The K-Band Galaxy Luminosity Function

By C. Kochanek, M. Pahre, Emilio E. Falco, J. Huchra, J. Mader, Thomas H. Jarrett, T. Chester, R. Cutri, S. E. S. H. C. F. A. Processing, A. L. D. O. Astronomy and 1 more. 2000

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We measured the K-band luminosity function using a complete sample of 4192 morphologically typed 2MASS galaxies with μ = 20 mag arcsec-2 isophotal magnitudes 7 < K20 < 11.25 mag spread over 2.12 sr. Early-type (T ≤ -0.5) and late-type (T > -0.5) galaxies have similarly shaped luminosity functions, αe = -0.92 ± 0.10 and αl = -0.87 ± 0.09. The early-type galaxies are brighter, MK*e = -23.53 ± 0.06 mag compared to MK*l = -22.98 ± 0.06 mag, but less numerous, n*e = (0.45 ± 0.06) × 10-2 h3 Mpc-3 compared to n*l = (1.01 ± 0.13) × 10-2 h3 Mpc-3 for H0 = 100 h km s-1 Mpc-1, such that the late-type galaxies slightly dominate the K-band luminosity density, jlate/jearly = 1.17 ± 0.12. Including a factor of 1.20 ± 0.04 correction for the conversion of the isophotal survey magnitudes to total magnitudes, the local K-band luminosity density is j = (7.14 ± 0.75) × 108 h L☉ Mpc-3, which implies a stellar mass density relative to critical of Ω*h = (1.9 ± 0.2) × 10-3 for a Kennicutt initial mass function (IMF) and Ω*h = (3.4 ± 0.4) × 10-3 for a Salpeter IMF. Our morphological classifications are internally consistent, are consistent with previous classifications, and lead to luminosity functions unaffected by the estimated uncertainties in the classifications. These luminosity functions accurately predict the K-band number counts and redshift distributions for K ≲ 18 mag, beyond which the results depend on galaxy evolution and merger histories.

Subfields: Astronomy and Astrophysics

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Citations in the corpus

K-band Properties of Galaxy Clusters and Groups: Brightest Cluster Galaxies and Intracluster Light (2004, methodology): “We note that the observedN (Mh) relation is derived for galaxies brighter than MK ¼ 21; from the observed galaxy luminosity function (Kochanek et al. 2001) and the theoretical halo mass function (Sheth & Tormen 1999) we estimate the mass of such galaxies to be 1011M .”
The K20 survey - I. Disentangling old and dusty star-forming galaxies in the ERO population (2001, methodology): “%) is applied to the surface density of EROs derived by D00 in a much wider field (0.67 arcmin−2 over 450 arcmin2), or if the 2MASS K-band local luminosity function of early type galaxies is used (Kochanek et al. 2001), the lower limit becomes zf ∼ 2.”
Semianalytical Model of Galaxy Formation with High-Resolution N-Body Simulations (2004, methodology): “The smooth solid curve in this panel shows the result of the Schechter function fit obtained by Kochanek et al. (2001) from 2MASS.”
The Stellar Mass Assembly of Galaxies from z = 0 to z = 4: Analysis of a Sample Selected in the Rest-Frame Near-Infrared with Spitzer (2007, background): “2005, ApJ, 634, 137 Hughes, D. H. et al. 1998, Nature, 394, 241 Ilbert, O. et al. 2004, MNRAS, 351, 541 Im, M., Yamada, T., Tanaka, I., & Kajisawa, M. 2002, ApJ, 578, L19 Jimenez, R., Bernardi, M., Haiman, Z., Panter, B., & Heavens, A. F. 2007, ApJ, 669, 947 Juneau, S. et al. 2005, ApJ, 619, L135 Ka”
An Observational Determination of the Bolometric Quasar Luminosity Function (2006, background): “…estimates fromShankar et al. (2004) andMarconi et al. (2004) determined from local bulge velocity dispersion, mass, and luminosity function observations (Marzke et al. 1994; Kochanek et al. 2001; Cole et al. 2001; Nakamura et al. 2003; Blanton et al. 2003; Bernardi et al. 2003; Sheth et al. 2003).”
Quasars, their host galaxies and their central black holes (2001, background): “If instead Wisotzki et al. were to adopt the Kochanek et al. (2001) luminosity function then it is clear that (at least for the mass range probed by the present study) Wisotzki et al.’s analysis would also yield an activation fraction of 0.1%.”
Galaxy And Mass Assembly (GAMA): the galaxy stellar mass function at z < 0.06 (2011, methodology): “109L⊙ (Cole et al. 2001; Kochanek et al. 2001) or using UKIDSS with SDSS redshifts (Smith, Loveday, & Cross 2009); see fig 14. of Smith et al. for a compilation.”
DEMOGRAPHICS OF THE GALAXIES HOSTING SHORT-DURATION GAMMA-RAY BURSTS (2013, background): “…short GRB rate tracks stellar mass alone, the relative detection rates in early- and late-type galaxies should match the distribution of stellar mass, which is roughly equal atz ∼ 0 (Kochanek et al. 2001; Bell et al. 2003; Driver et al. 2007) and shows little evolution toz ∼ 1 (Ilbert et al. 2010).”
The evolution of the luminosity functions in the FORS Deep Field from low to high redshift: I. The blue bands (2004, background): “…Stoughton et al. 2002) and the 2MASS survey (Jarrett et al., 2000) have provided superb reference points for galaxy luminosity functions over a large wavelength range (see Norberg et al. 2002 for 2dFGRS, Blanton et al. 2001, 2003 for the SDSS, and Kochanek et al. 2001; Cole et al. 2001 for 2MASS).”
Fueling Low-Level AGN Activity through Stochastic Accretion of Cold Gas (2006, methodology): “Grouping the E and S0 galaxies as “early-type” and Sa/b, Sc/d, and Sm/Im galaxies as “late-type,” we compare these directly to theK-band luminosity functions of Kochanek et al. (2001), and find agreement (as the authors derive).”
The Non-Parametric Model for Linking Galaxy Luminosity with Halo/Subhalo Mass: Are First Brightest Galaxies Special? (2005, positive): “In this paper, we use mostly the K-band luminosity function from the 2MASS survey, with parameters given by α = −1.09, φ∗ = 1.16 × 10−2h3Mpc−3 and M∗ − 5logh = −23.39 (Kochanek et al. 2001).”
The K20 survey. V. The evolution of the near-IR Luminosity Function (2003, background): “…et al. 2000) surveys allowed accurate determinations of the local near-IR luminosity and of the Galaxy Stellar-mass functions (Cole et al. 2001; Kochanek et al. 2001), while only few attempts have been made to reconstruct their evolution with redshift using deep surveys of near-IR selected…”
Direct Cosmological Simulations of the Growth of Black Holes and Galaxies (2007, background): “The z ¼ 0 constraint is indicated by the dark gray area taken from the compilation of Marconi et al. (2004), which is based on a combination of different observational data (Kochanek et al. 2001; Nakamura et al. 2003; Bernardi et al. 2003; Sheth et al. 2003).”
Nearby supernova rates from the Lick Observatory Supernova Search – III. The rate–size relation, and the rates as a function of galaxy Hubble type and colour (2010, methodology): “Rates 15 nosity function and density published by Kochanek et al. (2001).”
The 400 Square Degree ROSAT PSPC Galaxy Cluster Survey: Catalog and Statistical Calibration (2006, neutral): “…et al. (2002); 31 — Binggeli et al. (1993); 32 — Falco et al. (1999); 33 — Hewitt & Burbidge (1991); 34 — Keel (1996); 35 — Huchra et al. (1990); 36 — Wegner et al. (1999); 37 — Miller et al. (2004); 38 — Owen et al. (1995); 39 — Kochanek et al. (2001); 40 — Gioia et al. (2003); 41 — da Costa et…”