Multiple Rings of Millimeter Dust Emission in the HD 15115 Debris Disk
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Author
MacGregor, Meredith A.Weinberger, Alycia J.
Nesvold, Erika R.
Hughes, A. Meredith
Wilner, D. J.
Currie, Thayne
Debes, John H.

Donaldson, Jessica K.
Redfield, Seth

Roberge, Aki
Schneider, Glenn

Affiliation
Univ Arizona, Steward ObservIssue Date
2019-05-31
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IOP PUBLISHING LTDCitation
Meredith A. MacGregor et al 2019 ApJL 877 L32Journal
ASTROPHYSICAL JOURNAL LETTERSRights
Copyright © 2019. The American Astronomical Society. All rights reserved.Collection Information
This 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 repository@u.library.arizona.edu.Abstract
We present observations of the HD 15115 debris disk from the Atacama Large Millimeter/submillimeter Array (ALMA) at 1.3 mm that capture this intriguing system with the highest resolution (0 ''.6 or 29 au) at millimeter wavelengths to date. This new ALMA image shows evidence for two rings in the disk separated by a cleared gap. By fitting models directly to the observed visibilities within a Markov Chain Monte Carlo framework, we are able to characterize the millimeter continuum emission and place robust constraints on the disk structure and geometry. In the best-fit model of a power-law disk with a Gaussian gap, the disk inner and outer edges are at 43.9 +/- 5.8 au (0 ''.89 +/- 0 ''.12) and 92.2 +/- 2.4 au (1 ''.88 +/- 0 ''.49), respectively, with a gap located at 58.9 +/- 4.5 au (1 ''.2 +/- 0 ''.10) with a fractional depth of 0.88 +/- 0.10 and a width of 13.8 +/- 5.6 au (0 ''.28 +/- 0 ''.11). Because we do not see any evidence at millimeter wavelengths for the dramatic east-west asymmetry seen in scattered light, we conclude that this feature most likely results from a mechanism that only affects small grains. Using dynamical modeling and our constraints on the gap properties, we are able to estimate a mass for the possible planet sculpting the gap to be 0.16 +/- 0.06 M-Jup.ISSN
2041-8205Version
Final published versionSponsors
National Science Foundation Astronomy and Astrophysics Postdoctoral Fellowship [AST-1701406]; NSF [AST-1412647, AST-1313268]ae974a485f413a2113503eed53cd6c53
10.3847/2041-8213/ab21c2