<i>Suzaku</i>observations of the low surface brightness cluster A76

Ota, Naomi; Fujino, Y.; Ibaraki, Y.; Böhringer, H.; Chon, G.

doi:10.1051/0004-6361/201321676

Cited by 7 publications

(16 citation statements)

References 25 publications

(18 reference statements)

Supporting

Mentioning

Contrasting

Order By: Relevance

“…1 of Bird et al (1995)) -contrasts it with relaxed and evolved clusters like Coma (Neumann et al 2003). The clumped and irregular X-ray morphology observed in A2151C is similar to that observed in the nearby cluster Abell 76 which is believed to be in the early phase of cluster formation (Ota et al 2013). Similar clumpiness is also found in A2147 (Jones et al 1979;Reichert et al 1981) which along with A2151 and A2152 forms the Hercules supercluster, and is also considered to be in its early evolutionary phase.…”

Section: Discussionsupporting

confidence: 62%

The Hercules cluster in X-rays with XMM-Newton and Chandra

Tiwari

Singh

2020

Monthly Notices of the Royal Astronomical Society

View full text Add to dashboard Cite

We present a detailed X-ray study of the central subcluster of the nearby (z ∼0.0368) Hercules cluster (Abell 2151) identified as A2151C that shows a bimodal structure. A bright clump of hot gas with X-ray emission extending to radius r ∼304 kpc and $L_X = 3.03_{-0.04}^{+0.02}\times 10^{43}$ erg s−1 in the 0.4−7.0 keV energy range is seen as a fairly regular subclump towards the west (A2151C(B)). An irregular, fainter and cooler subclump with radius r ∼364 kpc is seen towards the east (A2151C(F)) and has LX = 1.13 ± 0.02 × 1043 erg s−1 in the 0.4−7.0 keV energy band. The average temperature and elemental abundance of A2151C(B) are 2.01 ± 0.05 keV and 0.43 ± 0.05 Z⊙ respectively, while these values are 1.17 ± 0.04 keV and 0.13 ± 0.02 Z⊙ for A2151C(F). Low temperature (1.55 ± 0.07 keV) and a short cooling time (∼0.81 Gyr) within the central 15 arcsec region confirm the presence of a cool core in A2151C(B). We identify several compact groups of galaxies within A2151C(F). We find that A2151C(F) is a distinct galaxy group in the process of formation and likely not a ram-pressure stripped part of the eastern subcluster in Hercules (A2151E). X-ray emission from A2151C shows a region of overlap between A2151C(B) and A2151C(F) but without any enhancement of temperature or entropy in the two-dimensional (2D) projected thermodynamic maps that could have indicated an interaction due to merger between the two subclumps.

show abstract

Section: Discussionsupporting

confidence: 62%

The Hercules cluster in X-rays with XMM-Newton and Chandra

Tiwari

Singh

2020

Monthly Notices of the Royal Astronomical Society

View full text Add to dashboard Cite

show abstract

“…This yields a central entropy value of 190±14 keV cm −2 , which is well in the regime of non-cool core clusters (see Pratt et al (2010)). It is less extreme than that of Coma with its central entropy value of 535 keV cm −2 (Fusco-Femiano et al 2013), and that of the low surface brightness cluster A76 with a value of 400 keV cm −2 (Ota et al 2013), but it shows that the properties of the main cluster is far from the stage where it could have developed a cool core, in agreement with our conclusion above.…”

Section: Modelling the Main Cluster Componentsupporting

confidence: 89%

Witnessing a merging bullet being stripped in the galaxy cluster RXCJ2359.3-6042

Chon

Böhringer

2015

A&A

View full text Add to dashboard Cite

We report the discovery of the merging cluster, RXCJ2359.3-6042, from the REFLEX II cluster survey and present our results from all three detectors combined in the imaging and spectral analysis of the XMM-Newton data. Also known as Abell 4067, this is a unique system, where a compact bullet penetrates an extended, low density cluster at redshift z = 0.0992 clearly seen from our follow-up XMM-Newton observation. The bullet goes right through the central region of the cluster without being disrupted and we can clearly see how the bullet component is stripped of its layers outside the core. There is an indication of a shock heated region in the east of the cluster with a higher temperature. The bulk temperature of the cluster is about 3.12(±0.13) keV implying a lower mass system. Spearheading the bullet is a cool core centred by a massive early type galaxy. The temperatures and metallicities of a few regions in the cluster derived from the spectral analysis supports our conjecture based on the surface brightness image that a much colder compact component at 1.55(±0.10) keV with large metallicity (0.75 Z ) penetrates the main cluster, where the core of the infalling component survived the merger and left stripped gas behind at the centre of the main cluster. We also give an estimate of the total mass within r 500 , which is about 2 × 10 14 M from the deprojected spherical β modelling of the cluster in good agreement with other mass estimates from the M−T X and M−σ v relations.

show abstract

“…As already noted in, e.g. Ota et al (2014), the ICM cannot be radiatively cooled down to the "ordinary" entropy within 10 10 years, and thus this cluster remains LSB for a long period.…”

Section: Icm Properties In View Of Gas Mass Fractionmentioning

confidence: 57%

“…They all lack bright central core, apparently elongated and/or have sub-structures, showing that they are dynamically young (Böringer et al 2007). Another template of this type of cluster is Abell 76, which has a very low surface brightness and a complicated structure (Ota et al 2014). By the Suzaku observations, its ICM with a temperature of ∼ 3 keV is shown to have very high entropy of ∼ 400 keV cm 2 in its center.…”

Section: Introductionmentioning

confidence: 99%

Suzaku observation of a high-entropy cluster Abell 548W

Nakazawa

Kato

et al. 2016

Publications of the Astronomical Society of Japan

View full text Add to dashboard Cite

Abell 548W, one of the galaxy clusters located in the Abell 548 region, has about an order of magnitude lower X-ray luminosity compared to ordinal clusters in view of the well known intracluster medium (ICM) temperature vs X-ray luminosity (kT -L X ) relation. The cluster hosts a pair of diffuse radio sources to the north west and north, both about 10 ′ apart from the cluster center. They are candidate radio relics, frequently associated with merging clusters. A Suzaku deep observation with exposure of 84.4 ks was performed to search signatures for merging in this cluster. The XIS detectors successfully detected the ICM emission out to 16 ′ from the cluster center. The temperature is ∼ 3.6 keV around its center, and ∼ 2 keV at the outermost regions. The hot region (∼ 6 keV) aside the relic candidates shifted to the cluster center reported by XMM-Newton was not seen in the Suzaku data, although its temperature of 3.6 keV itself is higher than the average temperature of 2.5 keV around the radio sources. In addition, a signature of a cool (kT ∼ 0.9 keV) component was found around the north west source. A marginal temperature jump at its outer-edge was also found, consistent with the canonical idea of shock acceleration origin of the radio relics. The cluster has among the highest central entropy of ∼ 400 keV cm 2 and is one of the so-called low surface brightness clusters. Taking into account the fact that its shape itself is relatively circular and smooth and also its temperature structure is nearly flat, possible scenarios for merging is discussed.

show abstract

Suzakuobservations of the low surface brightness cluster A76

Cited by 7 publications

References 25 publications

The Hercules cluster in X-rays with XMM-Newton and Chandra

The Hercules cluster in X-rays with XMM-Newton and Chandra

Witnessing a merging bullet being stripped in the galaxy cluster RXCJ2359.3-6042

Suzaku observation of a high-entropy cluster Abell 548W

Contact Info

Product

Resources

About