Automated Analysis Pipelines For The Galactic Plane Infrared Polarization Survey: From Basic Image Processing To Crowded-field, Variable-PSF, Imaging Polarimetry.

Details Automated Analysis Pipelines For The Galactic Plane Infrared Polarization Survey: From Basic Image Processing To Crowded-field, Variable-PSF, Imaging Polarimetry. Automated Analysis Pipelines For The Galactic Plane Infrared Polarization Survey: From Basic Image Processing To Crowded-field, Variable-PSF, Imaging Polarimetry.

Jan 2010

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2010aas...21543801c&link_type=abstract

American Astronomical Society, AAS Meeting #215, #438.01; Bulletin of the American Astronomical Society, Vol. 42, p.392

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The Galactic Plane Infrared Polarization Survey (GPIPS) is being conducted on the 1.83m Perkins telescope outside Flagstaff, Arizona using the Mimir instrument configured as a near-infrared imaging polarimeter. The 10x10 arcmin field of view captures H-band (1.6 um) images of thousands of stars in every image. GPIPS collects over 50,000 of these images each year and when completed, will have over 300,000 images. Automated methods of basic data processing, including astrometry, flat, dark, and linearity corrections must be applied with a minimum of human intervention. Advanced analyses, including removal of atmospheric transmission variations, registration and averaging of dither-offset images, high precision photometry, removal of instrumental polarization effects, and final computation of linear polarizations must find and preserve the best signal-to-noise present in the data. Achieving the GPIPS science goals requires being able to extract useful polarization information for around 200 stars per image, for images with a variety of PSF sizes, PSF quality, and stellar crowding. Also challenging is to achieve similarly consistent analyses of image fields toward infrared polarimetric standards, which are exceedingly sparse, and globular clusters, used to establish polarization nulls across the field of view. This poster will highlight the steps in our automated pipelines and some of the lessons learned in developing, testing, and using these pipelines for milli-mag level, crowded-field, infrared imaging polarimetry.
Supported by NSF grants AST 06-07500 and AST 09-07790

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