Welcome & ALMA Project Report
Satoru Iguchi
26 December 2017
National Astronomical Observatory of Japan

Science Papers – Output Rate

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ALMA Project Report

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ALMA Status – Summary 1
 Construction Project ended in Sep. 2014 (there are still a numberof remaining construction items to be finished, e.g. theResidencia, which was fully completed in 2017)

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ALMA Status – Summary 2

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Availability of Array Elements(October 2016 to September 2017)

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ALMA Capabilities from Cycle 0 to 5164530

10515

Band 9: 450 μm (602-720 GHz)o Both single field interferometry andpointed mosaicso Up to four simultaneous spectral
windows available with same
bandwidth and resolution

10.50(84-116 GHz)

Band 6: 1 mm (211-275 GHz)
Band 7: 850 μm (275-370 GHz)
Baselines (in km)

Minimum Number of Antennas

60Band 3: 3 mm0.02

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Cycle 0(~600 h)
Sep. 2011

8ALMA Capabilities from Cycle 0 to 5164530

10515

Band 9: 450 μm (602-720 GHz)o Both single field interferometry andmosaics
o Mixed correlator modes (both highand low frequency resolution in thesame observation)

10.50(84-116 GHz)

Band 6: 1 mm (211-275 GHz)
Band 7: 850 μm (275-370 GHz)
Baselines (in km)

Minimum Number of Antennas

60Band 3: 3 mm

0.02

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Cycle 1(800 h)
Jan. 2013

9ALMA Capabilities from Cycle 0 to 516453010Baselines (in km)

Minimum Number of Antennas

6051510.500.02

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Band 3: 3 mm (84-116 GHz)
Band 4: 2 mm (125-163 GHz)
Band 6: 1 mm (211-275 GHz)
Band 7: 850 μm (275-370 GHz)
Band 8: 650 μm (385-500 GHz)
Band 9: 450 μm (602-720 GHz)

Cycle 2(2000 h)
June 2014

o Both single field interferometry and mosaics
o Spectral-line observations with all Arrays andcontinuum observations with the 12-m Array
and the 7-m Array.
o Polarization (on-axis, continuum, selected
frequencies in Band 3, 6 and 7, no ACA, nomosaics)o Mixed correlator modes (both high and low
frequency resolution in the sameobservation)
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10ALMA Capabilities from Cycle 0 to 5164530

10Baselines (in km)

Minimum Number of Antennas

60

515

10.50

Band 3: 3 mm (84-116 GHz)
Band 4: 2 mm (125-163 GHz)
Band 6: 1 mm (211-275 GHz)
Band 7: 850 μm (275-370 GHz)
Band 8: 650 μm (385-500 GHz)
Band 9: 450 μm (602-720 GHz) )Band 10: 350 μm (787-950 GHz)o High-fidelity imaging, mosaickingo Flexible correlator (up to 16narrow spectral windows, or 8 GHzbandwidth)o Polarization (linear polarization incontinuum and spectral line)

0.02

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Cycle 3(2100 h)
Oct. 2015

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ALMA Capabilities from Cycle 0 to 516453010Baselines (in km)

Minimum Number of Antennas

60

5151

Band 3: 3 mm (84-116 GHz)
Band 4: 2 mm (125-163 GHz)
Band 6: 1 mm (211-275 GHz)
Band 7: 850 μm (275-370 GHz)
Band 8: 650 μm (385-500 GHz)
Band 9: 450 μm (602-720 GHz)Band 10: 350 μm (787-950 GHz)

oooo

Large program
ACA standalone
mmVLBI
Solar Observation

0.500.02

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NAOJ Project WeekCycle 4(3000 h)
Oct. 2016

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ALMA Capabilities from Cycle 0 to 516453010Baselines (in km)

Minimum Number of Antennas

60

5151

Band 3: 3 mm (84-116 GHz)
Band 4: 2 mm (125-163 GHz)
Band 6: 1 mm (211-275 GHz)
Band 7: 850 μm (275-370 GHz)
Band 8: 650 μm (385-500 GHz)
Band 9: 450 μm (602-720 GHz) )Band 10: 350 μm (787-950 GHz)
Band 5: 1.5 mm (163-211 GHz)o Maximum baseline length of 16 km at Bands
3, 4, and 6
o Band 5 at short baseline configuration only

0.500.02

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Cycle 5(4000 h)
Oct. 2017

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13Planned ALMA Capabilities of Cycle 6164530

10Baselines (in km)

Minimum Number of Antennas

6051510.500.02

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Band 3: 3 mm (84-116 GHz)
Band 4: 2 mm (125-163 GHz)
Band 6: 1 mm (211-275 GHz)
Band 7: 850 μm (275-370 GHz)
Band 8: 650 μm (385-500 GHz)
Band 9: 450 μm (602-720 GHz)
Band 10: 350 μm (787-950 GHz)
Band 5: 1.5 mm (163-211 GHz)

Cycle 6(~4300 h)
Oct. 2018o Maximum baseline length of 16 km at Bands
3, 4, 5, 6, 7?
o Band 8 as a standard modeo Circular polarization (possibly)o Proposal deadline is on April 19
o APRC chair – Masao Saito
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14Planned ALMA Capabilities of Cycle 7164530

10Baselines (in km)

Minimum Number of Antennas

60515

10.500.02

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Band 3: 3 mm (84-116 GHz)
Band 4: 2 mm (125-163 GHz)
Band 6: 1 mm (211-275 GHz)
Band 7: 850 μm (275-370 GHz)
Band 8: 650 μm (385-500 GHz)
Band 9: 450 μm (602-720 GHz)
Band 10: 350 μm (787-950 GHz)
Band 5: 1.5 mm (163-211 GHz)

Cycle 7(~4300 h)
Oct. 2019o Maximum baseline length of 16 km at Bands
3, 4, 5, 6, and 7
o Circular polarization (possible for Cycle 6)o Wide-field mosaicking in polarizationo Single-dish spectral line by Band 9&10
o Total Power Continuumo APRC chair – Masao Saito
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15ALMA Status: Receivers
Receiver Bands currently installed on all antennas,in construction and under study: Band 1: 6 mm
 Band 2: 4 mm
 Band 3: 3 mm
 Band 4: 2 mm
 Band 5: 1.5 mm
 Band 6: 1 mm
 Band 7: 850 μm
 Band 8: 650 μm
 Band 9: 450 μm
 Band 10: 350 μm

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1 2

(35-52 GHz)
(65-90 GHz)(84-116 GHz)
(125-163 GHz)
(163-211 GHz)
(211-275 GHz)
(275-370 GHz)(385-500 GHz)(602-720 GHz)(787-950 GHz)NAOJ Project Week

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Steady State Operations and Beyond Performance based milestone– 7300 hours scheduled for science activities annually• Successful hours offered ~ 4300 (85% of array elements at a given time of 5000)• ≤970 h for weather and array calibration each• ≤320 h for technical issues• Testing and further development ~730 hours– Minimum of 56 antennas in service (daytime)• 43 12-m + 10 7-m + 3 SD Challenges– Weather recovery; Antenna/receiver uptime (corrective maintenance) Capability Driven Milestone– 7300 hours scheduled for science activities annually– Single Dish: continuum and high frequency– Polarization: Stokes V and wide fields– Long Baseline: Band 7 maximum baseline length
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ALMA Status – Summary 3
 Bring ALMA to Full & Stable Operations
 Increase the new science capabilities• Roadmap for Future Developments in next 10-20 years that will
enable ALMA to extend the frontiers of science even further

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ALMA Upgrade Planning

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EA ALMA Development Workshops – Status –Output: three EA led projects/studies

2011
Development WS

Band 1

Output: New science demands for ALMA
Angular Res.
Fidelity

2013
Development WS
2014
ASTE/ALMA
Development WS

FOV

Sensitivity

Wide IF

Output: Science requirements, ASTE/ALMA dev timeline
Multi-beam

2015
Antenna Structure
Development WS

THz

TES Cam

Wideband Spectrometer

Output: Antenna Cost vs performance

http://almaintweb.mtk.nao.ac.jp/~diono/meetin
gs/EA_Development_Meeting/
http://almaintweb.mtk.nao.ac.jp/~diono/meetin
gs/ASTE_ALMA_2014/
http://almaintweb.mtk.nao.ac.jp/~diono/meetin
gs/NRO_ALMA_2015/

Output: Software/Calibration strategies and demands

http://almaintweb.mtk.nao.ac.jp/~diono/meetin
gs/NRO_ALMA_2016/

Output: AIs for long baseline testing. Need to identify solid science case.

http://almaintweb.mtk.nao.ac.jp/~diono/meetin
gs/longBL2017/

2016
Development WS2017
Long Baseline WS(Kyoto, Oct 3-5, 2017)

Artificial Calibration Source

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20First five year Science Goals of ALMA Operations• Origins of Galaxies– The ability to detect spectral line emission from CO or C+ in a normal
galaxy like the Milky Way at a redshift of z = 3, in less than 24 hours ofobservation;• Origins of Planets– The ability to image the gas kinematics in a solar-mass protoplanetary disk
at a distance of 150 pc, enabling one to study the physical, chemical, andmagnetic field structure of the disk and to detect the tidal gaps created byplanets undergoing formation;• High-fidelity Images– The ability to provide precise images at an angular resolution of 0.1.”

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21ALMA Long Baseline Workshop• Organized by D. Iono

http://alma-intweb.mtk.nao.ac.jp/~diono/meetings/longBL2017/– Participants: more than 80

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22Spatial Resolution [arcsec]

Finer resolution

ALMA Potential Performance
Solid lines：under operation or
terminatedDashed lines：under construction orplanning
ALMA will continue to be the forefront
telescope in spatial resolution among
the next generation telescopes
planning in the coming 30 years.

/ SUBARU/ TMT

Wavelength [µm]CHILE | S. I. | 26 Dec. 2017

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0.01 arcsec corresponds to 1 AU
at the distance of ~300 light yrswhere many protoplanetarydisks are present.
Credit: AURA

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ALMA Management Structure

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ALMA Top Management– 2017 Dec: ALMA Management Team (AMT) –• ALMA Top Management

JAO: Stuartt Corder (Acting Director)

EA: Satoru Iguchi
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Sean Dougherty

EU: Leonardo Testi (Interim)
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NA: Phil Jewell24

EA ALMA Support Center (EAASC)– Previous Organization Structure –EAASC Head(S. Iguchi)

EA IET
Manager(S. Asayama)

EA ICTManager(G. Kosugi)

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EADevelopment
Programme
Manager(S. Asayama)

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EA Project
Scientist(D. Iono)

EA ARCManager(K. Tatematsu)

EA EPO
Officer(M. Hiramatsu)

EA ALMA Support Center (EAASC)– New Organization Structure –EAASC Head(S. Iguchi)

EA IET
Manager(S. Asayama)

EA ICT
Manager(G. Kosugi)

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EADevelopment
Programme
Manager(A.Gonzalez)

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EA Project
Scientist(D. Iono)

EA ARCManager(H. Nagai)

EA EPO
Officer(M. Hiramatsu)

The Atacama Large Millimeter/submillimeter Array (ALMA), an international astronomy facility, is apartnership of ESO (representing its members states), NSF (USA) and NINS (Japan), together with
NRC (Canada), NSC and ASIAA (Taiwan), and KASI (Republic of Korea), in cooperation with theRepublic of Chile. The Joint ALMA Observatory is operated by ESO, AUI/NRAO and NAOJ. The
National Radio Astronomy Observatory is a facility of the National Science Foundation operated
under the cooperative agreement by Associated Universities Inc. We than all those who have
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Project Week
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contributed tomaking
the ALMA project possible.