Characterization of the gaseous companion κ Andromedae b: New Keck and LBTI high-contrast observations

M. Bonnefoy; T. Currie; G. D. Marleau; J. E. Schlieder; J. Wisniewski; J. Carson; K. R. Covey; T. Henning; B. Biller; P. Hinz; H. Klahr; A. N. Marsh Boyer; N. Zimmerman; M. Janson; M. McElwain; C. Mordasini; A. Skemer; V. Bailey; D. Defrère; C. Thalmann; M. Skrutskie; F. Allard; D. Homeier; M. Tamura; M. Feldt; A. Cumming; C. Grady; W. Brandner; C. Helling; S. Witte; P. Hauschildt; R. Kandori; M. Kuzuhara; M. Fukagawa; J. Kwon; T. Kudo; J. Hashimoto; N. Kusakabe; L. Abe; T. Brandt; S. Egner; O. Guyon; Y. Hayano; M. Hayashi; S. Hayashi; K. Hodapp; M. Ishii; M. Iye; G. Knapp; T. Matsuo; K. Mede; M. Miyama; J. I. Morino; A. Moro-Martin; T. Nishimura; T. Pyo; E. Serabyn; T. Suenaga; H. Suto; R. Suzuki; T. Takahashi; M. Takami; N. Takato; H. Terada; D. Tomono; E. Turner; M. Watanabe; T. Yamada; H. Takami; T. Usuda

doi:10.1051/0004-6361/201322119

Characterization of the gaseous companion κ Andromedae b: New Keck and LBTI high-contrast observations

M. Bonnefoy, T. Currie, G. D. Marleau, J. E. Schlieder, J. Wisniewski, J. Carson, K. R. Covey, T. Henning, B. Biller, P. Hinz, H. Klahr, A. N. Marsh Boyer, N. Zimmerman, M. Janson, M. McElwain, C. Mordasini, A. Skemer, V. Bailey, D. Defrère, C. ThalmannM. Skrutskie, F. Allard, D. Homeier, M. Tamura, M. Feldt, A. Cumming, C. Grady, W. Brandner, C. Helling, S. Witte, P. Hauschildt, R. Kandori, M. Kuzuhara, M. Fukagawa, J. Kwon, T. Kudo, J. Hashimoto, N. Kusakabe, L. Abe, T. Brandt, S. Egner, O. Guyon, Y. Hayano, M. Hayashi, S. Hayashi, K. Hodapp, M. Ishii, M. Iye, G. Knapp, T. Matsuo, K. Mede, M. Miyama, J. I. Morino, A. Moro-Martin, T. Nishimura, T. Pyo, E. Serabyn, T. Suenaga, H. Suto, R. Suzuki, T. Takahashi, M. Takami, N. Takato, H. Terada, D. Tomono, E. Turner, M. Watanabe, T. Yamada, H. Takami, T. Usuda

Astrophysical Sciences

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Abstract

Context. We previously reported the direct detection of a low-mass companion at a projected separation of 55 ± 2 AU around the B9-type star κ Andromedae. The properties of the system (mass ratio, separation) make it a benchmark for understanding the formation and evolution of gas giant planets and brown dwarfs on wide orbits. Aims. We present new angular differential imaging (ADI) images of the system at 2.146 (K_s), 3.776 (L0), 4.052 (NB-4:05), and 4.78 μm (M') obtained with Keck/NIRC2 and LBTI/LMIRCam, as well as more accurate near-infrared photometry of the star with the MIMIR instrument. We aim to determine the near-infrared spectral energy distribution of the companion and use it to characterize the object. Methods. We used analysis methods adapted to ADI to extract the companion flux. We compared the photometry of the object to reference young, and old objects and to a set of seven PHOENIX-based atmospheric models of cool objects accounting for the formation of dust. We used evolutionary models to derive mass estimates considering a wide range of plausible initial conditions. Finally, we used dedicated formation models to discuss the possible origin of the companion. Results. We derive a more accurate J = 15:86 ± 0:21, H = 14:95 ± 0:13, K_s = 14:32 ± 0:09 mag for κ And b. We detect the companion in all our high-contrast observations.We confirm previous contrasts obtained at Ks and L0 band. We derive NB-4:05 = 13:0 ± 0:2, and M' = 13:3 ± 0:3 mag and estimate log10(L=L) = -3:76 ± 0:06. Atmospheric models yield Teff = 1900+100 -200 K. They do not set any constraint on the surface gravity. "Hotstart" evolutionary models predict masses of 14⁺²⁵_-2 MJup based on the luminosity and temperature estimates, and when considering a conservative age range for the system (30 ⁺¹²⁰_-10 Myr), "warm-start" evolutionary tracks constrain the mass to M ≥ 10 M_Jup. Conclusions. The mass of κ Andromedae b mostly falls in the brown-dwarf regime, owing to remaining uncertainties in age and in mass-luminosity models. According to the formation models, disk instability in a primordial disk may account for the position and a wide range of plausible masses of κ And b.

Original language	English (US)
Article number	A111
Journal	Astronomy and Astrophysics
Volume	562
DOIs	https://doi.org/10.1051/0004-6361/201322119
State	Published - Feb 2014

All Science Journal Classification (ASJC) codes

Astronomy and Astrophysics
Space and Planetary Science

Keywords

Instrumentation: adaptive optics
Planetary systems
Stars: individual: kappa Andromedae
Techniques: photometric

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10.1051/0004-6361/201322119

Cite this

Bonnefoy, M., Currie, T., Marleau, G. D., Schlieder, J. E., Wisniewski, J., Carson, J., Covey, K. R., Henning, T., Biller, B., Hinz, P., Klahr, H., Marsh Boyer, A. N., Zimmerman, N., Janson, M., McElwain, M., Mordasini, C., Skemer, A., Bailey, V., Defrère, D., ... Usuda, T. (2014). Characterization of the gaseous companion κ Andromedae b: New Keck and LBTI high-contrast observations. Astronomy and Astrophysics, 562, Article A111. https://doi.org/10.1051/0004-6361/201322119

@article{4ffe4089e22d4c7c9ced203177cf6a83,

title = "Characterization of the gaseous companion κ Andromedae b: New Keck and LBTI high-contrast observations",

abstract = "Context. We previously reported the direct detection of a low-mass companion at a projected separation of 55 ± 2 AU around the B9-type star κ Andromedae. The properties of the system (mass ratio, separation) make it a benchmark for understanding the formation and evolution of gas giant planets and brown dwarfs on wide orbits. Aims. We present new angular differential imaging (ADI) images of the system at 2.146 (Ks), 3.776 (L0), 4.052 (NB-4:05), and 4.78 μm (M') obtained with Keck/NIRC2 and LBTI/LMIRCam, as well as more accurate near-infrared photometry of the star with the MIMIR instrument. We aim to determine the near-infrared spectral energy distribution of the companion and use it to characterize the object. Methods. We used analysis methods adapted to ADI to extract the companion flux. We compared the photometry of the object to reference young, and old objects and to a set of seven PHOENIX-based atmospheric models of cool objects accounting for the formation of dust. We used evolutionary models to derive mass estimates considering a wide range of plausible initial conditions. Finally, we used dedicated formation models to discuss the possible origin of the companion. Results. We derive a more accurate J = 15:86 ± 0:21, H = 14:95 ± 0:13, Ks = 14:32 ± 0:09 mag for κ And b. We detect the companion in all our high-contrast observations.We confirm previous contrasts obtained at Ks and L0 band. We derive NB-4:05 = 13:0 ± 0:2, and M' = 13:3 ± 0:3 mag and estimate log10(L=L) = -3:76 ± 0:06. Atmospheric models yield Teff = 1900+100 -200 K. They do not set any constraint on the surface gravity. {"}Hotstart{"} evolutionary models predict masses of 14+25-2 MJup based on the luminosity and temperature estimates, and when considering a conservative age range for the system (30 +120-10 Myr), {"}warm-start{"} evolutionary tracks constrain the mass to M ≥ 10 MJup. Conclusions. The mass of κ Andromedae b mostly falls in the brown-dwarf regime, owing to remaining uncertainties in age and in mass-luminosity models. According to the formation models, disk instability in a primordial disk may account for the position and a wide range of plausible masses of κ And b.",

keywords = "Instrumentation: adaptive optics, Planetary systems, Stars: individual: kappa Andromedae, Techniques: photometric",

author = "M. Bonnefoy and T. Currie and Marleau, {G. D.} and Schlieder, {J. E.} and J. Wisniewski and J. Carson and Covey, {K. R.} and T. Henning and B. Biller and P. Hinz and H. Klahr and {Marsh Boyer}, {A. N.} and N. Zimmerman and M. Janson and M. McElwain and C. Mordasini and A. Skemer and V. Bailey and D. Defr{\`e}re and C. Thalmann and M. Skrutskie and F. Allard and D. Homeier and M. Tamura and M. Feldt and A. Cumming and C. Grady and W. Brandner and C. Helling and S. Witte and P. Hauschildt and R. Kandori and M. Kuzuhara and M. Fukagawa and J. Kwon and T. Kudo and J. Hashimoto and N. Kusakabe and L. Abe and T. Brandt and S. Egner and O. Guyon and Y. Hayano and M. Hayashi and S. Hayashi and K. Hodapp and M. Ishii and M. Iye and G. Knapp and T. Matsuo and K. Mede and M. Miyama and Morino, {J. I.} and A. Moro-Martin and T. Nishimura and T. Pyo and E. Serabyn and T. Suenaga and H. Suto and R. Suzuki and T. Takahashi and M. Takami and N. Takato and H. Terada and D. Tomono and E. Turner and M. Watanabe and T. Yamada and H. Takami and T. Usuda",

note = "Funding Information: We are very grateful to our anonymous referee for reviewing this article. We thank the LMIRCam instrument team for operating the instrument during our observations. The authors recognize and acknowledge the significant cultural role and reverence that the summit of Mauna Kea has always had within the indigenous Hawaiian community. We thank Ginny McSwain for her complementary analysis of the high-resolution spectrum of And A. We thank Anne-Marie Lagrange for checking for past SOPHIE observations of And A, Julien Rameau for providing the detection limit on HR 7329B, Eric Nielsen and Michael Liu for discussion about their bayesian age-dating tool. We also thank Johan Olofsson for checking the spectral energy distribution of the star. This research was conducted in part using the MIMIR instrument, jointly developed at Boston University and Lowell Observatory and supported by NASA, NSF, and the W.M. Keck Foundation. J. Carson, J. Wisniewski, and C. Grady were supported by NSF awards 1009314, 1009203, and 1008440. Andrew Skemer was supported by the NASA Origins of Solar Systems Program, grant NNX13AJ17G. J. Kwon is supported by the JSPS Research Fellowships for Young Scientists (PD: 24 110). The research leading to these results has received funding from the French “Agence Nationale de la Recherche” through project grant ANR10-BLANC0504-01, the “Programme National de Physique Stellaire” (PNPS) of CNRS (INSU), and the European Research Council under the European Community{\textquoteright}s Seventh Framework Programs (FP7/2007-2013 Grant Agreement no. 247060). It was also conducted within the Lyon Institute of Origins under grant ANR-10-LABX-66.",

year = "2014",

month = feb,

doi = "10.1051/0004-6361/201322119",

language = "English (US)",

volume = "562",

journal = "Astronomy and Astrophysics",

issn = "0004-6361",

publisher = "EDP Sciences",

}

Bonnefoy, M, Currie, T, Marleau, GD, Schlieder, JE, Wisniewski, J, Carson, J, Covey, KR, Henning, T, Biller, B, Hinz, P, Klahr, H, Marsh Boyer, AN, Zimmerman, N, Janson, M, McElwain, M, Mordasini, C, Skemer, A, Bailey, V, Defrère, D, Thalmann, C, Skrutskie, M, Allard, F, Homeier, D, Tamura, M, Feldt, M, Cumming, A, Grady, C, Brandner, W, Helling, C, Witte, S, Hauschildt, P, Kandori, R, Kuzuhara, M, Fukagawa, M, Kwon, J, Kudo, T, Hashimoto, J, Kusakabe, N, Abe, L, Brandt, T, Egner, S, Guyon, O, Hayano, Y, Hayashi, M, Hayashi, S, Hodapp, K, Ishii, M, Iye, M, Knapp, G, Matsuo, T, Mede, K, Miyama, M, Morino, JI, Moro-Martin, A, Nishimura, T, Pyo, T, Serabyn, E, Suenaga, T, Suto, H, Suzuki, R, Takahashi, T, Takami, M, Takato, N, Terada, H, Tomono, D, Turner, E, Watanabe, M, Yamada, T, Takami, H & Usuda, T 2014, 'Characterization of the gaseous companion κ Andromedae b: New Keck and LBTI high-contrast observations', Astronomy and Astrophysics, vol. 562, A111. https://doi.org/10.1051/0004-6361/201322119

TY - JOUR

T1 - Characterization of the gaseous companion κ Andromedae b

T2 - New Keck and LBTI high-contrast observations

AU - Bonnefoy, M.

AU - Currie, T.

AU - Marleau, G. D.

AU - Schlieder, J. E.

AU - Wisniewski, J.

AU - Carson, J.

AU - Covey, K. R.

AU - Henning, T.

AU - Biller, B.

AU - Hinz, P.

AU - Klahr, H.

AU - Marsh Boyer, A. N.

AU - Zimmerman, N.

AU - Janson, M.

AU - McElwain, M.

AU - Mordasini, C.

AU - Skemer, A.

AU - Bailey, V.

AU - Defrère, D.

AU - Thalmann, C.

AU - Skrutskie, M.

AU - Allard, F.

AU - Homeier, D.

AU - Tamura, M.

AU - Feldt, M.

AU - Cumming, A.

AU - Grady, C.

AU - Brandner, W.

AU - Helling, C.

AU - Witte, S.

AU - Hauschildt, P.

AU - Kandori, R.

AU - Kuzuhara, M.

AU - Fukagawa, M.

AU - Kwon, J.

AU - Kudo, T.

AU - Hashimoto, J.

AU - Kusakabe, N.

AU - Abe, L.

AU - Brandt, T.

AU - Egner, S.

AU - Guyon, O.

AU - Hayano, Y.

AU - Hayashi, M.

AU - Hayashi, S.

AU - Hodapp, K.

AU - Ishii, M.

AU - Iye, M.

AU - Knapp, G.

AU - Matsuo, T.

AU - Mede, K.

AU - Miyama, M.

AU - Morino, J. I.

AU - Moro-Martin, A.

AU - Nishimura, T.

AU - Pyo, T.

AU - Serabyn, E.

AU - Suenaga, T.

AU - Suto, H.

AU - Suzuki, R.

AU - Takahashi, T.

AU - Takami, M.

AU - Takato, N.

AU - Terada, H.

AU - Tomono, D.

AU - Turner, E.

AU - Watanabe, M.

AU - Yamada, T.

AU - Takami, H.

AU - Usuda, T.

N1 - Funding Information: We are very grateful to our anonymous referee for reviewing this article. We thank the LMIRCam instrument team for operating the instrument during our observations. The authors recognize and acknowledge the significant cultural role and reverence that the summit of Mauna Kea has always had within the indigenous Hawaiian community. We thank Ginny McSwain for her complementary analysis of the high-resolution spectrum of And A. We thank Anne-Marie Lagrange for checking for past SOPHIE observations of And A, Julien Rameau for providing the detection limit on HR 7329B, Eric Nielsen and Michael Liu for discussion about their bayesian age-dating tool. We also thank Johan Olofsson for checking the spectral energy distribution of the star. This research was conducted in part using the MIMIR instrument, jointly developed at Boston University and Lowell Observatory and supported by NASA, NSF, and the W.M. Keck Foundation. J. Carson, J. Wisniewski, and C. Grady were supported by NSF awards 1009314, 1009203, and 1008440. Andrew Skemer was supported by the NASA Origins of Solar Systems Program, grant NNX13AJ17G. J. Kwon is supported by the JSPS Research Fellowships for Young Scientists (PD: 24 110). The research leading to these results has received funding from the French “Agence Nationale de la Recherche” through project grant ANR10-BLANC0504-01, the “Programme National de Physique Stellaire” (PNPS) of CNRS (INSU), and the European Research Council under the European Community’s Seventh Framework Programs (FP7/2007-2013 Grant Agreement no. 247060). It was also conducted within the Lyon Institute of Origins under grant ANR-10-LABX-66.

PY - 2014/2

Y1 - 2014/2

N2 - Context. We previously reported the direct detection of a low-mass companion at a projected separation of 55 ± 2 AU around the B9-type star κ Andromedae. The properties of the system (mass ratio, separation) make it a benchmark for understanding the formation and evolution of gas giant planets and brown dwarfs on wide orbits. Aims. We present new angular differential imaging (ADI) images of the system at 2.146 (Ks), 3.776 (L0), 4.052 (NB-4:05), and 4.78 μm (M') obtained with Keck/NIRC2 and LBTI/LMIRCam, as well as more accurate near-infrared photometry of the star with the MIMIR instrument. We aim to determine the near-infrared spectral energy distribution of the companion and use it to characterize the object. Methods. We used analysis methods adapted to ADI to extract the companion flux. We compared the photometry of the object to reference young, and old objects and to a set of seven PHOENIX-based atmospheric models of cool objects accounting for the formation of dust. We used evolutionary models to derive mass estimates considering a wide range of plausible initial conditions. Finally, we used dedicated formation models to discuss the possible origin of the companion. Results. We derive a more accurate J = 15:86 ± 0:21, H = 14:95 ± 0:13, Ks = 14:32 ± 0:09 mag for κ And b. We detect the companion in all our high-contrast observations.We confirm previous contrasts obtained at Ks and L0 band. We derive NB-4:05 = 13:0 ± 0:2, and M' = 13:3 ± 0:3 mag and estimate log10(L=L) = -3:76 ± 0:06. Atmospheric models yield Teff = 1900+100 -200 K. They do not set any constraint on the surface gravity. "Hotstart" evolutionary models predict masses of 14+25-2 MJup based on the luminosity and temperature estimates, and when considering a conservative age range for the system (30 +120-10 Myr), "warm-start" evolutionary tracks constrain the mass to M ≥ 10 MJup. Conclusions. The mass of κ Andromedae b mostly falls in the brown-dwarf regime, owing to remaining uncertainties in age and in mass-luminosity models. According to the formation models, disk instability in a primordial disk may account for the position and a wide range of plausible masses of κ And b.

AB - Context. We previously reported the direct detection of a low-mass companion at a projected separation of 55 ± 2 AU around the B9-type star κ Andromedae. The properties of the system (mass ratio, separation) make it a benchmark for understanding the formation and evolution of gas giant planets and brown dwarfs on wide orbits. Aims. We present new angular differential imaging (ADI) images of the system at 2.146 (Ks), 3.776 (L0), 4.052 (NB-4:05), and 4.78 μm (M') obtained with Keck/NIRC2 and LBTI/LMIRCam, as well as more accurate near-infrared photometry of the star with the MIMIR instrument. We aim to determine the near-infrared spectral energy distribution of the companion and use it to characterize the object. Methods. We used analysis methods adapted to ADI to extract the companion flux. We compared the photometry of the object to reference young, and old objects and to a set of seven PHOENIX-based atmospheric models of cool objects accounting for the formation of dust. We used evolutionary models to derive mass estimates considering a wide range of plausible initial conditions. Finally, we used dedicated formation models to discuss the possible origin of the companion. Results. We derive a more accurate J = 15:86 ± 0:21, H = 14:95 ± 0:13, Ks = 14:32 ± 0:09 mag for κ And b. We detect the companion in all our high-contrast observations.We confirm previous contrasts obtained at Ks and L0 band. We derive NB-4:05 = 13:0 ± 0:2, and M' = 13:3 ± 0:3 mag and estimate log10(L=L) = -3:76 ± 0:06. Atmospheric models yield Teff = 1900+100 -200 K. They do not set any constraint on the surface gravity. "Hotstart" evolutionary models predict masses of 14+25-2 MJup based on the luminosity and temperature estimates, and when considering a conservative age range for the system (30 +120-10 Myr), "warm-start" evolutionary tracks constrain the mass to M ≥ 10 MJup. Conclusions. The mass of κ Andromedae b mostly falls in the brown-dwarf regime, owing to remaining uncertainties in age and in mass-luminosity models. According to the formation models, disk instability in a primordial disk may account for the position and a wide range of plausible masses of κ And b.

KW - Instrumentation: adaptive optics

KW - Planetary systems

KW - Stars: individual: kappa Andromedae

KW - Techniques: photometric

UR - http://www.scopus.com/inward/record.url?scp=84894307804&partnerID=8YFLogxK

UR - http://www.scopus.com/inward/citedby.url?scp=84894307804&partnerID=8YFLogxK

U2 - 10.1051/0004-6361/201322119

DO - 10.1051/0004-6361/201322119

M3 - Article

AN - SCOPUS:84894307804

SN - 0004-6361

VL - 562

JO - Astronomy and Astrophysics

JF - Astronomy and Astrophysics

M1 - A111

ER -

Characterization of the gaseous companion κ Andromedae b: New Keck and LBTI high-contrast observations

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