As its mission continues, Chandra will continue to discover startling new science about our high-energy Universe. Chandra has traced the separation of dark matter from normal matter in the collision of galaxies in a cluster and is contributing to both dark matter and dark energy studies. Chandra has observed the region around the supermassive black hole in the center of our Milky Way, and found black holes across the Universe. Depending on which detector is used, very detailed images or spectra of the cosmic source can be made and analyzed.Ĭhandra has imaged the spectacular, glowing remains of exploded stars, and taken spectra showing the dispersal of elements. The energetic X-rays strike the insides of the hollow shells and are focussed onto electronic detectors at the end of the 9.2- m (30-ft.) optical bench. X-ray telescopes cannot focus X-ray light the same way that ordinary. Similar to optical astronomy, in X-ray astronomy we call a mechanism, which collects incoming X-rays and guides them to the detector, an optical system. The Center maintains an extensive public web site about the science results and an education program.Ĭhandra carries four very sensitive mirrors nested inside each other. Telescopes that capture radio waves look nothing like optical telescopes, but the. The Smithsonian's Astrophysical Observatory in Cambridge, MA, hosts the Chandra X-ray Center which operates the satellite, processes the data, and distributes it to scientists around the world for analysis. Because X-rays are absorbed by Earth's atmosphere, Chandra must orbit above it, up to an altitude of 139,000 km (86,500 mi) in space. NASA's Chandra X-ray Observatory is a telescope specially designed to detect X-ray emission from very hot regions of the Universe such as exploded stars, clusters of galaxies, and matter around black holes. Mission for X-ray astronomy, taking its place in X-ray Observatory has been NASA's flagship Designing a telescope system to focus X-ray photons requires a radically different approach from traditional telescope systems. X-ray photons cannot be focused in this way because they have so much energy that they simply pass through the materials used in traditional telescope designs. As a result, telescopes at other wavelengths either view changes on spatial scales larger than those observed with the EHT, or have a difficulty in discerning where exactly (with respect to the black hole) the changes are happening.Since its launch on July 23, 1999, the Chandra For example, optical telescopes use refracting lenses or reflecting mirrors to focus visible light photons, which are plentiful, onto a focal plane. Other radio arrays, including global ones like the GMVA, do not operate at short enough wavelengths, while at wavelengths shorter than about a tenth of a millimeter long-distance interferometry becomes technically impossible. Resolving power scales directly with the observing wavelength and inversely with the distance between the furthest telescopes in an interferometric array such as the EHT. tic giant branch stars, X-ray binaries and active.
OPTICAL TELESCOPE AND X RAY INSTALL
Only observations with the Earth-sized EHT array at wavelength below approximately 2 mm have the theoretical resolving power sufficient to discern the very small size of the event horizons of black holes in SgrA* and M87. of India plans to install a 3.6-m modern state-of-the-art optical telescope at Devasthal near. What makes the radio observations at 1 mm wavelength different from observations in any other wavelength band is the spatial resolution. A number of optical and infrared telescopes monitored the EHT targets, as did X-ray telescopes Chandra, Swift, NuSTAR, and AstroSat, and high-energy gamma-ray observatories MAGIC, VERITAS, and HESS. In 20, coordinated observations were performed by various radio telescope arrays operating at wavelengths longer than 1 mm, such as GMVA, VLBA, KVN, HSA, EVN, RadioAstron. The aim of this is to provide multi-wavelength coverage in order to investigate potential correlations in source brightness in various bands across the electromagnetic spectrum. Scientists of the EHT and their collaborators try to organize observations with a number of different telescopes so that they coincide with observations with EHT observations. The two-mirror telescopes/cameras that have no coma, no spherical aberration and arbitrarily fast focal ratios form a two-parameter ( s, K) family of exact optical designs analytically derived earlier.
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