Spectral energy distributions for galaxies in high-redshift clusters – II. 0016 + 16 at z = 0.54

Ellis, Richard S.; Couch, Warrick J.; MacLaren, Iain; Koo, David C.

doi:10.1093/mnras/217.2.239

Cited by 28 publications

(22 citation statements)

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“…This source structure is most likely to be extended too. Galaxy number 43, defined by BR, having a redshift of z=0.38, indicated in the figure, coincides with the maximum of this source, so that it might be, that there is emission from a small foreground group, as already suggested by Ellis et al (1985). However, optical source number 36 also in this enhancement is a star and might contribute partly to the emission.…”

Section: The X-ray Datamentioning

confidence: 51%

X-ray properties of the distant cluster Cl0016 + 16

Neumann¹,

Böhringer²

1997

Monthly Notices of the Royal Astronomical Society

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We present X-ray data on the distant cluster Cl0016+16 (z=0.5545) from ROSAT PSPC and HRI observations and use them to study the physics of the intracluster medium (ICM) and the dynamical state of the cluster. The surface brightness distribution is not only described by a spherically symmetric model but also by a twodimensional β-model fit. Subtracting an elliptical model cluster as defined by the best fit parameters of the two-dimensional model we find significant residuals, indicating an additional, extended X-ray source within the cluster. This source, likely to be a merging subcomponent of the cluster, coincides with a peak in the weak lensing mass map of Smail et. al. (1995). In the course of this analysis we present a new approach to quantify the significance of substructure in cluster X-ray images dominated by Poisson noise and smoothed with a Gauss filter. We determine the radial mass profile integrated out to a radius of 3Mpc and find for the total mass of the cluster a value of ∼ 1.4 − 3.3 × 10 15 M ⊙ and ∼ 4.5 × 10 14 M ⊙ for the gas mass, yielding a gas-to-total mass ratio of 14 -32%. There is no significant radial dependence of the gas-to-total mass ratio in the cluster.

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Section: The X-ray Datamentioning

confidence: 51%

X-ray properties of the distant cluster Cl0016 + 16

Neumann¹,

Böhringer²

1997

Monthly Notices of the Royal Astronomical Society

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“…Optically, the cluster is very easy to recognize with three bright galaxies in a line running north-east to south-west, the BCG being the central galaxy of the three, surrounded by a large number of fainter galaxies. MS0015.9 + 1609 has the highest number of color selected cluster galaxies in the sample, but these counts may be enriched by a foreground structure at z ∼ 0.3 (Ellis et al 1985). As can be seen in Figure 8, while the three large galaxies cause the smoothed central light peak to be elliptical with the major axis running north-east south-west, the fainter galaxies in the core are distributed circularly about the BCG, with a slight over-density to the west of the BCG.…”

Section: Cluster Propertiesmentioning

confidence: 99%

Weak Lensing by High‐Redshift Clusters of Galaxies. I. Cluster Mass Reconstruction

Clowe¹,

Luppino²,

Kaiser³

et al. 2000

ApJ

109

142

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We present the results of a weak lensing survey of six high-redshift (z > 0.5), X-ray selected clusters of galaxies. We have obtained ultra-deep R-band images of each cluster with the Keck Telescope, and have measured a weak lensing signal from each cluster. From the background galaxy ellipticities we create two-dimensional maps of the surface mass density of each cluster. We find that the substructure seen in the mass reconstructions typically agree well with substructure in both the cluster galaxy distributions and X-ray images of the clusters. We also measure the one-dimensional radial profiles of the lensing signals and fit these with both isothermal spheres and "universal" CDM profiles. We find that the more massive clusters are less compact and not as well fit by isothermal spheres as the less massive clusters, possibly indicating that they are still in the process of collapse.

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“…The crucial next step toward understanding the B-O effect involved obtaining confirmation that the blue galaxies are indeed cluster members, through both narrow band photometry (e.g., Couch et al 1983;Ellis et al 1985;MacClaren et al 1988;Rakos & Schombert 1994;Belloni et al 1995) and spectroscopy (Dressler & Gunn 1982, 1992Lavery & Henry 1986;Henry & Lavery 1987;Couch & Sharples 1987;Soucail et al 1988;Pickles & van der Kruit 1991). These studies have indeed confirmed membership for a majority of the blue galaxies.…”

Section: Introductionmentioning

confidence: 99%

The Butcher-Oemler Effect at Low Redshift: Spectroscopy of Five Nearby Clusters of Galaxies

Caldwell¹,

Rose²

1997

The Astronomical Journal

130

163

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We present multi-fiber spectroscopy and broadband imaging of early-type galaxies in five nearby rich clusters of galaxies. The main purpose was to look for "abnormal" spectrum galaxies (i.e., post-starburst galaxies which have strong Balmer absorption lines and emission line galaxies) in nearby clusters that are similar to those found by Caldwell et al. (1993) in the Coma cluster. Three of the clusters were purposefully selected to have pronounced double structure in their spatial distribution of the galaxies.Our primary conclusion is that ∼15% of the early-type galaxies in these nearby rich clusters have signs of ongoing or recent star formation. Furthermore, the starburst and post-starburst nature of these abnormal spectra is reminiscent of that seen in distant clusters, although at a reduced frequency and burst strength. Thus activity similar to that seen in distant clusters is still ongoing, at a reduced level, in present-epoch rich clusters. The frequency of such galaxies appears to be enhanced significantly over that seen in field galaxies. Most of the new post-starburst galaxies are disk galaxies; three E galaxies in one cluster and one in another cluster have current star formation.We also find evidence in the spatial and kinematic structure of several of the clusters that subclusters have recently passed through the main clusters and are now emerging out the other side. This inference is based on a comparison of the spatial and kinematic cluster data with N-body simulations of infalling clusters. Specifically, we see evidence of velocity gradients and/or a dispersed appearance of the observed subclusters, both of which are produced by tidal distension and disruption of infalling subclusters. If, as we suspect, the subclusters passed through the main clusters more than a Gyr ago, then the post-starburst timescales of ∼1 Gyr imply that the star formation bursts are only triggered during (or after) the subcluster passage through the center of the main cluster. We speculate that shocks induced in the collisions of the cluster and subcluster ICM's may trigger the galaxy starbursts. using the Argus 24-arm positioner and spectrograph, which is a facility instrument on the CTIO 4m telescope. Input coordinates for the galaxies in these clusters were measured using either the Grant measuring engine at CTIO, or the one at KPNO, using the Dressler (1980) coordinates or those of Malumuth et al. (1992) as first estimates. The coordinates reported in the table below are accurate to about 1.5˝. Observations were limited to the early-type galaxies as classified by , except as noted in section 3 below. Because of the density of targets in these clusters, several setups were required per field observed. Statistics on the numbers of galaxies observed relative to the number of candidates appear below.The fibers fed a bench mounted spectrograph, whose detector was a Reticon 1200X400 CCD. A blue-blazed grating was used that gave a resolution of 2 pixels or 3.6Å, and a wavelength coverage from 3500 to 5700Å. Exposure times for ...

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Spectral energy distributions for galaxies in high-redshift clusters – II. 0016 + 16 at z = 0.54

Cited by 28 publications

References 0 publications

X-ray properties of the distant cluster Cl0016 + 16

X-ray properties of the distant cluster Cl0016 + 16

Weak Lensing by High‐Redshift Clusters of Galaxies. I. Cluster Mass Reconstruction

The Butcher-Oemler Effect at Low Redshift: Spectroscopy of Five Nearby Clusters of Galaxies

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