The ESO-Sculptor Survey: Evolution of late-type galaxies at redshifts 0.1–0.5

Lapparent, V. de; Arnouts, S.; Galaz, Gaspar; Bardelli, S.

doi:10.1051/0004-6361:20047140

Cited by 12 publications

(23 citation statements)

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“…The strong density evolution of late type galaxies we find in the redshift range [0.2-1.5] extends to significantly higher redshift the results found by de Lapparent et al (2004) for their latest type at z ∼ 0.5.…”

Section: Comparison With Previous Literature Resultssupporting

confidence: 82%

The VIMOS VLT Deep Survey

Zucca¹,

Ilbert

Bardelli³

et al. 2006

A&A

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From first epoch observations of the VIMOS VLT Deep Survey (VVDS) we have derived luminosity functions for galaxy samples selected by spectral type out to z = 1.5. With the VVDS we are able to investigate within the same sample the evolution of the type dependent luminosity function selected in several rest-frame bands over 70% of the age of the Universe. The simple I AB = 24 VVDS magnitude limit is significantly fainter than other complete spectroscopic surveys and allows the determination of the faint end slope of the luminosity function with unprecedented accuracy. Galaxies have been classified in four spectral types, from early type to irregular galaxies, using their colours and redshift. Luminosity functions have been computed in the U, B, V, R and I rest frame bands for each type, in redshift bins from z = 0.05 to z = 1.5. In all the considered rest frame bands, we find a significant steepening of the luminosity function from early to late types. The characteristic luminosity M * of the Schechter function is significantly fainter for late type galaxies and this difference between types increases in the redder bands. For each spectral type we find a brightening of M * with increasing redshift, ranging from 0.5 mag for early type galaxies to ∼1 mag for the latest type galaxies, while the slope of the luminosity function of each spectral type is consistent with being redshift-independent. The luminosity function of early type galaxies is consistent with passive evolution up to z ∼ 1.1, whilst the number of bright (M B AB < −20) early type galaxies has decreased by ∼40% from z ∼ 0.3 to z ∼ 1.1. The normalisation of the luminosity function of latest type galaxies evolves strongly with redshift with an increase of more than a factor 2 from z ∼ 0.3 to z ∼ 1.3: the density of bright (M B AB < −20) late type galaxies in the same redshift range increases of a factor ∼6.6. These results indicate a strong type-dependent evolution and identifies the latest spectral types as responsible for most of the evolution of the UV-optical luminosity function out to z = 1.5.

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Section: Comparison With Previous Literature Resultssupporting

confidence: 82%

The VIMOS VLT Deep Survey

Zucca¹,

Ilbert

Bardelli³

et al. 2006

A&A

Self Cite

111

136

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“…The parameters listed in Table 2 are those derived by de Lapparent et al (2004) from the R c ≤ 21.5 sample. For the early-type and intermediate-type classes, the listed values of φ 0 are those listed as Φ 1 (0.51) in Table 2 of de Lapparent et al (2004), derived using an "equal pair" weighting for the mean density estimator (see Eqs.…”

Section: The Luminosity Functionsmentioning

confidence: 99%

“…(F.1) and (D.1)); they thus yield a total expected number of galaxies over the redshift interval 0.1−0.51 for a homogeneous distribution which is equal to the observed number of galaxies in each spectral class. For the late-type class, we use (and list here in Table 2) the parameterization Φ 1 (z) provided in Table 2 of de Lapparent et al (2004), which reflects the marked evolution of the amplitudes φ 0 and φ * for the ESS late-type galaxies. This evolution could also be due to pure luminosity evolution, but the available data do not allow us to discriminate between the 2 effects (de Lapparent et al 2004).…”

Section: The Luminosity Functionsmentioning

confidence: 99%

“…For the late-type class, we use (and list here in Table 2) the parameterization Φ 1 (z) provided in Table 2 of de Lapparent et al (2004), which reflects the marked evolution of the amplitudes φ 0 and φ * for the ESS late-type galaxies. This evolution could also be due to pure luminosity evolution, but the available data do not allow us to discriminate between the 2 effects (de Lapparent et al 2004). Whatever the nature of this evolution, the parameterized amplitude evolution listed in Table 2 does allow us to estimate the selection function (Appendix C) required for calculating correlation functions.…”

Section: The Luminosity Functionsmentioning

confidence: 99%

“…1 and 2 and are compared with the ESS observed distributions for each spectral class and galaxy type. To calculate the expected redshift distribution, we also use for each sub-sample the K-correction function K(z, δ) provided by de Lapparent et al (2004) at the mean value of the spectral-type δ listed in the Table 1. Note that comparison of the observed and expected distributions for the 3 spectral classes shown in Fig.…”

Section: The Luminosity Functionsmentioning

confidence: 99%

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Spatial clustering in the ESO-Sculptor survey: two-point correlation functions by galaxy type at redshifts 0.1–0.5

Lapparent¹,

Slezak²

2007

A&A

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Context. Galaxy clustering shows segregation effects with galaxy type, color and luminosity, which bring clues on the relationship with the underlying density field. Aims. We explore these effects among the populations of giant and dwarf galaxies detected in the ESO-Sculptor survey. Methods. We calculate the spatial two-point auto and cross-correlation functions for the 765 galaxies with R c ≤ 21.5 and 0.1 ≤ z ≤ 0.51 and for subsets by spectral type and luminosity. Results. At separation of 0.3 h −1 Mpc, pairs of early-type galaxies dominate the clustering over all the other types of pairs. At intermediate scales, 0.3−5 h −1 Mpc, mixed pairs of dwarf and giant galaxies contribute equally as pairs of giant galaxies, whereas the latter dominate at 10 h −1 Mpc. Moreover, the correlation functions per galaxy type display the expected transition between the 1-halo and 2-halo regimes in the scenario of hierarchical merging of dark matter halos. The 1-halo component of the early-type galaxies largely outdoes that for the late spiral galaxies, and that for the dwarf galaxies is intermediate between both. In contrast, the 2-halo component of the early-type galaxies and late spiral galaxies are comparable, whereas that for the dwarf galaxies is consistent with null clustering. Conclusions. We link the clustering segregation of the early-type and late spiral galaxies to their spatial distribution within the underlying dark matter halos. The early-type galaxies are preferentially located near the centers of the most massive halos, whereas late spiral galaxies tend to occupy their outskirts or the centers of less massive halos. This appears to be independent of luminosity for the early-type galaxies, whereas faint late spiral galaxies might reside in less dense regions than their bright analogs. The present analysis also unveils unprecedented results on the contribution from dwarf galaxies: at the scale at which they significantly cluster inside the halos (≤0.3 h −1 Mpc), they are poorly mixed with the late spiral galaxies, and appear preferentially as satellites of early-type galaxies.

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Classification and redshift estimation by principal component analysis

Cabanac

Lapparent

Hickson

2002

A&A

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Abstract. We show that the first 10 eigencomponents of the Karhunen-Loève expansion or Principal Component Analysis (PCA) provide a robust classification scheme for the identification of stars, galaxies and quasi-stellar objects from multi-band photometry. To quantify the efficiency of the method, realistic simulations are performed which match the planned Large Zenith Telescope survey. This survey is expected to provide spectral energy distributions with a resolution R 40 for ∼10 6 galaxies to R ≤ 23 (z ∼ 1), ∼ 10 4 QSOs, and ∼ 10 5 stars. We calculate that for a median signal-to-noise ratio of 6, 98% of stars, 100% of galaxies and 93% of QSOs are correctly classified. These values increase to 100% of stars, 100% of galaxies and 100% of QSOs at a median signal-to-noise ratio of 10. The 10-component PCA also allows measurement of redshifts with an accuracy of σRes. < ∼ 0.05 for galaxies with z < ∼ 0.7, and to σRes. < ∼ 0.2 for QSOs with z > ∼ 2, at a median signal-to-noise ratio of 6. At a median signal-to-noise ratio 20, σRes. < ∼ 0.02 for galaxies with z < ∼ 1 and for QSOs with z > ∼ 2.5 (note that for a median S/N ratio of 20, the bluest/reddest objects will have a signal-to-noise ratio of < ∼ 2 in their reddest/bluest filters). This redshift accuracy is inherent to the R 40 resolution provided by the set of medium-band filters used by the Large Zenith Telescope survey. It provides an accuracy improvement of nearly an order of magnitude over the photometric redshifts obtained from broad-band BV RI photometry.

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The ESO-Sculptor Survey: Evolution of late-type galaxies at redshifts 0.1–0.5

Cited by 12 publications

References 100 publications

The VIMOS VLT Deep Survey

The VIMOS VLT Deep Survey

Spatial clustering in the ESO-Sculptor survey: two-point correlation functions by galaxy type at redshifts 0.1–0.5

Classification and redshift estimation by principal component analysis

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