The luminosity function for different morphological types in the CfA Redshift Survey

Marzke, Ronald O.; Geller, Margaret J.; Huchra, J. P.; Corwin, H. G.

doi:10.1086/117081

Cited by 209 publications

(267 citation statements)

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“…To estimate the parameters of the LF, we use the STY method (Sandage et al 1979;Loveday et al 1992;Marzke et al 1994Marzke et al , 1998Efstathiou, Ellis, & Peterson 1988;Willmer 1997), assuming that the LF is described by the Schechter form (Schechter 1976),…”

Section: Sty Methodsmentioning

confidence: 99%

“…Since we do not have a reliable scheme to distinguish E's from S0's quantitatively, we instead divide the sample above and below M B < À20. According to the LFs of local field E/S0's (Marzke et al 1994) and cluster E/S0's (e.g., Dressler 1980), E's are more abundant than S0's at M B d À 20, while S0's are more abundant than E's at M B e À 20. Figures 19 and 20 show the ellipticity distribution of Groth Strip QS-E/S0's divided this way.…”

Section: Ellipticity Distributionmentioning

confidence: 99%

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The DEEP Groth Strip Survey. X. Number Density and Luminosity Function of Field E/S0 Galaxies atz< 1

Simard

Faber

et al. 2002

ApJ

142

133

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We present the luminosity function and color-redshift relation of a magnitude-limited sample of 145 mostly red field E/S0 galaxies at zd1 from the DEEP Groth Strip Survey (GSS). Using nearby galaxy images as a training set, we develop a quantitative method to classify E/S0 galaxies based on smoothness, symmetry, and bulge-to-total light ratio. Using this method, we identify 145 E/S0's at 16:5 < I < 22 within the GSS, for which 44 spectroscopic redshifts (z spec ) are available. Most of the galaxies with spectroscopic redshifts (86%) form a '' red envelope '' in the redshift-color diagram, consistent with predictions of spectral synthesis models in which the dominant stellar population is formed at redshifts ze1:5. We use the tight correlation between VÀI and z spec for this red subset to estimate redshifts of the remaining E/S0's to an accuracy of $10%, with the exception of a small number (16%) of blue interlopers at low redshift that are quantitatively classified as E/S0's but are not contained within the red envelope. Constructing a luminosity function of the full sample of 145 E/S0's, we find that there is about 1.1-1.9 mag brightening in rest-frame B-band luminosity back to z ' 0:8 from z ¼ 0, consistent with other studies. Together with the red colors, this brightening is consistent with models in which the bulk of stars in red field E/S0's formed before z for e1:5 and have been evolving rather quiescently, with few large starbursts since then. Evolution in the number density of field E/ S0 galaxies is more difficult to measure, and uncertainties in the raw counts and their ratio to local samples might amount to as much as a factor of 2. Within that uncertainty, the number density of red E/S0's to z ' 0:8 seems relatively static, being comparable to or perhaps moderately less than that of local E/S0's, depending on the assumed cosmology. A doubling of E/S0 number density since z ¼ 1 can be ruled out with high confidence (97%) if m ¼ 1. Taken together, our results are consistent with the hypothesis that the majority of luminous field E/S0's were already in place by z $ 1, that the bulk of their stars were already fairly old, and that their number density has not changed by large amounts since then.

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Section: Sty Methodsmentioning

confidence: 99%

Section: Ellipticity Distributionmentioning

confidence: 99%

The DEEP Groth Strip Survey. X. Number Density and Luminosity Function of Field E/S0 Galaxies atz< 1

Simard

Faber

et al. 2002

ApJ

142

133

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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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“…where the parameters θ * , M 0 and γ where calculated for the different morphological types, using the luminosity distribution functions by [38]. The parameter ǫ = 0.8 ± 0.1 depends on the slopes of the adopted M bh − σ 1D and L − σ 1D relations.…”

Section: The Expected Number Of Eventsmentioning

confidence: 99%

Capture rates of compact objects by supermassive black holes

Pacheco

Filloux²,

Regimbau³

2006

Phys. Rev. D

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Capture rates of compact objects were calculated by using a recent solution of the Fokker-Planck equation in energy-space, including two-body resonant effects. The fraction of compact objects (white dwarfs, neutron stars and stellar black holes) was estimated as a function of the luminosity of the galaxy from a new grid of evolutionary models. Stellar mass densities at the influence radius of central supermassive black holes were derived from brightness profiles obtained by Hubble Space Telescope observations. The present study indicates that the capture rates scale as ∝ M −1.048 bh , consequence of the fact that dwarf galaxies have denser central regions than luminous objects. If the mass distribution of supermassive black holes has a lower cutoff at ∼ 1.4×10 6 M⊙ (corresponding to the lowest observed supermassive black hole mass, located in M32), then 9 inspiral events are expected to be seen by LISA (7-8 corresponding to white dwarf captures and 1-2 to neutron star and stellar black hole captures) after one year of operation. However, if the mass distribution extends down to ∼ 2 × 10 5 M⊙, then the total number of expected events increases up to 579 (corresponding to ∼ 274 stellar black hole captures, ∼ 194 neutron star captures and ∼ 111 white dwarf captures).

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The luminosity function for different morphological types in the CfA Redshift Survey

Cited by 209 publications

References 0 publications

The DEEP Groth Strip Survey. X. Number Density and Luminosity Function of Field E/S0 Galaxies atz< 1

The DEEP Groth Strip Survey. X. Number Density and Luminosity Function of Field E/S0 Galaxies atz< 1

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

Capture rates of compact objects by supermassive black holes

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