Direct confirmation of the radial-velocity planet β Pictoris c

M. Nowak; S. Lacour; A. M. Lagrange; P. Rubini; J. Wang; T. Stolker; R. Abuter; A. Amorim; R. Asensio-Torres; M. Bauböck; M. Benisty; J. P. Berger; H. Beust; S. Blunt; A. Boccaletti; M. Bonnefoy; H. Bonnet; W. Brandner; F. Cantalloube; B. Charnay; E. Choquet; V. Christiaens; Y. Clénet; V. Coudé Du Foresto; A. Cridland; P. T. De Zeeuw; R. Dembet; J. Dexter; A. Drescher; G. Duvert; A. Eckart; F. Eisenhauer; F. Gao; P. Garcia; R. Garcia Lopez; T. Gardner; E. Gendron; R. Genzel; S. Gillessen; J. Girard; A. Grandjean; X. Haubois; G. Heißel; T. Henning; S. Hinkley; S. Hippler; M. Horrobin; M. Houllé; Z. Hubert; A. Jiménez-Rosales; L. Jocou; J. Kammerer; P. Kervella; M. Keppler; L. Kreidberg; M. Kulikauskas; V. Lapeyrère; J. B. Le Bouquin; P. Léna; A. Mérand; A. L. Maire; P. Mollière; J. D. Monnier; D. Mouillet; A. Müller; E. Nasedkin; T. Ott; G. Otten; T. Paumard; C. Paladini; K. Perraut; G. Perrin; L. Pueyo; O. Pfuhl; J. Rameau; L. Rodet; G. Rodríguez-Coira; G. Rousset; S. Scheithauer; J. Shangguan; J. Stadler; O. Straub; C. Straubmeier; E. Sturm; L. J. Tacconi; E. F. Van Dishoeck; A. Vigan; F. Vincent; S. D. Von Fellenberg; K. Ward-Duong; F. Widmann; E. Wieprecht; E. Wiezorrek; J. Woillez; The GRAVITY Collaboration

doi:10.1051/0004-6361/202039039

Direct confirmation of the radial-velocity planet β Pictoris c

M. Nowak, S. Lacour, A. M. Lagrange, P. Rubini, J. Wang, T. Stolker, R. Abuter, A. Amorim, R. Asensio-Torres, M. Bauböck, M. Benisty, J. P. Berger, H. Beust, S. Blunt, A. Boccaletti, M. Bonnefoy, H. Bonnet, W. Brandner, F. Cantalloube, B. CharnayE. Choquet, V. Christiaens, Y. Clénet, V. Coudé Du Foresto, A. Cridland, P. T. De Zeeuw, R. Dembet, J. Dexter, A. Drescher, G. Duvert, A. Eckart, F. Eisenhauer, F. Gao, P. Garcia, R. Garcia Lopez, T. Gardner, E. Gendron, R. Genzel, S. Gillessen, J. Girard, A. Grandjean, X. Haubois, G. Heißel, T. Henning, S. Hinkley, S. Hippler, M. Horrobin, M. Houllé, Z. Hubert, A. Jiménez-Rosales, L. Jocou, J. Kammerer, P. Kervella, M. Keppler, L. Kreidberg, M. Kulikauskas, V. Lapeyrère, J. B. Le Bouquin, P. Léna, A. Mérand, A. L. Maire, P. Mollière, J. D. Monnier, D. Mouillet, A. Müller, E. Nasedkin, T. Ott, G. Otten, T. Paumard, C. Paladini, K. Perraut, G. Perrin, L. Pueyo, O. Pfuhl, J. Rameau, L. Rodet, G. Rodríguez-Coira, G. Rousset, S. Scheithauer, J. Shangguan, J. Stadler, O. Straub, C. Straubmeier, E. Sturm, L. J. Tacconi, E. F. Van Dishoeck, A. Vigan, F. Vincent, S. D. Von Fellenberg, K. Ward-Duong, F. Widmann, E. Wieprecht, E. Wiezorrek, J. Woillez, The GRAVITY Collaboration

School of Physics and Astronomy

Research output: Contribution to journal › Article › Research › peer-review

81 Citations (Scopus)

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.

Original language	English
Article number	L2
Number of pages	8
Journal	Astronomy & Astrophysics
Volume	642
Issue number	October 2020
DOIs	https://doi.org/10.1051/0004-6361/202039039
Publication status	Published - 1 Oct 2020

Keywords

Planets and satellites: detection
Planets and satellites: formation
Techniques: interferometric

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10.1051/0004-6361/202039039Licence: CC BY

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Nowak, M., Lacour, S., Lagrange, A. M., Rubini, P., Wang, J., Stolker, T., Abuter, R., Amorim, A., Asensio-Torres, R., Bauböck, M., Benisty, M., Berger, J. P., Beust, H., Blunt, S., Boccaletti, A., Bonnefoy, M., Bonnet, H., Brandner, W., Cantalloube, F., ... The GRAVITY Collaboration (2020). Direct confirmation of the radial-velocity planet β Pictoris c. Astronomy & Astrophysics, 642(October 2020), Article L2. https://doi.org/10.1051/0004-6361/202039039

@article{ae4b4b08e4954a9dbfde8923d713f460,

title = "Direct confirmation of the radial-velocity planet β Pictoris c",

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. ",

keywords = "Planets and satellites: detection, Planets and satellites: formation, Techniques: interferometric",

author = "M. Nowak and S. Lacour and Lagrange, {A. M.} and P. Rubini and J. Wang and T. Stolker and R. Abuter and A. Amorim and R. Asensio-Torres and M. Baub{\"o}ck and M. Benisty and Berger, {J. P.} and H. Beust and S. Blunt and A. Boccaletti and M. Bonnefoy and H. Bonnet and W. Brandner and F. Cantalloube and B. Charnay and E. Choquet and V. Christiaens and Y. Cl{\'e}net and {Coud{\'e} Du Foresto}, V. and A. Cridland and {De Zeeuw}, {P. T.} and R. Dembet and J. Dexter and A. Drescher and G. Duvert and A. Eckart and F. Eisenhauer and F. Gao and P. Garcia and {Garcia Lopez}, R. and T. Gardner and E. Gendron and R. Genzel and S. Gillessen and J. Girard and A. Grandjean and X. Haubois and G. Hei{\ss}el and T. Henning and S. Hinkley and S. Hippler and M. Horrobin and M. Houll{\'e} and Z. Hubert and A. Jim{\'e}nez-Rosales and L. Jocou and J. Kammerer and P. Kervella and M. Keppler and L. Kreidberg and M. Kulikauskas and V. Lapeyr{\`e}re and {Le Bouquin}, {J. B.} and P. L{\'e}na and A. M{\'e}rand and Maire, {A. L.} and P. Molli{\`e}re and Monnier, {J. D.} and D. Mouillet and A. M{\"u}ller and E. Nasedkin and T. Ott and G. Otten and T. Paumard and C. Paladini and K. Perraut and G. Perrin and L. Pueyo and O. Pfuhl and J. Rameau and L. Rodet and G. Rodr{\'i}guez-Coira and G. Rousset and S. Scheithauer and J. Shangguan and J. Stadler and O. Straub and C. Straubmeier and E. Sturm and Tacconi, {L. J.} and {Van Dishoeck}, {E. F.} and A. Vigan and F. Vincent and {Von Fellenberg}, {S. D.} and K. Ward-Duong and F. Widmann and E. Wieprecht and E. Wiezorrek and J. Woillez and {The GRAVITY Collaboration}",

year = "2020",

month = oct,

day = "1",

doi = "10.1051/0004-6361/202039039",

language = "English",

volume = "642",

journal = "Astronomy & Astrophysics",

issn = "0004-6361",

publisher = "EDP Sciences",

number = "October 2020",

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Nowak, M, Lacour, S, Lagrange, AM, Rubini, P, Wang, J, Stolker, T, Abuter, R, Amorim, A, Asensio-Torres, R, Bauböck, M, Benisty, M, Berger, JP, Beust, H, Blunt, S, Boccaletti, A, Bonnefoy, M, Bonnet, H, Brandner, W, Cantalloube, F, Charnay, B, Choquet, E, Christiaens, V, Clénet, Y, Coudé Du Foresto, V, Cridland, A, De Zeeuw, PT, Dembet, R, Dexter, J, Drescher, A, Duvert, G, Eckart, A, Eisenhauer, F, Gao, F, Garcia, P, Garcia Lopez, R, Gardner, T, Gendron, E, Genzel, R, Gillessen, S, Girard, J, Grandjean, A, Haubois, X, Heißel, G, Henning, T, Hinkley, S, Hippler, S, Horrobin, M, Houllé, M, Hubert, Z, Jiménez-Rosales, A, Jocou, L, Kammerer, J, Kervella, P, Keppler, M, Kreidberg, L, Kulikauskas, M, Lapeyrère, V, Le Bouquin, JB, Léna, P, Mérand, A, Maire, AL, Mollière, P, Monnier, JD, Mouillet, D, Müller, A, Nasedkin, E, Ott, T, Otten, G, Paumard, T, Paladini, C, Perraut, K, Perrin, G, Pueyo, L, Pfuhl, O, Rameau, J, Rodet, L, Rodríguez-Coira, G, Rousset, G, Scheithauer, S, Shangguan, J, Stadler, J, Straub, O, Straubmeier, C, Sturm, E, Tacconi, LJ, Van Dishoeck, EF, Vigan, A, Vincent, F, Von Fellenberg, SD, Ward-Duong, K, Widmann, F, Wieprecht, E, Wiezorrek, E, Woillez, J & The GRAVITY Collaboration 2020, 'Direct confirmation of the radial-velocity planet β Pictoris c', Astronomy & Astrophysics, vol. 642, no. October 2020, L2. https://doi.org/10.1051/0004-6361/202039039

TY - JOUR

T1 - Direct confirmation of the radial-velocity planet β Pictoris c

AU - Nowak, M.

AU - Lacour, S.

AU - Lagrange, A. M.

AU - Rubini, P.

AU - Wang, J.

AU - Stolker, T.

AU - Abuter, R.

AU - Amorim, A.

AU - Asensio-Torres, R.

AU - Bauböck, M.

AU - Benisty, M.

AU - Berger, J. P.

AU - Beust, H.

AU - Blunt, S.

AU - Boccaletti, A.

AU - Bonnefoy, M.

AU - Bonnet, H.

AU - Brandner, W.

AU - Cantalloube, F.

AU - Charnay, B.

AU - Choquet, E.

AU - Christiaens, V.

AU - Clénet, Y.

AU - Coudé Du Foresto, V.

AU - Cridland, A.

AU - De Zeeuw, P. T.

AU - Dembet, R.

AU - Dexter, J.

AU - Drescher, A.

AU - Duvert, G.

AU - Eckart, A.

AU - Eisenhauer, F.

AU - Gao, F.

AU - Garcia, P.

AU - Garcia Lopez, R.

AU - Gardner, T.

AU - Gendron, E.

AU - Genzel, R.

AU - Gillessen, S.

AU - Girard, J.

AU - Grandjean, A.

AU - Haubois, X.

AU - Heißel, G.

AU - Henning, T.

AU - Hinkley, S.

AU - Hippler, S.

AU - Horrobin, M.

AU - Houllé, M.

AU - Hubert, Z.

AU - Jiménez-Rosales, A.

AU - Jocou, L.

AU - Kammerer, J.

AU - Kervella, P.

AU - Keppler, M.

AU - Kreidberg, L.

AU - Kulikauskas, M.

AU - Lapeyrère, V.

AU - Le Bouquin, J. B.

AU - Léna, P.

AU - Mérand, A.

AU - Maire, A. L.

AU - Mollière, P.

AU - Monnier, J. D.

AU - Mouillet, D.

AU - Müller, A.

AU - Nasedkin, E.

AU - Ott, T.

AU - Otten, G.

AU - Paumard, T.

AU - Paladini, C.

AU - Perraut, K.

AU - Perrin, G.

AU - Pueyo, L.

AU - Pfuhl, O.

AU - Rameau, J.

AU - Rodet, L.

AU - Rodríguez-Coira, G.

AU - Rousset, G.

AU - Scheithauer, S.

AU - Shangguan, J.

AU - Stadler, J.

AU - Straub, O.

AU - Straubmeier, C.

AU - Sturm, E.

AU - Tacconi, L. J.

AU - Van Dishoeck, E. F.

AU - Vigan, A.

AU - Vincent, F.

AU - Von Fellenberg, S. D.

AU - Ward-Duong, K.

AU - Widmann, F.

AU - Wieprecht, E.

AU - Wiezorrek, E.

AU - Woillez, J.

AU - The GRAVITY Collaboration

PY - 2020/10/1

Y1 - 2020/10/1

N2 - 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.

AB - 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.

KW - Planets and satellites: detection

KW - Planets and satellites: formation

KW - Techniques: interferometric

UR - http://www.scopus.com/inward/record.url?scp=85095113544&partnerID=8YFLogxK

U2 - 10.1051/0004-6361/202039039

DO - 10.1051/0004-6361/202039039

M3 - Article

AN - SCOPUS:85095113544

SN - 0004-6361

VL - 642

JO - Astronomy & Astrophysics

JF - Astronomy & Astrophysics

IS - October 2020

M1 - L2

ER -

Direct confirmation of the radial-velocity planet β Pictoris c

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