Middei, R.R.MiddeiMatzeu, G. A.G. A.MatzeuBIANCHI, SIMONESIMONEBIANCHIBRAITO, ValentinaValentinaBRAITOReeves, J.J.ReevesDE ROSA, AlessandraAlessandraDE ROSADADINA, MAUROMAURODADINAMarinucci, A.A.MarinucciPERRI, MatteoMatteoPERRIZaino, A.A.Zaino2022-06-102022-06-1020210004-6361http://hdl.handle.net/20.500.12386/32282We 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 were obtained with different X-ray satellites, namely XMM-Newton, NuSTAR, Swift, and Chandra, and cover different time intervals, from a few days to years. From 2006 to 2013 the source had a 2-10 keV flux of ∼1.5 × 10<SUP>−11</SUP> erg cm<SUP>−2</SUP> s<SUP>−1</SUP>, consistent with archival observations based on HEAO and BeppoSAX data, though a 2019 Chandra snapshot caught the source in an extreme low flux state a factor of ∼10 fainter than its historical level. 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 Γ = 1.76 ± 0.09 with a high energy cut-off at E<SUB>c</SUB> = 70<SUB>−14</SUB><SUP>+21</SUP> keV that is absorbed by a fairly constant column density of N<SUB>H</SUB> = (6.3 ± 0.5) × 10<SUP>22</SUP> cm<SUP>−2</SUP>. 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<SUB>e</SUB> = 27<SUB>−4</SUB><SUP>+8</SUP> keV, τ<SUB>e</SUB> = 5.5 ± 1.3 and kT<SUB>e</SUB> = 28<SUB>−5</SUB><SUP>+7</SUP> keV, τ = 3.2 ± 0.8, respectively. Finally, despite the short duration of the exposures, possible evidence of the presence of outflows is discussed.STAMPAenArticle10.1051/0004-6361/2020399842-s2.0-85102963474http://arxiv.org/abs/2101.08793v1https://www.aanda.org/articles/aa/full_html/2021/03/aa39984-20/aa39984-20.html2021A&A...647A.102MFIS/05 - ASTRONOMIA E ASTROFISICA