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

Fritz, A.; Jørgensen, Inger; Schiavon, Ricardo P.; Chiboucas, Kristin

doi:10.1002/asna.200911266

Cited by 11 publications

(13 citation statements)

References 49 publications

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“…Similarly for the KR, Studies of the KR at intermediate redshift show changes in Δβ KR consistent with ETGs becoming more luminous with lookback time and the slope generally appears to be unchanged (Barrientos, Schade & Lopez‐Cruz 1996; Pahre, Djorgovski & de Carvalho 1996; Schade et al 1996; Schade, Barrientos & Lopez‐Cruz 1997; Ziegler et al 1999; La Barbera et al 2003; Fritz et al 2005; Holden et al 2005b). Similar conclusions are drawn from the evolution of the FJR (Bender, Ziegler & Bruzual 1996; Ziegler et al 2001, 2005; Fritz et al 2005) and the FP (van Dokkum & Franx 1996; van Dokkum et al 1998, 2001; Kelson et al 2000; Treu et al 2001; van Dokkum & Ellis 2003; Fritz et al 2005, 2009; Holden et al 2005a, 2010; Moran et al 2005; van der Wel et al 2005, 2006; Barr et al 2006; Jørgensen et al 2006; van Dokkum & van der Marel 2007; van der Marel & van Dokkum 2007; Saglia et al 2010).…”

Section: Introductionsupporting

confidence: 75%

“…Recently, there has been debate over the observation of downsizing (Cowie et al 1996; Thomas et al 2005) and the role of selection effects: the study of Holden et al (2010) at z ∼ 0.8 found no evidence that the tilt of the high‐ z FP changes from its local value, which implies that the findings of Jørgensen et al (2006), Fritz et al (2009) and Saglia et al (2010) are biased by selection effects.…”

Section: Introductionmentioning

confidence: 99%

See 1 more Smart Citation

Data and two-dimensional scaling relations for galaxies in Abell 1689: a hint of size evolution at z∼ 0.2

Houghton¹,

Davies²,

Bontà³

et al. 2012

Monthly Notices of the Royal Astronomical Society

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We present imaging and spectroscopy of Abell 1689 (z=0.183) from the GMOS multi-object spectrograph on the Gemini-North telescope and the Advanced Camera for Surveys (ACS) on the Hubble Space Telescope (HST). We measure integrated photometry from the GMOS g ′ and r ′ images (for 531 galaxies) and surface photometry from the HST F625W image (for 43 galaxies) as well as velocities and velocity dispersions from the GMOS spectra (for 71 galaxies). We construct the Kormendy, Faber-Jackson and colour-magnitude relations for early-type galaxies in Abell 1689 using this data and compare them to those of the Coma cluster. We measure the intrinsic scatter of the colour-magnitude relation in Abell 1689 to be σ CMR =0.054 ± 0.004 mag which places degenerate constraints on the ratio of the assembly timescale to the time available (β) and the age of the population. Making the assumption that galaxies in Abell 1689 will evolve into those of Coma over an interval of 2.26 Gyr breaks this degeneracy and limits β to be > 0.6 and the age of the red sequence to be > 5.5 Gyr (formed at z > 0.55). Without corrections for size evolution but accounting for magnitude cuts and selection effects, the Kormendy and Faber-Jackson relations are inconsistent and disagree at the 2σ level regarding the amount of luminosity evolution in the last 2.26 Gyr. However, after correcting for size evolution the Kormendy and Faber-Jackson relations show similar changes in luminosity (0.22 ± 0.11 mag) that are consistent with the passive evolution of the stellar populations from a single burst of star formation 10.2 ± 3.3 Gyr ago (z = 1.8± ∞ 0.9 ). Thus the changes in the Kormendy, Faber-Jackson and colour-magnitude relations of Abell 1689 relative to Coma all agree and suggest old galaxy populations with little or no synchronisation in the star formation histories. Furthermore, the weak evidence for size evolution in the cluster environment in the last 2.26 Gyr places interesting constraints on the possible mechanisms at work, favouring harassment or secular processes over merger scenarios.Key words: for more luminous galaxies, suggesting more massive galaxies are slightly older (by ∼ 0.5 Gyr). We note that Stanford et al. (1998) discuss a gap in the estimates of the CMR scatter between 0.1 < z < 0.3 which, together with their slightly higher CMR scatter at z > 0.3, led them to suggest possible evolution of the CMR scatter during this epoch.

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Section: Introductionsupporting

confidence: 75%

Section: Introductionmentioning

confidence: 99%

Data and two-dimensional scaling relations for galaxies in Abell 1689: a hint of size evolution at z∼ 0.2

Houghton¹,

Davies²,

Bontà³

et al. 2012

Monthly Notices of the Royal Astronomical Society

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“…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). This difference in the zero-point is usually interpreted as a difference in surface brightness caused by luminosity evolution, under the assumption that all early-type galaxies evolve in the same way, i.e.…”

Section: The Fundamental Planesupporting

confidence: 83%

“…According to this, massive galaxies evolve passively on longer time-scales, whereas less massive systems have more extended star-formation histories and continue to form stars at much later epochs. The recent studies of Fritz et al (2009a) for a sample of 24 field galaxies covering redshifts 0.20 < z < 0.75, and Fritz et al (2009b) for a sample of 50 cluster galaxies at z ∼ 1, also support the evolution in the slope of the FP for both field and cluster galaxies, suggesting that the internal properties of a galaxy are more important to its evolutionary history than its enviroment.…”

Section: Introductionmentioning

confidence: 65%

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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“…The BCG of WARPJ1415 is very large, luminous and unusually massive, with a reported stellar mass of 2 × 10 12 M (Fritz et al 2009). The color image obtained with SUBARU-Suprime Cam BRZ (Fig.…”

Section: Connection Between Icm Core Properties and The Bcgmentioning

confidence: 99%

DeepChandraobservation of the galaxy cluster WARPJ1415.1+3612 atz=1

Santos

Tozzi

Rosati

et al. 2012

A&A

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Aims. Using the deepest (370 ks) Chandra observation of a high-redshift galaxy cluster, we perform a detailed characterization of the intra-cluster medium (ICM) of WARPJ1415.1+3612 at z = 1.03, particularly its core region. We also explore the connection between the ICM core properties and the radio/optical properties of the brightest cluster galaxy (BCG). Methods. We perform a spatially resolved analysis of the ICM to obtain temperature, metallicity and surface brightness profiles over the 8-400 kpc radial range. We measure the following cool-core diagnostics: central temperature drop, central metallicity excess, central cooling time, and central entropy. Using the deprojected temperature and density profiles, we accurately derive the cluster hydrostatic mass at different overdensities. In addition to the X-ray data, we use archival radio VLA imaging and optical GMOS spectroscopy of the central galaxy to investigate the feedback between the central galaxy and the ICM. Results. Our spatially resolved spectral analysis shows a significant temperature drop from a maximum of 8.0 keV to a projected core value T c = 4.6 ± 0.4 keV, and a remarkably high central iron abundance peak, Z Fe,c = 3.60 +1.50 −0.85 Z , measured within a radius of 12 kpc. We measure M 500 = M(r < R 500 ) = 2.4 ± 0.4 M and a corresponding gas fraction f gas = 0.10 ± 0.02. The central cooling time is shorter than 0.1 Gyr and the entropy K c is equal to 9.9 keV cm 2 . We detect a strong [OII] emission line in the optical spectra of the BCG with an equivalent width of -25 Å, for which we derive a star formation rate within the range 2-8 M yr −1 . The VLA data reveals a central radio source coincident with the BCG with a luminosity L 1.4 GHz = 2.0 × 10 25 W Hz −1 , and a faint one-sided jet-like feature with an extent of ∼80 kpc. We do not find clear evidence for cavities associated to the radio AGN activity. Conclusions. Our analysis shows that WARPJ1415 has a well developed cool-core with ICM properties similar to those found in the local Universe. Its properties and the clear sign of feedback activity found in the central galaxy in the optical and radio bands, show that feedback processes are already established at z ∼ 1 (a lookback time of 7.8 Gyr). In addition, the presence of a strong metallicity peak shows that the central regions have been promptly enriched by star formation processes in the central galaxy already at z > 1. Our results significantly constrain the timescale for the formation and self-stabilization of cool-cores.

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

Cited by 11 publications

References 49 publications

Data and two-dimensional scaling relations for galaxies in Abell 1689: a hint of size evolution at z∼ 0.2

Data and two-dimensional scaling relations for galaxies in Abell 1689: a hint of size evolution at z∼ 0.2

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

DeepChandraobservation of the galaxy cluster WARPJ1415.1+3612 atz=1

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