COSMOS Morphological Classification with the Zurich Estimator of Structural Types (ZEST) and the Evolution Since
                    <i>z</i>
                    = 1 of the Luminosity Function of Early, Disk, and Irregular Galaxies

Scarlata, Claudia; Carollo, C. M.; Lilly, S. J.; Sargent, M.; Feldmann, Robert; Kampczyk, P.; Porciani, Cristiano; Koekemoer, Anton M.; Scoville, N. Z.; Kneib, Jean-Paul; Leauthaud, Alexie; Massey, Richard; Rhodes, Jason; Tasca, L.; Capak, P.; Maier, C.; McCracken, H. J.; Mobasher, Bahram; Renzini, A.; Taniguchi, Y.; Thompson, D. J.; Sheth, Kartik; Ajiki, Masaru; Aussel, H.; Murayama, Takashi; Sanders, D. B.; Sasaki, S.; Shioya, Yasuhiro; Takahashi, Mari

doi:10.1086/516582

Cited by 234 publications

(141 citation statements)

References 55 publications

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“…Therefore, for consistency, we decided to simply use Sersic indices (n) to compare the structures (morphologies) of zCOSMOS and SDSS galaxies. As is well known (e.g., Blanton et al 2003a;Scarlata et al 2007) n > 2.5 galaxies correspond mostly to galaxies classified as early-types spheroid-dominated galaxies, while n < 1.5 galaxies are mostly objects classified as late-type diskdominated galaxies.…”

Section: Structural Parametersmentioning

confidence: 58%

“…Automated morphological classifications using the ZEST scheme (ZEST; Scarlata et al 2007) are also available.…”

Section: Sample Selectionmentioning

confidence: 99%

“…Although the ZEST automated morphological classification (Scarlata et al 2007) is available for the entire zCOSMOS sample, it has not been applied to the SDSS. Therefore, for consistency, we decided to simply use Sersic indices (n) to compare the structures (morphologies) of zCOSMOS and SDSS galaxies.…”

Section: Structural Parametersmentioning

confidence: 99%

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THE DEPENDENCE OF STAR FORMATION ACTIVITY ON STELLAR MASS SURFACE DENSITY AND SERSIC INDEX IN zCOSMOS GALAXIES AT 0.5 <z< 0.9 COMPARED WITH SDSS GALAXIES AT 0.04 <z< 0.08

Maier

Lilly

Zamorani

et al. 2009

ApJ

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In order to try to understand the internal evolution of galaxies and relate this to the global evolution of the galaxy population, we present a comparative study of the dependence of star formation rates on the average surface mass densities (Σ M ) of galaxies at 0.5 < z < 0.9 and 0.04 < z < 0.08, using the zCOSMOS and Sloan Digital Sky Survey (SDSS) surveys, respectively. We derive star formation rates, stellar masses, and structural parameters in a consistent way for both samples, and apply them to samples that are complete down to the same stellar mass at both redshifts. We first show that the characteristic step-function dependence of median specific star formation rate (SSFR) on Σ M in SDSS, seen by Brinchmann et al., is due to the change over from predominantly disk galaxies to predominantly spheroidal galaxies at the surface mass density logΣ Mchar ∼8.5 at which the SSFR is seen to drop. Turning to zCOSMOS, we find a similar shape for the median SSFR-Σ M relation, but with median SSFR values that are about 5-6 times higher than for SDSS, across the whole range of Σ M , and in galaxies with both high and low Sersic indices. This emphasizes that galaxies of all types are contributing, proportionally, to the global increase in star formation rate density in the Universe back to these redshifts. The Σ Mchar "step" shifts to slightly higher values of Σ M in zCOSMOS relative to SDSS, but this can be explained by a modest differential evolution in the size-mass relations of disk and spheroid galaxies. For low Sersic index galaxies, there is little change in the size-mass relation, as seen by Barden et al., although we suggest that this does not necessarily imply inside-out growth of disks, at least not in this redshift range. On the other hand, there is a modest evolution in the stellar mass-size relation for high Sersic index galaxies, with galaxies smaller by ∼25% at z ∼ 0.7. Taken together these produce a modest increase in Σ Mchar . Low Sersic index galaxies have a SSFR that is almost independent of Σ M , and the same is probably also true of high Sersic index galaxies once obvious disk systems are excluded.

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Section: Structural Parametersmentioning

confidence: 58%

“…Automated morphological classifications using the ZEST scheme (ZEST; Scarlata et al 2007) are also available.…”

Section: Sample Selectionmentioning

confidence: 99%

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THE DEPENDENCE OF STAR FORMATION ACTIVITY ON STELLAR MASS SURFACE DENSITY AND SERSIC INDEX IN zCOSMOS GALAXIES AT 0.5 <z< 0.9 COMPARED WITH SDSS GALAXIES AT 0.04 <z< 0.08

Maier

Lilly

Zamorani

et al. 2009

ApJ

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“…For the purposes of this paper, we consider the 'environment' of a galaxy to be defined by the local mass overdensity, measured using the local overdensity of galaxies as a proxy; over quasi-linear 1 It should be noted that other studies have arrived at different conclusions regarding the evolution in the early-type luminosity density (e.g. Scarlata et al 2007a), especially at the massive end of the red sequence (Scarlata et al 2007b). 2 There is some debate within the community regarding the evolution in the number density of blue galaxies at intermediate and low redshift.…”

Section: Measurements Of Local Galaxy Environmentmentioning

confidence: 99%

The DEEP2 Galaxy Redshift Survey: the role of galaxy environment in the cosmic star formation history

Cooper

Newman

Weiner

et al. 2007

Monthly Notices of the Royal Astronomical Society

244

206

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Using galaxy samples drawn from the Sloan Digital Sky Survey and the DEEP2 Galaxy Redshift Survey, we study the relationship between star formation and environment at z∼ 0.1 and 1. We estimate the total star formation rate (SFR) and specific star formation rate (sSFR) for each galaxy according to the measured [O ii]λ 3727 Å nebular line luminosity, corrected using empirical calibrations to match more robust SFR indicators. Echoing previous results, we find that in the local Universe star formation depends on environment such that galaxies in regions of higher overdensity, on average, have lower SFRs and longer star formation time‐scales than their counterparts in lower density regions. At z∼ 1, we show that the relationship between sSFR and environment mirrors that found locally. However, we discover that the relationship between total SFR and overdensity at z∼ 1 is inverted relative to the local relation. This observed evolution in the SFR–density relation is driven, in part, by a population of bright, blue galaxies in dense environments at z∼ 1. This population, which lacks a counterpart at z∼ 0, is thought to evolve into members of the red sequence from z∼ 1 to ∼0. Finally, we conclude that environment does not play a dominant role in the cosmic star formation history at z < 1: the dependence of the mean galaxy SFR on local galaxy density at constant redshift is small compared to the decline in the global SFR space density over the last 7 Gyr.

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“…After the initial work by Abraham et al (1994Abraham et al ( , 1996, the Concentration-Asymmetry-Smoothness (CAS) space was established by Conselice (2003) and the Gini and Asymmetry parameters by Lotz et al (2004). Scarlata et al (2007) added ellipticity for Hubble type classification. The benefits of quantified morphology parameters are that there is no need for an observer, they can be applied to rest-frame UV images, which trace the triggered star-formation in interacting galaxies and the galaxies have an intrinsically high surface brightness, aiding their detection.…”

Section: Quantified Morphologymentioning

confidence: 99%

HI Disks in the high-redshift Universe; Size and Quantified Morphology

Holwerda¹,

Blok²,

Bouchard³

et al. 2010

Proceedings of Panoramic Radio Astronomy: Wide-Field 1-2 GHz Research on Galaxy Evolution — PoS(PRA2009)

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The upcoming new perspective of the high redshift Universe in the 21 cm line of atomic hydrogen opens possibilities to explore topics of spiral disk evolution, hitherto reserved for the optical regime. The growth of spiral gas disks over Cosmic time can be explored with the new generation of radio telescopes, notably the SKA, and its precursors, as accurately as with the Hubble Space Telescope for stellar disks. Since the atomic hydrogen gas is the building block of these disks, it should trace their formation accurately. Morphology of H I disks can now equally be quantified over Cosmic time. In studies of HST deep fields, the optical or UV morphology of high-redshift galaxy disks have been characterised using a few quantities: concentration (C), asymmetry (A), smoothness (S), second-order-moment (M 20 ), the GINI coefficient (G), and Ellipticity (E). We have applied these parameters across wavelengths and compared them to the HI morphology over the THINGS sample. NGC 3184, an unperturbed disk, and NGC 5194, the canonical 3:1 interaction, serve as examples for quantified morphology. We find that morphology parameters determined in H I are as good or better a tracer of interaction compared to those in any other wavelength, notably in Asymmetry, Gini and M 20 . This opens the possibility of using them in the parameterization pipeline for SKA precursor catalogues to select interacting or harassed galaxies from their H I morphology. Asymmetry, Gini and M 20 may be redefined for use on data-cubes rather than H I column density image.

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COSMOS Morphological Classification with the Zurich Estimator of Structural Types (ZEST) and the Evolution Since z = 1 of the Luminosity Function of Early, Disk, and Irregular Galaxies

Cited by 234 publications

References 55 publications

THE DEPENDENCE OF STAR FORMATION ACTIVITY ON STELLAR MASS SURFACE DENSITY AND SERSIC INDEX IN zCOSMOS GALAXIES AT 0.5 <z< 0.9 COMPARED WITH SDSS GALAXIES AT 0.04 <z< 0.08

THE DEPENDENCE OF STAR FORMATION ACTIVITY ON STELLAR MASS SURFACE DENSITY AND SERSIC INDEX IN zCOSMOS GALAXIES AT 0.5 <z< 0.9 COMPARED WITH SDSS GALAXIES AT 0.04 <z< 0.08

The DEEP2 Galaxy Redshift Survey: the role of galaxy environment in the cosmic star formation history

HI Disks in the high-redshift Universe; Size and Quantified Morphology

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