 Looking down on the top of Mount Wilson, including the historic 100"Hooker telescope (center), the 60" telescope (center left), and the CHARA array | |||||||||
| Alternative names | 672 MW | ||||||||
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| Organization | |||||||||
| Observatory code | 672 | ||||||||
| Location | Mount Wilson, California, US | ||||||||
| Coordinates | 34°13′30″N118°03′26″W / 34.22503°N 118.05719°W /34.22503; -118.05719 | ||||||||
| Altitude | 1,742 m (5,715 ft) | ||||||||
| Website | www | ||||||||
| Telescopes | |||||||||
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  Location of Mount Wilson Observatory | |||||||||
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TheMount Wilson Observatory (MWO) is anastronomical observatory inLos Angeles County, California, United States. The MWO is located onMount Wilson, a 5,710-foot (1,740-meter) peak in theSan Gabriel Mountains nearPasadena, northeast of Los Angeles.
The observatory contains two historically important telescopes: the 100-inch (2.5 m)Hooker telescope, which was the largest aperture telescope in the world from its completion in 1917 to 1949, and the60-inch telescope which was the largest operational telescope in the world when it was completed in 1908. It also contains theSnow solar telescope completed in 1905, the 60-foot (18 m) solar tower completed in 1908, the 150-foot (46 m) solar tower completed in 1912, and theCHARA array, built byGeorgia State University, which became fully operational in 2004 and was the largest optical interferometer in the world at its completion.
Due to theinversion layer that traps warm air andsmog over Los Angeles, Mount Wilson has steadier air than any other location in North America, making it ideal for astronomy and in particular forinterferometry.[1] The increasinglight pollution due to 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 the CHARA array continuing important stellar research.
The initial efforts to mount a telescope to Mount Wilson occurred in the 1880s by one of the founders ofUniversity of Southern California,Edward Falles Spence, but he died without finishing the funding effort.[2] The observatory was conceived and founded byGeorge Ellery Hale, who had previously built the 1 meter telescope at theYerkes Observatory, then the world's largest telescope. The Mount Wilson Solar Observatory was first funded by theCarnegie 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.[3]
There are threesolar telescopes at Mount Wilson Observatory. Just one of these telescopes, the 60-foot (18 m) Solar Tower, is still used for solar research.
The Snow Solar Telescope was the first telescope installed at the fledgling Mount Wilson Solar Observatory. It was the world's first permanently mounted solar telescope. Solar telescopes had previously been portable so they could be taken to solar eclipses around the world. The telescope was donated to Yerkes Observatory by Helen Snow of Chicago. George Ellery Hale, then director of Yerkes, had the telescope brought to Mount Wilson to put it into service as a proper scientific instrument. Its 24-inch (61 cm) primary mirror with a 60-foot (18 m) focal length, coupled with a spectrograph, did groundbreaking work on the spectra of sunspots, doppler shift of the rotating solar disc and daily solar images in several wavelengths. Stellar research soon followed as the brightest stars could have their spectra recorded with very long exposures on glass plates.[4] The Snow solar telescope is mostly used by undergraduate students who get hands-on training in solar physics and spectroscopy.[5]It was also used publicly for the May 9, 2016 transit of Mercury across the face of the Sun.
The 60-foot (18 m) Solar Tower soon built on the work started at the Snow telescope. At its completion in 1908, the vertical tower design of the 60-foot focal length solar telescope allowed much higher resolution of the solar image and spectrum than the Snow telescope could achieve. The higher resolution came from situating the optics higher above the ground, thereby avoiding the distortion caused by the heating of the ground by the Sun. On June 25, 1908, Hale would recordZeeman splitting in the spectrum of a sunspot, showing for the first time that magnetic fields existed somewhere besides the Earth. A later discovery was of the reversed polarity in sunspots of the new solar cycle of 1912. The success of the 60-foot Tower prompted Hale to pursue yet another, taller tower telescope. In the 1960s, Robert Leighton discovered the Sun had a 5-minute oscillation and the field of helioseismology was born.[4][6] The 60-foot Tower is operated by the Department of Physics and Astronomy atUniversity of Southern California.
The 150-foot (46 m) focal length solar tower expanded on the solar tower design with its tower-in-a-tower design. (The tower is actually 176 feet (54 m) tall.) An inner tower supports the optics above, while an outer tower, which completely surrounds the inner tower, supports the dome and floors around the optics. This design allowed complete isolation of the optics from the effect of wind swaying the tower. Two mirrors feed sunlight to a 12-inch (30 cm) lens which focuses light down at the ground floor. It was first completed in 1910, but unsatisfactory optics caused a two-year delay before a suitable doublet lens was installed. Research included solar rotation, sunspot polarities, dailysunspot drawings, and many magnetic field studies. The solar telescope would be the world's largest for 50 years until theMcMath–Pierce solar telescope was completed atKitt Peak in Arizona in 1962. In 1985, UCLA took over operation of the solar tower from the Carnegie Observatories after they decided to stop funding the observatory.[7]
For the 60-inch telescope,George Ellery Hale received the 60-inch (1.5 m) mirror blank, cast bySaint-Gobain in France, in 1896 as a gift from his father, William Hale. It was a glass disk 19 cm (7.5 in) thick and weighing 860 kg (1,900 lb). However it was not until 1904 that Hale received funding from the Carnegie Institution to build an observatory. Grinding began in 1905 and took two years. The mounting and structure for the telescope were built inSan Francisco and barely survived the1906 earthquake. Transporting the pieces to the top of Mount Wilson was an enormous task.First light was December 8, 1908. It was, at the time, the largest operational telescope in the world.[1] Lord Rosse'sLeviathan of Parsonstown, a 72-inch (1.8-meter) telescope built in 1845, was, by the 1890s, out of commission.
Although slightly smaller than the Leviathan, the 60-inch had many advantages including a far better site, a glass mirror instead of speculum metal, and a precision mount which could accurately track any direction in the sky, so the 60-inch was a major advance.
The 60-inch telescope is a reflector telescope built forNewtonian,Cassegrain andcoudé configurations. It is currently used in the bent Cassegrain configuration. It became one of the most productive and successful telescopes in astronomical history. Its design and light-gathering power allowed the pioneering ofspectroscopic analysis,parallax measurements,nebula photography, andphotometric photography.[8] Though surpassed in size by the§ 100-inch Hooker telescope nine years later, the 60-inch telescope remained one of the largest in use for decades.
In 1992, the 60-inch telescope was fitted with an earlyadaptive optics system, theAtmospheric Compensation Experiment (ACE). The 69-channel system improved the potential resolving power of the telescope from 0.5 to 1.0 arc sec to 0.07 arc sec. ACE was developed byDARPA for theStrategic Defense Initiative system, and theNational Science Foundation funded the civilian conversion.
The telescope is used for public outreach as the second largest telescope in the world devoted to the general public. Custom made 10 cm eyepieces are fitted to its focus using the bent cassegrain configuration to provide views of the Moon, planetary, and deep-sky objects. Groups may book the telescope for an evening of observing.[9]
The 100-inch (2.5 m)Hooker telescope was completed in 1917, and was theworld's largest telescope until 1949. It is one of the most famous telescopes inobservational astronomy of the 20th century. It was used byEdwin Hubble to make observations with which he produced two fundamental results which changed the scientific view of the Universe. Using observations he made in 1922–1923, Hubble wasable to prove that the Universe extends beyond the Milky Way galaxy, and that severalnebulae were millions of light-years away. He then showed that the universe wasexpanding.[10]
| Year | Description |
|---|---|
| 1923 | Edwin Hubble conclusively proves theAndromeda nebula to be external to the Milky Way galaxy |
| 1929 | Hubble andMilton Humason confirm that the Universe is expanding, measure its expansion rate, and measure the size of the known Universe |
| 1930s | Fritz Zwicky finds evidence fordark matter |
| 1938 | Seth Nickolson finds two satellites ofJupiter, referred to as#10 and#11.[11] |
| 1940s | Walter Baade's observations lead to the distinction ofstellar populations and to the discovery of two different types ofCepheid variable stars, which double the size of the known universe previously calculated by Hubble |
| 1963 | Water vapor on Mars.[12] |
Once the sixty-inch telescope project was well underway, Hale immediately set about creating a larger telescope.John D. Hooker provided crucial funding of $45,000[13] for the purchase and grinding of the mirror, whileAndrew Carnegie[14] provided funds to complete the telescope and dome. 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 Hooker telescope was completed and saw "first light" on November 2, 1917. As with the sixty-inch telescope, the bearings are assisted by the use of mercury floats to support the 100 ton weight of the telescope.
In 1919 the Hooker telescope was equipped with a special attachment, a 6-meter opticalastronomical interferometer developed byAlbert A. 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 asBetelgeuse, 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.
In 1935 the silver coating used since 1917 on the Hooker mirror was replaced with a more modern and longer lasting aluminum coating that reflected 50% more light than the older silver coating. The newer method of coating for the telescope mirrors was first tested on the older 1.5 meter mirror.[15]
Edwin Hubble performed many critical calculations from work on the Hooker telescope. In 1923, Hubble discovered the firstCepheid variable in the spiral nebula of Andromeda using the 2.5-meter telescope. This discovery allowed him to calculate the distance to the spiral nebula of Andromeda and show that it was actually agalaxy outside theMilky Way. Hubble, assisted byMilton L. Humason, observed the magnitude of theredshift in many galaxies and published a paper in 1929 that showed the universe is expanding.
The Hooker's reign of three decades as the largest telescope came to an end when theCaltech-Carnegie consortium completed its 200-inch (5.1 m)Hale Telescope atPalomar Observatory, 144 km south, inSan Diego County, California. The Hale Telescope saw first light in January 1949.[16]
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 the ever-increasing problem oflight pollution. In 1989, theCarnegie Institution, which ran the observatory, handed it over to the non-profit Mount Wilson Institute. At that time, the 2.5-meter telescope was deactivated, but it was restarted in 1992 and in 1995 it was outfitted with a visible light adaptive optics system and later in 1997, it hosted the UnISIS, laser guide star adaptive optics system.[17][18]
As the use of the telescope for scientific work diminished again, a decision was made to convert it to use for visual observing. Because of the high position of the Cassegrain focus above the observing floor, a system of mirrors and lenses was developed to allow viewing from a position at the bottom of the telescope tube. With the conversion completed in 2014, the 2.5 meter telescope began its new life as the world's largest telescope dedicated to public use. Regularly scheduled observing began with the 2015 observing season.[19]
The telescope has a resolving power of 0.05arcsecond.
Astronomical interferometry has a rich history at Mount Wilson. No fewer than seven interferometers have been located here. The reason for this is the extremely steady air over Mount Wilson is well suited to interferometry, the use of multiple viewing points to increase resolution enough to allow for the direct measurement of details such as star diameters.
The first of these interferometers was the 20-foot Stellar Interferometer. In 1919 the 100-inch Hooker telescope was equipped with a special attachment, a 20-foot optical astronomical interferometer developed by Albert A. Michelson and Francis G. Pease. It was attached to the end of the 100-inch telescope and used the telescope as a guiding platform to maintain alignment with the stars being studied. By December 1920, Michelson and Pease were able to use the equipment to determine the precise diameter of a star, the red giant Betelgeuse, the first time the angular size of a star had ever been measured. In the next year, Michelson and Pease measured the diameters of six more red giants before reaching the resolution limit of the 20-foot beam interferometer.[20]
To expand on the work of the 20-foot interferometer, Pease, Michelson and George E. Hale designed a 50-foot interferometer which was installed at Mount Wilson Observatory in 1929. It successfully measured the diameter of Betelgeuse, but, other than beta Andromedae, could not measure any stars not already measured by the 20-foot interferometer.[21]
Optical interferometry reached the limit of the available technology and it took about thirty years for faster computing, electronic detectors and lasers to make larger interferometers possible again.
TheInfrared Spatial Interferometer (ISI), run by an arm of theUniversity of California, Berkeley, is an array of three 1.65 meter 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 meters apart, giving the resolution of a telescope of that diameter. The signals are converted to radio frequencies throughheterodyne circuits and then combined electronically using techniques copied fromradio astronomy.[22] The longest, 70-meter baseline provides a resolution of 0.003 arcsec at a wavelength of 11 micrometers. On July 9, 2003, ISI recorded the firstclosure phaseaperture synthesis measurements in the mid infrared.[23]
TheCenter for High Angular Resolution Astronomy (CHARA), built and operated byGeorgia State University, is an interferometer formed from six 1 meter telescopes arranged along three axes with a maximum separation of 330 m. The light beams travel through vacuum pipes and are delayed and combined optically, requiring a building 100 meters long with movable mirrors on carts to keep the light in phase as the Earth rotates. CHARA began scientific use in 2002 and "routine operations" in early 2004. In the infrared, the integrated image can resolve down to 0.0005 arcseconds. Six telescopes are in regular use for scientific observations and as of late 2005 imaging results are routinely acquired. The array captured the first image of the surface of amain sequence star other than the Sun published in early 2007.[24]
A 61 cm telescope fitted with an infrared detector purchased from a military contractor was used byEric Becklin in 1966 to determine the center of theMilky Way for the first time.[25]
In 1968, the first large-area near-IR (2.2 μm) survey of the sky was conducted byGerry Neugebauer andRobert B. Leighton using a 157 cm reflecting dish they had built in the early 1960s.[26] Known as theCaltech Infrared Telescope, it operated in an unguideddrift scanning mode using alead(II) sulfide (PbS)photomultiplier read out on paper charts.[27] The telescope is now on display at theUdvar-Hazy Center, part of theSmithsonian Air and Space Museum.[27]
On one Sunday each month during the warmer months of the year, Mt. Wilson Observatory hosts a chamber music or jazz concert in the dome.[36] The idea to use the dome as a venue for live music originated in 2017 from a conversation between Dan Kohne, a board member of the Mt. Wilson Institute, and Cécilia Tsan, an internationally recognized cellist.[37] Tsan agreed that the acoustics in the dome were "extraordinary", comparable to such world-renowned venues as thePalais Garnier (Opéra de Paris) and theCoolidge Auditorium at the Library of Congress.[38] Kohne and Tsan worked together to create the series, which has run every concert season except for a break during theCOVID-19 pandemic. Given that the observatory is no longer able to do significant research due to light pollution, it receives no scientific funding; the concerts therefore provide a significant portion of the budget needed to maintain the observatory as an historic landmark, along with ticketed events such as public viewing nights.[39]
The observatory was the primary setting of "Nothing Behind the Door", the first episode of the radio seriesQuiet, Please which originally aired June 8, 1947.
The observatory was a filming location in a space-themed episode ofCheck It Out! with Dr. Steve Brule.
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