Critical analysis of the luminosity functions per galaxy type measured from redshift surveys

Lapparent, V. de

doi:10.1051/0004-6361:20030898

Cited by 31 publications

(26 citation statements)

References 111 publications

(418 reference statements)

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“…The LF parameters are extracted from Table 6 of de for the shape parameters (using 2 for ellipticals and Centaurus parameters for dE+dS0 and Im+BCD galaxies) and from Table 1 of de Lapparent (2003) for the amplitudes φ * . The mapping made between the LF morphological types and the EFIGI types is given in Table 2.…”

Section: Morphological Fractionsmentioning

confidence: 99%

The EFIGI catalogue of 4458 nearby galaxies with detailed morphology

Baillard

Bertin

Lapparent

et al. 2011

A&A

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145

111

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Context. Now that modern imaging surveys have produced large databases of galaxy images advanced morphological studies have become possible. This has driven the need for well-defined calibration samples. Aims. We present the EFIGI catalogue, a multi-wavelength database specifically designed to densely sample all Hubble types. The catalogue merges data from standard surveys and catalogues (Principal Galaxy Catalogue, Sloan Digital Sky Survey, Value-Added Galaxy Catalogue, HyperLeda, and the NASA Extragalactic Database) and provides detailed morphological information. Methods. Imaging data were obtained from the SDSS DR4 in the u, g, r, i, and z bands for a sample of 4458 PGC galaxies, whereas photometric and spectroscopic data were obtained from the SDSS DR5 catalogue. Point-spread function models were derived in all five bands. Composite colour images of all objects were visually examined by a group of astronomers, and galaxies were assigned positions in the Hubble sequence and classified according to 16 morphological attributes describing their structure, texture, environment and appearance on a five-level scale. Results. The EFIGI Hubble sequence is in remarkably good agreement with the RC3 Revised Hubble Sequence. The main characteristics and reliability of the catalogue are examined, including photometric completeness, type mix, systematic trends and correlations. Conclusions. The final EFIGI database is a large sub-sample of the local Universe which densely samples Sd, Sdm, Sm and Im types compared to magnitude-limited catalogues. We estimate that the photometric catalogue is more than ≈80% complete for galaxies with 10 < g < 14. More than 99.5% of EFIGI galaxies have known redshifts in the HyperLeda and NED databases.

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Section: Morphological Fractionsmentioning

confidence: 99%

The EFIGI catalogue of 4458 nearby galaxies with detailed morphology

Baillard

Bertin

Lapparent

et al. 2011

A&A

Self Cite

145

111

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“…The LF is well reproduced by the Schechter (1976) function where φ* is the number of galaxies per unit volume, L * is the characteristic luminosity which separates bright sources from faint sources and α is the slope of the LF. Different determinations of the local LF exist (see de Lapparent 2003 for a review) and they show several differences, in the sense that the parameters of the Schechter function are not fully constrained by observations. The LF can be measured in several bands, obviously depending on the redshift regime under investigation.…”

Section: Chemical and Photometric Evolution Of Galaxiesmentioning

confidence: 99%

Cosmic star formation rate: a theoretical approach

Vincoletto

Matteuccí

Calura

et al. 2012

Monthly Notices of the Royal Astronomical Society

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The cosmic star formation rate (CSFR), namely the SFR in a unitary comoving volume of the Universe, is an important clue to investigate the history of the assembly and evolution of galaxies. Here, we develop a method to study the CSFR from a purely theoretical point of view. Starting from detailed models of chemical evolution, which best fit the properties of local galaxies, we obtain the histories of star formation of galaxies of different morphological types (ellipticals, spirals, irregulars). These histories are then used to determine the luminosity functions of the same galaxies by means of a spectrophotometric code. We obtain the CSFR under different hypothesis about galaxy formation scenarios. First, we study the hypothesis of a pure luminosity evolution scenario, in which all galaxies are supposed to form at the same redshift and then evolve only in luminosity without any merging or interaction. Then we consider scenarios in which the number density or the slope of the luminosity functions is assumed to vary with redshift. After comparison of our results with the data available in the literature, we conclude that a pure luminosity evolution does not provide a good fit to the data, especially at very high redshift, although many uncertainties are still present in the data because of the unknown dust corrections and assumed initial mass function. On the other hand, a variation in the number density of ellipticals and spirals as a function of redshift can provide a better fit to the observed CSFR. We critically discuss the possible scenarios for galaxy formation derived from this finding. We also explore cases of variable slope of the luminosity functions with redshift as well as variations of number density and slope at the same time. We cannot find any of those cases which can fit the data as well as solely the number density variation. Finally, we compute the evolution of the average cosmic metallicity in galaxies with redshift and show that in the pure luminosity evolution case the ellipticals dominate the metal production in the Universe, whereas in the case of number density evolution are the spirals the main producers of metals

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“…We can understand this luminosity dependence for the level of aperture bias as the combination of two effects: (i) more luminous galaxies at the same distance will have larger apparent sizes, and so the fraction of flux covered by the SDSS fibres will be reduced and (ii) low‐luminosity galaxies tend to be either late‐type spirals or dwarf ellipticals and hence do not have such significant radial gradients in their SFRs. The luminosity function of early‐type spirals (Sa+b) for which aperture biases are by far the most important has a Gaussian distribution centred at M r =−21.7 and width σ∼ 0.9 mag (de Lapparent 2003), and hence are rare at M r ≳−20.…”

Section: Aperture Biases In the Sdss Spectroscopic Samplementioning

confidence: 99%

The SDSS-GALEX viewpoint of the truncated red sequence in field environments at z ∼ 0

Haines¹,

Gargiulo²,

Merluzzi³

2008

Monthly Notices RAS

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We combine Galaxy Evolution ExplorerGALEX near‐ultraviolet (NUV) photometry with a volume‐limited sample of local (0.005 < z < 0.037) Sloan Digital Sky Survey (SDSS) DR4 galaxies to examine the composition and the environmental dependencies of the optical and ultraviolet (UV)‐optical colour–magnitude (CM) diagrams. We find that ∼30 per cent of red‐sequence galaxies in the optical CM diagram show signs of ongoing star formation from their spectra having EW(Hα) > 2 Å. This contamination is greatest at faint magnitudes (Mr > −19) and in field regions where as many as three‐quarters of red‐sequence galaxies are star forming, and as such has important consequences for following the build‐up of the red sequence. The NUV −r colour instead allows a much more robust separation of passively evolving and star‐forming galaxies, which allows the build‐up of the UV‐selected red sequence with redshift and environment to be directly interpreted in terms of the assembly of stellar mass in passively evolving galaxies. In isolated field regions, the number density of UV‐optical red‐sequence galaxies declines rapidly at magnitudes fainter than Mr∼−19 and appears completely truncated at Mr∼−18. These results support the downsizing paradigm whereby the red sequence is assembled from the top down, being already largely in place at the bright end by z∼ 1, and the faint end filled in at later epochs in clusters and groups through environment‐related processes such as ram‐pressure stripping or galaxy harassment.

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Critical analysis of the luminosity functions per galaxy type measured from redshift surveys

Cited by 31 publications

References 111 publications

The EFIGI catalogue of 4458 nearby galaxies with detailed morphology

The EFIGI catalogue of 4458 nearby galaxies with detailed morphology

Cosmic star formation rate: a theoretical approach

The SDSS-GALEX viewpoint of the truncated red sequence in field environments at z ∼ 0

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