![]() ![]() The Pan-STARRS Data Release 2 (DR2) astrometric system is tied to the Gaia DR1 coordinate frame with a systematic uncertainty of ∼5 mas. ![]() The bright-star systematic error floor for individual astrometric measurements is 16 mas. Pan-STARRS1 (PS1) is the first part of Pan-STARRS to be completed and is the basis for both Data Releases 1 and 2 (DR1 and DR2). The astrometric calibration compensates for similar systematic effects so that positions, proper motions, and parallaxes are reliable as well. Pan-STARRS is a system for wide-field astronomical imaging developed and operated by the Institute for Astronomy at the University of Hawaii. 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. 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. With single-epoch astrometry of 10 milliarcseconds, these observations will yield parallaxes for stars within 100 pc and proper motions out to several hundred. Williams (from 34 observations spanning 2018 Aug. ![]() 13, when the magnitude was given as 21.2-21.4, 23.5, and 22.7-23.5, respectively), the following elliptical orbital elements by G. 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°. The available astrometry (including additional pre-discovery Pan-STARRS2 observations from 2018 Oct. We present the details of the photometric and astrometric calibration of the Pan-STARRS1 3π Survey. ![]()
0 Comments
Leave a Reply. |