X-ray Observation of a Magnetized Hot Gas Outflow in the Galactic Center Region. (arXiv:1903.02571v1 [astro-ph.GA])

X-ray Observation of a Magnetized Hot Gas Outflow in the Galactic Center Region. (arXiv:1903.02571v1 [astro-ph.GA])
<a href="http://arxiv.org/find/astro-ph/1/au:+Nakashima_S/0/1/0/all/0/1">Shinya Nakashima</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Koyama_K/0/1/0/all/0/1">Katsuji Koyama</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Wang_Q/0/1/0/all/0/1">Q. Daniel Wang</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Enokiya_R/0/1/0/all/0/1">Rei Enokiya</a>

We report the discovery of a $1^circ$ scale X-ray plume in the northern
Galactic Center (GC) region observed with Suzaku. The plume is located at ($l$,
$b$) $sim$ ($0mbox{$.!!^circ$}2$, $0mbox{$.!!^circ$}6$), east of the
radio lobe reported by previous studies. No significant X-ray excesses are
found inside or to the west of the radio lobe. The spectrum of the plume
exhibits strong emission lines from highly ionized Mg, Si, and S that is
reproduced by a thin thermal plasma model with $kT sim 0.7$ keV and solar
metallicity. There is no signature of non-equilibrium ionization. The
unabsorbed surface brightness is $3times10^{-14}$ erg cm$^{-2}$ s$^{-1}$
arcmin$^{-2}$ in the 1.5-3.0 keV band. Strong interstellar absorption in the
soft X-ray band indicates that the plume is not a foreground source but is at
the GC distance, giving a physical size of $sim$100 pc, a density of 0.1
cm$^{-3}$, thermal pressure of $1times10^{-10}$ erg cm$^{-3}$, mass of 600
$M_odot$ and thermal energy of $7times10^{50}$ erg. From the apparent
association with a polarized radio emission, we propose that the X-ray plume is
a magnetized hot gas outflow from the GC.

We report the discovery of a $1^circ$ scale X-ray plume in the northern
Galactic Center (GC) region observed with Suzaku. The plume is located at ($l$,
$b$) $sim$ ($0mbox{$.!!^circ$}2$, $0mbox{$.!!^circ$}6$), east of the
radio lobe reported by previous studies. No significant X-ray excesses are
found inside or to the west of the radio lobe. The spectrum of the plume
exhibits strong emission lines from highly ionized Mg, Si, and S that is
reproduced by a thin thermal plasma model with $kT sim 0.7$ keV and solar
metallicity. There is no signature of non-equilibrium ionization. The
unabsorbed surface brightness is $3times10^{-14}$ erg cm$^{-2}$ s$^{-1}$
arcmin$^{-2}$ in the 1.5-3.0 keV band. Strong interstellar absorption in the
soft X-ray band indicates that the plume is not a foreground source but is at
the GC distance, giving a physical size of $sim$100 pc, a density of 0.1
cm$^{-3}$, thermal pressure of $1times10^{-10}$ erg cm$^{-3}$, mass of 600
$M_odot$ and thermal energy of $7times10^{50}$ erg. From the apparent
association with a polarized radio emission, we propose that the X-ray plume is
a magnetized hot gas outflow from the GC.

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