Catálogo de publicaciones - revistas

<jats:title>Abstract</jats:title> <jats:p>The Pan-STARRS data-processing system is responsible for the steps needed to downloaded, archive, and process all images obtained by the Pan-STARRS telescopes, including real-time detection of transient sources such as supernovae and moving objects including potentially hazardous asteroids. With a nightly data volume of up to 4 TB and an archive of over 4 PB of raw imagery, Pan-STARRS is solidly in the realm of Big Data astronomy. The full data-processing system consists of several subsystems covering the wide range of necessary capabilities. This article describes the Image Processing Pipeline and its connections to both the summit data systems and the outward-facing systems downstream. The latter include the Moving Object Processing System (MOPS) and the public database: the Published Science Products Subsystem.</jats:p>

<jats:title>Abstract</jats:title> <jats:p>The Pan-STARRS1 (PS1) Science Consortium has carried out a set of imaging surveys using the 1.4 gigapixel GPC1 camera on the PS1 telescope. As this camera is composed of many individual electronic readouts and covers a very large field of view, great care was taken to ensure that the many instrumental effects were corrected to produce the most uniform detector response possible. We present the image-detrending steps used as part of the processing of the data contained within the public release of Pan-STARRS1 Data Release 1 (DR1). In addition to the single image processing, the methods used to transform the 375,573 individual exposures into a common sky-oriented grid are discussed, as well as those used to produce both the image stack and difference combination products.</jats:p>

<jats:title>Abstract</jats:title> <jats:p>Over 3 billion astronomical sources have been detected in the more than 22 million orthogonal transfer CCD images obtained as part of the Pan-STARRS1 3<jats:italic>π</jats:italic> survey. Over 85 billion instances of those sources have been automatically detected and characterized by the Pan-STARRS Image Processing Pipeline photometry software, <jats:monospace>psphot</jats:monospace>. This fast, automatic, and reliable software was developed for the Pan-STARRS project but is easily adaptable to images from other telescopes. We describe the analysis of the astronomical sources by <jats:monospace>psphot</jats:monospace> in general as well as for the specific case of the third processing version used for the first two public releases of the Pan-STARRS 3<jats:italic>π</jats:italic> Survey data.</jats:p>

<jats:title>Abstract</jats:title> <jats:p>We present the details of the photometric and astrometric calibration of the Pan-STARRS1 3<jats:italic>π</jats:italic> Survey. The photometric goals were to reduce the systematic effects introduced by the camera and detectors, and to place all of the observations onto a photometric system with consistent zero-points over the entire area surveyed, the ≈30,000 deg<jats:sup>2</jats:sup> north of <jats:italic>δ</jats:italic> = −30°. Using external comparisons, we demonstrate that the resulting photometric system is consistent across the sky to between 7 and 12.4 mmag depending on the filter. For bright stars, the systematic error floor for individual measurements is (<jats:italic>σ</jats:italic> <jats:sub> <jats:italic>g</jats:italic> </jats:sub>, <jats:italic>σ</jats:italic> <jats:sub> <jats:italic>r</jats:italic> </jats:sub>, <jats:italic>σ</jats:italic> <jats:sub> <jats:italic>i</jats:italic> </jats:sub>, <jats:italic>σ</jats:italic> <jats:sub> <jats:italic>z</jats:italic> </jats:sub>, <jats:italic>σ</jats:italic> <jats:sub> <jats:italic>y</jats:italic> </jats:sub>) = (14, 14, 15, 15, 18) mmag. The astrometric calibration compensates for similar systematic effects so that positions, proper motions, and parallaxes are reliable as well. The bright-star systematic error floor for individual astrometric measurements is 16 mas. The Pan-STARRS Data Release 2 (DR2) astrometric system is tied to the Gaia DR1 coordinate frame with a systematic uncertainty of ∼5 mas.</jats:p>