Mission Overview The Copernicus satellite was launched into a nearly circular 7123 km radius orbit, inclined at 35 degrees, on 21 August 1972. Select any satellite orbiting the Earth and check where is located now. To obtain the entire spectrum required 16,000 separate 14-second exposures. Satellite Fact Sheet. atmosphere. However, it also contained a cosmic X-ray experiment provided by University College London/MSSL. In the case of the Copernicus satellite, the far UV spectrograph provided access to 800 Å of the UV spectrum but the detector recorded only 0.05 Å of that spectrum at a time. The detector count rate is plotted against the ultraviolet wavelength, in Å, over the short wavelength range from 1047 to 1055 Å. were stored on an onboard tape recorder and in core storage. each side of the spacecraft at angles of 34 degrees and had an area of 38.2 square m. A Ordering Information Order Now. Two redundant VHF (136.26 MHz) transmitters were used in a narrow-band The only way to study H2 in the cold ISM is through its UV absorption. Their detectors of UV radiation were simple photomultiplier tubes that were only able to record the UV photons in a single spectral resolution element at a time. The Copernicus satellite operated until 1982 and produced a wealth of information about the physical state of the ISM and about the mass outflow from hot stars. OAO 3 (Orbiting Astronomical Observatory), also known as Copernicus, was the third in the OAO program and its second successful spacecraft to observe the celestial sphere from above the earth's atmosphere. Two redundant pairs of VHF command (OAO-3) satellite in orbit. This Princeton University project was led by Lyman Spitzer. Its name was soon changed to the Copernicus satellite. A service of the High Energy Astrophysics Science Archive Research Center (HEASARC), Dr. Alan Smale (Director), within the Astrophysics Science Division (ASD) at NASA/GSFC, National Aeronautics and Space Administration, Long-term monitoring of pulsars and other bright X-ray Spacecraft attitude General. I thereby moved from doing low-resolution UV spectroscopy with OAO-2 to very high-resolution spectroscopy with the Copernicus satellite. measurements of celestial X-ray sources and interstellar absorption between 1 and 100 A. second successful spacecraft to observe the celestial sphere from above the earth's Please make a donation to support Gunter's Space Page. The Satellite Encyclopedia. An artist's conception of the Copernicus The satellite contained a telescope with an 0.8-meter mirror followed by a very high-resolution UV spectrometer operating from 912 to 1450 Å and from 1650 to 3000 Å. A UV telescope with a spectrometer measured high-resolution spectra of stars, could control the pitch and yaw to within 0.1 arc-s on bright stars. Complete spectra were only obtained for several bright stars. was controlled by inertia wheels and thrusters. The main instrument on the Copernicus satellite, or the Orbiting Astronomical Observatory 3, was an ultraviolet telescope for cosmic observations. Cold molecular hydrogen in the interstellar gas can only be studied at UV wavelengths. OAO 3 Also called Copernicus for the 500th anniversary of Copernic. H2 has very strong absorption lines at far UV wavelengths between 912 and 1100 Å. I benefited from such a program and with Ralph Bohlin pursued a major survey of interstellar atomic and molecular hydrogen. Designation: 06153 / 72065A Launch date 21 Aug 1972 Country of origin: United States: Mission: uplink. This mission was the third in the OAO program and its second successful spacecraft to observe the celestial sphere from above the Earth's atmosphere. telemetry link primarily for transmitting spacecraft housekeeping data, although they In addition to its main ultraviolet telescope, Copernicus carried an Engineering Physics and College Internships, Beginnings of Space Astronomy at Princeton University, International Ultraviolet Spectroscopic Explorer. absorption lines. The last of the OAOs, OAO-C, was launched in 1972 becoming OAO-3. In general, the detectors on the early satellites were extremely inefficient for recording complete UV spectra. Copernicus (OAO-3) was equipped with more powerful instruments, including a reflecting telescope with a 32-inch (81-cm) mirror. The main instrument on the Copernicus satellite, or the Orbiting Although most of the observations obtained by the Copernicus satellite were analyzed and interpreted by Princeton University astronomers, NASA began to require that observations obtained with their expensive satellites be made available to astronomers not formally involved with the design and building of the satellite. Copernicus (OAO-3) Mission Overview ; Instrumentation . The main experiment was an ultraviolet telescope. The last of the OAOs, OAO-C, was launched in 1972 becoming OAO-3. Redundant tracking beacons facilitated ground tracking of the spacecraft. The various molecular hydrogen lines measure the molecule in different rotationally excited states. monitored telemetry data, issued commands, and was programmed via the command receiver The satellite contained a telescope with an 0.8-meter mirror followed by a very high-resolution UV spectrometer operating from 912 to 1450 Å and from 1650 to 3000 Å. Two UHF The main experiment on board was the Princeton University UV telescope, Its name was soon changed to the Copernicus satellite. In (400.55 MHz) transmitters provided wideband telemetry for transmitting digital data to the The Copernicus Satellite (OAO-3) Copernicus, or Orbiting Astronomical Observatory 3 (OAO-3)was a collaborative effort between the USA (NASA) and the UK (SERC). served as backups for the wideband telemetry system. Astronomical Observatory 3, was an ultraviolet telescope for cosmic In addition to studying very cold gas in the ISM, the Copernicus satellite revealed the presence of hot gas in the ISM through the presence of very strong absorption of five-times ionized oxygen (O+5), which has absorption lines at 1031.9 and 1037.6 Å. A complete spectrum took three days. Company. A boresight star sun baffle protected the experiments and increased the length of the spacecraft to 4.9 m. Data Focus Version 0.81 comes with a new web design! OAO 3 (Orbiting Astronomical Observatory), also known as Copernicus, was the third in the OAO program and its NNX09AD33G and NNX10AE80G issued through the SMD ROSES 2009 Program. binaries, Observed rapid intensity variability in Centaurus A. Spectrum originally published in Morton, D.C.. 1975, ApJ, 197, 85. Credit: Courtesy Ed Jenkins and the American Physical Society. For more information about this spectrum, see Spitzer, L., Jenkins, E. B. While the OAO program of satellites greatly advanced the field of ultraviolet space astronomy, they had significant observational limitations. Two scientific highlights of the Copernicus mission include the first comprehensive assessment of the physical state and distribution of molecular hydrogen (H2) in the ISM. For most scientific programs spectroscopic information was only obtained for very narrow spectral ranges. This Princeton University project was led by Lyman Spitzer. ground stations. Copernicus (OAO-3) High-resolution Observation of Very Strong Molecular Hydrogen Absorption in the Spectrum of the Zeta (ζ) Ophiuchi: ζ Ophiuchi is situated beyond a strongly absorbing interstellar cloud of gas and dust. Check satellite passes over your location and receive alerts on your phone. Therefore, OAO-2 and OAO-3 were limited to only observing the brightest UV-emitting stars. Tracking 20724 objects as of 4-Jun-2020 HD Live streaming from Space Station. (Credit: NASA), Country (primary): United States and United Kingdom. 2 deployable fixed solar arrays, batteries. observations. three-axis gyro inertial system), sun sensors, a magnetometer, and star trackers, which galaxies, and planets with the main emphasis on the determination of interstellar Launched Aug. 21, 1972, this satellite was primarily used to study ultraviolet emissions from interstellar gas and stars in the far reaches of the Milky Way. central tubular area, which housed the experiment container. tracker, sensitive to sixth magnitude, controlled pitch and yaw to within 5 arc-s. 1975, ARA&A, 13, 133. addition, the high-resolution telescope experiment had a fine pointing control, which In order to have further advances in UV astronomy it was necessary to develop UV area detectors with large multiplexing advantages that could operate successfully in the space environment. For example, the range from 1031 to 1033 Å was used to study the important O+5 absorption line at 1031.9 Å.

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