Hale Telescope

(Redirected from Hale telescope) Telescope at Palomar Observatory in California, USA For the smaller Hale Telescope at Mount Wilson, see 60-inch Hale Telescope

Hale Telescope

Alternative names	palomar
Named after	George Ellery Hale
Part of	Palomar Observatory
Location(s)	Palomar Mountain, California, US
Coordinates	33°21′23″N 116°51′54″W / 33.35628°N 116.86489°W / 33.35628; -116.86489
Altitude	1,713 m (5,620 ft)
First light	January 26, 1949, 10:06 pm PST
Discovered	Caliban, Sycorax, Jupiter LI, Alcor B
Telescope style	optical telescope reflecting telescope
Diameter	200 in (5.1 m)
Collecting area	31,000 sq in (20 m)
Focal length	16.76 m (55 ft 0 in)
Mounting	equatorial mount
Website	www.astro.caltech.edu/palomar/about/telescopes/hale.html
Location of Hale Telescope
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The Hale Telescope is a 200-inch (5.1 m), f/3.3 reflecting telescope at the Palomar Observatory in San Diego County, California, US, named after astronomer George Ellery Hale. With funding from the Rockefeller Foundation in 1928, he orchestrated the planning, design, and construction of the observatory, but with the project ending up taking 20 years he did not live to see its commissioning. The Hale was groundbreaking for its time, with double the diameter of the second-largest telescope, and pioneered many new technologies in telescope mount design and in the design and fabrication of its large aluminum coated "honeycomb" low thermal expansion Pyrex mirror. It was completed in 1949 and is still in active use.

The Hale Telescope represented the technological limit in building large optical telescopes for over 30 years. It was the largest telescope in the world from its construction in 1949 until the Soviet BTA-6 was built in 1976, and the second largest until the construction of the Keck Observatory Keck 1 in Hawaii in 1993.

History

Hale supervised the building of the telescopes at the Mount Wilson Observatory with grants from the Carnegie Institution of Washington: the 60-inch (1.5 m) telescope in 1908 and the 100-inch (2.5 m) telescope in 1917. These telescopes were very successful, leading to the rapid advance in understanding of the scale of the Universe through the 1920s, and demonstrating to visionaries like Hale the need for even larger collectors.

The chief optical designer for Hale's previous 100-inch telescope was George Willis Ritchey, who intended the new telescope to be of Ritchey–Chrétien design. Compared to the usual parabolic primary, this design would have provided sharper images over a larger usable field of view. However, Ritchey and Hale had a falling-out. With the project already late and over budget, Hale refused to adopt the new design, with its complex curvatures, and Ritchey left the project. The Mount Palomar Hale Telescope turned out to be the last world-leading telescope to have a parabolic primary mirror.

In 1928 Hale secured a grant of $6 million from the Rockefeller Foundation for "the construction of an observatory, including a 200-inch reflecting telescope" to be administered by the California Institute of Technology (Caltech), of which Hale was a founding member. In the early 1930s, Hale selected a site at 1,700 m (5,600 ft) on Palomar Mountain in San Diego County, California, US, as the best site, and less likely to be affected by the growing light pollution problem in urban centers like Los Angeles. The Corning Glass Works was assigned the task of making a 200-inch (5.1 m) primary mirror. Construction of the observatory facilities and dome started in 1936, but because of interruptions caused by World War II, the telescope was not completed until 1948 when it was dedicated. Due to slight distortions of images, corrections were made to the telescope throughout 1949. It became available for research in 1950.

Postage Stamp. The US Post Office issued a 3c postage stamp in 1948 commemorating the Hale Telescope and Observatory.

A functioning one-tenth scale model of the telescope was also made at Corning.

The 200-inch (510 cm) telescope saw first light on January 26, 1949, at 10:06 pm PST under the direction of American astronomer Edwin Powell Hubble, targeting NGC 2261, an object also known as Hubble's Variable Nebula.

The telescope continues to be used every clear night for scientific research by astronomers from Caltech and their operating partners, Cornell University, the University of California, and the Jet Propulsion Laboratory. It is equipped with modern optical and infrared array imagers, spectrographs, and an adaptive optics system. It has also used lucky cam imaging, which in combination with adaptive optics pushed the mirror close to its theoretical resolution for certain types of viewing.

One of the Corning Labs' glass test blanks for the Hale was used for the C. Donald Shane telescope's 120-inch (300 cm) primary mirror.

The collecting area of the mirror is about 31,000 square inches (20 square meters).

Components

Mounting structures

The Hale Telescope uses a special type of equatorial mount called a "horseshoe mount", a modified yoke mount that replaces the polar bearing with an open "horseshoe" structure that gives the telescope full access to the entire sky, including Polaris and stars near it. The optical tube assembly (OTA) uses a Serrurier truss, then newly invented by Mark U. Serrurier of Caltech in Pasadena in 1935, designed to flex in such a way as to keep all of the optics in alignment.

Left: The 200-inch (508 cm) Hale Telescope inside on its equatorial mount.
Right: Principle of operation of a Serrurier truss similar to that of the Hale Telescope compared to a simple truss. For clarity, only the top and bottom structural elements are shown. Red and green lines denote elements under tension and compression, respectively.

200-inch mirror

Originally, the Hale Telescope was going to use a primary mirror of fused quartz manufactured by General Electric, but instead the primary mirror was cast in 1934 at Corning Glass Works in New York state using Corning's then new material called Pyrex (borosilicate glass).

The mirror was cast in a mold with 36 raised mold blocks (similar in shape to a waffle iron). This created a honeycomb mirror that cut the amount of Pyrex needed down from over 40 short tons (36 t) to just 20 short tons (18 t), making a mirror that would cool faster in use and have multiple "mounting points" on the back to evenly distribute its weight (note – see external links 1934 article for drawings). The shape of a central hole was also part of the mold so light could pass through the finished mirror when it was used in a Cassegrain configuration (a Pyrex plug for this hole was also made to be used during the grinding and polishing process). While the glass was being poured into the mold during the first attempt to cast the 200-inch mirror, the intense heat caused several of the molding blocks to break loose and float to the top, ruining the mirror. The defective mirror was used to test the annealing process. After the mold was re-engineered, a second mirror was successfully cast.

After cooling several months, the finished mirror blank was transported by rail to Pasadena, California. Once in Pasadena the mirror was transferred from the rail flat car to a specially designed semi-trailer for road transport to where it would be polished. In the optical shop in Pasadena (now the Synchrotron building at Caltech) standard telescope mirror making techniques were used to turn the flat blank into a precise concave parabolic shape, although they had to be executed on a grand scale. A special 240 in (6.1 m) 25,000 lb (11 t) mirror cell jig was constructed which could employ five different motions when the mirror was ground and polished. Over 13 years almost 10,000 lb (4.5 t) of glass was ground and polished away, reducing the weight of the mirror to 14.5 short tons (13.2 t). The mirror was coated (and still is re-coated every 18–24 months) with a reflective aluminum surface using the same aluminum vacuum-deposition process invented in 1930 by Caltech physicist and astronomer John Strong.

The Hale's 200 in (510 cm) mirror was near the technological limit of a primary mirror made of a single rigid piece of glass. Using a monolithic mirror much larger than the 5-meter Hale or 6-meter BTA-6 is prohibitively expensive due to the cost of both the mirror, and the massive structure needed to support it. A mirror beyond that size would also sag slightly under its own weight as the telescope is rotated to different positions, changing the precision shape of the surface, which must be accurate to within 2 millionths of an inch (50 nm). Modern telescopes over 9 meters use a different mirror design to solve this problem, with either a single thin flexible mirror or a cluster of smaller segmented mirrors, whose shape is continuously adjusted by a computer-controlled active optics system using actuators built into the mirror support cell.

Dome

The moving weight of the upper dome is about 1000 US tons, and can rotate on wheels. The dome doors weigh 125 tons each. The dome is made of welded steel plates about 10 mm thick.

Observations and research

The first observation of the Hale Telescope was of NGC 2261 on January 26, 1949.

During its first 50 years, the Hale Telescope made many significant contributions to stellar evolution, cosmology, and high-energy astrophysics. Similarly, the telescope, and the technology developed for it, advanced the study of the spectra of stars, interstellar matter, AGNs, and quasars.

Quasars were first identified as high redshift sources by spectra taken with the Hale Telescope.

Halley's Comet (1P) upcoming 1986 approach to the Sun was first detected by astronomers David C. Jewitt and G. Edward Danielson on 16 October 1982 using the 200-inch Hale Telescope equipped with a CCD camera.

Two moons of the planet Uranus were discovered in September 1997, bringing the planet's total known moons to 17 at that time. One was Caliban (S/1997 U 1), which was discovered on 6 September 1997 by Brett J. Gladman, Philip D. Nicholson, Joseph A. Burns, and John J. Kavelaars using the 200-inch Hale Telescope. The other Uranian moon discovered then is Sycorax (initial designation S/1997 U 2) and was also discovered using the 200 inch Hale Telescope.

The Cornell Mid-Infrared Asteroid Spectroscopy (MIDAS) survey used the Hale Telescope with a spectrograph to study spectra from 29 asteroids.

In 2009, using a coronograph, the Hale Telescope was used to discover the star Alcor B, which is a companion to Alcor in the Big Dipper.

In 2010, a new satellite of planet Jupiter was discovered with the 200-inch Hale, called S/2010 J 1 and later named Jupiter LI.

In October 2017 the Hale Telescope was able to record the spectrum of the first recognized interstellar object, 1I/2017 U1 ("ʻOumuamua"); while no specific mineral was identified it showed the visitor had a reddish surface color.

In December 2023 the Hale Telescope began serving as the receiving antenna for the Deep Space Optical Communications experiment on NASA's Psyche mission.

Direct imaging of exoplanets

Up until the year 2010, telescopes could only directly image exoplanets under exceptional circumstances. Specifically, it is easier to obtain images when the planet is especially large (considerably larger than Jupiter), widely separated from its parent star, and hot so that it emits intense infrared radiation. However, in 2010 a team from NASA's Jet Propulsion Laboratory demonstrated that a vortex coronagraph could enable small scopes to directly image planets.

Comparison

The Hale had four times the light-collecting area of the second-largest scope when it was commissioned in 1949. Other contemporary telescopes were the Hooker Telescope at the Mount Wilson Observatory and the Otto Struve Telescope at the McDonald Observatory.

The three largest telescopes in 1949
#	Name / Observatory	Aperture	Altitude	First Light	Special advocate(s)
1	Hale Telescope Palomar Obs.	200-inch 508 cm	1713 m (5620 ft)	1949	George Ellery Hale John D. Rockefeller Edwin Hubble
2	Hooker Telescope Mount Wilson Obs.	100-inch 254 cm	1742 m (5715 ft)	1917	George Ellery Hale Andrew Carnegie
3	McDonald Obs. 82-inch McDonald Observatory (i.e. Otto Struve Telescope)	82-inch 210 cm	2070 m (6791 ft)	1939	Otto Struve

References

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