The X-ray emission of the Seyfert 2 galaxy MCG-01-24-12
  We present a detailed X-ray spectral analysis of the nearby Seyfert 2 galaxy
MCG-01-24-12 based on a multi-epoch data set. Data have been taken with
different X-ray satellites, namely XMM-Newton, NuSTAR, Swift and Chandra and
cover different time intervals, from years down to a few days. From 2006 to
2013 the source had a 2-10 keV flux of $\sim$1.5$\times$10$^{-11}$ erg
cm$^{-2}$ s$^{-1}$, consistent with archival observations based on
\textit{HEAO} and \textit{BeppoSAX} data, though a 2019 \textit{Chandra}
snapshot caught the source in an extreme low flux state, a factor of $\sim$10
fainter than its historical one. Based on phenomenological and physically
motivated models, we find the X-ray spectrum of MCG-01-24-12 to be best
modelled by a power-law continuum emission with $\Gamma$=1.76$\pm$0.09 with a
high energy cut-off at E$_{\rm c}=70^{+21}_{-14}$ keV that is absorbed by a
fairly constant column density of N$_{\rm H}$=(6.3$\pm$0.5)$\times10^{22}$
cm$^{-2}$. These quantities allowed us to estimate the properties of the hot
corona in MCG-01-24-12 for the cases of a spherical or slab-like hot
Comptonising plasma to be kT$_{\rm e}$=27$^{+8}_{-4}$ keV, $\tau_{\rm
e}$=5.5$\pm$1.3 and kT$_{\rm e}$=28$^{+7}_{-5}$ keV, $\tau$=3.2$\pm$0.8,
respectively. Finally, despite the short duration of the exposures, possible
evidence of the presence of outflows is discussed.
