PANCHROMATIC IMAGING OF A TRANSITIONAL DISK: THE DISK OF GM AUR IN OPTICAL AND FUV SCATTERED LIGHT
AuthorHornbeck, J. B.
Swearingen, J. R.
Grady, C. A.
Williger, G. M.
Sitko, M. L.
Wisniewski, J. P.
Perrin, M. D.
Lauroesch, J. T.
Brown, J. M.
Champney, E. H.
Lynch, D. K.
Russell, R. W.
Walter, F. M.
AffiliationUniv Arizona, Steward Observ
Univ Arizona, Dept Planetary Sci
Univ Arizona, Lunar & Planetary Lab
stars: individual (GM Aur)
stars: variables: T Tauri, Herbig Ae/Be
ultraviolet: planetary systems
MetadataShow full item record
PublisherIOP PUBLISHING LTD
CitationPANCHROMATIC IMAGING OF A TRANSITIONAL DISK: THE DISK OF GM AUR IN OPTICAL AND FUV SCATTERED LIGHT 2016, 829 (2):65 The Astrophysical Journal
JournalThe Astrophysical Journal
Rights© 2016. 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 have imaged GM Aurigae with the Hubble Space Telescope, detected its disk in scattered light at 1400 and 1650 angstrom, and compared these with observations at 3300 angstrom, 5550 angstrom, 1.1 mu m, and 1.6 mu m. The scattered light increases at shorter wavelengths. The radial surface brightness profile at 3300 angstrom shows no evidence of the 24 au radius cavity that has been previously observed in submillimeter observations. Comparison with dust grain opacity models indicates that. the surface of the entire disk is populated with submicron grains. We have compiled a. spectral energy distribution from 0.1 mu m to 1 mm. and used it to constrain a model of the star + disk system that includes the submillimeter cavity using the Monte Carlo radiative transfer code by Barbara Whitney. The best-fit model image indicates that the cavity should be detectable in the F330W bandpass if the cavity has been cleared of both large and small dust grains, but we do not detect it. The lack of an observed cavity can be explained by the presence of submicron grains interior to the submillimeter cavity wall. We suggest one explanation for this that. could be due to a planet of mass <9 M-J interior to 24 au. A unique cylindrical structure is detected in the far-UV data from the Advanced Camera for Surveys/ Solar Blind Channel. It is aligned along the system semiminor axis, but does not resemble an accretion-driven jet. The structure is limb. brightened and extends 190 +/- 35 au above the disk midplane. The inner radius of the limb. brightening is 40 +/- 10 au, just beyond the submillimeter cavity wall.
VersionFinal published version
SponsorsNASA [NAS 5-26555, NNH06CC28C, NNX09AC73G]; NASA Kentucky Space Grant Consortium [3049024102-11-175]; [HST-GO-10864]; [HST-GO-11336]; [HST-GO-12016]; [HST-GO-11336.01-A]