scholarly journals Binary Aggregations in Hierarchical Galaxy Formation: The Evolution of the Galaxy Luminosity Function

2002 ◽  
Vol 575 (1) ◽  
pp. 18-32 ◽  
Author(s):  
N. Menci ◽  
A. Cavaliere ◽  
A. Fontana ◽  
E. Giallongo ◽  
F. Poli
Keyword(s):  
Galaxy Formation ◽  
Luminosity Function ◽  
The Galaxy ◽  
Galaxy Luminosity Function

DARK MATTER IN SPIRAL HALOS AND THE HALO MASS FUNCTION

1994 ◽  
Vol 03 (supp01) ◽  
pp. 87-92
Author(s):  
KEITH M. ASHMAN ◽  
PAOLO SALUCCI ◽  
MASSIMO PERSIC
Keyword(s):  
Dark Matter ◽  
Hierarchical Clustering ◽  
Galaxy Formation ◽  
Luminosity Function ◽  
Mass Function ◽  
Dark Halo ◽  
Constant Mass ◽  
High Luminosity ◽  
The Galaxy ◽  
Galaxy Luminosity Function

Evidence that low-luminosity spirals have a higher dark matter fraction than their high-luminosity counterparts is discussed. The empirical correlation between dark matter fraction and luminosity is used, in conjunction with the galaxy luminosity function of spirals, to derive the dark halo mass function of these galaxies. The mass function is shown to be consistent with hierarchical clustering models of galaxy formation. This contrasts with previous results based on the assumption of a constant mass-to-light ratio for all spirals, which predict too many low-luminosity galaxies.

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.

The Faint End of the Galaxy Luminosity Function in Abell 426 and 539

1998 ◽  
Vol 116 (3) ◽  
pp. 1118-1124 ◽  
Author(s):  
Roberto De Propris ◽  
Christopher J. Pritchet
Keyword(s):  
Luminosity Function ◽  
The Galaxy ◽  
Galaxy Luminosity Function

scholarly journals The faint end of the galaxy luminosity function in moderate-redshift clusters

1997 ◽  
Vol 284 (4) ◽  
pp. 915-930 ◽  
Author(s):  
G. Wilson ◽  
I. Smail ◽  
R. S. Ellis ◽  
J. C. Warrick
Keyword(s):  
Luminosity Function ◽  
The Galaxy ◽  
Galaxy Luminosity Function

scholarly journals The galaxy luminosity function and its evolution withChandra

2008 ◽  
Vol 480 (3) ◽  
pp. 663-670 ◽  
Author(s):  
P. Tzanavaris ◽  
I. Georgantopoulos
Keyword(s):  
Luminosity Function ◽  
The Galaxy ◽  
Galaxy Luminosity Function

scholarly journals Galaxy Counts

1984 ◽  
Vol 78 ◽  
pp. 489-498
Author(s):  
J.A. Tyson
Keyword(s):  
Luminosity Function ◽  
Automated Detection ◽  
Color Evolution ◽  
Faint Galaxy ◽  
New Information ◽  
The Galaxy ◽  
Color Data ◽  
Photographic Survey ◽  
Galaxy Luminosity Function

AbstractCounts of faint galaxies should reveal any evidence of galaxy luminosity or color evolution, as well as new information on the faint end of the galaxy luminosity function. The FOCAS automated detection and classification software is reviewed, and results of the deep 4m PF photographic survey to 24th magnitude in 23 fields covering 9 sq. degrees are presented. Color-magnitude plots for stars and galaxies are shown, and galaxy color evolution is discussed. Evidence is found for a faint galaxy blue trend at 22-24 J mag. However, the k-correction becomes so severe at redshift ~1 that the intrinsically fainter galaxies are emphasized in any magnitude-limited survey. No unambiguous evidence is found for evolution. New 4m limit CCD multi-color data are shown and discussed. The limiting magnitude for detection is 27th J magnitude in 2 hours integration. The data exclude evolution starting at any one epoch for z<10.

scholarly journals The galaxy–halo connection in modified gravity cosmologies: environment dependence of galaxy luminosity function

2019 ◽  
Vol 488 (1) ◽  
pp. 782-802 ◽  
Author(s):  
N Chandrachani Devi ◽  
Aldo Rodríguez-Puebla ◽  
O Valenzuela ◽  
Vladimir Avila-Reese ◽  
César Hernández-Aguayo ◽  
...  
Keyword(s):  
Modified Gravity ◽  
Luminosity Function ◽  
Cold Dark Matter ◽  
Density Field ◽  
High Density ◽  
Gravity Models ◽  
The Galaxy ◽  
Galaxy Halo ◽  
Environment Dependence ◽  
Galaxy Luminosity Function

Abstract We investigate the dependence of the galaxy–halo connection and galaxy density field in modified gravity models using the N-body simulations for f(R) and nDGP models at z = 0. Because of the screening mechanisms employed by these models, chameleon and Vainshtein, haloes are clustered differently in the non-linear regime of structure formation. We quantify their deviations in the galaxy density field from the standard Λ cold dark matter (ΛCDM) model under different environments. We populate galaxies in haloes via the (sub)halo abundance matching. Our main results are as follows: (1) The galaxy–halo connection strongly depends on the gravity model; a maximum variation of ${\sim }40{{\ \rm per\ cent}}$ is observed between halo occupational distribution (HOD) parameters; (2) f(R) gravity models predict an excess of galaxies in low-density environments of ${\sim }10{{\ \rm per\ cent}}$ but predict a deficit of ${\sim }10{{\ \rm per\ cent}}$ at high-density environments for |fR0| = 10−4 and 10−6 while |fR0| = 10−5 predicts more high-density structures; nDGP models are consistent with ΛCDM; (3) different gravity models predict different dependences of the galaxy luminosity function (GLF) with the environment, especially in void-like regions we find differences around ${\sim }10{{\ \rm per\ cent}}$ for the f(R) models while nDPG models remain closer to ΛCDM for low-luminosity galaxies but there is a deficit of ${\sim }11{{\ \rm per\ cent}}$ for high-luminosity galaxies in all environments. We conclude that the dependence of the GLF with environment might provide a test to distinguish between gravity models and their screening mechanisms from the ΛCDM. We provide HOD parameters for the gravity models analysed in this paper.

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