Observatory. On behalf of RANGD project & Radio Astronomy Group and S. Koichiro (NAOJ)
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1 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
2 Radio Astronomy Network and Geodesy for Development (RANGD) 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
3 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 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.
4 RANGD International Technical Advisory Committee (1st Meeting; March 18) 2 nd Meeting will be ~Nov. 2018
5 RANGD Phase I ( ) Timeline Sitework 40m TNRT Installation L-, K-band Backend SAT Science Commissioning
6 40m Thai National Radio Telescope `Updated version of IGN s 40m Yebes Radio Telescope 40m Paraboloid Antenna, Cassegrain-Nasmyth optics 300 MHz 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
7 Sensitivity L-band K-band Location Primary Focus Nasmyth Focus Frequency range (GHz) Centre wavelength (cm) Beam width (arcmin) 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 Gain (K/Jy) Trx (K) Tsky (K) Tsys (K) SEFD (Jy)
8 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)
9 Participating in VLBI networks e-vlbi?
10 6m foundation excavation +6m piles
11 RANGD Phase I+II Timeline Sitework 40m TNRT Installation L-, K-band Backend SAT Science Commissioning C-band Rx (TBC) Q+W Rx (TBC) 13m VGOS (SHAO)
12 Time-domain Astronomy (S. Koichiro, NAOJ) Key advantages Extensive observing frequency : 300 MHz 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
13 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!
14 ขอบค ณค ะ KOB KOON KA 대단히감사합니다.
15 Highlights on pulsar ligo.org Fast rotating neutron stars Unique properties mass (canonical) ~ 1.4 solar masses radius (canonical) ~ 10 km rotational period ~ 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 part in ) -> Gravitational Waves detection astrobites
16 timescale (second) Highlights on pulsar :Timescales Physics 10 8 Intermittent pulsars magnetosphere 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
17 13m VGOS Utility 40m TNRT
18 S
19 40m TNRT Location Huai Hongkhrai Royal Development Study Center Utility 13m VGOS
20 KVN CVN VERA TNRT A semester (Sep 1, 2018 Jan 15, 2019) (EAVN) from EAVN web-site
21 UV-coverage : EAVN + TNRT40 Declination +40 Declination 29
22 EAVN + TNRT40 + Nanshan 26- m Declination +40 Declination 29
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