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  Direct confirmation of the radial-velocity planet β Pictoris c

Nowak, M., Lacour, S., Lagrange, A.-M., Rubini, P., Wang, J., Stolker, T., et al. (2020). Direct confirmation of the radial-velocity planet β Pictoris c. Astronomy and Astrophysics, 642: L2. doi:10.1051/0004-6361/202039039.

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Item Permalink: http://hdl.handle.net/21.11116/0000-0007-8BA3-4 Version Permalink: http://hdl.handle.net/21.11116/0000-0007-8BA4-3
Genre: Journal Article

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Nowak, M., Author
Lacour, S., Author
Lagrange, A.-M., Author
Rubini, P., Author
Wang, J., Author
Stolker, T., Author
Abuter, R., Author
Amorim, A., Author
Asensio-Torres, R., Author
Bauböck, M.1, Author              
Benisty, M., Author
Berger, J. P., Author
Beust, H., Author
Blunt, S., Author
Boccaletti, A., Author
Bonnefoy, M., Author
Bonnet, H., Author
Brandner, W., Author
Cantalloube, F., Author
Charnay, B., Author
Choquet, E., AuthorChristiaens, V., AuthorClénet, Y., Authordu Foresto, V. Coudé, AuthorCridland, A., Authorde Zeeuw, P. T.1, Author              Dembet, R., AuthorDexter, J.1, Author              Drescher, A.1, Author              Duvert, G., AuthorEckart, A., AuthorEisenhauer, F.1, Author              Gao, F.1, Author              Garcia, P., AuthorLopez, R. Garcia, AuthorGardner, T., AuthorGendron, E., AuthorGenzel, R.1, Author              Gillessen, S.1, Author              Girard, J., AuthorGrandjean, A., AuthorHaubois, X., AuthorHeißel, G., AuthorHenning, T., AuthorHinkley, S., AuthorHippler, S., AuthorHorrobin, M., AuthorHoullé, M., AuthorHubert, Z., AuthorJiménez-Rosales, A.1, Author              Jocou, L., AuthorKammerer, J., AuthorKervella, P., AuthorKeppler, M., AuthorKreidberg, L., AuthorKulikauskas, M., AuthorLapeyrère, V., AuthorLe Bouquin, J.-B., AuthorLéna, P., AuthorMérand, A., AuthorMaire, A.-L., AuthorMollière, P., AuthorMonnier, J. D., AuthorMouillet, D., AuthorMüller, A., AuthorNasedkin, E., AuthorOtt, T.1, Author              Otten, G., AuthorPaumard, T., AuthorPaladini, C., AuthorPerraut, K., AuthorPerrin, G., AuthorPueyo, L., AuthorPfuhl, O., AuthorRameau, J., AuthorRodet, L., AuthorRodríguez-Coira, G., AuthorRousset, G., AuthorScheithauer, S., AuthorShangguan, J.1, Author              Stadler, J.1, Author              Straub, O.1, Author              Straubmeier, C., AuthorSturm, E.1, Author              Tacconi, L. J.1, Author              Dishoeck, E. F. van1, Author              Vigan, A., AuthorVincent, F., AuthorFellenberg, S. D. von1, Author              Ward-Duong, K., AuthorWidmann, F.1, Author              Wieprecht, E.1, Author              Wiezorrek, E.1, Author              Woillez, J., Authorthe GRAVITY Collaboration, Author more..
Affiliations:
1Infrared and Submillimeter Astronomy, MPI for Extraterrestrial Physics, Max Planck Society, ou_159889              

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 Abstract: Context. Methods used to detect giant exoplanets can be broadly divided into two categories: indirect and direct. Indirect methods are more sensitive to planets with a small orbital period, whereas direct detection is more sensitive to planets orbiting at a large distance from their host star. This dichotomy makes it difficult to combine the two techniques on a single target at once. Aims. Simultaneous measurements made by direct and indirect techniques offer the possibility of determining the mass and luminosity of planets and a method of testing formation models. Here, we aim to show how long-baseline interferometric observations guided by radial-velocity can be used in such a way. Methods. We observed the recently-discovered giant planet β Pictoris c with GRAVITY, mounted on the Very Large Telescope Interferometer. Results. This study constitutes the first direct confirmation of a planet discovered through radial velocity. We find that the planet has a temperature of T = 1250 ± 50 K and a dynamical mass of M = 8.2 ± 0.8 MJup. At 18.5 ± 2.5 Myr, this puts β Pic c close to a ‘hot start’ track, which is usually associated with formation via disk instability. Conversely, the planet orbits at a distance of 2.7 au, which is too close for disk instability to occur. The low apparent magnitude (MK = 14.3 ± 0.1) favours a core accretion scenario. Conclusions. We suggest that this apparent contradiction is a sign of hot core accretion, for example, due to the mass of the planetary core or the existence of a high-temperature accretion shock during formation.

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Language(s): eng - English
 Dates: 2020-10-02
 Publication Status: Published online
 Pages: -
 Publishing info: -
 Table of Contents: -
 Rev. Type: -
 Identifiers: DOI: 10.1051/0004-6361/202039039
Other: LOCALID: 3270725
 Degree: -

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Title: Astronomy and Astrophysics
  Other : Astron. Astrophys.
Source Genre: Journal
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Publ. Info: France : EDP Sciences S A
Pages: - Volume / Issue: 642 Sequence Number: L2 Start / End Page: - Identifier: ISSN: 1432-0746
CoNE: https://pure.mpg.de/cone/journals/resource/954922828219_1