The merger history of the complex cluster Abell 1758: a combined weak lensing and spectroscopic view

Monteiro-Oliveira, R.; Cypriano, E. S.; Machado, Rubens E. G.; Neto, G. B. Lima; Ribeiro, André; Sodré, L.; Dupke, Renato A.

doi:10.1093/mnras/stw3238

Cited by 36 publications

(48 citation statements)

References 68 publications

(111 reference statements)

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“…Our entropy map of Fig. 8 (right panel) highlights the presence of the two cores in A1758N and the single core in A1758S, characterized by the lowest values of entropy in the map, in line with the bimodal (A1758N) and single clump (A1758S) mass distribution already inferred from optical studies (Dahle et al 2002;Okabe & Umetsu 2008;Ragozzine et al 2012;Monteiro-Oliveira et al 2017).…”

Section: X-ray Properties Of A1758n and A1758ssupporting

confidence: 82%

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LOFAR discovery of a double radio halo system in Abell 1758 and radio/X-ray study of the cluster pair

Botteon

Shimwell

Bonafede

et al. 2018

Monthly Notices of the Royal Astronomical Society

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Radio halos and radio relics are diffuse synchrotron sources that extend over Mpcscales and are found in a number of merger galaxy clusters. They are believed to form as a consequence of the energy that is dissipated by turbulence and shocks in the intra-cluster medium (ICM). However, the precise physical processes that generate these steep synchrotron spectrum sources are still poorly constrained. We present a new LOFAR observation of the double galaxy cluster Abell 1758. This system is composed of A1758N, a massive cluster hosting a known giant radio halo, and A1758S, which is a less massive cluster whose diffuse radio emission is confirmed here for the first time. Our observations have revealed a radio halo and a candidate radio relic in A1758S, and a suggestion of emission along the bridge connecting the two systems which deserves confirmation. We combined the LOFAR data with archival VLA and GMRT observations to constrain the spectral properties of the diffuse emission. We also analyzed a deep archival Chandra observation and used this to provide evidence that A1758N and A1758S are in a pre-merger phase. The ICM temperature across the bridge that connects the two systems shows a jump which might indicate the presence of a transversal shock generated in the initial stage of the merger.

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Section: X-ray Properties Of A1758n and A1758ssupporting

confidence: 82%

“…A compilation of the different mass estimates reported for A1758N is given in Tab. 1 of Monteiro-Oliveira et al (2017). Note that the mass of A1758S is more uncertain whilst it appears to be at least a factor of 1.5 smaller than that of A1758N (David & Kempner 2004;Ragozzine et al 2012;Haines et al 2017).…”

Section: The Double Cluster Abell 1758mentioning

confidence: 91%

LOFAR discovery of a double radio halo system in Abell 1758 and radio/X-ray study of the cluster pair

Botteon

Shimwell

Bonafede

et al. 2018

Monthly Notices of the Royal Astronomical Society

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“…The velocity dispersion, however, is known to be boosted in epochs close to pericentric passages (e.g. Pinkney et al 1996;Monteiro-Oliveira et al 2017), which can lead to mass overestimation.…”

mentioning

confidence: 99%

Weak lensing and spectroscopic analysis of the nearby dissociative merging galaxy cluster Abell 3376

Monteiro-Oliveira

Neto

Cypriano

et al. 2017

Monthly Notices of the Royal Astronomical Society

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The galaxy cluster Abell 3376 is a nearby (z = 0.046) dissociative merging cluster surrounded by two prominent radio relics and showing an X-ray comet-like morphology. The merger system is comprised of the subclusters A3376W & A3376E. Based on new deep multiwavelength large-field images and published redshifts, we bring new insights about the history of this merger. Despite the difficulty of applying the weak lensing technique at such low redshift, we successfully recovered the mass distribution in the cluster field. Moreover, with the application of a two-body model, we have addressed the dynamics of these merging system. We have found the individual masses of M M ⊙ . The cometary shaped X-ray distribution shows only one peak spatially coincident with both Eastern BCG and the A3376E mass peak whereas the gas content of A3376W seems to be stripped out. Our data allowed us to confirm the existence of a third subcluster located at the North, 1147 ± 62 kpc apart from the neighbour subcluster A3376E and having a mass M N 200 = 1.4+0.7 −1.0 × 10 14 M ⊙ . From our dynamical analysis, we found the merging is taking place very close to the plane of the sky, with the merger axis just 10• ± 11• from it. The application of a two-body analysis code showed that the merging cluster is seen 0.9 +0.2 −0.3 Gyr after the pericentric passage and it is currently going to the point of maximum separation between the subclusters.

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“…From the Illustris simulation (Vogelsberger et al 2014;Genel et al 2014), Schaal & Springel (2015) find that nearly 75 per cent of shocks have Mach numbers M < 6, regardless of redshift. Depending on the time scale, strong simulated shock fronts may not be detectable in X-ray data, presumably because they have already travelled to the low-density outskirts of the clusters Monteiro-Oliveira et al 2017). So shock fronts are more likely to be detectable shortly before or shortly after central passage.…”

Section: Introductionmentioning

confidence: 99%

Two merging galaxy clusters with very hot shock fronts observed shortly before pericentric passage

Laganá

Machado

et al. 2019

Monthly Notices of the Royal Astronomical Society

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We present a detailed analysis of two merging clusters, from XMM-Newton X-ray archival data: PLCKESZ G036.7+14.9 (z = 0.15; hereafter G036) and PLCK G292.5+22.0 (z = 0.30; hereafter G292). We notice that the intracluster medium is heated as a result of the merger, and we find evidence for a merger shock in the region between both subcluster haloes. Xray observations confirm that the shocks in these systems are among the hottest known in the literature. From the ICM analysis of temperature discontinuity, the Mach numbers were determined to be M G036 = 1.3 and M G292 = 1.5 for G036 and G292, respectively. In this paper, for each cluster, we propose a hydrodynamic model for the merger as a whole, compatible with their diffuse X-ray emission and temperature maps. The simulations suggest that both clusters are observed shortly before pericentric passage. Our simulation results indicate that the merger of the G036 system is seen at an inclination of 50 • (the angle between the plane of the orbit and the plane of the sky), and merely 50 Myr prior to the pericentric passage. In the case of G292, the subclusters would be merging not far from the plane of the sky (i = 18 • ) and are observed 150 Myr before the two cores collide.

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The merger history of the complex cluster Abell 1758: a combined weak lensing and spectroscopic view

Cited by 36 publications

References 68 publications

LOFAR discovery of a double radio halo system in Abell 1758 and radio/X-ray study of the cluster pair

LOFAR discovery of a double radio halo system in Abell 1758 and radio/X-ray study of the cluster pair

Weak lensing and spectroscopic analysis of the nearby dissociative merging galaxy cluster Abell 3376

Two merging galaxy clusters with very hot shock fronts observed shortly before pericentric passage

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