3360m2

2000m2

Spec. of STELab IPS
Observatory
TypeFeedobservation
Beam
Aperture (m2)Frequency (MHz)
Bandwidth (MHz)Tsys (K)integration (ms)NSEW

Toyokawa
Double Cylindrical Parabola394(=192x2) l/2dipoles
transitelectronical phasing
fixed
3360

146
20Fuji

Kiso
Sugadaira
Cylindrical Parabola
192, 144, 192 l/2dipoles
trackingmechanical pointing
electronical phasing
2000
327MHz
10MHz
151
221
229
20 (100)

FE configuration at Toyokawa
32LNAs×6blocks＝192

W-dpl
E-dpl
LNA
D

D

DDA2
D

Delay（＋AMP） Unit

A3

A4

A5A6DD130m
outside building
FE box↑RFIF

SQD/LF
Delay module→

inside building
327MHz70MHz

PC

10kHz sampling, 16bitA/DMedian filter +Averaging
50Hz sampling

WS

FTP to Nagoya every nightLevel diagram of TY systemantenna

Back-end in building
ant. house RFIF

LF

No. of sources
No. of LOSHistory of STEL-IPS

150

100
500

1970

1975

1980

1985

1990

1995

2000

2005

• 1970’s: VHF observations(STELab data were combined with Cambridge data)• 1983- : UHF observations• 1994 : KS ant. started.
• 2005 : Old TY ant. closed.
• 2009 : New TY started• 2011 : replacement of dipoles in FJ and KS• 2012- : Upgrade of Backend in FJ and KS• 2013- : Upgrade of Frontend and refreshment of ant structure.

2010

grey area: Velocity is not derived bytomographic analysis because of insufficient
coverage of LOS≓≧≲≥≹≃≯≶≥≲≡≧≥ ∽ ∱ ⊡ ≓≴≯≴≡≬

Long Term Variation of Solar WindNo. of sources
No. of LOSHistory of STEL-IPS

150

100
500

1970

1975

1980

1985

1990

1995

2000

2005

2010

• VHF data consist of STEL and Cambridge observations.
• Coverage of VHF observation is insufficient to reconstruct V mapeven if number of LOS are comparable to UHF observation because
the number of radio sources were very limited.
• Selection of IPS sources and the number of IPS sources areimportant to research whole interplanetary space.

Upgrades of FJ, KS, and SG antenna
Upgradepainting (antirust)
Antenna
KS motor (NS pointing)reflector (efficiency)
FE receiver (Low noise)
Ant. Elevation Control system @KS

cost
0.5 M$
0.33 M$
0.03 M$• Refreshments of Antenna have been finished in last month.
• FE receivers has been installed in FJ obs. in last month and willbe installed in KS obs. in next spring.
• Antenna Control system will be upgraded in next week.

Spec. of Front-end receiverFrequency
Gain
Noise Figure
VSWR
Gain Controller
Phase shifter

327±10MHz33 dB
0.8 dB (max)
1.3:1
0.25 dB step / 5Bits
11.25 deg step / 5 Bits

RFRF out

CAL1
CAL2

LNA
BPF
PATT+33dB 10MHz 5bits

PS
RF short5bits

painting after removing rust and moldrustmold

rupturedSummaryObservatory
Typeobservation
Beam
Aperture (m2)Frequency (MHz)
Bandwidth (MHz)Tsys (K)integration (ms)NSEWToyokawa
Double Cylindrical Parabolatransitelectronical phasing
fixed3360

14620Fuji

327MHz
10MHz
151

Kiso
Sugadaira
Cylindrical Parabola
trackingmechanical pointing
electronical phasing
2000

221
20229

• Antennas at Fuji, Kiso and Sugadaira are in upgrading phase.
• Refreshment of Antenna has been finished in last month.
• FE receivers has been installed in FJ antenna in last month and will
be installed in KS antenna in next spring.
• Upgrade of elevation controller will be started today.
• We will check total performance of the IPS system in next season.

Is Fuji-ant. Improved ?
Front-end configuration
dipoleLNA
A1
A2

A3

A4

installation of new LNA• Easy maintenance• fine beam
• but it often deforms .
• trouble of phasing controller/control
line (optical & metal)• S/N is not improved.
• Same level as old LNA.
• Output of amp. in signal combiner line
may saturate.
 BPF will be inserted at input of amp.

saturated?

outside buildingRFinside building

IFSQD/LF
PCWSBack-end