The Evolution of the Field and Cluster Morphology-Density Relation for Mass-Selected Samples of Galaxies

The Sloan Digital Sky Survey (SDSS) and photometric/spectroscopic surveys in the GOODS-South field (the Chandra Deep Field-South, CDF-S) are used to construct volume-limited, stellar-mass-selected samples of galaxies at redshifts 0 < z < 1. The CDF-S sample at 0.6 < z < 1.0 contains 207 galaxies complete down to M = 4 × 1010 M☉ (for a "diet" Salpeter initial mass function), corresponding to a luminosity limit for red galaxies of MB = -20.1. The SDSS sample at 0.020 < z < 0.045 contains 2003 galaxies down to the same mass limit, which corresponds to MB = -19.3 for red galaxies. Morphologies are determined with an automated method, using the Sérsic parameter n and a measure of the residual from the model fits, called "bumpiness," to distinguish different morphologies. These classifications are verified with visual classifications. In agreement with previous studies, 65%-70% of the galaxies are located on the red sequence, both at z ~ 0.03 and at z ~ 0.8. Similarly, 65%-70% of the galaxies have n > 2.5. The fraction of E + S0 galaxies is 43% ± 3% at z ~ 0.03 and 48% ± 7% at z ~ 0.8; i.e., it has not changed significantly since z ~ 0.8. When combined with recent results for cluster galaxies in the same redshift range, we find that the morphology-density relation for galaxies more massive than 0.5M* has remained constant since at least z ~ 0.8. This implies that galaxies evolve in mass, morphology, and density such that the morphology-density relation does not change. In particular, the decline of star formation activity and the accompanying increase in the stellar mass density of red galaxies since z ~ 1 must happen without large changes in the early-type galaxy fraction in a given environment.

[1]  P. S. Bunclark,et al.  Astronomical Data Analysis Software and Systems , 2008 .

[2]  M. Raddick,et al.  The Fifth Data Release of the Sloan Digital Sky Survey , 2007, 0707.3380.

[3]  M. Postman,et al.  Mass Selection and the Evolution of the Morphology-Density Relation from z = 0.8 to 0 , 2007, 0707.2782.

[4]  G. Illingworth,et al.  Low Star Formation Rates for z = 1 Early-Type Galaxies in the Very Deep GOODS MIPS Imaging: Implications for Their Optical/Near-Infrared Spectral Energy Distributions , 2007, 0705.3394.

[5]  K. Sheth,et al.  The Effects of Environment on Morphological Evolution at 0 < z < 1.2 in the COSMOS Survey , 2007 .

[6]  P. Rosati,et al.  The Rest-Frame K-Band Luminosity Function of Galaxies in Clusters to z = 1.3 , 2007, astro-ph/0702050.

[7]  P. McCarthy,et al.  The Gemini Deep Deep Survey. VIII. When Did Early-Type Galaxies Form? , 2007, astro-ph/0701779.

[8]  R. Pelló,et al.  The Morphological Content of 10 EDisCS Clusters at 0.5 < z < 0.8 , 2007, astro-ph/0701788.

[9]  B. Weiner,et al.  The Stellar Mass Tully-Fisher Relation to z = 1.2 from AEGIS , 2006, astro-ph/0702643.

[10]  G. Kauffmann,et al.  How special are Brightest Group and Cluster Galaxies , 2006, astro-ph/0611196.

[11]  R. Pelló,et al.  The build-up of the colour-magnitude relation in galaxy clusters since z ~ 0.8 , 2006, astro-ph/0610373.

[12]  M. Brodwin,et al.  The Evolving Luminosity Function of Red Galaxies , 2006, astro-ph/0609584.

[13]  P. Dokkum,et al.  The Star Formation Epoch of the Most Massive Early-Type Galaxies , 2006, astro-ph/0609587.

[14]  P. P. van der Werf,et al.  What Do We Learn from IRAC Observations of Galaxies at 2 < z < 3.5? , 2006, astro-ph/0609548.

[15]  H. Rix,et al.  Comparing Dynamical and Photometric Mass Estimates of Low- and High-Redshift Galaxies: Random and Systematic Uncertainties , 2006, astro-ph/0607649.

[16]  S. Bamford,et al.  Galaxy bimodality versus stellar mass and environment , 2006, astro-ph/0607648.

[17]  Tod R. Lauer,et al.  The Masses of Nuclear Black Holes in Luminous Elliptical Galaxies and Implications for the Space Density of the Most Massive Black Holes , 2006, astro-ph/0606739.

[18]  M. Postman,et al.  The Possible z = 0.83 Precursors of z = 0, M* Early-Type Cluster Galaxies , 2006, astro-ph/0603839.

[19]  R. Bouwens,et al.  Clusters at Half Hubble Time: Galaxy Structure and Colors in RX J0152.7–1357 and MS 1054–03 , 2006, astro-ph/0603058.

[20]  UCOLick,et al.  Submitted to ApJ Preprint typeset using L ATEX style emulateapj v. 6/22/04 THE MASS ASSEMBLY HISTORY OF FIELD GALAXIES: DETECTION OF AN EVOLVING MASS LIMIT FOR STAR FORMING GALAXIES , 2005 .

[21]  H. Rix,et al.  Detecting Faint Galaxies by Stacking at 24 μm , 2005, astro-ph/0512203.

[22]  S. Okamura,et al.  The Build-up of the Colour-Magnitude Relation , 2005, Proceedings of the International Astronomical Union.

[23]  Tucson,et al.  Infrared Luminosity Functions from the Chandra Deep Field-South: The Spitzer View on the History of Dusty Star Formation at 0 ≲ z ≲ 1* , 2005, astro-ph/0506462.

[24]  A. Szalay,et al.  Galaxy Luminosity Functions to z~1 from DEEP2 and COMBO-17: Implications for Red Galaxy Formation , 2005, astro-ph/0506044.

[25]  Christopher D. Martin,et al.  Spitzer View on the Evolution of Star-forming Galaxies from z = 0 to z ~ 3 , 2005, astro-ph/0505101.

[26]  A. Fontana,et al.  The K20 survey. VII. The spectroscopic catalogue: spectral properties and evolution of the galaxy population ⋆, ⋆⋆ , 2005, astro-ph/0504248.

[27]  R. S. Ellis,et al.  The Assembly History of Field Spheroidals: Evolution of Mass-to-Light Ratios and Signatures of Recent Star Formation , 2005, astro-ph/0503164.

[28]  H. Rix,et al.  Toward an Understanding of the Rapid Decline of the Cosmic Star Formation Rate , 2005, astro-ph/0502246.

[29]  H. Rix,et al.  Mass-to-Light Ratios of Field Early-Type Galaxies at z ~ 1 from Ultradeep Spectroscopy: Evidence for Mass-dependent Evolution , 2005, astro-ph/0502228.

[30]  C. Conselice,et al.  The Mass Assembly Histories of Galaxies of Various Morphologies in the GOODS Fields , 2005, astro-ph/0502204.

[31]  R. Bouwens,et al.  The Morphology-Density Relation in z ~ 1 Clusters , 2005, astro-ph/0501224.

[32]  I. Hook,et al.  Cosmic Star Formation History and Its Dependence on Galaxy Stellar Mass , 2004, astro-ph/0411775.

[33]  J. Brinkmann,et al.  The Properties and Luminosity Function of Extremely Low Luminosity Galaxies , 2004, astro-ph/0410164.

[34]  Paul S. Smith,et al.  The Multiband Imaging Photometer for Spitzer (MIPS) , 2004 .

[35]  Gary J. Melnick,et al.  In-flight performance and calibration of the Infrared Array Camera (IRAC) for the Spitzer Space Telescope , 2004, SPIE Astronomical Telescopes + Instrumentation.

[36]  T. Treu,et al.  Evolution since z = 1 of the Morphology-Density Relation for Galaxies , 2004, astro-ph/0403455.

[37]  J. Brinkmann,et al.  The environmental dependence of the relations between stellar mass, structure, star formation and nuclear activity in galaxies , 2004, astro-ph/0402030.

[38]  Chisato Yamauchi,et al.  The morphology–density relation in the Sloan Digital Sky Survey , 2003, astro-ph/0312043.

[39]  P. Madau,et al.  A New Nonparametric Approach to Galaxy Morphological Classification , 2003, astro-ph/0311352.

[40]  J. Brinkmann,et al.  The physical properties of star-forming galaxies in the low-redshift universe , 2003, astro-ph/0311060.

[41]  J. Brinkmann,et al.  Relationship between Environment and the Broadband Optical Properties of Galaxies in the Sloan Digital Sky Survey , 2003, astro-ph/0310453.

[42]  G. Bruzual,et al.  Stellar population synthesis at the resolution of 2003 , 2003, astro-ph/0309134.

[43]  R. Nichol,et al.  Early-Type Galaxies in the Sloan Digital Sky Survey. I. The Sample , 2003 .

[44]  Heidelberg,et al.  Nearly 5000 Distant Early-Type Galaxies in COMBO-17: A Red Sequence and Its Evolution since z ~ 1 , 2003, astro-ph/0303394.

[45]  J. Kneib,et al.  A Wide-Field Hubble Space Telescope Study of the Cluster Cl 0024+16 at z = 0.4. I. Morphological Distributions to 5 Mpc Radius , 2003, astro-ph/0303267.

[46]  C. Conselice The Relationship between Stellar Light Distributions of Galaxies and Their Formation Histories , 2003, astro-ph/0303065.

[47]  E. Bell,et al.  The Optical and Near-Infrared Properties of Galaxies. I. Luminosity and Stellar Mass Functions , 2003, astro-ph/0302543.

[48]  University of Toronto,et al.  A New Approach to Galaxy Morphology. I. Analysis of the Sloan Digital Sky Survey Early Data Release , 2003, astro-ph/0301239.

[49]  D. York,et al.  The Overdensities of Galaxy Environments as a Function of Luminosity and Color , 2002, astro-ph/0212085.

[50]  Oxford,et al.  The COMBO-17 survey: Evolution of the galaxy luminosity function from 25,000 galaxies with 0.2 < z < 1.2 , 2002, astro-ph/0208345.

[51]  V. Narayanan,et al.  Spectroscopic Target Selection in the Sloan Digital Sky Survey: The Main Galaxy Sample , 2002, astro-ph/0206225.

[52]  Mamoru Doi,et al.  Estimating Fixed-Frame Galaxy Magnitudes in the Sloan Digital Sky Survey , 2002, astro-ph/0205243.

[53]  L. Ho,et al.  Detailed Structural Decomposition of Galaxy Images , 2002, astro-ph/0204182.

[54]  R. Nichol,et al.  Stellar masses and star formation histories for 105 galaxies from the Sloan Digital Sky Survey , 2002, astro-ph/0204055.

[55]  V. Narayanan,et al.  Color Separation of Galaxy Types in the Sloan Digital Sky Survey Imaging Data , 2001, astro-ph/0107201.

[56]  D. Elbaz,et al.  Interpreting the Cosmic Infrared Background: Constraints on the Evolution of the Dust-enshrouded Star Formation Rate , 2001, astro-ph/0103067.

[57]  Walter A. Siegmund,et al.  The Sloan Digital Sky Survey: Technical Summary , 2000, astro-ph/0006396.

[58]  M. Bershady,et al.  The Asymmetry of Galaxies: Physical Morphology for Nearby and High-Redshift Galaxies , 1999, astro-ph/9907399.

[59]  Jr.,et al.  STAR FORMATION IN GALAXIES ALONG THE HUBBLE SEQUENCE , 1998, astro-ph/9807187.

[60]  Jr.,et al.  Evolution since z = 0.5 of the Morphology-Density Relation for Clusters of Galaxies , 1997, astro-ph/9707232.

[61]  A. Fruchter,et al.  HIGH-REDSHIFT GALAXIES IN THE HUBBLE DEEP FIELD : COLOUR SELECTION AND STAR FORMATION HISTORY TO Z 4 , 1996, astro-ph/9607172.

[62]  E. Bertin,et al.  SExtractor: Software for source extraction , 1996 .

[63]  I. Jørgensen,et al.  The Fundamental Plane for cluster E and S0 galaxies , 1995, astro-ph/9511139.

[64]  A. Dressler Galaxy morphology in rich clusters: Implications for the formation and evolution of galaxies , 1980 .