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The Progress Report for KVN Construction. Seog-Tae Han and KVN staffs Korea Astronomy and Space Science Institute March18 th 2009. Outline. Overview of KVN Antenna construction Receivers and their test results
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The Progress Report for KVN Construction Seog-Tae Han and KVN staffs Korea Astronomy and Space Science Institute March18th 2009
Outline • Overview of KVN • Antenna construction • Receivers and their test results • DAS(Data Acquisition System) • Future plan and Summary
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 Seoul (Yonsei) Ulsan (Ulsan) Overview of KVN Jeju(Tamna)
KVN Yonsei Observatory (Yonsei University at Seoul)
KVN Ulsan Observatory (Ulsan University)
KVN Tamna Observatory (Tamna University)
Aperture efficiencies • Pointing Accuracy- 4 arcsec at 100GHz
Outline • Receivers and their test results
(단위 : 백만원) Quasi-optical circuit for Multi-band receivers
(단위 : 백만원) Quasi-optical circuit installed at receiver room of antenna 22GHz RX 43GHz RX M3 M2 Cal chopper M5 M4 M1
The Pointing offset between 22GHz and 43GHz band at Jupiter 22GHz ( Red ) 43GHz ( Black )
Orion-KL H2O and SiO Maser Line Simultaneous Observation Results !!!!! on October 28th 2008
East Asian VLBI Network with KVN Mizusawa YonseiUniv.
W49N H2O Maser Dater : 2008. 11. 1. W49N H2O maser Star formation region Honma et al.(2008)
Development of 22GHz receiver Polarizer & OMT Isolator RHCP LHCP LNAs
Development of 22GHz receiver Amplitude and phase Calibrator for receiver IF converter 22GHz down to 9GHz/2GHz
M&C Development of 43GHz receiver Local osc LHCP LNAs RHCP Polarizer & OMT Isolator
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
Receiver Noise temperature of 22GHz and 43GHz band Receivers
Q-band HEMT amplifier from NRAO Expected Receiver noise temperature : 35~40K
Outline • DAS(Data Acquisition System)
4channels 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 DAS (Data Acquisition System)
Digital Filter mode 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
Outline • Future plan and Summary
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.