<i>Hubble Space Telescope</i>Imaging of the CFRS and LDSS Redshift Surveys. I. Morphological Properties

Brinchmann, Jarle; Abraham, Roberto; Schade, David; Tresse, L.; Ellis, Richard S.; Lilly, S. J.; Fèvre, O. Le; Glazebrook, Karl; Hammer, F.; Colless, Matthew; Crampton, D.; Broadhurst, T.

doi:10.1086/305621

Cited by 209 publications

(309 citation statements)

References 36 publications

(48 reference statements)

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“…11). In contrast, none of our Groth Strip QS-E/S0's are classified as non-E/S0's by Brinchmann et al (1998). Thus, we conclude that our method is somewhat more conservative than the AC method in picking up only morphologically featureless E/S0's.…”

Section: No 1 2002mentioning

confidence: 68%

“…E/S0's in Im et al (1999) are selected as galaxies that have a significant bulge (B=Te0:3) and appear morphologically featureless when visually classified. They present redshift distributions of various galaxy types and find that that of E/S0's is consistent with no number density evolution out to z $ 1 (for similar works, see Roche et al 1998;Driver et al 1998;Brinchmann et al 1998). However, the number of early-type galaxies in both of these studies is small (about 40), and thus it is difficult to draw firm conclusions.…”

Section: Introductionmentioning

confidence: 82%

“…Studies of early-type galaxies by Brinchmann et al (1998) and Schade et al (1999) have included objects from a part of the GSS. Using these overlaps, we compare our selection criteria with theirs.…”

Section: Comparison With Previous Studiesmentioning

confidence: 99%

“…Currently, the determination of redshifts of I $ 22 early-type galaxies is feasible with ground-based telescopes of aperture e4 m (Koo et al 1996;Lilly et al 1995;Cowie et al 1996;Cohen et al 1996Cohen et al , 2000. Moreover, previous studies have shown that morphological classification of faint galaxies is possible down to I ' 22:5 using Hubble Space Telescope (HST) images with exposure times e1 hr (Griffiths et al 1994a(Griffiths et al , 1994bDriver, Windhorst, & Griffiths 1995;Glazebrook et al 1995;Im et al 1996Im et al , 1995aAbraham et al 1996;Brinchmann et al 1998;Schade et al 1999;Im, Griffiths, & Ratnatunga 2000;Roche et al 1996Roche et al , 1998. Thus, in principle, a combination of HST imaging and spectroscopy using large ground-based telescopes can provide the data to constrain the number-density evolution of E/ S0's at z < 1.…”

Section: Introductionmentioning

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: No 1 2002mentioning

confidence: 68%

Section: Introductionmentioning

confidence: 82%

Section: Comparison With Previous Studiesmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

See 2 more Smart Citations

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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“…A large sample of faint galaxies with spectroscopic redshift is quite difficult to obtain at high redshift, but is necessary to properly estimate the environment. Intermediate depth surveys with HST combined with ground based spectroscopy have shown that the Hubble sequence is in place at z ∼ 1 (e.g., Lilly et al 1995;Abraham et al 1996;Brinchmann et al 1998;Abraham et al 2007). Likewise, deep observations at high resolution were difficult to achieve before the advent of the Hubble Space Telescope (HST) Advanced Camera for Survey (ACS).…”

Section: Introductionmentioning

confidence: 99%

The zCOSMOS redshift survey: the role of environment and stellar mass in shaping the rise of the morphology-density relation from z ~ 1

Tasca

Kneib²,

Iovino

et al. 2009

A&A

152

146

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Context. For more than two decades we have known that galaxy morphological segregation is present in the Local Universe. It is important to see how this relation evolves with cosmic time. Aims. To investigate how galaxy assembly took place with cosmic time, we explore the evolution of the morphology-density relation up to redshift z ∼ 1 using about 10 000 galaxies drawn from the zCOSMOS Galaxy Redshift Survey. Taking advantage of accurate HST/ACS morphologies from the COSMOS survey, of the well-characterised zCOSMOS 3D environment, and of a large sample of galaxies with spectroscopic redshift, we want to study here the evolution of the morphology-density relation up to z ∼ 1 and its dependence on galaxy luminosity and stellar mass. The multi-wavelength coverage of the field also allows a first study of the galaxy morphological segregation dependence on colour. We further attempt to disentangle between processes that occurred early in the history of the Universe or late in the life of galaxies. Methods. The zCOSMOS field benefits of high-resolution imaging in the F814W filter from the Advanced Camera for Survey (ACS). We use standard morphology classifiers, optimised for being robust against band-shifting and surface brightness dimming, and a new, objective, and automated method to convert morphological parameters into early, spiral, and irregular types. We use about 10 000 galaxies down to I AB = 22.5 with a spectroscopic sampling rate of 33% to characterise the environment of galaxies up to z ∼ 1 from the 100 kpc scales of galaxy groups up to the 100 Mpc scales of the cosmic web. The evolution of the morphology-density relation in different environments is then studied for luminosity and stellar-mass selected, volume-limited samples of galaxies. The trends are described and related to the various physical processes that could play a relevant role in the build-up of the morphology-density relation. Results. We confirm that the morphological segregation is present up to z ∼ 1 for luminosity-selected, volume-limited samples. The behaviour of the morphology-density relation gets flatter at fixed masses expecially above 10 10.6 M . We suggest the existence of a critical mass above which the physical processes governing galaxy stellar mass also determine the shaping of the galaxy more than its environment. We finally show that at a fixed morphology there is still a residual variation in galaxy colours with density. Conclusions. The observed evolution with redshift of the morphology-density relation offers an opportunity to trace the effect of nature and nurture as a function of environment. Even though it is based mainly on a biased view, the environmental dependence of the morphological evolution for luminosity-selected, volume-limited samples seems to indicate that nurture is in play. On the other hand, the lack of evolution observed for earlytype and spiral galaxies that are more massive than 10 10.8 M independents of the environment indicates that nature has imprinted these properties early in the life of...

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Observations of an Evolving Universe

Springer Praxis Books

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Hubble Space TelescopeImaging of the CFRS and LDSS Redshift Surveys. I. Morphological Properties

Cited by 209 publications

References 36 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

The zCOSMOS redshift survey: the role of environment and stellar mass in shaping the rise of the morphology-density relation from z ~ 1

Observations of an Evolving Universe

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