Science of the Thai National Radio Observatory National - - PowerPoint PPT Presentation

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Science of the Thai National Radio Observatory National - - PowerPoint PPT Presentation

May 02, 2023 110 likes •337 views

Progress and Early Science of the Thai National Radio Observatory National Astronomical Institute of Thailand (Public Organisation) Ministry of Science and Technology On behalf of RANGD project & Radio Astronomy Group and S. Koichiro

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SLIDE 1

Progress and Early Science of the Thai National Radio Observatory

National Astronomical Institute of Thailand (Public Organisation) Ministry of Science and Technology

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

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SLIDE 2

“Capacity Building Through Radio Astronomy”

Radio Astronomy Network and Geodesy for Development (RANGD) 2017-2021

  • Thai National Radio Observatory (TNRO)
  • 40m Thai Radio Telescope (TNRT)
  • 13m VGOS Telescope
  • Visitor Centre
  • Receiver and Electronics Laboratories

Human Expertise

  • Workshops & Seminars
  • Trainings & Staff exchange
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SLIDE 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 - 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.

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SLIDE 4

RANGD International Technical Advisory Committee

(1st Meeting; March ’18)

2nd Meeting will be ~Nov. 2018

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SLIDE 5

Timeline 2018 2019 2020

Sitework 40m TNRT Installation L-, K-band Backend SAT Science Commissioning

RANGD Phase I (2017-2018)

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SLIDE 6

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
  • bservation
  • Generates demand for R&D on

State-of-the-art technology

40 40m Ye Yebes, , Spain

40m RT Contract Signing March ‘17

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SLIDE 7

Sensitivity

L-band K-band Location Primary Focus Nasmyth Focus Frequency ra range (G (GHz) 1. 1.0-1.8 18 18.0-26.5 Centre wavelength (c (cm) 21.4 1.36 Beam wid idth (a (arcmin in) 22 1.4 Polarisation Linear Circular Cross po polarisation

  • 25 dB
  • 25 dB

RF BW 80 800 MHz 8 GHz sampler 3 Gsps >4 Gsps Packetizer BW 1.5 GHz >2 2 GHz dig igitisation bi bits < 12 bit < 12 bit Total eff fficie iency 0.7 0.5 Gain in (K (K/Jy) 0.32 0.23 Trx (K (K) 13 20 Tsky (K (K) 12 50 Tsys (K (K) 25 70 SEFD (Jy Jy) 78 78 30 304

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SLIDE 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)

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SLIDE 9

Participating in VLBI networks

e-VLBI?

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SLIDE 10

6m foundation excavation +6m piles

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SLIDE 11

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)

RANGD Phase I+II

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SLIDE 12

Time-domain Astronomy

(S. Koichiro, NAOJ)

  • 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

Key advantages Extensive observing frequency : 300 MHz - 115 GHz Ideal latitude location : +18 N

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SLIDE 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!

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SLIDE 14

ขอบคุณค่ะ

KOB KOON KA

대단히 감사합니다.

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SLIDE 15

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 1015) -> Gravitational Waves detection

astrobites

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SLIDE 16

magnetosphere emission physics

Highlights on pulsar :Timescales Physics

108 106 104 102 100 10-2 10-4 10-6 10-8 Intermittent pulsars Rotating Radio Transients (RRATs) nulling, moding, drifting Pulse-to-pulse variations micro-structure nano-structure

timescale (second)

modified from Kramer et al. 2006

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SLIDE 17

13m VGOS 40m TNRT Utility

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SLIDE 18

S

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SLIDE 19

Location

Huai Hongkhrai Royal Development Study Center

13m VGOS 40m TNRT Utility

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SLIDE 20

(EAVN)

from EAVN web-site

TNRT40

VERA KVN CVN

2019A semester (Sep 1, 2018 – Jan 15, 2019)

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SLIDE 21

UV-coverage : EAVN + TNRT40

Declination +40° Declination −29°

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SLIDE 22

EAVN + TNRT40 + Nanshan 26- m

Declination +40° Declination −29°