The Pan-Starrs 1 Photometric Reference Ladder, Release 12.01

Abstract

As of 2012 Jan 21, the Pan-STARRS 1 3π Survey has observed the 3/4 of the sky visible from Hawaii with a minimum of 2 and mean of 7.6 observations in 5 filters, g P1 ,r P1 ,i P1 ,z P1 ,y P1 . Now at the end of the second year of the mission, we are in a position to make an initial public release of a portion of this unprecedented dataset. This article describes the PS1 Photometric Ladder, Release 12.01 This is the first of a series of data releases to be generated as the survey coverage increases and the data analysis improves. The Photometric Ladder has rungs every hour in RA and at 4 intervals in declination. We will release updates with increased area coverage (more rungs) from the latest dataset until the PS1 survey and the final re-reduction are completed. The currently released catalog presents photometry of ∼ 1000 objects per square degree in the rungs of the ladder. Saturation occurs at g P1 , r P1 , i P1 ∼ 13.5; z P1 ∼ 13.0; and y P1 ∼ 12.0. Photometry is provided for stars down to g P1 , r P1 , i P1 ∼ 19.1 in the AB system. This data release depends on the rigid 'Ubercal' photometric calibration using only the photometric nights, with systematic uncertainties of (8.0, 7.0, 9.0, 10.7, 12.4) millimags in (g P1 ,r P1 ,i P1 ,z P1 ,y P1 ). Areas covered only with lower quality nights are also included, and have been tied to the Ubercal solution via relative photometry; photometric accuracy of the non-photometric regions is lower and should be used with caution.

The Optical–infrared Extinction Curve and Its Variation in the Milky Way

“…The effective wavelengths of the filters are roughly 480, 620, 750, 870, and 960 nm, for the g P1 , r P1 , i P1 , z P1 , and y P1 filters, respectively. The data are automatically processed by the PS1 image processing pipeline (Magnier 2006), which analyzes images to deliver photometry, astrometry, and morphology (Magnier 2007;Magnier et al 2008Magnier et al , 2013. The photometric calibration of the survey, both relative and absolute, is accurate to better than 1% (Schlafly et al 2012;Tonry et al 2012).…”

2MASS 0213+3648 C: A wide T3 benchmark companion to an an active, old M dwarf binary

“…Pan-STARRS 1 data are reduced and calibrated photometrically and astrometrically by a process described by Magnier (2006Magnier ( , 2007, Magnier et al (2013Magnier et al ( , 2016, and Schlafly et al (2012). The telescope undertook a series of sky surveys including the 3π Survey, covering 30 000 deg 2 north of δ = −30 • with two pairs of observations per year in each of five filters.…”

Three-Dimensional Dust Mapping Reveals That Orion Forms Part of a Large Ring of Dust

“…The imager is optimized for survey operations, featuring a wide 3 • field of view outfitted with the billion-pixel GPC1 camera (Hodapp et al 2004;Tonry & Onaka 2009;Onaka et al 2008). This work relies on data from the Pan-STARRS1 3π survey, which is designed to observe three-quarters of the sky four times a year, in each of five filters (Magnier et al 2013). These filters include the SDSS-like gri P1 as well as z P1 and y P1 , at which wavelengths the Pan-STARRS1 system is much more sensitive than the SDSS (Stubbs et al 2010).…”