Simultaneous 183 GHz H2O maser and SiO observations towards evolved stars using APEX SEPIA Band 5

摘要

Aims. The aim is to investigate the use of 183 GHz H _(2) O masers for characterization of the physical conditions and mass loss process in the circumstellar envelopes of evolved stars. Methods. We used APEX SEPIA Band 5 (an ALMA Band 5 receiver on the APEX telescope) to observe the 183 GHz H _(2) O line towards two red supergiant (RSG) and three asymptotic giant branch (AGB) stars. Simultaneously, we observed the J = 4 ? 3 line for ~(28) SiO v = 0 , 1, 2 and 3, and for ~(29) SiO v = 0 and 1. We compared the results with simulations and radiative transfer models for H _(2) O and SiO, and examined data for the individual linear orthogonal polarizations. Results. We detected the 183 GHz H _(2) O line towards all the stars with peak flux densities & 100 Jy, including a new detection from VY?CMa. Towards all five targets, the water line had indications of being caused by maser emission and had higher peak flux densities than for the SiO lines. The SiO lines appear to originate from both thermal and maser processes. Comparison with simulations and models indicate that 183 GHz maser emission is likely to extend to greater radii in the circumstellar envelopes than SiO maser emission and to similar or greater radii than water masers at 22, 321 and 325 GHz. We speculate that a prominent blue-shifted feature in the W?Hya 183 GHz spectrum is amplifying the stellar continuum, and is located at a similar distance from the star as mainline OH maser emission. We note that the coupling of an SiO maser model to a hydrodynamical pulsating model of an AGB star yields qualitatively similar simulated results to the observations. From a comparison of the individual polarizations, we find that the SiO maser linear polarization fraction of several features exceeds the maximum fraction allowed under standard maser assumptions and requires strong anisotropic pumping of the maser transition and strongly saturated maser emission. The low polarization fraction of the H _(2) O maser however, fits with the expectation for a non-saturated maser. Conclusions. 183 GHz H _(2) O masers can provide strong probes of the mass loss process of evolved stars. Higher angular resolution observations of this line using ALMA Band 5 will enable detailed investigation of the emission location in circumstellar envelopes and can also provide information on magnetic field strength and structure.