Bernardini, F.F.BernardiniDE MARTINO, DomitillaDomitillaDE MARTINOMukai, K.K.MukaiRussell, D. M.D. M.RussellFalanga, M.M.FalangaMASETTI, NICOLANICOLAMASETTIFerrigno, C.C.FerrignoISRAEL, Gian LucaGian LucaISRAEL2020-09-102020-09-1020170035-8711http://hdl.handle.net/20.500.12386/27277We 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 (N<SUB>H</SUB> ∼ 10<SUP>22 - 23</SUP> cm<SUP>-2</SUP>). 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<SUB>☉</SUB>, 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.STAMPAenArticle10.1093/mnras/stx14942-s2.0-85026320425000408207600074https://academic.oup.com/mnras/article/470/4/4815/3906588https://arxiv.org/pdf/1706.04005.pdf2017MNRAS.470.4815BFIS/05 - ASTRONOMIA E ASTROFISICAERC sectors::Physical Sciences and Engineering