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Owens Valley Solar Array

Astronomical observatories in CaliforniaBuildings and structures in Inyo County, CaliforniaOwens ValleyRadio telescopesUse American English from July 2025
OVSA2
OVSA2

The Owens Valley Solar Array (OVSA), also known as Expanded Owens Valley Solar Array (EOVSA), is an astronomical radio telescope array, located at Owens Valley Radio Observatory (OVRO), near Big Pine, California, with main interests in studying the physics of the Sun. The instruments of the observatory are designed and employed specifically for studying the activities and phenomena of our solar system's sun. Other solar dedicated instruments operated on the site include the Solar Radio Burst Locator (SRBL), the FASR Subsystem Testbed (FST), and the Korean SRBL (KSRBL). The OVSA is operated by the New Jersey Institute of Technology (NJIT), which also operates the Big Bear Solar Observatory.

Excerpt from the Wikipedia article Owens Valley Solar Array (License: CC BY-SA 3.0, Authors, Images).

Owens Valley Solar Array
Leighton Lane,

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Latitude Longitude
N 37.23389 ° E -118.28486 °
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Address

Owens Valley Radio Observatory

Leighton Lane 100
93513
California, United States
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Phone number
California Institute of Technology

call+17609382075

Website
ovro.caltech.edu

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OVSA2
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Sunyaev–Zel'dovich Array
Sunyaev–Zel'dovich Array

The Sunyaev–Zeldovich Array (SZA) in California is an array of eight 3.5 meter telescopes that was operated as part of the now-closed Combined Array for Research in Millimeter-wave Astronomy (CARMA). Its initial goals were to survey the cosmic microwave background (CMB) in order to measure its fine-scale anisotropies and to find clusters of galaxies. The survey was completed in 2007, and the array is now used primarily to characterize clusters via the Sunyaev–Zeldovich effect. Observations commenced at the SZA in April 2005. One of the most important developments of the last few years has been the detection, through observations of the CMB and supernova studies, of a form of energy that is accelerating the expansion of the universe. Dubbed dark energy by analogy with dark matter, it is believed to account for roughly 70% of the universe's energy content. While dark energy cannot be observed directly, its basic properties can be inferred from its effect on structure formation in the universe. Just as an ecologist can learn about the food supply by studying how animal populations evolve with time, physicists can learn about dark energy by studying the population statistics of the universe's inhabitants—in this case, galaxy clusters. The SZA gets its name from the means by which it measures galaxy clusters: the scattering of CMB light as it passes through the hot ionized cluster gas, known as the Sunyaev–Zeldovich effect (SZ effect). In short, the CMB is used as a backlight against which galaxy clusters can be seen by the shadows they cast. Since the SZA sees the shadow rather than the light emitted by the cluster itself, it can be used to measure sufficiently large clusters nearly independently of their redshift, back to the epoch at which clusters first began to form.