IGR J14257−6117, a magnetic accreting white dwarf with a very strong strong X-ray orbital modulation
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Type of Work8 pages
Citation of Original PublicationBernardini, F.; de Martino, D.; Mukai, K.; Falanga, M.; IGR J14257−6117, a magnetic accreting white dwarf with a very strong strong X-ray orbital modulation; Monthly Notices of the Royal Astronomical Society, Volume 478, Issue 1, (2018); https://academic.oup.com/mnras/article/478/1/1185/4989942
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IGR J14257−6117 (aka 4PBC J1425.1-6118)
IGR J14257−6117 is an unclassified source in the hard X-ray catalogues. Optical follow-ups suggest it could be a Cataclysmic Variable (CV) of the magnetic type. We present the first high signal-to-noise (S/N) X-ray observation performed by XMM–Newton at 0.3–10 keV, complemented with 10–80 keV coverage by Swift/BAT, aimed at revealing the source nature. We detected for the first time a fast periodic variability at 509.5 s and a longer periodic variability at 4.05 h, ascribed to the white dwarf (WD) spin and binary orbital periods, respectively. These unambiguously identify IGR J14257−6117 as a magnetic CV of the intermediate polar (IP) type. The energy-resolved light curves at both periods reveal amplitudes decreasing with increasing energy, with the orbital modulation reaching ∼100 per cent in the softest band. The energy spectrum shows optically thin thermal emission with an excess at the iron complex, absorbed by two dense media (NH ∼ 10²²⁻²³ cm⁻²), partially covering the X-ray source. These are likely localized in the magnetically confined accretion flow above the WD surface and at the disc rim, producing the energy-dependent spin and orbital variabilities, respectively. IGR J14257−6117 joins the group of strongest orbitally modulated IPs now counting four systems. Drawing similarities with low-mass X-ray binaries displaying orbital dips, these IPs should be seen at large orbital inclinations allowing azimuthally extended absorbing material fixed in the binary frame to intercept the line of sight. For IGR J14257−6117, we estimate 50⁰ < i < 70⁰. Whether also the mass accretion rate plays a role in the large orbital modulations in IPs cannot be established with the present data.