Page History
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- What is Pan-STARRS? Why was it done?
- What types of data were obtained? What can they tell me about the sky?
- How does Pan-STARRS PS1 compare to other surveys such as the Sloan Digital Sky Survey (SDSS)?
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- What filters did PS1 use?
- The PS1 survey used 5 broadband (R ~ 3.5) 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?
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