Ooty Radio Telescope

Ooty Radio Telescope

Radio Telescope at Ooty
Organisation Tata Institute of Fundamental Research
Location(s) Muthorai, near Ooty, Tamil Nadu, India
Coordinates 11°23′00″N 76°39′58″E / 11.383404°N 76.66616°E / 11.383404; 76.66616Coordinates: 11°23′00″N 76°39′58″E / 11.383404°N 76.66616°E / 11.383404; 76.66616
Altitude 2240 m
Weather 70% clear days
Wavelength 0.92 m[1]
Built 1970
Telescope style Cylindrical Paraboloid
Angular resolution 2.3deg x 5.5sec(dec)'[2]
Collecting area 16000 m2[2]
Mounting Equatorial
Website Official Website

The Ooty Radio Telescope is located in Muthorai near Ootacamund (Ooty), south India.[3] It is part of the National Centre for Radio Astrophysics (NCRA)[4][5][6] of the well known Tata Institute of Fundamental Research (TIFR) which is funded by the Government of India through the Department of atomic energy.[1] The Ooty Radio Telescope (ORT) is a 530-metre (1,740 ft) long and 30-metre (98 ft) wide Cylindrical Paraboloid telescope.[4][7][8] It operates at a frequency of 326.5 MHz with a maximum bandwidth of 15 MHz at the front-end.[9]

Design

The Ooty Radio telescope has been designed and fabricated with domestic Indian technological resources. The ORT was completed in 1970[10] and continues to be one of the most sensitive radio telescopes in the world.

Observations made using this telescope have led to important discoveries and to explain various phenomena occurring in our solar system and in other celestial bodies.[11]

The reflecting surface of the telescope is made of 1100 thin stainless-steel wires running parallel to each other for the entire length of the cylinder and supported on 24 steerable parabolic frames.

An array of 1056 half-wave dipoles in front of a 90 degrees corner reflector forms the primary feed of the telescope.[9][12][13]

History

The structure of a radio telescope was designed in July 1963. Muthorai village near Ooty was selected as the suitable location and the construction work began in 1965. The telescope was completed in 1969.[14] Normal post commissioning and calibration use began in 1971.

Features

The large size of the telescope makes it highly sensitive. As an example, it is in principle capable of detecting signals from a mere 1 watt radio station located 10 million km away in space.[11] The telescope sits on a natural slope of 11°, which matches the latitude of the location. This gives the telescope an equatorial mount which allows tracking of celestial sources for up to ten hours in the east-west direction.[15] In the north-south direction, the telescope operates as a phased-array and is steerable by varying the phase gradients[12][16]

The telescope can be operated in either total power or correlation mode. In each mode, 12 beams are formed and Beam 1 is the southern most beam and Beam 12 is the northern most. These 12-beam systems are useful in sky-survey type of observations. Recently, the reflecting surface of the ORT has been refurbished. A new digital back-end has been built for the ORT by the colleagues at Raman Research Institute (RRI), Bangalore.[11]

Observations

The ORT has produced results on radio galaxies, quasars, supernovae and pulsars,[17][18] One long-term program determined the angular structure of several hundred distant radio galaxies and quasars using the lunar occultation method.

The application of this database to observational cosmology provided independent evidence against the Steady State theory and supported the Big Bang model of the universe.

The telescope is currently being used mainly to observe interplanetary scintillation, which may provide valuable information about the solar wind and magnetic storms that affect the near - earth environment.[9] Interplanetary scintillation observations provide a database to understand space weather changes and their predictability.[1]

Backends

Analog Correlator

This is widely used for IPS observations .

Upgrade

The upgraded telescope has been used for observing pulse nulling.[19] The interferometer can be used at Channel 37 (608 MHz to 614 MHz, important radio astronomy frequencies) with lesser performance.

Ongoing Projects

See also

References

  1. 1 2 3 "Ooty Radio Telescope". Ooty.com. Retrieved 2011-02-04.
  2. 1 2 "ORT Specifications". Ncra.tifr.res.in. Retrieved 2011-02-04.
  3. ↑ "THE OOTY RADIO TELESCOPE". nilgiris.tn.gov.in. Retrieved 2011-02-04.
  4. 1 2 "National Centre for Radio Astrophysics". Indianspacestation.com. Retrieved 2011-02-04.
  5. ↑ "National Centre for Radio Astrophysics". Puneeducation.net. Retrieved 2011-02-04.
  6. ↑ "Science Exhibition On Feb 28, 29 At Khodad In Junnar Taluka, Approximately 80 Km North Of Pune". Punescoop.com. Retrieved 2011-02-04.
  7. ↑ "Cylindrical Palaboloyds telescopes". web listing. Buzzle.com. Retrieved 2011-02-04.
  8. ↑ "The Ooty Synthesis Radio Telescope: First Results". Citeseerx.ist.psu.edu. Retrieved 2011-02-04.
  9. 1 2 3 "Callisto spectrum measurements in Ootacamund-1.1. Station description" (PDF). E-collection.ethbib.ethz.ch. Retrieved 2011-02-04.
  10. ↑ "Ooty Radio Telescope". Mapsofindia.com. Retrieved 2011-02-04.
  11. 1 2 3 4 "Ooty Radio Telescope". Rac.ncra.tifr.res.in. Retrieved 2011-02-04.
  12. 1 2 3 "Ooty Radio Telescope (ORT)". Ncra.tifr.res.in. Retrieved 2011-02-04.
  13. ↑ "IndianPost-RADIO TELESCOPE OOTY". Indianpost.com. Retrieved 2011-02-04.
  14. ↑ "Radio Astronomy Centre - Radio Astronomy Centre, Ooty". saasems.com. Retrieved 2011-02-04.
  15. ↑ "Information and Announcements - The National Centre for Radio Astrophysics (NCRA)" (PDF). Ias.ac.in. Retrieved 2011-02-04.
  16. ↑ Kapahi, V. K (2007). "The National Centre for Radio Astrophysics(NCRA)Resonance". Resonance. 3 (9): 90–92. doi:10.1007/BF02836088.
  17. ↑ "A digital signal pre processor for pulsar search using Ooty radio telescope" (PDF). Dspace.rri.res.in. Retrieved 2011-02-04.
  18. ↑ "Study of the LISM using Pulsar Scintillation - 2 Observations and Data Analysis" (PDF). Cdsweb.cern.ch. Retrieved 2011-02-04.
  19. ↑ Vivekanand, M. (June 1995). "Observation of nulling in radio pulsars with the Ooty Radio Telescope". Monthly Notices of the Royal Astronomical Society. 274 (3). Bibcode:1995MNRAS.274..785V. doi:10.1093/mnras/274.3.785.
  20. ↑ "Geo-effectiveness of CMEs". Britannica.com. Retrieved 2011-02-04.
  21. ↑ Ajaysinh, K; Iyer, K. N; Vats, Hari Om; Manoharan, P. K (2007). "Geo-effectiveness of CMEs". Journal of Astrophysics and Astronomy. 29: 287–291. Bibcode:2008JApA...29..287J. doi:10.1007/s12036-008-0038-6.
  22. ↑ "Toyokawa IPS Workshop 2007-Ooty IPS Studies and IPS Network" (PDF). Smei.ucsd.edu. Retrieved 2011-02-04.
  23. ↑ "Historical perspective and research centres in India in the fields of solar astronomy and Sun-Earth relationship - National Centre for Radio Astrophysics (NCRA/TIFR)" (PDF). Cdaw.gsfc.nasa.gov. Retrieved 2011-02-04.

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