Chandra X-ray Observatory, NASA/CXC/SAOU.S. satellite, one of the National Aeronautics and Space Administration (NASA) fleet of “Great Observatories” satellites, which is designed to make high-resolution images of celestial X-ray sources. In operation since 1999, it is named in honour of Subrahmanyan Chandrasekhar, a pioneer of the field of stellar evolution.
Chandra was preceded by two X-ray satellites, the U.S. Einstein Observatory (1978–81) and the multinational Röntgensatellit (1990–99), which produced surveys across the entire sky of sources emitting at X-ray wavelengths. Chandra (originally known as the Advanced X-Ray Astrophysics Facility) was designed to study individual sources in detail. Following deployment by the space shuttle Columbia on July 23, 1999, a solid-rocket stage boosted the observatory into a highly elliptical orbit with an apogee, or farthest position from Earth, of 140,000 km (87,000 miles) and a perigee, or closest position to Earth, of 10,000 km (6,200 miles) in order to remain above the worst interference by Earth’s radiation and to provide long periods of uninterrupted study of almost any part of the sky.
In effect, Chandra is to X-ray astronomy what the Hubble Space Telescope is to optical astronomy. It focuses X-rays by using four pairs of nested iridium mirrors, with an aperture of 1.2 metres (4 feet) and a focal length of 10 metres (33 feet), and is capable of unprecedented spatial resolution. A transmission grating can be inserted into the optical path before the camera to create a high-resolution spectrum in the energy range of 0.07–10 keV (kiloelectron volts, or thousand electron volts) to investigate the characteristics of sources in this range and measure the temperatures, densities, and composition of the glowing plasma clouds that pervade space.
X-ray: NASA/CXC/CfA/M.Markevitch Optical: NASA/STScI; Magellan/U.Arizona/D.Clowe Lensing Map: NASA/STScI; ESO WFI; Magellan/U.Arizona/D.CloweAs a “high-energy” facility, Chandra has as its primary focus black holes, supernova remnants, starburst galaxies, and the panoply of exotic objects at the farthest reaches of the universe. Much of a starburst galaxy’s luminosity is produced outside of the core region, and Chandra found that these galaxies have a proportionally higher number of intermediate-size black holes that sink to the centre, where they merge with each other. In following up on the Hubble Space Telescope’s “deep field” study of the earliest period of galaxy formation, Chandra found evidence that giant black holes were much more active in the past than now, so that after an initial period of extreme activity they appear to grow quiescent. (Supermassive black holes in the cores of galaxies are believed to have been responsible for the quasar phase of a galaxy’s life.) By detecting emissions from infalling material, Chandra confirmed that there is a quiescent supermassive black hole at the centre of the Milky Way Galaxy. In addition, Chandra found direct proof of the existence of dark matter in the merging of two galaxy clusters in which the hot gas (which is ordinary visible matter) was slowed by the drag effect of one cluster passing through the other, whereas the mass was not, which showed that most of the mass is dark matter. Observations of four other galaxy clusters showed that dark energy, the dominant component of the universe, has not changed greatly over time, suggesting that the universe’s expansion might continue indefinitely.
Chandra was later complemented in December 1999 by Europe’s X-ray Multi-Mirror Mission (XMM-Newton, named for Sir Isaac Newton), which carries a cluster of coaligned X-ray telescopes, and in July 2005 by the joint U.S.-Japanese Suzaku satellite, which carries five X-ray telescopes. These later facilities have larger mirrors and are sensitive to higher energies, but, because there is an inherent trade-off in mirror design, their larger light-collecting area has been secured at the expense of higher-resolution imaging.