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Magnier, Eugene. A.; Schlafly, Edward. F.; Finkbeiner, Douglas P.; Tonry, J. L.; Goldman, B.; Röser, S.; Schilbach, E.; Casertano, S.; Chambers, K. C.; Flewelling, H. A.; Huber, M. E.; Price, P. A.; Sweeney, W. E.; Waters, C. Z.; Denneau, L.; Draper, P. W.; Hodapp, K. W.; Jedicke, R.; Kaiser, N.; Kudritzki, R.-P.; Metcalfe, N.; Stubbs, C. W.; Wainscoat, R. J.
The Astrophysical journal. Supplement series, 11/2020, Letnik: 251, Številka: 1Journal Article
Abstract We present the details of the photometric and astrometric calibration of the Pan-STARRS1 3 π 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 2 north of δ = −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 ( σ g , σ r , σ i , σ z , σ y ) = (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.
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JCR | SNIP | JCR | SNIP | JCR | SNIP | JCR | SNIP |
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in: SICRIS
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