Progress and Early Science of the Thai National Radio National Astronomical Institute of Thailand (Public Organisation) Ministry of Science and Technology Observatory On behalf of RANGD project & Radio Astronomy Group and S. Koichiro (NAOJ) Dr.Kitiyanee Asanok (NARIT) EAVN2018, Pyeong Chang, South Korea, Sep. 4-7, 2018
Radio Astronomy Network and Geodesy for Development (RANGD) 2017-2021 Capacity Building Through Radio Astronomy Thai National Radio Observatory (TNRO) 40m Thai Radio Telescope (TNRT) 13m VGOS Telescope Visitor Centre Receiver and Electronics Laboratories Workshops & Seminars Human Expertise Trainings & Staff exchange
Background of TNRT Multipurpose ~40m RT with flexibility (preferably) Existing Design limited experience Frequency ~ UHF - ~115 GHz determined by Science area, Radio Frequency Interference, Weather conditions Key attributes Extensive observing frequency : 300 MHz - 115 GHz Ideal latitude location : +18 N Single Dish Applications focus on Time Domain astronomy, such as pulsars and radio transients and variability of masers and extra-galactic sources.
RANGD International Technical Advisory Committee (1st Meeting; March 18) 2 nd Meeting will be ~Nov. 2018
RANGD Phase I (2017-2018) Timeline 2018 2019 2020 Sitework 40m TNRT Installation L-, K-band Backend SAT Science Commissioning
40m Thai National Radio Telescope `Updated version of IGN s 40m Yebes Radio Telescope 40m Paraboloid Antenna, Cassegrain-Nasmyth optics 300 MHz - 115 GHz Multi-propose Antenna Geodesy & Time standards Strategic location for VLBI observation Generates demand for R&D on State-of-the-art technology 40m Yebes, Spain 40m RT Contract Signing March 17
Sensitivity L-band K-band Location Primary Focus Nasmyth Focus Frequency range (GHz) 1.0-1.8 18.0-26.5 Centre wavelength (cm) 21.4 1.36 Beam width (arcmin) 22 1.4 Polarisation Linear Circular Cross polarisation -25 db -25 db RF BW 800 MHz 8 GHz sampler 3 Gsps >4 Gsps Packetizer BW 1.5 GHz >2 GHz digitisation bits < 12 bit < 12 bit Total efficiency 0.7 0.5 Gain (K/Jy) 0.32 0.23 Trx (K) 13 20 Tsky (K) 12 50 Tsys (K) 25 70 SEFD (Jy) 78 304
System Diagram Develop a single unit capable of pulsar mode; coherent dedispersion, full-stokes filterbank files, transient search spectral-line mode; CLASS format (GILDAS) write vdif to mark6 Pros expandability; flexibility; real-time RFI excision; COTS components Cons low performance per watt (not a problem for single pixel Rx)
Participating in VLBI networks e-vlbi?
6m foundation excavation +6m piles
RANGD Phase I+II Timeline 2018 2019 2020 2021 Sitework 40m TNRT Installation L-, K-band Backend SAT Science Commissioning C-band Rx (TBC) Q+W Rx (TBC) 13m VGOS (SHAO)
Time-domain Astronomy (S. Koichiro, NAOJ) Key advantages Extensive observing frequency : 300 MHz - 115 GHz Ideal latitude location : +18 N Maser & Molecular thermal lines (L & K bands) Flux variability in star-forming regions Flux variability in late-type (evolved) stars Radial velocity drift in mega-masers Pulsars & Transients Pulsar timing, millisecond pulsars, etc Fast Radio Bursts The Milky Way & Active Galactic Nuclei
How important the TNRT40m (S. Koichiro, NAOJ) Great contribution for better uv-coverage Fill in the southernmost location in the EAVN One of the longest baselines in the EAVN High sensitivity with one of larger diameters The third largest telescope of 40-m in the current EAVN Enable us to conduct VLBI at L-band One of a few telescopes usable at L-band in the EAVN Providing us great opportunity for collaborations and unprecedented scientific results!
ขอบค ณค ะ KOB KOON KA 대단히감사합니다.
Highlights on pulsar ligo.org Fast rotating neutron stars Unique properties mass (canonical) ~ 1.4 solar masses radius (canonical) ~ 10 km rotational period ~ 0.0014-8.5 s magnetic filed ~ 10^(8-14) gauss highly polarised emission Over 2,600 discovered so far (ATNF) (some) optical/x-/gamma-rays (some) of them are extremely stable (e.g. PSR 0437-4715 @1 part in 10 15 ) -> Gravitational Waves detection astrobites
timescale (second) Highlights on pulsar :Timescales Physics 10 8 Intermittent pulsars magnetosphere 10 6 10 4 10 2 10 0 10-2 10-4 10-6 Rotating Radio Transients (RRATs) nulling, moding, drifting Pulse-to-pulse variations micro-structure 10-8 nano-structure emission physics modified from Kramer et al. 2006
13m VGOS Utility 40m TNRT
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40m TNRT Location Huai Hongkhrai Royal Development Study Center Utility 13m VGOS
KVN CVN VERA TNRT40 2019A semester (Sep 1, 2018 Jan 15, 2019) (EAVN) from EAVN web-site
UV-coverage : EAVN + TNRT40 Declination +40 Declination 29
EAVN + TNRT40 + Nanshan 26- m Declination +40 Declination 29