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Title:
IRACproc: a software suite for processing and analyzing Spitzer/IRAC data
Authors:
Schuster, Michael T.; Marengo, Massimo; Patten, Brian M.
Affiliation:
AA(Harvard-Smithsonian Ctr. for Astrophysics (USA) and Univ. of Minnesota (USA)), AB(Harvard-Smithsonian Ctr. for Astrophysics (USA)), AC(Harvard-Smithsonian Ctr. for Astrophysics (USA))
Publication:
Observatory Operations: Strategies, Processes, and Systems. Edited by Silva, David R.; Doxsey, Rodger E.. Proceedings of the SPIE, Volume 6270, pp. 627020 (2006). (SPIE Homepage)
Publication Date:
07/2006
Origin:
SPIE
DOI:
10.1117/12.673134
Bibliographic Code:
2006SPIE.6270E..65S

Abstract

We have developed a post-Basic Calibrated Data pipeline processing software suite called "IRACproc". This package facilitates the co-addition of dithered or mapped Spitzer/IRAC data to make them ready for further analysis with application to a wide variety of IRAC observing programs. In acting as a wrapper for the Spitzer Science Center's MOPEX software, IRACproc improves the rejection of cosmic rays and other transients in the co-added data. In addition, IRACproc performs (optional) Point Spread Function (PSF) fitting, subtraction, and masking of saturated stars. The under/critically sampled IRAC PSFs are subject to large variations in shape between successive frames as a result of sub-pixel shifts from dithering or telescope jitter. IRACproc improves cosmic ray and other transient rejection by using spatial derivative images to map the locations and structure of astronomical sources. By protecting sources with a metric that accounts for these large variations in the PSFs, our technique maintains the structure and photometric reliability of the PSF, while at the same time removing transients at the lowest level. High Dynamic Range PSFs for each IRAC band were obtained by combining an unsaturated core, derived from stars in the IRAC PSF calibration project, with the wings of a number of bright stars. These PSFs have dynamic ranges of ~107 and cover the entire IRAC field of view. PSF subtraction can drastically reduce the light from a bright star outside the saturated region. For a bright star near the array center it is possible to detect faint sources as close as ~15-20" that would otherwise be lost in the glare. In addition, PSF fitting has been shown to provide photometry accurate to 1-2% for over-exposed stars.
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