scholarly journals The Faint End of the Galaxy Luminosity Function in Rich Clusters

1999 ◽  
Vol 171 ◽  
pp. 60-67
Author(s):  
R.M. Smith ◽  
S. Phillips ◽  
S.P. Driver ◽  
W.J. Couch
Keyword(s):  
Surface Brightness ◽  
Luminosity Function ◽  
Large Population ◽  
Low Surface Brightness ◽  
The Galaxy ◽  
Low Surface Brightness Galaxies ◽  
Galaxy Luminosity Function

AbstractRecent results on the determination of the shape of the faint end of the galaxy luminosity function in rich clusters are discussed. There is increasing evidence that in many cases the faint end of the function is steep, indicating a large population of dwarf, possibly low surface-brightness, galaxies. In addition, the magnitude at which the turn-up appears is approximately constant with richness and distance. However, it is clear that not all clusters show such a feature.

scholarly journals Low Luminosity Galaxies in Large Surveys

1999 ◽  
Vol 171 ◽  
pp. 45-51
Author(s):  
John P. Huchra
Keyword(s):  
Surface Brightness ◽  
Luminosity Function ◽  
Morphological Type ◽  
Large Excess ◽  
Redshift Surveys ◽  
Low Surface Brightness ◽  
The Galaxy ◽  
Emission Line Galaxies ◽  
Low Surface Brightness Galaxies ◽  
Galaxy Luminosity Function

AbstractThe debate about the slope and amplitude of the galaxy luminosity function at the faint end is discussed w.r.t. faint galaxies in large surveys, in particular the second CfA (CfA2) and the Las Campanas (LCRS) redshift surveys. Large surveys are necessary to determine the statistics of rare objects or objects that can only be seen out to limited volumes. Both surveys show excesses of faint galaxies over Schechter function fits, but the parent sample for the LCRS survey generally does not contain large or low surface brightness galaxies which do appear in the CfA2 survey. The objects that comprise the relatively large excess of faint galaxies in the CfA2 survey are shown to be primarily of low surface brightness and late morphological type and are generally emission line galaxies. Galaxy samples constructed like the LCRS will generally always be deficient in low luminosity galaxies and thus are not useful for constraining the faint end of the 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 Securing the Faint End of the Galaxy Luminosity Function

2004 ◽  
Vol 21 (4) ◽  
pp. 356-359 ◽  
Author(s):  
Helmut Jerjen ◽  
Brent Tully ◽  
Neil Trentham
Keyword(s):  
Surface Brightness ◽  
Luminosity Function ◽  
Dwarf Galaxy ◽  
Full Range ◽  
Mass Function ◽  
Wide Field ◽  
Distance Information ◽  
The Galaxy ◽  
Brightness Fluctuation ◽  
Galaxy Luminosity Function

AbstractThe history of the formation of galaxies must leave an imprint in the properties of the mass function of collapsed objects and in its observational manifestation, the galaxy luminosity function. At present the faint end of the luminosity function is poorly known. Accurate knowledge of the luminosity function over the full range of galaxy clustering scales would provide serious constraints on both initial cosmological conditions and modulating astrophysical processes.Wide field imaging surveys with large ground-based telescopes now provide the capability to identify dwarf galaxy candidates to very faint levels (μR ≈ 26 mag arcsec–2), too low in surface brightness for spectroscopy (measuring redshifts) even with telescopes like Keck. Other means have to be explored to get distance information for these candidates in order to separate cluster members from back/foreground systems beyond doubt. On the quest to establish the properties (slope and possible turning point) of the the faint end of the galaxy luminosity function we are employing the surface brightness fluctuation (SBF) method to determine adequate distances, potentially resulting in the best definition ever of the luminosity function to MR ≈ –11 in the cluster and group environments.

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 A Robust Technique for Estimating Cosmological Parameters

2005 ◽  
Vol 201 ◽  
pp. 467-468
Author(s):  
Martin A. Hendry ◽  
Stéphane Rauzy
Keyword(s):  
Luminosity Function ◽  
Spatial Clustering ◽  
Cosmological Parameters ◽  
Bias Parameter ◽  
Galaxy Surveys ◽  
The Galaxy ◽  
Distance Data ◽  
Galaxy Luminosity Function

We present a new ROBUST technique for extracting information from galaxy surveys which allows determination of cosmological parameters free of almost any model assumptions concerning the galaxy luminosity function and spatial clustering. We illustrate ROBUST by estimating H0 and the linear bias parameter, β, from recent redshift-distance data.

scholarly journals Radio Observations of the AGN and Gas in Low Surface Brightness Galaxies

2006 ◽  
Vol 2 (S235) ◽  
pp. 90-90
Author(s):  
M. Das ◽  
K. O'Neil ◽  
N. Kantharia ◽  
S. N. Vogel ◽  
S. S. McGaugh
Keyword(s):  
Surface Brightness ◽  
Continuum Emission ◽  
Molecular Gas ◽  
Gas Distribution ◽  
Continuum Source ◽  
Low Surface Brightness ◽  
The Galaxy ◽  
Low Surface Brightness Galaxies ◽  
Lsb Galaxies ◽  
The Continuum

AbstractLSB galaxies have low metallicities, diffuse stellar disks, and massive HI disks. We have detected molecular gas in two giant LSB galaxies, UGC 6614 and F568-6. A millimeter continuum source has been detected in UGC 6614 as well. At centimeter wavelengths we have detected and mapped the continuum emission from the giant LSB galaxy 1300+0144. The emission is extended about the nucleus and is most likely originating from the AGN in the galaxy. The HI gas distribution and velocity field in 1300+0144 was also mapped. The HI disk extends well beyond the optical disk and appears lopsided in the intensity maps.

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