The Dark Energy Survey (DES) is a five-year optical imaging campaign with the goal of understanding the origin of cosmic acceleration. DES performs a 5000 square degree survey of the southern sky in five optical bands (g,r,i,z,Y) to a depth of ~24th magnitude. Contemporaneously, DES performs a deep, time-domain survey in four optical bands (g,r,i,z) over 27 square degrees. DES exposures are processed nightly with an evolving data reduction pipeline and evaluated for image quality to determine if they need to be retaken. Difference imaging and transient source detection are also performed in the time domain component nightly. On a bi-annual basis, DES exposures are reprocessed with a refined pipeline and coadded to maximize imaging depth. Here we describe the DES image processing pipeline in support of DES science, as a reference for users of archival DES data, and as a guide for future astronomical surveys.
Morganson, E.. "The Dark Energy Survey Image Processing Pipeline." Publications of the Astronomical Society of the Pacific, vol. 130, no. 989, Jan. 2018. https://doi.org/10.1088/1538-3873/aab4ef
Morganson, E. (2018). The Dark Energy Survey Image Processing Pipeline. Publications of the Astronomical Society of the Pacific, 130(989). https://doi.org/10.1088/1538-3873/aab4ef
Morganson, E., "The Dark Energy Survey Image Processing Pipeline," Publications of the Astronomical Society of the Pacific 130, no. 989 (2018), https://doi.org/10.1088/1538-3873/aab4ef
@article{osti_1422722,
author = {Morganson, E.},
title = {The Dark Energy Survey Image Processing Pipeline},
annote = {The Dark Energy Survey (DES) is a five-year optical imaging campaign with the goal of understanding the origin of cosmic acceleration. DES performs a 5000 square degree survey of the southern sky in five optical bands (g,r,i,z,Y) to a depth of ~24th magnitude. Contemporaneously, DES performs a deep, time-domain survey in four optical bands (g,r,i,z) over 27 square degrees. DES exposures are processed nightly with an evolving data reduction pipeline and evaluated for image quality to determine if they need to be retaken. Difference imaging and transient source detection are also performed in the time domain component nightly. On a bi-annual basis, DES exposures are reprocessed with a refined pipeline and coadded to maximize imaging depth. Here we describe the DES image processing pipeline in support of DES science, as a reference for users of archival DES data, and as a guide for future astronomical surveys.},
doi = {10.1088/1538-3873/aab4ef},
url = {https://www.osti.gov/biblio/1422722},
journal = {Publications of the Astronomical Society of the Pacific},
issn = {ISSN 0004-6280},
number = {989},
volume = {130},
place = {United States},
publisher = {Astronomical Society of the Pacific},
year = {2018},
month = {01}}
Brookhaven National Laboratory (BNL), Upton, NY (United States); SLAC National Accelerator Laboratory (SLAC), Menlo Park, CA (United States); Fermi National Accelerator Laboratory (FNAL), Batavia, IL (United States); Lawrence Berkeley National Laboratory (LBNL), Berkeley, CA (United States)
Sponsoring Organization:
USDOE Office of Science (SC), High Energy Physics (HEP) (SC-25)
Contributing Organization:
DES
DOE Contract Number:
AC02-07CH11359
OSTI ID:
1422722
Report Number(s):
arXiv:1801.03177; FERMILAB-PUB-17-524-AE; 1647428
Journal Information:
Publications of the Astronomical Society of the Pacific, Journal Name: Publications of the Astronomical Society of the Pacific Journal Issue: 989 Vol. 130; ISSN 0004-6280