Bernardini, F.F.BernardiniDE MARTINO, DomitillaDomitillaDE MARTINOMukai, K.K.MukaiISRAEL, Gian LucaGian LucaISRAELFalanga, M.M.FalangaRamsay, G.G.RamsayMASETTI, NICOLANICOLAMASETTI2020-03-042020-03-0420150035-8711http://hdl.handle.net/20.500.12386/23114This work is based on observations obtained with XMM–Newton an ESA science mission directly funded by ESA Member States, with Swift , a National Aeronautics and Space Administration (NASA) science mission with Italian participation. This publication also makes use of data products from the Two Micron All Sky Survey (2MASS), which is a joint project of the University of Massacusetts and the Infrared Processing and Analysis Center (California Institute of Technology), funded by NASA and National Science Fundation. It also makes use of data products from the WISE , which is a joint project of the University of California, Los Angeles and the Jet Propulsion Laboratory/California Institute of Technology, funded by the NASA. We acknowledge financial support from ASI INAF I/037/12/0.IGR J04571+4527 and Swift J0525.6+2416 are two hard X-ray sources detected in the Swift/BAT and INTEGRAL/IBIS surveys. They were proposed to be magnetic cataclysmic variables of the intermediate polar (IP) type, based on optical spectroscopy. IGR J04571+4527 also showed a 1218 s optical periodicity, suggestive of the rotational period of a white dwarf, further pointing towards an IP classification. We here present detailed X-ray (0.3-10 keV) timing and spectral analysis performed with XMM-Newton, complemented with hard X-ray coverage (15-70 keV) from Swift/BAT. These are the first high-S/N observations in the soft X-ray domain for both sources, allowing us to identify the white dwarf X-ray spin period of Swift J0525.6+2416 (226.28 s), and IGR J04571+4527 (1222.6 s). A model consisting of multitemperature optically thin emission with complex absorption adequately fits the broad-band spectrum of both sources. We estimate a white dwarf mass of about 1.1 and 1.0 M<SUB>☉</SUB> for IGR J04571+4527 and Swift J0525.6+2416, respectively. The above characteristics allow us to unambiguously classify both sources as IPs, confirming the high incidence of this subclass among hard X-ray emitting cataclysmic variables.STAMPAenArticle10.1093/mnras/stv16732-s2.0-84947753061000363649000067https://academic.oup.com/mnras/article/453/3/3100/10753762015MNRAS.453.3100BFIS/05 - ASTRONOMIA E ASTROFISICAScienze Fisiche Settori ERC (ERC) di riferimento::PE9 Universe sciences: astro-physics/chemistry/biology; solar systems; stellar, galactic and extragalactic astronomy, planetary systems, cosmology, space science, instrumentation::PE9_11 Relativistic astrophysics