The structure of the Virgo cluster of galaxies from Rosat X-ray images

Böhringer, H.; Briel, U. G.; Schwarz, R.; Voges, W.; Hartner, Gisela; Trümper, J.

doi:10.1038/368828a0

Cited by 295 publications

(352 citation statements)

References 24 publications

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“…Our Virgo-like cluster is slightly more massive than the Virgo cluster mass adopted in Mamon et al (2004), but lies in the middle of the range 1.5 -6.0×10 14 M given in Böhringer et al (1994). The virial radius of the simulated cluster is slightly larger than that of the Virgo cluster.…”

Section: Simulated Cluster Properties: Comparison To Virgomentioning

confidence: 85%

Warm gas in and around simulated galaxy clusters as probed by absorption lines

Emerick

Bryan

Putman

2015

Mon. Not. R. Astron. Soc.

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Understanding gas flows into and out of the most massive dark matter structures in our Universe, galaxy clusters, is fundamental to understanding their evolution. Gas in clusters is well studied in the hot (> 10 6 K) and cold (< 10 4 K) regimes, but the warm gas component (10 4 -10 6 K) is poorly constrained. It is challenging to observe directly, but can be probed through Lyα absorption studies. We produce the first systematic study of the warm gas content of galaxy clusters through synthetic Lyα absorption studies using cosmological simulations of two galaxy clusters produced with Enzo. We explore the spatial and kinematic properties of our cluster absorbers, and show that the majority of the identified absorbers are due to fast moving gas associated with cluster infall from IGM filaments. Towards the center of the clusters, however, the warm IGM filaments are no longer dominant and the absorbers tend to have higher column densities and metallicities, representing stripped galaxy material. We predict that the absorber velocity distribution should generally be bi-modal and discuss the effects of cluster size, mass, and morphology on the properties of the identified absorbers, and the overall cluster warm gas content. We find tentative evidence for a change in the well known increasing N HI with decreasing impact parameter for the most massive dark matter halos. Our results are compared directly to observations of Lyα absorbers in the Virgo cluster, and provide predictions for future Lyα absorption studies.

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Section: Simulated Cluster Properties: Comparison To Virgomentioning

confidence: 85%

Warm gas in and around simulated galaxy clusters as probed by absorption lines

Emerick

Bryan

Putman

2015

Mon. Not. R. Astron. Soc.

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“…If we further assume the hydrostatic equilibrium, the dynamical mass in the same region was ∼ 3 × 10 12 M⊙, giving the ratio of the gas mass to the dynamical mass Mgas/M dyn ∼ 0.01. If we adopt the dynamical mass within 230 kpc provided by Böhringer et al (1994), the ratio becomes ∼ 10 −3 . These ratios suggest the halo of M86 is significantly affected by the interaction with the Virgo ICM.…”

Section: Discussionmentioning

confidence: 99%

“…Then the ratio of the gas mass to the dynamical mass Mgas/M dyn became ∼ 0.01. Böhringer et al (1994) decomposed the X-ray surface brightness distribution obtained with ROSAT into several components, and estimated the total mass within 280 kpc is (1-3)×10 13 M⊙. If we use their number, Mgas/M dyn becomes only ∼ 10 −3 .…”

Section: Estimation Of the Gas Mass And The Dynamical Massmentioning

confidence: 99%

“…Since the sound speed is 730 km s −1 for the cluster ICM of kT = 2 keV, M86 is moving with a Mach number of > ∼ 2. M86 is thought to be the dominant member of one of the subgroups within the Virgo cluster (e.g., Böhringer et al 1994;Schindler et al 1999). Therefore, M86 provides a good opportunity to study the interaction between the interstellar medium (ISM) and the ICM as well as the interaction between the subcluster and the ICM.…”

Section: Introductionmentioning

confidence: 99%

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X-ray study of extended emission around M 86 observed with Suzaku

Hishi

Fujimoto

Kotake

et al. 2017

Publications of the Astronomical Society of Japan

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We analyzed the Suzaku data of M86 and its adjacent regions to study the extended emission around it. The M86 core, the plume, and the tail extending toward the northwest were clearly detected, as well as the extended halo around them. From the position angle ∼ 45 • to ∼ 275 • , the surface brightness distribution of the core and the extended halo was represented relatively well with a single β-model of β ∼ 0.5 up to 15 ′ -20 ′ . The X-ray spectra of the core was represented with a two-temperature model of kT ∼ 0.9 keV and ∼ 0.6 keV. The temperatures of the core and the halo have a positive gradient in the center, and reach the maximum of kT ∼ 1.0 keV at r ∼ 7 ′ , indicating that the halo gas is located in a larger scale potential structure than that of the galaxy. The temperatures of the plume and the tail were 0.86 ± 0.01 keV and 1.00 ± 0.01 keV. We succeeded in determining the abundances of α-element separately, for the core, the plume, the tail, and the halo for the first time. Abundance ratios with respect to Fe were consistent with the solar ratios everywhere, except for Ne. The abundance of Fe was ∼ 0.7 in the core and in the plume, while that in the tail was ∼ 1.0, but the difference was not significant considering the uncertainties of the ICM. The abundance of the halo was almost the same up to r ∼ 10 ′ , and then it becomes significantly smaller (0.2-0.3) at r > ∼ 10 ′ , indicating the gas with low metal abundance still remains in the outer halo. From the surface brightness distribution, we estimated the gas mass (∼ 3 × 10 10 M ⊙ ) and the dynamical mass (∼ 3 × 10 12 M ⊙ ) in r < 100 kpc. The gas mass to the dynamical mass ratio was 10 −3 -10 −2 , suggesting a significant fraction of the halo gas has been stripped.

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“…Kenney et al (2004Kenney et al ( , 2008, Oosterloo & van Gorkom 2005, and Chung et al (2007 find that many spiral galaxies near the center of the Virgo cluster show long Hα or H I tails interpreted to be cold gas that is being stripped by the ambient X-ray-emitting gas (Böhringer et al 1994). Kormendy and Bender emphasize that these galaxies and the H I -depleted galaxies are substantially brighter than almost all Sphs: "If even the deep gravitational potential wells of still-spiral galaxies suffer H I stripping, then the shallow potential wells of dS + Im galaxies are more likely to be stripped."…”

Section: Environmental Processes Imentioning

confidence: 99%

Structure and Evolution of Dwarf Galaxies

Kormendy

2014

Lessons From the Local Group

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Abstract. Different structural parameter correlations show how classical bulge components and elliptical galaxies are different from spiral and S0 galaxy disks, irregular (Im) galaxies, and spheroidal (Sph) galaxies. In contrast, the latter, apparently diverse galaxies or galaxy components have almost identical parameter correlations. This shows that they are related. A review of galaxy transformation processes suggests that S0 and spheroidal galaxies are star-formation-quenched, "red and dead" versions of spiral and Im galaxies. In particular, Sph galaxies are bulgeless S0s. This motivates a parallel sequence galaxy classification in which an S0a-S0b-S0c-Sph sequence of decreasing bulge-to-total ratios is juxtaposed to an Sa-Sb-Sc-Im sequence of star-forming galaxies. All parameter sequences show a complete continuity from giant galaxies to the tiniest dwarfs. Dwarfs are not a new or different class of galaxies. Rather, they are the extreme products of transformation processes that get more important as gravitational potential wells get more shallow. Smaller Sph and S+Im galaxies have lower stellar densities because they retain fewer baryons. Comparison of the baryonic parameter correlations with those for dark matter halos allows us to estimate baryon loss as a function of galaxy mass. Extreme dwarfs are almost completely dominated by dark matter.

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The structure of the Virgo cluster of galaxies from Rosat X-ray images

Cited by 295 publications

References 24 publications

Warm gas in and around simulated galaxy clusters as probed by absorption lines

Warm gas in and around simulated galaxy clusters as probed by absorption lines

X-ray study of extended emission around M 86 observed with Suzaku

Structure and Evolution of Dwarf Galaxies

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