First Scattered-light Images of the Gas-rich Debris Disk around 49 Ceti
Chen, Christine H.
Debes, John H.
Burgo, Carlos del
Dent, William R. F.
Girard, Julien H.
Golimowski, David A.
González, Carlos A. Gómez
Hagan, J. Brendan
Hines, Dean C.
Kennedy, Grant M.
Perrin, Marshall D.
AffiliationUniv Arizona, Dept Astron, Steward Observ
MetadataShow full item record
PublisherIOP PUBLISHING LTD
CitationFirst Scattered-light Images of the Gas-rich Debris Disk around 49 Ceti 2017, 834 (2):L12 The Astrophysical Journal
JournalThe Astrophysical Journal
Rights© 2017. 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 email@example.com.
AbstractWe present the first scattered-light images of the debris disk around 49 Ceti, a similar to 40 Myr A1 main-sequence star at 59 pc, famous for hosting two massive dust belts as well as large quantities of atomic and molecular gas. The outer disk is revealed in reprocessed archival Hubble Space Telescope NICMOS-F110W images, as well as new coronagraphic H-band images from the Very Large Telescope SPHERE instrument. The disk extends from 1 1 (65 au) to 4.'' 6 (250 au) and is seen at an inclination of 73 degrees, which refines previous measurements at lower angular resolution. We also report no companion detection larger than 3 M-Jup at projected separations beyond 20 au from the star (0.'' 34). Comparison between the F110W and H-band images is consistent with a gray color of 49 Ceti's dust, indicating grains larger than greater than or similar to 2 mu m. Our photometric measurements indicate a scattering efficiency/infrared excess ratio of 0.2-0.4, relatively low compared to other characterized debris disks. We find that 49 Ceti presents morphological and scattering properties very similar to the gas-rich HD 131835 system. From our constraint on the disk inclination we find that the atomic gas previously detected in absorption must extend to the inner disk, and that the latter must be depleted of CO gas. Building on previous studies, we propose a schematic view of the system describing the dust and gas structure around 49 Ceti and hypothetical scenarios for the gas nature and origin.
VersionFinal published version
SponsorsNASA through Hubble Fellowship - STScI [HST-HF2-51355]; AURA, Inc. [NAS5-26555]; ESO through the ESO fellowship program; DFG [Kr 2164/15-1]; Mexican CONACyT [CB-2012-183007]; STFC; Programme National de Plane-tologie; European Union through ERC [337569, 279973]; [HST-AR-12652]