Download - The Progress Report for KVN Construction
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The Progress Report for KVN Construction
Seog-Tae Han and KVN staffs
Korea Astronomy and Space Science Institute
March18th 2009
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Outline
- Overview of KVN- Antenna construction- Receivers and their test results- DAS(Data Acquisition System)- Future plan and Summary
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Seoul (Yonsei)
Ulsan (Ulsan)
Jeju(Tamna)
2001 ~ 2008 3 stations with 21m radio telescopes - Cassegrain type 22,43,86 and 129GHz band Receiver - Simultaneous observation of four bands - first proposed in the world Digital DAS system has been completed Correlators will be completed in 2010 Millimeter-wave VLBI Astronomy
Overview of KVN
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KVN Yonsei Observatory(Yonsei University at Seoul)
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KVN Ulsan Observatory(Ulsan University)
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KVN Tamna Observatory(Tamna University)
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Efficiency(%)
EL(°)
Remark TB*(K)
Aperture efficiencies at 22GHz
Venus 68(70) 30 LPF2 505+-25**
Aperture efficiencies at 43GHz
Venus 68.8(70) 32 LPF2 450+-32
Aperture efficiencies at 100GHz
Venus 51 40
• Aperture efficiencies
• Pointing Accuracy - 4 arcsec at 100GHz
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Outline
- Receivers and their test results
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Quasi-optical circuit forMulti-band receivers
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Quasi-optical circuit installed at receiver room of antennaQuasi-optical circuit installed at receiver room of antenna
M5
Calchopper
22GHz RX
43GHz RX
M4 M1
M2M3
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43GHz( Black )
The Pointing offset between 22GHz and 43GHz band at Jupiter
)"7.0,"1.0(, ELAZ22GHz( Red )
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Orion-KL H2O and SiO Maser Line
Simultaneous Observation Results !!!!!on October 28th 2008
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East Asian VLBI Network with KVNEast Asian VLBI Network with KVN
YonseiUniv.
Mizusawa
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W49N H2O maserStar formation region
W49N H2O MaserDater : 2008. 11. 1.
Honma et al.(2008)
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Development of 22GHz receiver
RHCP LHCP
LNAs
Polarizer & OMT
Isolator
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Development of 22GHz receiver
IF converter22GHz down to 9GHz/2GHz
Amplitude and phaseCalibrator for receiver
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Development of 43GHz receiver
Isolator
RHCPLHCP LNAs
Polarizer & OMT
M&CLocal osc
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KVN Down Converter Properties
Input Frequency : 8-10 GHz
Output Frequency : 512-1024 MHz
LO Frequency : 8.7-10.8 GHz, LSB
Number of Channel : 4 Channel
Output Power : ~ 0 dBm
Headroom : > 20 dB
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Receiver Noise temperature of 22GHz and 43GHz band Receivers
F.S.+F.S Mode(22 GHz) & F.S.+F.M. Mode(43 GHz)Receiver Noise Temperature
0.010.020.030.040.050.060.070.080.090.0
9000 9500 10000 10500
FSyn [MHz]
Trx
[K
] 22G LCP22G RCP43G LCP43G RCP
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Q-band HEMT amplifier from NRAO
Expected Receiver noise temperature : 35~40K
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Outline
- DAS(Data Acquisition System)
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DAS (Data Acquisition System)
4 channels Analog Inputs( 750MHz/500MHz IFs of 22, 43, 86, 129GHz ) 4 channels 2Gbps(500MHz) samplers 1Gbps recorder (MK5B) 256MHz, 128NHz,64MHz, 32MHz,16MHz and 8MHz 500MHz 4 channels digital spectrometers - single antenna observation mode It has been completed for 3 stations
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Digital Spectrometer Mode 1. Wide band mode - 512MHz X 4 bands ( 22,43,86,129GHz) @4096ch. 2. Narrow band mode - 256MHz, 128MHz, 64MHz, 32MHz, 16MHz, 8MHz
Digital Filter mode
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Outline
- Future plan and Summary
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Timeline for system development2008 2009 2010 2011
Optics86/129G
22GHz
43GHz
86GHz
129GHz
Phase cal.System
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Summary and Discussion
- Simultaneous observation for 22/43GHz and VLBI Observation between KVN and VERA successfully have been performed - Aperture efficiency : 51%@100GHz- Pointing accuarcy : 4”@ 100GHzx- 22/43GHz Receivers will be installed at KVN Ulsan and Tamna observatories in this year - 86GHz and 129GHz will be completed until 2011.
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Thanks for your attention