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ALMA sub-mm maser and dust distribution of VY Canis Majoris

dc.contributor.authorRICHARDS, A. M. S.
dc.contributor.authorIMPELLIZZERI, C. M. V.
dc.contributor.authorHUMPHREYS, E. M.
dc.contributor.authorVLAHAKIS, C.
dc.contributor.authorVLEMMINGS, W.
hal.structure.identifierFORMATION STELLAIRE 2014
hal.structure.identifierObservatoire aquitain des sciences de l'univers [OASU]
hal.structure.identifierLaboratoire d'Astrophysique de Bordeaux [Pessac] [LAB]
dc.contributor.authorBAUDRY, Alain
dc.contributor.authorDE BECK, E.
dc.contributor.authorDECIN, L.
dc.contributor.authorETOKA, S.
dc.contributor.authorGRAY, M. D.
dc.contributor.authorHARPER, G. M.
dc.contributor.authorHUNTER, T. R.
hal.structure.identifierLaboratoire d'études spatiales et d'instrumentation en astrophysique [LESIA]
dc.contributor.authorKERVELLA, P.
dc.contributor.authorKERSCHBAUM, F.
dc.contributor.authorMCDONALD, I.
hal.structure.identifierInstitut de Planétologie et d'Astrophysique de Grenoble [IPAG ]
dc.contributor.authorMELNICK, G.
hal.structure.identifierLaboratoire Biodiversité et Fonctionnement des Ecosystèmes [LBFE]
dc.contributor.authorMULLER, S.
hal.structure.identifierJohns Hopkins University [JHU]
dc.contributor.authorNEUFELD, D.
dc.contributor.authorO’GORMAN, E.
dc.contributor.authorPARFENOV, S. Yu.
dc.contributor.authorPECK, A. B.
dc.contributor.authorSHINNAGA, H.
hal.structure.identifierUral State University
dc.contributor.authorSOBOLEV, A. M.
hal.structure.identifierEuropean Southern Observatory [ESO]
dc.contributor.authorTESTI, L.
dc.contributor.authorUSCANGA, L.
dc.contributor.authorWOOTTEN, A.
dc.contributor.authorYATES, J. A.
dc.contributor.authorZIJLSTRA, A.
dc.date.issued2014-12
dc.identifier.issn0004-6361
dc.description.abstractEnAims: Cool, evolved stars have copious, enriched winds. Observations have so far not fully constrained models for the shaping and acceleration of these winds. We need to understand the dynamics better, from the pulsating stellar surface to ~10 stellar radii, where radiation pressure on dust is fully effective. Asymmetric nebulae around some red supergiants imply the action of additional forces. Methods: We retrieved ALMA Science Verification data providing images of sub-mm line and continuum emission from VY CMa. This enables us to locate water masers with milli-arcsec accuracy and to resolve the dusty continuum. Results: The 658, 321, and 325 GHz masers lie in irregular, thick shells at increasing distances from the centre of expansion. For the first time this is confirmed as the stellar position, coinciding with a compact peak offset to the NW of the brightest continuum emission. The maser shells overlap but avoid each other on scales of up to 10 au. Their distribution is broadly consistent with excitation models but the conditions and kinematics are complicated by wind collisions, clumping, and asymmetries.Appendices are available in electronic form at http://www.aanda.org
dc.language.isoen
dc.publisherEDP Sciences
dc.title.enALMA sub-mm maser and dust distribution of VY Canis Majoris
dc.typeArticle de revue
dc.identifier.doi10.1051/0004-6361/201425024
dc.subject.halPhysique [physics]/Astrophysique [astro-ph]
dc.subject.halPlanète et Univers [physics]/Astrophysique [astro-ph]/Astrophysique stellaire et solaire [astro-ph.SR]
dc.identifier.arxiv1409.5497
bordeaux.journalAstronomy and Astrophysics - A&A
bordeaux.pageid.L9
bordeaux.volume572
bordeaux.peerReviewedoui
hal.identifierhal-01092644
hal.version1
hal.popularnon
hal.audienceInternationale
hal.origin.linkhttps://hal.archives-ouvertes.fr//hal-01092644v1
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