2001/04/17 by Michael L. Balogh, Michael Balogh, Daniel Christlein +3 · 4 citations
Engineering · Physics and Astronomy · #Astronomy and Astrophysical Research #Emission spectrum #Galaxies: Formation, Evolution, Phenomena #Galaxy #Infrared #Luminosity #Luminosity function #Luminous infrared galaxy #Photometry (optics) #Redshift #Sky #Space Technology and Applications #Stellar mass #astro-ph
paper · pdf · doi:10.1086/321670
14 pages, 13 figures, emulateapj style ApJ, post-referee. Very minor changes, mostly typographical in nature
arxiv created 2001/04/17 · openalex publication_date 2001/08/10 · arxiv updated 2009/12/01 · openalex created_date 2016/06/24 · openalex updated_date 2026/08/05
We investigate the dependence of the galaxy infrared luminosity function (LF) and the associated stellar mass function (SMF) on environment and spectral type using photometry from the Two Micron All Sky Survey and redshifts from the Las Campanas Redshift Survey for galaxies brighter than M J < -19 + 5 log h . In the field environment, the LFs of galaxies with emission lines have much steeper faint-end slopes (α J = -1.39) than those of galaxies without emission lines (α J = -0.59). In the cluster environment, however, even the non-emission-line galaxies have a steep faint-end LF (α J = -1.22). There is also a significant (95%) difference between the overall cluster and field LFs, Δα J = -0.34 and Δ M * J = -0.54. All these variations are more pronounced in the SMFs, which we compute by relating the strength of the 4000 Å break in the optical spectra to a stellar mass-to-light ratio.