Introduction of Korea Radio Astronomy Facilities · Introduction of Korea Radio Astronomy...
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Introduction of Korea Radio Astronomy Facilities Hyunwoo Kang, Tae-Hyun Jung, Jung-Won Lee, Do-Heung Je,& Bangwon Lee Korea Astronomy and Space Science Institute Korea Astronomy and Space Science Institute (KASI) has grown with radio astronomy in 1986. Taeduk Radio Astronomy Observatory (TRAO) has 14m telescope, and it is the first telescope for Korean radio astronomers. Korea VLBI Network (KVN) has born by experience on the TRAO, and the three 21m telescopes has become one of the important facility on VLBI network. As a member of East-Asia community, JCMT and ALMA are also supported to Korean Astronomers. Technical in-kind contribution at receiver and GPU spectrometer parts is based on the ALMA utilization. Phased Array Feed (PAF) is on long term project of single dish facility. KASI will be good companion for the future development. SEQUOIA-TRAO (SEcond QUabbin Optical Imaging Array) Type : InP MMIC preamplifier Pixels : 16 pixels in a 4X4 array Range : 85~115.6 GHz 1st IF : 5~20 GHz (BW:15 GHz) 2nd IF : two output (0~62.5 MHz) with individual LO T sys : 170K @ 100 GHz ~ 400K @ 150 GHz New Backend - FFT2G Input port : 32 inputs, SMA type (8 inputs per module) Bandwidth : 125 MHz (0~125 MHz) Resolution : 15kHz with 0.05 km/sec Channel : 8192 ch A 2GHz wide band down converter TRAO homepage Youtube Changing Radome
Transcript of Introduction of Korea Radio Astronomy Facilities · Introduction of Korea Radio Astronomy...
Introduction of Korea Radio Astronomy FacilitiesHyunwoo Kang, Tae-Hyun Jung, Jung-Won Lee, Do-Heung Je,& Bangwon Lee
Korea Astronomy and Space Science Institute
Korea Astronomy and Space Science Institute (KASI) has grown with radio astronomy in 1986. Taeduk Radio Astronomy Observatory (TRAO)
has 14m telescope, and it is the first telescope for Korean radio astronomers. Korea VLBI Network (KVN) has born by experience on the TRAO, and the
three 21m telescopes has become one of the important facility on VLBI network. As a member of East-Asia community, JCMT and ALMA are also supported
to Korean Astronomers. Technical in-kind contribution at receiver and GPU spectrometer parts is based on the ALMA utilization. Phased Array Feed (PAF) is on long term project of single dish facility. KASI will be good companion for the future development.
SEQUOIA-TRAO (SEcond QUabbin Optical Imaging Array)
Type : InP MMIC preamplifier Pixels : 16 pixels in a 4X4 array Range : 85~115.6 GHz 1st IF : 5~20 GHz (BW:15 GHz) 2nd IF : two output (0~62.5 MHz) with individual LO Tsys : 170K @ 100 GHz ~ 400K @ 150 GHz
New Backend - FFT2G
Input port : 32 inputs, SMA type (8 inputs per module) Bandwidth : 125 MHz (0~125 MHz) Resolution : 15kHz with 0.05 km/sec Channel : 8192 ch
A 2GHz wide band down converter
TRAO homepage
Youtube Changing Radome
Introduction of Korea Radio Astronomy FacilitiesHyunwoo Kang, Tae-Hyun Jung, Jung-Won Lee, Do-Heung Je,& Bangwon Lee
Korea Astronomy and Space Science Institute
Site Locations
KVN & Extended KVN INFORMATION
Simulation on KVN and Extended KVNSource KVN Extended KVN
Miniaturization & Modulation on M.F.Rx
smaller
Separated
KVN homepage
Extended KVN (2020~)
Simulation shows that Extended KVN adds short baseline for VLBI, and it make extended source can be detected.
For Extended KVN, new multi-frequency Rx is being developed by KVN team. There are two module, one is for three low frequencies (22, 44, & 86 GHz), and the other is for high frequencies (125 & 230 GHz).
Introduction of Korea Radio Astronomy FacilitiesHyunwoo Kang, Tae-Hyun Jung, Jung-Won Lee, Do-Heung Je,& Bangwon Lee
Korea Astronomy and Space Science Institute
Beam Measurement System
Other Projects
(ASTE) Band 7+8 Receiver
Beam Measurement System (BMS) is developed for BAND7+8 horn test by KASI team. It measures beam parameters with semi-OTF method that one-side horn flies on one-direction only. It results fast and more reliable data.
