The Fundamental Plane for
                    <i>z</i>
                    = 0.8-0.9 Cluster Galaxies

Jørgensen, Inger; Chiboucas, Kristin; Flint, K.; Bergmann, Marcel; Barr, Jordi; Davies, Roger L.

doi:10.1086/501348

Cited by 76 publications

(180 citation statements)

References 26 publications

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“…Several papers have mentioned that the intrinsic dispersion of the FP is small (∼0.1 dex) (Kjaergaard et al 1993;Jørgensen et al 1996;Kelson et al 1997;Jørgensen et al 1999;Blakeslee et al 2002;Bernardi et al 2003c;Reda et al 2005;Jørgensen et al 2006), although other studies demonstrate that the intrinsic dispersion is far from being small (∼0.3 dex) (Bender et al 1992;La Barbera et al 2003;Nigoche-Netro et al 2009). This dispersion causes the galaxy distribution in the space defining the FP to follow a surface whose width is determined by this dispersion.…”

Section: Discussionmentioning

confidence: 99%

“…Nevertheless, their results conflict with those of other authors. For example, Treu et al (2005), Jørgensen et al (2006), and Fritz et al (2009) find that the zero point of the FP depends on redshift but that the slope of the FP is steeper for higher redshift galaxies than for galaxies in the local Universe. They interpret this as a mass dependence of the star formation history, that is, the low-mass galaxies (10 10.3 M ) have experienced star formation as recently as z form ∼ 1.1, while, galaxies with masses ∼10 10.8 M and masses >10 11.3 M had their last major star formation episode at z form > 1.25 and z form > 1.6 (Jørgensen et al 2007).…”

Section: Introductionmentioning

confidence: 99%

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The Faber-Jackson relation for early-type galaxies: dependence on the magnitude range

Nigoche-Netro

Aguerri

Lagos

et al. 2010

A&A

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Aims. Previous studies have found that the coefficients and intrinsic dispersions of both the Kormendy relation and the Fundamental Plane depend on the magnitude range within which the galaxies are contained. We study whether this type of behaviour is also present for the Faber-Jackson relation. Methods. We take a sample of early-type galaxies from the Sloan Digital Sky Survey (SDSS-DR7, ∼90 000 galaxies) spanning a range of approximately 7 mag in both g and r filters and analyse the behaviour of the Faber-Jackson relation parameters as functions of the magnitude range. We calculate the parameters in two ways: i) we consider the faintest (brightest) galaxies in each sample and we progressively increase the width of the magnitude interval by inclusion of the brighter (fainter) galaxies (increasing-magnitudeintervals); and ii) we consider narrow-magnitude intervals of the same width (ΔM = 1.0 mag) over the whole magnitude range available (narrow-magnitude-intervals). Results. Our main results are that: i) in both increasing and narrow-magnitude-intervals the Faber-Jackson relation parameters change systematically, ii) non-parametric tests show that the fluctuations in the values of the slope of the Faber-Jackson relation are not products of chance variations. Conclusions. We conclude that the values of the Faber-Jackson relation parameters depend on the width of the magnitude range and the luminosity of galaxies within the magnitude range. This dependence is caused, to a great extent by the selection effects and because the geometrical shape of the distribution of galaxies on the M − log(σ 0 ) plane depends on luminosity. We therefore emphasize that if the luminosity of galaxies or the width of the magnitude range or both are not taken into consideration when comparing the structural relations of galaxy samples for different wavelengths, environments, redshifts and luminosities, any differences found may be misinterpreted.

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Section: Discussionmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

The Faber-Jackson relation for early-type galaxies: dependence on the magnitude range

Nigoche-Netro

Aguerri

Lagos

et al. 2010

A&A

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“…Since the galaxy M/L depends on both the star formation history of the galaxies and the cosmology, the study of the FP is a valuable tool for studying the evolution of the stellar population in early-type galaxies. Several studies of intermediate (z ∼ 0.3) and high-redshift (z ∼ 0.85) clusters of galaxies have used the ZP shift of the plane to estimate the average formation redshifts of stars in early-type galaxies (e.g., Bender et al 1998;van Dokkum et al 1998;Jørgensen et al 1999;Kelson et al 2000;van Dokkum & Stanford 2003;Wuyts et al 2004;Jørgensen et al 2006). In general, they have all found values compatible with a redshift formation greater than 3.…”

Section: Introductionmentioning

confidence: 99%

“…These differences manifest themselves as an evolution in the FP coefficient α at increasing redshift, from 1.2 (in the B band) at redshift 0.0 to 0.8 at z ∼ 0.8−1.3 (van der Wel et al 2004;Treu et al 2005a,b;van der Wel et al 2005;di Serego Alighieri et al 2005;Holden et al 2005;Jørgensen et al 2006). However, this change in the slope has not been observed at 0.2 < z < 0.8 (e.g., van Dokkum & Franx 1996;Kelson et al 2000;Wuyts et al 2004;van der Marel & van Dokkum 2007b;MacArthur et al 2008).…”

Section: Introductionmentioning

confidence: 99%

The fundamental plane of EDisCS galaxies

Saglia

Sánchez‐Blázquez

Bender

et al. 2010

A&A

108

185

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We study the evolution of spectral early-type galaxies in clusters, groups, and the field up to redshift 0.9 using the ESO Distant Cluster Survey (EDisCS) dataset. We measure structural parameters (circularized half-luminosity radii R e , surface brightness I e , and velocity dispersions σ) for 154 cluster and 68 field galaxies. On average, we achieve precisions of 10% in R e , 0.1 dex in log I e , and 10% in σ. We sample ≈20% of cluster and ≈10% of field spectral early-type galaxies to an I band magnitude in a 1 arcsec radius aperture as faint as I 1 = 22. We study the evolution of the zero point of the fundamental plane (FP) and confirm results in the literature, but now also for the low cluster velocity dispersion regime. Taken at face value, the mass-to-light ratio varies as Δ log M/L B = (−0.54 ± 0.01)z = (−1.61 ± 0.01) log(1 + z) in clusters, independent of their velocity dispersion. The evolution is stronger (Δ log M/L B = (−0.76 ± 0.01)z = (−2.27 ± 0.03) log(1 + z)) for field galaxies. A somewhat milder evolution is derived if a correction for incompleteness is applied. A rotation in the FP with redshift is detected with low statistical significance. The α and β FP coefficients decrease with redshift, or, equivalently, the FP residuals correlate with galaxy mass and become progressively negative at low masses. The effect is visible at z ≥ 0.7 for cluster galaxies and at lower redshifts z ≥ 0.5 for field galaxies. We investigate the size evolution of our galaxy sample. In agreement with previous results, we find that the half-luminosity radius for a galaxy with a dynamical or stellar mass of 2 × 10 11 M varies as (1 + z) −1.0±0.3 for both cluster and field galaxies. At the same time, stellar velocity dispersions grow with redshift, as (1 + z) 0.59±0.10 at constant dynamical mass, and as (1 + z) 0.34±0.14 at constant stellar mass. The measured size evolution reduces to R e ∝ (1 + z) −0.5±0.2 and σ ∝ (1 + z) 0.41±0.08 , at fixed dynamical masses, and R e ∝ (1 + z) −0.68±0.4 and σ ∝ (1 + z) 0.19±0.10 , at fixed stellar masses, when the progenitor bias (PB, galaxies that locally are of spectroscopic early-type, but are not very old, disappear progressively from the EDisCS high-redshift sample; often these galaxies happen to be large in size) is taken into account. Taken together, the variations in size and velocity dispersion imply that the luminosity evolution with redshift derived from the zero point of the FP is somewhat milder than that derived without taking these variations into account. When considering dynamical masses, the effects of size and velocity dispersion variations almost cancel out. For stellar masses, the luminosity evolution is reduced to L B ∝ (1 + z) 1.0 for cluster galaxies and L B ∝ (1 + z) 1.67 for field galaxies. Using simple stellar population models to translate the observed luminosity evolution into a formation age, we find that massive (>10 11 M ) cluster galaxies are old (with a formation redshift z f > 1.5) and lower mass galaxies are 3−4 Gyr younger, in agreement with...

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“…The behaviour of the intrinsic dispersions in the FJR and the KR have not been studied thoroughly because a third variable is believed to cause most of the intrinsic dispersion in both these relations. The intrinsic dispersion in the FP has been barely studied because, it has been assumed to be small (∼0.1 dex, Kjaergaard et al 1993;Jørgensen et al 1996;Kelson et al 1997;Jørgensen et al 1999;Blakeslee et al 2002;Bernardi et al 2003c;Reda et al 2005;Jørgensen et al 2006). However, some studies have found that the intrinsic dispersion is far from small (∼0.3 dex, Bender et al 1992;La Barbera et al 2003;Nigoche-Netro et al 2009).…”

Section: Introductionmentioning

confidence: 99%

The intrinsic dispersion in the Faber-Jackson relation for early-type galaxies as function of the mass and redshift

Nigoche-Netro

Aguerri

Lagos

et al. 2011

A&A

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Context. It has been reported that the intrinsic dispersion at constant magnitude in the structural relations of early-type galaxies is a useful tool to study the universality of these structural relations, that is to say, to study whether the structural relations depend on luminosity, wavelength, redshift, and/or environment. Aims. We study the intrinsic dispersion at approximately constant magnitude in the Faber-Jackson relation as a function of luminosity, mass, and redshift. Methods. We use a sample of approximately 90 000 early-type galaxies from the Sloan Digital Sky Survey (SDSS-DR7) spanning a magnitude range of 7 mag in both g and r filters. We calculate the intrinsic dispersion in the Faber-Jackson relation at approximately constant magnitude and compare this at different luminosities, masses, and redshifts. Results. The main results are the following: i) the intrinsic dispersion in the Faber-Jackson relation depends on the luminosity, mass, and redshift; ii) the distribution for brighter and more massive galaxies has smaller intrinsic dispersion than that for fainter and less massive galaxies; iii) the distribution of bright and massive galaxies at higher redshift has smaller intrinsic dispersion than similar galaxies at low redshift. Conclusions. Comparisons of the results found in this work with recent studies from the literature make us conclude that the intrinsic dispersion in the Faber-Jackson relation could depend on the history of galaxies, in other words, the intrinsic dispersion could depend on the number and nature of transformation events that have affected the galaxies during their life times, such as collapse, accretion, interaction, and merging.

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The Fundamental Plane for z = 0.8-0.9 Cluster Galaxies

Cited by 76 publications

References 26 publications

The Faber-Jackson relation for early-type galaxies: dependence on the magnitude range

The Faber-Jackson relation for early-type galaxies: dependence on the magnitude range

The fundamental plane of EDisCS galaxies

The intrinsic dispersion in the Faber-Jackson relation for early-type galaxies as function of the mass and redshift

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