![]() The Pan-STARRS Data Release 2 (DR2) astrometric system is tied to the Gaia DR1 coordinate frame with a systematic uncertainty of ∼5 mas. Astrometric Residuals : Large-Scale Circular Pattern. The bright-star systematic error floor for individual astrometric measurements is 16 mas. Pan-STARRS 1: a 1.8m survey telescope (1.4Gpix & 7deg2 F.O.V.). The astrometric calibration compensates for similar systematic effects so that positions, proper motions, and parallaxes are reliable as well. The result will be an unprecedented view on nearby stellar populations and insight into the dynamical structure of the local portions of the Galaxy. Good-quality measurement in our data (eg,PS). These values are also listed in the system metadata table ObjectQualityFlags. For bright stars, the systematic error floor for individual measurements is (σ g, σ r, σ i, σ z, σ y) = (14, 14, 15, 15, 18) mmag. With single-epoch astrometry of 10 milliarcseconds, these observations will yield parallaxes for stars within 100 pc and proper motions out to several hundred pc. ObjectQualityFlags values for column qualityFlag in table ObjectThin. 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. 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 2 north of δ = -30°. We present the details of the photometric and astrometric calibration of the Pan-STARRS1 3π Survey.
0 Comments
Leave a Reply. |
AuthorWrite something about yourself. No need to be fancy, just an overview. ArchivesCategories |