The Fundamental Plane in RX J0142.0+2131: A Galaxy Cluster Merger at [FORMULA][F]z=0.28[/F][/FORMULA]

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

doi:10.1086/508257

Cited by 19 publications

(25 citation statements)

References 28 publications

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“…-When structural relations of galaxy samples are studied at different redshifts, several studies indicate that only the zero point of these relations depends on the redshift (Barger et al 1998;Ziegler et al 1999;La Barbera et al 2003;Barr et al 2006). Other authors find that there is a dependence of the zero point on redshift but that the slopes of the structural relations are steeper for higher redshift galaxies than for galaxies in the local Universe (Treu et al 2005;Jørgensen et al 2006;Fritz et al 2009).…”

Section: Discussionmentioning

confidence: 99%

“…When the structural relations are constructed for galaxy samples at different redshifts, several studies report similarly (Barger et al 1998;Ziegler et al 1999;La Barbera et al 2003;Barr et al 2006) that only the zero point of these relations depends on the redshift and this dependence may be caused by the passive evolution of the stellar populations that form at high redshift (z form > 2). Nevertheless, their results conflict with those of other authors.…”

Section: Introductionmentioning

confidence: 95%

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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: 95%

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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“…This cluster has a velocity dispersion of 1278 ± 134 km s −1 ; however, no substructure in the velocity distribution (Barr et al 2005). Based on the mass-to-light ratios of galaxies and α-element abundance ratios, a possibility of a past merger in the cluster has been inferred (Barr et al 2006). …”

Section: Rx J01420+2131mentioning

confidence: 94%

The Extended GMRT Radio Halo Survey

Kale

Venturi

Giacintucci

et al. 2013

A&A

122

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Context. A fraction of galaxy clusters host diffuse radio sources called radio halos, radio relics and mini-halos. These are associated with the relativistic electrons and magnetic fields present on ∼Mpc scales in the intra-cluster medium. Aims. We aim to carry out a systematic radio survey of all luminous galaxy clusters selected from the REFLEX and eBCS X-ray catalogues with the Giant Metrewave Radio Telescope, to understand the statistical properties of the diffuse radio emission in galaxy clusters. Methods. We present the sample and first results from the Extended GMRT Radio Halo Survey (EGRHS), which is an extension of the GMRT Radio Halo Survey (GRHS, Venturi et al. 2007. Analysis of radio data at 610/ 235/ 325 MHz on 12 galaxy clusters are presented. Results. We report the detection of a newly discovered mini-halo in the cluster RX J1532.9+3021 at 610 MHz. The presence of a small-scale relic (∼200 kpc) is suspected in the cluster Z348. We do not detect cluster-scale diffuse emission in 11 clusters. Robust upper limits on the detection of radio halo of size of 1 Mpc are determined. We also present upper limits on the detections of minihalos in a sub-sample of cool-core clusters. The upper limits for radio halos and mini-halos are plotted in the radio power-X-ray luminosity plane and the correlations are discussed. Diffuse extended emission that is not related to the target clusters, but detected as by-products in the sensitive images of two of the cluster fields (A689 and RX J0439.0+0715) is also reported. Conclusions. Based on the information about the presence of radio halos (or upper limits), available on 48 clusters out of the total sample of 67 clusters (EGRHS+GRHS), we find that 23±7% of the clusters host radio halos. The radio halo fraction rises to 31±11%, when only the clusters with X-ray luminosities >8 × 10 44 erg s −1 are considered. Mini-halos are found in ∼50% of cool-core clusters. A qualitative examination of the X-ray images of the clusters with no diffuse radio emission indicates that a majority of these clusters do not show extreme dynamical disturbances and supports the idea that mergers play an important role in generating radio halos and relics. The analysis of the full sample will be presented in a future work.

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“…Studies of rich clusters at intermediate redshift show that S0s must have undergone starbursts in the not too distant past (e.g. Treu et al 2003;Dressler et al 2004;McIntosh et al 2004;Barr et al 2006). Other studies favouring the "violent" formation scenario show tidally-induced star formation (e.g.…”

Section: Comparison With Other Studiesmentioning

confidence: 99%

The formation of S0 galaxies: evidence from globular clusters

Barr¹,

Bedregal²,

Aragón-Salamanca³

et al. 2007

A&A

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Aims. We devise a simple experiment to test the theory that lenticular (S0) galaxies form from spirals whose star formation has been shut down. An individual galaxy's fading is measured using the globular cluster specific frequency (S N ), defined as the number of globular clusters normalised by the galaxy luminosity. This is compared with a spectroscopically-derived age estimate. Methods. We make NTT/EMMI long-slit spectroscopic observations of 11 S0 galaxies at z < 0.006. We measure the absorption-line indices, Hδ, Hγ, Mgb, Fe5270 and Fe5335 within the central r e /8. By inverting single-stellar population models, luminosity-weighted mean ages, metallicities and α-element abundance ratios are derived. We estimate the amount of fading a galaxy has undergone by comparing each galaxy's S N with its deviation from the mean spiral S N . Results. Galaxies with higher S N have older stellar populations. Moreover, we find that the zero-point and amount of fading is consistent with a scenario where lenticulars are formed by the quenching of star formation in spiral galaxies. Our data also rule out any formation method for S0s which creates a large number of new globular clusters. We confirm that previous results showing a relationship between S N and color are driven by the S N −Age relation. Five galaxies show detectable Hβ,lines. However, only in the two youngest galaxies is this emission unambiguously from star formation. Conclusions. Our results are consistent with the theory that S0 galaxies are formed when gas in normal spirals is removed, possibly as a result of a change in environment. The on-going star formation in the youngest galaxies hints that the timescale of quenching is 1 Gyr. We speculate, therefore, that the truncation of star formation is a rather gentle process unlikely to involve a rapid burst of star formation.

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The Fundamental Plane in RX J0142.0+2131: A Galaxy Cluster Merger at [FORMULA][F]z=0.28[/F][/FORMULA]

Cited by 19 publications

References 28 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 Extended GMRT Radio Halo Survey

The formation of S0 galaxies: evidence from globular clusters

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