russia. The Analysis Center participates in

geodetic and astrometric VLBI analysis, software development, and research aimed at improving

the VLBI technique.

2. Component Description

AC SAI performs data processing of all kinds of VLBI observation sessions. For VLBI data

analysis we use the ARIADNA software package developed at SAI. All reductions are performed

in agreement with the IERS Conventions (2003). A new version of the package is being developed

that will use the IERS Conventions (2010).

ARIADNA uses files in NGS format as input data.

The latest version named as ORBITA is used on the correlator of the AstroSpace Center in

support of the Radioastron mission.

3. Staff

• Vladimir Zharov, Prof.: development of the ARIADNA software, development of the methods

of parameter estimation.

• Aleksander Akosta, post-graduate student: development of the ORBITA software, analysis

of the Radioastron data

• Dmitry Duev, post-graduate student: VLBI data processing, troposphere modeling

• Nikolay Voronkov, scientific researcher: global solution

• Svetlana Nosova, engineer: VLBI data processing

4. Current Status and Activities

• Software development for VLBI processing

The ARIADNA software is being developed to provide contributions to IVS products. The

software is used for calculating all types of IVS products.

The latest version of the software called ORBITA is used for solving many tasks during the

Radioastron mission: calculation of delay and delay rate for the ground-space interferometer,

IVS 2011 Annual Report 259
SAI Analysis Center Sternberg State Astronomical Institute (SAI) of Lomonosov Moscow State University

orbit determination of the space telescope by numerical integration of the differential equations of motion and use of Doppler tracking, laser ranging and VLBI observations for improvement of the Radioastron orbit on the basis of the Kalman filter. The report about the first successful detection of the interference fringes – a correlated signal on ground-to-space baselines

can be found online (http://www.asc.rssi.ru/radioastron/news/newsl/en/newsl 10 en.pdf).

The successful detection of interference fringes demonstrates the overall adequacy of the

technique used in the ORBITA software.

• Routine analysis

During 2011 the routine data processing was performed with the ARIADNA software using

the least-squares method with rigid constraints. A new approach with non-rigid constraints

will be developed for the generation of SINEX files too.

AC SAI operationally processed the 24-hour and Intensive VLBI sessions. The formation of

databases for the VLBI sessions and processing of all sessions is fully automated. The EOP

series sai2011a.eops and sai2011a.eopi were calculated. These series were computed with the

catalog VTRF2008 of station positions and velocities.

• Global solution

N. Voronkov developed software to obtain a global solution. The radio source coordinates

and velocities and the station coordinates and velocities were estimated as global parameters.

EOP, troposphere wet zenith delay (approximated as a polynomial function), troposphere

gradients, and station clocks (approximated as a polynomial function) were estimated as

arc parameters for each session. An experimental catalog of the radio source positions and

velocities was obtained.

• Troposphere modeling

At the stations with the meteorological data missing we used surface data files (temporal coverage: four-times daily, spatial coverage: 2.5 degrees latitude x 2.5 degrees longitude global grid) from NCEP/NCAR Reanalyses(http://www.cdc.noaa.gov/data/gridded/

data.ncep.reanalysis.surface.html) for calculating air temperature, pressure, and relative humidity. For that purpose a program was written, which interpolates these data to the given

coordinates of the station at the time of the observations.

A test version of the software was developed to use the troposphere zenith delay from the

GNSS service in the VLBI analysis.

5. Future Plans

• Continue investigations of VLBI estimation of EOP, station coordinates, and troposphere

parameters, and comparison with satellite techniques.

• Development and testing of the version of ARIADNA in which all reductions are performed

according to the IERS Conventions (2010).

• Improvement of the ARIADNA software for processing of the GNSS troposphere zenith

delays.

260 IVS 2011 Annual Report
SHAO, Chinese Academy of Sciences Shanghai Astronomical Observatory VLBI Analysis Center

SHAO Analysis Center 2011 Annual Report

Guangli Wang, Jinling Li, Minghui Xu, Li Guo, Fengchun Shu, Zhihan Qian, Liang Li

Abstract

This report presents the activities of the Shanghai Astronomical Observatory (SHAO) Analysis

Center in 2011. The SHAO Analysis Center performs data processing and analysis of the geodetic

experiments of the Chinese VLBI Network (CVN), analyzes all of the IVS 24h sessions, and submits

the analysis products (EOP, TRF, and CRF) to the IVS regularly. We have carried out research

work on estimation of Solar acceleration and the consistency analysis of the UT1 time series from IVS

Intensive sessions.

1. General Information

We are in charge of the data processing and analysis of the CVN experiments and analyzing the

IVS data using the CALC/SOLVE software. The members involved in the IVS analysis activities

are Guangli Wang, Jinling Li, Minghui Xu, Li Guo, Liang Li, Fengchun Shu, and Zhihan Qian.

2. Activities in 2011

2.1. Data Processing and Analysis of the CVN Geodetic Experiments

Since the year 2009, China has carried out the Project of Crustal Monitoring Network of the

Chinese Mainland Geological Environment (CMNOC). In this project, the CVN carries out more

than eight 24-hour experiments per year. SHAO undertakes the operations of CVN and data

analysis.

The CVN started to conduct astrometric and geodetic VLBI experiments in 2006. But regular

observations did not take place before 2010. Table 1 shows the statistical information about the

CVN experiments.

The SHAO Analysis Center is in charge of the routine analysis of the CVN data, including:

• Calculation of the delay and delay rate of the CVN observations at each band, resolving group

delay ambiguities, and computation of ionosphere calibrations utilizing the post-correlator

software pps, which is developed based on software made especially for the post-correlation

in the Chang’E Program.

• Generation of the VLBI group delay in the NGS format using the software gngs.

• Analysis of all CVN sessions using software shops, which is developed based on the software

OCCAM6.1E(Linux) with modifications mainly in VLBI data processing models.

2.2. Regular Data Analysis of the IVS 24h Sessions and Product Submission

We restarted routinely analyzing all IVS 24h sessions using the CALC/SOLVE software, and

in this year we also regularly submitted our analysis products (EOP, TRF, and CRF) to the IVS

Data Centers.

IVS 2011 Annual Report 261
Shanghai Astronomical Observatory VLBI Analysis Center SHAO, Chinese Academy of Sciences

Table 1. The statistical information of the CVN experiments.

Experiment Code Date Duration (hr) Stations Obs. Number Delay wrms (ps)

s6602 20060601 10 ShBjKmUr 171 30.3

r7404a 20070404 24 ShBjKmUr 1561 57.3

r7620a 20070620 24 ShBjKmUr 479 32.7

r8919a 20080901 24 ShBjKmUr 282 36.1

g1003d 20100602 24 ShKmUr 545 65.8

g1004a 20100720 24 ShKmUr 368 48.5

g1005a 20100810 24 ShKmUr 414 64.5

r0902a 20100902 24 ShBjKmUr 1590 46.0

r1117a 20110117 24 ShBjKmUr 2534 34.3

r1325a 20110325 24 ShBjKmUr 1598 54.0

r1425a 20110425 23 ShBjKmUr 902 55.7

r1524a 20110524 24 ShKmUr 1136 44.4

t2078 20110720 24 ShKmUr 641 112

r1b14a 20111114 24 ShKmUr 1302 100.1

r1b28a 20111128 24 ShBjKmUr – –

Table 2. Statistical information of the results from the different INT1 types.

Year 1984 - 1994 1994 - 2000 2000 - 2011

Stations Wettzell Wettzell Wettzell

Westford Green Bank Kokee Park

Number of sessions 1854 1359 2374

Length of baseline (km) 5998 6724 10357

East-West-dimension (km) 5977 6669 10072

Avg. number of scans per session 9.6 17.2 20.9

Avg. normal error of ∆UT1 (μs) 124.6 26.2 11.7

Avg. offset w.r.t. C04/precision (μs) -14.1 / 2.4 14.0 / 1.7 10.4 / 0.5

Standard derivation w.r.t. C04 (μs) 101.8 61.8 25.6

Table 3. Comparison of the results from the different Intensive types.

Avg. number of scans Avg. normal error Avg. offset / precision Standard deviation

per session (μs) w.r.t. C04 (μs) w.r.t. C04 (μs)

INT1 20.9 11.7 10.4 / 0.5 25.6

INT2 29.7 10.3 10.3 / 0.9 21.4

INT3 70.2 8.6 31.0 / 2.8 28.3

262 IVS 2011 Annual Report
SHAO, Chinese Academy of Sciences Shanghai Astronomical Observatory VLBI Analysis Center

2.3. Analysis of UT1 Determined from IVS Intensive Observations

We carried out an analysis of the IVS Intensive data from 1984.02 to 2011.08 with different

observation networks, INT1, INT2 and INT3, and we discussed the progress of the UT1 accuracy.

By comparing UT1 results from different networks, we have found a difference on the order of

dozens of microseconds between the networks. The results from the IVS Intensive observations

in which the Seshan station observed showed a similar performance to that of other stations.

From the comparison and analysis of different UT1 series, there exists a level of 10 μs uncertainty

between UT1 estimations obtained from the IVS Intensive observations and from the IERS C04.

The results are presented in Table 2 and Table 3.

2.4. Estimation of Solar Acceleration

The secular aberration drift observed as the apparent proper motion of extragalactic radio

sources is caused by the acceleration of the coordinate origin, the Solar system barycenter. For

30 years, this effect will accumulate up to about 200 μas, which is far beyond the declared several

tens of μas-level of the ICRF2 accuracy. We estimated the acceleration as a global parameter

by using the 30 years of global geodetic/astrometric VLBI data. This estimation is independent

of any kinematic or dynamic model of the Milky Way or statistics hypothesis. The estimated

acceleration in the direction of the Galactic center is 0.75 ± 0.05 cm·s

−1

·yr−1, while the other two

components are -0.02 ± 0.06 and 0.40 ± 0.05 cm·s

−1

·yr−1in the direction along the Solar motion

in the Galactic plane and in the direction normal to the Galactic plane, respectively.

3. Plans for 2012

We will continue to submit our analysis products to the IVS Data Centers regularly. In order

to submit the CVN observations to the IVS, we will conduct the work of transferring the data

format of CVN observations from NGS to netcdf. The research activities will focus on the ICRF

with the consideration of the secular aberration and the study of the high frequency variations of

EOP.

IVS 2011 Annual Report 263
Tsukuba VLBI Analysis Center Geospatial Information Authority of Japan

Tsukuba VLBI Analysis Center

Kensuke Kokado, Shinobu Kurihara, Ryoji Kawabata, Kentaro Nozawa

Abstract

The aim of activities at Tsukuba VLBI Analysis Center is to examine the VLBI data processing

and analysis method to obtain EOP values within the shortest possible time after the VLBI observing

session. The most successful result in 2011 was an ultra-rapid dUT1 measurement during the CONT11

session, which is a campaign of 15 days of continuous VLBI sessions. In this article, the improved data

processing/analysis system and the results of our analysis activities are reported.

1. General Information

The Tsukuba VLBI Analysis Center is located at the Geospatial Information Authority of

Japan (GSI). We became an IVS Operational Analysis Center on April 7, 2010 and started to

submit an ultra-rapid dUT1 solution of IVS-INT2 sessions to IVS in January 2011. The rapid

solution has been used for the calculation of USNO EOP daily solutions. We have also implemented

the ultra-rapid dUT1 experiments during IVS 24-hour sessions in cooperation with the National

Institute of Information and Communications Technology (NICT) and Onsala Space Observatory

(OSO) in Sweden since 2007. These experiments were a good opportunity to improve the data

processing/analysis program for ultra-rapid dUT1 measurement. In 2011, most of the experiments

succeeded, and we could obtain dUT1 solutions during the 24-hour observing sessions.

2. Data Proccessing and Analysis System for Ultra-rapid Measurement

Onsala station  

PC-EVN

Mark5

Real-time data transfer

 + Automatic data conversion

Data transfer

Automatic correlation

Automatic analysis (C5++)

Tsukuba analysis center

Tsukuba station

Tsukuba

 correlator

Management server

K5VSSP

×4 ×4 ×4

Figure 1. Ultra-rapid dUT1 measurement system.

The data processing system for the ultra-rapid dUT1 measurement is shown in Figure 1. The

data of the foreign observatories, such as Wettzell, Onsala, or Hobart, is transferred in real-time

264 IVS 2011 Annual Report
Geospatial Information Authority of Japan Tsukuba VLBI Analysis Center

during the observation. The data from the Onsala or the Hobart station are converted to K5/VSSP

format after the data transfer because the format of the transferred data is Mark 5B. On the other

hand, the format of the transferred data from Wettzell is VDIF, and it is converted to K5/VSSP

format with a real-time data transfer system developed by NICT at the same time of recording on

a data server at Tsukuba correlator. It enables us to reduce the latency of VLBI sessions.

The converted data is correlated as soon as the data conversion is completed. We use about

16 servers for the correlation process, and the processes are completed within a few minutes after

the observing session. When the correlation results for all of the data, or enough data for dUT1

analysis, are ready, the analysis program “c5++” developed by NICT runs automatically, and we

can obtain a dUT1 solution within five minutes after the observing session. All of the programs

run automatically, so we do not have to type any commands during the session. If any error occurs

during data processing, the programs send any error e-mail messages to the operators. We used

the data processing system for ultra-rapid dUT1 measurement on IVS-INT2 sessions, some of the

24-hour sessions, and CONT11 sessions.

3. Results of Our Activities

The Tsukuba VLBI Analysis Center implements three different kinds of ultra-rapid dUT1

measurements. This section shows the results of these dUT1 measurements.

3.1. Ultra-rapid dUT1 Measurement in INT2 Sessions

The Tsukuba VLBI Analysis Center has implemented the ultra-rapid dUT1 measurement in

INT2 sessions in 2009 and started to provide the solution “eopi” file to the IVS Data Center at the

end of January, 2011. All of the solutions were analyzed by c5++, and results were provided within

seven hours after the observing sessions. It is possible to provide the dUT1 solution within a few

minutes after the observing sessions on the Tsukuba-Wettzell baseline session, but it is not possible

to provide the solution so quickly for the sessions with the Kokee-Wettzell baseline, because the

data from the Kokee station are not transferred in real-time. As the data transfer is completed

about six hours after the session, the submission of the dUT1 solution is about seven hours after

the observing session on the Tsukuba-Wettzell baseline. The automated data transfer or the data

analysis program sometimes stopped due to some kinds of error, so we could not submit the dUT1

solution the same day in about 30% of the sessions. We try to solve the problem of this program

every time the ultra-rapid dUT1 measurement fails.

3.2. Ultra-rapid dUT1 Measurement in IVS 24-hour Sessions

In 2011, we also implemented the ultra-rapid dUT1 measurement in 18 IVS 24-hour sessions

(e.g., R1, RD, and T2) in which the Tsukuba, Onsala, Wettzell, or Hobart station participated. In

the case of 24-hour sessions, we can obtain a number of dUT1 values during the observing session

because the data analysis is done every several tens of scans. We sometimes failed in the data

transfer process from the Onsala station but succeeded in ultra-rapid dUT1 measurement in most

of the sessions. Most of the failure is due to human error, so we may have to make a check sheet

or automated check program for the preparation of data transfer.

The new approach in 2011 was that we implemented the ultra-rapid EOP experiment with the

Onsala and Hobart stations. We processed the data of North-South baselines for estimating X/Y

IVS 2011 Annual Report 265
Tsukuba VLBI Analysis Center Geospatial Information Authority of Japan

parameters of polar motion and East-West baselines for dUT1 measurement. We implemented

the experiment in the RD1106 session and an additional session named “UREO01” at the end of

November. Although we had some problems with the data transfer, all of the data processing was

completed within 24 hours after the observing session. We plan to improve the system and want

to process all of the data without any problem with the next experiment. The solution of dUT1

and X/Y parameters of polar motion estimated from the UREO01 session are shown in Figures 2,

3, and 4.

-0.3856

-0.3860

-0.3864

-0.3868

-0.3872

22:00 00:00 02:00 04:00 06:00 08:00 10:00

UT1-UTC [sec]

12:00 14:00

Predicted value

Observed value

Time (Nov.30-Dec.01, 2011)

Figure 2. dUT1 values estimated from the “UREO01” session.

0.178

0.174

0.170

0.166

0.162

22:00 00:00 02:00 04:00 06:00 08:00 10:00

Xp [arcsec]

12:00 14:00

Predicted value

Observed value

Time (Nov.30-Dec.01, 2011)

Figure 3. X-parameter of polar motion estimated from the “UREO01” session.

0.287

0.286

0.285

0.284

0.283

22:00 00:00 02:00 04:00 06:00 08:00 10:00

Yp [arcsec]

12:00 14:00

Predicted value

Observed value

Time (Nov.30-Dec.01, 2011)

0.282

Figure 4. Y-parameter of polar motion estimated from the “UREO01” session.

266 IVS 2011 Annual Report
Geospatial Information Authority of Japan Tsukuba VLBI Analysis Center

3.3. Ultra-rapid dUT1 Measurement in the CONT11 Session

The ultra-rapid dUT1 measurement during the CONT11 campaign was performed on the

Tsukuba-Onsala baseline. The data was transferred to the Tsukuba correlator, correlated, and

analyzed in near real-time during the session. As CONT11 was a campaign of 15 days of continuous

VLBI sessions, we could obtain continuous dUT1 values for 15 days about 30 minutes after the

observation of each scan. Unfortunately, we were forced to stop the ultra-rapid dUT1 measurement

for about one day from September 21 to September 22, because the Tsukuba station was affected

by a big typhoon. We failed in data transfer from Onsala and could not analyze the data for about

three hours on September 25 and 26, but we succeeded in the ultra-rapid dUT1 measurement for

most of the scans of CONT11. The estimated dUT1 values are shown in Figures 5 and 6.

-0.306

-0.310

-0.314

-0.318

-0.322

9/16 0:00 9/18 0:00 9/20 0:00 9/22 0:00 9/24 0:00 9/26 0:00 9/28 0:00

Time

UT1-UTC [sec]

⁂⁤′′′′⁖⁛⁕⁦′′′′⁖‒?!⁓⁞⁧′′′′‒

⁁⁔⁥′′′′⁤⁨′′′′⁖‒?!⁓⁞⁧′′′′‒

⁆⁥⁧⁝⁧⁔⁓‒′′⁠⁦′′′′⁠⁠⁓‒⁩⁓⁥‒⁥⁦⁡⁢⁢′′′′⁖‒

‒⁖⁧′′′′‒⁦⁡‒⁓‒⁔⁛⁙‒⁦⁫⁢⁚⁡⁡⁠‒

‸⁓⁛⁞⁧⁤′′′′‒⁡⁘‒‵‵⁓⁦⁓‒⁦⁤⁓⁠⁥⁘′′′′⁤‒‒

⁘⁤⁡ ‒⁁⁠⁥⁓⁞⁓‒

⁁⁠⁥⁓⁞⁓‒′′⁠⁦′′′′⁠⁠⁓‒⁩⁓⁥‒⁥⁦⁡⁢⁢′′′′⁖‒

Figure 5. dUT1 values of the ultra-rapid dUT1 experiment during CONT11.

-0.3160

-0.3164

-0.3168

-0.3172

-0.3176

0:00 4:00 8:00 12:00 16:00 20:00 24:00

Time [ 2011/9/27]

UT1-UTC [sec]

⁂⁤′′′′⁖⁛⁕⁦′′′′⁖‒?!⁓⁞⁧′′′′‒

⁁⁔⁥′′′′⁤⁨′′′′⁖‒?!⁓⁞⁧′′′′‒

-0.3156

The difference between predicted

and Observed Value is about 100 usec.

Figure 6. dUT1 values of the ultra-rapid dUT1 experiment on September 27.

4. Staff

• Kensuke Kokado (GSI): Correlation Chief, Management of overall activity

• Kentaro Nozawa (AES): Main operator of the analysis work

5. Plan for 2012

We will continuously implement an ultra-rapid dUT1 or EOP measurement with selected IVS

24-hour sessions and try to submit the rapid solutions to the IVS data center. In addition, we plan

to analyze the data to determine the optimum analysis method for each 24-hour session.

IVS 2011 Annual Report 267
USNO VLBI Analysis Center United States Naval Observatory

U.S. Naval Observatory VLBI Analysis Center

David A. Boboltz, Alan L. Fey, Nicole Geiger, Kerry A. Kingham, David M. Hall

Abstract

This report summarizes the activities of the VLBI Analysis Center at the United States Naval

Observatory for calendar year 2011. Over the course of the year, Analysis Center personnel continued

analysis and timely submission of IVS-R4 databases for distribution to the IVS. During the 2011

calendar year, the USNO VLBI Analysis Center produced one periodic global solution designated

usn2011a. Earth orientation parameters (EOP), based on this solution and updated by the latest

diurnal (IVS-R1 and IVS-R4) experiments, were routinely submitted to the IVS. Sinex files based

upon the bi-weekly 24-hr experiments were also submitted to the IVS.

During the 2011 calendar year, Analysis Center personnel focused much of their efforts on both the

DiFX software correlator implementation at USNO and on implementing a program of daily Intensive

sessions to measure UT1–UTC using two stations of the Very Long Baseline Array (VLBA) operated by

the National Radio Astronomy Observatory (NRAO). High-speed network connections were established

to the Mauna Kea, HI and Pie Town, NM stations for the purpose of electronically transferring the

data back to USNO for correlation and analysis.

1. Introduction

The USNO VLBI Analysis Center is supported and operated by the United States Naval

Observatory (USNO) in Washington, DC. The primary services provided by the Analysis Center

are the analysis of diurnal experiments, the production of periodic global Terrestrial Reference

Frame (TRF) and Celestial Reference Frame (CRF) solutions, and the submission to the IVS

of Intensive (EOP-I) and session-based (EOP-S) Earth orientation parameters based on USNO

global TRF solutions. Analysis Center personnel maintain the necessary software required to

continue these services to the IVS including periodic updates of the GSFC CALC/SOLVE software

package. In addition to operational VLBI analysis, Analysis Center personnel are actively engaged

in research related to future reference frames, the electronic transfer of VLBI data, and software

correlation.

2. Current Analysis Center Activities

2.1. IVS Experiment Analysis and Database Submission

During the 2011 calendar year, personnel at the USNO VLBI Analysis Center continued to

be responsible for the timely analysis of the IVS-R4 experiments, with the resulting databases

submitted within 24 hours of correlation for dissemination by the IVS. Analysis Center personnel

continue to be responsible for the analysis and database submission for the periodic IVS-CRF

experiments. In 2011, USNO scheduled and analyzed 11 CRF related experiments including IVSCRF62 through IVS-CRF66 and IVS-CRDS50 through IVS-CRDS55. The analyzed databases

were submitted to the IVS. Analysis Center personnel also continued analyzing IVS Intensive

experiments for use in the USN-EOPI time series.

268 IVS 2011 Annual Report
United States Naval Observatory USNO VLBI Analysis Center

2.2. Global TRF Solutions, EOP, and Sinex Submission

USNO VLBI Analysis Center personnel continued to produce periodic global EOP/TRF solutions over the course of the 2011 calendar year. This year a single solution (usn2011a) was produced

and submitted to the IVS. Analysis Center personnel continued to submit the USN-EOPS series,

which are now based upon the 2011a solution and are updated with new IVS-R1/R4 experiments.

The updated EOPS series was submitted to the IVS twice weekly within 24 hours of experiment

correlation and is included in the IERS Bulletin A. Analysis Center personnel also continued routine submission of Sinex format files based upon the 24-hr VLBI sessions. In addition to EOPS

and Sinex series, USNO VLBI Analysis Center personnel continued to produce and submit an

EOPI series based upon the IVS Intensive experiments.

2.3. Celestial Reference Frame (CRF)

During the 2011 calendar year, Analysis Center personnel continued work on the production

of global CRF solutions. In 2011, a single solution (crf2011a) was produced for local use within

USNO. The global CRF solutions produced are routinely compared to the current ICRF (ICRF2).

2.4. Software Correlator

Over the course of the 2011 calendar year, Analysis Center personnel continued the implementation, testing, and evaluation of the DiFX software correlator. The software correlator implementation at USNO currently consists of four nodes (workstations) with a total of 28 processing

cores and two Mark 5 data playback units. The correlator nodes and Mark 5 units are connected

through a 1 Gbps ethernet switch. Since April 2011, Analysis Center personnel have been regularly correlating one IVS-INT1 (Kk-Wz) Intensive session per week on the software correlator in

parallel with the WACO hardware correlator. In addition, the post-correlation calibration path

has been fully exercised with the DiFX output converted to traditional Mark IV-style correlator

output using the difx2mark4 software developed at Haystack Observatory. The Mark IV output

has been fringe-fitted and calibrated within FOURFIT/HOPS, and geodetic databases have been

produced using DBEDIT.

Analysis Center personnel continue to interface with colleagues from various institutions within

the DiFX consortium, and they attended the DiFX meetings in Bonn, Germany (March 2011) and

at Haystack Observatory in Westford, MA (December 2011). To facilitate the smooth transition

to the software correlator and to expand USNO’s involvement in the DiFX consortium, a software

engineer (Dr. John Spitzak) was hired to work on the development of a graphical user interface

(GUI) for DiFX.

2.5. VLBA Intensive Experiments

Over the course of the 2011 calendar year, Analysis Center personnel made considerable

progress with regard to the implementation of a new Intensive series using two stations of the

VLBA. USNO contracted with NRAO and the University of Hawaii to install and maintain 1Gbps

fiber links to the stations at Pie Town, NM and Mauna Kea, HI. These fiber links were in service

on March 1, 2011 for PT and on July 15, 2011 for MK. In addition, both stations were outfitted

with the network infrastructure and new Mark 5C units necessary to record the data and e-transfer

it back to USNO. Both fiber links have been tested, and data have been transmitted at speeds up

IVS 2011 Annual Report 269
USNO VLBI Analysis Center United States Naval Observatory

to 400 Mbps from each station back to USNO via the links.

A series of test observations began in September 2011 using the upgraded MK and PT stations.

The wide-band tests were conducted using the newly available digital backends with sixteen 32

MHz wide channels at a data rate of 2 Gbps. Intensives run for 40 minutes with approximately 12

seconds per scan on source resulting in roughly 30 – 35 scans per session. The 12-second scan length

allows the data size to be ∼100 GB per station per session, which makes for more manageable

e-transfers. From the start, the VLBA Intensive tests have been correlated on the DiFX software

correlator. Mark IV style output is generated using the difx2mark4 software, and the data are

fringe-fitted using FOURFIT/HOPS. Geodetic-style databases are generated with DBEDIT and

analyzed within SOLVE. The analyzed databases have been put into a SOLVE batch solution

along with the other Intensive sessions for comparison. Figure 1 shows the differences between

the VLBA MK-PT baseline UT1–UTC results and IERS C04 from October 2011 through January

2012. Differences between IERS C04 and the USN-EOPI and USN-EOPS series are also shown

for comparison.

Figure 1. Differences in UT1-UTC between data from the VLBA Intensive test sessions using the MKPT baseline and IERS C04. Also shown are differences between IERS C04 and both the USN-EOPI and

USN-EOPS standard series for comparison. Error bars are 1σ formal uncertainties.

The plan is for these sessions to become operational in the summer of 2012. Once fully operational, they will be scheduled as IVS-INT4 Intensive sessions, and data will be released to the IVS

270 IVS 2011 Annual Report
United States Naval Observatory USNO VLBI Analysis Center

for community-wide distribution.

3. Staff

The staff of the VLBI Analysis Center is drawn from individuals in both the Astrometry and

Earth Orientation departments at the U.S. Naval Observatory. The staff and their responsibilities

are as follows:

Name Responsibilities

David Boboltz VLBA Intensive program; software correlator implementation; VLBI

data analysis.

Alan Fey Periodic global CRF/TRF/EOP solutions and comparisons; CRF

densification research; software correlator implementation; VLBI

data analysis.

Nicole Geiger software correlator implementation; VLBI data analysis; EOP,

database and Sinex submission.

Kerry Kingham Hardware correlator interface; software correlator implementation;

VLBI data analysis.

David Hall Hardware correlator interface; software correlator implementation;

VLBI data analysis.

4. Future Activities

For the upcoming year, January 2012 – December 2012, USNO VLBI Analysis Center personnel

plan to accomplish the following activities:

• Continue testing and evaluation of the USNO implementation of the DiFX software correlator. Streamline pre- and post-correlation processing.

• Procure a new software correlator system to replace the current WACO hardware correlator.

• Continue testing the electronic transfer of VLBI Intensive data from the MK and PT VLBA

stations with regular operations beginning summer 2012.

• Continue analysis and submission of IVS-R4 experiments for dissemination by the IVS.

• Continue the production of periodic global TRF solutions and the submission of EOP-S

estimates to the IVS updated by the IVS-R1/R4 experiments.

• Continue submission of Sinex format files based on the 24-hr experiments and begin production of a Sinex series based upon the Intensive experiments.

• Continue the analysis of Intensive experiments and submission of EOP-I estimates to the

IVS.

• Continue the scheduling, analysis, and database submission for IVS-CRF and IVS-CRDS

experiments.

• Continue the production of periodic global CRF solutions.

IVS 2011 Annual Report 271
USNO Analysis Center for Source Structure United States Naval Observatory

USNO Analysis Center for Source Structure Report

Alan L. Fey, David A. Boboltz, Ralph A. Gaume, Kerry A. Kingham

Abstract

This report summarizes the activities of the United States Naval Observatory Analysis Center for

Source Structure for calendar year 2011 and the activities planned for the year 2012.

1. Analysis Center Operation

The Analysis Center for Source Structure is supported and operated by the United States

Naval Observatory (USNO). The charter of the Analysis Center is to provide products directly

related to the IVS determination of the “definition and maintenance of the celestial reference

frame”. These include, primarily, radio frequency images of International Celestial Reference

Frame (ICRF) sources, intrinsic structure models derived from the radio images, and an assessment

of the astrometric quality of the ICRF sources based on their intrinsic structure.

The Web server for the Analysis Center is hosted by the USNO and can be accessed by pointing

your browser to

http://rorf.usno.navy.mil/ivs saac/

The primary service of the Analysis Center is the Radio Reference Frame Image Database

(RRFID), a Web accessible database of radio frequency images of ICRF sources. The RRFID

contains 7,279 Very Long Baseline Array (VLBA) images of 782 sources at radio frequencies of

2.3 GHz and 8.4 GHz. Additionally, the RRFID contains 1,706 images of 282 sources at frequencies

of 24 GHz and 43 GHz. The RRFID can be accessed from the Analysis Center Web page or directly

at

http://rorf.usno.navy.mil/rrfid.shtml

The RRFID also contains 74 images of 69 Southern Hemisphere ICRF sources using the Australian Long Baseline Array (LBA) at a radio frequency of 8.4 GHz.

Images of ICRF sources can also be obtained from the Bordeaux VLBI Image Database (BVID)

at

http://www.obs.u-bordeaux1.fr/m2a/BVID/

2. Current Activities

Maintaining the Radio Reference Frame Image Database (RRFID) as a Web accessible database

of radio frequency images of ICRF sources.

3. Staff

The staff of the Analysis Center is drawn from individuals who work at the USNO. The staff

are: Alan L. Fey, David A. Boboltz, Ralph A. Gaume, and Kerry A. Kingham.

272 IVS 2011 Annual Report
United States Naval Observatory USNO Analysis Center for Source Structure

4. Future Activities

The Analysis Center currently has a program of active research investigating the effects of

intrinsic source structure on astrometric position determination. Results from this program are

published in the scientific literature.

The following activities for 2012 are planned:

• Continue imaging and analysis of VLBA 2.3/8.4/24/43 GHz experiments.

• Maintain the Radio Reference Frame Image Database (RRFID) as a Web accessible database

of radio frequency images of ICRF sources.

5. Relevant Publications

Publications of relevance to Analysis Center activities:

• “TANAMI: tracking active galactic nuclei with austral milliarcsecond interferometry. I. Firstepoch 8.4 GHz images,” Ojha, R., Kadler, M., B ̈ock, M., Booth, R., Dutka, M. S., Edwards,

P. G., Fey, A. L., Fuhrmann, L., Gaume, R. A., Hase, H., Horiuchi, S., Jauncey, D. L.,

Johnston, K. J., Katz, U., Lister, M., Lovell, J. E. J., M ̈uller, C., Pl ̈otz, C., Quick, J. F. H.,

Ros, E., Taylor, G. B., Thompson, D. J., Tingay, S. J., Tosti, G., Tzioumis, A. K., Wilms,

J. and Zensus, J. A. 2010, A&A, 519, 45

• “The Celestial Reference Frame at 24 and 43 GHz. I. Astrometry,” Lanyi, G. E., Boboltz,

D. A., Charlot, P., Fey, A. L., Fomalont, E. B., Geldzahler, B. J., Gordon, D., Jacobs, C. S.,

Ma, C., Naudet, C. J., Romney, J. D., Sovers, O. J. and Zhang, L. D. 2010, AJ, 139, 1695

• “The Celestial Reference Frame at 24 and 43 GHz. II. Imaging,” Charlot, P., Boboltz, D.

A., Fey, A. L., Fomalont, E. B., Geldzahler, B. J., Gordon, D., Jacobs, C. S., Lanyi, G. E.,

Ma, C., Naudet, C. J., Romney, J. D., Sovers, O. J. and Zhang, L. D. 2010, AJ, 139, 1713

IVS 2011 Annual Report 273

Technology Development Centers

Technology Development Centers

Geodetic Survey Division, Natural Resources Canada Canadian TD Center

Canadian VLBI Technology Development Center

Bill Petrachenko

Abstract

The Canadian VLBI Technology Development Center (TDC) is involved in activities related to the

realization of VLBI2010.

1. Introduction

The Canadian TDC is a collaborative effort of the National partners interested in the advancement of VLBI technology, namely the Geodetic Survey Division of Natural Resources Canada

(GSD/NRCan) and the Dominion Radio Astrophysical Observatory (DRAO) of the Herzberg Institute for Astrophysics of the National Research Council of Canada (DRAO/HIA/NRC).

2. VLBI2010 Committee (V2C)

The Canadian TDC is primarily focused on encouraging the realization of VLBI2010. This is

done by Bill Petrachenko of NRCan, who is chairman of the V2C. In collaboration with others,

this year’s activity focused on the following areas.

• Development of algorithms for processing broadband data.

• Development of FPGA algorithms for VLBI2010 digital back ends.

• Development of specifications for VLBI2010 sub-systems.

• Execution of studies into the nature, impact, and mitigation of Radio Frequency Interference

(RFI)

• Development of strategies for the mitigation of the impact of source structure.

• Participation in the VLBI2010 Project Executive Group.

3. DRAO Activities

Under the leadership of Gordon Lacy, designs are complete and fabrication plans in place for a

15-m off-axis Gregorian top-fed composite antenna that is light, stiff, efficient, and cost effective.

Under the leadership of Brent Carlson, correlator development at DRAO is focused on novel

designs for the SKA.

Development also progresses in the areas of focal plane arrays and a general purpose highcapacity multi-FPGA signal processing platform.

IVS 2011 Annual Report 277
FFI TD Center Forsvarets forskningsinstitutt (FFI) (Norwegian Defence Research Establishment)

FFI Technology Development Center - Software Development

Per Helge Andersen

Abstract

This report discusses the current status of the FFI Technical Development Center as well as upcoming changes.

1. Status and Future Changes

FFI is currently an Associate Analysis Center for IVS and ILRS, and a Technology Development

Center for IVS. The Norwegian Mapping Authority (NMA) and FFI have a close cooperation in

the analysis of space geodetic data using the GEOSAT software. NMA has recently been given

the status of an Associate Analysis Center of IVS (28 October 2010). The plan is that NMA will

apply to become a Technology Development Center for IVS and that FFI will end this formal role

in 2012. The GEOSAT TD and AC activities at both institutions will be coordinated by NMA.

This also implies that FFI will stop being an IVS Associate Analysis Center in 2012.

2. The GEOSAT Software and Activities in 2011

FFI’s contribution to the IVS as a Technology Development Center focuses primarily on the

development and validation of the GEOSAT software for a combined analysis at the observation

level of data from VLBI, GPS (ground-based and LEO), SLR, DORIS, altimetry, accelerometry,

and GRACE KBR. The advantages of the combination of independent and complementary space

geodetic data at the observation level is discussed in Andersen [1].

Space borne accelerometry has been implemented, and a small set of data has been tested

(GOCE and GRACE). Software to convert space-based gravity models and accelerometry / gradiometry data to geoid information is being implemented right now. A complete production line

for altimetry (Topex, ENVISAT, JASON 1 and 2) has been implemented and tested. Map animations of sea level rise have been developed, so far based on GDR-orbits. Software for the analysis

of cross-over data is being developed right now. In the near future the altimeter analyses will be

based on orbits determined with GEOSAT instead of the GDR-orbits, to be more consistent with

the TRF realized with GEOSAT. The cross-over software can be used for quality evaluation of the

GDR and GEOSAT orbits.

The GEOSAT orbit model has been validated against external LEO orbits. The RMS difference between JPL GRACE orbits and internal GEOSAT orbits is typically 4 mm in each Cartesian

direction. The corresponding RMS difference between external GOCE orbits (ESA official, approximately 250 km altitude) and internal GEOSAT orbits is typically 11 mm. This work will continue

in 2012.

A lot of work has been done to improve the consistency between VLBI results from GEOSAT

and results from the other IVS Analysis Centers.

• The VMF1 model for tropospheric refraction has been implemented.

• A LSQ-module quite similar to GSFC SOLVE, including continuous linear spline parameter

representations, has been implemented and tested. The plan is however to use the UD-filter

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Forsvarets forskningsinstitutt (FFI) (Norwegian Defence Research Establishment) FFI TD Center

estimator available in GEOSAT for the production of SINEX files. The LSQ estimator was

implemented for the purpose of data editing and as an external check of the filter solutions.

• A misinterpretation of the NGS-format has been corrected, giving more consistent estimates

of UT1-UTC.

• A number of options have been implemented for the detection and correction of clock breaks,

for the suppression of one or more individual stations, for manual detection and rejection of

individual outlier observations, and for validating the results.

NMA has now taken over a version of VLBI/GEOSAT with these improvements, and a production

line for the routine generation of normal equations for IVS combination will be established in the

near future. There are now options in GEOSAT so that the VLBI model is in compliance with

the other VLBI analysis software packages.

3. Staff

Dr. Per Helge Andersen - Research Professor of Forsvarets forskningsinstitutt (FFI and NMA).

Dr. Eirik Mysen - Research geodesist at the Norwegian Mapping Authority (NMA). Dr. Kristian

Breili - Research geodesist at the Norwegian Mapping Authority (NMA). Dr. Halfdan Kierulf

- Research geodesist at the Norwegian Mapping Authority (NMA). Dr. Oddgeir Kristiansen -

Section Manager at the Norwegian Mapping Authority (NMA).

References

[1] Andersen, P. H. Multi-level arc combination with stochastic parameters. Journal of Geodesy (2000) 74:

531-551.

IVS 2011 Annual Report 279
GSFC Technology Development Center NASA Goddard Space Flight Center

GSFC Technology Development Center Report

Ed Himwich, John Gipson

Abstract

This report summarizes the activities of the GSFC Technology Development Center (TDC) for

2011 and forecasts planned activities for 2012. The GSFC TDC develops station software including

the Field System (FS), scheduling software (SKED), hardware including tools for station timing and

meteorology, scheduling algorithms, and operational procedures. It provides a pool of individuals to

assist with station implementation, check-out, upgrades, and training.

1. Technology Center Activities

The GSFC IVS Technology Development Center (TDC) develops hardware, software, algorithms, and operational procedures. It provides manpower for station visits for training and

upgrades. Other technology development areas at GSFC are covered by other IVS components

such as the GSFC Analysis Center. The current staff of the GSFC TDC consists of John Gipson

and Ed Himwich, both employed by NVI, Inc. The remainder of this report covers the status of

the main areas supported by the TDC.

2. Field System

The GSFC TDC is responsible for development, maintenance, and documentation of the Field

System (FS) software package. The FS provides equipment control at VLBI stations. It interprets

the .snp schedule and .prc procedure files (both as prepared by DRUDG from the .skd schedule).

The FS controls the antenna, data acquisition hardware, and related ancillary equipment needed

for making VLBI measurements. All major VLBI data acquisition backends are supported. The

FS is customizable to allow it to control station specific equipment. It is used at all the IVS

Network Stations (i.e., more than 30) and also at many stations that do VLBI only for astronomical

observations. The only major VLBI facilities not using it are the VLBA and VERA.

There were no new releases of the FS during this period. However, several development projects

were underway:

• Patriot 12-m Interface. A preliminary interface to Patriot 12-m antennas was developed.

This was implemented using the position and velocity tracking mode in the Patriot antenna

controller. All aspects of this appear to work, but final testing is delayed until next year

when the antenna controller and receiver will be more nearly in their final configuration.

• Satellite Tracking. A satellite tracking capability was developed for the FS. This will allow

an antenna to be pointed at a satellite in one of three modes: (1) Ephemeris, (2) Az-El, or

(3) RA-Dec. The Ephemeris tracking mode is the most flexible and precise. A one second

ephemeris for several hours is built in memory, which the antcn antenna interface can use

to guide the antenna. However, this requires special programming of the antenna interface,

and some antennas may not be able to support this mode. The Az-El mode is useful for

geo-synchronous or possibly slowly moving satellites, if the antenna being used supports

commanding with fixed Az-El coordinates. The RA-Dec mode is the most universal since all

antennas support RA-Dec pointing, but it may have limited usefulness if the satellite is not

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NASA Goddard Space Flight Center GSFC Technology Development Center

moving at a nearly sidereal rate. It is expected that the Az-El and RA-Dec modes will be

enhanced to allow periodic recommanding of the position. This may help with tracking slow

moving objects. However, depending on the behavior of the antenna, this may introduce

unacceptable jumps in the antenna tracking. The open source predict program is used to

calculate the pointing angles from the orbital elements.

• Holography. A new SNAP command holog was developed to support holographic measurements of antennas. In its simplest form, this command will move an antenna in a boustrophedon pattern around a grid centered on either an Az-El or RA-Dec commanded position.

A user-defined SNAP procedure is run to collect data at each grid point. Various options

are available including specifying a “return to center” interval for recalibration, changing the

order in which the grid points are visited, and allowing single “cuts” to be made on each

axis.

These new capabilities will be included in FS releases next year. Several other improvements

are expected in future releases, including:

• Support for DBBC and RDBE racks

• Support for Mark 5C recorders

• Use of idl2rpc for remote operation

• A complete update to the documentation and conversion to a more modern format that will

be easier to use

• Conversion of the FORTRAN source to use the gfortran compiler; this will enable use of the

source level debugger, gdb, for development and field debugging

• Chekr support for Mark 5A and Mark 5B systems

• Use of the Mark IV Decoder for phase-cal extraction in the field

• FS Linux 9 (based on Debian squeeze) distribution

• Support for periodic firing of the noise diode during observations

• Distribution of the new gnplt.

3. SKED and DRUDG

The GSFC TDC is responsible for the development, maintenance, and documentation of SKED

and DRUDG. These two programs are very closely related, and they operate as a pair for the

preparation of the detailed observing schedule for a VLBI session and its proper execution in the

field. In the normal data flow for geodetic schedules, first SKED is run at the Operation Centers

to generate the .skd file that contains the full network observing schedule. Then stations use the

.skd file as input to DRUDG for making the control files and procedures for their station. Catalogs

are used to define the equipment, stations, sources, and observing modes which are selected when

writing a schedule with SKED.

Changes to SKED and DRUDG are driven by changes in equipment and by feedback from the

users. The following summarizes some of the important changes to these programs in 2011 and

plans for 2012.

IVS 2011 Annual Report 281
GSFC Technology Development Center NASA Goddard Space Flight Center

3.1. SKED

The only changes made to SKED this year were bug fixes and minor enhancements. The

following is a list of bug fixes:

• Fixed a problem with writing out the lower sideband in VEX files.

• Fixed an issue in writing schedule files if the fan-out mode varied from station to station.

• Fixed a bug in tag-along mode that affects the calculation of slewing time. Previously the

slewing time started from the last time the antenna was used. However, if the last time a

station observed was a long time ago, the calculation was not accurate and could lead to

problems with cable wrap.

• Made the list of valid correlators consistent with the list in the VLBI master files.

Following is a list of minor enhancements:

• Added the parameter MaxAngle which specifies the maximum distance to move.

• Added the command NOW <time> which sets the time of all stations to the current time.

This was done to aid in the scheduling of CONT11.

• Increased the number of downtimes from 20 to 2000. CONT11 required around 450.

In addition we continued working on updating the SKED documentation. The last time the

documentation was revised was in 1996. We expect to finish this project in 2012.

3.2. DRUDG

No changes were made to drudg during 2011.

3.3. Plans for Next Year

Plans for next year include:

• Releasing the new SKED documentation;

• Making VEX the native format for SKED and DRUDG

• Better source modeling

• Modifying SKED and DRUDG as necessary to support VLBI2010.

282 IVS 2011 Annual Report
MIT Haystack Observatory Haystack Technology Development Center

Haystack Observatory Technology Development Center

Chris Beaudoin, Brian Corey, Arthur Niell, Alan Whitney

Abstract

Technology development at MIT Haystack Observatory was focused on four areas in 2011: 1)

Development of VLBI2010 receiver hardware, 2) Digital Backend development, 3) RFI compatibility

at GGOS stations, and 4) Mark 6 VLBI Data System development.

1. Development of VLBI2010 Receiver Hardware

In 2011 Haystack Observatory was engaged in the development of a second receiver frontend

for the new GGAO Cobham 12-m antenna as well as for the Westford antenna. Both receivers

are based on the Caltech-designed/built QRFH shown in Figure 1 and the CRYO1-12 low-noise

amplifiers, also developed at Caltech. The geometric design of these two feeds is quite different;

the GGAO 12-m QRFH is circular [1] while the Westford QRFH is square. The difference in the

geometric design is attributed to the difference in the Westford and GGAO 12-m reflector optical

configurations; the GGAO 12-m requires a feed beamwidth of 100◦ while Westford requires a feed

having 160◦ beamwidth.

Prior to installing the QRFH-based frontend on the GGAO 12-m antenna, Y-factor measurements of the frontend were conducted; these measurements demonstrated 30K noise temperature

over 2-12 GHz. After installing the QRFH-based receiver on the GGAO 12-m, the broadband

SEFD of the receiver was estimated from on-source/off-source total power measurements of Taurus A. Initially, the SEFD performance was poorer than expected due, it was discovered, to a

misalignment of the subreflector. Repeated SEFD measurements were utilized to fine tune the

position of the subreflector, and peak sensitivity was achieved when the subreflector was 15.9 mm

further from the vertex than the original position. After re-aligning the subreflector, the receiver

temperature was estimated by the Y-factor method, and the SEFD was immediately re-measured.

Given the radio telescope’s SEFD and system temperature, the aperture efficiency of the telescope

was computed. Figure 2 shows the broadband aperture efficiency of the radio telescope as estimated from the measurements collected on day 249. The theoretically expected aperture efficiency

of the 12-m radio telescope under illumination by its QRFH was computed by William Imbriale

(JPL) using a custom physical-optics solver; Figure 2 shows this expectation as well. Given that

the solution does not incorporate blockage losses from the support struts and subreflector, the

agreement shown in Figure 2 is considered to be quite reasonable. The expected efficiency loss due

to the supporting structure is under investigation.

Figure 2 also shows the system temperature of the complete receiver system, from frontend

to backend in the control room, as measured on days 249 and 336. As can be seen, the system

temperature on the first day increases significantly at higher frequencies. It was subsequently

discovered that this was due to an unspecified increase in the noise figure of the microwave-overfiber link. Additional gain, preceding the fiber link, was introduced to overcome the high frequency

noise figure (at the expense of less saturation overhead) and led to the substantial improvement

in receiver system temperature as shown in Figure 2 for day 336. Given the aperture efficiency

reported in Figure 2 and the improvements in system temperature (day 336), the SEFD over the 3-

12 GHz band is expected to be below 2500 Jy, which is the VLBI2010 goal. The fiber link was also

IVS 2011 Annual Report 283
Haystack Technology Development Center MIT Haystack Observatory

being driven into saturation by strong S-band RFI at GGAO. For this reason, a 3.9 GHz highpass

pre-link filter was installed in the receiver; hence the system temperatures shown in Figure 2 are

limited to 3 GHz on the low end of the spectrum. Until the GGAO receiver can accommodate

S-band observing, it will not be fully compliant with VLBI2010 specifications. This is a topic of

current investigation.

Figure 1. Broadband microwave feeds for NASA broadband receivers: (left) GGAO 12-m QRFH feed,

(right) Westford 18-m QRFH feed.

Figure 2. Simulated and measured (on day 249) aperture efficiencies of the GGAO 12-m under illumination

by the QRFH. Also shown is the measured system temperature of the GGAO 12-m receiver on days 249

and 336 of year 2011, before and after the introduction of additional pre-fiber gain, respectively. Strong 4

GHz RFI was present on day 336.

2. Digital Backend Development

In the past year collaborations between Haystack and NRAO have continued to further the

development of the RDBE subsystem. In 2011 the RDBE geodetic polyphase filter bank (PFB)

284 IVS 2011 Annual Report
MIT Haystack Observatory Haystack Technology Development Center

personality bitcode version 1.4 was officially released, and RDBEs can now be ordered through

DigiCom1for new station construction and current station upgrades. The RDBE provides 16

user-selectable 32 MHz channels from a choice of 16 uniformly-spaced channels in each of the

512 MHz IF inputs. Initially, a PFB personality providing 8 MHz channels was also planned for

development for compatibility with operational S/X observations. However, a development in the

DiFX correlator now supports the correlation of channels of differing bandwidth, provided there

is common spectral overlap in the channels. This feature of the DiFX software provides the final

missing link required to allow RDBE backends to co-observe with stations incorporating legacy

baseband converters.

3. RFI Compatibility at GGOS Stations

Haystack Observatory has been involved in studies of the compatibility of DORIS and the SLR

aircraft radar with the VLBI2010 receiver since these two active techniques pose a potential to

degrade VLBI data quality and, in the worst case, damage the frontend of the VLBI receiver at a

fundamental GGOS station. To support this effort, X-band power level measurements of the SLR

aircraft tracking radars at GGAO were conducted to verify the expected radiation properties of

these systems. The results of this study have been reported in [2].

As described in [2] GGAO operates two SLR systems, NGSLR and Moblas7, both of which

employ aircraft-tracking radars. To avoid potential damage to the 12-m frontend electronics, both

SLR systems and the 12-m system now have programmed pointing masks to exclude observations

within 30 degrees of the other technique. These masks are not intended to avoid degradation

of broadband VLBI data; such masks would be prohibitively large and would severely impact

operations [3]. For this reason, Haystack is involved in an electromagnetic-barrier study, the goal

of which is to reduce the pointing restrictions on the unshielded radar and VLBI systems. The

DORIS transmitter at GGAO does not pose a threat of damaging the electronics of the 12-m

receiver.

4. Mark 6 Data System Development

The demand for greater VLBI observation sensitivity continues to push required dataacquisition and playback rates to higher and higher levels. The current Mark 5 generation of

data systems tops out at sustained 4 Gbps per system. However, near-term demands are for 8

Gbps, pushing to sustained recording and playback at 16 Gbps within about a year. These rates are

required to support the 1-mm global measurement precision demanded by the VLBI2010 system.

In order to meet these needs, Haystack Observatory, in collaboration with the High-End Network Computing Group at NASA/GSFC, has embarked on the design of a 16-Gbps VLBI data

system. Unlike its Mark 5 predecessor, the Mark 6 system is based entirely on commercial-off-theshelf hardware. The only exception is the continued use of customized 8-disk modules which are

similar to the disk modules used in the Mark 5 system and which provide the necessary portability

demanded by the geodetic VLBI application. We are partnering with Conduant Corporation of

Longmont, CO, who also partnered with Haystack on the Mark 5 system, for development of specific items to support the custom Mark 6 disk modules, and who will also act as the manufacturer

1Digicom Electronics, Inc. info@digicom.org

IVS 2011 Annual Report 285
Haystack Technology Development Center MIT Haystack Observatory

and distributor of Mark 6 systems for the global VLBI community.

Figure 3. Diagram of the experimental setup for the 16 Gbps Mark 6 demonstration.

The cost of the Mark 6 system will be lower than that of the Mark 5 system, but the data-rate

capability will be four times greater. This will help to significantly reduce the cost of supporting

the new demand for higher dates. The Mark 6 system is expected to be available for operational

use in the latter half of 2012.

In late October 2011, early Mark 6 prototype systems were used in a VLBI demonstration

experiment between the Westford 18-m and GGAO 12-m antennas. Figure 3 shows a diagram of

the experiment setup. Eight duplicated 512 MHz bands were processed through RDBE backends to

produce four 10GigE data streams of 4 Gbps each, which were recorded at each station to 32 disks

on a Mark 6 system. The data were processed with the DiFX correlator at Haystack Observatory.

The cross-correlation of all eight bands showed nominal results, verifying the operation of the

prototype Mark 6 system.

Acknowledgements

We wish to thank Ahmed Akigray (Caltech), Sandy Weinreb (Caltech), and Bill Imbriale (JPL)

for their contributions to the development of the GGAO and Westford receiver frontends.

References

[1] Akgiray, A., Weinreb, S., Imbriale, W., and Beaudoin, C. “Circular Quadruple-Ridged Flared Horn

Achieving Near-Constant Beamwidth Over Multi-Octave Bandwidth; Design, Measurements and System Performance,” Submitted for Publication to IEEE Transactions on Antennas and Propagation.

[2] Beaudoin, C. and Cappallo, S., MOBLAS7 and NG SLR Radar Power Level Measurements Collected

at GGAO, MIT Haystack Observatory VLBI Broad Band Memo Series, No. 37, 2011.

[3] Beaudoin, C., Corey, B.E., Petrachenko, W.T., “Radio frequency compatibility of VLBI, SLR, and

DORIS at GGOS stations,” poster presented at AGU 2010 fall meeting in San Francisco, CA.

286 IVS 2011 Annual Report
Institute of Applied Astronomy of Russian Academy of Sciences IAA Technology Development Center

IAA Technology Development Center Report 2011

Dmitry Marshalov, Evgeny Nosov, Leonid Fedotov, Dmitry Ivanov, Andrey Karpichev

1. R1002M Data Acquisition System (DAS)

The new DAS R1002M is developed by IAA RAS for replacement of existing analog DASs

of the VLBI network “Quasar” [1]. The R1002M system was set in operation at the Svetloe,

Zelenchukskaya, and Badary observatories.

R1002M uses digital signal processing on video frequencies and provides enhanced performance.

It is compatible with existing analog DASs. The system consists of 16 Base Band Converters

(BBC), IF-distributor, Clock Generator, Data Stream Combining Board (DSCB), and auxiliary

units (Figure 1). It has four IF-inputs which can be electronically connected to the BBCs in the

required way by IF-distributor unit. The BBCs’ output data streams are combined via DSCB and

available in its output in VSI-H format with up to 2048 Mbps data rate (Table 1). The DAS is well

suited to work with the Mark 5B+ recording system, but it can also work with Mark 5B in case of

1024 Mbps and lower data rates. For proper synchronization, the DAS is required for 1PPS and 5

or 10 MHz signals. The clock generator automatically determines which input reference frequency

(5 or 10 MHz) is used.

Figure 1. Simplified structure of R1002M DAS and pictures of the BBC and DSCB.

In R1002M the translation to baseband is performed by high quality analog mixer and local

oscillator (LO). The output signals of the mixer are then digitized, and all subsequent processing

is implemented by an FPGA. The digitizing is performed by 2-channels analog-to-digital converter

(ADC) with a sample rate of 64 Msps (Figure 2). To separate the side bands a special multirate

filter bank with complex-valued coefficients was developed and realized as FPGA. Use of this

technique allows the achievement of a relatively high image rejection rate. The typical value for

the digital BBC is −40 to −45 dB (at frequencies below 16 MHz) while in existing analog BBCs

the typical value is about −20 to −25 dB.

A few additional switchable FIR-filters are used for forming six possible bandwidths: 0.5, 2,

4, 8, 16, and 32 MHz. The resulting amplitude-frequency characteristics of the digital BBCs are

made similar to BBCs of existing analog DASs for improving compatibility between the systems.

IVS 2011 Annual Report 287
IAA Technology Development Center Institute of Applied Astronomy of Russian Academy of Sciences

Table 1. R1002M DAS specification

Input frequency range 100 to 1000 MHz

Number of IF-inputs 4

Number of channels (BBCs) 16

Selectable bandwidths 0.5, 2, 4, 8, 16, 32 MHz

Separated sidebands Both lower and upper

Image rejection rate (typ.) −40 to −45 dB

Commutation of input and output signals Electronically

Local oscillators phase noise (rms) ≤ 0.7

◦

(measured in 30 Hz÷30 MHz range)

Ripple of amplitude-frequency response of the BBCs ≤ 0.3 dB

Output data format VSI-H

Output data rate Up to 2 Gbps

Available control interfaces RS-232, RS-485, 100/10 Ethernet

Total dimension (three 19′′ subracks) 445 × 950 × 315 mm

Figure 2. Simplified structure of the BBC.

From November 2011 all observations on the VLBI network “Quasar” have been performed

by using R1002M DAS (Figure 3). It decreases the errors of EOP measurements (root-mean

square deviation from the IERS 08 C04 series) on network “Quasar” to 0.38 mas for Celestial Pole

position, 1 mas for Pole position, and 34 microseconds for Universal Time.

2. Broadband Phase Calibration System

The primary goal of the phase calibration system is to monitor the instrumental phase delay.

For this purpose a spectrally pure reference signal is transmitted by cable to the mirror room of

the radio telescope where it synchronizes generator of very short impulses of about 40 ps duration.

In the current phase calibration system the impulses are injected through direction coupler into

the input of receiver before the first LNA and passed with the received signal through receiver and

data acquisition devices to digitization, after which the phases of the tones are extracted.

The broadband phase calibration system has been developed for the Russian VLBI new generation network. The goal of this phase calibration system is to radiate phase cal impulses from

a special broadband feed (TEM horn, Figure 4) located ahead of the receiving feed. The main

advantage of injecting phase cal ahead of the receiving feed is in putting most of the VLBI signal

path into the phase calibration loop.

The broadband phase calibration system consists of TEM horn connected to the generator of

picosecond-level impulses. The generator is placed into the thermo stating block, providing a time288 IVS 2011 Annual Report
Institute of Applied Astronomy of Russian Academy of Sciences IAA Technology Development Center

Figure 3. R1002M DAS and Mark 5B+ in Svetloe observatory.

Figure 4. TEM horn.

constant temperature. All of the system together with power units is located in the all-weather

plastic case, which easily mounts on a metal ware of a radio telescope.

The breadboard model of the broadband phase calibration system has been mounted on a

radio telescope in the “Svetloe” observatory (Figure 5), and some testing on radiation of a phase

calibration signal through a broadband horn has been carried out.

The impulses of two signals are registered upon exiting the receiver. The first impulse is from

the regular generator of picosecond-level impulses, and the second is from the block of the broadband phase calibration system (Figure 6). These experiments showed the absence of multipath

effects in the external radiation phase cal signal.

However, further research has revealed essential non-uniformity of phase calibration signal in

different bands. Power of a cal signal upon exit of the S and X-band receivers differs by 10 dB.

Analytical estimations (calculated by taking into account horn gain, losses in a radio line and gain

of receivers) and experimental values of phase calibration power upon exit of the S and X-band

receivers are represented in Table 2.

At the same time, in all channels of the receiver equipment the signal has sufficient (and at

places even superfluous) power for the correct operation of the phase calibration system. It means

that additional balance of power at various places along a frequency band is needed. Probably,

the cascade of the adjustable filters located between the picosecond-level generator and the TEM

horn is capable of solving this problem. But it demands additional research.

IVS 2011 Annual Report 289
IAA Technology Development Center Institute of Applied Astronomy of Russian Academy of Sciences

Table 2. Power of a cal signal upon exit of S and X-band receivers

Band Power of a signal upon exit of receivers

Analytical estimations Experimental

X −80 dBm −85 dBm

S −70 dBm −72 dBm

Figure 5. The breadboard model of the broadband phase calibration system mounted on a radio telescope

(“Svetloe” observatory).

Figure 6. Oscillogram of output signal for S-band receiver.

References

[1] S. A. Grenkov, E. V. Nosov, L. V. Fedotov, N. E. Koltsov. A Digital Radio Interferometric Signal

Conversion System. Instruments and Experimental Techniques, 2010, Vol. 53, No. 5. P. 675–681.

290 IVS 2011 Annual Report
Kashima Space Research Center, NICT Technology Development Center at NICT

Technology Development Center at NICT

Kazuhiro Takefuji, Hideki Ujihara

Abstract

The National Institute of Information and Communications Technology (NICT) has led a development of the VLBI technique and has been keeping high activities in both observations and technical

developments. This report gives a review of the Technology Development Center (TDC) at NICT and

summarizes recent activities.

1. NICT as an IVS-TDC and Staff Members

The National Institute of Information and Communications Technology (NICT) has published a newsletter, “IVS NICT-TDC News (former IVS CRL-TDC News)”, at least once

a year in order to inform readers about NICT’s development of VLBI-related technology as

an IVS Technology Development Center. The newsletter is available at the following URL:

http://www2.nict.go.jp/w/w114/stmg/ivstdc/news-index.html. Table 1 lists the staff

members at NICT who are involved in the VLBI Technology Development Center at NICT.

Table 1. Staff Members of NICT TDC as of January 2012 (alphabetical).

AMAGAI, Jun HASEGAWA, Shingo HOBIGER, Thomas ICHIKAWA, Ryuichi

KAWAI, Eiji KONDO, Tetsuro KOYAMA, Yasuhiro MIYAUCHI, Yuka

SEKIDO, Mamoru TAKEFUJI, Kazuhiro TSUTSUMI, Masanori UJIHARA, Hideki

2. Current Status and Activities

2.1. RF Direct Sampling System for Geodetic VLBI

We have carried out a test VLBI experiment by using a so-called “RF direct sampling” technique. In a conventional VLBI system, RF signals are converted to IF band signals, then converted

to baseband signals using an analog baseband converter, then sampled and converted to digital

signals. IF signals travel a few hundred meters down a coaxial cable or an optical cable; so temperature variations will affect the cable and change the internal group delay. Phase calibration, which

inserts 1 or 5 MHz step comb signals in frequency before a low noise amplifier, will compensate

for this group delay. However, if RF signals are sampled just after the low noise amplifier, a phase

calibration system is not necessary. Recently it became possible to sample IF signals directly due

to progress of the sampling device, and then a digital baseband converter, like ADS3000+ [1], was

developed. Now some sampling devices have a wider input frequency bandwidth – more than 10

GHz. If RF signals such as 8 GHz band signals can be sampled directly, an IF converter is omissible

from the receiving system. This will reduce the cost of the system associated with the converter

and will increase the reliability of the system. ADX-831, developed by the ELECS INDUSTRY

CO. LTD., is a sampler that has an input band width of 10 GHz.

IVS 2011 Annual Report 291
Technology Development Center at NICT Kashima Space Research Center, NICT

TSUKUBA 32m KASHIMA 11m

SAMPLER

ADX-831

PC

PLO(8192MHz)

10MHz 1PPS

X-BAND

LNA

AMP

Optical

Fiber

E/O

O/E

ANTENNA 

CABIN

VDIF

OBSERVATION 

ROOM

10G Ether SAMPLER

ADX-831

PC

SG(8192MHz)

10MHz 1PPS

X-BAND

LNA

AMP

Optical

Fiber

E/O

O/E

ANTENNA 

CABIN

VDIF

OBSERVATION 

ROOM

10G Ether

Figure 1. A system block diagram. RF direct sampling was operated at Kashima 11-m and Tsukuba 32-m.

We have carried out a test VLBI

observation with ADX-831 to evaluate the feasibility of the RF direct sampling VLBI. The RF direct

sampling system was installed at the

Tsukuba 32-m and Kashima 11-m

antennas. Figure 1 shows a system block diagram. The RF direct sampling has sampling modes

of 2bit-1024Msps. According to the

Nyquist theorem, it needs 18 GHz

speed to record X-band (9 GHz)

signal. However since the X-band

bandwidth is around 1 GHz, a 1024

MHz sampling speed (under sampling of digital technique) was almost enough. The signal after 1024

MHz sampling (0 to 512 MHz) is exactly the same as the band-filtered

signal (8192 to 8704 MHz). It acts

like a “digital” base band converter.

High order sampling is mainly used

for filtered band; then the sampled band can be reconstructed to the original. But an anti-alias

filter was not inserted before the sampler in this case, so other folded signals from out of band

( ≤ 8192 MHz and ≥ 8704 MHz ) will overlap. The overlapped signal will make noise (system

temperature) increase, reducing the fringe amplitude. But we could detect fringes of overlapped

signals with difference of fringe rotation (Figure 2). So we think that the reduced fringe amplitude

will be canceled after bandwidth synthesis. This technique is named “DSAMS” (Direct Sampling

Applied for Mixed Signals). DSAMS was also adopted to S/X band which were connected after

LNA in RF frequency. Figure 3 shows synthesized S and X-band and their fringes [2].

Frequency: +7680.0 [MHz]

0.0e+00

1.0e-04

2.0e-04

3.0e-04

4.0e-04

5.0e-04

6.0e-04

7.0e-04

-400 -200 0 200 400

Amplitude

Delay [Sample] 

0.0e+00

1.0e-04

2.0e-04

3.0e-04

4.0e-04

5.0e-04

6.0e-04

7.0e-04

-0.4 -0.2 0 0.2 0.4

Amplitude

Rate [ Hz ] 

0.0e+00

1.0e-05

2.0e-05

3.0e-05

4.0e-05

5.0e-05

6.0e-05

7.0e-05

-400 -200 0 200 400

Amplitude

Delay [Sample] 

0.0e+00

1.0e-05

2.0e-05

3.0e-05

4.0e-05

5.0e-05

6.0e-05

7.0e-05

-0.4 -0.2 0 0.2 0.4

Amplitude

Rate [ Hz ] 

Frequency: +8704.0 [MHz]

0.0e+00

5.0e-05

1.0e-04

1.5e-04

2.0e-04

2.5e-04

3.0e-04

3.5e-04

4.0e-04

4.5e-04

-400 -200 0 200 400

Amplitude

Delay [Sample] 

0.0e+00

5.0e-05

1.0e-04

1.5e-04

2.0e-04

2.5e-04

3.0e-04

3.5e-04

4.0e-04

4.5e-04

5.0e-04

-0.4 -0.2 0 0.2 0.4

Amplitude

Rate [ Hz ] 

Frequency: +8192.0 [MHz]

0.0e+00

5.0e-05

1.0e-04

1.5e-04

2.0e-04

2.5e-04

3.0e-04

-400 -200 0 200 400

Amplitude

Delay [Sample] 

0.0e+00

5.0e-05

1.0e-04

1.5e-04

2.0e-04

2.5e-04

3.0e-04

-0.4 -0.2 0 0.2 0.4

Amplitude

Rate [ Hz ] 

Frequency: +7168.0 [MHz]

Figure 2. First fringes for DSAMS (Direct Sampling Applied for Mixed Signals) applied for X-band VLBI.

The sampling mode of ADX-831 is 2bit-1024Msps. All four X-band fringes were simultaneously obtained

with just one sampler.

292 IVS 2011 Annual Report
Kashima Space Research Center, NICT Technology Development Center at NICT

S+X Band character

 @ Kashima 11m

S-Band X-Band

Figure 3. First fringe of DSAMS (Direct sampling applied for mixed signals) applied for geodetic VLBI. The

sampling mode of ADX-831 is 2bit-1024Msps. Fringes of S-band and X-band were simultaneously obtained

with only one sampler.

3. Development of Wide Band Feeds

Figure 4. Experimental elements for wideband feeds.

Wideband feeds are being developed at NICT, NAOJ,

and other Japanese universities for VLBI2010, SKA,

and MARBLE. SKA is an international radio astronomy project for constructing the Square Kilometer Array.

MARBLE is a small portable VLBI station developed by

NICT and GSI in Japan. They all need wideband feed

with a 1:10 or more frequency ratio.

We are now studying Arrayed Travel Wave Antennas

(Arrayed TWA) with dual linear polarization for them,

which is shown in Figure 4. Several elemental feeds were

tested, and their beam patterns were measured at METLAB at Kyoto University in 2011. Grading robes are

clearly seen [Figure 5], because of the lack of a central

feed element, which was not yet placed properly. Also,

numerical simulations were carried out with COMSOL

for the feed elements [Figure 6]. The element size is

(L = 280mm) × (W = 120mm) × (t = 1mm), and the relative permitivity of the dielectric

substrate is tested on ǫr = 1, 2.2, 4, 10. We are now planning to assemble the elements into an

Arrayed TWA for evaluation of beam shaping before installing it on the MARBLE.

IVS 2011 Annual Report 293
Technology Development Center at NICT Kashima Space Research Center, NICT

Farfield pattern of the feed elements at 3 GHz Farfield pattern of the feed elements at 4 GHz

Figure 5. Farfield patterns of experimental elements for the wideband feed [Figure 4].

Ey field on the element at 6 GHz ǫr = 2.2 Ey field on the element at 6 GHz ǫr = 10

Figure 6. Simulated E field component parallel to the substrate of feed element [Figure 4].

References

[1] Takefuji K., Koyama Y., Takeuchi H., First Fringe Detection with Next-Generation A/D Sampler

ADS3000+, IVS TDC News, No. 30, pp.17-21, 2009.

[2] Takefuji K., Kondo T., Sekido M., RF direct sampling applied for geodetic VLBI, 2012, in preparation.

294 IVS 2011 Annual Report
Onsala Space Observatory (OSO) Onsala Space Observatory (OSO), TDC

Onsala Space Observatory – IVS Technology Development Center

Miroslav Pantaleev, Ulf Kylenfall, Leif Helldner, Karl- ̊Ake Johansson, R ̈udiger Haas

Abstract

The present report describes in brief the technical development done during 2011 at the Onsala

Space Observatory in relation to geodetic/astrometric VLBI. The activities focussed on the development

of a front-end for VLBI2010 and the integration of a digital back end in the VLBI system.

1. A Front-end for VLBI2010

During 2011 the activities related to the improvement of the performance of an Eleven feed for

VLBI2010 can be summarized as follows:

• design of passive balun

• design of new feed petals

• cryogenic tests and noise model

This work was done as a collaboration with the Antenna Group at the Department of Signals and

Systems at Chalmers University of Technology. The integration of the Eleven feed into a cryogenic

front-end suitable for VLBI2010 was done in collaboration with Omnisys AB.

1.1. Design of a Passive Balun

Two designs for passive feeding networks were developed at the Antenna Group during 2011.

At the Onsala Space Observatory (OSO) we made the mechanical design suitable for cryogenic

operation and produced two prototypes, see Figure 1.

Figure 1. Balun-fed Eleven feeds with linear taper (left) and with Klopfenstein taper (right).

IVS 2011 Annual Report 295
Onsala Space Observatory (OSO), TDC Onsala Space Observatory (OSO)

The design of the passive feeding solution to the Eleven feed consists of two passive ultra

wideband (UWB) baluns and two UWB power dividers [1]. This feeding solution transforms the

four differential ports of the feed to two single ended ports, one for each polarization. Therefore,

four differential low noise amplifiers (LNAs) can be replaced by two single ended LNAs, which leads

to a much simpler and lower cost system. Two versions of UWB baluns have been developed: a

liner taper and a Klopfenstein taper one. Figure 2 shows the measured performance. The prototype

with the Klopfenstein taper balun has an improved performance compared to the one with the

linear taper balun.

Figure 2. Measured reflection coefficient for the two balun-fed Eleven feed prototypes: linear taper (dashed

line, red) and Klopfenstein taper (solid line, blue).

1.2. Design of New Feed Petals

During the last months of 2011 we were working with the mechanical implementation and

prototype fabrication of a new circular Eleven feed that was designed by the Antenna Group at

Chalmers. Figure 3 shows the CAD model of the production prototype. The circular Eleven feed is

constructed of “circularly” curved folded dipoles on a flat printed circuit board (PCB), with the aim

of making this antenna structure more rotationally symmetric at a very low manufacturing cost.

According to the simulations, it is expected that the circular Eleven feed achieves a BOR1 (body

of revolution type 1) efficiency of better than −1 dB over a decade bandwidth of 1.3–14.0 GHz.

This is a significant progress for decade-bandwidth feed technology.

296 IVS 2011 Annual Report
Onsala Space Observatory (OSO) Onsala Space Observatory (OSO), TDC

Figure 3. Drawing of the new circular Eleven feed.

1.3. Cryogenic Tests and Noise Model

To characterize the system noise, the 2–13 GHz Eleven feed prototype was integrated with a

20 K cryostat. The feed prototype has eight 50 Ω ports, four for each polarization. Since only four

LNAs were available for the tests, the ports for one polarization were terminated with 50 Ω loads.

The LNAs are CITCRY01-12 wideband cryogenic 50 Ω amplifiers, purchased from Caltech. The

feed system including the cryostat was placed outdoors, with the feed window pointing upwards.

The receiver noise was measured by the Y-factor method using hot and cold loads. An absorber

at ambient temperature is used as the hot load and the sky as the cold load. A metal pyramid is

used as a shielding for the cryostat, in order to reduce the noise pick-up from the ground and the

surroundings.

Although the tests were done at the observatory, which is a radio-quiet zone, a strong RFI was

observed in the cold spectra from 2 to 3 GHz. Since the system was shielded with the absorber for

the hot load measurement when measuring the hot load, the RFI cannot be calibrated out, and

the measured Y-factor is not representative for the frequency range 2–3 GHz. A new algorithm

for improving the data analysis in the 2–3 GHz band is under development.

The measured system noise temperature was compared with the one predicted by our noise

model, shown in Figure 4. The model predictions agree well with the measurements.

2. Integration of a Digital Backend

In 2011 the observatory purchased a digital backend of type DBBC (Digital Base Band Converter) [2], and the work to adapt it to the observatory’s instruments was initiated. For geodetic

S/X-observations we use coaxial cables to carry the IF-signals from the 20-m telescope down to

IVS 2011 Annual Report 297
Onsala Space Observatory (OSO), TDC Onsala Space Observatory (OSO)

Figure 4. Measured (dashed line, red) and predicted system noise temperature (solid line, blue). The noise

temperature of the LNAs is shown as thin solid line in green.

the VLBI backends (Mark IV and DBBC). This implies that the band pass has a slope, with attenuation increasing with increasing frequency. Since the dynamic range of the DBBC is limited,

such a band pass slope will degrade the usable signal range of the digital system. We thus decided

to introduce equalizers for the IF-signals, and the work to implement these is ongoing.

3. Outlook and Future Plans

We will continue to work on the development of an Eleven feed for VLBI2010. We also aim

at preparing the 20-m telescope to become fully compatible with VLBI2010 within the next few

years.

References

[1] Raza H, Yang J, Pantaleev M (2011) A compact UWB passive balun solution for cryogenic 2–13 GHz

Eleven feed for future wideband radio telescopes. 5th Eur. Conf. on Antennas Propagat. (EuCAP2011),

Rome, Italy, 11-15 April 2011.

[2] Tuccari G (2004) DBBC - a wide band digital base band convertor, In: International VLBI Service

for Geodesy and Astrometry 2004 General Meeting Proceedings, edited by Nancy R. Vandenberg and

Karen D. Baver, NASA/CP-2004-212255, 234–237.

298 IVS 2011 Annual Report
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1. Introduction

The following bibliography compiles papers that were published in the field of geodetic and

astrometric VLBI during the year 2011. There is no distinction between peer-reviewed, reviewed,

or proceedings publications. This list is by no means exhaustive.

2. Geodetic and Astrometric VLBI Publications of 2011

W. Alef, H. Rottmann, A. Bertarini, A. Muskens:  ̈ “Bonn Correlator Status Report”. In:

Proceedings of the 20th Meeting of the European VLBI Group for Geodesy and Astrometry,

edited by W. Alef, S. Bernhart, A. Nothnagel, Schriftenreihe des Instituts f ̈ur Geod ̈asie und

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P. Andersen: “FFI Analysis Center”. In: International VLBI Service for Geodesy and Astrometry 2010 Annual Report, edited by D. Behrend and K. Baver, NASA/TP-2011-215880, 192–193,

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P. Andersen: “FFI Technology Development Center – Software Development”. In: International

VLBI Service for Geodesy and Astrometry 2010 Annual Report, edited by D. Behrend and K.

Baver, NASA/TP-2011-215880, 268, 2011.

T. Artz, A. Nothnagel, P. Steigenberger, S. Tesmer: “Evaluation of Combined Sub-daily

UT1 Estimates from GPS and VLBI Observations”. In: Proceedings of the 20th Meeting of

the European VLBI Group for Geodesy and Astrometry, edited by W. Alef, S. Bernhart, A.

Nothnagel, Schriftenreihe des Instituts f ̈ur Geod ̈asie und Geoinformation der Universit ̈at Bonn,

Nr. 22, ISSN 1864-1113, 97–101, 2011.

T. Artz, S. Tesmer nee B  ́ ockmann, A. Nothnagel:  ̈ “Assessment of periodic sub-diurnal

Earth rotation variations at tidal frequencies through transformation of VLBI normal equation

systems”. Journal of Geodesy, 85(9), doi:10.1007/s00190-011-0457-z, 565–584, 2011.

S. Bachmann, R. Heinkelmann, M. Gerstl: “BKG/DGFI Combination Center Annual Report 2010”. In: International VLBI Service for Geodesy and Astrometry 2010 Annual Report,

edited by D. Behrend and K. Baver, NASA/TP-2011-215880, 183–186, 2011.

C. Barache, S. Lambert: “Paris Observatory (OPAR) Data Center”. In: International VLBI

Service for Geodesy and Astrometry 2010 Annual Report, edited by D. Behrend and K. Baver,

NASA/TP-2011-215880, 167–170, 2011.

C. Beaudoin, B. Corey, A. Niell, A. Whitney: “Haystack Observatory Technology Development Center”. In: International VLBI Service for Geodesy and Astrometry 2010 Annual

Report, edited by D. Behrend and K. Baver, NASA/TP-2011-215880, 272–275, 2011.

C. Beaudoin, B. Whittier: “Sensitivity evaluation of two VLBI2010 candidate feeds”. In:

Proceedings of the 20th Meeting of the European VLBI Group for Geodesy and Astrometry,

edited by W. Alef, S. Bernhart, A. Nothnagel, Schriftenreihe des Instituts f ̈ur Geod ̈asie und

Geoinformation der Universit ̈at Bonn, Nr. 22, ISSN 1864-1113, 71–73, 2011.

D. Behrend: “Coordinating Center Report”. In: International VLBI Service for Geodesy and

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13–15, 2011.

S. Bernhart, A. Bertarini, A. Muskens, W. Alef:  ̈ “The Bonn Astro/Geo Correlator”.

In: International VLBI Service for Geodesy and Astrometry 2010 Annual Report, edited by D.

Behrend and K. Baver, NASA/TP-2011-215880, 133–136, 2011.

A. Bertarini, A. Roy, B. Corey, C. Walker, W. Alef, A. Nothnagel: “Effects on

geodetic VLBI measurements due to polarization leakage in S/X receivers”. Journal of Geodesy,

85(10), doi:10.1007/s00190-011-0478-7, 715–721, 2011.

I. Bezrukov, A. Finkelstein, A. Ipatov, M. Kaidanovsky, A. Mikhailov, A. Salnikov,

V. Yakovlev: “The Quasar Network Observations in e-VLBI Mode”. In: Proceedings of the

20th Meeting of the European VLBI Group for Geodesy and Astrometry, edited by W. Alef,

S. Bernhart, A. Nothnagel, Schriftenreihe des Instituts f ̈ur Geod ̈asie und Geoinformation der

Universit ̈at Bonn, Nr. 22, ISSN 1864-1113, 49–51, 2011.

G. Bianco, G. Colucci, F. Schiavone: “Matera CGS VLBI Station”. In: International VLBI

Service for Geodesy and Astrometry 2010 Annual Report, edited by D. Behrend and K. Baver,

NASA/TP-2011-215880, 54–57, 2011.

D. Boboltz, A. Fey, N. Geiger, K. Kingham, D. Hall: “U.S. Naval Observatory VLBI

Analysis Center”. In: International VLBI Service for Geodesy and Astrometry 2010 Annual

Report, edited by D. Behrend and K. Baver, NASA/TP-2011-215880, 257–260, 2011.

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IVS Information

IVS Information

Terms of Reference

IVS Terms of Reference

1. Summary

1.1. Charter

The International VLBI Service for Geodesy and Astrometry (IVS) is an international collaboration of organizations which operate or support Very Long Baseline Interferometry (VLBI)

components. IVS provides a service which supports geodetic and astrometric work on reference

systems, Earth science research, and operational activities. IVS is a Service of the International

Association of Geodesy (IAG) and of the International Astronomical Union (IAU).

1.2. Objectives

IVS fulfills its charter through the following objectives.

1. foster and carry out VLBI programs. This is accomplished through close coordination of the

participating organizations to provide high-quality VLBI data and products.

2. promote research and development activities in all aspects of the geodetic and astrometric

VLBI technique.

3. advance the education and training of VLBI participants through workshops, reports, and

other means.

4. support the integration of new components into IVS.

5. interact with the community of users of VLBI products. IVS represents VLBI in the Global

Geodetic Observing System (GGOS) of the IAG and interacts closely with the International

Earth Rotation and Reference Systems Service (IERS).

In support of these objectives, IVS coordinates VLBI observing programs, sets performance

standards for VLBI stations, establishes conventions for VLBI data formats and data products,

issues recommendations for VLBI data analysis software, sets standards for VLBI analysis documentation, and institutes appropriate VLBI product delivery methods to ensure suitable product

quality and timeliness. IVS coordinates its activities with the astronomical community because of

the dual use of many VLBI facilities and technologies for both astronomy and astrometry/geodesy.

1.3. Data Products

VLBI data products contribute uniquely to these important activities:

• defining and maintaining the celestial reference frame,

• monitoring universal time (UT1),

• monitoring the coordinates of the celestial pole (nutation and precession).

These results are the foundation of many scientific and practical applications requiring the use

of an accurate quasi-inertial reference frame, such as high-precision positioning, navigation, and

timing. In addition IVS provides a variety of VLBI products with differing applications, timeliness,

detail, and temporal resolution, such as:

IVS 2011 Annual Report 317
Terms of Reference

• all components of Earth orientation parameters,

• terrestrial reference frame,

• baseline lengths,

• tropospheric parameters.

All VLBI data and products are publicly available in appropriate formats from IVS Data

Centers.

1.4. Research

The IVS data and products are used for research in many areas of geodesy, geophysics, and

astronomy, such as:

• UT1 and polar motion excitation over periods of hours to decades,

• solid Earth interior research (e.g., mantle rheology, anelasticity, libration, core modes),

• characterization of celestial reference frame sources and improvements to the frame,

• tidal variations (solid Earth, oceanic, and atmospheric),

• improvements in the terrestrial reference frame, especially in the scale,

• climate studies (e.g., sea level change, deglaciation, water vapor),

• regional and global geodynamics,

• general relativity.

To support these activities, there are ongoing research efforts to improve and extend the VLBI

technique in areas such as:

• instrumentation, data acquisition, and correlation,

• data analysis techniques,

• spacecraft tracking and navigation (Earth-orbiting and interplanetary)

• combination of VLBI data and results with other techniques.

2. Permanent Components

IVS acquires, correlates, and analyzes VLBI data to produce geodetic, astrometric, and other

results that are archived and publicized. IVS accomplishes its objectives through the following

permanent components:

• Network Stations,

• Operation Centers,

• Correlators,

• Analysis Centers,

• Data Centers,

• Technology Development Centers,

• Coordinating Center.

318 IVS 2011 Annual Report
Terms of Reference

2.1. Network Stations

The IVS observing network consists of high performance VLBI stations.

• Stations may either be dedicated to geodesy or have multiple uses (including astronomical

observations or satellite tracking applications).

• Stations comply with performance standards for data quality and operational reliability

specified by the Directing Board.

• Stations provide local tie information, timing and meteorological data to the IVS Data Centers.

• VLBI data acquisition sessions are conducted by groups of Network Stations that may be

distributed either globally or over a geographical region.

2.2. Operation Centers

The IVS Operation Centers coordinate the routine operations of specific networks. Operation

Center activities include:

• planning network observing programs,

• supporting the network stations in improving their performance,

• generating the detailed observing schedules for use in data acquisition sessions by IVS Network Stations, item posting the observing schedule to an IVS Data Center for distribution

and archiving.

IVS Operation Centers follow guidelines from the Coordinating Center for timeliness and schedule file formats.

2.3. Correlators

The IVS Correlators process raw VLBI data. Their other tasks are to:

• provide timely feedback to the Network Stations about data quality,

• jointly maintain the geodetic/astrometric community’s media pool and transport,

• manage electronic data transfer,

• make processed data available to the Data Centers,

• regularly compare processing techniques, models, and outputs to ensure that data from

different Correlators are identical.

2.4. Analysis Centers

The IVS coordinates VLBI data analysis to provide high-quality products for its users. The

analyses are performed by

• Operational Analysis Center,

• Associate Analysis Centers,

IVS 2011 Annual Report 319
Terms of Reference

• Special Analysis Centers for Specific Observing Sessions, and

• Combination Centers

All Analysis Centers maintain and/or develop appropriate VLBI analysis software.

Operational Analysis Centers are committed to producing results to the specifications of the

IVS Analysis Coordinator and always on schedule to meet IVS requirements. In addition, Operational Analysis Centers may produce Earth orientation parameters, station coordinates, and

source positions in regular intervals.

Operational Analysis Centers place their final results in IVS Data Centers for dissemination

to researchers and other users. They adhere to IVS recommendations for the creation of highquality products and their timely archiving and distribution. Any deviations that an Operational

Analysis Center makes from IVS recommendations are properly documented. Operational Analysis

Centers provide timely feedback about station performance. In addition to these regular services,

Operational Analysis Centers may also perform any task of an Associate Analysis Center.

Associate Analysis Centers are committed to regularly submit specialized products using complete series or subsets of VLBI observing sessions. The analysis is performed for specific purposes

as recognized by the Directing Board, such as exploitation of VLBI data for new types of results,

investigations of regional phenomena, reference frame maintenance, or special determinations of

Earth orientation parameters. The Associate Analysis Centers place their final results in IVS Data

Centers for dissemination to researchers and other users. They adhere to IVS recommendations for

the creation of high-quality products and their timely archiving and distribution. Any deviations

that an Associate Analysis Center makes from IVS recommendations are properly documented.

Special Analysis Centers for Specific Observing Sessions have responsibility for ongoing seriesrelated investigations of one or more existing session types. They perform detailed and comparative

analyses of each session of a series within a reasonable time after correlation. In addition, they

report deficits and technical complications to the observing sites, the correlators, and to the schedulers as well as to the IVS Network and Analysis Coordinators.

Combination Centers are committed to produce combination results from the individual submissions of the Operational Analysis Centers as official IVS products. For this purpose they

monitor the quality of the submissions. The official IVS products include, but are not limited

to, EOP time series derived from session-based results for 24-hour network sessions and 1-hour

Intensive sessions. Combination Centers also contribute to the generation of the official IVS input

to International Terrestrial Reference Frame (ITRF) computations. The combination work is done

in a timely fashion and in close cooperation with the IVS Analysis Coordinator.

2.5. Data Centers

The IVS Data Centers are repositories for VLBI observing schedules, station log files, data and

products. Data Centers may mirror other Data Centers to make the distribution and maintenance

of data more efficient and reliable.

• Data Centers are the primary means of distributing VLBI products to users.

• Data Centers work closely with the Coordinating Center and with the Analysis Centers to

ensure that all the information and data required by IVS components are quickly and reliably

available.

Data Centers provide the following functions:

320 IVS 2011 Annual Report
Terms of Reference

• receive and archive schedule files from Operation Centers,

• receive and archive log files and ancillary data files from the Network Stations,

• receive and archive data products from the Analysis Centers,

• provide access and public availability to IVS data products for all users.

2.6. Technology Development Centers

The IVS Technology Development Centers contribute to the development of new VLBI technology for improvement of the VLBI technique. They:

• investigate new equipment and approaches,

• develop, test, and document new hardware, firmware, and software for operations,

• assist with deployment, installation, and training for any new approved technology,

• maintain and support operational equipment.

2.7. Coordinating Center

The IVS Coordinating Center is responsible for coordination of both the day-to-day and the

long-term activities of IVS, consistent with the directives and policies established by the Directing

Board. Specifically, the Coordinating Center monitors, coordinates, and supports the activities

of the Network Stations, Operation Centers, Correlators, Data Centers, Analysis Centers, and

Technology Development Centers. The Coordinating Center works closely with the Technology

Coordinator, the Network Coordinator, and the Analysis Coordinator to coordinate IVS activities.

The primary functions of the Coordinating Center are to:

• coordinate observing programs approved by the Directing Board,

• create and maintain the master schedule of observing sessions in coordination with IVS

Network Stations and astronomical observing programs,

• foster communications among all components of the IVS,

• coordinate the best use of community resources,

• develop standard procedures for IVS components,

• organize training in VLBI techniques,

• organize workshops and meetings, including IVS technical meetings,

• produce and publish reports of activities of IVS components,

• maintain the IVS information system and archive all documents, standards, specifications,

manuals, reports, and publications,

• coordinate IVS outreach and educational activities,

• provide liaison with the IAU, IAG, GGOS, IERS, and other organizations,

• provide the Secretariat of the Directing Board.

IVS 2011 Annual Report 321
Terms of Reference

2.8. Becoming a Permanent Component

IVS will accept proposals at any time to become a permanent component. Such proposals will

be reviewed for approval by the Directing Board.

3. Coordinators

Specific IVS activities regarding network data quality, products, and technology are accomplished through the functions performed by three coordinators: a Network Coordinator, an Analysis Coordinator, and a Technology Coordinator.

3.1. Network Coordinator

The IVS Network Coordinator is selected by the Directing Board from responses to an open

solicitation to all IVS components. The Network Coordinator represents the IVS Network Stations

on the Directing Board and works closely with the Coordinating Center. The Network Coordinator

is responsible for stimulating the maintenance of a high quality level in the station operation and

data delivery. The Network Coordinator performs the following functions:

• monitors adherence to standards in the network operation,

• participates in the quality control of the data acquisition performance of the network stations,

• tracks data quality and data flow problems and suggests actions to improve the level of

performance,

• coordinates software development for station control and monitoring.

The Network Coordinator works closely with the geodetic and astronomical communities who

are using the same network stations for observations. The Network Coordinator takes a leading

role in ensuring the visibility and representation of the network stations.

3.2. Analysis Coordinator

The IVS Analysis Coordinator is selected by the Directing Board from responses to an open

solicitation to the IVS Analysis Centers. The Analysis Coordinator is responsible for coordinating

the analysis activities of IVS and for stimulating VLBI product development and delivery. The

Analysis Coordinator performs the following functions:

• fosters comparisons of results from different VLBI analysis software packages and different

analysis strategies,

• encourages documentation of analysis and combination software,

• participates in comparisons of results from different space geodetic techniques,

• monitors Analysis Centers’ products for high quality results and for adherence to IVS standards and IERS Conventions,

• ensures that IVS analysis and combination products are archived and are available to the

scientific community, and

• supervises the formation of the official IVS products specified by the IVS Directing Board.

322 IVS 2011 Annual Report
Terms of Reference

The Analysis Coordinator plays a leadership role in the development of methods for generation

and distribution of VLBI products so that the products reach the users in a timely manner. The

Analysis Coordinator interacts with GGOS and the IERS and promotes the use of VLBI products

by the broader scientific community. The Analysis Coordinator works closely with the astronomical

communities who are using some of the same analysis methods and software.

3.3. Technology Coordinator

The IVS Technology Coordinator is selected by the Directing Board from responses to an open

solicitation to the IVS Technology Development Centers. The Technology Coordinator performs

the following functions:

• stimulates advancement of the VLBI technique,

• maintains awareness of all current VLBI technologies and ongoing development,

• coordinates development of new technology among all IVS Technology Development Centers,

• encourages technical compatibility with the astronomical community,

• encourages and oversees development of VLBI-related technical standards,

• coordinates the distribution of and access to technical documents and standards,

• helps promulgate new technologies to the IVS community.

The Technology Coordinator works closely with the astronomical community, both to maintain

technical compatibility between the geodetic and astronomical communities and to take advantage

of technology development activities in the astronomical community.

4. Directing Board

4.1. Roles and Responsibilities

The Directing Board sets objectives, determines policies, adopts standards, and sets the scientific and operational goals for IVS. The Directing Board exercises general oversight of the activities

of IVS including modifications to the organization that are deemed appropriate and necessary to

maintain efficiency and reliability. The Directing Board may determine appropriate actions to

ensure the quality of the IVS products.

The Directing Board will receive and review proposals for non-IVS research programs that

request IVS resources.

4.2. Membership

The Directing Board consists of representatives of the IVS components, members at-large,

appointed members, and ex officio members. The members are:

Representatives of IVS Components (see below):

• Correlators and Operation Centers representative (1)

• Analysis and Data Centers representatives (2)

IVS 2011 Annual Report 323
Terms of Reference

• Networks representatives (2)

• Technology Development Centers representative (1)

Elected by the Directing Board upon recommendation from the Coordinating Center (see below):

• Members at large (3)

Selected by Directing Board upon review of proposals from IVS Member Organizations:

• Coordinating Center Director

• Network Coordinator

• Analysis Coordinator

• Technology Coordinator

Appointed members:

• IAU representative

• IAG representative

• IERS representative

Through a reciprocity agreement between IVS and IERS, the IVS serves as the VLBI Technique

Center for IERS, and as such its designated representative(s) serve on the IERS Directing Board.

In turn, the IERS Directing Board designates a representative to the IVS Directing Board. This

arrangement is to assure full cooperation between the two services.

Total number: 16

The members appointed by IAU, IAG, and IERS are not subject to institutional restrictions.

The six members who are the representatives of the IVS components are elected by the IVS

Associate Members. All elected members serve staggered four-year terms once renewable.

At-large members are intended to ensure representation on the Directing Board of each of the

components of IVS and to balance representation from as many countries and institutions and IVS

interests as possible. At-large members serve two-year terms once renewable.

A Directing Board member who departs before the end of his/her term is replaced by a person

selected by the Directing Board. The new member will serve until the next official elections. The

position will then be filled for a full term.

An individual can only serve two consecutive full terms on the Board in any of the representative

and at-large positions. Partial terms are not counted to this limit. After serving two consecutive

full terms, an individual becomes eligible again for a position on the Board following a two-year

absence.

The three Coordinators are selected by the Directing Board on the basis of proposals from

IVS Member Organizations. On a two-thirds vote the Directing Board may call for new proposals

for any Coordinator when it determines that a new Coordinator is required. Coordinators are

encouraged to give at least six months notice before resigning.

324 IVS 2011 Annual Report
Terms of Reference

4.3. Elections

Election of Board members from the IVS components shall be conducted by a committee of

three Directing Board members, the chair of which is appointed by the chair of the Directing Board.

The committee solicits nominations for each representative from the relevant IVS components. For

each position, the candidate who receives the largest number of votes from the Associate Members

will be elected. In case of a tie the Directing Board will make the decision.

4.4. Chair

The chair is one of the Directing Board members and is elected by the Board for a term

of four years with the possibility of reelection for one additional term. The chair is the official

representative of IVS to external organizations.

4.5. Decisions

Most decisions by the Directing Board are made by consensus or by simple majority vote of the

members present. In case of a tie, the chair decides how to proceed. If a two-thirds quorum is not

present, the vote shall be held later by electronic mail. A two-thirds vote of all Board members is

required to modify the Terms of Reference, to change the chair, or to replace any of the members

before their normal term expires.

4.6. Meetings

The Directing Board meets at least annually, or more frequently if meetings are called by the

chair or at the request of at least three Board members. The Board will conduct periodic reviews

of the IVS organization and its mandate, functions, and components.

5. Definitions

5.1. Member Organizations

Organizations that support one or more IVS components are IVS Member Organizations.

Individuals associated with IVS Member Organizations may become IVS Associate Members.

5.2. Affiliated Organizations

Organizations that cooperate with IVS on issues of common interest, but do not support an

IVS component, are IVS Affiliated Organizations. Affiliated Organizations express an interest in

establishing and maintaining a strong working association with IVS to mutual benefit. Individuals

affiliated with IVS Affiliated Organizations may become IVS Corresponding Members.

5.3. Associate Members

Individuals associated with organizations that support an IVS component may become IVS

Associate Members. Associate Members take part in the election of the incoming members of the

Directing Board representing the IVS components.

IVS 2011 Annual Report 325
Terms of Reference

5.4. Corresponding Members

IVS Corresponding Members are individuals who express interest in receiving IVS publications,

wish to participate in workshops or scientific meetings organized by IVS, or generally are interested

in IVS activities. Ex officio Corresponding Members are the following:

• IAG Secretary General

• Chair of GGOS

• President of IAG Commission 1 – Reference Frames

• President of IAG Commission 3 - Earth Rotation and Geodynamics

• President of IAU Division I – Fundamental Astronomy

• President of IAU Commission 8 – Astrometry

• President of IAU Commission 19 – Rotation of the Earth

• President of IAU Commission 31 – Time

• President of IAU Commission 40 – Radio Astronomy

• President of URSI Commission 52 – Relativity in Fundamental Astronomy

• President of URSI Commission J – Radio Astronomy

Individuals are accepted as IVS Corresponding Members upon request to the Coordinating

Center.

Last modified: 23 September 2011

326 IVS 2011 Annual Report
Members

IVS Member Organizations

(alphabetized by country)

Organization Country

Commonwealth Scientific and Industrial Research Organisation (CSIRO) Australia

Geoscience Australia Australia

University of Tasmania Australia

Vienna University of Technology Austria

Centro de R ́adio Astronomia e Aplica ̧c ̃oes Espaciais Brazil

Dominion Radio Astrophysical Observatory Canada

Geodetic Survey Division, Natural Resources Canada Canada

Instituto Geogr ́afico Militar Chile

Universidad de Concepci ́on Chile

Chinese Academy of Sciences China

Laboratoire d’Astrophysique de Bordeaux France

Observatoire de Paris France

Bundesamt f ̈ur Kartographie und Geod ̈asie Germany

Deutsches Geod ̈atisches Forschungsinstitut Germany

Forschungseinrichtung Satellitengeod ̈asie, TU Munich Germany

Institut f ̈ur Geod ̈asie und Geoinformation der Universit ̈at Bonn Germany

Max-Planck-Institut f ̈ur Radioastronomie Germany

Agenzia Spaziale Italiana Italy

Istituto di Radioastronomia INAF Italy

Politecnico di Milano DIIAR Italy

Geospatial Information Authority of Japan Japan

National Astronomical Observatory of Japan Japan

National Institute of Information and Communications Technology Japan

National Institute of Polar Research Japan

Auckland University of Technology New Zealand

Norwegian Defence Research Establishment Norway

Norwegian Mapping Authority Norway

Astronomical Institute of St.-Petersburg University Russia

Institute of Applied Astronomy Russia

Pulkovo Observatory Russia

Sternberg State Astronomical Institute, Lomonosov Moscow State University Russia

Hartebeesthoek Radio Astronomy Observatory South Africa

Korea Astronomy and Space Science Institute South Korea

Instituto Geogr ́afico Nacional Spain

Chalmers University of Technology Sweden

Karadeniz Technical University Turkey

Laboratory of Radioastronomy of Crimean Astrophysical Observatory Ukraine

IVS 2011 Annual Report 327
Members

Organization Country

Main Astronomical Observatory, National Academy of Sciences, Kiev Ukraine

Jet Propulsion Laboratory USA

NASA Goddard Space Flight Center USA

U. S. Naval Observatory USA

328 IVS 2011 Annual Report
Affiliates

IVS Affiliated Organizations

Organization Country

Australian National University Australia

University of New Brunswick Canada

FO ̈MI Satellite Geodetic Observatory Hungary

Joint Institute for VLBI in Europe (JIVE) Netherlands

Westerbork Observatory Netherlands

National Radio Astronomy Observatory USA

IVS 2011 Annual Report 329
Associate Members

IVS Associate Members

Name Institution Country E-mail

Alef, Walter Max-Planck-Institut f ̈ur

Radioastronomie

Germany walef@mpifr-bonn.mpg.de

Amagai, Jun National Institute of Information

and Communications Technology

Japan amagai@nict.go.jp

Andersen, Per

Helge

Norwegian Defence Research

Establishment

Norway per-helge.andersen@ffi.no

Andreeva,

Tatiana

Institute of Applied Astronomy Russia ats@urania.rtf32s.nw.ru

Artz, Thomas Institut f ̈ur Geod ̈asie und

Geoinformation der Universit ̈at

Bonn

Germany thomas.artz@uni-bonn.de

Barache,

Christophe

Observatoire de Paris France Christophe.Barache@obspm.fr

Baudry, Alain Laboratoire d’Astrophysique de

Bordeaux

France baudry@obs.u-bordeaux1.fr

Bauernfeind,

Erhard

Geodetic Observatory Germany bauernfeind@fs.wettzell.de

Baver, Karen NVI, Inc. USA karen.d.baver@nasa.gov

Beaudoin,

Christopher

MIT Haystack Observatory USA cbeaudoin@haystack.mit.edu

Beck, Norman Natural Resources Canada Canada beck@nrcan.gc.ca

Behrend, Dirk NVI, Inc. USA Dirk.Behrend@nasa.gov

Bellanger,

Antoine

Laboratoire d’Astrophysique de

Bordeaux

France bellanger@obs.u-bordeaux1.fr

Berdnikov,

Anton

Institute of Applied Astronomy Russia

Bergman, Per Onsala Space Observatory Sweden bergman@oso.chalmers.se

Bernhart,

Simone

Institut f ̈ur Geod ̈asie und

Geoinformation der Universit ̈at

Bonn

Germany simone@mpifr-bonn.mpg.de

Bertarini,

Alessandra

Institut f ̈ur Geod ̈asie und

Geoinformation der Universit ̈at

Bonn

Germany abertari@mpifr-bonn.mpg.de

Bianco,

Giuseppe

Agenzia Spaziale Italiana Italy bianco@asi.it

Bielmaier,

Ewald

Geodetic Observatory Germany bielmaier@fs.wettzell.de

Boboltz, David U. S. Naval Observatory USA dboboltz@usno.navy.mil

B ̈ohm, Johannes Institute of Geodesy and

Geophysics

Austria johannes.boehm@tuwien.ac.at

B ̈ohm, Sigrid Institute of Geodesy and

Geophysics

Austria sigrid.boehm@tuwien.ac.at

330 IVS 2011 Annual Report
Associate Members

Name Institution Country E-mail

Boer, Armin BKG/Project TIGO Chile armin.boer@bkg.bund.de

Bolotin, Sergei NVI, Inc. USA sergei.bolotin@nasa.gov

Bougeard,

Mireille

Observatoire de Paris France mireille.bougeard@obspm.fr

Bourda,

Geraldine

Laboratoire d’Astrophysique de

Bordeaux

France bourda@obs.u-bordeaux1.fr

Buttaccio, Salvo Istituto di Radioastronomia

INAF

Italy s.buttaccio@ira.inaf.it

Cappallo, Roger MIT Haystack Observatory USA rcappallo@haystack.mit.edu

Carlson, Brent Dominion Radio Astrophysical

Observatory

Canada bcarlson@drao.nrc.ca

Carter, Merri

Sue

U. S. Naval Observatory,

Flagstaff Station

USA msc@nofs.navy.mil

Charlot, Patrick Laboratoire d’Astrophysique de

Bordeaux

France charlot@obs.u-bordeaux1.fr

Cho, Jungho Korea Astronomy & Space

Science Institute

Korea jojh@kasi.re.kr

Collioud,

Arnaud

Laboratoire d’Astrophysique de

Bordeaux

France collioud@obs.u-bordeaux1.fr

Colomer,

Francisco

Instituto Geogr ́afico Nacional Spain f.colomer@oan.es

Colucci,

Giuseppe

Telespazio SpA Italy giuseppe.colucci@telespazio.com

Combrinck,

Ludwig

Hartebeesthoek Radio

Astronomy Observatory

South

Africa

ludwig@bootes.hartrao.ac.za

Conway, John Onsala Space Observatory Sweden jconway@chalmers.se

Corey, Brian MIT Haystack Observatory USA bcorey@haystack.mit.edu

Curtis, Ronald ITT Information Systems USA ronald.curtis@exelisinc.com

Dassing, Reiner Bundesamt f ̈ur Kartographie

und Geod ̈asie

Germany reiner.dassing@bkg.bund.de

Del Rosso,

Domenico

Telespazio SpA Italy domenico delrosso@telespazio.it

de-Vicente,

Pablo

Instituto Geogr ́afico Nacional Spain p.devicente@oan.es

Diakov, Alexey Institute of Applied Astronomy Russia ipazel@mail.svkchr.ru

Dickey, John University of Tasmania Australia John.Dickey@utas.edu.au

Diegel, Irv Honeywell TSI USA irv.diegel@honeywell-tsi.com

Doi, Koichiro National Institute of Polar

Research

Japan doi@nipr.ac.jp

Dong, Yousuo Urumqi Astronomical

Observatory

China dongys@ms.xjb.ac.cn

Drewes,

Hermann

Deutsches Geod ̈atisches

Forschungsinstitut

Germany drewes@dgfi.badw.de

Dube, Maurice SSAI USA maurice.p.dube@nasa.gov

IVS 2011 Annual Report 331
Associate Members

Name Institution Country E-mail

Elgered, Gunnar Onsala Space Observatory Sweden kge@chalmers.se

Engelhardt,

Gerald

Bundesamt f ̈ur Kartographie

und Geod ̈asie

Germany gerald.engelhardt@bkg.bund.de

Engen, Bjorn Norwegian Mapping Authority Norway bjorn.engen@statkart.no

Evangelista,

Mark

Honeywell TSI USA mark.evangelista@honeywelltsi.com

Fan, Qingyuan Shanghai Astronomical

Observatory

China qyfan@center.shao.ac.cn

Fedotov, Leonid Institute of Applied Astronomy Russia flv@ipa.nw.ru

Fey, Alan U. S. Naval Observatory USA afey@usno.navy.mil

Fukuzaki,

Yoshihiro

Geospatial Information

Authority of Japan

Japan fukuzaki@gsi.go.jp

Gambis, Daniel Observatoire de Paris France daniel.gambis@obspm.fr

Garc ́ıa–Espada,

Susana

Instituto Geogr ́afico Nacional Spain s.gespada@oan.es

Gaume, Ralph U. S. Naval Observatory USA rgaume@usno.navy.mil

Gipson, John NVI, Inc. USA john.m.gipson@nasa.gov

Gomez, Frank Raytheon USA frank.g.gomez@nasa.gov

G ́omez–

Gonz ́alez,

Jes ́us

Instituto Geogr ́afico Nacional Spain gomez@oan.es

Gordon, David NVI, Inc. USA david.gordon-1@nasa.gov

Govind, Ramesh Geoscience Australia Australia ramesh.govind@ga.gov.au

Gubanov,

Vadim

Institute of Applied Astronomy Russia gubanov@quasar.ipa.nw.ru

Gulyaev, Sergei Auckland University of

Technology

New

Zealand

sergei.gulyaev@aut.ac.nz

Haas, R ̈udiger Onsala Space Observatory Sweden rudiger.haas@chalmers.se

Hall, David U. S. Naval Observatory USA dhall@usno.navy.mil

Hammargren,

Roger

Onsala Space Observatory Sweden rogham@chalmers.se

Hanssen, Rune Norwegian Mapping Authority Norway rune.hanssen@statkart.no

Hase, Hayo BKG/Project TIGO Chile hayo.hase@bkg.bund.de

Heinkelmann,

Robert

Deutsches Geod ̈atisches

Forschungsinstitut

Germany heinkelmann@dgfi.badw.de

Helldner, Leif Onsala Space Observatory Sweden helldner@chalmers.se

Herrera,

Cristian

TIGO/Universidad de

Concepci ́on

Chile cristian.herrera@tigo.cl

Himwich, Ed NVI, Inc. USA Ed.Himwich@nasa.gov

Hirabaru,

Masaki

National Institute of Information

and Communications Technology

Japan masaki@nict.go.jp

Hobiger,

Thomas

National Institute of Information

and Communications Technology

Japan hobiger@nict.go.jp

332 IVS 2011 Annual Report
Associate Members

Name Institution Country E-mail

Hong, Xiaoyu Shanghai Astronomical

Observatory

China xhong@center.shao.ac.cn

Honma, Mareki National Astronomical

Observatory of Japan

Japan honmamr@cc.nao.ac.jp

Huang, Xinyong Shanghai Astronomical

Observatory

China xhuang@center.shao.ac.cn

Hugentobler,

Urs

Geodetic Observatory Germany urs.hugentobler@bv.tu-muenchen.de

Ichikawa,

Ryuichi

National Institute of Information

and Communications Technology

Japan richi@nict.go.jp

Ihde, Johannes Bundesamt f ̈ur Kartographie

und Geod ̈asie

Germany johannes.ihde@bkg.bund.de

Ilijin, Gennadiy Institute of Applied Astronomy Russia

Ipatov,

Alexander

Institute of Applied Astronomy Russia ipatov@ipa.rssi.ru

Ipatova, Irina Institute of Applied Astronomy Russia ipatova@isida.ipa.rssi.ru

Ishihara, Misao Geospatial Information

Authority of Japan

Japan vlbi@gsi.go.jp

Ishii, Atsutoshi National Institute of Information

and Communications Technology

Japan ishii@nict.go.jp

Ivanov, D.V. Institute of Applied Astronomy Russia

Jacobs, Chris Jet Propulsion Laboratory USA chris.jacobs@jpl.nasa.gov

Jara, Cristobal TIGO/Universidad de

Concepci ́on

Chile cristobal.jara@tigo.cl

Jike, Takaaki National Astronomical

Observatory of Japan

Japan jike@miz.nao.ac.jp

Johansson, Jan Onsala Space Observatory Sweden jmj@chalmers.se

Johansson,

Karl- ̊Ake

Onsala Space Observatory Sweden karlake@chalmers.se

Johnson, Heidi MIT Haystack Observatory USA hjohnson@haystack.mit.edu

Johnston,

Kenneth

U. S. Naval Observatory USA kjj@astro.usno.navy.mil

Karasawa,

Masao

Geospatial Information

Authority of Japan

Japan vlbi@gsi.go.jp

Kaufmann,

Pierre

Centro de R ́adio Astronomia e

Aplica ̧c ̃oes Espaciais

Brazil kaufmann@usp.br

Kawabata,

Ryoji

Geospatial Information

Authority of Japan

Japan r-kawabata@gsi.go.jp

Kawaguchi,

Noriyuki

National Astronomical

Observatory of Japan

Japan kawagu.nori@nao.ac.jp

Kawai, Eiji National Institute of Information

and Communications Technology

Japan kawa@nict.go.jp

Kaydanovsky,

Michael

Institute of Applied Astronomy Russia kmn@isida.ipa.rssi.ru

IVS 2011 Annual Report 333
Associate Members

Name Institution Country E-mail

Kayık ̧cı, Emine

Tanır

Karadeniz Technical University Turkey etanir@ktu.edu.tr

Kharinov,

Mikhail

Institute of Applied Astronomy Russia kharinov@ipa.rssi.ru

Kimura,

Moritaka

National Institute of Information

and Communications Technology

Japan mkimura@nict.go.jp

Kingham, Kerry U. S. Naval Observatory USA kak@usno.navy.mil

Kobayashi,

Hideyuki

National Astronomical

Observatory of Japan

Japan hideyuki.kobayashi@nao.ac.jp

Kokado,

Kensuke

Geospatial Information

Authority of Japan

Japan vlbi@gsi.go.jp

Kondo, Tetsuro National Institute of Information

and Communications Technology

Japan kondo@nict.go.jp

Korkin, Edward Institute of Applied Astronomy Russia korkin@isida.ipa.rssi.ru

Koyama,

Yasuhiro

National Institute of Information

and Communications Technology

Japan koyama@nict.go.jp

Kronschnabl,

Gerhard

Bundesamt f ̈ur Kartographie

und Geod ̈asie

Germany gerhard.kronschnabl@bkg.bund.de

Kuboki,

Hiromitsu

National Institute of Information

and Communications Technology

Japan kuboki@nict.go.jp

Kudryashova,

Maria

Astronomical Institute of

St.-Petersburg

Russia kudryashova@mercury.astro.spbu.ru

Kurdubov,

Sergey

Institute of Applied Astronomy Russia ksl@quasar.ipa.nw.ru

Kurihara,

Shinobu

Geospatial Information

Authority of Japan

Japan skuri@gsi.go.jp

Kuroda, Jiro Geospatial Information

Authority of Japan

Japan vlbi@gsi.go.jp

Labelle, Ruth SSAI USA ruth.e.labelle@nasa.gov

Lambert,

S ́ebastien

Observatoire de Paris France sebastien.lambert@obspm.fr

Langkaas, Line Norwegian Mapping Authority Norway Line.Langkaas@statkart.no

Lanotte,

Roberto

Telespazio SpA Italy lanotte@asi.it

Lauber, Pierre Geodetic Observatory Germany lauber@fs.wettzell.de

Lavrov, Alexey Institute of Applied Astronomy Russia

Le Bail, Karine NVI, Inc. USA karine.lebail@nasa.gov

Li, Bing Shanghai Astronomical

Observatory

China bing@center.shao.ac.cn

Li, Huihua Shanghai Astronomical

Observatory

China hhl@center.shao.ac.cn

Li, Jinling Shanghai Astronomical

Observatory

China jll@center.shao.ac.cn

Liang, Shiguang Shanghai Astronomical

Observatory

China sgliang@center.shao.ac.cn

334 IVS 2011 Annual Report
Associate Members

Name Institution Country E-mail

Lindqvist,

Michael

Onsala Space Observatory Sweden Michael.Lindqvist@chalmers.se

Liu, Xiang Urumqi Astronomical

Observatory

China liux@ms.xjb.ac.cn

Long, Jim NASA Goddard Space Flight

Center

USA jim.l.long@nasa.gov

Lonsdale, Colin MIT Haystack Observatory USA clonsdale@haystack.mit.edu

Lovell, Jim University of Tasmania Australia Jim.Lovell@utas.edu.au

Lowe, Stephen Jet Propulsion Laboratory USA steve.lowe@jpl.nasa.gov

Lucena, Antonio Centro de R ́adio Astronomia e

Aplica ̧c ̃oes Espaciais

Brazil macilio@roen.inpe.br

Luzum, Brian U. S. Naval Observatory USA bjl@maia.usno.navy.mil

Ma, Chopo NASA Goddard Space Flight

Center

USA chopo.ma-1@nasa.gov

Maccaferri,

Giuseppe

Istituto di Radioastronomia

INAF

Italy g.maccaferri@ira.inaf.it

Machida,

Morito

Geospatial Information

Authority of Japan

Japan machida@gsi.go.jp

MacMillan, Dan NVI, Inc. USA daniel.s.macmillan@nasa.gov

Malkin, Zinovy Pulkovo Observatory Russia malkin@gao.spb.ru

Manabe, Seiji National Astronomical

Observatory of Japan

Japan manabe@miz.nao.ac.jp

Mantovani,

Franco

Istituto di Radioastronomia

INAF

Italy f.mantovani@ira.inaf.it

Mardyshkin,

Vyacheslav

Institute of Applied Astronomy Russia vvm@isida.ipa.rssi.ru

Marshalov,

Dmitry

Institute of Applied Astronomy Russia

Mathiassen,

Geir

Norwegian Mapping Authority Norway matgei@statkart.no

Matsuzaka,

Shigeru

Geospatial Information

Authority of Japan

Japan shigeru@gsi.go.jp

McCarthy,

Dennis

U. S. Naval Observatory USA dmc@maia.usno.navy.mil

Melnikov,

Alexey

Institute of Applied Astronomy Russia melnikov@quasar.ipa.nw.ru

Michailov,

Andrey

Institute of Applied Astronomy Russia agm@isida.ipa.rssi.ru

Miller, Natalia Pulkovo Observatory Russia natmiller@list.ru

Mitchell,

Donald

Honeywell TSI USA kokee@pele.kpgo.hawaii.edu

M ̈uskens, Arno Institut f ̈ur Geod ̈asie und

Geoinformation der Universit ̈at

Bonn

Germany mueskens@mpifr-bonn.mpg.de

IVS 2011 Annual Report 335
Associate Members

Name Institution Country E-mail

Mukai, Yasuko Geospatial Information

Authority of Japan

Japan mukai@gsi.go.jp

Nakajima,

Junichi

National Institute of Information

and Communications Technology

Japan nakaji@nict.go.jp

Nanni, Mauro Istituto di Radioastronomia

INAF

Italy m.nanni@ira.inaf.it

Natusch, Tim Auckland University of

Technology

New

Zealand

tim.natusch@aut.ac.nz

Negusini, Monia Istituto di Radioastronomia

INAF

Italy m.negusini@ira.inaf.it

Neidhardt,

Alexander

Geodetic Observatory Germany neidhardt@fs.wettzell.de

Nicolson,

George

Hartebeesthoek Radio

Astronomy Observatory

South

Africa

george@bootes.hartrao.ac.za

Niell, Arthur MIT Haystack Observatory USA aniell@haystack.mit.edu

Nielsen,

Carl-Petter

Norwegian Mapping Authority Norway carl-petter.nielsen@statkart.no

Nikitin, Pavel Crimean Astrophysical

Observatory

Ukraine nikitin@crao.crimea.ua

Nilsson, Tobias Institute of Geodesy and

Geophysics

Austria tobias.nilsson@tuwien.ac.at

Noll, Carey NASA Goddard Space Flight

Center

USA Carey.Noll@nasa.gov

Nothnagel, Axel Institut f ̈ur Geod ̈asie und

Geoinformation der Universit ̈at

Bonn

Germany nothnagel@uni-bonn.de

Nozawa,

Kentarou

Geospatial Information

Authority of Japan

Japan nozawa@gsi.go.jp

Ogaja, Clement Geoscience Australia Australia Clement.Ogaja@ga.gov.au

Olofsson, Hans Onsala Space Observatory Sweden hans.olofsson@chalmers.se

O ̃nate, Eric TIGO/Universidad del B ́ıo B ́ıo Chile eric.onate@tigo.cl

Orfei, Sandro Istituto di Radioastronomia

INAF

Italy a.orfei@ira.inaf.it

Petrachenko,

William

Natural Resources Canada Canada Bill.Petrachenko@nrc-cnrc.gc.ca

Pettersson, Lars Onsala Space Observatory Sweden d8lars@chalmers.se

Plank, Lucia Institute of Geodesy and

Geophysics

Austria lucia.plank@tuwien.ac.at

Pl ̈otz, Christian Bundesamt f ̈ur Kartographie

und Geod ̈asie

Germany christian.ploetz@bkg.bund.de

Poirier, Michael MIT Haystack Observatory USA mpoirier@haystack.mit.edu

Qian, Zhihan Shanghai Astronomical

Observatory

China qzh@center.shao.ac.cn

Quick, Jonathan Hartebeesthoek Radio

Astronomy Observatory

South

Africa

jon@bootes.hartrao.ac.za

336 IVS 2011 Annual Report
Associate Members

Name Institution Country E-mail

Rahimov, Ismail Institute of Applied Astronomy Russia rahimov@urania.rtf32s.nw.ru

Redmond, Jay Honeywell TSI USA jay.redmond@honeywell-tsi.com

Reid, Brett University of Tasmania Australia brett.reid@utas.edu.au

Rekkedal, Svein Norwegian Mapping Authority Norway svein.rekkedal@statkart.no

Richter, Bernd Bundesamt f ̈ur Kartographie

und Geod ̈asie

Germany bernd.richter@bkg.bund.de

Rioja, Maria Instituto Geogr ́afico Nacional Spain mj.rioja@oan.es

Romero-Wolf,

Andres

Jet Propulsion Laboratory USA andrew.romero-wolf@jpl.nasa.gov

Ruszczyk,

Chester

MIT Haystack Observatory USA chester@haystack.mit.edu

Salnikov,

Alexander

Institute of Applied Astronomy Russia salnikov@isida.ipa.rssi.ru

Sarti, Pierguido Istituto di Radioastronomia

INAF

Italy p.sarti@ira.inaf.it

Schatz,

Raimund

Geodetic Observatory Germany schatz@fs.wettzell.de

Scherneck,

Hans-Georg

Onsala Space Observatory Sweden hgs@chalmers.se

Schuh, Harald Institute of Geodesy and

Geophysics

Austria harald.schuh@tuwien.ac.at

Schwarz, Walter Bundesamt f ̈ur Kartographie

und Geod ̈asie

Germany walter.schwarz@bkg.bund.de

Schwegmann,

Wolfgang

Bundesamt f ̈ur Kartographie

und Geod ̈asie

Germany wolfgang.schwegmann@bkg.bund.de

Sciarretta,

Cecilia

Telespazio SpA Italy cecilia@asi.it

Searle, Anthony Natural Resources Canada Canada asearle@NRCan.gc.ca

Sekido, Mamoru National Institute of Information

and Communications Technology

Japan sekido@nict.go.jp

Seitz, Manuela Deutsches Geod ̈atisches

Forschungsinstitut

Germany seitz@dgfi.badw.de

Shao, Minghui Urumqi Astronomical

Observatory

China nanshan@ms.xjb.ac.cn

Shibuya, Kazuo National Institute of Polar

Research

Japan shibuya@nipr.ac.jp

Shishikin,

Alexandr

Institute of Applied Astronomy Russia

Shu, Fengchun Shanghai Astronomical

Observatory

China sfc@center.shao.ac.cn

Skurikhina,

Elena

Institute of Applied Astronomy Russia sea@quasar.ipa.nw.ru

Smolentsev,

Sergey

Institute of Applied Astronomy Russia smolen@isida.ipa.rssi.ru

Smythe, Dan MIT Haystack Observatory USA dsmythe@haystack.mit.edu

IVS 2011 Annual Report 337
Associate Members

Name Institution Country E-mail

Sobarzo, Sergio TIGO/Universidad de

Concepci ́on

Chile sergio.sobarzo@tigo.cl

Sousa, Don MIT Haystack Observatory USA dsousa@haystack.mit.edu

Sovers, Ojars Remote Sensing Analysis Inc. USA ojars@oregonfast.net

Spicakova, Hana Institute of Geodesy and

Geophysics

Austria hana@mars.hg.tuwien.ac.at

Stanghellini,

Carlo

Istituto di Radioastronomia

INAF

Italy c.stanghellini@ira.inaf.it

Steppe, Alan Jet Propulsion Laboratory USA as@logos.jpl.nasa.gov

Surkis, Igor Institute of Applied Astronomy Russia surkis@isida.ipa.rssi.ru

Takashima,

Kazuhiro

Geospatial Information

Authority of Japan

Japan takasima@gsi.go.jp

Takiguchi,

Hiroshi

National Institute of Information

and Communications Technology

Japan htaki@nict.go.jp

Tamura,

Yoshiaki

National Astronomical

Observatory of Japan

Japan tamura@miz.nao.ac.jp

Tanimoto,

Daisuke

Geospatial Information

Authority of Japan

Japan vlbi@gsi.go.jp

Tao, An Shanghai Astronomical

Observatory

China antao@center.shao.ac.cn

Tateyama,

Claudio

Centro de R ́adio Astronomia e

Aplica ̧c ̃oes Espaciais

Brazil tateyama@craam.mackenzie.br

Teke, Kamil Hacettepe University Turkey kteke@hacettepe.edu.tr

Thomas,

Cynthia

NVI, Inc. USA cynthia.c.thomas@nasa.gov

Thorandt,

Volkmar

Bundesamt f ̈ur Kartographie

und Geod ̈asie

Germany volkmar.thorandt@bkg.bund.de

Thornton,

Bruce

U. S. Naval Observatory USA blt@usno.navy.mil

Titov, Oleg Geoscience Australia Australia Oleg.Titov@ga.gov.au

Titus, Mike MIT Haystack Observatory USA mtitus@haystack.mit.edu

Todorova, Sonja Institute of Geodesy and

Geophysics

Austria stodo@mars.hg.tuwien.ac.at

Tomasi, Paolo Istituto di Radioastronomia

INAF

Italy tomasi@ira.inaf.it

Trigilio,

Corrado

Istituto di Radioastronomia

INAF

Italy ctrigilio@oact.inaf.it

Tsutsumi,

Masanori

National Institute of Information

and Communications Technology

Japan tsutsumi@nict.go.jp

Tuccari, Gino Istituto di Radioastronomia

INAF

Italy g.tuccari@ira.inaf.it

Ullrich, Dieter Bundesamt f ̈ur Kartographie

und Geod ̈asie

Germany dieter.ullrich@bkg.bund.de

Venturi, Tiziana Istituto di Radioastronomia

INAF

Italy t.venturi@ira.inaf.it

338 IVS 2011 Annual Report
Associate Members

Name Institution Country E-mail

Verdugo, Carlos TIGO/Universidad de

Concepci ́on

Chile carlos.verdugo@tigo.cl

Vespe,

Francesco

Agenzia Spaziale Italiana Italy vespe@asi.it

Vityazev,

Veniamin

Astronomical Institute of

St.-Petersburg

Russia vityazev@list.ru

Volvach,

Alexandr

Crimean Astrophysical

Observatory

Ukraine volvach@crao.crimea.ua

Vytnov,

Alexander

Institute of Applied Astronomy Russia vytnov@isida.ipa.rssi.ru

Wang, Guangli Shanghai Astronomical

Observatory

China wgl@center.shao.ac.cn

Wang, Jinqing Shanghai Astronomical

Observatory

China jqwang@center.shao.ac.cn

Wang, Lingling Shanghai Astronomical

Observatory

China llwang@center.shao.ac.cn

Wang, Na Urumqi Astronomical

Observatory

China Na.wang@ms.xjb.ac.cn

Wang, Weixia Urumqi Astronomical

Observatory

China wangwx@ms.xjb.ac.cn

Wei, Wenren Shanghai Astronomical

Observatory

China wwr@center.shao.ac.cn

Whitney, Alan MIT Haystack Observatory USA awhitney@haystack.mit.edu

Wojdziak,

Reiner

Bundesamt f ̈ur Kartographie

und Geod ̈asie

Germany reiner.wojdziak@bkg.bund.de

Yatskiv,

Yaroslav

Main Astronomical Observatory Ukraine yatskiv@mao.kiev.ua

Ye, Shuhua Shanghai Astronomical

Observatory

China ysh@center.shao.ac.cn

Yusup, Aili Urumqi Astronomical

Observatory

China aliyu@ms.xjb.ac.cn

Zeitlh ̈ofler,

Reinhard

Geodetic Observatory Germany zeitlhoefler@fs.wettzell.de

Zhang, Ali Urumqi Astronomical

Observatory

China zhangal@uao.ac.cn

Zhang, Jin Urumqi Astronomical

Observatory

China zhangj@ms.xjb.ac.cn

Zhang,

Xiuzhong

Shanghai Astronomical

Observatory

China xzhang@shao.ac.cn

Zhao, Rongbing Shanghai Astronomical

Observatory

China zhaorb@center.shao.ac.cn

Zheng, Weimin Shanghai Astronomical

Observatory

China zhwm@shao.ac.cn

Zhou, Ruixian Shanghai Astronomical

Observatory

China zrx@center.shao.ac.cn

IVS 2011 Annual Report 339
IVS Permanent Components

IVS Permanent Components

(listed by types, within types alphabetical by component name)

Network Stations

Component Name Sponsoring Organization Country

Radioastronomical Observatory Badary Institute of Applied Astronomy RAS Russia

Fortaleza, Radio Observat ́orio Espacial do

Nordeste (ROEN)

Centro de R ́adio Astronomia e Aplica ̧c ̃oes

Espaciais

Brazil

Goddard Geophysical and Astronomical

Observatory

NASA Goddard Space Flight Center USA

Hartebeesthoek Radio Astronomy

Observatory

Foundation for Research and Development South Africa

Hobart 12-m and 26-m, Katherine and

Yarragadee

University of Tasmania Australia

Kashima 34-m National Institute of Information and

Communications Technology (NICT)

Japan

Key Stone Project Kashima 11-m National Institute of Information and

Communications Technology (NICT)

Japan

Key Stone Project Koganei National Institute of Information and

Communications Technology (NICT)

Japan

Kokee Park Geophysical Observatory National Earth Orientation Service

(NEOS)

USA

Matera Agenzia Spaziale Italiana (ASI) Italy

Medicina Istituto di Radioastronomia Italy

Mizusawa 10-m National Astronomical Observatory of

Japan (NAOJ)

Japan

Noto (Sicily) Istituto di Radioastronomia Italy

Ny- ̊Alesund Geodetic Observatory Norwegian Mapping Authority Norway

ERS/VLBI Station O’Higgins Bundesamt f ̈ur Kartographie und

Geod ̈asie (BKG)

Germany

Onsala Space Observatory Chalmers University of Technology Sweden

Parkes Observatory CSIRO Astronomy and Space Science Australia

Seshan Joint Laboratory for Radio Astronomy

(JLRA), CAS and Shanghai Observatory,

CAS

China

Simeiz Laboratory of Radioastronomy of Crimean

Astrophysical Observatory

Ukraine

Svetloe Radio Astronomy Observatory Institute of Applied Astronomy RAS Russia

JARE Syowa Station National Institute of Polar Research Japan

340 IVS 2011 Annual Report
IVS Permanent Components

Transportable Integrated Geodetic

Observatory (TIGO)

Universidad de Concepci ́on (UdeC),

Instituto Geogr ́afico Militar (IGM),

Bundesamt f ̈ur Kartographie und

Geod ̈asie (BKG)

Germany,

Chile

Tsukuba VLBI Station Geospatial Information Authority of Japan

(GSI)

Japan

Nanshan VLBI Station Chinese Academy of Sciences China

Warkworth Observatory Auckland University of Technology New Zealand

Westford Antenna, Haystack Observatory NASA Goddard Space Flight Center USA

Geod ̈atisches Observatorium Wettzell Bundesamt f ̈ur Kartographie und Geod ̈asie

(BKG) and Forschungseinrichtung

Satellitengeod ̈asie der Technischen

Universit ̈at M ̈unchen (FESG)

Germany

Observat ́orio Astron ́omico Nacional -

Yebes

Instituto Geogr ́afico Nacional Spain

Radioastronomical Observatory

Zelenchukskaya

Institute of Applied Astronomy RAS Russia

Operation Centers

Component Name Sponsoring Organization Country

Institut f ̈ur Geod ̈asie und Geoinformation

(IGGB)

Universit ̈at Bonn Germany

CORE Operation Center NASA Goddard Space Flight Center USA

NEOS Operation Center National Earth Orientation Service

(NEOS)

USA

Correlators

Component Name Sponsoring Organization Country

Astro/Geo Correlator at MPI Bundesamt f ̈ur Kartographie und

Geod ̈asie, Institut f ̈ur Geod ̈asie und

Geoinformation der Universit ̈at Bonn,

Max-Planck-Institut f ̈ur Radioastronomie

Germany

MIT Haystack Correlator NASA Goddard Space Flight Center USA

Institute of Applied Astronomy Correlator Institute of Applied Astronomy RAS Russia

National Institute of Information and

Communications Technology (NICT)

National Institute of Information and

Communications Technology (NICT)

Japan

Tsukuba VLBI Center Geospatial Information Authority of Japan

(GSI)

Japan

Washington Correlator National Earth Orientation Service

(NEOS)

USA

IVS 2011 Annual Report 341
IVS Permanent Components

Data Centers

Component Name Sponsoring Organization Country

BKG, Leipzig Bundesamt f ̈ur Kartographie und Geod ̈asie Germany

Crustal Dynamics Data Information

System (CDDIS)

NASA Goddard Space Flight Center USA

GeoDAF Agenzia Spaziale Italiana (ASI) Italy

Italy INAF Istituto di Radioastronomia INAF Italy

National Institute of Information and

Communications Technology

National Institute of Information and

Communications Technology

Japan

Observatoire de Paris Observatoire de Paris France

Analysis Centers

Component Name Sponsoring Organization Country

Astronomical Institute of St.-Petersburg

University

Astronomical Institute of St.-Petersburg

University

Russia

Geoscience Australia Geoscience Australia Australia

BKG/DGFI Combination Center Bundesamt f ̈ur Kartographie und

Geod ̈asie and Deutsches Geod ̈atisches

Forschungsinstitut

Germany

Laboratoire d’Astrophysique de Bordeaux Laboratoire d’Astrophysique de Bordeaux France

Centro di Geodesia Spaziale (CGS) Agenzia Spaziale Italiana Italy

DGFI Deutsches Geod ̈atisches Forschungsinstitut Germany

Forsvarets forskningsinstitutt (FFI) Norwegian Defence Research

Establishment

Norway

IGGB-BKG Analysis Center Institut f ̈ur Geod ̈asie und Geoinformation

der Universit ̈at Bonn and Bundesamt f ̈ur

Kartographie und Geod ̈asie

Germany

Goddard Space Flight Center NASA Goddard Space Flight Center USA

Haystack Observatory MIT Haystack Observatory and NASA

Goddard Space Flight Center

USA

Institute of Applied Astronomy Analysis

Center

Institute of Applied Astronomy RAS Russia

Institute of Geodesy and Geophysics

(IGG)

Institute of Geodesy and Geophysics

(IGG) of Vienna University of Technology

Austria

Italy INAF Istituto di Radioastronomia INAF Italy

Jet Propulsion Laboratory Jet Propulsion Laboratory USA

Karadeniz Technical University (KTU) Karadeniz Technical University Turkey

Korea Astronomy and Space Science

Institute

Korea Astronomy and Space Science

Institute

South Korea

342 IVS 2011 Annual Report
IVS Permanent Components

Main Astronomical Observatory Main Astronomical Observatory, National

Academy of Sciences, Kiev

Ukraine

National Astronomical Observatory of

Japan

National Astronomical Observatory of

Japan

Japan

National Institute of Information and

Communications Technology

National Institute of Information and

Communications Technology

Japan

Norwegian Mapping Authority (NMA) Norwegian Mapping Authority (NMA) Norway

Observatoire de Paris Observatoire de Paris France

Onsala Space Observatory Chalmers University of Technology Sweden

Politecnico di Milano DIIAR Politecnico di Milano DIIAR (PMD) Italy

Pulkovo Observatory Pulkovo Observatory Russia

Sternberg State Astronomical Institute Lomonosov Moscow State University Russia

Shanghai Observatory Shanghai Observatory, Chinese Academy

of Sciences

China

Tsukuba VLBI Analysis Center Geospatial Information Authority of Japan

(GSI)

Japan

U. S. Naval Observatory Analysis Center U. S. Naval Observatory USA

U. S. Naval Observatory Analysis Center

for Source Structure

U. S. Naval Observatory USA

Technology Development Centers

Component Name Sponsoring Organization Country

Canadian VLBI Technology Development

Center

NRCan, DRAO Canada

Forsvarets forskningsinstitutt (FFI) Norwegian Defence Research

Establishment

Norway

Goddard Space Flight Center NASA Goddard Space Flight Center USA

Haystack Observatory MIT Haystack Observatory and NASA

Goddard Space Flight Center

USA

Institute of Applied Astronomy

Technology Development Center

Institute of Applied Astronomy RAS Russia

National Institute of Information and

Communications Technology

National Institute of Information and

Communications Technology

Japan

Onsala Space Observatory Chalmers University of Technology Sweden

IVS 2011 Annual Report 343
Contributing Institutions

Addresses of Institutions of Authors Contributing to this Report

(listed alphabetically by country)

CSIRO Astronomy and Space Science

PO Box 76

Epping

NSW 1710

Australia

http://www.atnf.csiro.au

Geoscience Australia

PO Box 378

Canberra ACT

2601

Australia

http://ga.gov.au

University of Tasmania

School of Mathematics and Physics

University of Tasmania

Private Bag 37

Hobart 7001

Australia

http://auscope.phys.utas.edu.au

Institute of Geodesy and Geophysics/University of Technology, Vienna

Gusshausstrasse 27-29

1040 Vienna

Austria

http://www.hg.tuwien.ac.at

CRAAM, Universidade Presbiteriana Mackenzie, S ̃ao Paulo

CRAAM

Instituto Presbiteriano Mackenzie

Rua da Consola ̧c ̃ao 896

01302-907 S ̃ao Paulo

SP

Brazil

http://www.craam.mackenzie.br

Instituto Nacional de Pesquisas Espaciais

Estrada do Fio 6000

Bairro Tupui ́u

1760-000 Eus ́ebio

CE

Brazil

http://www.roen.inpe.br

344 IVS 2011 Annual Report
Contributing Institutions

Geodetic Survey Division, Natural Resources Canada

615 Booth St.

Ottawa

Ontario

Canada K1A 0E9

http://www.geod.nrcan.gc.ca

Bundesamt f ̈ur Kartographie und Geod ̈asie - TIGO

Casilla 4036

Correo 3

Concepci ́on

Chile

http://www.bkg.bund.de

Universidad de Concepci ́on - TIGO

Concepci ́on

Chile

http://www.udec.cl

Shanghai Astronomical Observatory, Chinese Academy of Sciences

80 Nandan Road

Shanghai 200030

China

http://www.shao.ac.cn/eng/

Xinjiang Astronomical Observatory, NAO–CAS

40-5 South Beijing Road

Urumqi

Xinjiang Uygur Autonomous Region

830011

China

http://www.uao.ac.cn

Laboratoire d’Astrophysique de Bordeaux

2 rue de l’Observatoire

BP 89

33271 Floirac Cedex

France

http://www.obs.u-bordeaux1.fr

Observatoire de Paris, SYRTE, CNRS/UMR8630

61 avenue de l’Observatoire

75014 Paris

France

http://www.obspm.fr

Bundesamt f ̈ur Kartographie und Geod ̈asie, BKG

Richard-Strauss-Allee 11

60598 Frankfurt am Main

Germany

http://www.bkg.bund.de

IVS 2011 Annual Report 345
Contributing Institutions

Deutsches Geod ̈atisches Forschungsinstitut, DGFI

Alfons-Goppel-Strasse 11

80539 M ̈unchen

Germany

http://www.dgfi.badw.de

Geod ̈atisches Observatorium Wettzell

Bundesamt f ̈ur Kartographie und Geod ̈asie (BKG) and

Forschungseinrichtung Satellitengeod ̈asie (FESG)

Sackenrieder Str. 25.

D-93444 Bad K ̈otzting

Germany

http://www.fs.wettzell.de

Institut f ̈ur Geod ̈asie und Geoinformation der Universit ̈at Bonn

Nussallee 17

D-53115 Bonn

Germany

http://vlbi.geod.uni-bonn.de

Max-Planck-Institute for Radioastronomy

Auf dem H ̈ugel 69

53121 Bonn

Germany

http://www.mpifr-bonn.mpg.de

Agenzia Spaziale Italiana

Centro di Geodesia Spaziale (CGS)

Contrada Terlecchia

75100 Matera

Italy

http://www.asi.it

Istituto di Radioastronomia–Bologna

Via P. Gobetti 101

40129 Bologna

Italy

http://www.ira.inaf.it

Istituto di Radioastronomia, Medicina

C.P. 14

40060 Villafontana

Bologna

Italy

http://www.med.ira.inaf.it

346 IVS 2011 Annual Report
Contributing Institutions

Istituto di Radioastronomia INAF, Stazione VLBI di Noto

C.P. 161

I-96017 Noto SR

Italy

http://www.noto.ira.inaf.it

Politecnico di Milano, DIIAR

Politecnico di Milano University

DIIAR

Sezione Rilevamento

Piazza Leonardo da Vinci 32

I-20133 Milano

Italy

http://www.diiar.polimi.it

Geospatial Information Authority of Japan

Code 305-0811

Kitasato 1

Tsukuba

Ibaraki

Japan

http://www.spacegeodesy.go.jp/vlbi/en

Mizusawa VLBI Observatory, NAOJ

2-12 Hoshigaoka-cho

Mizusawa-kuk

Oshu-shi

Iwateken

023-0861

Japan

http://www.miz.nao.ac.jp

National Institute of Information and Communications Technology

893-1 Hirai

Kashima

Ibaraki 314-08501

Japan

http://www2.nict.go.jp/w/w114/stmg/index e.html

National Institute of Polar Research

10-3

Midori-cho

Tachikawa-shi

Tokyo 190-8518

Japan

http://www.nipr.ac.jp

IVS 2011 Annual Report 347
Contributing Institutions

Institute for Radio Astronomy and Space Research, Auckland University of Technology

Private Bag 92006

Auckland 1142

New Zealand

http://www.irasr.aut.ac.nz

Forsvarets forskningsinstitutt (FFI) (Norwegian Defence Research Establishment)

FFI/III

Box 25

2007 Kjeller

Norway

http://www.ffi.no/

Norwegian Mapping Authority (NMA)

Kartverksveien 21

3507 H ̈onefoss

Norway

http://www.kartverket.no/

Institute of Applied Astronomy of Russian Academy of Sciences (IAA)

nab. Kutuzova 10

St. Petersburg

191187

Russia

http://www.ipa.nw.ru

Pulkovo Observatory

Pulkovskoe Ch. 65

St. Petersburg

196140

Russia

http://www.gao.spb.ru

Sobolev Astronomical Institute of Saint Petersburg University

Universitetskii pr. 28

Starii Peterhof

Saint Petersburg

198504

Russia

http://www.astro.spbu.ru

Sternberg State Astronomical Institute (SAI) of Lomonosov Moscow State University

Universitetskij prospekt 13

Moscow

119991

Russia

http://www.sai.msu.ru

348 IVS 2011 Annual Report
Contributing Institutions

HartRAO, NRF

PO Box 443

Krugersdorp

1740

South Africa

http://www.hartrao.ac.za

Korea Astronomy and Space Science Institute

305-348

South Korea

http://www.kasi.re.kr

Instituto Geogr ́afico Nacional

Calle General Iba ̃nez de Ibero 3

E-28003 Madrid

Spain

http://www.ign.es/

Observat ́orio Astron ́omico Nacional

Calle Alfonso XII 3

E-28014 Madrid

Spain

http://www.oan.es/

Onsala Space Observatory (OSO)

SE-439 92

Onsala

Sweden

http://www.oso.chalmers.se

Hacettepe University, Department of Geomatics Engineering

Beytepe

06800

Ankara

Turkey

http://geomatik.hacettepe.edu.tr

Karadeniz Technical University, Department of Geomatics Engineering

Trabzon

61080

Turkey

http://www.harita.ktu.edu.tr

Main Astronomical Observatory, National Academy of Sciences of Ukraine

Main Astronomical Observatory

27 Akademika Zabolotnoho St.

Kiev

03680

Ukraine

http://www.mao.kiev.ua

IVS 2011 Annual Report 349
Contributing Institutions

Radio Astronomy Lab of Crimean Astrophysical Observatory

RT-22

Katsively

Yalta Crimea 98688

Ukraine

http://www.crao.crimea.ua

Jet Propulsion Laboratory, California Institute of Technology

Mail Stop 238-600

4800 Oak Grove Dr.

Pasadena, CA 91109

USA

http://www.jpl.nasa.gov

Kokee Park Geophysical Observatory

Kokee State Park

P.O. Box 538

Waimea, Hawaii 96796

USA

http://lupus.gsfc.nasa.gov/kokee park.htm

MIT Haystack Observatory

Off Route 40

Westford, MA 01886

USA

http://www.haystack.mit.edu/

NASA Goddard Space Flight Center

Code 698.2

Greenbelt, MD 20771

USA

http://www.nasa.gov

U.S. Naval Observatory

3450 Massachusetts Ave. NW

Washington, DC 20392

USA

http://www.usno.navy.mil

U.S. Naval Observatory, Flagstaff Station

10391 West Naval Observatory Rd.

Flagstaff, AZ 86001

USA

http://www.nofs.navy.mil

350 IVS 2011 Annual Report
List of Acronyms

List of Acronyms

AAM Atmosphere Angular Momentum

AARNet Australia Academic and Research Network

AAS American Astronomical Society

AC (IVS) Analysis Center

ACF AutoCorrelation Function

ACU Antenna Control Unit

AD Analog-to-Digital

ADB Analog to Digital Board

ADC Analog to Digital Converter

ADEV Allan DEViation

AEB Agˆencia Espacial Brasileira (Brazilian Space Agency) (Brazil)

AER Atmospheric and Environmental Research, Inc. (USA)

AES Advanced Engineering Services Co., Ltd (Japan)

AGILE Astro-rivelatore Gamma ad Immagini LEggero satellite (Italy)

AGN Active Galactic Nuclei

AGU American Geophysical Union

AIPS Astronomical Image Processing System

AIUB Astronomical Institute, University of Bern (Switzerland)

ALMA Atacama Large Millimeter Array

AMRFP Access to Major Research Facilities Program

ANU Australian National University (Australia)

AO Astronomical Object

AOA Allen Osborne Associates

AOC Array Operation Center (Japan)

AOG Auxilliary Output Generator

APEX Atacama Pathfinder EXperiment (Chile)

API Application Programming Interface

APPS Advanced Precise Positioning System

APSG Asia-Pacific Space Geodynamics program

APT Asia Pacific Telescope

APTF Asian Pacific Time and Frequency

ARC Astrometric Radiointerferometric Correlator

ARIES Astronomical Radio Interferometric Earth Surveying program

ARO Algonquin Radio Observatory (Canada)

ASC Astro Space Center (Russia)

ASD Allan Standard Deviation

ASI Agenzia Spaziale Italiana (Italy)

ASKAP Australian Square Kilometre Array Pathfinder (Australia)

ATA Advanced Technology Attachment

ATA Allen Telescope Array (USA)

ATCA Australia Telescope Compact Array (Australia)

ATM Asynchronous Transfer Mode

IVS 2011 Annual Report 351
List of Acronyms

ATNF Australia Telescope National Facility (Australia)

AUSLIG AUstralian Surveying and Land Information Group (now Geoscience Australia

(GA)) (Australia)

AUT Auckland University of Technology (New Zealand)

A-WVR Advanced Water Vapor Radiometer

BAdW Bayerische Akademie der Wissenschaften (Bavarian Academy of Sciences and

Humanities) (Germany)

BBC Base Band Converter

BdRAO Badary Radio Astronomical Observatory (Russia)

BEK Bayerische Kommission f ̈ur die internationale Erdmessung (Germany)

BIPM Bureau Internacional de Poids et Mesures (France)

BKG Bundesamt f ̈ur Kartographie und Geod ̈asie (Germany)

BMC Basic Module of Correlator

BOR1 Body Of Revolution type 1

BOSSNET BOSton South NETwork

BPE Bernese Processing Engine

BPF Band Pass Filter

BVID Bordeaux VLBI Image Database

BW Band Width

BWG Beam WaveGuide

CACS Canadian Active Control System

CAGS Council of Astronomical and Geophysical data analysis Services

CARAVAN Compact Antenna of Radio Astronomy for VLBI Adapted Network (Japan)

CAS Chinese Academy of Sciences (China)

CASPER Center for Astronomy Signal Processing and Electronics Research (USA)

CAY Centro Astron ́omico de Yebes (Spain)

CC (IVS) Combination Center

CC (IVS) Coordinating Center

CDDIS Crustal Dynamics Data Information System (USA)

CDP Crustal Dynamics Project

CDT Centro de Desarrollo Tecnol ́ogico at Yebes Observatory (Spain)

CE Conformit ́e Europ ́eene

CE-1 Chang’E-1 (China)

CfA Harvard-Smithsonian Center for Astrophysics (USA)

CGE Centrum f ̈ur Geod ̈atische Erdsystemforschung (Germany)

CGLBI Canadian Geodetic Long Baseline Interferometry

CGPS Continuous GPS

CGS Centro di Geodesia Spaziale (Italy)

CHAMP Challenging Mini-Satellite Payload

CIB Correlator Interface Board

CIP Celestial Intermediate Pole

CLARA Cooperaci ́on Latino Americana de Redes Avanzadas

CLIWA-NET Cloud LIquid WAter NETwork

CMB Core-Mantle Boundary

352 IVS 2011 Annual Report
List of Acronyms

CMNOC Crustal Monitoring Network Of the Chinese mainland geological environment

(China)

CMONC Crustal Movement Observation Network of China (China)

CMVA Coordinated Millimeter VLBI Array

CNES Centre National d’Etudes Spatiales (France)

CNIG Centro Nacional de Informaci ́on Geogr ́afica (Spain)

CNR Consiglio Nazionale delle Ricerche (Italy)

CNRS Centre National de la Recherche Scientifique (France)

CNS Communication, Navigation and Surveillance systems, Inc. (USA)

CODA Correlator Output Data Analyzer

COL Combination at the Observation Level

CONGO COoperative Network for GIOVE Observation

CORE Continuous Observations of the Rotation of the Earth

CORS Continuously Operating Reference Stations

COTS Commercial-Off-The-Shelf

CP Circularly Polarized

CPO Celestial Pole Offset

CPP IERS Combination Pilot Project

CRAAE Centro de R ́adio Astronomia e Aplica ̧c ̃oes Espaciais (Brazil)

CRAAM Centro de R ́adio Astronomia e Astrof ́ısica Mackenzie (Brazil)

CrAO Crimean Astrophysical Observatory (Ukraine)

CRDS Celestial Reference frame Deep South

CRESTech Centre for Research in Earth and Space Technology (Canada)

CRF Celestial Reference Frame

CRL Communications Research Laboratory (now NICT) (Japan)

CRS Celestial Reference System

CSA Canadian Space Agency (Canada)

C-SART Constrained Simultaneous Algebraic Reconstruction Technique

CSCU Cryogenic System Control Unit

CSIR Council for Scientific and Industrial Research (South Africa)

CSIRO Commonwealth Scientific and Industrial Research Organisation (Australia)

CSRIFS Combined Square Root Information Filter and Smoother

CSRS Canadian Spatial Reference System

CSTnet China Science and Technology Network (China)

CTVA Canadian Transportable VLBI Antenna

CUTE CRL and University Telescopes Experiment (Japan)

CVN Chinese VLBI Network

CW Continuous Wave

CWDM Coarse Wavelength Division Multiplexer

CYLAR CDT Yebes Laser Ranging

DAO GSFC Data Assimilation Office (USA)

DAR Data Acquisition Rack

DAS Data Acquisition System

DASOS DAS Operating System

DAT Digital Audio Tape

IVS 2011 Annual Report 353
List of Acronyms

DBBC Digital Base Band Converter

DBE Digital BackEnd

DDC Digital DownConverter

DDOR Delta Differenced One-way Range

DeltaDOR Delta Differenced One-way Range

DFG Deutsche Forschungsgemeinschaft (German Research Foundation) (Germany)

DFT Discrete Fourier Transform

DGFI Deutsches Geod ̈atisches ForschungsInstitut (Germany)

DGK Deutsche Geod ̈atische Kommission (Germany)

dGPS differential GPS

DHC de Havilland Canada Company

DIIAR Dipartimento di Ingegneria Idraulica, Ambientale, Infrastrutture viarie,

Rilevamento (Italy)

DIISR Department of Innovation, Industry, Science and Research (Australia)

DIM Data Input Module

DISTART Dipartimento di Ingegneria delle Strutture, dei Trasporti, delle Acque,

del Rilevamento del Territorio (Italy)

DLR Deutsches Zentrum f ̈ur Luft- und Raumfahrt (German Aerospace Center)

DNSC Danish National Space Center (Denmark)

DOM Data Output Module

DOMES Directory Of MERIT Sites

DORIS Doppler Orbitography and Radiopositioning Integrated by Satellite

DPFU Degrees Per Flux Unit

DPN Dual Pseudo-random Noise

DR Dichroic Reflector

DRAGON Dynamic Resource Allocation through GMPLS over Optical Networks

DRAO Dominion Radio Astrophysical Observatory (Canada)

DSAMS Direct Sampling Applied for Mixed Signals

DSCB Data Stream Combining Board

DSCIG Direc ̧c ̃ao de Servi ̧cos de Cartografia e Informa ̧c ̃ao Geogr ́afica (Portugal)

DSIF Deep Space Instrumentation Facility

DSN Deep Space Network

DSNA Deep Space Network Array (USA)

DSP Digital Signal Processor

DSS Deep Space Station

DTU10 Danmarks Tekniske Universitet (Denmark)

D-VLBI Differential VLBI

EAN Eastern Asia VLBI Network

EAS European Astronomical Society

ECMWF European Centre for Medium-Range Weather Forecasts

EDM Electronic Distance Measurement

EFTF European Frequency and Time Forum

EGAE Experiment Guided Adaptive Endpoint

EGS European Geophysical Society

EGU European Geosciences Union

354 IVS 2011 Annual Report
List of Acronyms

EIA Environmental Impact Assessment

ELSA European Leadership in Space Astrometry

ENC GNSS European Navigation Conference on Global Navigation Satellite Systems

ENSG L’Ecole Nationale des Sciences G ́eographiques  ́

ENSO El-Ni ̃no/Southern Oscillation

ENVISAT ENVIronmental SATellite

EOP Earth Orientation Parameter

EOP-PC Earth Orientation Parameter Product Center (France)

EOS Earth Observing System

EOT Empirical Ocean Tide

EOT8A Empirical Ocean Tide 2008 model from multi-mission satellite Altimetry

ERP Earth Rotation Parameter

ERS European Remote Sensing Satellites

ESA European Space Agency

ESO European Southern Observatory

ETS-8 Engineering Test Satellite 8

ETSIT Escuela T ́ecnica Superior de Ingenieros de Telecomunicaci ́on

ETS-Lindgren EMC Test Systems-Lindgren (USA)

ETS-VIII Engineering Test Satellite 8

EU European Union

EuCAP European Conference on Antennas and Propagation

EUREF EUropean REFerence Frame

EVGA European VLBI for Geodesy and Astrometry

EVLA Expanded Very Large Array

e-VLBI Electronic VLBI

EVN European VLBI Network

EXPReS Express Production Real-time e-VLBI Service

FACH Fuerza A ́erea de Chile (Air Force of Chile) (Chile)

FAGS Federation of Astronomical and Geophysical data analysis Services

FCN Free Core Nutation

FEM Finite Element Modeling

FES Finite Element Solution

FESG Forschungseinrichtung Satellitengeod ̈asie/Technical University of Munich

(Germany)

FFI Forsvarets ForskningsInstitutt (Norwegian Defence Research Establishment)

(Norway)

FFT Fast Fourier Transform

FFTS Fast Fourier Transform Spectrometer

FGS Forschungsgruppe Satellitengeod ̈asie (Germany)

FICN Free Inner Core Nutation

FILA FIrst LAst

FINEP Financiadora de Estudos e Projetos (Brazilian Innovation Agency) (Brazil)

FIR Finite Impulse Response

FITS Flexible Image Transport System

FOV Field Of View

IVS 2011 Annual Report 355
List of Acronyms

FPDP Front Panel Data Port

FPGA Field-programmable Gate Array

FS Field System

FTP File Transfer Protocol

FWF Fonds zur F ̈orderung der wissenschaftlichen Forschung (Austrian Science Fund)

GA Geoscience Australia (Australia)

GALAXY Giga-bit Astronomical Large Array with cross connect

GAPE Great Alaska and Pacific Experiment

GARNET GSI Advanced Radiotelescope NETwork (Japan)

GARR Gruppo per l’Armonizzazione delle Reti della Ricerca

(Italian Academic and Research Network) (Italy)

GARS German Antarctic Receiving Station (Germany)

GASP GLAST-AGILE Support Program

GBT Green Bank Telescope (USA)

GCGO Gilmore Creek Geophysical Observatory (USA)

GDR altimeter Geophysical Data Record

GEMD Geospatial and Earth Monitoring Division (Australia)

GeoDAF Geodetic Data Archiving Facility (Italy)

GEX Giga-bit series VLBI EXperiment

GFZ GeoForschungsZentrum (Germany)

GGAO Goddard Geophysical and Astronomical Observatory (USA)

GGFC Global Geophysical Fluids Center

GGN Global GPS Network

GGOS Global Geodetic Observing System

GGP Global Geodynamics Project

GICO GIga-bit COrrelator

GINS G ́eod ́esie par Int ́egrations Num ́eriques Simultan ́ees

GIOVE Galileo In-Orbit Validation Element

GISTM GPS Ionospheric Scintillation and TEC Monitor

GIUB Geodetic Institute of the University of Bonn (now IGGB) (Germany)

GLAST Gamma ray Large Area Space Telescope (USA)

GLDAS Global Land Data Assimilation System

GLONASS GLObal NAvigation Satellite System (Russia)

GLORIA GLObal Radio Interferometry Analysis

GMF Global Mapping Function

GMPLS Generalized MultiProtocol Label Switching

GMST Greenwich Mean Sideral Time

GNS Science Geological and Nuclear Sciences Research Institute (New Zealand)

GNSS Global Navigation Satellite Systems

GOCE Gravity field and steady-state Ocean Circulation Explorer

GOT Goddard/Grenoble Ocean Tide

GOW Geodetic Observatory Wettzell

GP-B Gravity Probe B

GPS Global Positioning System

GPT Global Pressure and Temperature

356 IVS 2011 Annual Report
List of Acronyms

GR General Relativity

GRACE Gravity Recovery and Climate Experiment (USA)

GREAT-ESF Gaia Research for European Astronomy Training — European Science

Foundation

GREF German GPS REFerence network

GRGS Groupe de Recherches de G ́eod ́esie Spatiale (France)

GSD Geodetic Survey Division of Natural Resources Canada (Canada)

GSFC Goddard Space Flight Center (USA)

GSI Geospatial Information Authority of Japan (formerly Geographical Survey

Institute) (Japan)

GSK Generalized Spectral Kurtosis

GSOS GPS Surface Observing System

GSS Generator of Synchronization Signals

GST Greenwich Sideral Time

HAMTIDE Hamburg direct data Assimilation Methods for TIDEs

HartRAO Hartebeesthoek Radio Astronomy Observatory (South Africa)

HAT-Lab High Advanced Technology-Lab (Italy)

HEMT High Electron Mobility Transistor

HF High Frequency

HIA Herzberg Institute for Astrophysics (Canada)

HIRLAM High Resolution Limited Area Model

Honeywell TSI Honeywell Technology Solutions Inc. (USA)

HOPS Haystack Observatory Postprocessing System

HPBW Half Power Beam Width

HPC High Performance Compute

HSI High Speed Input bus

HSIR High Speed Input Replicated bus

HTS High Temperature Superconductor

HTSI Honeywell Technology Solutions Incorporated (USA)

HVAC Heating, Ventilation, and Air Conditioning

IAA Institute of Applied Astronomy (Russia)

IAG International Association of Geodesy

IAPG Institute of Astronomical and Physical Geodesy (Germany)

IAU International Astronomical Union

IBGE Instituto Brasileiro de Geografia e Estatistica (Brazil)

IBM International Business Machines Corporation (USA)

iBOB Interconnect Break Out Board

ICRAR International Centre for Radio Astronomy Research (Australia)

ICRF International Celestial Reference Frame

ICRF2 2nd Realization of the International Celestial Reference Frame

ICRS International Celestial Reference System

IDS International DORIS Service

IDV IntraDay Variability

IERS International Earth Rotation and Reference Systems Service

IETF Internet Engineering Task Force

IVS 2011 Annual Report 357
List of Acronyms

IF Intermediate Frequency

IGFN Italian Space Agency GPS Fiducial Network (Italy)

IGFS2 second International Symposium of the Gravity Field of the earth

IGG Institute of Geodesy and Geophysics (Austria)

IGGB Institut f ̈ur Geod ̈asie und Geoinformation der Universit ̈at Bonn (Germany)

IGGOS Integrated Global Geodetic Observing System (now GGOS)

IGM Instituto Geogr ́afico Militar (Chile)

IGN Institut Geographique National (France)

IGN Instituto Geogr ́afico Nacional (Spain)

IGS International GNSS Service

IISGEO International Institute for Space Geodesy and Earth Observation

I-JUSE Institute of Japanese Union of Scientists and Engineers (Japan)

IKAROS Interplanetary Kite-craft Accelerated by Radiation of the Sun (Japan)

ILRS International Laser Ranging Service

IMC Interface Module of Correlator

IMF Isobaric Mapping Function

INACH Institute for Antarctic Research Chile

INAF Istituto Nazionale di Astrofisica (Italy)

INGV Institute of Geophysics and Volcanology (Italy)

INPE Instituto Nacional de Pesquisas Espaciais (Brazil)

InSAR Interferometric Synthetic Aperture Radar

IP Internet Protocol

IPWV Integrated Precipitable Water Vapor

IRA Istituto di RadioAstronomia (Italy)

IRAS InfraRed Astronomy Satellite

IRASR Institute for Radio Astronomy and Space Research (New Zealand)

IRIS International Radio Interferometric Surveying

IRP Invariant Reference Point

IRSR Institute for Radiophysics and Space Research (New Zealand)

ISACCO Ionospheric Scintillations Arctic Campaign Coordinated Observation

ISAS Institute of Space and Astronautical Science (Japan)

ISBN International Standard Book Number

ISI Information Sciences Institute (USA)

ISV Instantaneous State Vector

ITIS Istituto di Tecnologia Informatica Spaziale (Italy)

ITRF International Terrestrial Reference Frame

ITRS International Terrestrial Reference System

ITSS (Raytheon) Information Technology and Science Services (USA)

IUGG International Union of Geodesy and Geophysics

IVOA International Virtual Observatory Alliance

IVP Invariant Point

IVS International VLBI Service for Geodesy and Astrometry

IWV Integrated Water Vapor

IYA International Year of Astronomy

JADE JApanese Dynamic Earth observation by VLBI

358 IVS 2011 Annual Report
List of Acronyms

JARE Japanese Antarctic Research Expedition (Japan)

JAXA Japan Aerospace Exploration Agency (Japan)

JENAM Joint European and National Astronomy Meeting

JGN Japan Gigabit Network (Japan)

JGR Journal of Geophysical Research

JHB JoHannesBurg

JIVE Joint Institute for VLBI in Europe

JLRA Joint Laboratory for Radio Astronomy (China)

JMA Japan Meteorological Agency (Japan)

JPL Jet Propulsion Laboratory (USA)

JSPS Japanese Society for the Promotion of Science (Japan)

JST Japan Standard Time

KARAT KAshima RAy-tracing Tools (Japan)

KARATS KAshima RAy-Tracing Service (Japan)

KAREN Kiwi Advanced Research and Education Network (New Zealand)

KASI Korea Astronomy and Space Science Institute (Korea)

KAT Karoo Array Telescope (South Africa)

KBR K-Band Ranging

KEG Kommission f ̈ur Erdmessung und Glaziologie (Germany)

KPGO Kokee Park Geophysical Observatory (USA)

KPSS Kwiatkowski-Phillips-Schmidt-Shin

KSP KeyStone Project (Japan)

KSRC Kashima Space Research Center (Japan)

KSTC Kashima Space Technology Center

KTU Karadeniz Technical University (Turkey)

KTU-GEOD Karadeniz Technical University (KTU), Department of Geomatics Engineering

(Turkey)

KVG Korea VLBI system for Geodesy (Korea)

KVM Keyboard, Video, and Mouse

KVN Korean VLBI Network

LAB Laboratoire d’Astrophysique de Bordeaux (France)

LAGEOS LAser GEOdynamic Satellite

LAMOST Large Sky Area Multi-object Fiber Spectroscopic Telescope (China)

LAREG Laboratoire de Recherches en G ́eod ́esie (France)

LBA Long Baseline Array (Australia)

LCP Left Circular Polarization

LCS Long baseline array Calibrator Survey

LD Laser Diode

LEA Lab of Ephemeris Astronomy (Russia)

LED Light-Emitting Diode

LEIF Large Equipment and Infrastructure Funding

LEO Low Earth Orbit

LHC Left Hand Circular

LIEF Large Infrastructure and Equipment Funding

LINZ Land Information New Zealand (New Zealand)

IVS 2011 Annual Report 359
List of Acronyms

LLR Lunar Laser Ranging

LNA Low Noise Amplifier

LNMAG Lab of New Methods in Astrometry and Geodynamics (Russia)

LO Local Oscillator

LOC Local Organizing Committee

LOD Length Of Day

LPF Low Pass Filter

LPI Lebedev Physical Institute (Russia)

LRS Laser Ranging System

LSB Lower Side Band

LSC Least Squares Collocation

LSF Large Scale Facility

LSGER Lab of Space Geodesy and Earth Rotation (Russia)

LSM Least Squares Method

LSQM Least Squares Method

MAO Main Astronomical Observatory (Ukraine)

MARBLE Multiple Antenna Radio-interferometry for Baseline Length Evaluation

MBH Mathews/Buffett/Herring Nutation Model

MCB Monitor and Control Bus

MCI Monitor and Control Infrastructure

MDION Multi-Dimensional IONosphere modeling

MEI Multivariate ENSO Index

MERIT Monitoring of Earth Rotation and Intercomparison of the Techniques of

Observation and Analysis

METLAB Microwave Energy Transmission LABoratory (Japan)

MEX Mars Express

MIT Massachusetts Institute of Technology (USA)

MITEQ Microwave Information Transmission EQuipment (USA)

MJD Modified Julian Date

MLRO Matera Laser Ranging Observatory (Italy)

MNHD Mineral and Natural Hazard Division (Australia)

MOBLAS MOBile LASer

MODEST MODel and ESTimate

MOU Memorandum of Understanding

MPI Max-Planck-Institute (Germany)

MPIfR Max-Planck-Institute for Radioastronomy (Germany)

MPM Millimeter-wave Propagation Model

MRO Mars Reconnaissance Orbiter

MRO Mets ̈ahovi Radio Observatory (Finland)

MSL Mars Science Laboratory

MTLRS Modular Transportable Laser Ranging System

NAO National Astronomical Observatories (China)

NAO National Astronomical Observatory (Japan)

NAOC National Astronomical Observatories of China (China)

NAOJ National Astronomical Observatory of Japan (Japan)

360 IVS 2011 Annual Report
List of Acronyms

NAR Noise-Adding Radiometer

NASA National Aeronautics and Space Administration (USA)

NASU National Academy of Sciences of Ukraine (Ukraine)

NCAR National Center for Atmospheric Research (USA)

NCEP National Centers for Environmental Prediction (USA)

NCRIS National Collaborative Research Infrastructure Strategy (Australia)

NDBC National Data Buoy Center

NDRE Norwegian Defence Research Establishment (Norway)

NEA Near-Earth Asteroid

NENS Near Earth Network Services

NEOS National Earth Orientation Service (USA)

NEQ Normal Equation System

NESDIS National Environmental Satellite, Data, and Information Service (USA)

NetCDF Network Common Data Form

NEXPReS Novel EXploration Pushing Robust e-VLBI Services

NGII National Geographic Information Institute (Korea)

NGS National Geodetic Survey (USA)

NGSLR Next Generation Satellite Laser Ranging

NICT National Institute of Information and Communications Technology (Japan)

NII National Institute of Informatics (Japan)

NIPR National Institute of Polar Research (Japan)

NMA Norwegian Mapping Authority (Norway)

NMF Niell Mapping Function

NNR No-Net-Rotation

NNT No-Net-Translation

NOAA National Oceanic and Atmospheric Administration (USA)

NOFS U.S. Naval Observatory, Flagstaff Station (USA)

NORAD North American Aerospace Defense Command

NOT Nordic Optical Telescope

NRAO National Radio Astronomy Observatory (USA)

NRCan Natural Resources Canada (Canada)

NRF National Research Foundation (South Africa)

NSF National Science Foundation (USA)

NTT New Technology Telescope (Chile)

NTT Nippon Telegraph and Telephone Corporation (Japan)

NVI NVI, Inc. (USA)

NWP Numerical Weather Prediction

NySMAC Ny- ̊Alesund Science Managers Committee

OAM Observatorio Astron ́omico de Madrid (Spain)

OAN Observatorio Astron ́omico Nacional (Spain)

OCA Observatoire de la Cˆote d’Azur (France)

OCARS Optical Characteristics of Astrometric Radio Sources

OPAR Observatoire de Paris (France)

OPC (IVS) Observing Program Committee

ORCA Optical ReCeiver/splitter/Amplifier

IVS 2011 Annual Report 361
List of Acronyms

OS Operating System

OSI Operator Software Impact

OSO Onsala Space Observatory (Sweden)

OTL Ocean Tidal Loading

PARNASSUS Processing Application in Reference to NICT’s Advanced Set of Softwares Usable

for Synchronization

PASJ Publications of the Astronomical Society of Japan

PASP Publications of the Astronomical Society of the Pacific

PATA Parallel Advanced Technology Attachment

PCAL Phase CALibration

PCB Printed Circuit Board

PCU Power Control Unit

PEACESAT Pan-Pacific Education and Communication Experiments by Satellite

PERSAC Pulkovo EOP and Reference Systems Analysis Center (Russia)

PF Processing Factor

PFB Polyphase Filter Bank

PIVEX Platform Independent VLBI EXchange format

PLC Programmable Logic Controller

PLO Phase Locked Oscillator

PM Polar Motion

PMD Politecnico di Milano DIIAR (Italy)

PNR Peak to Noise Ratio

POLARIS POLar motion Analysis by Radio Interferometric Surveying

POP Point of Presence

PPN Parameterized Post-Newtonian

PPP Precise Point Positioning

PRAO Pushchino Radio Astronomy Observatory (Russia)

PRARE Precise RAnge and Range-rate Equipment

PSD Power Spectrum Density

QDOR Quadruply Differenced One-way Ranging

QRFH Quad Ridge Feed Horn

QRHA Quad-Ridge Horn Antenna

QZSS Quasi Zenith Satellite System (Japan)

RAEGE Red Atl ́antica de Estaciones Geodin ́amicas y Espaciales

RAS Russian Academy of Sciences (Russia)

RCP Right Circular Polarization

RCU Receiver Control Unit

RDBE Roach Digital Back End

RDV Research and Development sessions using the VLBA

RedCLARA CLARA (Cooperaci ́on Latino Americana de Redes Avanzadas) network

REFAG Reference Frames for Applications in Geosciences

REGINA REseau GNSS pour l’IGS et la NAvigation (GNSS Receiver Network for IGS and

Navigation) (France)

REPA REsidual Plotting and Ambiguity resolution

REUNA Red Universitaria Nacional (Chile)

362 IVS 2011 Annual Report
List of Acronyms

RF Radio Frequency

RFCN Retrograde Free Core Nutation

RFI Radio Frequency Interference

RHC Right Hand Circular

ROACH Reconfigurable Open Architecture Computing Hardware

ROEN R ́adio-Observat ́orio Espacial do Nordeste (Brazil)

ROM Real Observatorio de Madrid (Spain)

RRFID Radio Reference Frame Image Database

RS-232C Recommended Standard-232C

RT Radio Telescope

RTK Real-Time Kinematic

RTNF Radio Telescope National Facility (New Zealand)

RTP Real-Time Protocol

RTW Radio Telescope in Wettzell

SAC Satellite Application Centre

SAGE Small Advanced Geodetic e-VLBI System

SAI Sternberg State Astronomical Institute (Russia)

SAN Storage Area Network

SAR Synthetic Aperture Radar

SATA Serial Advanced Technology Attachment

SBIR Small Business Innovation Research

SCG SuperConducting Gravimeter

SCNS Space Communications Network Services

SCR Silicon Controlled Rectifier

SDK Software Development Kit

SDM Signal Distribution Modules

SDSS Signal Distribution and Synchronization System

SEAC Sociedad Espa ̃nola de Aplicaciones Cibern ́eticas (Spain)

SEFD System Equivalent Flux Density

SETI Search for Extraterrestrial Intelligence

SGL Space Geodynamics Laboratory (Canada)

SGT Stinger Ghaffarian Technologies (USA)

SHAO SHanghai Astronomical Observatory (China)

SI Special Issue

SI Structure Index

SIMD Single Instruction Multiple Data

SINEX Solution INdependent EXchange

SISMA Seismic Information System for Monitoring and Alert

SK Spectral Kurtosis

SKA Square Kilometre Array

SLR Satellite Laser Ranging

SMART Small Missions for Advanced Research and Technology

SMHI Swedish Meteorological and Hydrological Institute (Sweden)

SNAP Standard Notation for Astronomical Procedures

SNR Signal to Noise Ratio

IVS 2011 Annual Report 363
List of Acronyms

SNSN Swedish National Seismic Network (Sweden)

SOD Site Occupation Designator

SOSW Satellite Observing System Wettzell (Germany)

SPb Saint-Petersburg (Russia)

SPbU Saint-Petersburg University (Russia)

SPEED Short Period and Episodic Earth rotation Determination

SPU Saint-Petersburg University (Russia)

SPV Signal Path Variation

SRIF Square Root Information Filter

SRT Sardinia Radio Telescope (Italy)

SRTM Shuttle Radar Topography Mission

SSA Singular Spectrum Analysis

SSAI Science Systems and Applications, Inc. (USA)

STDN Satellite Tracking Data Network (NASA)

STEREO Solar TErrestrial RElations Observatory

SU Station Unit

SVD Singular Value Decomposition

SvRAO Svetloe Radio Astronomical Observatory (Russia)

SWT SW Technology (USA)

SYRTE SYst`eme de R ́ef ́erences Temps-Espace

TAC Totally Accurate Clock

TAI Temps Atomique International (International Atomic Time)

TAL Terrestrial Air Link

TANAMI Tracking Active galactic Nuclei with Austral Milliarcsecond Interferometry

(Australia)

TanDEM-X TerraSAR-X add-on for Digital Elevation Measurement (Germany)

TAO Telecommunications Advanced Organization (Japan)

TCE Time Comparison Equipment

TDC (IVS) Technology Development Center

TEC Total Electron Content

TECU Total Electron Content Units

TEM Transverse ElectroMagnetic

TEMPO Time and Earth Motion Precision Observations

TENET Tertiary Education and Research Network of South Africa (South Africa)

TERENA Trans-European Research and Education Networking Association

TerraSAR Terra Synthetic Aperture Radars (Germany)

TerraSAR-X Terra Synthetic Aperture Radars X-band (Germany)

TID Traveling Ionospheric Disturbance

TIGA–PP GPS TIde GAuge Benchmark Monitoring Pilot Project

TIGO Transportable Integrated Geodetic Observatory (Germany, Chile)

TLE Two Line Elements

TLRS Transportable Laser Ranging System

TMR Training and Mobility of Researchers program of the European Community

ToR IVS Terms of Reference

TOW Technical Operations Workshop

364 IVS 2011 Annual Report
List of Acronyms

TRF Terrestrial Reference Frame

TSPM Test Synchronization Pulsar gating Module

TTW TWIN-Telescope Wettzell (Germany)

TU Technische Universit ̈at

TUM Technical University of Munich (Germany)

TWA Travel Wave Antennas

TWSTFT Two-Way Satellite Time and Frequency Transfer

UAO Urumqi Astronomical Observatory (China)

UBB Universidad del B ́ıo B ́ıo (Chile)

UC Berkeley University of California, Berkeley (USA)

UD Upper Diagonal

UDC Up-Down Converter

UEN Up East North

UMTS Universal Mobile Telecommunications System

UNAVCO University NAVSTAR Consortium

UNICAMP Universidade Estadual de Campinas (Brazil)

UNISEC UNIversity Space Engineering Consortium (Japan)

UNITEC-1 UNIsec Technological Experiment Carrier-1 (Japan)

UREO Ultra-Rapid Earth Orientation

URSI Union Radio-Scientifique Internationale

USB Unified S-Band

USB Upper Side Band

USNO United States Naval Observatory (USA)

USP Universidade de S ̃ao Paulo (Brazil)

USS Uniform Sky Strategy

UT Universal Time

UT1 Universal Time

UTAS University of TASmania (Australia)

UTC Coordinated Universal Time

u-VLBI Ultra High Sensitivity VLBI

UWB Ultra WideBand

V2PEG VLBI2010 Project Executive Group

VC Video Converter

VCS VLBA Calibrator Survey

VDBE VLBA Digital BackEnd

VDIF VLBI Data Interchange Format

VEGA Venus-Halley project (Russia)

VERA VLBI Exploration of Radio Astrometry

VEX Venus EXpress

VEX VLBI EXchange format

VHDL Very High-level Design Language

VieVS Vienna VLBI Software

VLA Very Large Array (USA)

VLBA Very Long Baseline Array (USA)

VLBI Very Long Baseline Interferometry

IVS 2011 Annual Report 365
List of Acronyms

VMF Vienna Mapping Function

VO Virtual Observatory

VSI VLBI Standard Interface

VSI-C Mets ̈ahovi VSI-H Converter board

VSI-H VLBI Standard Interface Hardware

VSI-S VLBI Standard Interface Software

VSN Volume Serial Number

VSOP VLBI Space Observatory Program

VSR VLBI Science Recorder

VSSP Versatile Scientific Sampling Processor

VTEC Vertical Total Electron Content

VTM Vienna TEC (Total Electron Content) Model

VTP VLBI Transport Protocol

VTRF VLBI Terrestrial Reference Frame

WACO WAshington COrrelator (USA)

WEBT Whole Earth Blazar Telescope

WEGENER Working Group of European Geoscientists for the Establishment of Networks for

Earth-science Research

WG Working Group

WGS84 World Geodetic System 1984

WIDAR Wideband Interferometric Digital ARchitecture

WLRS Wettzell Laser Ranging System (Germany)

WMAP Wilkinson Microwave Anisotropy Probe

WVR Water Vapor Radiometer

WVSR Wideband VLBI Science Recorder

WWW World Wide Web

XDM eXperimental Development Model

ZcRAO Zelenchukskaya Radio Astronomical Observatory (Russia)

ZTD Zenith Total Delay

ZWD Zenith Wet Delay

366 IVS 2011 Annual Report

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30-06-2012 Technical Publication

International VLBI Service for Geodesy and Astrometry 2011 Annual Report

Karen D. Baver, Dirk Behrend

Goddard Space Flight Center

Greenbelt, MD 20771

National Aeronautics and Space Administration

Washington, DC 20546-0001

NASA GSFC

NASA/TP-2012-217505

Unclassified-Unlimited, Subject Category: 46

Report available from the NASA Center for Aerospace Information,7115 Standard Drive, Hanover, MD 21076. (443) 757-5802

Karen Baver, NVI, Inc., Greenbelt, MD; Dirk Behrend, NVI, Inc., Greenbelt, MD

This volume of reports is the 2011 Annual Report of the International VLBI Service for Geodesy and Astrometry (IVS). The

individual reports were contributed by VLBI groups in the international geodetic and astrometric community who constitute the

components of IVS. The 2011 Annual Report documents the work of these IVS components over the period January 1, 2011

through December 31, 2011. The reports document changes, activities, and progress of the IVS. The entire contents of this Annual

Report also appear on the IVS Web site at http://ivscc.gsfc.nasa.gov/publications/ar2011.

Geodesy, astrometry, VLBI, geophysics, Earth orientation, very long baseline interferometry, radio astronomy, geodynamics,

reference frames, terrestrial reference frame, celestial reference frame, length of day, Earth system science, Earth rotation.

Unclassified Unclassified Unclassified Unclassified 366

Chopo Ma

(301) 614-6101
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Front cover:

The development and use of new technology continues to advance within IVS. The front cover shows four selected examples of design and development work described 

in this year’s Annual Report (in clockwise direction): [top right] broadband phase calibration system (breadboard model) at Svetloe Observatory; [bottom right] 

experimental wide-band feed elements for Arrayed Travel Wave Antenna studies developed at NICT and cooperating Japanese institutions; [bottom left] prototype of 

a Balun-fed Eleven feed with a linear taper developed at Chalmers University; and [top left] QRFH broadband feed at the Westford 18-m antenna. More details about 

the displayed technology are available in the Technology Development (TD) Center reports of IAA (p. 287ff), NICT (p. 291ff), Onsala Space Observatory (p. 295ff) and 

Haystack Observatory (p. 283ff), respectively. Photos are courtesy of these TD Centers and their collaborators at other institutions.
International VLBI Service for Geodesy and Astrometry

IVS Coordinating Center

NASA Goddard Space Flight Center

Code 698.2

Greenbelt, MD 20771

http://ivscc.gsfc.nasa.gov

ivscc@ivscc.gsfc.nasa.gov

phone: 301-614-5939

fax: 301-286-0239