The starting point for the PS1 data archive is at The Pan-STARRS1 data archive home page.
The following information is taken from these papers, which should be cited appropriately
- Chambers et al. 2016, The Pan-STARRS1 Surveys
D. Scolnic et al. 2015, Supercal: Cross-calibration of Multiple Photometric Systems to Improve Cosmological Measurements with Type Ia Supernovae
- A link the the overall Pan-STARRS throughputs as shown in the Tonry et al. figure below are here at Vizier or also as a machine readable ascii file here
|Figure from Tonry et al. 2012 : The PS1 capture cross-section in m2/e/photon|
to produce a detected e− for an incident photon for the six Pan-STARRS1 bandpasses, grizy and w for a standard airmass of 1.2
|Figure from Scolnic et al. 2015, showing comparisons between the grizP1 and other survey filters (CSP = Carnegie Supernova Project and CfAK = CfA-Keplercam, SNLS = Supernova Legacy Survey|
Pan-STARRS is primarily sensitive to visible light, though observations extend slightly into the infrared passbands. Each camera included an identical set of 5 to 6 optical filters that can be remotely positioned in front of the focal plane.
The searches for asteroids and potentially hazardous objects may use a wide filter w ("g+r+i") that covers most of the visible waveband from 0.5 to 0.8 microns. This filter provides maximum sensitivity for detecting solar system objects. Surveys for stars and galaxies are much more valuable when they include color information, so Pan-STARRS will include standard photometric g-, r-, i-, and z-band filters, as used in the Sloan Digital Sky Survey. The excellent near-infrared response of the Pan-STARRS detectors means that we can also make use of a y-band filter (1.0 microns). All magnitiudes are quoted on the AB system.
Tonry PS1 photometric system: http://adsabs.harvard.edu/abs/2012ApJ...750...99T
Scolnic Supercal: http://adsabs.harvard.edu/abs/2015ApJ...815..117S
for throughput measurement article see: http://inspirehep.net/record/849309/plots