Hydrogen Intensity and Real-time Analysis eXperiment (HIRAX) In progress – currently nineteen 14 m reflectors with crossed dipole antennas as feed. Hydrogen Epoch of Reionization Array (HERA) Hartebeesthoek Radio Astronomy Observatory, Johannesburg, South Africaġ5 m Experimental Demonstrator Model originally build as a technology demonstrator for MeerKAT The first radio telescope was invented in 1932, when Karl Jansky at Bell Telephone Laboratories observed radiation coming from the Milky Way.ģ2-metre (104 foot) single dish, first of African VLBI Network ħ.6-metre (24.9 foot) dish with polarimeter back end The list is sorted by region, then by name unnamed telescopes are in reverse size order at the end of the list. The list includes both single dishes and interferometric arrays. This is a list of radio telescopes – over one hundred – that are or have been used for radio astronomy. MPE contributes the MOS-unit handling the slit masks.West arm of the low-frequency Ukrainian T-shaped Radio telescope, second modification (UTR-2) radio telescope phased array antenna LUCI is built by a German consortium led by the Landessternwarte in Heidelberg. Like all infrared instruments, LUCI is operated at cryogenic temperatures, and is therefore enclosed in a cryostat of 1.6 m diameter and 1.6 m height, and cooled down to about -200 C by two closed cycle coolers. Three camera optics with numerical apertures of 1.8, 3.75 and 30 provide image scales of 0.25, 0.12, and 0.015 arcsec/detector element for wide field, seeing-limited and diffraction-limited observations. A fixed collimator produces an image of the entrance aperture in which either a mirror (for imaging) or a grating can be positioned. In its focal plane area, long-slit and multi-slit masks can be installed for single- and multi-object spectroscopy. LUCI operates in the 0.9 - 2.5 µm spectral range using a 2048 x 2048 element Hawaii II detector array from Rockwell and provides imaging and spectroscopic capabilities in seeing- and diffraction limited modes. The name of the instrument was officially changed to LUCI in 2012. LUCIFER ( LBT Near Infrared Spectroscopic Utility with Camera and Integral Field Unit for Extragalactic Research) is the near-infrared instrument for the LBT. The pink area indicates the location of the MOS-unit Shipping of both MODS 2 and LUCI 2 is planned in 2013.įig.2: Cut through the LUCI cryostat. First light for LUCI 1 was obtained in 2008, regular observing started at the end of 2009. The first prime-focus camera arrived at the telescope in 2005. The beams of the two primary mirrors are combined in a near- to mid-infrared interferometer (LINC-NIRVANA) and in an optical to near-infrared interferometer (LBTI). Each of the two telescopes is equipped with three single beam instruments: a prime focus camera, an optical spectrograph (MODS), and a near-infrared instrument (LUCI, formerly LUCIFER). The LBT observing instruments split into single beam instruments receiving light from one primary mirror only, and instruments combining the beams of the two mirrors while conserving their phase relation (interferometers). The first deformable secondary was delivered in 2010, the second one in 2012. The first mirror arrived on the mountain in September 2003, the second one in September 2005. The two 8.4-meter primary mirrors have been molded and polished by the University of Arizona Mirror Lab. The telescope mount was completed in Italy and shipped to Arizona in the summer of 2002. This configuration mimimizes the instrumental background radiation and thus makes the LBT well suited for infrared observations. At the LBT, the secondary mirrors provide the deformable surfaces, therefore, in contrary to other telescopes, no additional components in the optical path are required. The essential component of an adaptive optics system is a deformable mirror which corrects the wavefront deformations in realtime. A major innovative feature of the LBT is the integrated adaptive optics (which compensates the image perturbation caused by atmospheric turbulences). Because of its binocular arrangement, the telescope achieves a resolving power corresponding to a 22.8-meter telescope. This telescope is equivalent in light-gathering power to a single 11.8 meter instrument. The LBT is a binocular telescope consisting of two 8.4-meter mirrors on a common mount (Fig. The telescope is located on Mount Graham, near Tucson, Arizona at an altitude of about 3200 m. The LBT ( Large Binocular Telescope) is a collaboration between astronomical institutes in Germany, Italy, and the US.
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