scholarly journals Luminosity Functions from the 2dF Galaxy Redshift Survey

2004 ◽  
Vol 21 (4) ◽  
pp. 352-355 ◽  
Author(s):  
Matthew Colless
Keyword(s):  
Spectral Type ◽  
Surface Brightness ◽  
Luminosity Function ◽  
Local Density ◽  
Luminosity Functions ◽  
The Galaxy ◽  
Redshift Survey ◽  
Galaxy Redshift ◽  
Galaxy Luminosity Function

AbstractA summary of the main results from the 2dF Galaxy Redshift Survey of over 221 000 galaxies on the galaxy luminosity function and its dependence on surface brightness, spectral type, environment, and local density.

scholarly journals The Deep Evolutionary Exploratory Probe 2 Galaxy Redshift Survey: The Galaxy Luminosity Function toz ∼ 1

2006 ◽  
Vol 647 (2) ◽  
pp. 853-873 ◽  
Author(s):  
C. N. A. Willmer ◽  
S. M. Faber ◽  
D. C. Koo ◽  
B. J. Weiner ◽  
J. A. Newman ◽  
...  
Keyword(s):  
Luminosity Function ◽  
The Galaxy ◽  
Redshift Survey ◽  
Galaxy Redshift ◽  
Galaxy Luminosity Function

scholarly journals Low Surface Brightness Galaxies and the Field Galaxy Luminosity Function

1996 ◽  
Vol 171 ◽  
pp. 446-446 ◽  
Author(s):  
D. Sprayberry ◽  
C. D. Impey ◽  
G. D. Bothun ◽  
M. J. Irwin
Keyword(s):  
Surface Brightness ◽  
Luminosity Function ◽  
Substantial Fraction ◽  
Low Surface Brightness ◽  
Blue Galaxies ◽  
Best Fitting ◽  
Redshift Survey ◽  
Low Surface Brightness Galaxies ◽  
Galaxy Luminosity Function ◽  
Field Galaxy

We have developed a catalog of local low surface brightness galaxies (LSBGs) which is selected by objective criteria. We present here a luminosity function (LF) for LSBGs based on that catalog. This LF includes the effects of the completeness corrections to the LSBG catalog, and includes only galaxies with surface brightnesses (22.25 ≤ μB(0) ≤ 24.5) fainter than those included in the CfA Redshift Survey (see Marzke et al. 1994, AJ 108, 437). The best-fitting Schechter function has parameters α = –1.42, M∗B = −18.34, and Φ∗ = 0.0036 h3 Mpc–3 mag–1. Thus, surveys which do not take account of the observational selection bias imposed by surface brightness are missing a substantial fraction of the local galaxies, but, this missed fraction is not large enough to explain the counts of faint blue galaxies observed at moderate redshift.

scholarly journals Beyond the Galaxy Luminosity Function

2004 ◽  
Vol 21 (4) ◽  
pp. 344-351 ◽  
Author(s):  
Simon Driver
Keyword(s):  
Surface Brightness ◽  
Luminosity Function ◽  
Large Scale ◽  
Evolutionary Processes ◽  
Multivariate Distributions ◽  
Independent Investigation ◽  
Current State ◽  
The Galaxy ◽  
Galaxy Population ◽  
Galaxy Luminosity Function

AbstractWith the advent of large-scale surveys (i.e. Legacy Surveys) it is now possible to start looking beyond the galaxy luminosity function (LF) to more detailed statistical representations of the galaxy population, i.e multivariate distributions. In this review I first summarise the current state-of-play of the B-band global and cluster LFs and then briefly present two promising bivariate distributions: the luminosity–surface brightness plane (LSP) and the colour–luminosity plane (CLP). In both planes galaxy bulges and galaxy disks form marginally overlapping but distinct distributions, indicating two key formation/evolutionary processes (presumably merger and accretion). Forward progress in this subject now requires the routine application of reliable bulge–disk decomposition codes to allow independent investigation of these two key components.

scholarly journals The Local Density and Morphology Dependence of the Galaxy Luminosity Function

1987 ◽  
Vol 127 ◽  
pp. 457-457
Author(s):  
Jacek Choloniewski ◽  
Miroslaw Panek
Keyword(s):  
Galaxy Formation ◽  
Luminosity Function ◽  
Local Density ◽  
Elliptical Galaxies ◽  
Low Density ◽  
Early Type ◽  
The Galaxy ◽  
The Moment ◽  
Galaxy Luminosity Function ◽  
Selection Of

We obtained the luminosity function (LF) for samples of galaxies from the CfA North catalogue (Huchra, Davis, Latham and Tonry, 1983). the criteria of selection of samples were the local density (range—more than 2 orders of magnitude) and/or the morphology. No difference in the combined LF for all morphological types is found for subsamples of different density. the LF of elliptical galaxies is found to be less steep at the faint end than the LFs for S and SO galaxies. E galaxies are on the average brighter than the other morphological types. the LFs measured for early–type galaxies (E + S0) in high and low density regions show marginal difference—the low density LF has a steeper faint end slope. (Such a difference is not found for S galaxies). If this feature is maintained for larger samples it may indicate that the LF determined at the moment of galaxy formation is only weakly influenced by the phenomena present in dense regions. This is because these phenomena would rather leave the opposite imprint on the LF—the tidal stripping in dense regions would populate them with faint remnants of disrupted, bright, low angular momentum galaxies. Mergers could not reverse this trend because they act mainly on the bright galaxies.

scholarly journals Autofib Redshift Survey -- I. Evolution of the galaxy luminosity function

1996 ◽  
Vol 280 (1) ◽  
pp. 235-251 ◽  
Author(s):  
R. S. Ellis ◽  
M. Colless ◽  
T. Broadhurst ◽  
J. Heyl ◽  
K. Glazebrook
Keyword(s):  
Luminosity Function ◽  
The Galaxy ◽  
Redshift Survey ◽  
Galaxy Luminosity Function

scholarly journals The faint-end of galaxy luminosity functions at the Epoch of Reionization

2017 ◽  
Vol 12 (S333) ◽  
pp. 52-55
Author(s):  
B. Yue ◽  
M. Castellano ◽  
A. Ferrara ◽  
A. Fontana ◽  
E. Merlin ◽  
...  
Keyword(s):  
Star Formation ◽  
Formation Process ◽  
Luminosity Function ◽  
Feedback Effects ◽  
Circular Velocity ◽  
Luminosity Functions ◽  
The Galaxy ◽  
Turn Over ◽  
Number Counts ◽  
Galaxy Luminosity Function

AbstractDuring the Epoch of Reionization (EoR), feedback effects reduce the efficiency of star formation process in small halos or even fully quench it. The galaxy luminosity function (LF) may then turn over at the faint-end. We analyze the number counts of z > 5 galaxies observed in the fields of four Frontier Fields (FFs) clusters and obtain constraints on the LF faint-end: for the turn-over magnitude at z ∼ 6, MUVT ≳-13.3; for the circular velocity threshold of quenching star formation process, vc* ≲ 47 km s−1. We have not yet found significant evidence of the presence of feedback effects suppressing the star formation in small galaxies.

scholarly journals The Canada-France Redshift Survey. VI. Evolution of the Galaxy Luminosity Function to Z approximately 1

1995 ◽  
Vol 455 ◽  
pp. 108 ◽  
Author(s):  
S. J. Lilly ◽  
L. Tresse ◽  
F. Hammer ◽  
David Crampton ◽  
O. Le Fevre
Keyword(s):  
Luminosity Function ◽  
The Galaxy ◽  
Redshift Survey ◽  
Galaxy Luminosity Function
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