Ultraviolet astronomy

Caltech

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Ultraviolet astronomy is the observation of electromagnetic radiation at ultraviolet wavelengths between approximately 10 and 320 nanometres; shorter wavelengths—higher energy photons—are studied by X-ray astronomy and gamma-ray astronomy.^[1] Ultraviolet light is not visible to the human eye.^[2] Most of the light at these wavelengths is absorbed by the Earth's atmosphere, so observations at these wavelengths must be performed from the upper atmosphere or from space.^[1]

Overview

Ultraviolet line spectrum measurements (spectroscopy) are used to discern the chemical composition, densities, and temperatures of the interstellar medium, and the temperature and composition of hot young stars. UV observations can also provide essential information about the evolution of galaxies. They can be used to discern the presence of a hot white dwarf or main sequence companion in orbit around a cooler star.^[3][4]

The ultraviolet

. Most stars are actually relatively cool objects emitting much of their electromagnetic radiation in the visible or near-infrared part of the spectrum. Ultraviolet radiation is the signature of hotter objects, typically in the early and late stages of their evolution. In the Earth's sky seen in ultraviolet light, most stars would fade in prominence. Some very young massive stars and some very old stars and galaxies, growing hotter and producing higher-energy radiation near their birth or death, would be visible. Clouds of gas and dust would block the vision in many directions along the Milky Way.

Space-based solar observatories such as

for observing the Sun in ultraviolet.

The

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Pioneers in ultraviolet astronomy include George Robert Carruthers, Robert Wilson, and Charles Stuart Bowyer.

high-energy X-ray

and ultraviolet light (released 5 January 2016).

Ultraviolet space telescopes

• - Far Ultraviolet Camera/Spectrograph on Apollo 16 (April 1972)
• ESRO - TD-1A
  (135-286 nm; 1972–1974)
• - Orbiting Astronomical Observatory (#2:1968-73. #3:1972-1981)
• Orion 1 and Orion 2 Space Observatories
  (#1: 200-380 nm, 1971; #2: 200-300 nm, 1973)
• + - Astronomical Netherlands Satellite (150-330 nm, 1974–1976)
• + - International Ultraviolet Explorer (115-320 nm, 1978–1996)
• - Astron-1 (150-350 nm, 1983–1989)
• - Glazar 1 and 2 on Mir (in Kvant-1, 1987–2001)
• - FAUST (140-180 nm, in ATLAS-1 Spacelab aboard STS-45 mission, March 1992)^[5]
• - EUVE (7-76 nm, 1992–2001)
• - FUSE (90.5-119.5 nm, 1999–2007)
• + - Extreme ultraviolet Imaging Telescope (on SOHO imaging Sun at 17.1, 19.5, 28.4, and 30.4 nm)
• + - Hubble Space Telescope (various 115-800 nm,1990-1997-) (STIS 115–1030 nm, 1997–) (WFC3 200-1700 nm, 2009–)
• Swift Gamma-Ray Burst Mission
  (170–650 nm, 2004- )
• - Hopkins Ultraviolet Telescope (flew in 1990 and 1995)
• - ROSAT XUV^[6] (17-210eV) (30-6 nm, 1990–1999)
• - Far Ultraviolet Spectroscopic Explorer (90.5-119.5 nm, 1999–2007)
• - Galaxy Evolution Explorer (135–280 nm, 2003–2012)
• - Hisaki (130-530 nm, 2013 - 2023)
• - Lunar-based ultraviolet telescope (LUT) (on Chang'e 3 lunar lander, 245-340  nm, 2013 -)
• Astrosat
  (130-530 nm, 2015 -)
• - Colorado Ultraviolet Transit Experiment (CUTE) - (255-330 nm spectrograph, 2021- )
• - Public Telescope (PST)^[7] (100-180 nm, Proposed 2015, EU funded study )
• - Viewpoint-1 SpaceFab.US (200-950 nm, Launch planned 2022)^[8]

See also List of ultraviolet space telescopes

Ultraviolet instruments on planetary spacecraft

• - UVIS (Cassini) - 1997 (at Saturn from 2004 to 2017)
• - MASCS (MESSENGER) - 2004 (at Mercury from 2011 to 2015)
• - Alice (New Horizons) - 2006 (Pluto flyby in 2015)
• - UVS (Juno) - 2011 (at Jupiter since 2016)
• - IUVS (MAVEN) - 2013 (at Mars since 2014)

See also

• Markarian galaxies – Galaxy with a nucleus emitting exceptionally large amounts of ultraviolet
• Pea galaxy – Possible type of luminous blue compact galaxy

References

External links

• Media related to Ultraviolet astronomy at Wikimedia Commons