Astronomy and Astrophysics, volume 592A, 31-31 (2016/8-1)
Physical characteristics of bright Class I methanol masers.
LEURINI S., MENTEN K.M. and WALMSLEY C.M.
Abstract (from CDS):
Context. Class I methanol masers are thought to be tracers of interstellar shock waves. However, they have received relatively little attention mostly as a consequence of their low luminosities compared to other maser transitions. This situation has changed recently and Class I methanol masers are now routinely used as signposts of outflow activity especially in high extinction regions. The recent detection of polarisation in Class I lines now makes it possible to obtain direct observational information about magnetic fields in interstellar shocks. Aims. We make use of newly calculated collisional rate coefficients for methanol to investigate the excitation of Class I methanol masers and to reconcile the observed Class I methanol maser properties with model results. Methods. We performed large velocity gradient calculations with a plane-parallel slab geometry appropriate for shocks to compute the pump and loss rates which regulate the interactions of the different maser systems with the maser reservoir. We study the dependence of the pump rate coefficient, the maser loss rate, and the inversion efficiency of the pumping scheme of several Class I masers on the physics of the emitting gas. Results. We predict inversion in all transitions where maser emission is observed. Bright Class I methanol masers are mainly high-temperature (>100 K) high-density (n(H2)∼107-108cm–3) structures with methanol maser emission measures, ξ, corresponding to high methanol abundances close to the limits set by collisional quenching. Our model predictions reproduce reasonably well most of the observed properties of Class I methanol masers. Class I masers in the 25GHz series are the most sensitive to the density of the medium and mase at higher densities than other lines. Moreover, even at high density and high methanol abundances, their luminosity is predicted to be lower than that of the 44GHz and 36GHz masers. Our model predictions also reflect the observational result that the 44GHz line is almost always stronger than the 36GHz maser. By comparison between observed isotropic photon luminosities and our model predictions, we infer maser beam solid angles of roughly 10–3 steradian. Conclusions. We find that the Class I masers can reasonably be separated into three families: the (J+1)–1-J0-E type series, the (J+1)0-J1-A type, and the J2-J1-E lines at 25GHz. The 25GHz lines behave in a different fashion from the other masers as they are only inverted at high densities above 106cm–3 in contrast to other Class I masers. Therefore, the detection of maser activity in all three families is a clear indication of high densities.