Upload
darci
View
37
Download
0
Tags:
Embed Size (px)
DESCRIPTION
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 - PowerPoint PPT Presentation
Citation preview
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
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
KVN Yonsei Observatory(Yonsei University at Seoul)
KVN Ulsan Observatory(Ulsan University)
KVN Tamna Observatory(Tamna University)
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
Outline
- Receivers and their test results
Quasi-optical circuit forMulti-band receivers
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
43GHz( Black )
The Pointing offset between 22GHz and 43GHz band at Jupiter
)"7.0,"1.0(, ELAZ22GHz( Red )
Orion-KL H2O and SiO Maser Line
Simultaneous Observation Results !!!!!on October 28th 2008
East Asian VLBI Network with KVNEast Asian VLBI Network with KVN
YonseiUniv.
Mizusawa
W49N H2O maserStar formation region
W49N H2O MaserDater : 2008. 11. 1.
Honma et al.(2008)
Development of 22GHz receiver
RHCP LHCP
LNAs
Polarizer & OMT
Isolator
Development of 22GHz receiver
IF converter22GHz down to 9GHz/2GHz
Amplitude and phaseCalibrator for receiver
Development of 43GHz receiver
Isolator
RHCPLHCP LNAs
Polarizer & OMT
M&CLocal osc
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
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
Q-band HEMT amplifier from NRAO
Expected Receiver noise temperature : 35~40K
Outline
- DAS(Data Acquisition System)
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
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
Outline
- Future plan and Summary
Timeline for system development2008 2009 2010 2011
Optics86/129G
22GHz
43GHz
86GHz
129GHz
Phase cal.System
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.
Thanks for your attention