Bernardini, F.de Martino, D.Mukai, K.Russell, D.M.Falanga, M.Masetti, N.Ferrigno, C.Israel, G.2018-01-042018-01-042017-10Monthly Notices of the Royal Astronomical Society, 470 (4) pp. 4815 - 48370035-8711https://doi.org/10.1093/mnras/stx1494http://repositorio.unab.cl/xmlui/handle/ria/5032Indexación: Web of Science; Scopus.We present timing and spectral analysis of a sample of seven hard X-ray selected cataclysmic variable candidates based on simultaneous X-ray and optical observations collected with XMM–Newton, complemented with Swift/BAT and INTEGRAL /IBIS hard X-ray data and ground-based optical photometry. For six sources, X-ray pulsations are detected for the first time in the range of ∼296–6098 s, identifying them as members of the magnetic class. Swift J0927.7−6945, Swift J0958.0−4208, Swift J1701.3−4304, Swift J2113.5+5422 and possibly PBC J0801.2−4625 are intermediate polars (IPs), while Swift J0706.8+0325 is a short (1.7 h) orbital period polar, the 11th hard X-ray-selected identified so far. X-ray orbital modulation is also observed in Swift J0927.7−6945 (5.2 h) and Swift J2113.5+5422 (4.1 h). Swift J1701.3−4304 is discovered as the longest orbital period (12.8 h) deep eclipsing IP. The spectra of the magnetic systems reveal optically thin multitemperature emission between 0.2 and 60 keV. Energy-dependent spin pulses and the orbital modulation in Swift J0927.7−6945 and Swift J2113.5+5422 are due to intervening local high-density absorbing material (NH ∼ 1022 − 23 cm−2). In Swift J0958.0−4208 and Swift J1701.3−4304, a soft X-ray blackbody (kT ∼ 50 and ∼80 eV) is detected, adding them to the growing group of ‘soft’ IPs. White dwarf masses are determined in the range of ∼0.58–1.18 M, indicating massive accreting primaries in five of them. Most sources accrete at rates lower than the expected secular value for their orbital period. Formerly proposed as a long-period (9.4 h) nova-like CV, Swift J0746.3−1608 shows peculiar spectrum and light curves suggesting either an atypical low-luminosity CV or a low-mass X-ray binary.ennovae, cataclysmic variables – white dwarfs – X-rays: binaries – X-rays: individual: Swift J0706.8+0325 – X-rays: individual: Swift J0746.3−1608 (aka 1RXS J074616.8−161127) – X-rays: individual: Swift J0927.7−6945 – X-rays: individual: Swift J0958.0−4208 – X-rays: individual: PBC J0801.2−4625 (aka 1RXS J080114.6-462324) – X-rays: individual: Swift J1701.3−4304 (aka IGR J17014-4306) – X-rays: individual: Swift J2113.5+5422.Artículo