The galaxy luminosity function in groups and clusters: the faint-end upturn and the connection to the field 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.

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The galaxy luminosity function and the morphological type

The Astrophysical Journal ◽

10.1086/166633 ◽

1988 ◽

Vol 332 ◽

pp. 89 ◽

Cited By ~ 3

Author(s):

E. Martinez-Gonzalez ◽

J. L. Sanz

Keyword(s):

Luminosity Function ◽

Morphological Type ◽

The Galaxy ◽

Galaxy Luminosity Function

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

Monthly Notices of the Royal Astronomical Society ◽

10.1093/mnras/stz1664 ◽

2019 ◽

Vol 488 (1) ◽

pp. 782-802 ◽

Cited By ~ 1

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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