The cluster of galaxies Abell 970

Sodré, L.; Proust, D.; Capelato, H. V.; Neto, G. B. Lima; Cuevas, H.; Quintana, H.; Fouqué, P.

doi:10.1051/0004-6361:20011134

Cited by 10 publications

(11 citation statements)

References 41 publications

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“…The X-ray contours seem to be highly compressed along the south-east and elongated along the north-west. A similar compression of contours towards the south-east was also observed in the Einstein Imaging Proportional Counter (IPC) image of the cluster (see Sodré et al 2001). The X-ray peak seems to be significantly shifted (by about 2 ′ ∼140 kpc) towards the south-east from the centre of the outer X-ray contours.…”

Section: A376supporting

confidence: 69%

Dynamics of 10 Clusters of Galaxies With Substructures

Lakhchaura

Singh

2014

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We present a detailed Chandra study of a sample of ten clusters of galaxies selected based on the presence of substructures in their optical images. The X-ray surface brightness maps of most of these clusters show anisotropic morphologies, especially in the central regions. A total of 22 well resolved significantly bright X-ray peaks (corresponding with high-density regions) are seen in the central parts (within r c /2) of the clusters. Multiple peaks are seen in central parts of six clusters. Eleven peaks are found to have optical counterparts (10 coinciding with the BCGs of the 10 clusters and one coinciding with the second brightest galaxy in A539). For most of the clusters, the optical substructures detected in the previous studies are found to be outside the field of view of Chandra. In the spectroscopically produced 2-D temperature maps, significantly lower temperatures are seen at the location of three peaks (two in A539 and one in A376).The centers of five clusters in our sample also host regions of higher temperature compared to the ambient medium, indicating the presence of galaxy scale mergers. The X-ray luminosity, gas mass and central cooling time estimates for all the clusters are presented. The radial X-ray surface-brightness profiles of all but one of the clusters are found to be best-fitted with a double-β model, pointing towards the presence of double-phased central gas due to cool-cores. The cooling time estimates of all the clusters, however, indicate that none of them hosts a strong cool-core, although the possibility of weak cool-cores cannot be ruled out.

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Section: A376supporting

confidence: 69%

Dynamics of 10 Clusters of Galaxies With Substructures

Lakhchaura

Singh

2014

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“…number of the object. For A376, this number refers to Dressler (1980) and for A970 it continues the list of Sodré et al (2001); 2. right ascension (J2000); 3. declination (J2000); 4. morphological type either from Dressler's (1980) catalog for A376 and from a visual inspection on the Palomar Sky Survey (POSS) for A970; 5. heliocentric radial velocity with its error in km s −1 ; 6. R-value derived from Tonry & Davis (1979); 7. notes.…”

Section: Observations and Data Reductionsmentioning

confidence: 99%

New measurements of radial velocities in clusters of galaxies-V

Proust¹,

Capelato²,

Neto³

et al. 2010

A&A

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As a part of our galaxy-cluster redshift survey, we present a set of 79 new velocities in the 4 clusters Abell 376, Abell 970, Abell 1356, and Abell 2244, obtained at Haute-Provence observatory. This set now completes our previous analyses, especially for the first two clusters. Data on individual galaxies are presented, and we discuss some cluster properties. For A376, we obtained an improved mean redshift z = 0.04750 with a velocity dispersion of σ V = 860 km s −1 . For A970, we have z = 0.05875 with σ V = 881 km s −1 . We show that the A1356 cluster is not a member of the "Leo-Virgo" supercluster at a mean redshift z = 0.112 and should be considered just as a foreground group of galaxies at z = 0.0689, as well as A1435 at z = 0.062. We obtain z = 0.09962 for A2244 with σ V = 965 km s −1 . The relative proximity of clusters A2244 and A2245 (z = 0.08738, σ V = 992 km s −1 ) suggests that these could be members of a supercluster that would include A2249; however, from X-ray data there is no indication of interaction between A2244 and A2245.

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“…But it will also make a nasty mess of both the chemical and the temperature gradients that are actually seen in some "cooling flow" clusters. This disruption might persist for the age of the universe (Ritchie & Thomas 2002), in which case mergers are probably not even part of the answer, or perhaps only briefly Sodre et al 2001), in which case one might reduce the total amount of cool stuff dumped at the center over a Hubble time, though not, one would suppose, the current throughout in O vi gas, H-alpha emitting gas, and so forth.…”

Section: Cooling Flows Reheated?mentioning

confidence: 99%

Astrophysics in 2002

Trimble

Aschwanden

2003

PUBL ASTRON SOC PAC

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ABSTRACT. This has been the Year of the Baryon. Some low temperature ones were seen at high redshift, some high temperature ones were seen at low redshift, and some cooling ones were (probably) reheated. Astronomers saw the back of the Sun (which is also made of baryons), a possible solution to the problem of ejection of material by Type II supernovae (in which neutrinos push out baryons), the production of R Coronae Borealis stars (previously-owned baryons), and perhaps found the missing satellite galaxies (whose failing is that they have no baryons). A few questions were left unanswered for next year, and an attempt is made to discuss these as well.

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The cluster of galaxies Abell 970

Cited by 10 publications

References 41 publications

Dynamics of 10 Clusters of Galaxies With Substructures

Dynamics of 10 Clusters of Galaxies With Substructures

New measurements of radial velocities in clusters of galaxies-V

Astrophysics in 2002

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