We present the details of the photometric and astrometric calibration of the Pan-STARRS1 3πSurvey. 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 deg² 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.

我们介绍了 Pan-STARRS1 3 π巡天的光度和天体校准的详细信息。光度测量目标是减少由相机和探测器引入的系统效应，并将所有观测结果放置在一个光度测量系统上，在整个调查区域内具有一致的零点，δ = -30以北≈30,000 度²。使用外部比较，我们证明最终的光度系统在整个天空中是一致的，取决于过滤器，在 7 到 12.4 mmag 之间。对于明亮的恒星，单个测量的系统误差基底为 ( σ _g , σ _r , σ _i , σ _z , σ _y )=(14, 14, 15, 15, 18) mmag。天体测量校准补偿了类似的系统效应，因此位置、自行和视差也是可靠的。单个天体测量的亮星系统误差底限为 16 mas。Pan-STARRS Data Release 2 (DR2) 天体测量系统与 Gaia DR1 坐标系相关联，系统不确定性约为 5 mas。