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

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.

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The brightest galaxies in the dark ages: Galaxies’ dust continuum emission out to the reionization era

Proceedings of the International Astronomical Union ◽

10.1017/s1743921320001350 ◽

2019 ◽

Vol 15 (S352) ◽

pp. 349-349

Author(s):

Caitlin Casey

Keyword(s):

Star Formation ◽

Early Universe ◽

Luminosity Function ◽

Formation Rate ◽

Continuum Emission ◽

Spectral Energy ◽

Universe Model ◽

Star Forming ◽

Number Counts ◽

Galaxy Luminosity Function

AbstractThough half of cosmic starlight is absorbed by dust and reradiated at long wavelengths (3μ m – 3 mm), constraints on the infrared through millimeter galaxy luminosity function (the ‘IRLF’) are poor in comparison to the rest-frame ultraviolet and optical galaxy luminosity function, particularly at z ⩾ 2.5. Here we present a backward evolution model for interpreting number counts, redshift distributions, and cross-band flux density correlations in the infrared and submillimeter sky, from 70μm – 2 mm, using a model for the IRLF out to the epoch of reionization. Mock submillimeter maps are generated by injecting sources according to the prescribed IRLF and flux densities drawn from model spectral energy distributions that mirror the distribution of SEDs observed in 0 < z 0 < 5 dusty star-forming galaxies (DSFGs). We explore two extreme hypothetical case-studies: a dust-poor early Universe model, where DSFGs contribute negligibly (< 10%) to the integrated star-formation rate density at z > 4, and an alternate dust-rich early Universe model, where DSFGs dominate > 90% of z > 4 star-formation. We find that current submm/mm datasets do not clearly rule out either of these extreme models. We suggest that future surveys at 2 mm – both from ALMA and single-dish facilities – will be crucial to measuring the IRLF beyond z > 4.

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Luminosity Functions from the 2dF Galaxy Redshift Survey

Publications of the Astronomical Society of Australia ◽

10.1071/as04041 ◽

2004 ◽

Vol 21 (4) ◽

pp. 352-355 ◽

Cited By ~ 1

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.

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

Proceedings of the International Astronomical Union ◽

10.1017/s1743921318006233 ◽

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.

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

Proceedings of the International Astronomical Union ◽

10.1017/s1743921306006533 ◽

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.

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

Symposium - International Astronomical Union ◽

10.1017/s0074180900233032 ◽

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.

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Galaxies, Clusters and Fluctuations

Symposium - International Astronomical Union ◽

10.1017/s007418090013606x ◽

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.

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

Symposium - International Astronomical Union ◽

10.1017/s0074180900185730 ◽

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.

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