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The Pan-STARRS project

• What is Pan-STARRS?  Why was it done?
• What types of data were obtained?  What can they tell me about the sky?
• How does PS1 compare to other surveys such as the Sloan Digital Sky Survey (SDSS)?

PS1 data access

• How do I get started?  Are there examples of data queries?
• How do I get PS1 data for a list of sources I have?
• What tools are available to extract and examine PS1 data?
• How do I access PS1 image data?

PS1 catalog data

• How do I make sense of the entries in the PS1 data tables?

PS1 astrometry

• How good is PS1 astrometry?

PS1 photometry

• What filters did PS1 use?
  • The PS1 camera surveyed the sky using 5 filters: g, r, i, z, and y. The effective wavelengths (and spectral resolutions) of these 5 filters are 481 nm (R = 3.5), 617 nm (R = 4.4), 752 nm (R = 5.8), 866 nm (R = 8.3), and 962 nm (R = 11.6), respectively. Please refer to Table 1 in Schlafly et al. (2012) for further details.
• How good is PS1 photometry?
  •  The PS1 photometric system is shown by Schlafly et al. (2012) to have reliability across the survey region at the level of (8.0, 7.0, 9.0, 10.7, 12.4) millimags in (g, r, i, z, y). The Haleakala site is good enough to enable <1% photometry over much of the sky. The PS1 photometric calibration pipeline process is described in Magnier et al. (2016). 
• Which magnitudes should I use?
• What are the brightest and faintest stars for which the data are reliable?
• How reliable is PS1 photometry of nearby, bright galaxies?