Discovery of a low-mass companion inside the debris ring surrounding the F5V star HD 206893Reportar como inadecuado


Discovery of a low-mass companion inside the debris ring surrounding the F5V star HD 206893


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Publication Date: 2017-01

Journal Title: Astronomy and Astrophysics

Publisher: EDP Sciences

Volume: 597

Number: L2

Language: English

Type: Article

This Version: VoR

Metadata: Show full item record

Citation: Milli, J., Hibon, P., Christiaens, V., Choquet,, Bonnefoy, M., Kennedy, G. M., Wyatt, M. C., et al. (2017). Discovery of a low-mass companion inside the debris ring surrounding the F5V star HD 206893. Astronomy and Astrophysics, 597 (L2)https://doi.org/10.1051/0004-6361/201629908

Abstract: Aims. 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 × 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 MJup 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 β Pictoris, HR 8799 or HD 95086 and requires now further characterisation of both components to understand their interactions.

Sponsorship: J.M. is supported by the ESO fellowship programme. E.C. is supported by NASA through Hubble Fellowship grant HST-HF2-51355 and HST-AR-12652 awarded by STScI, operated by the AURA, Inc., for NASA under contract NAS5-26555. O.A. is a F.R.S.-FNRS Research Associate. The research leading to these results was partly funded by the European Research Council under the European Union’s Seventh Framework Programme (ERC Grant Agreement No. 337569), and by the French Community of Belgium through an ARC grant for Concerted Research Action. G.M.K. is supported by the Royal Society as a Royal Society University Research Fellow. M.C.W. and L.M. are supported by the European Union through ERC grant 279973. V.C. is supported by the Millennium Science Initiative (Chilean Ministry of Economy) through grant RC130007. C.d.B. acknowledges support from the Mexican CONACyT research grant CB-2012-183007.

Embargo Lift Date: 2100-01-01

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External DOI: https://doi.org/10.1051/0004-6361/201629908

This record's URL: https://www.repository.cam.ac.uk/handle/1810/263767



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Autor: Milli, JHibon, PChristiaens, VChoquet,Bonnefoy, M Kennedy, Grant Malcolm Wyatt, Mark CharlesAbsil, OGonzález, CAGDel Burgo, C Mat

Fuente: https://www.repository.cam.ac.uk/handle/1810/263767



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