scholarly journals Constraints on Galaxy Evolution from Faint Redshift Surveys, Keck, and HST

1996 ◽  
Vol 171 ◽  
pp. 384-384
Author(s):  
Caryl Gronwall
Keyword(s):  
Galaxy Evolution ◽  
Luminosity Function ◽  
Current Model ◽  
Angular Size ◽  
Small Sample ◽  
Redshift Surveys ◽  
Luminosity Functions ◽  
The Galaxy ◽  
Deep Survey ◽  
Galaxy Luminosity Function

The nature of faint field galaxy evolution remains controversial. While many workers advocate exotic theories, such as rapid merging or disappearing populations, we have found that it is possible to explain the published counts and redshift data with traditional luminosity evolution models which derive an optimal set of local luminosity functions for different galaxy types (Gronwall & Koo 1995). Recently, there has been a tremendous amount of new data addressing this question, including 1) the measurement of the galaxy luminosity function vs. redshift from faint redshift surveys down to B = 24 and I = 22 (Colless 1995; Lilly et al. 1995), 2) morphological and angular size data from the HST Medium Deep Survey (Driver et al. 1995; Phillips et al. 1995), and 3) redshift measurements with Keck for a small sample of galaxies with I > 22 (Koo 1995). We have explored these new data and have found that while our model continues to provide an excellent match to the faintest observed redshift and angular size distributions, it underpredicts the faint counts and luminosity function evolution for very blue late-type galaxies. Since our current model includes only minimal evolution of these galaxies, the new observations suggest a need for additional evolution, perhaps through a starbursting or mild merging component.

scholarly journals The WIRCam Ultra Deep Survey (WUDS)

2018 ◽  
Vol 620 ◽  
pp. A51 ◽  
Author(s):  
R. Pelló ◽  
P. Hudelot ◽  
N. Laporte ◽  
Y. Mellier ◽  
H. J. McCracken ◽  
...  
Keyword(s):  
Luminosity Function ◽  
Formation Rate ◽  
Forthcoming Paper ◽  
Spectroscopic Studies ◽  
Photometric Redshifts ◽  
Near Ir ◽  
Luminosity Functions ◽  
The Galaxy ◽  
Deep Survey ◽  
Galaxy Population

The aim of this paper is to introduce the WIRCam Ultra Deep Survey (WUDS), a near-IR photometric survey carried out at the CFH Telescope in the field of the CFHTLS-D3 field (Groth Strip). WUDS includes four near-IR bands (Y, J, H and Ks) over a field of view of ∼400 arcmin2. The typical depth of WUDS data reaches between ∼26.8 in Y and J, and ∼26 in H and Ks (AB, 3σ in 1.3″ aperture), whereas the corresponding depth of the CFHTLS-D3 images in this region ranges between 28.6 and 29 in ugr, 28.2 in i and 27.1 in z (same S/N and aperture). The area and depth of this survey were specifically tailored to set strong constraints on the cosmic star formation rate and the luminosity function brighter or around L⋆ in the z ∼ 6 − 10 redshift domain, although these data are also useful for a variety of extragalactic projects. This first paper is intended to present the properties of the public WUDS survey in details: catalog building, completeness and depth, number counts, photometric redshifts, and global properties of the galaxy population. We have also concentrated on the selection and characterization of galaxy samples at z ∼ [4.5 − 7] in this field. For these purposes, we include an adjacent shallower area of ∼1260 arcmin2 in this region, extracted from the WIRCam Deep Survey (WIRDS), and observed in J, H and Ks bands. UV luminosity functions were derived at z ∼ 5 and z ∼ 6 taking advantage from the fact that WUDS covers a particularly interesting regime at intermediate luminosities, which allows a combined determination of M⋆ and Φ⋆ with increased accuracy. Our results on the luminosity function are consistent with a small evolution of both M⋆ and Φ⋆ between z = 5 and z = 6, irrespective of the method used to derive them, either photometric redshifts applied to blindly-selected dropout samples or the classical Lyman Break Galaxy color-preselected samples. Our results lend support to higher Φ⋆ determinations at z = 6 than usually reported. The selection and combined analysis of different galaxy samples at z ≥ 7 will be presented in a forthcoming paper, as well as the evolution of the UV luminosity function between z ∼ 4.5 and 9. WUDS is intended to provide a robust database in the near-IR for the selection of targets for detailed spectroscopic studies, in particular for the EMIR/GTC GOYA Survey.

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 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.

The evolution of the luminosity function faint end of cluster galaxies in the Cluster-EAGLE simulation

2018 ◽  
Vol 14 (S344) ◽  
pp. 495-497
Author(s):  
Andrea Negri ◽  
Claudio Dalla Vecchia ◽  
Alfonso Aguerri ◽  
Yannick Bahé ◽  
David Barnes ◽  
...  
Keyword(s):  
Galaxy Clusters ◽  
Luminosity Function ◽  
Cluster Galaxies ◽  
Cluster Mass ◽  
Luminosity Functions ◽  
The Galaxy ◽  
Zoom In ◽  
Dust Attenuation ◽  
Galaxy Luminosity Function

AbstractIn the last decade observations have been able to probe the evolution of the galaxy luminosity function, in particular showing a variation of its faint-end with redshift. We employ the data of the Cluster-EAGLE project, a set of cosmological, hydrodynamical zoom-in simulations of 30 galaxy clusters, to study the evolution of the galaxy luminostity functions in clusters with redshift. We compile a catalogue of simulated galaxies’ luminosities in the SDSS bands using the E-MILES spectra database, and taking into account dust attenuation. Stacked luminosity functions present little evolution with redshift of the faint-end slope from z=3.5 to z=0, regardless of the cluster mass.

scholarly journals The Faint-End of the Galaxy Luminosity Function in the Hydra I Cluster

2006 ◽  
Vol 2 (S235) ◽  
pp. 257-257
Author(s):  
H. Yamanoi ◽  
M. Tanaka ◽  
Keyword(s):  
Luminosity Function ◽  
Dwarf Galaxies ◽  
Steep Slope ◽  
Cluster Center ◽  
Magnitude Range ◽  
Luminosity Functions ◽  
The Galaxy ◽  
Blue Galaxies ◽  
Galaxy Luminosity Function

AbstractWe examine the galaxy luminosity functions (LFs) in the Hydra I cluster (Abell 1060) at z = 0.0126, for which very faint galaxies (down to M ~ −10) have not been surveyed yet. We conclude that the total LF has a slightly steep slope (α ~ −1.6) at −20 < M < −10 in the B- and RC-bands. The numbers of galaxies at the faint end (M ≳ −14) differ in between the cluster center and the outskirts slightly. We divide the Hydra member galaxies into red/blue galaxies and find that the shape of LFs in the faint magnitude range is determined by red dwarf galaxies.

scholarly journals Galaxies, Clusters and Fluctuations

1988 ◽  
Vol 130 ◽  
pp. 215-220
Author(s):  
Richard Schaeffer
Keyword(s):  
Luminosity Function ◽  
Two Dimensions ◽  
Many Body ◽  
Microwave Background ◽  
Scale Invariant ◽  
Galaxy Distribution ◽  
Luminosity Functions ◽  
The Galaxy ◽  
The Many ◽  
Galaxy Luminosity Function

The luminosity function of galaxies and clusters as well as their correlations can be calculated assuming the many-body correlation functions are scale invariant. The same hypothesis leads to predictions on the fractal dimension of the galaxy distribution. The latter is found to be bifractal that is characterized by two dimensions D=3−γ in the cluster region, and D = (3−γ)(2+α) in the nearly empty regions, α being the index introduced by Schechter for the galaxy luminosity function. Finally, the same models lead to predictions for the evolution of the cluster and x-ray luminosity functions, as well as for the Sunyaev-Zeldovich effect due to all virialized clusters, which is found to be large and to produce fluctuations of order 10−5 at sub-arc minute scalar in the microwave background.

scholarly journals An Investigation of the Radial Dependence of the Galaxy Luminosity Function in Abell Clusters

1987 ◽  
Vol 127 ◽  
pp. 459-460
Author(s):  
Phyllis M Lugger
Keyword(s):  
Luminosity Function ◽  
Nonparametric Tests ◽  
Radial Dependence ◽  
Cluster Center ◽  
Abell Clusters ◽  
Luminosity Functions ◽  
The Galaxy ◽  
Kolmogorov Smirnov ◽  
Galaxy Luminosity Function ◽  
Central Concentration

The luminosity functions of inner and outer regions of six Abell clusters (A569, A1656, A2147, A2151, A2199, and A2634) were compared. These clusters have a single, reasonably symmetric central concentration of galaxies within the central Mpc. For three other clusters with irregular spatial distributions of galaxies (A779, A1367, and A2197) luminosity functions for high and low density regions were compared. For three of the clusters in the first group (A1656, A2147, and A2199) there is a deficit of bright galaxies, according to the Kolmogorov-Smirnov and Wilcoxon rank-sum nonparametric tests, in a region of radius 0.5 Mpc about the cluster center compared to a concentric annular region with bounds of 0.5 and 1.0 Mpc.

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 Tracing Galaxy Evolution by Their Present-Day Luminosity Function

2011 ◽  
Vol 20 (2) ◽  
Author(s):  
E. Tempel
Keyword(s):  
Galaxy Evolution ◽  
Luminosity Function ◽  
Large Scale ◽  
A Priori ◽  
Elliptical Galaxies ◽  
Global Environmental ◽  
Luminosity Functions ◽  
Group Environment ◽  
The Galaxy ◽  
Formation And Evolution

AbstractGalaxy luminosity functions are derived for different morphological types and various colors of galaxies, to trace the evolutionary effects which a priori should be different for void and supercluster galaxies. We also analyse how the galaxy group content changes in the large-scale environment. One of the principal results is the conclusion that the evolution of spiral galaxies is almost independent of the global environment. Meanwhile, the luminosity function of elliptical galaxies depends strongly on the environment. This shows that the global environmental density is an important factor in the formation of elliptical galaxies. The results of the present study clearly show that, except the local/group environment, the global (supercluster-void) environment plays an important role in the formation and evolution of 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
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