SIMBAD references

Spectrophotometric observations of the Hα and He I λ6678 emission lines of the nova-like cataclysmic variable V3885 Sgr are presented and analyzed. The binary orbital period was determined as P=0.20716071(22) days. Doppler tomography was performed with both Hα and He I lines. Disk radial emissivity profiles were also computed. The tomography mapping of flickering sources was performed using the Hα line, from which we concluded that the flickering is not uniformly distributed on the disk. The observed tomogram of the flickering was compared with simulations, suggesting that the most intense flickering source in the Hα is not located in the accretion disk. It is proposed that the main line-flickering source might be associated with the illuminated secondary star.