Quantitative Morphology of Galaxies in the Core of the Coma Cluster

Gutiérrez, Carlos M.; Trujillo, Ignacio; Aguerri, J. A. L.; Graham, Alister W.; Caon, N.

doi:10.1086/381022

Cited by 69 publications

(91 citation statements)

References 74 publications

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“…3 shows the size distribution, vs. R band magnitude (shifted to z = 0.22 assuming the concordance cosmology and a passively evolving model as described above), for all galaxies in the CLASH cluster sample and the sample from Paper I. The appearance of the distribution is similar to that found in local systems (e.g., Coma in Gutiérrez et al 2004), with a cloud of systems at intermediate sizes of 1-2 kpc and a brighter sequence of large, luminous galaxies; these latter objects tend to be high n early-type spheroiddominated galaxies (classical E/S0). We compare the size distributions of galaxies brighter than Rz=0.22 = 21 in the right-hand panel of Fig.…”

Section: Structural Parameter Evolutionmentioning

confidence: 57%

Morphological evolution of cluster red sequence galaxies in the past 9 Gyr

Propris¹,

Bremer²,

Phillipps³

2016

Mon. Not. R. Astron. Soc.

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Galaxies arrive on the red sequences of clusters at high redshift (z > 1) once their star formation is quenched and evolve passively thereafter. However, we have previously found that cluster red sequence galaxies (CRSGs) undergo significant morphological evolution subsequent to the cessation of star formation, at some point in the past 9-10 Gyr. Through a detailed study of a large sample of cluster red sequence galaxies spanning 0.2 < z < 1.4 we elucidate the details of this evolution. Below z ∼ 0.5 − 0.6 (in the last 5-6 Gyr) there is little or no morphological evolution in the population as a whole, unlike in the previous 4-5 Gyrs. Over this earlier time (i) disklike systems with Sérsic n < 2 progressively disappear, as (ii) the range of their axial ratios similarly decreases, removing the most elongated systems (those consistent with thin disks seen at an appreciable inclination angle), and (iii) radial colour gradients (bluer outwards) decrease in an absolute sense from significant age-related gradients to a residual level consistent with the metallicity-induced gradients seen in low redshift cluster members. The distribution of their effective radii shows some evidence of evolution, consistent with growth of at most a factor < 1.5 between z ∼ 1.4 and z ∼ 0.5, significantly less than for comparable field galaxies, while the distribution of their central (< 1kpc) bulge surface densities shows no evolution at least at z < 1. A simple model involving the fading and thickening of a disk component after comparatively recent quenching (after z ∼ 1.5) around an otherwise passively evolving older spheroid component is consistent with all of these findings.

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Section: Structural Parameter Evolutionmentioning

confidence: 57%

Morphological evolution of cluster red sequence galaxies in the past 9 Gyr

Propris¹,

Bremer²,

Phillipps³

2016

Mon. Not. R. Astron. Soc.

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“…However, other studies show that the structural relations depend on wavelength (Jørgensen et al 1996;Hudson et al 1997;Pahre et al 1998;Scodeggio et al 1998;Jun & Im 2008). -As far as the environment is concerned, several studies imply that the structural relations and/or the structural parameters of galaxies are affected by the environment (Bender et al 1992(Bender et al , 1998Trujillo et al 2001Trujillo et al , 2002Bernardi et al 2003b;Aguerri et al 2004;Gutiérrez et al 2004;Denicoló et al 2005;Jørgensen et al 2005), although other studies reach exactly the opposite conclusion (de la Rosa et al 2001;Treu et al 2001;Evstigneeva et al 2002;Gonzáles-García & van Albada 2003;Reda et al 2004Reda et al , 2005Nigoche-Netro et al 2007). …”

Section: Discussionmentioning

confidence: 99%

“…Several studies have also discovered that the structural relations and/or the structural parameters of galaxies are affected by the environment (Bender et al 1992(Bender et al , 1998Trujillo et al 2001Trujillo et al , 2002Bernardi et al 2003b;Aguerri et al 2004;Gutiérrez et al 2004;Denicoló et al 2005;Jørgensen et al 2005), although other studies have reached exactly the opposite conclusion (de la Rosa et al 2001;Treu et al 2001;Evstigneeva et al 2002;Gonzáles-García & van Albada 2003;Reda et al 2004Reda et al , 2005Nigoche-Netro et al 2007). This second set of results suggest that galaxies very quickly absorb the changes caused by gravitational interactions, not keeping memory of these changes in regard to the structural relations.…”

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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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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“…In these, the stellar scale lengths of the disc galaxies were measured to be 20−30% smaller than those in the field Gutiérrez et al 2004;Koopmann et al 2006). The stellar population properties make a decomposition into bulge and disc galaxies necessary.…”

Section: Introductionmentioning

confidence: 99%

Disc colours in field and cluster spiral galaxies at 0.5 ≲z≲ 0.8

Cantale

Jablonka

Courbin

et al. 2016

A&A

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We present a detailed study of the colours of late-type galaxy discs for ten of the EDisCS galaxy clusters with 0.5 z 0.8. Our cluster sample contains 172 spiral galaxies, and our control sample is composed of 96 field disc galaxies. We deconvolved their ground-based V and I images obtained with FORS2 at the VLT with initial spatial resolutions between 0.4 and 0.8 arcsec to achieve a final resolution of 0.1 arcsec with 0.05 arcsec pixels, which is close to the resolution of the ACS at the HST. After removing the central region of each galaxy to avoid pollution by the bulges, we measured the V − I colours of the discs. We find that 50% of cluster spiral galaxies have disc V − I colours redder by more than 1σ of the mean colours of their field counterparts. This is well above the 16% expected for a normal distribution centred on the field disc properties. The prominence of galaxies with red discs depends neither on the mass of their parent cluster nor on the distance of the galaxies to the cluster cores. Passive spiral galaxies constitute 20% of our sample. These systems are not abnormally dusty. They are are made of old stars and are located on the cluster red sequences. Another 24% of our sample is composed of galaxies that are still active and star forming, but less so than galaxies with similar morphologies in the field. These galaxies are naturally located in the blue sequence of their parent cluster colour-magnitude diagrams. The reddest of the discs in clusters must have stopped forming stars more than ∼5 Gyr ago. Some of them are found among infalling galaxies, suggesting preprocessing. Our results confirm that galaxies are able to continue forming stars for some significant period of time after being accreted into clusters, and suggest that star formation can decline on seemingly long (1 to 5 Gyr) timescales.

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Quantitative Morphology of Galaxies in the Core of the Coma Cluster

Cited by 69 publications

References 74 publications

Morphological evolution of cluster red sequence galaxies in the past 9 Gyr

Morphological evolution of cluster red sequence galaxies in the past 9 Gyr

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

Disc colours in field and cluster spiral galaxies at 0.5 ≲z≲ 0.8

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