The DEEP Groth Strip Survey. IX. Evolution of the Fundamental Plane of Field Galaxies

Gebhardt, Karl; Faber, S. M.; Koo, David C.; Im, Myungshin; Simard, Luc; Illingworth, G. D.; Phillips, Andrew C.; Sarajedini, Vicki L.; Vogt, Nicole P.; Weiner, Benjamin J.; Willmer, Christopher N. A.

doi:10.1086/378401

Cited by 113 publications

(191 citation statements)

References 48 publications

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“…3 we present the edge-on projection of the FP in the local (left) and high-redshift samples (right), in addition to the zeropoint and total rms scatter obtained in each case. For our local sample we obtained a zeropoint of c = −9.093, which agrees well with the previous result of Gebhardt et al (2003) (−9.062); and the resulting rms scatter σ tot = 0.113 is not significantly higher than the local value (∼0.1 dex; Fritz et al 2005). However, we found a different FP intercept for the high-redshift galaxies, according to previous studies of FP evolution (for example Gebhardt et al 2003;Fritz et al 2009b).…”

Section: The Fundamental Planesupporting

confidence: 91%

“…In addition, found that the M/L ratios of field galaxies evolves as Δ ln(M/L B ) = (−1.35 ± 0.35)z, similar to cluster galaxies. In contrast, the studies at higher redshift of Treu et al (2002) and Gebhardt et al (2003) found a greater brightening for field galaxies than the one found for cluster galaxies. Restricting the Gebhardt et al (2003) sample to galaxies at z = 0.4, the B luminosities of early-type galaxies would have been ∼0.7 mag brighter than nowadays, which was attributed to a more recent formation epoch of around z = 1.5.…”

Section: Introductioncontrasting

confidence: 68%

“…They found a good correlation between both measures by using a maximum-penalized likelihood approach and a set of stellar templates of 12 Galactic A main-sequence through K giant stars. In addition, Gebhardt et al (2003) obtained good agreement between the internal kinematic measured separately over the G and the H+K regions using the same procedure for a sample of early-type galaxies. Nevertheless, choosing an appropriate set of stellar templates is of the utmost importance to obtain a reliable kinematic from the H+K region (Kobulnicky & Gebhardt 2000).…”

Section: Velocity Dispersionmentioning

confidence: 71%

“…This number of galaxies is insufficient for determining the local FP parameters, but it can be used to calibrate the local FP used as comparison to the high-redshift galaxies, since both samples were analysed following the same procedure. We accordingly adopt for the local coefficients the same values used by Gebhardt et al (2003) and Fritz et al (2009a) in the rest-frame B-band: a = 1.25 and b = 0.32, and calculated the zeropoint c for the local and highredshift samples by using a non-linear weighted least-squares fit. These a and b values were obtained by these authors from the local samples of Faber et al (1989) and Saglia et al (1993) respectively, using the same cosmology that we adopted in the present work.…”

Section: The Fundamental Planementioning

confidence: 99%

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Evolution of the fundamental plane of 0.2 < z < 1.2 early-type galaxies in the EGS

Lorenzo

Cepa

Bongiovanni

et al. 2010

A&A

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Context. The fundamental plane links the structural properties of early-type galaxies such as its surface brightness and effective radius with its dynamics. The study of the fundamental plane evolution therefore has important implications for models of galaxy formation and evolution. Aims. This work aims to identify signs of evolution of early-type galaxies through the study of parameter correlations such as the fundamental plane, the Kormendy, and the Faber-Jackson relations, using a sample of 135 field galaxies extracted from the Extended Groth Strip in the redshift range 0.2 < z < 1.2. Methods. We calculate the internal velocity dispersions with DEEP2 data by extracting the stellar kinematics from absorption line spectra, using a maximum penalized-likelihood approach. Morphology was determined through visual classification of the V + I images of ACS. The structural parameters of these galaxies were obtained by fitting de Vaucouleurs stellar profiles to the ACS I-band images with the GALFIT code. To check the effect on the fundamental plane of the structural parameters, Sérsic and bulge-to-disc decomposition models were fitted to our sample of galaxies. A good agreement was found in the fundamental plane derived from the three models. Results. Assuming that effective radii and velocity dispersions do not evolve with redshift, we found a brightening of 0.68 mag in the B-band and 0.52 mag in the g-band at z = 0.7. However, the scatter in the fundamental plane for our high-redshift sample is reduced by half when we allow the fundamental plane slope to evolve, suggesting a different evolution of early-type galaxies according to their intrinsic properties such as total mass, size, or luminosity. The study of the Kormendy relation shows a population of very compact (R e < 2 Kpc) and bright galaxies (−21.5 > M g > −22.5), of which there are only a small fraction (0.4%) at z = 0. Studying the luminosity-size and stellar mass-size relations, we show that the evolution of these compact objects is mainly caused by an increase in size that could be explained by the action of dry minor mergers. We also detect an evolution in the fundamental plane caused mainly by this population of very compact and bright galaxies. Unfortunately, we cannot distinguish a change in the slope from an increase in the scatter of the fundamental plane because our high-redshift sample is biased to the brightest objects.

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Section: The Fundamental Planesupporting

confidence: 91%

Section: Introductioncontrasting

confidence: 68%

Section: Velocity Dispersionmentioning

confidence: 71%

Section: The Fundamental Planementioning

confidence: 99%

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Evolution of the fundamental plane of 0.2 < z < 1.2 early-type galaxies in the EGS

Lorenzo

Cepa

Bongiovanni

et al. 2010

A&A

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“…In the local Universe, red early-type galaxies are the dominant population in rich galaxy clusters, while blue late-type galaxies are the dominant population in the low-density field. Not only galaxy properties, but the formation epoch of galaxies also depends on environment in the sense that cluster galaxies form earlier than field galaxies (e.g., Kuntschner et al 2002;Gebhardt et al 2003;Thomas et al 2005). Earlier studies concentrated on nearby galaxies, but with the recent advent of large telescopes, environment studies at z ∼ 1 became possible.…”

Section: Introductionmentioning

confidence: 99%

The environmental dependence of galaxy properties atz = 2

Tanaka¹,

Breuck²,

Venemans³

et al. 2010

A&A

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We report on the environmental dependence of galaxy properties at z = 2.15. We construct multi-band photometric data sets in the (proto-)cluster PKS1138-26 field and in the GOODS field. We then fit spectral energy distributions of the galaxies with model templates generated with the latest stellar population synthesis code and derive physical properties of galaxies from the fits. To quantify the environmental dependence of galaxy properties, a special care is taken of systematic errors -we use data sets that have almost the same wavelength samplings, use the same code to fit SEDs with the same set of templates, and compare relative differences between the two samples. We find that the PKS1138 galaxies have similar ages, shorter star formation time scales, lower star formation rates, and weaker dust extinction compared to the GOODS galaxies at z ∼ 2. This trend is similar to that observed locally, suggesting that the environmental dependence of galaxy properties is already partly in place as early as z = 2.15. We show that the PKS1138 galaxies assemble the bulk of their masses ∼1 Gyr earlier than field galaxies, i.e., the galaxy formation depends on environment. Galaxy mergers should frequently occur during the first collapse of clusters and they might play an important role in driving the observed environmental dependence of galaxy properties at z = 2.15.

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The evolution of cluster early‐type galaxies over the past 8 Gyr

et al. 2009

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We present the Fundamental Plane (FP) of early-type galaxies in the clusters of galaxies RXJ1415.1+3612 at z = 1.013. This is the first detailed FP investigation of cluster early-type galaxies at redshift z = 1. The distant cluster galaxies follow a steeper FP relation compared to the local FP. The change in the slope of the FP can be interpreted as a massdependent evolution. To analyse in more detail the galaxy population in high redshift galaxy clusters at 0.8 < z < 1, we combine our sample with a previous detailed spectroscopic study of 38 early-type galaxies in two distant galaxy clusters, RXJ0152.7-1357 at z = 0.83 and RXJ1226.9+3332 at z = 0.89. For all clusters Gemini/GMOS spectroscopy with high signal-to-noise and intermediate-resolution has been acquired to measure the internal kinematics and stellar populations of the galaxies. From HST/ACS imaging, surface brightness profiles, morphologies and structural parameters were derived for the galaxy sample. The least massive galaxies (M = 2×10 10 M ) in our sample have experienced their most recent major star formation burst at z form ∼ 1.1. For massive galaxies (M > 2×10 11 M ) the bulk of their stellar populations have been formed earlier z form > ∼ 1.6. Our results confirm previous findings by Jørgensen et al. This suggests that the less massive galaxies in the distant clusters have much younger stellar populations than their more massive counterparts. One explanation is that low-mass cluster galaxies have experienced more extended star formation histories with more frequent bursts of star formation with shorter duration compared to the formation history of high-mass cluster galaxies.

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The DEEP Groth Strip Survey. IX. Evolution of the Fundamental Plane of Field Galaxies

Cited by 113 publications

References 48 publications

Evolution of the fundamental plane of 0.2 < z < 1.2 early-type galaxies in the EGS

Evolution of the fundamental plane of 0.2 < z < 1.2 early-type galaxies in the EGS

The environmental dependence of galaxy properties atz = 2

The evolution of cluster early‐type galaxies over the past 8 Gyr

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