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Parent page for the description of the observatory.
The information for this page should be taken from Chambers et al 2016.
Planned contents:
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Here is from PS1 dox summary:
The hardware and the survey operations (scheduling) and cadence is described in Chambers 2016.
- Design, construction (UH: Ken Chambers):
- Telescope, location
- FOV
- Image quality
- Site quality (seeing, clarity, backgrounds)
- Detectors: (UH, Tonry?)
- Relation to data quality
- Dynamic range (depth tables)
- Filters: (UH data; Scolnic)
- Illustration
- Compare to others that are nominally the same or similar.
- Observing strategy: (UH)
- Faint- and bright limits.
- Areal coverage versus time
- Distributions of data taking: Numbers of visits; ...
- Surveys (Ken?, Stephen?)
- 3PI. (cut & paste? Smart/Chambers --> DRS)
- Medium Deep Fields.
- 3PI. (cut & paste? Smart/Chambers --> DRS)
The Pan-STARRS telescopes are located at Haleakala Observatories on the island of Maui. The first telescope built, the Pan-STARRS1 Telescope (PS1), is an alt-az telescope with an 1.8m diameter mirror. With a field-of-view diameter of 3 degrees, it can observe a 7 square degree are on the sky with every exposure. The PS1: GPC1 camera, which uses 60 Orthogonal Transfer Arrays devices, is mounted in its focal plane. The PS1 observations are obtained through a set of five broadband filters, designated as grizyP1. Under certain circumstances PS1 observations are obtained with a sixth, “wide” filter designated as wP1 that essentially spans the gri bands. The PS1 Observing strategy was optimized for detecting moving objects as well as a uniform coverage of the 3pi survey (see PS1 Description of the surveys). |
The starting point for the PS1 data archive is at Pan-STARRS1 data archive home page.
The information on the pages below is taken from Chambers et al 2016, "The Pan-STARRS1 Surveys" and this paper should be cited when information is used.