The X-ray Coronae of two massive galaxies in the core of the Perseus
  cluster
  We study the X-ray properties of two elliptical galaxies, NGC 1270 and NGC
1272, in the core of the Perseus cluster with deep Chandra observations. Both
galaxies have central supermassive black holes, the mass of which is $6.0
\times 10^{9}$ M$_{\odot}$ and $2.0 \times 10^{9}$ M$_{\odot}$ respectively.
Our aim is to examine relatively cool soft X-ray emitting gas within the
central region of these massive early-type galaxies. Such gas, referred to as a
Minicorona in previous studies is common in the core of large elliptical
cluster galaxies. It has not been completely stripped or evaporated by the
surrounding hot intracluster medium and nor fully accreted onto the central
black hole. With thermal emission from the minicorona dominating over any
power-law radiation components, we find that both NGC 1270 and NGC 1272
encompass minicoronae, the temperature and radius of which are $0.99$ keV and
$0.63$ keV; $1.4$ kpc and $1.2$ kpc respectively. For NGC 1272, the thermal
coronal component dominates the core emission by a factor of over 10. We show
that the depletion time scale of minicoronal gas via viscous stripping is
shorter by a factor of $100$ than the replenishment time scale due to stellar
mass loss. Magnetic fields are presumably responsible for suppression of the
transport processes. Finally, we show that both objects have to meet a balance
between cooling and heating as well as that among mass replenishment, stripping
and accretion.
