This page is still being populated. Please be patient. We will provide the answers over the next few weeks.

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

What should I know about the current data release?

See the PS1 DR1 caveats page for more information.

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 4 in Tonry et al. (2012) for bandpass details. Schlafly et al. (2012) provides updated zeropoints in Table 1.

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?

There are several different kinds of magnitudes in the PS1 catalog (aperture, PSF-fitting, Kron, etc.), and there are also several different sources for those magnitudes (means from multi-epoch measurements, measurements from deep stack images, "forced mean" measurements where a stack image is used to identify objects but the photometry is determined by fits to the single-epoch warp images).  Which magnitude should you used for your science?

A comparison between different photometric measures provides some guidance. The answer is complex, but here is a high-level summary:

• For point sources use PSF magnitudes.
  • Mean PSF magnitudes have the lowest noise (because the PSF model is most accurate in single-epoch images). They are good for brighter objects, but for objects near the single-epoch detection limit they will be biased (due to the absence of sub-threshold detections), and objects too faint to detect in a single epoch are missing.
  • Stack PSF magnitudes are noisier because the PSF model is less accurate. But the stack detections are more than a magnitude deeper and so have many more faint objects than mean detections.
  • Forced mean PSF magnitudes use PSF-fitting photometry on the single-epoch images at positions of stack detections. They are a reasonable compromise: they have slightly lower noise than the stack PSF magnitudes, and they are deep and unbiased (because they use data from all warps).  Their noise is higher than the mean PSF magnitudes, however.
• For extended objects use Kron magnitudes.
  • Stack Kron magnitudes are usually the first choice as a general-purpose, deep magnitude.
  • de Vaucouleurs and exponential model fits could be better in some cases, and the mean measurements can be useful for objects that are barely resolved (where the PSF is important).
  • Extended object photometry using the PS1 catalog will require research and analysis by the user to determine the best approach.

What are the brightest and faintest stars for which the data are reliable?

The answer is it depends on band and FWHM. A very conservative estimate for the bright limit is as follows:

You may find individual fields where you can do up to a magnitude brighter than this.

How reliable is PS1 photometry of nearby, bright galaxies?

There are two main problems you should be aware of which affect bright galaxies:

(1) oversubtraction of the sky background - this affects most Messier galaxies and some (most?) of the larger NGC objects. As the background is subtracted independently from each filter, this can induce colour changes across the galaxy. In principle the polynomial used to store the background is stored and can be de-applied. However, as the subtraction is done at the warp stage, if you want stacked data the stacking procedure would have to be re-run. This facility is not available in DR1.

	Messier 31 from the 3pi stacks showing an extreme example of the over-subtraction of the background.

(2) issues with the row-by-row bias and continuity corrections - these are applied and therefore seen on individual ccd scales (~600 pixels). As this is done at the detrending stage this is currently very difficult to correct. There is an aspiration to re-analyse all bright galaxies but this has not yet been done.

	Messier 106 - this is an extreme stretch of the r-band stack showing problems on the scale of individual ccds.