Discovery of a low-mass companion inside the debris ring surrounding the F5V star HD 206893
Kennedy, G. M.
Wyatt, M. C.
Gómez González, C. A.
del Burgo, C.
Dent, W. R. F.
Girard, J. H.
AffiliationUniv Arizona, Steward Observ
MetadataShow full item record
PublisherEDP SCIENCES S A
CitationDiscovery of a low-mass companion inside the debris ring surrounding the F5V star HD 206893 2016, 597:L2 Astronomy & Astrophysics
JournalAstronomy & Astrophysics
Rights© ESO, 2016
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.
AbstractAims. Uncovering the ingredients and the architecture of planetary systems is a very active field of research that has fuelled many new theories on giant planet formation, migration, composition, and interaction with the circumstellar environment. We aim at discovering and studying new such systems, to further expand our knowledge of how low-mass companions form and evolve. Methods. We obtained high-contrast H-band images of the circumstellar environment of the F5V star HD 206893, known to host a debris disc never detected in scattered light. These observations are part of the SPHERE High Angular Resolution Debris Disc Survey (SHARDDS) using the InfraRed Dual-band Imager and Spectrograph (IRDIS) installed on VLT/SPHERE. Results. We report the detection of a source with a contrast of 3 : 6 x 10(-5) in the H-band, orbiting at a projected separation of 270 milliarcsec or 10 au, corresponding to a mass in the range 24 to 73 M-Jup for an age of the system in the range 0.2 to 2 Gyr. The detection was confirmed ten months later with VLT /NaCo, ruling out a background object with no proper motion. A faint extended emission compatible with the disc scattered light signal is also observed. Conclusions. The detection of a low-mass companion inside a massive debris disc makes this system an analog of other young planetary systems such as beta Pictoris, HR 8799 or HD 95086 and requires now further characterisation of both components to understand their interactions.
VersionFinal published version
SponsorsESO fellowship programme; NASA through Hubble Fellowship by STScI [HST-HF2-51355, HST-AR-12652]; NASA [NAS5-26555]; European Research Council under the European Union's Seventh Framework Programme (ERC Grant) ; French Community of Belgium through an ARC grant for Concerted Research Action; Royal Society; European Union through ERC grant ; Millennium Science Initiative (Chilean Ministry of Economy) [RC130007]; Mexican CONACyT [CB-2012-183007]