“infrared astronomy”的概念、定义、翻译、参考文献-科学参考

infrared astronomy

Physics

The study of radiation from space in the infrared region of the spectrum (see infrared radiation). Some infrared radiation is absorbed by water and carbon dioxide molecules in the atmosphere but there are several narrow atmospheric windows in the near-infrared (1.15–1.3 μm‎, 1.5–1.75 μm‎, 2–2.4 μm‎, 3.4–4.2 μm‎, 4.6–4.8 μm‎, 8–13 μm‎, and 16–18 μm‎). Longer-wavelength observations must be made from balloons, rockets, or satellites. Infrared sources are either thermal, i.e. emitted by the atoms or molecules of gases or dust particles in the temperature range 100–3000 K, or electronic, i.e. emitted by high-energy electrons interacting with magnetic fields as in synchrotron radiation. Detectors are either modified reflecting telescopes or solid-state photon detectors, usually incorporating photovoltaic devices.

Astronomy

The study of the Universe in the infrared part of the spectrum, at wavelengths of 1–300 μ‎m. Infrared astronomy is hampered by the Earth’s atmosphere, which is opaque and bright throughout much of the infrared band due mainly to water vapour and carbon dioxide. Another source of interference is warmth from a telescope’s surroundings, including the telescope itself, which peaks around 10 μ‎m. Ground-based infrared astronomy is restricted to the few infrared windows in the Earth’s atmosphere, especially in the near-infrared 1–5 μ‎m region, and around 10 μ‎m. Even then, infrared telescopes are placed on high, dry mountain tops. High-altitude balloons and aircraft have also been used, notably the Kuiper Airborne Observatory (KAO) and more recently the Stratospheric Observatory for Infrared Astronomy (SOFIA). But unimpeded viewing of the infrared sky requires telescopes in space, such as the Infrared Astronomical Satellite (IRAS), the Infrared Space Observatory (ISO), the Spitzer Space Telescope, and the Herschel Space Observatory.
Prominent infrared sources include red giants and supergiants with dust shells, H II regions, the galactic centre, star-forming regions, and active galaxies. Many active galaxies emit the bulk of their energy in the infrared, and the infrared luminosity of spiral galaxies has become a key element in the Tully–Fisher relation method of measuring extragalactic distances. Infrared waves can readily penetrate interstellar dust, and infrared astronomy has played an important role in the study of obscured regions such as the galactic disk and dark nebulae. Spectroscopy at infrared wavelengths is an important source of information about interstellar molecules.
The type of detector used depends on the wavelength to be detected. At near-infrared wavelengths, photovoltaic detectors (such as indium antimonide) are common, while at far-infrared wavelengths bolometers are used. Arrays of detectors are used for imaging. Infrared detectors are cooled by liquid helium (to 4 K) or liquid nitrogen (to 77 K) to reduce thermal noise.

Space Exploration

The study of infrared radiation produced by relatively cool gas and dust in space, as in the areas around forming stars. In 1983 the US–Dutch–British Infrared Astronomical Satellite (IRAS) surveyed almost the entire sky at infrared wavelengths. It found five new comets, thousands of galaxies undergoing bursts of star formation, and the possibility of planetary systems forming around several dozen stars.
Planets and gas clouds emit their light in the far- and mid-infrared regions of the spectrum. The Infrared Space Observatory (ISO), launched in 1995, observed a broad wavelength (3–200 micrometres) in these regions. The work of these pioneer observations has been extended by the Spitzer Space Telescope and, extending observations into the submillimetre range, the Herschel Space Observatory.

单词	infrared astronomy
释义	infrared astronomy Physics The study of radiation from space in the infrared region of the spectrum (see infrared radiation). Some infrared radiation is absorbed by water and carbon dioxide molecules in the atmosphere but there are several narrow atmospheric windows in the near-infrared (1.15–1.3 μm‎, 1.5–1.75 μm‎, 2–2.4 μm‎, 3.4–4.2 μm‎, 4.6–4.8 μm‎, 8–13 μm‎, and 16–18 μm‎). Longer-wavelength observations must be made from balloons, rockets, or satellites. Infrared sources are either thermal, i.e. emitted by the atoms or molecules of gases or dust particles in the temperature range 100–3000 K, or electronic, i.e. emitted by high-energy electrons interacting with magnetic fields as in synchrotron radiation. Detectors are either modified reflecting telescopes or solid-state photon detectors, usually incorporating photovoltaic devices. Astronomy The study of the Universe in the infrared part of the spectrum, at wavelengths of 1–300 μ‎m. Infrared astronomy is hampered by the Earth’s atmosphere, which is opaque and bright throughout much of the infrared band due mainly to water vapour and carbon dioxide. Another source of interference is warmth from a telescope’s surroundings, including the telescope itself, which peaks around 10 μ‎m. Ground-based infrared astronomy is restricted to the few infrared windows in the Earth’s atmosphere, especially in the near-infrared 1–5 μ‎m region, and around 10 μ‎m. Even then, infrared telescopes are placed on high, dry mountain tops. High-altitude balloons and aircraft have also been used, notably the Kuiper Airborne Observatory (KAO) and more recently the Stratospheric Observatory for Infrared Astronomy (SOFIA). But unimpeded viewing of the infrared sky requires telescopes in space, such as the Infrared Astronomical Satellite (IRAS), the Infrared Space Observatory (ISO), the Spitzer Space Telescope, and the Herschel Space Observatory. Prominent infrared sources include red giants and supergiants with dust shells, H II regions, the galactic centre, star-forming regions, and active galaxies. Many active galaxies emit the bulk of their energy in the infrared, and the infrared luminosity of spiral galaxies has become a key element in the Tully–Fisher relation method of measuring extragalactic distances. Infrared waves can readily penetrate interstellar dust, and infrared astronomy has played an important role in the study of obscured regions such as the galactic disk and dark nebulae. Spectroscopy at infrared wavelengths is an important source of information about interstellar molecules. The type of detector used depends on the wavelength to be detected. At near-infrared wavelengths, photovoltaic detectors (such as indium antimonide) are common, while at far-infrared wavelengths bolometers are used. Arrays of detectors are used for imaging. Infrared detectors are cooled by liquid helium (to 4 K) or liquid nitrogen (to 77 K) to reduce thermal noise. Space Exploration The study of infrared radiation produced by relatively cool gas and dust in space, as in the areas around forming stars. In 1983 the US–Dutch–British Infrared Astronomical Satellite (IRAS) surveyed almost the entire sky at infrared wavelengths. It found five new comets, thousands of galaxies undergoing bursts of star formation, and the possibility of planetary systems forming around several dozen stars. Planets and gas clouds emit their light in the far- and mid-infrared regions of the spectrum. The Infrared Space Observatory (ISO), launched in 1995, observed a broad wavelength (3–200 micrometres) in these regions. The work of these pioneer observations has been extended by the Spitzer Space Telescope and, extending observations into the submillimetre range, the Herschel Space Observatory.
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