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The PanSTARRS telescope surveyed the sky in several different areas using various observing strategies.  The 3PI survey covers the 30,000 deg2 (3 steradians) of sky north of Declination -30º in 5 filters (grizy) with approximately 10 exposures per filter to a combined depth of approximately 21-23 mag.  The Medium Deep Survey covers 10 fields, each about 7 deg2, with hundreds to thousands of exposures per filter to reach a combined depth of 24–26 mag.  Other secondary surveys (M31 survey, ecliptic plane survey, celestial north pole) also were carried out.  The initial PS1 data release includes only the 3PI survey, but other data will be released as processing is completed.



Parent page for description of the surveys.  Outline of things to include:


  • Summary table:
    • Faint- and bright limits
    • locations and areal coverage versus time
    • Data-taking statistics: numbers of visits, quality, etc.
  • 3pi Survey (3PI):
    • Definition in terms of coverage maps, depth, observing cadences
  • Medium Deep Survey(MDS):
    • Location on sky, depth, observing cadences
  • Calibration fields

3PI Survey

The 3PI Survey covers the sky north of  -30º in 5 filters (grizy).  There are typically a dozen pointings in each filter, with the pointing centers dithered to enable the construction of a seamless image that fills in regions of bad pixels in most parts of the sky.  A typical point in the sky has about 10 pointings available.  The median seeing in the images is 1.1" FWHM.  The depth is given in the table below for both the individual exposures and the stacked image sum.

Image Datag limitr limiti limitz limity limit
Single epoch22.222.021.520.819.8
Stacked sum23.423.222.722.021.1

Medium Deep Survey

The 10 fields in the Medium Deep Survey are described below.  Each field was observed several times a night during the months of the year when it was observable.  In total there are hundreds to thousands of exposures in each of the 5 filters (grizy), enabling the construction of very deep stacked images.  The depth of individual exposures is the same as for the 3PI survey in the table above; the depend of the stacked image sum is shown below.

Field #NameAlt NameRA (J2000)RA (deg)Dec (J2000)Dec (deg)Commentg limitr limiti limitz limity limit
01PS1MD01XMM-LSS-DXS/VVDS-02h02 23 3035.875-04 15 00-4.250Multi-wavelength Survey Field25.925.826.025.624.3
02PS1MD02CDFS/GOODS/GEMS03 32 2453.100-27 48 00-27.800Multi-wavelength Survey Field25.625.425.825.324.1
03PS1MD03IFA/Lynx08 42 22130.592+44 19 00+44.317Radio Survey Field25.825.826.025.624.3
04PS1MD04COSMOS10 00 00150.000+02 12 00+2.200Multi-wavelength Survey Field25.825.725.825.424.0
05PS1MD05Lockman-DXS10 47 40161.917+58 05 00+58.083Multi-wavelength Survey Field25.825.725.925.423.9
06PS1MD06NGC 425812 20 00185.000+47 07 00+47.117H20 Maser25.825.625.925.323.9
07PS1MD07DEEP2 Field 1/Extended Groth Strip14 14 49213.704+53 05 00+53.083Multi-wavelength Survey Field25.825.725.925.424.1
08PS1MD08ELAIS-N1-DXS16 11 09242.787+54 57 00+54.950Multi-wavelength Survey Field25.925.826.025.424.2
09PS1MD09SA22-DXS/VVDS-22h22 16 45334.188+00 17 00+0.283Multi-wavelength Survey Field26.025.926.125.624.1
10PS1MD10DEEP2-Field323 29 15352.312-00 26 00-0.433Multi-wavelength Survey Field25.925.826.125.624.1

The detection limits come from a 2015 January analysis by Nigel Metcalfe and will probably change in the final processing.  They are 5-sigma point source detection limits calculated from the databases by measuring (roughly) where psfflux_err/psfflux=0.2.

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