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Discovery of a Companion Candidate in the HD 169142 Transition Disk and the Possibility of Multiple Planet Formation

Reggiani, Maddalena and Quanz, Sascha P. and Meyer, Michael R. and Pueyo, Laurent and Absil, Olivier and Amara, Adam and Anglada, Guillem and Avenhaus, Henning and Girard, Julien and Carrasco Gonzalez, Carlos and Graham, James and Mawet, Dimitri and Meru, Farzan and Milli, Julien and Osorio, Mayra and Wolff, Schuyler and Torrelles, Jose-Maria (2014) Discovery of a Companion Candidate in the HD 169142 Transition Disk and the Possibility of Multiple Planet Formation. Astrophysical Journal Letters, 792 (1). Art. No. L23. ISSN 2041-8205. doi:10.1088/2041-8205/792/1/L23.

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We present L'- and J-band high-contrast observations of HD 169142, obtained with the Very Large Telescope/NACO AGPM vector vortex coronagraph and the Gemini Planet Imager, respectively. A source located at 0."156 ± 0.''032 north of the host star (P.A. = 7°.4 ± 11°.3) appears in the final reduced L' image. At the distance of the star (~145 pc), this angular separation corresponds to a physical separation of 22.7 ± 4.7 AU, locating the source within the recently resolved inner cavity of the transition disk. The source has a brightness of L' = 12.2 ± 0.5 mag, whereas it is not detected in the J band (J >13.8 mag). If its L' brightness arose solely from the photosphere of a companion and given the J – L' color constraints, it would correspond to a 28-32 M Jupiter object at the age of the star, according to the COND models. Ongoing accretion activity of the star suggests, however, that gas is left in the inner disk cavity from which the companion could also be accreting. In this case, the object could be lower in mass and its luminosity enhanced by the accretion process and by a circumplanetary disk. A lower-mass object is more consistent with the observed cavity width. Finally, the observations enable us to place an upper limit on the L'-band flux of a second companion candidate orbiting in the disk annular gap at ~50 AU, as suggested by millimeter observations. If the second companion is also confirmed, HD 169142 might be forming a planetary system, with at least two companions opening gaps and possibly interacting with each other.

Item Type:Article
Related URLs:
URLURL TypeDescription Paper
Reggiani, Maddalena0000-0003-2911-0898
Quanz, Sascha P.0000-0003-3829-7412
Meyer, Michael R.0000-0003-1227-3084
Pueyo, Laurent0000-0003-3818-408X
Absil, Olivier0000-0002-4006-6237
Girard, Julien0000-0001-8627-0404
Mawet, Dimitri0000-0002-8895-4735
Milli, Julien0000-0001-9325-2511
Additional Information:© 2014 American Astronomical Society. Received 2013 November 19; accepted 2014 July 29; published 2014 August 20. Based on observations obtained at the Gemini Observatory, operated by the Association of Universities for Research in Astronomy, Inc., under a cooperative agreement with the NSF on behalf of the Gemini partnership: NSF (United States), the National Research Council (Canada), CONICYT (Chile), the Australian Research Council (Australia), Ministério da Ciência, Tecnologia e Inovação (Brazil) and Ministerio de Ciencia, Tecnología e Innovación Productiva (Argentina). We thank Bruce Macintosh and the GPI team for support during the observations. G.A., C.C.-G., M.O., and J.M.T. acknowledge support from MINECO (Spain) AYA2011-30228-C03 grant. Facility: VLT:Yepun (NACO) - Very Large Telescope (Yepun)
Funding AgencyGrant Number
Ministerio de Economía y Competitividad (MINECO)AYA2011-30228-C03
Subject Keywords:brown dwarfs; planet-disk interactions; planets and satellites: formation; protoplanetary disks; stars: individual (HD 169142); stars: low-mass
Issue or Number:1
Record Number:CaltechAUTHORS:20150526-162651428
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Official Citation:Discovery of a Companion Candidate in the HD 169142 Transition Disk and the Possibility of Multiple Planet Formation Maddalena Reggiani et al. 2014 ApJ 792 L23
Usage Policy:No commercial reproduction, distribution, display or performance rights in this work are provided.
ID Code:57835
Deposited On:27 May 2015 23:20
Last Modified:10 Nov 2021 21:55

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