The 2.4 μm Galaxy Luminosity Function as Measured Using WISE . II. Sample Selection

Lake, S. E.; Wright, E. L.; Assef, R. J.; Jarrett, T. H.; Petty, S.; Stanford, S. A.; Stern, D.; Tsai, C. -W.

doi:10.3847/1538-4357/aae096

Title: The 2.4 μm Galaxy Luminosity Function as Measured Using WISE . II. Sample Selection

Journal Article · 09 October 2018 · The Astrophysical Journal (Online)

DOI: https://doi.org/10.3847/1538-4357/aae096 · OSTI ID:1545274

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^[4]; Stanford, S. A. ^[5];

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Univ. of California, Los Angeles, CA (United States)
Univ. Diego Portales, Santiago (Chile)
Univ. of Cape Town (South Africa)
NorthWest Research Associates, Redmond, WA (United States)
Univ. of California, Davis, CA (United States); Lawrence Livermore National Lab. (LLNL), Livermore, CA (United States)
California Inst. of Technology (CalTech), La Canada Flintridge, CA (United States). Jet Propulsion Lab.
Univ. of California, Los Angeles, CA (United States); California Inst. of Technology (CalTech), La Canada Flintridge, CA (United States). Jet Propulsion Lab.

The WISE satellite surveyed the entire sky multiple times in four infrared (IR) wavelengths (3.4, 4.6, 12, and 22 $$μ$$m). This all-sky IR photometric survey makes it possible to leverage many of the large publicly available spectroscopic redshift surveys to measure galaxy properties in the IR. While characterizing the cross-matching of WISE data to a single survey is a straightforward process, doing it with six different redshift surveys takes a fair amount of space to characterize adequately, because each survey has unique caveats and characteristics that need addressing. This work describes a data set that results from matching five public redshift surveys with the AllWISE data release, along with a reanalysis of the data described in Lake et al. The combined data set has an additional flux limit of 80 $$μ$$Jy (19.14 AB mag) in WISE's W1 filter, imposed in order to limit it to targets with high completeness and reliable photometry in the AllWISE data set. Consistent analysis of all of the data is only possible if the color bias discussed in Ilbert et al. is addressed (e.g., the techniques explored in Lake et al.). Finally, the sample defined herein is used in a companion paper in this series to measure the luminosity function of galaxies at 2.4 μm rest-frame wavelength, and the selection process of the sample is optimized for this purpose.

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Research Organization:: Lawrence Livermore National Laboratory (LLNL), Livermore, CA (United States)

Sponsoring Organization:: USDOE Office of Science (SC)

Grant/Contract Number:: AC52-07NA27344

OSTI ID:: 1545274

Journal Information:: The Astrophysical Journal (Online), Journal Name: The Astrophysical Journal (Online) Journal Issue: 1 Vol. 866; ISSN 1538-4357

Publisher:: Institute of Physics (IOP)Copyright Statement

Country of Publication:: United States

Language:: English

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