Establishing the accuracy of asteroseismic mass and radius estimates of giant stars: III. KIC 4054905, an eclipsing binary with two 10 Gyr thick disk RGB stars

K. Brogaard; T. Arentoft; D. Slumstrup; F. Grundahl; M. N. Lund; L. Arndt; S. Grund; J. Rudrasingam; A. Theil; K. Christensen; M. Sejersen; F. Vorgod; L. Salmonsen; L. Ã Rtoft Endelt; S. Dainese; S. Frandsen; A. Miglio; J. Tayar; D. Huber

doi:10.1051/0004-6361/202244345

Establishing the accuracy of asteroseismic mass and radius estimates of giant stars: III. KIC 4054905, an eclipsing binary with two 10 Gyr thick disk RGB stars

K. Brogaard, T. Arentoft, D. Slumstrup, F. Grundahl, M. N. Lund, L. Arndt, S. Grund, J. Rudrasingam, A. Theil, K. Christensen, M. Sejersen, F. Vorgod, L. Salmonsen, L. Ã Rtoft Endelt, S. Dainese, S. Frandsen, A. Miglio, J. Tayar, D. Huber

Physics and Astronomy

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Abstract

Context. Eclipsing binary stars with an oscillating giant component allow accurate stellar parameters to be derived and asteroseismic methods to be tested and calibrated. To this aim, suitable systems need to be firstly identified and secondly measured precisely and accurately. KIC 4054905 is one such system, which has been identified, but with measurements of a relatively low precision and with some confusion regarding its parameters and evolutionary state.

Aims. Our aim is to provide a detailed and precise characterisation of the system and to test asteroseismic scaling relations.

Methods. Dynamical and asteroseismic parameters of KIC 4054905 were determined from Kepler time-series photometry and multi-epoch high-resolution spectra from FIES at the Nordic Optical Telescope.

Results. KIC 4054905 was found to belong to the thick disk and consist of two lower red giant branch (RGB) components with nearly identical masses of 0.95 M_⊙ and an age of 9.9 ± 0.6 Gyr. The most evolved star with R ≃ 8.4 R_⊙ displays solar-like oscillations. These oscillations suggest that the star belongs to the RGB, supported also by the radius, which is significantly smaller than the red clump phase for this mass and metallicity. Masses and radii from corrected asteroseismic scaling relations can be brought into full agreement with the dynamical values if the RGB phase is assumed, but a best scaling method could not be identified.

Conclusions. The dynamical masses and radii were measured with a precision better than 1.0%. We firmly establish the evolutionary nature of the system to be that of two early RGB stars with an age close to 10 Gyr, unlike previous findings. The metallicity and Galactic velocity suggest that the system belongs to the thick disk of the Milky Way. We investigate the agreement between dynamical and asteroseismic parameters for KIC 4054905 measured in various ways. This suggests that consistent solutions exist, but the need to analyse more of these systems continues in order to establish the accuracy of asteroseismic methods.

Original language	English
Article number	A82
Number of pages	11
Journal	Astronomy and Astrophysics
Volume	668
DOIs	https://doi.org/10.1051/0004-6361/202244345
Publication status	Published - 8 Dec 2022

Bibliographical note

Funding Information:
We thank the anonymous referee for useful comments that helped improve the paper. We thank Saul A. Rappaport for help with details on the method to estimate the potential systematic error in the Gaia parallax due to the binary orbit. Based on observations made with the Nordic Optical Telescope, owned in collaboration by the University of Turku and Aarhus University, and operated jointly by Aarhus University, the University of Turku and the University of Oslo, representing Denmark, Finland and Norway, the University of Iceland and Stockholm University at the Observatorio del Roque de los Muchachos, La Palma, Spain, of the Instituto de Astrofisica de Canarias. Funding for the Stellar Astrophysics Centre is provided by The Danish National Research Foundation (Grant DNRF106). AM acknowledges support from the ERC Consolidator Grant funding scheme (project ASTEROCHRONOMETRY, https://www.asterochronometry.eu , G.A. n. 772293). D.H. acknowledges support from the Alfred P. Sloan Foundation and the National Aeronautics and Space Administration (80NSSC19K0597). We thank D. A. VandenBerg for providing Victoria isochrones assuming specific element compositions and ages at our request. This work has made use of data from the European Space Agency (ESA) mission Gaia ( https://www.cosmos.esa.int/gaia ), processed by the Gaia Data Processing and Analysis Consortium (DPAC, https://www.cosmos.esa.int/web/gaia/dpac/consortium ). Funding for the DPAC has been provided by national institutions, in particular the institutions participating in the Gaia Multilateral Agreement. This paper includes data collected by the Kepler mission. Funding for the Kepler mission is provided by the NASA Science Mission directorate. Some of the data presented in this paper were obtained from the Mikulski Archive for Space Telescopes (MAST). STScI is operated by the Association of Universities for Research in Astronomy, Inc., under NASA contract NAS5-26555. Support for MAST for non-HST data is provided by the NASA Office of Space Science via grant NNX09AF08G and by other grants and contracts.

Keywords

Binaries: eclipsing
Stars: abundances
Stars: evolution
Stars: fundamental parameters
Stars: individual: KIC 4054905
Stars: oscillations

ASJC Scopus subject areas

Astronomy and Astrophysics
Space and Planetary Science

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Cite this

Brogaard, K., Arentoft, T., Slumstrup, D., Grundahl, F., Lund, M. N., Arndt, L., Grund, S., Rudrasingam, J., Theil, A., Christensen, K., Sejersen, M., Vorgod, F., Salmonsen, L., Ã Rtoft Endelt, L., Dainese, S., Frandsen, S., Miglio, A., Tayar, J., & Huber, D. (2022). Establishing the accuracy of asteroseismic mass and radius estimates of giant stars: III. KIC 4054905, an eclipsing binary with two 10 Gyr thick disk RGB stars. Astronomy and Astrophysics, 668, Article A82. https://doi.org/10.1051/0004-6361/202244345

@article{afb13d08bca84fcd9eb65c15cb99f5fd,

title = "Establishing the accuracy of asteroseismic mass and radius estimates of giant stars: III. KIC 4054905, an eclipsing binary with two 10 Gyr thick disk RGB stars",

abstract = "Context. Eclipsing binary stars with an oscillating giant component allow accurate stellar parameters to be derived and asteroseismic methods to be tested and calibrated. To this aim, suitable systems need to be firstly identified and secondly measured precisely and accurately. KIC 4054905 is one such system, which has been identified, but with measurements of a relatively low precision and with some confusion regarding its parameters and evolutionary state. Aims. Our aim is to provide a detailed and precise characterisation of the system and to test asteroseismic scaling relations. Methods. Dynamical and asteroseismic parameters of KIC 4054905 were determined from Kepler time-series photometry and multi-epoch high-resolution spectra from FIES at the Nordic Optical Telescope. Results. KIC 4054905 was found to belong to the thick disk and consist of two lower red giant branch (RGB) components with nearly identical masses of 0.95 M⊙ and an age of 9.9 ± 0.6 Gyr. The most evolved star with R ≃ 8.4 R⊙ displays solar-like oscillations. These oscillations suggest that the star belongs to the RGB, supported also by the radius, which is significantly smaller than the red clump phase for this mass and metallicity. Masses and radii from corrected asteroseismic scaling relations can be brought into full agreement with the dynamical values if the RGB phase is assumed, but a best scaling method could not be identified. Conclusions. The dynamical masses and radii were measured with a precision better than 1.0%. We firmly establish the evolutionary nature of the system to be that of two early RGB stars with an age close to 10 Gyr, unlike previous findings. The metallicity and Galactic velocity suggest that the system belongs to the thick disk of the Milky Way. We investigate the agreement between dynamical and asteroseismic parameters for KIC 4054905 measured in various ways. This suggests that consistent solutions exist, but the need to analyse more of these systems continues in order to establish the accuracy of asteroseismic methods.",

keywords = "Binaries: eclipsing, Stars: abundances, Stars: evolution, Stars: fundamental parameters, Stars: individual: KIC 4054905, Stars: oscillations",

author = "K. Brogaard and T. Arentoft and D. Slumstrup and F. Grundahl and Lund, {M. N.} and L. Arndt and S. Grund and J. Rudrasingam and A. Theil and K. Christensen and M. Sejersen and F. Vorgod and L. Salmonsen and {{\~A} Rtoft Endelt}, L. and S. Dainese and S. Frandsen and A. Miglio and J. Tayar and D. Huber",

note = "Funding Information: We thank the anonymous referee for useful comments that helped improve the paper. We thank Saul A. Rappaport for help with details on the method to estimate the potential systematic error in the Gaia parallax due to the binary orbit. Based on observations made with the Nordic Optical Telescope, owned in collaboration by the University of Turku and Aarhus University, and operated jointly by Aarhus University, the University of Turku and the University of Oslo, representing Denmark, Finland and Norway, the University of Iceland and Stockholm University at the Observatorio del Roque de los Muchachos, La Palma, Spain, of the Instituto de Astrofisica de Canarias. Funding for the Stellar Astrophysics Centre is provided by The Danish National Research Foundation (Grant DNRF106). AM acknowledges support from the ERC Consolidator Grant funding scheme (project ASTEROCHRONOMETRY, https://www.asterochronometry.eu , G.A. n. 772293). D.H. acknowledges support from the Alfred P. Sloan Foundation and the National Aeronautics and Space Administration (80NSSC19K0597). We thank D. A. VandenBerg for providing Victoria isochrones assuming specific element compositions and ages at our request. This work has made use of data from the European Space Agency (ESA) mission Gaia ( https://www.cosmos.esa.int/gaia ), processed by the Gaia Data Processing and Analysis Consortium (DPAC, https://www.cosmos.esa.int/web/gaia/dpac/consortium ). Funding for the DPAC has been provided by national institutions, in particular the institutions participating in the Gaia Multilateral Agreement. This paper includes data collected by the Kepler mission. Funding for the Kepler mission is provided by the NASA Science Mission directorate. Some of the data presented in this paper were obtained from the Mikulski Archive for Space Telescopes (MAST). STScI is operated by the Association of Universities for Research in Astronomy, Inc., under NASA contract NAS5-26555. Support for MAST for non-HST data is provided by the NASA Office of Space Science via grant NNX09AF08G and by other grants and contracts. ",

year = "2022",

month = dec,

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doi = "10.1051/0004-6361/202244345",

language = "English",

volume = "668",

journal = "Astronomy and Astrophysics",

issn = "0004-6361",

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Brogaard, K, Arentoft, T, Slumstrup, D, Grundahl, F, Lund, MN, Arndt, L, Grund, S, Rudrasingam, J, Theil, A, Christensen, K, Sejersen, M, Vorgod, F, Salmonsen, L, Ã Rtoft Endelt, L, Dainese, S, Frandsen, S, Miglio, A, Tayar, J & Huber, D 2022, 'Establishing the accuracy of asteroseismic mass and radius estimates of giant stars: III. KIC 4054905, an eclipsing binary with two 10 Gyr thick disk RGB stars', Astronomy and Astrophysics, vol. 668, A82. https://doi.org/10.1051/0004-6361/202244345

TY - JOUR

T1 - Establishing the accuracy of asteroseismic mass and radius estimates of giant stars

T2 - III. KIC 4054905, an eclipsing binary with two 10 Gyr thick disk RGB stars

AU - Brogaard, K.

AU - Arentoft, T.

AU - Slumstrup, D.

AU - Grundahl, F.

AU - Lund, M. N.

AU - Arndt, L.

AU - Grund, S.

AU - Rudrasingam, J.

AU - Theil, A.

AU - Christensen, K.

AU - Sejersen, M.

AU - Vorgod, F.

AU - Salmonsen, L.

AU - Ã Rtoft Endelt, L.

AU - Dainese, S.

AU - Frandsen, S.

AU - Miglio, A.

AU - Tayar, J.

AU - Huber, D.

N1 - Funding Information: We thank the anonymous referee for useful comments that helped improve the paper. We thank Saul A. Rappaport for help with details on the method to estimate the potential systematic error in the Gaia parallax due to the binary orbit. Based on observations made with the Nordic Optical Telescope, owned in collaboration by the University of Turku and Aarhus University, and operated jointly by Aarhus University, the University of Turku and the University of Oslo, representing Denmark, Finland and Norway, the University of Iceland and Stockholm University at the Observatorio del Roque de los Muchachos, La Palma, Spain, of the Instituto de Astrofisica de Canarias. Funding for the Stellar Astrophysics Centre is provided by The Danish National Research Foundation (Grant DNRF106). AM acknowledges support from the ERC Consolidator Grant funding scheme (project ASTEROCHRONOMETRY, https://www.asterochronometry.eu , G.A. n. 772293). D.H. acknowledges support from the Alfred P. Sloan Foundation and the National Aeronautics and Space Administration (80NSSC19K0597). We thank D. A. VandenBerg for providing Victoria isochrones assuming specific element compositions and ages at our request. This work has made use of data from the European Space Agency (ESA) mission Gaia ( https://www.cosmos.esa.int/gaia ), processed by the Gaia Data Processing and Analysis Consortium (DPAC, https://www.cosmos.esa.int/web/gaia/dpac/consortium ). Funding for the DPAC has been provided by national institutions, in particular the institutions participating in the Gaia Multilateral Agreement. This paper includes data collected by the Kepler mission. Funding for the Kepler mission is provided by the NASA Science Mission directorate. Some of the data presented in this paper were obtained from the Mikulski Archive for Space Telescopes (MAST). STScI is operated by the Association of Universities for Research in Astronomy, Inc., under NASA contract NAS5-26555. Support for MAST for non-HST data is provided by the NASA Office of Space Science via grant NNX09AF08G and by other grants and contracts.

PY - 2022/12/8

Y1 - 2022/12/8

N2 - Context. Eclipsing binary stars with an oscillating giant component allow accurate stellar parameters to be derived and asteroseismic methods to be tested and calibrated. To this aim, suitable systems need to be firstly identified and secondly measured precisely and accurately. KIC 4054905 is one such system, which has been identified, but with measurements of a relatively low precision and with some confusion regarding its parameters and evolutionary state. Aims. Our aim is to provide a detailed and precise characterisation of the system and to test asteroseismic scaling relations. Methods. Dynamical and asteroseismic parameters of KIC 4054905 were determined from Kepler time-series photometry and multi-epoch high-resolution spectra from FIES at the Nordic Optical Telescope. Results. KIC 4054905 was found to belong to the thick disk and consist of two lower red giant branch (RGB) components with nearly identical masses of 0.95 M⊙ and an age of 9.9 ± 0.6 Gyr. The most evolved star with R ≃ 8.4 R⊙ displays solar-like oscillations. These oscillations suggest that the star belongs to the RGB, supported also by the radius, which is significantly smaller than the red clump phase for this mass and metallicity. Masses and radii from corrected asteroseismic scaling relations can be brought into full agreement with the dynamical values if the RGB phase is assumed, but a best scaling method could not be identified. Conclusions. The dynamical masses and radii were measured with a precision better than 1.0%. We firmly establish the evolutionary nature of the system to be that of two early RGB stars with an age close to 10 Gyr, unlike previous findings. The metallicity and Galactic velocity suggest that the system belongs to the thick disk of the Milky Way. We investigate the agreement between dynamical and asteroseismic parameters for KIC 4054905 measured in various ways. This suggests that consistent solutions exist, but the need to analyse more of these systems continues in order to establish the accuracy of asteroseismic methods.

AB - Context. Eclipsing binary stars with an oscillating giant component allow accurate stellar parameters to be derived and asteroseismic methods to be tested and calibrated. To this aim, suitable systems need to be firstly identified and secondly measured precisely and accurately. KIC 4054905 is one such system, which has been identified, but with measurements of a relatively low precision and with some confusion regarding its parameters and evolutionary state. Aims. Our aim is to provide a detailed and precise characterisation of the system and to test asteroseismic scaling relations. Methods. Dynamical and asteroseismic parameters of KIC 4054905 were determined from Kepler time-series photometry and multi-epoch high-resolution spectra from FIES at the Nordic Optical Telescope. Results. KIC 4054905 was found to belong to the thick disk and consist of two lower red giant branch (RGB) components with nearly identical masses of 0.95 M⊙ and an age of 9.9 ± 0.6 Gyr. The most evolved star with R ≃ 8.4 R⊙ displays solar-like oscillations. These oscillations suggest that the star belongs to the RGB, supported also by the radius, which is significantly smaller than the red clump phase for this mass and metallicity. Masses and radii from corrected asteroseismic scaling relations can be brought into full agreement with the dynamical values if the RGB phase is assumed, but a best scaling method could not be identified. Conclusions. The dynamical masses and radii were measured with a precision better than 1.0%. We firmly establish the evolutionary nature of the system to be that of two early RGB stars with an age close to 10 Gyr, unlike previous findings. The metallicity and Galactic velocity suggest that the system belongs to the thick disk of the Milky Way. We investigate the agreement between dynamical and asteroseismic parameters for KIC 4054905 measured in various ways. This suggests that consistent solutions exist, but the need to analyse more of these systems continues in order to establish the accuracy of asteroseismic methods.

KW - Binaries: eclipsing

KW - Stars: abundances

KW - Stars: evolution

KW - Stars: fundamental parameters

KW - Stars: individual: KIC 4054905

KW - Stars: oscillations

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U2 - 10.1051/0004-6361/202244345

DO - 10.1051/0004-6361/202244345

M3 - Article

AN - SCOPUS:85145357016

SN - 0004-6361

VL - 668

JO - Astronomy and Astrophysics

JF - Astronomy and Astrophysics

M1 - A82

ER -

Establishing the accuracy of asteroseismic mass and radius estimates of giant stars: III. KIC 4054905, an eclipsing binary with two 10 Gyr thick disk RGB stars

Abstract

Bibliographical note

Keywords

ASJC Scopus subject areas

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