X-ray study of extended emission around M86 observed with Suzaku

Abstract

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 $\sim 45°$ to $\sim 275°$, the surface brightness distribution of the core and the extended halo was represented relatively well with a single $\beta$-model of $\beta \sim 0.5$ up to 15'-20'. The X-ray spectra of the core was represented with a two-temperature model of $kT\sim 0.9$ keV and $\sim 0.6$ keV. The temperatures of the core and the halo have a positive gradient in the center, and reach the maximum of $kT\sim 1.0$ keV at $r\sim 7^{\prime }$, 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 $0.86\pm 0.01$ keV and $1.00\pm 0.01$ keV. We succeeded in determining the abundances of $\alpha$-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 $\sim 0.7$ in the core and in the plume, while that in the tail was $\sim 1.0$, but the difference was not significant considering the uncertainties of the ICM. The abundance of the halo was almost the same up to $r\sim 10^{\prime }$, and then it becomes significantly smaller (0.2-0.3) at $r\gtrsim 10^{\prime }$, indicating the gas with low metal abundance still remains in the outer halo. From the surface brightness distribution, we estimated the gas mass ($\sim 3\times 10^{10}{M}_{\odot }$) and the dynamical mass ($\sim 3\times 10^{12}{M}_{\odot }$) 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.

arXiv comment17 pages, 14 figures, 7 tables

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Cited by in corpus (2)

• Implications of the mild gas motion found with Hitomi in the core of the Perseus cluster
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