The Mount Wilson Observatory (MWO) is an astronomical observatory in Los Angeles County, California. The MWO is located on Mount Wilson, a 5,715 foot (1,742 m) peak in the San Gabriel Mountains near Pasadena, northeast of Los Angeles.
Thanks to the inversion layer that traps smog over Los Angeles, Mount Wilson has naturally steadier air than any other location in North America, making it ideal for astronomy and in particular for interferometry. The growth of greater Los Angeles has limited the ability of the observatory to engage in deep space astronomy, but it remains a productive center with many new and old instruments in use for science.
It was first directed by George Ellery Hale, who had built the 40 inch (1 m) telescope at the Yerkes Observatory. The Mount Wilson Solar Observatory was first funded by the Carnegie Institution of Washington in 1904, leasing the land from the owners of the Mount Wilson Hotel in 1904. Among the conditions of the lease was that it allow public access.
The 60 inch (1.5 m) reflector became one of the most productive and successful telescopes in astronomical history. Its design and light-gathering power allowed the pioneering of spectroscopic analysis, parallax measurements, nebula photography, and photometric photography. Though surpassed in size by the Hooker telescope nine years later, the Hale telescope remained one of the largest in use for decades.
In 1992 the telescope was fitted with an early adaptive optics system, the Atmospheric Compensation Experiment (ACE). The 69-channel system improved the potential resolving power of the telescope from 0.5-1.0 arc sec to 0.07 arc sec. ACE was developed by DARPA for the Strategic Defense Initiative system, and the National Science Foundation funded the civilian conversion.
Today the telescope is used for public outreach. Eyepieces are fitted to its focus instead of instruments. It is one of the largest telescopes in the world which the general public can look through freely.
Another telescope, the telescope at the Palomar Observatory, is also called the "Hale Telescope".
Hale immediately set about creating a larger telescope. John D. Hooker provided crucial funding for it, along with Carnegie. The Saint-Gobain factory was again chosen to cast a blank in 1906, which it completed in 1908, After considerable trouble over the blank (and potential replacements), the 100 inch (2.5 m) telescope was completed and saw "first light" on November 2, 1917.
The mechanism incorporates a mercury float to provide smooth operation. The Hooker telescope was equipped in 1919 with a special attachment, an optical astronomical interferometer developed by Albert Michelson, much larger than the one he had used to measure Jupiter's satellites. Michelson was able to use the equipment to determine the precise diameter of stars, such as Betelgeuse, the first time the size of a star had ever been measured. Henry Norris Russell developed his star classification system based on observations using the Hooker.
Edwin Hubble performed his critical calculations from work on the 100 inch (2.5 m) telescope. He determined that some nebulae were actually galaxies outside our own Milky Way. Hubble, assisted by Milton L. Humason, discovered the presence of the redshift that indicated the universe is expanding.
The Hooker's long reign as the largest telescope came to an end when the Caltech-Carnegie consortium completed its 200 inch (5 m) telescope in 1948 at Mount Palomar, 90 miles (150 km) south, in San Diego County, California.
By the 1980s, the focus of astronomy research had turned to deep space observation, which required darker skies than what could be found in the Los Angeles area, due to ever-increasing problem of light pollution. In 1986, the Carnegie Institution, which ran the observatory, handed it over to the non-profit Mount Wilson Institute. At that time, the 100 inch (2.5 m) telescope was deactivated, but it was restarted in 1992 and outfitted with adaptive optics. The Hooker telescope remains one of the pre-eminent scientific instruments of the 20th century.
The telescope has a resolving power of 0.05 arcsec.
The Infrared Spatial Interferometer (ISI) is an array of three 65 inch (1.65 m) telescopes operating in the mid-infrared. The telescopes are fully mobile and their current site on Mount Wilson allows for placements as far as 70 m apart, giving the resolution of a telescope of that diameter. The signals are converted to radio frequencies through heterodyne circuits and then combined electronically using techniques copied from radio astronomy. ISI is run by an arm of the University of California, Berkeley. The longest (70m) baseline provides a resolution of 0.003 arcsec at 11 micrometers. On July 9, 2003, ISI recorded the first closure phase aperture synthesis measurements in the mid infrared.
The Center for High Angular Resolution Astronomy (CHARA) array is an interferometer formed from six 1 m (40-inch) telescopes arranged along three axes with a maximum separation length of 330 m. The light beams travel through vacuum tubes and are combined optically, requiring a building 100 meters long with movable mirrors to keep the light in phase as the earth rotates. CHARA is operated by the Georgia State University and began scientific use in 2002 and began "routine operations" in early 2004. In infrared the integrated image can resolve down to 0.0005 arcseconds. As of 2005 four of the six telescopes have been commissioned for interferometric observations.
These and other astronomical interferometers are included in the List of astronomical interferometers at visible and infrared wavelengths. The history of the development of these instruments is given in History of astronomical interferometry.
In 1968, the first large-area near-IR (2.2 µm) survey of the sky was conducted by Gerry Neugebauer and Robert B. Leighton using a reflecting dish they had built. The instrument is now in the Smithsonian.
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