Abstract
The spectral and photometric studies of the cataclysmic variable Gaia 19cwm (or ZTF19aamkwxk) have been performed. Based on the analysis of long-term variability, it is concluded that the object belongs to WZ Sge type stars. The light curves show eclipses recurring with an orbital period of \(86.32048\pm 0.00005\) min, as well as an out-of-eclipse variability with a period of \({\approx}6.45\) min. The latter period is stable for \({\sim}4\) years and appears to correspond to the rotation of a magnetic white dwarf, i.e., Gaia 19cwm is an intermediate polar. The Gaia 19cwm spectra show photospheric lines of the white dwarf, and Doppler tomograms demonstrate the presence of an accretion disk and a hot spot. Analysis of the eclipse light curve gives an estimates of the white dwarf mass \(M_{1}=0.66\pm 0.06\) \(M_{\odot}\) , the donor mass \(M_{2}=0.073\pm 0.015\) \(M_{\odot}\) , and the orbital inclination \(i=83.8^{\circ}\pm 1.1^{\circ}\) . Modeling of the spectral energy distribution gives the white dwarf temperature of \(T_{\textrm{eff}}\approx 13\,000\) K. The X-ray luminosity \(L_{X}=(1.6\pm 0.3)\times 10^{31}\) erg/s allows to assign Gaia 19cwm to a small group of low-luminosity intermediate polars.
