The Luminosity Function of Morphologically Classified Galaxies in the Sloan Digital Sky Survey

By O. Nakamura, M. Fukugita, N. Yasuda, J. Loveday, J. Brinkmann, D. Schneider, K. Shimasaku, Mark SubbaRao. 2002

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The morphological dependence of the luminosity function is studied, using a sample containing approximately 1500 bright galaxies classified into Hubble types by visual inspection, for a homogeneous sample obtained from the Sloan Digital Sky Survey northern equatorial stripes. Early-type galaxies are shown to have a characteristic magnitude 0.45 mag brighter than that of spiral galaxies in the r* band, consistent with the "universal characteristic luminosity" in the B band. The shape of the luminosity function differs rather little among different morphological types: we do not see any symptoms of the sharp decline in the faint end of the luminosity function for early-type galaxies at least 2 mag fainter than the characteristic magnitude, although the faint-end behavior shows a slight decline (α ≲ -1) compared with the total sample. We also show that the rather flat faint-end slope for early-type galaxies is not due to an increasing mixture of dwarf galaxies, which have softer cores. This means that there are numerous faint early-type galaxies with highly concentrated cores.

Subfields: Astronomy and Astrophysics, Instrumentation

View Paper: https://www.semanticscholar.org/paper/638e14903ef9d731a3bcec6b69bf448e1bf5d4ca

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Citations in the corpus

THE IMPACT OF INTERACTIONS, BARS, BULGES, AND ACTIVE GALACTIC NUCLEI ON STAR FORMATION EFFICIENCY IN LOCAL MASSIVE GALAXIES (2012, result): “…populations, as reported by studies which compared this indicator to traditional visual morphologies, quantitative bulge/disk decompositions, and stellar population indicators (e.g. Strateva et al. 2001; Shimasaku et al. 2001; Nakamura et al. 2003; Weinmann et al. 2009; Kauffmann et al. 2003b).”
Galaxy luminosities, stellar masses, sizes, velocity dispersions as a function of morphological type (2009, methodology): “…galaxies, which are more centrally concentrated, are expected to have larger values of Cr, and two values are in common use: a more conservative Cr ≥ 2.86 (e.g. Nakamura et al. 2003; Shen et al. 2003) and a more cavalier Cr ≥ 2.6 (e.g. Strateva et al. 2001; Bell et al. 2003; Kauffmann et al. 2003).”
The Optical and Near-Infrared Properties of Galaxies. I. Luminosity and Stellar Mass Functions (2003, methodology): “A value of 85% was recently found by Nakamura et al. (2003) for bright SDSS galaxies (r ≤ 15.9) in the EDR: we adopt the difference between our and Nakamura et al.’s measurements as the systematic error in the completeness, which is propagated throughinto theφ∗ and j estimates later.”
The Recent and Continuing Assembly of Field Elliptical Galaxies by Red Mergers (2005, background): “Although greatly outnumbered by spiral galaxies, elliptical galaxies contain 20% of the stellar mass in the present-day universe (Fukugita et al. 1998) and dominate the high-mass end of the galaxy mass function (e.g., Nakamura et al. 2003).”
A CATALOG OF DETAILED VISUAL MORPHOLOGICAL CLASSIFICATIONS FOR 14,034 GALAXIES IN THE SLOAN DIGITAL SKY SURVEY (2010, methodology): “For example, Shen et al. (2003) use aR90/R50 concentration cut of 2.86 as defined by Nakamura et al. (2003) to distinguish between early type and late type galaxies.”
The Cosmic Energy Inventory (2004, background): “The observed rates of Type Ia supernovae in morphologically separated galaxies seem to be proportional to the r band luminosity density; the luminosity density in E/S0 galaxies is 31% of the total (Nakamura et al. 2003).”
Quantifying the Bimodal Color-Magnitude Distribution of Galaxies (2003, background): “However, the equivalent steepening of the faintend slope toward late types based on morphological classification appears less significant (Nakamura et al. 2003).”
Local supermassive black holes, relics of active galactic nuclei and the X-ray background (2003, methodology): “• Nakamura et al. 2003: we use the luminosity function in the SDSS r⋆ band and we apply the color correction K = r⋆ − (2.8 ± 0.2) described previously and the Bulge-Total corrections of Tab.”
Internal and Collective Properties of Galaxies in the Sloan Digital Sky Survey (2006, methodology): “Nakamura et al. (2003) studied the dependence of the luminosity function on galaxy morphology and the correlation between galaxy morphology and other photometric properties such as color and concentration index using a sample of SDSS galaxies with visually identified morphological types.”
Fueling Low-Level AGN Activity through Stochastic Accretion of Cold Gas (2006, background): “…0.02), and all types (black solid) are shown, and compared to the 1σ range of the inferred mass function from Marconi et al. (2004), based on the observations of Marzke et al. (1994a); Kochanek et al. (2001); Nakamura et al. (2003); Bernardi et al. (2003); Sheth et al. (2003) (yellow shaded range).”
Morphology Segregation of Galaxies in Color-Color Gradient Space (2005, methodology): “The second training set is a catalog by Fukugita et al. (2006, in preparation; see also Nakamura et al. 2003) listing 1875 galaxies with (after Galactic extinction correction), with∗r ≤ 15.9pet visually identified morphological types from to 6 in 0.5T p 0 steps.”
The size distribution of galaxies in the Sloan Digital Sky Survey (2003, methodology): “The luminosity function has been derived by Blanton et al. (2001, 2003c) and the dependence of luminosity function on galaxy type has been analysed by Nakamura et al. (2003).”
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).”
Environmental effects on satellite galaxies: the link between concentration, size and colour profile (2008, unknown): “As shown by Strateva (2001), Nakamura et al. (2003) and Shimasaku et al. (2001), concentration can be used to roughly distinguish between early type and late type galaxies, at least for the relative massive and luminous galaxies we use in this study.”
A Unified, Merger-driven Model of the Origin of Starbursts, Quasars, the Cosmic X-Ray Background, Supermassive Black Holes, and Galaxy Spheroids (2005, background): “The observations shown are again from Marconi et al. (2004), based on the combination of the observations of Marzke et al. (1994); Kochanek et al. (2001); Nakamura et al. (2003); Bernardi et al. (2003); Sheth et al. (2003).”
The fundamental properties of galaxies and a new galaxy classification system (2006, result): “Our densities however generally agree well with the densities derived from the morphological-type specific Schechter functions published in Marzke et al. (1998) and Nakamura et al. (2003).”
Galaxy Zoo: the fraction of merging galaxies in the SDSS and their morphologies (2009, background): “Nakamura et al. (2003) visually classified 2418 images of SDSS galaxy objects with Petrosian r < 16.0 (i.e. low redshift) finding that 35/1875 of their morphological classifi- 2 “Men trust their ears less than their eyes.””