Pan-STARRS

s detected by various projects: The Pan-STARRS Project is a collaboration between the University of Hawaiʻi Institute for Astronomy, MIT Lincoln Laboratory, Maui High Performance Computing Center and Science Applications International Corporation. Telescope construction was funded by the U.S. Air Force. By detecting differences from previous observations of the same areas of the sky, Pan-STARRS is discovering many new asteroids, The first Pan-STARRS telescope (PS1) is located at the summit of Haleakalā on Maui, Hawaii, on 30 June 2006 and went online on 6 December 2008 under the administration of the University of Hawaiʻi. PS1 began full-time science observations on 13 May 2010 and the PS1 Science Mission ran until March 2014. Operations were funded by the PS1 Science Consortium, PS1SC, a consortium including the Max Planck Society in Germany, National Central University in Taiwan, Edinburgh, Durham and Queen's Belfast Universities in the UK, and Johns Hopkins and Harvard Universities in the United States and the Las Cumbres Observatory Global Telescope Network. Consortium observations for the all sky (as visible from Hawaii) survey were completed in April 2014. Having completed PS1, the Pan-STARRS Project focused on building Pan-STARRS 2 (PS2), for which first light was achieved in 2013, with full science operations scheduled for 2014 and then the full array of four telescopes, sometimes called PS4. Completing the array of four telescopes is estimated at a total cost of US$100 million for the entire array. In the wake of substantial funding problems, no clear timeline existed for additional telescopes beyond the second. In March 2018, Pan-STARRS 2 was credited by the Minor Planet Center for the discovery of the potentially hazardous Apollo asteroid , its first minor-planet discovery made at Haleakala on 13 May 2015. == Instruments ==

Pan-STARRS consists of two 1.8-m Ritchey–Chrétien telescopes located at Haleakala in Hawaii. The initial telescope, PS1, saw first light using a low-resolution camera in June 2006. The telescope has a 3° field of view, which is extremely large for telescopes of this size, and is equipped with what was the largest digital camera ever built, recording almost 1.4 billion pixels per image. The focal plane has 60 separately mounted close packed CCDs arranged in an 8 × 8 array. The corner positions are not populated, as the optics do not illuminate the corners. Each CCD device, called an Orthogonal Transfer Array (OTA), has 4800 × 4800 pixels, separated into 64 cells, each of 600 × 600 pixels. This gigapixel camera or 'GPC' saw first light on 22 August 2007, imaging the Andromeda Galaxy. After initial technical difficulties that were later mostly solved, PS1 began full operation on 13 May 2010. Nick Kaiser, principal investigator of the Pan-STARRS project, summed it up, saying, "PS1 has been taking science-quality data for six months, but now we are doing it dusk-to-dawn every night." The PS1 images, however, remain slightly less sharp than initially planned, which significantly affects some scientific uses of the data. Each image requires about 2 gigabytes of storage and exposure times will be 30 to 60 seconds (enough to record objects down to apparent magnitude 22), with an additional minute or so used for computer processing. Since images are taken on a continuous basis, about 10 terabytes of data are acquired by PS1 every night. Comparing against a database of known unvarying objects compiled from earlier observations will yield objects of interest: anything that has changed brightness and/or position for any reason. As of June 30, 2010, University of Hawaiʻi in Honolulu received an $8.4 million contract modification under the PanSTARRS multi-year program to develop and deploy a telescope data management system for the project. The very large field of view of the telescopes and the relatively short exposure times enable approximately 6000 square degrees of sky to be imaged every night. The entire sky is 4π steradians, or 4π × (180/π)2 ≈ 41,253.0 square degrees, of which about 30,000 square degrees are visible from Hawaii, which means that the entire sky can be imaged in a period of 40 hours (or about 10 hours per night on four days). Given the need to avoid times when the Moon is bright, this means that an area equivalent to the entire sky will be surveyed four times a month, which is entirely unprecedented. By the end of its initial three-year mission in April 2014, PS1 had imaged the sky 12 times in each of 5 filters ('g', 'r', 'i', 'z', and 'y'). Filters 'g', 'r', and 'i' have the bandpasses of the Sloan Digital Sky Survey (SDSS) filters. (Midpoints and bandwidths at half maximum are 464 nm and 128 nm, 658 nm and 138 nm, and 806 nm and 149 nm, respectively.) The'z' filter has the SDSS midpoint (900 nm), but its longwave cutoff avoids water absorptions bands beginning at 930 nm. The shortwave cutoff of the 'y' filter is set by the water absorption bands that end around 960 nm. The longwave cutoff band is currently at 1030 nm to avoid the worst of the detector sensitivity to temperature variations. == Science ==

has an orbit around the Sun that keeps it as a constant companion of Earth. Credit: NASA/JPL-Caltech Pan-STARRS is currently mostly funded by a grant from the NASA Near Earth Object Observations program. It therefore spends 90% of its observing time in dedicated searches for Near Earth Objects. Systematically surveying the entire sky on a continuous basis is an unprecedented project and is expected to produce a dramatically larger number of discoveries of various types of celestial objects. For instance, the current leading asteroid discovery survey, the Mount Lemmon Survey, reaches an apparent magnitude of 22 V. Pan-STARRS will go about one magnitude fainter and cover the entire sky visible from Hawaii. The ongoing survey will also complement the efforts to map the infrared sky by the NASA WISE orbital telescope, with the results of one survey complementing and extending the other. The second data release, Pan-STARRS DR2, announced in January 2019, is the largest volume of astronomical data ever released. At over 1.6 petabytes of images, it is equivalent to 30,000 times the text content of Wikipedia. The data reside in the Mikulski Archive for Space Telescopes (MAST). Military limitations (until end 2011) According to Defense Industry Daily, significant limitations were put on the PS1 survey to avoid recording sensitive objects. Streak detection software (known as "Magic") was used to censor pixels containing information about satellites in the image. Early versions of this software were immature, leaving a fill factor of 68% of the full field of view (which figure includes gaps between the detectors), but by March 2010 this had improved to 76%, a small reduction from the approximately 80% available. At the end of 2011, the USAF completely eliminated the masking requirement (for all images, past and future). Thus, with the exception of a few non-functioning OTA cells, the entire field of view can be used. Solar System observed by the Hubble Space Telescope (6 March 2014) In addition to the large number of expected discoveries in the asteroid belt, Pan-STARRS is expected to detect at least 100,000 Jupiter trojans (compared to 2900 known as of end-2008); at least 20,000 Kuiper belt objects (compared to 800 known as of mid-2005); thousands of trojan asteroids of Saturn, Uranus, and Neptune (currently eight Neptune trojans are known, none for Saturn, and one for Uranus); and large numbers of centaurs and comets. Apart from dramatically adding to the number of known Solar System objects, Pan-STARRS will remove or mitigate the observational bias inherent in many current surveys. For instance, among currently known objects there is a bias favoring low orbital inclination, and thus an object such as escaped detection until recently despite its bright apparent magnitude of 17, which is not much fainter than Pluto. Also, among currently known comets, there is a bias favoring those with short perihelion distances. Reducing the effects of this observational bias will enable a more complete picture of Solar System dynamics. For instance, it is expected that the number of Jupiter trojans larger than 1 km may in fact roughly match the number of asteroid-belt objects, although the currently known population of the latter is several orders of magnitude larger. Pan-STARRS data will elegantly complement the WISE (infrared) survey. WISE infrared images will permit an estimate of size for asteroids and trojan objects tracked over longer periods of time by Pan-STARRS. In 2017, Pan-STARRS detected the first known interstellar object, 1I/2017 U1 'Oumuamua, passing through the Solar System. During the formation of a planetary system, it is thought that a very large number of objects are ejected due to gravitational interactions with planets (as many as 1013 such objects in the case of the Solar System). Objects ejected from planetary systems of other stars might plausibly be throughout the Milky Way and some may pass through the Solar System. Pan-STARRS may detect collisions involving small asteroids. These are quite rare and none have yet been observed, but with a dramatic increase in the number of asteroids discovered it is expected from statistical considerations that some collision events may be observed. In November 2019, a review of images from Pan-STARRS revealed that the telescope had captured the disintegration of asteroid P/2016 G1. The asteroid was struck by a smaller object, and gradually fell apart. Astronomers speculate that the object that struck the asteroid may have massed only , traveling at . Beyond the Solar System It is expected that Pan-STARRS will discover an extremely large number of variable stars, including such stars in other nearby galaxies; this may lead to the discovery of previously unknown dwarf galaxies. In discovering numerous Cepheid variables and eclipsing binary stars, it will help determine distances to nearby galaxies with greater precision. It is expected to discover many Type Ia supernovae in other galaxies, which are important in studying the effects of dark energy, and also optical afterglows of gamma ray bursts. Because very young stars (such as T Tauri stars) are usually variable, Pan-STARRS should discover many of these and improve our understanding of them. It is also expected that Pan-STARRS may discover many extrasolar planets by observing their transits across their parent stars, as well as gravitational microlensing events. Pan-STARRS will also measure proper motion and parallax and should thereby discover many brown dwarfs, white dwarfs, and other nearby faint objects, and it should be able to conduct a complete census of all stars within 100 parsecs of the Sun. Prior proper motion and parallax surveys often did not detect faint objects such as the recently discovered Teegarden's star, which are too faint for projects such as Hipparcos. Also, by identifying stars with large parallax but very small proper motion for follow-up radial velocity measurements, Pan-STARRS may even be able to permit the detection of hypothetical Nemesis-type objects if these actually exist. Selected discoveries == See also ==