![]() The Pan-STARRS Data Release 2 (DR2) astrometric system is tied to the Gaia DR1 coordinate frame with a systematic uncertainty of ∼5 mas. For the DR2 version of the database, the astrometry was recalibrated against Gaia DR1 the coordinates reported in the ObjectThin table should be used as the best R.A. The bright-star systematic error floor for individual astrometric measurements is 16 mas. The coordinates in this table are the best ones to use for DR1. ground-based surveys as RAVE, SDSS, Pan-STARRS, APOGEE, LSST, etc. The astrometric calibration compensates for similar systematic effects so that positions, proper motions, and parallaxes are reliable as well. microarcsecond NIR astrometry and millimag photometry to penetrate obscured regions. So save a frame that you could not plate solve and use that frame to try different astrometry input parameters with until it does solve. 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. This is not a kstars/ekos issue, its an astrometry issue. Kuiper Belt Objects within the first year of operation and will obtain accurate astrometry for all of them on a weekly or. 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.
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