The mass of β Pictoris c from β Pictoris b orbital motion

S. Lacour; J. J. Wang; L. Rodet; M. Nowak; J. Shangguan; H. Beust; A. M. Lagrange; R. Abuter; A. Amorim; R. Asensio-Torres; M. Benisty; J. P. Berger; S. Blunt; A. Boccaletti; A. Bohn; M. L. Bolzer; M. Bonnefoy; H. Bonnet; G. Bourdarot; W. Brandner; F. Cantalloube; P. Caselli; B. Charnay; G. Chauvin; E. Choquet; V. Christiaens; Y. Clénet; V. Coudé Du Foresto; A. Cridland; R. Dembet; J. Dexter; P. T. De Zeeuw; A. Drescher; G. Duvert; A. Eckart; F. Eisenhauer; F. Gao; P. Garcia; R. Garcia Lopez; E. Gendron; R. Genzel; S. Gillessen; J. H. Girard; X. Haubois; G. Heißel; Th Henning; S. Hinkley; S. Hippler; M. Horrobin; M. Houllé; Z. Hubert; L. Jocou; J. Kammerer; M. Keppler; P. Kervella; L. Kreidberg; V. Lapeyrère; J. B. Le Bouquin; P. Léna; D. Lutz; A. L. Maire; A. Mérand; P. Mollière; J. D. Monnier; D. Mouillet; E. Nasedkin; T. Ott; G. P.P.L. Otten; C. Paladini; T. Paumard; K. Perraut; G. Perrin; O. Pfuhl; E. Rickman; L. Pueyo; J. Rameau; G. Rousset; Z. Rustamkulov; M. Samland; T. Shimizu; D. Sing; J. Stadler; T. Stolker; 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; S. Yazici; A. Young

doi:10.1051/0004-6361/202141889

The mass of β Pictoris c from β Pictoris b orbital motion

S. Lacour^*, J. J. Wang, L. Rodet, M. Nowak, J. Shangguan, H. Beust, A. M. Lagrange, R. Abuter, A. Amorim, R. Asensio-Torres, M. Benisty, J. P. Berger, S. Blunt, A. Boccaletti, A. Bohn, M. L. Bolzer, M. Bonnefoy, H. Bonnet, G. Bourdarot, W. BrandnerF. Cantalloube, P. Caselli, B. Charnay, G. Chauvin, E. Choquet, V. Christiaens, Y. Clénet, V. Coudé Du Foresto, A. Cridland, R. Dembet, J. Dexter, P. T. De Zeeuw, A. Drescher, G. Duvert, A. Eckart, F. Eisenhauer, F. Gao, P. Garcia, R. Garcia Lopez, E. Gendron, R. Genzel, S. Gillessen, J. H. Girard, X. Haubois, G. Heißel, Th Henning, S. Hinkley, S. Hippler, M. Horrobin, M. Houllé, Z. Hubert, L. Jocou, J. Kammerer, M. Keppler, P. Kervella, L. Kreidberg, V. Lapeyrère, J. B. Le Bouquin, P. Léna, D. Lutz, A. L. Maire, A. Mérand, P. Mollière, J. D. Monnier, D. Mouillet, E. Nasedkin, T. Ott, G. P.P.L. Otten, C. Paladini, T. Paumard, K. Perraut, G. Perrin, O. Pfuhl, E. Rickman, L. Pueyo, J. Rameau, G. Rousset, Z. Rustamkulov, M. Samland, T. Shimizu, D. Sing, J. Stadler, T. Stolker, 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, S. Yazici, A. Young

^*Corresponding author for this work

Physics and Astronomy

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Abstract

Aims. We aim to demonstrate that the presence and mass of an exoplanet can now be effectively derived from the astrometry of another exoplanet. Methods. We combined previous astrometry of β Pictoris b with a new set of observations from the GRAVITY interferometer. The orbital motion of β Pictoris b is fit using Markov chain Monte Carlo simulations in Jacobi coordinates. The inner planet, β Pictoris c, was also reobserved at a separation of 96 mas, confirming the previous orbital estimations. Results. From the astrometry of planet b only, we can (i) detect the presence of β Pictoris c and (ii) constrain its mass to 10.04-3.10+4.53 MJup. If one adds the astrometry of β Pictoris c, the mass is narrowed down to 9.15-1.06+1.08 MJup. The inclusion of radial velocity measurements does not affect the orbital parameters significantly, but it does slightly decrease the mass estimate to 8.89-0.75+0.75 MJup. With a semimajor axis of 2.68 ± 0.02 au, a period of 1221 ± 15 days, and an eccentricity of 0.32 ± 0.02, the orbital parameters of β Pictoris c are now constrained as precisely as those of β Pictoris b. The orbital configuration is compatible with a high-order mean-motion resonance (7:1). The impact of the resonance on the planets' dynamics would then be negligible with respect to the secular perturbations, which might have played an important role in the eccentricity excitation of the outer planet.

Original language	English (US)
Article number	L2
Journal	Astronomy and Astrophysics
Volume	654
DOIs	https://doi.org/10.1051/0004-6361/202141889
State	Published - Oct 1 2021

Funding

Acknowledgements. Letter based on observations collected at the European Organisation for Astronomical Research in the Southern Hemisphere, ID 1104.C-0651. This research has made use of the Jean-Marie Mariotti Center Aspro service (http://www.jmmc.fr/aspro). This research also made use of Astropy (http://www.astropy.org), a community-developed core Python package for Astronomy (Astropy Collaboration 2018). J.J.W. is supported by the Heising-Simons Foundation 51 Pegasi b Fellowship. The development of orbitize! is supported by the Heising-Simons Foundation through grant 2019-1698. We acknowledge support from the European Research Council under the Horizon 2020 Framework Program via the ERC grants 832428 (T.H.) and 757561 (A.V. and G.P.P.O.). A.A. and P.G. were supported by Fundação para a Ciência e a Tecnologia, with grants reference UIDB/00099/2020 and PTDC/FIS-AST/7002/2020.

Keywords

Astrometry
Instrumentation: high angular resolution
Instrumentation: interferometers
Planets and satellites: detection

ASJC Scopus subject areas

Astronomy and Astrophysics
Space and Planetary Science

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10.1051/0004-6361/202141889

Cite this

Lacour, S., Wang, J. J., Rodet, L., Nowak, M., Shangguan, J., Beust, H., Lagrange, A. M., Abuter, R., Amorim, A., Asensio-Torres, R., Benisty, M., Berger, J. P., Blunt, S., Boccaletti, A., Bohn, A., Bolzer, M. L., Bonnefoy, M., Bonnet, H., Bourdarot, G., ... Young, A. (2021). The mass of β Pictoris c from β Pictoris b orbital motion. Astronomy and Astrophysics, 654, Article L2. https://doi.org/10.1051/0004-6361/202141889

@article{342994f347dc47a58525017499707ff9,

title = "The mass of β Pictoris c from β Pictoris b orbital motion",

abstract = "Aims. We aim to demonstrate that the presence and mass of an exoplanet can now be effectively derived from the astrometry of another exoplanet. Methods. We combined previous astrometry of β Pictoris b with a new set of observations from the GRAVITY interferometer. The orbital motion of β Pictoris b is fit using Markov chain Monte Carlo simulations in Jacobi coordinates. The inner planet, β Pictoris c, was also reobserved at a separation of 96 mas, confirming the previous orbital estimations. Results. From the astrometry of planet b only, we can (i) detect the presence of β Pictoris c and (ii) constrain its mass to 10.04-3.10+4.53 MJup. If one adds the astrometry of β Pictoris c, the mass is narrowed down to 9.15-1.06+1.08 MJup. The inclusion of radial velocity measurements does not affect the orbital parameters significantly, but it does slightly decrease the mass estimate to 8.89-0.75+0.75 MJup. With a semimajor axis of 2.68 ± 0.02 au, a period of 1221 ± 15 days, and an eccentricity of 0.32 ± 0.02, the orbital parameters of β Pictoris c are now constrained as precisely as those of β Pictoris b. The orbital configuration is compatible with a high-order mean-motion resonance (7:1). The impact of the resonance on the planets' dynamics would then be negligible with respect to the secular perturbations, which might have played an important role in the eccentricity excitation of the outer planet.",

keywords = "Astrometry, Instrumentation: high angular resolution, Instrumentation: interferometers, Planets and satellites: detection",

author = "S. Lacour and Wang, {J. J.} and L. Rodet and M. Nowak and J. Shangguan and H. Beust and Lagrange, {A. M.} and R. Abuter and A. Amorim and R. Asensio-Torres and M. Benisty and Berger, {J. P.} and S. Blunt and A. Boccaletti and A. Bohn and Bolzer, {M. L.} and M. Bonnefoy and H. Bonnet and G. Bourdarot and W. Brandner and F. Cantalloube and P. Caselli and B. Charnay and G. Chauvin and E. Choquet and V. Christiaens and Y. Cl{\'e}net and {Coud{\'e} Du Foresto}, V. and A. Cridland and R. Dembet and J. Dexter and {De Zeeuw}, {P. T.} and A. Drescher and G. Duvert and A. Eckart and F. Eisenhauer and F. Gao and P. Garcia and {Garcia Lopez}, R. and E. Gendron and R. Genzel and S. Gillessen and Girard, {J. H.} and X. Haubois and G. Hei{\ss}el and Th Henning and S. Hinkley and S. Hippler and M. Horrobin and M. Houll{\'e} and Z. Hubert and L. Jocou and J. Kammerer and M. Keppler and P. Kervella and L. Kreidberg and V. Lapeyr{\`e}re and {Le Bouquin}, {J. B.} and P. L{\'e}na and D. Lutz and Maire, {A. L.} and A. M{\'e}rand and P. Molli{\`e}re and Monnier, {J. D.} and D. Mouillet and E. Nasedkin and T. Ott and Otten, {G. P.P.L.} and C. Paladini and T. Paumard and K. Perraut and G. Perrin and O. Pfuhl and E. Rickman and L. Pueyo and J. Rameau and G. Rousset and Z. Rustamkulov and M. Samland and T. Shimizu and D. Sing and J. Stadler and T. Stolker 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 S. Yazici and A. Young",

note = "Publisher Copyright: {\textcopyright} 2021 S. Lacour et al.",

year = "2021",

month = oct,

day = "1",

doi = "10.1051/0004-6361/202141889",

language = "English (US)",

volume = "654",

journal = "Astronomy and Astrophysics",

issn = "0004-6361",

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Lacour, S, Wang, JJ, Rodet, L, Nowak, M, Shangguan, J, Beust, H, Lagrange, AM, Abuter, R, Amorim, A, Asensio-Torres, R, Benisty, M, Berger, JP, Blunt, S, Boccaletti, A, Bohn, A, Bolzer, ML, Bonnefoy, M, Bonnet, H, Bourdarot, G, Brandner, W, Cantalloube, F, Caselli, P, Charnay, B, Chauvin, G, Choquet, E, Christiaens, V, Clénet, Y, Coudé Du Foresto, V, Cridland, A, Dembet, R, Dexter, J, De Zeeuw, PT, Drescher, A, Duvert, G, Eckart, A, Eisenhauer, F, Gao, F, Garcia, P, Garcia Lopez, R, Gendron, E, Genzel, R, Gillessen, S, Girard, JH, Haubois, X, Heißel, G, Henning, T, Hinkley, S, Hippler, S, Horrobin, M, Houllé, M, Hubert, Z, Jocou, L, Kammerer, J, Keppler, M, Kervella, P, Kreidberg, L, Lapeyrère, V, Le Bouquin, JB, Léna, P, Lutz, D, Maire, AL, Mérand, A, Mollière, P, Monnier, JD, Mouillet, D, Nasedkin, E, Ott, T, Otten, GPPL, Paladini, C, Paumard, T, Perraut, K, Perrin, G, Pfuhl, O, Rickman, E, Pueyo, L, Rameau, J, Rousset, G, Rustamkulov, Z, Samland, M, Shimizu, T, Sing, D, Stadler, J, Stolker, T, 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, Yazici, S & Young, A 2021, 'The mass of β Pictoris c from β Pictoris b orbital motion', Astronomy and Astrophysics, vol. 654, L2. https://doi.org/10.1051/0004-6361/202141889

TY - JOUR

T1 - The mass of β Pictoris c from β Pictoris b orbital motion

AU - Lacour, S.

AU - Wang, J. J.

AU - Rodet, L.

AU - Nowak, M.

AU - Shangguan, J.

AU - Beust, H.

AU - Lagrange, A. M.

AU - Abuter, R.

AU - Amorim, A.

AU - Asensio-Torres, R.

AU - Benisty, M.

AU - Berger, J. P.

AU - Blunt, S.

AU - Boccaletti, A.

AU - Bohn, A.

AU - Bolzer, M. L.

AU - Bonnefoy, M.

AU - Bonnet, H.

AU - Bourdarot, G.

AU - Brandner, W.

AU - Cantalloube, F.

AU - Caselli, P.

AU - Charnay, B.

AU - Chauvin, G.

AU - Choquet, E.

AU - Christiaens, V.

AU - Clénet, Y.

AU - Coudé Du Foresto, V.

AU - Cridland, A.

AU - Dembet, R.

AU - Dexter, J.

AU - De Zeeuw, P. T.

AU - Drescher, A.

AU - Duvert, G.

AU - Eckart, A.

AU - Eisenhauer, F.

AU - Gao, F.

AU - Garcia, P.

AU - Garcia Lopez, R.

AU - Gendron, E.

AU - Genzel, R.

AU - Gillessen, S.

AU - Girard, J. H.

AU - Haubois, X.

AU - Heißel, G.

AU - Henning, Th

AU - Hinkley, S.

AU - Hippler, S.

AU - Horrobin, M.

AU - Houllé, M.

AU - Hubert, Z.

AU - Jocou, L.

AU - Kammerer, J.

AU - Keppler, M.

AU - Kervella, P.

AU - Kreidberg, L.

AU - Lapeyrère, V.

AU - Le Bouquin, J. B.

AU - Léna, P.

AU - Lutz, D.

AU - Maire, A. L.

AU - Mérand, A.

AU - Mollière, P.

AU - Monnier, J. D.

AU - Mouillet, D.

AU - Nasedkin, E.

AU - Ott, T.

AU - Otten, G. P.P.L.

AU - Paladini, C.

AU - Paumard, T.

AU - Perraut, K.

AU - Perrin, G.

AU - Pfuhl, O.

AU - Rickman, E.

AU - Pueyo, L.

AU - Rameau, J.

AU - Rousset, G.

AU - Rustamkulov, Z.

AU - Samland, M.

AU - Shimizu, T.

AU - Sing, D.

AU - Stadler, J.

AU - Stolker, T.

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 - Yazici, S.

AU - Young, A.

PY - 2021/10/1

Y1 - 2021/10/1

N2 - Aims. We aim to demonstrate that the presence and mass of an exoplanet can now be effectively derived from the astrometry of another exoplanet. Methods. We combined previous astrometry of β Pictoris b with a new set of observations from the GRAVITY interferometer. The orbital motion of β Pictoris b is fit using Markov chain Monte Carlo simulations in Jacobi coordinates. The inner planet, β Pictoris c, was also reobserved at a separation of 96 mas, confirming the previous orbital estimations. Results. From the astrometry of planet b only, we can (i) detect the presence of β Pictoris c and (ii) constrain its mass to 10.04-3.10+4.53 MJup. If one adds the astrometry of β Pictoris c, the mass is narrowed down to 9.15-1.06+1.08 MJup. The inclusion of radial velocity measurements does not affect the orbital parameters significantly, but it does slightly decrease the mass estimate to 8.89-0.75+0.75 MJup. With a semimajor axis of 2.68 ± 0.02 au, a period of 1221 ± 15 days, and an eccentricity of 0.32 ± 0.02, the orbital parameters of β Pictoris c are now constrained as precisely as those of β Pictoris b. The orbital configuration is compatible with a high-order mean-motion resonance (7:1). The impact of the resonance on the planets' dynamics would then be negligible with respect to the secular perturbations, which might have played an important role in the eccentricity excitation of the outer planet.

AB - Aims. We aim to demonstrate that the presence and mass of an exoplanet can now be effectively derived from the astrometry of another exoplanet. Methods. We combined previous astrometry of β Pictoris b with a new set of observations from the GRAVITY interferometer. The orbital motion of β Pictoris b is fit using Markov chain Monte Carlo simulations in Jacobi coordinates. The inner planet, β Pictoris c, was also reobserved at a separation of 96 mas, confirming the previous orbital estimations. Results. From the astrometry of planet b only, we can (i) detect the presence of β Pictoris c and (ii) constrain its mass to 10.04-3.10+4.53 MJup. If one adds the astrometry of β Pictoris c, the mass is narrowed down to 9.15-1.06+1.08 MJup. The inclusion of radial velocity measurements does not affect the orbital parameters significantly, but it does slightly decrease the mass estimate to 8.89-0.75+0.75 MJup. With a semimajor axis of 2.68 ± 0.02 au, a period of 1221 ± 15 days, and an eccentricity of 0.32 ± 0.02, the orbital parameters of β Pictoris c are now constrained as precisely as those of β Pictoris b. The orbital configuration is compatible with a high-order mean-motion resonance (7:1). The impact of the resonance on the planets' dynamics would then be negligible with respect to the secular perturbations, which might have played an important role in the eccentricity excitation of the outer planet.

KW - Astrometry

KW - Instrumentation: high angular resolution

KW - Instrumentation: interferometers

KW - Planets and satellites: detection

UR - http://www.scopus.com/inward/record.url?scp=85117070383&partnerID=8YFLogxK

UR - http://www.scopus.com/inward/citedby.url?scp=85117070383&partnerID=8YFLogxK

U2 - 10.1051/0004-6361/202141889

DO - 10.1051/0004-6361/202141889

M3 - Article

AN - SCOPUS:85117070383

SN - 0004-6361

VL - 654

JO - Astronomy and Astrophysics

JF - Astronomy and Astrophysics

M1 - L2

ER -

The mass of β Pictoris c from β Pictoris b orbital motion

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