Very deep spectroscopy of the Coma cluster line of sight:
exploring new territories

Adami, C.; Brun, V. Le; Biviano, A.; Durret, F.; Lamareille, F.; Pelló, R.; Ilbert, O.; Mazure, A.; Trilling, R.; Ulmer, M. P.

doi:10.1051/0004-6361/200912228

Cited by 40 publications

(46 citation statements)

References 56 publications

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“…We do however have a filament along the Line-of-Sight, connecting to Coma approximately at the same position and along the same direction as the PFA structure. However, the PFA detected by Adami et al (2009) is defined on a much smaller scale than what analysed here and the position and direction of the filament is only hinted at by the position of knots detected on the LoS. This prevents us from drawing any further conclusion on the match between the filaments from DisPerSE and what found by Adami et al (2009).…”

Section: Indirect Confirmation Of the First Generation Filamentsmentioning

confidence: 64%

Like a spider in its web: a study of the large-scale structure around the Coma cluster

Malavasi

Aghanim

Tanimura

et al. 2020

A&A

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The Cosmic Web is a complex network of filaments, walls and voids that represent the largest structures in the Universe. In this network, which is the direct result of structure formation, galaxy clusters occupy central positions as the nodes, connected through the filaments. In this work, we investigate the position in the Cosmic Web of one of the most known and best studied clusters of galaxies, the Coma cluster. We make use of the Sloan Digital Sky Survey Data Release 7 (SDSS DR7) Main Galaxy Sample and of the Discrete Persistent Structure Extractor (DisPerSE ) to detect large scale filaments around the Coma cluster and we analyse the properties of the Cosmic Web. We study the network of filaments around Coma in a 75 Mpc radius region. We find that the Coma cluster has a median connectivity of 2.5, in agreement with measurements from clusters of similar mass in the literature, as well as with what expected from numerical simulations. It is indeed connected to 3 secure filaments which connect Coma to Abell 1367 and to several other clusters in the field. The location of these filaments in the vicinity of Coma is consistent with features detected in the X-ray, as well as the likely direction of infall of galaxies, as for example NGC4839. The overall picture that emerges of the Coma cluster is that of a highly connected structure occupying a central position as a dense node of the Cosmic Web. We also find a tentative detection, at 2.1σ significance, of the filaments in the SZ signal.

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Section: Indirect Confirmation Of the First Generation Filamentsmentioning

confidence: 64%

Like a spider in its web: a study of the large-scale structure around the Coma cluster

Malavasi

Aghanim

Tanimura

et al. 2020

A&A

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“…They noted that the mass distribution did not correspond to the X‐ray structure or to the distribution of bright galaxies. Adami et al (2009) did a very deep spectroscopic survey of these inner regions and concluded that there are a number of background groups, including a major concentration (BMG) at z = 0.054. They suggested that background structures may be responsible for some of the lensing‐derived surface mass distribution.…”

Section: X‐ray/optical Comparisons and Discussionmentioning

confidence: 99%

Diffuse radio emission in/around the Coma cluster: beyond simple accretion

Brown

Rudnick

2011

Monthly Notices of the Royal Astronomical Society

173

212

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We report on new 1.41‐GHz Green Bank Telescope (GBT) and 352‐MHz Westerbork Synthesis Radio Telescope observations of the Coma cluster and its environs. At 1.41 GHz, we tentatively detect an extension to the Coma cluster radio relic source 1253+275 which makes its total extent ∼2 Mpc. This extended relic is linearly polarized as seen in our GBT data, the NRAO VLA Sky Survey, and archival images, strengthening a shock interpretation. The extended relic borders a previously undetected ‘wall’ of galaxies in the infall region of the Coma cluster. We suggest that the radio relic is an infall shock, as opposed to the outgoing merger shocks believed responsible for other radio relics. We also find a sharp edge, or ‘front’, on the western side of the 352‐MHz radio halo. This front is coincident with a similar discontinuity in the X‐ray surface brightness and temperature in its southern half, suggesting a primary shock‐acceleration origin for the local synchrotron emitting electrons. The northern half of the synchrotron front is less well correlated with the X‐ray properties, perhaps due to projection effects. We confirm the global pixel‐to‐pixel power‐law correlation between the 352‐MHz radio brightness and X‐ray brightness with a slope that is inconsistent with predictions of either primary shock acceleration or secondary production of relativistic electrons in giant radio haloes, but is allowable in the framework of the turbulent re‐acceleration of relic plasma. The failure of these first‐order models and the need for a more comprehensive view of the intracluster medium energization are also highlighted by the very different shapes of the diffuse radio and X‐ray emission. We note the puzzling correspondence between the shape of the brighter regions of the radio halo and the surface mass density derived from weak lensing.

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“…In our merging system catalogue two smaller groups are also connected with the Coma cluster that probably belong to a filament connected with it. The substructure of the Coma cluster is rather rich and several subcomponents can be identified (Fitchett & Webster 1987;Gambera et al 1997;Adami et al 2005Adami et al , 2009. Figure 8 (see also Fig.…”

Section: Selected Known Clustersmentioning

confidence: 94%

Merging groups and clusters of galaxies from the SDSS data

Tempel

Tuvikene

Kipper

et al. 2017

A&A

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Context. Galaxy groups and clusters are the main tools used to test cosmological models and to study the environmental effect of galaxy formation. Aims. This work provides a catalogue of galaxy groups and clusters, as well as potentially merging systems based on the SDSS main galaxy survey. Methods. We identified galaxy groups and clusters using the modified friends-of-friends (FoF) group finder designed specifically for flux-limited galaxy surveys. The FoF group membership is refined by multimodality analysis to find subgroups and by using the group virial radius and escape velocity to expose unbound galaxies. We look for merging systems by comparing distances between group centres with group radii. Results. The analysis results in a catalogue of 88 662 galaxy groups with at least two members. Among them are 6873 systems with at least six members which we consider to be more reliable groups. We find 498 group mergers with up to six groups. We performed a brief comparison with some known clusters in the nearby Universe, including the Coma cluster and Abell 1750. The Coma cluster in our catalogue is a merging system with six distinguishable subcomponents. In the case of Abell 1750 we find a clear sign of filamentary infall toward this cluster. Our analysis of mass-to-light ratio (M/L) of galaxy groups reveals that M/L slightly increases with group richness.

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Very deep spectroscopy of the Coma cluster line of sight: exploring new territories

Cited by 40 publications

References 56 publications

Like a spider in its web: a study of the large-scale structure around the Coma cluster

Like a spider in its web: a study of the large-scale structure around the Coma cluster

Diffuse radio emission in/around the Coma cluster: beyond simple accretion

Merging groups and clusters of galaxies from the SDSS data

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