Morphology and Kinematics of Interstellar Matter in the Vicinity of Young Stars ZZ Tau and ZZ Tau IRS

Abstract

The morphology and kinematics of the matter in the vicinity of young stars ZZ Tau and ZZ Tau IRS are studied. It has been found that the emission nebula (the H\(\alpha\) filament) located southwest of these stars, as well as the Herbig–Haro object HH 393 projected onto it are moving away from ZZ Tau and ZZ Tau IRS with a radial velocity of about 50 km s\({}^{-1}\). On the inner edge of the western part of the H\(\alpha\) filament, there is a cooler filament emiting in the molecular hydrogen line (\(\lambda=2.12\) \(\mu\)m) and in the dust continuum. In the northeastern part of the studied region, a new Herbig–Haro object is discovered and assigned the number HH 1232. The presence of several more new emission nebulae is suspected. The electron density in the studied regions of the H\(\alpha\) filament, as well as HH 393 and HH 1232 \(N_{e}\lesssim 100\) cm\({}^{-3}\). Arguments are presented in favor of the fact that the dusty disk wind has created a gas-and-dust nebula around ZZ Tau IRS, along the symmetry axis of which there is a jet moving in the direction of HH 393.