Owens Valley Radio Observatory

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Owens Valley Radio Observatory
Owens Valley Radio Observatory.JPG
Alternative names OVRO Edit this on Wikidata
Organization California Institute of Technology Edit this on Wikidata
Location Owens Valley, California, US
Coordinates 37°14′02″N 118°16′55″W / 37.2339°N 118.282°W / 37.2339; -118.282Coordinates: 37°14′02″N 118°16′55″W / 37.2339°N 118.282°W / 37.2339; -118.282
Altitude 1,222 m (4,009 ft) Edit this at Wikidata
Established 1958 Edit this on Wikidata
Website www.ovro.caltech.edu Edit this at Wikidata
Telescopes C-BASS North
OVRO VLBA station
Combined Array for Research in Millimeter-wave Astronomy
Frequency-Agile Solar Radiotelescope
OVRO 40 meter Telescope
Owens Valley Solar Array
Sunyaev–Zel'dovich Array Edit this on Wikidata
Owens Valley Radio Observatory is located in the US
Owens Valley Radio Observatory
Location of Owens Valley Radio Observatory
Commons page Related media on Wikimedia Commons

Owens Valley Radio Observatory (OVRO) is a radio astronomy observatory located near Big Pine, California (US) in Owens Valley. It lies east of the Sierra Nevada approximately 350 kilometers (220 mi) north of Los Angeles and 20 kilometers (12 mi) southeast of Bishop. It was established in 1958, and is owned and operated by the California Institute of Technology (Caltech).

One of the ten dish-antenna radiotelescope systems of the Very Long Baseline Array is immediately adjacent to, but not part of, the Owens Valley observatory.


The Owens Valley Radio Observatory (OVRO), the largest university-operated radio observatory in the United States, came to life in the late 1940s through the influence of three individuals: Lee DuBridge, president of Caltech; Robert Bacher, chairman of the Division of Physics, Mathematics and Astronomy; and Jesse Greenstein, professor of astrophysics. In 1954, Caltech occupied a central position in the American radio astronomy program. John Bolton and Gordon Stanley, two respected Australian astronomers, joined the Caltech faculty in order to undertake the construction of large dishes. In 1956 the first radio telescope, a 32-foot antenna, was erected on Palomar Mountain. It was dismantled in 1958 and transferred to the Owens Valley site. At the same time, two 90-foot (27-meter) telescopes were completed. Ten years later, an even bigger antenna, a 130-foot (40-meter) dish was finished. It was originally built to study radio galaxies but is now used to look at the sun's magnetic field. The last major instrument at the observatory is the millimeter-wave array. It consists of six 34-foot (10.4-meter) dishes (also called Leighton's dishes).

OVRO, owned by Caltech, is one of the biggest radio observatories owned by a university.[1] OVRO uses its telescopes and other instruments (listed below) to improve on the locations of radio sources in the sky, as well as to study hydrogen clouds within the Milky Way.[1] The research that takes place at the observatory includes studies on blazars, the cosmic microwave background, and star-formation, and this research is done by the staff at the observatory with help from professors and post-doctoral students from many institutions. The observatory is different from other national radio observatories because of its extensive work with graduate students, who can come to the observatory for long-term observation, benefitting not only the students, but also the observatory as it allows for more comprehensive projects to take place[1]


OVRO staff was largely responsible for operating CARMA, which was located 20 miles east of OVRO in the Inyo Mountains, but is currently in storage at the OVRO site. CARMA is a collaboration between Caltech, University of California Berkeley, University of Illinois, University of Maryland, and University of Chicago to observe space at centimeter and millimeter wavelengths with a 23-element interferometer. CARMA used this interferometer to study the origins of planets, stars and galaxies, as well as to measure the distortions in the cosmic microwave background caused by clusters of galaxies formed soon after the Big Bang.[1]


Former instruments[edit]

  • The Huan Tran Telescope (HTT) is the primary instrument of the Polarbear project to measure the polarization of the cosmic microwave background radiation. It is a 3.5 m (11 ft) Gregorian telescope with bolometers cooled to less than 1 K (−458 °F). HHT was first installed for testing at the CARMA site in 2010. It was moved to Llano de Chajnantor Observatory in 2011 and is expected to start operating in early 2012. It was developed by a consortium led by the University of California, Berkeley.[8]
  • The Owens Valley Solar Array (OVSA) was a seven-dish solar radio telescope array located at the main OVRO site until 2008. It was built by Caltech and was operated by the New Jersey Institute of Technology (NJIT) from 1997. It consisted of two 27.5 m (90 ft) antennas and five 1.8 m (5.9 ft) antennas. The OVSA antennas are being incorporated into EOVSA in a different configuration.[9]
  • The FASR Subsystem Testbed (FST) was an interferometer which used three of the 1.8 m antennas from OVSA, but upgraded with a different electronics package. It operated from 2006 until 2008.[10]
  • The Millimeter Array (MMA) was a six-element radio telescope array located at the main OVRO site until 2005, when the dishes were moved to Cedar Flat and incorporated into CARMA.[2]
  • The Solar Radio Burst Locator (SRBL) was a 1.8 m (5.9 ft) radio telescope that operated at OVRO from 1998 until 2006. It identified radio bursts from the Sun using a single dish.[11]

Future Instruments[edit]

  • The Evolved Owens Valley Solar Array (EOVSA) is a solar radio telescope array currently under construction at OVRO. It will incorporate seven refurbished dishes from OVSA, along with eight new 2 m (6.6 ft) antennas. The small dishes will be arranged in a spiral pattern instead of the typical three-arm pattern.[12]
  • The Frequency-Agile Solar Radiotelescope (FASR) is a proposed solar radio telescope array that will incorporate 75 elements.[13]
  • The Ku-Band Experiment (KuBE) is a proposed 6 m (20 ft) radio telescope with the same objective as C-BASS, but would operate in the Ku-band.[14]

In popular culture[edit]

In the film The Arrival (1996), Zane Zaminsky (Charlie Sheen) and Calvin (Richard Schiff) work at Owens Valley for the SETI Project and discover an alien signal. (It's actually called the "Oro Valley Radio Observatory" in the movie. There is an Oro Valley in Arizona.)

In the film Contact (1997), the Owens Valley 40-meter telescope is mentioned as the location where Dr. Eleanor Arroway (Jodie Foster) did her thesis work.

See also[edit]


  1. ^ a b c d "The Owens Valley Radio Observatory". Retrieved 2012-04-14. 
  2. ^ a b "CARMA | Frequently Asked Questions". Combined Array for Research in Millimeter-wave Astronomy. Retrieved 2012-01-13. 
  3. ^ "OVRO 40m Telescope". Caltech Astronomy. Retrieved 2012-01-13. 
  4. ^ "C-BASS: C-Band All Sky Survey". Caltech Astronomy. Retrieved 2012-01-13. 
  5. ^ King, Oliver G.; Copley, Charles; Davies, Rod; Davis, Richard; Dickinson, Clive; Hafez, Yaser A.; Holler, Christian; John, Jaya John; Jonas, Justin L.; Jones, Michael E.; Leahy, J. Patrick; Muchovej, Stephen J. C.; Pearson, Timothy J.; Readhead, Anthony C. S.; Stevenson, Matthew A.; Taylor, Angela C. (2010). "The C-Band All-Sky Survey: Instrument design, status, and first-look data". Proceedings of SPIE. 7741: 77411I. arXiv:1008.4082Freely accessible. doi:10.1117/12.858011.  |chapter= ignored (help)
  6. ^ Dou, Yujiang; Gary, Dale E.; Liu, Zhiwei; Nita, Gelu M.; Bong, Su-Chan; Cho, Kyung-Suk; Park, Young-Deuk; Moon, Yong-Jae (2009). "The Korean Solar Radio Burst Locator (KSRBL)". Publications of the Astronomical Society of the Pacific. 121 (879): 512. Bibcode:2009PASP..121..512D. doi:10.1086/599624. 
  7. ^ "Powerful New Radio Telescope Array Searches the Entire Sky 24/7". Caltech Astronomy. Retrieved 2015-05-12. 
  8. ^ Keating, B.; Moyerman, S.; Boettger, D.; Edwards, J.; Fuller, G.; Matsuda, F.; Miller, N.; Paar, H.; Rebeiz, G.; et al. (2011). "Ultra High Energy Cosmology with POLARBEAR". 1110: 2101. arXiv:1110.2101Freely accessible. Bibcode:2011arXiv1110.2101K. 
  9. ^ "Legacy Owens Valley Solar Array". New Jersey Institute of Technology Department of Physics. Retrieved 2012-01-13. 
  10. ^ Liu, Zhiwei; Gary, Dale E.; Nita, Gelu M.; White, Stephen M.; Hurford, Gordon J. (2007). "A Subsystem Test Bed for the Frequency‐Agile Solar Radiotelescope". Publications of the Astronomical Society of the Pacific. 119 (853): 303. Bibcode:2007PASP..119..303L. doi:10.1086/512825. 
  11. ^ Hwangbo, J.-E.; Bong, Su-Chan; Cho, K.-S.; Moon, Y.-J.; Lee, D.-Y.; Park, Y. D.; Gary, Dale E.; Dougherty, Brian L. (2005). "An Evaluation of the Solar Radio Burst Locator (SRBL) at OVRO". Journal of the Korean Astronomical Society. 38: 437. Bibcode:2005JKAS...38..437H. doi:10.5303/jkas.2005.38.4.437. 
  12. ^ "OVSA Expansion Project". New Jersey Institute of Technology Department of Physics. Retrieved 2012-01-13. 
  13. ^ "FASR Fact Sheet". Frequency Agile Solar Radiotelescope. Retrieved 2012-01-13. 
  14. ^ "The Owens Valley Radio Observatory". Caltech Astronomy. Retrieved 2012-01-13.