vlbi 29-31 oct. 2014 development status of broadband vlbi system (gala-v) -(ii) m.sekido (1),...
DESCRIPTION
Space Technologies for Distant Frequency Comparison Space Technologies for Distant Frequency Comparison GNSS(Common view, PPP) Two way Satellite Time and Frequency Transfer(TWSTFT) VLBI VLBI TWSTFT GNSS Precise Frequency Transfer over intercontinental distancesTRANSCRIPT
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VLBI Consortium@Tsukuba 29-31 Oct. 2014Development Status of Broadband VLBI
System (Gala-V) -(II)
M.Sekido(1), K.Takefuji(1), H.Ujihara(1), M.Tsutsumi(1), Y.Miyauchi(1), S.Hasegawa(1), T.Kondo(1), E.Kawai(1), R.Ichikawa(1), H.Takiguchi(1), T.Goto(1), K.Watabe(2),
T.Suzuyama(2), Y.Koyama(1)
1) National Institute of Information and Communications Technology2) National Metrology Institute of Japan
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Contents of presentation Frequency transfer via VLBI Gala-V system Development
Broadband observation Marble1,2 (1.5m,1.6m) : 3-15GHz Kashima34m : 6-14GHz
Compliant with VGOS (Next generation Global VLBI system)
Installation to NMIJ(Tsukuba) and NICT(Koganei) First Geodetic observation after installation Principle proving
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Space Technologies for Distant Frequency Comparison
GNSS(Common view, PPP) Two way Satellite Time and Frequency Transfer(TWSTFT) VLBI
VLBITWSTFT
GNSS
Precise Frequency Transfer over intercontinental distances
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Comparison of TWSTFT,GPS,VLBIExp. on 19-22 Feb. 2012
TWSTFT
GPS
VLBI(500MHz)VLBI(1GHz)
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Comparison of TWSTFT,GPS,VLBIExp. on 19-22 Feb. 2012
TWSTFT
GPS
VLBI(500MHz)VLBI(1GHz)
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BW:500MHz BW:1GHz
σ: 3 4 p sec σ: 21 psec
VLBI Delay residual is improved by expanding observation frequency band.
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Precision of VLBI
Major error sources1. Error of atmospheric delay
estimation2. Thermal noise ∝ 1/(SNR x BW)
Tsukuba 32m – MBL2(1.5m)
Antenna Diameter
RMS residual
11m-11m ~ 30 psec.32m-11m ~ 20 psec.32m-1.5m ~ 30 psec.
Example of VLBI analysisDelay residual plot
MBL2(1.5m)Koganei
Tsukuba 32m
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Gala-V project OverviewCombination of Small and Large Diameter antennas
Obs. Freq. : 3-14GHz Freq. Range Observation: 4 band (1024MHz)
Fc = 4.0GHz, 5.6GHz, 10.4GHz, 13.6GHz,
Effective BW: 3.8GHz (10 times of conventional)
Station 1 Station 2
Station 3
1 3 2
1GHz
4.0GHz 5.6GHz 10.4GHz 13.6GHz
10 times fine delay resolution function is expected. 𝜏21=𝜏1 3−𝜏2 3
Delay observable of Baseline 1-2 is obtained from 1-3 and 2-3 baseline data.
VLBI Sensitivity :
VLBI SensitivityB: 16MHz → 1024MHz (64 times)
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Developments of New Technologies for the Gala-V system
Zero redundancy Array for 4 channels.
Fine Delay resolution without ambiguity.
1 3 2
1GHz
4.0GHz5.6GHz 10.4GHz 13.6GHz
Target Precision: 30 ps -> 7 ps
Bandwidth Synthesis for10 times wider frequency range
Broadband observation
High speed sampler (16GHz) GALAS
Direct RF Sampling
Broadband Feed Design
Image of `Iguana’ feed
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VLBI2010 Global Observing System VGOS(Next generation Geodetic
VLBI)
Radio Frequency: 2-14GHz Antenna Slew Speed:
( >3deg/sec) Target Accuracy: 1mm
GoddardNASA/GSFC(USA)
Spain
IshiokaGSI ( Japan)
Badary IAA(Russia) Wettzell
BKG(Germany)
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RFI 調査2-18GHz at Tokyo,Kashima, and Tsukuba
Tsukuba 2012.Jul 11
Koganei 2012 Jul. 5
Kashima 2012.Jul 4
18GHz2GHz
With 3.5GHz HPF before LNA
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• VLBI2010 仕様に 部分準拠• 1 GHz x 4 band 3-15GHz Frequency Range
Kashima 34m antenna1.5m compact antenna
1.6/1.5m and 34m VLBI antenna
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“Iguana” Feed
Image of `Iguana’ wideband feed
Requirement:• 35 deg. Beam width over the wide
frequency range.
Apparent diameter of subref. is 35 deg. from focal point.
Wideband prototype feed designed by Dr. Ujihara has been installed to Kashima 34m with room temp. LNA at the end of 2013.
This feed has sensitivity at 6.4-14GHz range at present. Upgraded feed with 2.2-18GHz Freq. range is intended.
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Performance of the Prototype broadband Feed
6 8 10 12 14 16 180
50100150200250300350400
Frequency [GHz]
Tsys
* [K
]
30 ~ 40 %
6 8 10 12 14 16 180
10
20
30
40
50
60
70 Aperture Efficiency
Frequency[GHz]
Effici
ency
[%]
6 8 10 12 14 16 180
5001000150020002500300035004000
SEFD-GalaV-high
Frequency[GHz]
SEFD
[Jy]
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Methanol Maser Simultaneous Observation of Methanol
Maser line at 6.7GHz and 12.2GHz on W3OH for test observation (first light) on 16 Jan.2014.
6.7GHz 12.2 GHz
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Kas34-Mbl1 (12GHz:512MHz) 3C273B
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Kas34-Mbl1 W3OH ( 12.181GHz )
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First Fringeswith VERA (6.7GHz)Observation on 1st-2nd Oct. 2014
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Data Acquisition: 1GHz x 4 Ch
Two Approaches1. Analog Down Converter + “ADS3000+”
Digital BBC function for legacy mode observation.
2. Direct Sampler “GALAS” Digital Down Conversion function for any
frequency by 1MHz step.
ADS3000+ SamplerDBBC or 1-2 Gsps
Direct Sampler K6/OCTAD-G code name=“GALAS”DBBC(BW=1024MHz)
K6/OCTAD-G‘GALAS’ K6/DAS PC
K6/DAS PC
10G Ether
D/CADS3000+
ADS3000+
K5/VSIK5/VSIK5/VSIK5/VSI
VSI-H
RF
RF IF
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RF-Box of MARBLE small antenna
Noise-Cal Controller
Equalizer and Coupler
Wide band optical Transmitter
HPF(3.5GHz)
PCAL Signal Generator
Monitoring at Observation Room (3-15GHz). RBW=5kHz
Peltier Cooler
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Observation Frequency Band &Ionosphere Delay Contribution
1 2 3 4 5 6 7 8 9 10 11 12 13 14 150.0
5.0
10.0
15.0
20.0
25.0
30.0
35.0
40.0
5TECU10TECU50TECU
Frequency [GHz]
Phas
e De
lay
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Ready for Observation
22
1.5mAntennaNICT Koganei
1.6m AntennaNMIJ Tsukuba
34m Antenna NICT Kashima
MARBLE2 MARBLE1KASHIMA 34m
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1.6m/1.5m and 34m VLBI antennas
NICT/Kashima
NMIJ
NICT/Koganei
have been installed for T&F.
Geodetic VLBI Experiments on Apr. 22, May 14, May30 to fix station coordinates.
Station Coordinates Repeatability: Horizontal < 6mm Vertical < 15mmDelay Residual WRMS is about 35 psec@30sec.
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Geodetic VLBI Observation Stations:
Kashima(34m),Tsukuba(1.6m),Koganei(1.5m)
Radio Frequency: X-band: 8080-9080MHz, Bandwidth: 1GHz
Experiments: Gx14112: 2014. Apr. 22-23 24 hours. Gx14134: 2014. May 14-15 24 hours. GX14150: 2014. May 30-31 24 hours.
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Geodetic Observation in April-May
-17 -16 -15 -14 -13 -12 -11 -1060
65
70
75
80
85
90
95
100East - Up [mm]
-17 -16 -15 -14 -13 -12 -11 -10
-24
-23
-22
-21
-20
-19
-18
-17
-16
-15East - North [mm]
5mm
5cm
5mm
5mm
41 41.5 42 42.5 43 43.5 44 44.5 45 45.5 46
-65
-60
-55
-50
-45
-40
-35
-30 East - Up [mm]
41 42 43 44 45 46
-10
-9
-8
-7
-6
-5
-4
-3
-2 East - North [mm]
10m
m
5mm
4c m
5mm
MARBLE1(NMIJ,Tsukuba) MARBLE2(NICT,Koganei)
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Clock Estimation Stations:
Kashima(34m),Tsukuba(1.6m),Koganei(1.5m)
Experiments: Gx14112: 2014. Apr. 22-23 24 hours. Gx14134: 2014. May 14-15 24 hours. GX14150: 2014. May 30-31 24 hours.
Analysis: OA,OB->AB baseline data conversion
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Time comparison Analysis
Apr.22
May 30
May 14
GPSGPS
GPS
VLBI
VLBI
VLBIBIPM-Final
BIPM-Rapid
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Clock Estimation from VLBI data
Clock parameters seems is stable against changes of analysis conditions.
Error of AB baseline data composed from OA,OB data increased by sqrt(2) as expected.
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Nest steps to be done Long span VLBI observations for
frequency comparison Broadband Observations
Domestic: Kashima34,Marble1,Marble2
Geodetic, Time transfer experiments International: We are planning to
perform intercontinental broadband observation with MIT/Haystack.
Target precision:
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Acknowledgements Broadband Feed Development is
supported by NAOJ-fund(Prof. Fujisawa et al.)
Gala-V Experiments is supported by NMIJ:(Dr.Watabe, Dr.Amemiya,
Dr.Suzuyama)
Thank you for Attention!
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-12 -10 -8 -6 -4 -2 0 2 4 6 8
-10
-8
-6
-4
-2
0
2
4
6
8
10E-N [mm]
AB Baseline Data
-8 -6 -4 -2 0 2 4 6
-30
-25
-20
-15
-10
-5
0
5E-U [mm]
15mm
3cm
10m
m
10mm