AuthorGordon, Michael S.
Jones, Terry J.
Humphreys, Roberta M.
Hinz, Philip M.
Hoffmann, William F.
AffiliationUniv Arizona, Dept Astron, Steward Observ
MetadataShow full item record
PublisherIOP PUBLISHING LTD
CitationMichael S. Gordon et al 2019 AJ 157 57
Rights© 2019. The American Astronomical Society. All rights reserved.
Collection InformationThis item from the UA Faculty Publications collection is made available by the University of Arizona with support from the University of Arizona Libraries. If you have questions, please contact us at firstname.lastname@example.org.
AbstractWe present high spatial resolution LBTI/NOMIC 9-12 mu m images of VY CMa and its massive outflow feature, the Southwest (SW) Clump. Combined with high-resolution imaging from the Hubble Space Telescope (0.4-1 mu m) and LBT/LMIRCam (1-5 mu m), we isolate the spectral energy distribution (SED) of the clump from the star itself. Using radiative-transfer code DUSTY, we model both the scattered light from VY CMa and the thermal emission from the dust in the clump to estimate the optical depth, mass, and temperature of the SW Clump. The SW Clump is optically thick at 8.9 mu m with a brightness temperature of similar to 200 K. With a dust chemistry of equal parts silicates and metallic iron, as well as assumptions on grain size distribution, we estimate a dust mass of 5.4 x 10(-5) M-circle dot. For a gas-to-dust ratio of 100, this implies a total mass of 5.4 x 10(-3) M-circle dot. Compared to the typical mass-loss rate of VY CMa, the SW Clump represents an extreme, localized mass-loss event from less than or similar to 300 yr ago.
VersionFinal published version
SponsorsUniversity of Minnesota Graduate School's Doctoral Dissertation Fellowship