The<i>K</i>‐Band Galaxy Luminosity Function

Kochanek, C. S.; Pahre, M. A.; Falco, E.; Huchra, J. P.; Mader, J.; Jarrett, T. H.; Chester, T. J.; Cutri, R. M.; Schneider, Stephen E.

doi:10.1086/322488

Cited by 461 publications

(854 citation statements)

References 72 publications

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“…The panels show the luminosity functions in the b J , z, H and K bands, as labelled. Data points show the observational estimates from the Two-Micron All-Sky Survey (Kochanek et al 2001), Two-degree Field Galaxy Redshift Survey (2dFGRS; Cole et al 2001;Norberg et al 2002), the Six-degree Field Galaxy Survey (6dFGS; Jones et al 2006) and the Galaxy And Mass Assembly Survey (GAMA; Driver et al 2012). The solid blue line shows the prediction for the fiducial GALFORM model with the default dust attenuation calculations.…”

Section: Agn Feedbackmentioning

confidence: 99%

The abundance and colours of galaxies in high-redshift clusters in the cold dark matter cosmology

Merson¹,

Baugh²,

González-Pérez³

et al. 2015

Mon. Not. R. Astron. Soc.

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High redshift galaxy clusters allow us to examine galaxy formation in extreme environments.Here we compile data for 15 z > 1 galaxy clusters to test the predictions from a state-of-theart semi-analytical model of galaxy formation. The model gives a good match to the slope and zero-point of the cluster red sequence. The model is able to match the cluster galaxy luminosity function at faint and bright magnitudes, but under-estimates the number of galaxies around the break in the cluster luminosity function. We find that simply assuming a weaker dust attenuation improves the model predictions for the cluster galaxy luminosity function, but worsens the predictions for the red sequence at bright magnitudes. Examination of the properties of the bright cluster galaxies suggests that the default dust attenuation is large due to these galaxies having large reservoirs of cold gas as well as small radii. We find that matching the luminosity function and colours of high redshift cluster galaxies, whilst remaining consistent with local observations, poses a challenge for galaxy formation models.

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Section: Agn Feedbackmentioning

confidence: 99%

The abundance and colours of galaxies in high-redshift clusters in the cold dark matter cosmology

Merson¹,

Baugh²,

González-Pérez³

et al. 2015

Mon. Not. R. Astron. Soc.

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“…The ∆'s indicate the assumed intrinsic dispersions of the M BH -σ⋆ or M BH -L bul relations. (b) Local BHMF for early type galaxies derived using the luminosity functions from different surveys (Bernardi et al 2003b;Marzke et al 1994;Kochanek et al 2001;Nakamura et al 2003) and the M BH -L bul relation with ∆(M BH )=0.3. The shaded area and errorbars have the same meaning as in (a).…”

Section: Consistency Of the Mbh-σ⋆ And Mbh-l Bul Relationsmentioning

confidence: 99%

Local Supermassive Black Holes, Relics of Active Galactic Nuclei and the X-ray background

Marconi

Risaliti

Gilli

et al. 2005

Growing Black Holes: Accretion in a Cosmological Context

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We quantify the importance of mass accretion during AGN phases in the growth of supermassive black holes (BH) by comparing the mass function of black holes in the local universe with that expected from AGN relics, which are black holes grown entirely with mass accretion during AGN phases. The local BH mass function (BHMF) is estimated by applying the well-known correlations between BH mass, bulge luminosity and stellar velocity dispersion to galaxy luminosity and velocity functions. We find that different correlations provide the same BHMF only if they have the same intrinsic dispersion. The density of supermassive black holes in the local universe which we estimate is ρ BH = 4.6 +1.9 −1.4 h 2 0.7 × 10 5 M ⊙ Mpc −3 . The relic BHMF is derived from the continuity equation with the only assumption that AGN activity is due to accretion onto massive BH's and that merging is not important. We find that the relic BHMF at z = 0 is generated mainly at z < 3 where the major part of BH's growth takes place. Moreover, the BH growth is anti-hierarchical in the sense that smaller BH's (M BH < 10 7 M ⊙ ) grow at lower redshifts (z < 1) with respect to more massive one's (z ∼ 1 − 3). Unlike previous work, we find that the BHMF of AGN relics is perfectly consistent with the local BHMF indicating the local black holes were mainly grown during AGN activity. This agreement is obtained while satisfying, at the same time, the constraints imposed from the X-ray background. The comparison between the local and relic BHMF's also suggests that the merging process is not important in shaping the relic BHMF, at least at low redshifts (z < 3), and allows us to estimate the average radiative efficiency (ε), the ratio between emitted and Eddington luminosity (λ) and the average lifetime of active BH's. Our analysis thus suggests the following scenario: local black holes grew during AGN phases in which accreting matter was converted into radiation with efficiencies ε = 0.04 − 0.16 and emitted at a fraction λ = 0.1 − 1.7 of the Eddington luminosity. The average total lifetime of these active phases ranges from ≃ 4.5 × 10 8 yr for M BH < 10 8 M ⊙ to ≃ 1.5 × 10 8 yr for M BH > 10 9 M ⊙ but can become as large as ∼ 10 9 yr for the lowest acceptable ǫ and λ values.

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“…The statistical properties of the stellar components of galaxies have been investigated by means of large surveys in the optical and near-infrared wavelengths (e.g. Cole et al 2001;Kochanek et al 2001). It is known that the galaxy formation models based on the canonical cold dark matter hypothesis (the so-called ΛCDM hypothesis) overpredict the number densities of less massive and massive galaxies when compared with the observed SMFs of galaxies (e.g.…”

Section: Introductionmentioning

confidence: 99%

Redshift evolution of stellar mass versus gas fraction relation in 0 <z< 2 regime: observational constraint for galaxy formation models

Morokuma-Matsui¹,

Baba²

2015

Mon. Not. R. Astron. Soc.

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We investigate the redshift evolution of the molecular gas mass fraction (f mol = M mol M⋆+M mol , where M mol is molecular gas mass and M ⋆ is stellar mass) of galaxies in the redshift range of 0 < z < 2 as a function of the stellar mass by combining CO literature data. We observe a stellar-mass dependence of the f mol evolution where massive galaxies have largely depleted their molecular gas at z = 1, whereas the f mol value of less massive galaxies drastically decreases from z = 1. We compare the observed M ⋆ −f mol relation with theoretical predictions from cosmological hydrodynamic simulations and semi-analytical models for galaxy formation. Although the theoretical studies approximately reproduce the observed mass dependence of f mol evolution, they tend to underestimate the f mol values, particularly of less massive (< 10 10 M ⊙ ) and massive galaxies (> 10 11 M ⊙ ) when compared with the observational values. Our result suggests the importance of the feedback models which suppress the star formation while simultaneously preserving the molecular gas in order to reproduce the observed M ⋆ − f mol relation.

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TheK‐Band Galaxy Luminosity Function

Cited by 461 publications

References 72 publications

The abundance and colours of galaxies in high-redshift clusters in the cold dark matter cosmology

The abundance and colours of galaxies in high-redshift clusters in the cold dark matter cosmology

Local Supermassive Black Holes, Relics of Active Galactic Nuclei and the X-ray background

Redshift evolution of stellar mass versus gas fraction relation in 0 <z< 2 regime: observational constraint for galaxy formation models

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