2006/10/16 by C. Goddi, L. Moscadelli, A. Sanna +2 · 37 citations
Chemistry · Earth and Planetary Sciences · Physics and Astronomy · #Angular resolution (graph drawing) #Astrophysics and Star Formation Studies #Atmospheric Ozone and Climate #Maser #Methanol #Molecular Spectroscopy and Structure #Outflow #Star formation #Stars #Young stellar object #astro-ph
paper · pdf · doi:10.1051/0004-6361:20066136
published in Astronomy and Astrophysics 461(3), 1027-1035 (EDP Sciences) · 11 pages, 3 figures, accepted for publication in Astronomy & Astrophysics
arxiv created 2006/10/16 · openalex publication_date 2006/10/16 · arxiv updated 2009/12/01 · openalex created_date 2016/06/24 · openalex updated_date 2026/08/05
<i>Context.<i/>While high-angular resolution observations have clarified that water masers originate from shocks associated with protostellar jets, different environments have been proposed in several sources to explain the origin of CH<sub>3<sub/>OH masers.<i>Aims.<i/>We wish to investigate the nature of the CH<sub>3<sub/>OH maser birthplace in SFRs and the association between the H<sub>2<sub/>O and CH<sub>3<sub/>OH maser emission in the same YSO. <i>Methods.<i/>We have conducted phase-reference VLBI observations of H<sub>2<sub/>O and CH<sub>3<sub/>OH masers toward two high-mass SFRs, Sh 2-255 IR and AFGL 5142.<i>Results.<i/>In Sh 2-255 IR water masers are aligned along a direction close to the orientation of the molecular outflow observed on angular scales of 1–10 arcsec, tracing possibly the disk-wind emerging from the disk atmosphere. In AFGL 5142 water masers trace expansion at the base of a protostellar jet, whilst methanol masers are more probably tracing infalling than outflowing gas.<i>Conclusions.<i/>The results for AFGL 5142 suggest that water and methanol masers trace different kinematic structures in the circumstellar gas.