PHOTOMETRIC PROPERTIES AND LUMINOSITY FUNCTION OF NEARBY MASSIVE EARLY-TYPE GALAXIES

• Published in: The Astrophysical journal Vol. 773; no. 1; pp. 1 - 12
• Main Authors: He, Y Q, Xia, X Y, Hao, C N, Jing, Y P, Mao, S, Li, Cheng
• Format: Journal Article
• Language: English
• Published: United States 10.08.2013
• Subjects: ALGORITHMS; Assembly; ASTROPHYSICS, COSMOLOGY AND ASTRONOMY; BRIGHTNESS; CLASSIFICATION; DENSITY; FORECASTING; GALAXIES; LUMINOSITY; MASS; Mathematical models; PHOTOMETRY; RED SHIFT; Sky surveys (astronomy); VISIBLE RADIATION
• ISSN: 0004-637X; 1538-4357
• DOI: 10.1088/0004-637X/773/1/37

We perform photometric analyses of a bright early-type galaxy sample with 2949 galaxies (M sub(r) < -22.5 mag) in the redshift range of 0.05-0.15, drawn from the Sloan Digital Sky Survey (SDSS) DR7 with morphological classification from Galaxy Zoo 1. We measure the Petrosian and isophotal magnitudes, as well as the corresponding half-light radius for each galaxy. We find that for the brightest galaxies (M sub(r) < -23 mag), our Petrosian magnitudes and isophotal magnitudes to 25 mag arcsec super(-2) and 1 % of the sky brightness are on average 0.16 mag, 0.20 mag, and 0.26 mag brighter than the SDSS Petrosian values, respectively. In the first case, the underestimations are caused by overestimations in the sky background by the SDSS PHOTO algorithm, while the latter two are also due to deeper photometry. Similarly, the typical half-light radii (r sub(50)) measured by the SDSS algorithm are smaller than our measurements. As a result, the bright end of the r-band luminosity function is found to decline more slowly than previous works. Our measured luminosity densities at the bright end are more than one order of magnitude higher than those of Blanton et ah, and the stellar mass densities at M sub(*) ~ 5 x 10 super(11) M sub([middot in circle]) and M sub(*) ~ 10 super(12) M sub([middot in circle]) are a few tenths and a factor of a few higher than those of Bernardi et al. These results may significantly alleviate the tension in the assembly of massive galaxies between observations and predictions of the hierarchical structure formation model.