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dc.contributor.authorWeintroub, Jonathan
dc.contributor.authorMoran, James M.
dc.contributor.authorWilner, David J.
dc.contributor.authorYoung, Ken Harbour
dc.contributor.authorRao, Ramprasad
dc.contributor.authorShinnaga, Hiroko
dc.date.accessioned2014-01-29T15:59:48Z
dc.date.issued2008
dc.identifier.citationWeintroub, Jonathan, James M. Moran, David J. Wilner, Ken Harbour Young, Ramprasad Rao, and Hiroko Shinnaga. 2008. “Submillimeter Array Imaging of the Maser Emission from the \(H30\alpha\) Radio Recombination Line in MWC 349A.” Astrophysical Journal 677 (2) (April 20): 1140-1150. doi:10.1086/529132.en_US
dc.identifier.issn0004-637Xen_US
dc.identifier.issn1538-4357en_US
dc.identifier.urihttp://nrs.harvard.edu/urn-3:HUL.InstRepos:11595848
dc.description.abstractWe used the Submillimeter Array to map the angular distribution of the H30α recombination line (231.9 GHz) in the circumstellar region of the peculiar star MWC 349A. The resolution was 1.2'', but because of high signal-to-noise ratio we measured the positions of all maser components to accuracies better than 0.01'', at a velocity resolution of \(1 km s^{−1}\). The two strongest maser components (called high-velocity components) at velocities near –14 and \(32 km s^{−1}\) are separated by 0.048'' ± 0.001'' (60 AU) along a position angle of 102° ± 1°. The distribution of maser emission at velocities between and beyond these two strongest components were also provided. The continuum emission lies at the center of the maser distribution to within 10 mas. The masers appear to trace a nearly edge-on rotating disk structure, reminiscent of the water masers in Keplerian rotation in the nuclear accretion disk of the galaxy NGC 4258. However, the maser components in MWC 349A do not follow a simple Keplerian kinematic prescription with v ~ \(r^{−1/2}\), but have a larger power-law index. We explore the possibility that the high-velocity masers trace spiral density or shock waves. We also emphasize caution in the interpretation of relative centroid maser positions where the maser is not clearly resolved in position or velocity, and we present simulations that illustrate the range of applicability of the centroiding method.en_US
dc.description.sponsorshipAstronomyen_US
dc.language.isoen_USen_US
dc.publisherAmerican Astronomical Societyen_US
dc.relation.isversionofdoi:10.1086/529132en_US
dc.relation.hasversionhttp://arxiv.org/abs/0801.0608
dash.licenseLAA
dc.subjectcircumstellar matteren_US
dc.subjectmasersen_US
dc.subjectradio linesen_US
dc.subjectstarsen_US
dc.subjectemission lineen_US
dc.subjectwindsen_US
dc.subjectoutflowsen_US
dc.titleSubmillimeter Array Imaging of the Maser Emission from the \(H30\alpha\) Radio Recombination Line in MWC 349Aen_US
dc.typeJournal Articleen_US
dc.description.versionVersion of Recorden_US
dc.relation.journalAstrophysical Journalen_US
dash.depositing.authorMoran, James M.
dc.date.available2014-01-29T15:59:48Z
dc.identifier.doi10.1086/529132*
workflow.legacycommentsPer Sherpa can deposit publisher's versionen_US
dash.contributor.affiliatedYoung, Ken
dash.contributor.affiliatedWeintroub, Jonathan
dash.contributor.affiliatedWilner, David
dash.contributor.affiliatedMoran, James


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