PLATO hare-and-hounds exercise: asteroseismic model fitting of main-sequence solar-like pulsators

M.S. Cunha; I.W. Roxburgh; Victor Aguirre Børsen-Koch; Warrick H.   Ball; S. Basu; William James  Chaplin; Marie-Jo Goupil; B. Nsamba; Joel J. M. Ong; Daniel R.  Reese; Kuldeep Verma; Kevin Belkacem; Tiago Campante; Jørgen Christensen-Dalsgaard; M. T. Clara; Sebastien Deheuvels; M. J. P. F. G. Monteiro; Anthony Noll; Rhita-Maria Ouazzani; Jakob Rørsted Mosumgaard; Amalie Stokholm; Mark Lykke Winther

doi:10.1093/mnras/stab2886

PLATO hare-and-hounds exercise: asteroseismic model fitting of main-sequence solar-like pulsators

M.S. Cunha^*, I.W. Roxburgh, Victor Aguirre Børsen-Koch, Warrick H. Ball, S. Basu, William James Chaplin, Marie-Jo Goupil, B. Nsamba, Joel J. M. Ong, Daniel R. Reese, Kuldeep Verma, Kevin Belkacem, Tiago Campante, Jørgen Christensen-Dalsgaard, M. T. Clara, Sebastien Deheuvels, M. J. P. F. G. Monteiro, Anthony Noll, Rhita-Maria Ouazzani, Jakob Rørsted MosumgaardAmalie Stokholm, Mark Lykke Winther

^*Corresponding author af dette arbejde

Institut for Fysik og Astronomi - Stellar Astrophysics Centre

Publikation: Bidrag til tidsskrift/Konferencebidrag i tidsskrift /Bidrag til avis › Tidsskriftartikel › Forskning › peer review

Abstract

Asteroseismology is a powerful tool to infer fundamental stellar properties. The use of these asteroseismic-inferred properties in a growing number of astrophysical contexts makes it vital to understand their accuracy. Consequently, we performed a hare-and-hounds exercise where the hares simulated data for six artificial main-sequence stars and the hounds inferred their properties based on different inference procedures. To mimic a pipeline such as that planned for the PLATO mission, all hounds used the same model grid. Some stars were simulated using the physics adopted in the grid, others a different one. The maximum relative differences found (in absolute value) between the inferred and true values of the mass, radius, and age were 4.32, 1.33, and 11.25 per cent, respectively. The largest systematic differences in radius and age were found for a star simulated assuming gravitational settling, not accounted for in the model grid, with biases of −0.88 per cent (radius) and 8.66 per cent (age). For the mass, the most significant bias (−3.16 per cent) was found for a star with a helium enrichment ratio outside the grid range. Moreover, an ∼7 per cent dispersion in age was found when adopting different prescriptions for the surface corrections or shifting the classical observations by ±1σ. The choice of the relative weight given to the classical and seismic constraints also impacted significantly the accuracy and precision of the results. Interestingly, only a few frequencies were required to achieve accurate results on the mass and radius. For the age the same was true when at least one l = 2 mode was considered.

Originalsprog	Engelsk
Tidsskrift	Monthly Notices of the Royal Astronomical Society
Vol/bind	508
Nummer	4
Sider (fra-til)	5864-5885
Antal sider	21
ISSN	0035-8711
DOI	https://doi.org/10.1093/mnras/stab2886
Status	Udgivet - dec. 2021

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10.1093/mnras/stab2886

https://arxiv.org/pdf/2110.03332.pdf

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Cunha, M. S., Roxburgh, I. W., Børsen-Koch, V. A., Ball, W. H., Basu, S., Chaplin, W. J., Goupil, M.-J., Nsamba, B., Ong, J. J. M., Reese, D. R., Verma, K., Belkacem, K., Campante, T., Christensen-Dalsgaard, J., Clara, M. T., Deheuvels, S., Monteiro, M. J. P. F. G., Noll, A., Ouazzani, R.-M., ... Winther, M. L. (2021). PLATO hare-and-hounds exercise: asteroseismic model fitting of main-sequence solar-like pulsators. Monthly Notices of the Royal Astronomical Society, 508(4), 5864-5885. https://doi.org/10.1093/mnras/stab2886

@article{47a9ea54cd3448c4bf8a9defe3953688,

title = "PLATO hare-and-hounds exercise: asteroseismic model fitting of main-sequence solar-like pulsators",

abstract = "Asteroseismology is a powerful tool to infer fundamental stellar properties. The use of these asteroseismic-inferred properties in a growing number of astrophysical contexts makes it vital to understand their accuracy. Consequently, we performed a hare-and-hounds exercise where the hares simulated data for six artificial main-sequence stars and the hounds inferred their properties based on different inference procedures. To mimic a pipeline such as that planned for the PLATO mission, all hounds used the same model grid. Some stars were simulated using the physics adopted in the grid, others a different one. The maximum relative differences found (in absolute value) between the inferred and true values of the mass, radius, and age were 4.32, 1.33, and 11.25 per cent, respectively. The largest systematic differences in radius and age were found for a star simulated assuming gravitational settling, not accounted for in the model grid, with biases of −0.88 per cent (radius) and 8.66 per cent (age). For the mass, the most significant bias (−3.16 per cent) was found for a star with a helium enrichment ratio outside the grid range. Moreover, an ∼7 per cent dispersion in age was found when adopting different prescriptions for the surface corrections or shifting the classical observations by ±1σ. The choice of the relative weight given to the classical and seismic constraints also impacted significantly the accuracy and precision of the results. Interestingly, only a few frequencies were required to achieve accurate results on the mass and radius. For the age the same was true when at least one l = 2 mode was considered.",

keywords = "asteroseismology, methods: statistical, stars: evolution, stars: fundamental parameters, stars: oscillations",

author = "M.S. Cunha and I.W. Roxburgh and B{\o}rsen-Koch, {Victor Aguirre} and Ball, {Warrick H.} and S. Basu and Chaplin, {William James} and Marie-Jo Goupil and B. Nsamba and Ong, {Joel J. M.} and Reese, {Daniel R.} and Kuldeep Verma and Kevin Belkacem and Tiago Campante and J{\o}rgen Christensen-Dalsgaard and Clara, {M. T.} and Sebastien Deheuvels and Monteiro, {M. J. P. F. G.} and Anthony Noll and Rhita-Maria Ouazzani and Mosumgaard, {Jakob R{\o}rsted} and Amalie Stokholm and Winther, {Mark Lykke}",

year = "2021",

month = dec,

doi = "10.1093/mnras/stab2886",

language = "English",

volume = "508",

pages = "5864--5885",

journal = "Monthly Notices of the Royal Astronomical Society",

issn = "0035-8711",

publisher = "Oxford University Press",

number = "4",

}

Cunha, MS, Roxburgh, IW, Børsen-Koch, VA, Ball, WH, Basu, S, Chaplin, WJ, Goupil, M-J, Nsamba, B, Ong, JJM, Reese, DR, Verma, K, Belkacem, K, Campante, T, Christensen-Dalsgaard, J, Clara, MT, Deheuvels, S, Monteiro, MJPFG, Noll, A, Ouazzani, R-M, Mosumgaard, JR , Stokholm, A & Winther, ML 2021, 'PLATO hare-and-hounds exercise: asteroseismic model fitting of main-sequence solar-like pulsators', Monthly Notices of the Royal Astronomical Society, bind 508, nr. 4, s. 5864-5885. https://doi.org/10.1093/mnras/stab2886

PLATO hare-and-hounds exercise: asteroseismic model fitting of main-sequence solar-like pulsators. / Cunha, M.S.; Roxburgh, I.W.; Børsen-Koch, Victor Aguirre et al.
I: Monthly Notices of the Royal Astronomical Society, Bind 508, Nr. 4, 12.2021, s. 5864-5885.

Publikation: Bidrag til tidsskrift/Konferencebidrag i tidsskrift /Bidrag til avis › Tidsskriftartikel › Forskning › peer review

TY - JOUR

T1 - PLATO hare-and-hounds exercise

T2 - asteroseismic model fitting of main-sequence solar-like pulsators

AU - Cunha, M.S.

AU - Roxburgh, I.W.

AU - Børsen-Koch, Victor Aguirre

AU - Ball, Warrick H.

AU - Basu, S.

AU - Chaplin, William James

AU - Goupil, Marie-Jo

AU - Nsamba, B.

AU - Ong, Joel J. M.

AU - Reese, Daniel R.

AU - Verma, Kuldeep

AU - Belkacem, Kevin

AU - Campante, Tiago

AU - Christensen-Dalsgaard, Jørgen

AU - Clara, M. T.

AU - Deheuvels, Sebastien

AU - Monteiro, M. J. P. F. G.

AU - Noll, Anthony

AU - Ouazzani, Rhita-Maria

AU - Mosumgaard, Jakob Rørsted

AU - Stokholm, Amalie

AU - Winther, Mark Lykke

PY - 2021/12

Y1 - 2021/12

N2 - Asteroseismology is a powerful tool to infer fundamental stellar properties. The use of these asteroseismic-inferred properties in a growing number of astrophysical contexts makes it vital to understand their accuracy. Consequently, we performed a hare-and-hounds exercise where the hares simulated data for six artificial main-sequence stars and the hounds inferred their properties based on different inference procedures. To mimic a pipeline such as that planned for the PLATO mission, all hounds used the same model grid. Some stars were simulated using the physics adopted in the grid, others a different one. The maximum relative differences found (in absolute value) between the inferred and true values of the mass, radius, and age were 4.32, 1.33, and 11.25 per cent, respectively. The largest systematic differences in radius and age were found for a star simulated assuming gravitational settling, not accounted for in the model grid, with biases of −0.88 per cent (radius) and 8.66 per cent (age). For the mass, the most significant bias (−3.16 per cent) was found for a star with a helium enrichment ratio outside the grid range. Moreover, an ∼7 per cent dispersion in age was found when adopting different prescriptions for the surface corrections or shifting the classical observations by ±1σ. The choice of the relative weight given to the classical and seismic constraints also impacted significantly the accuracy and precision of the results. Interestingly, only a few frequencies were required to achieve accurate results on the mass and radius. For the age the same was true when at least one l = 2 mode was considered.

AB - Asteroseismology is a powerful tool to infer fundamental stellar properties. The use of these asteroseismic-inferred properties in a growing number of astrophysical contexts makes it vital to understand their accuracy. Consequently, we performed a hare-and-hounds exercise where the hares simulated data for six artificial main-sequence stars and the hounds inferred their properties based on different inference procedures. To mimic a pipeline such as that planned for the PLATO mission, all hounds used the same model grid. Some stars were simulated using the physics adopted in the grid, others a different one. The maximum relative differences found (in absolute value) between the inferred and true values of the mass, radius, and age were 4.32, 1.33, and 11.25 per cent, respectively. The largest systematic differences in radius and age were found for a star simulated assuming gravitational settling, not accounted for in the model grid, with biases of −0.88 per cent (radius) and 8.66 per cent (age). For the mass, the most significant bias (−3.16 per cent) was found for a star with a helium enrichment ratio outside the grid range. Moreover, an ∼7 per cent dispersion in age was found when adopting different prescriptions for the surface corrections or shifting the classical observations by ±1σ. The choice of the relative weight given to the classical and seismic constraints also impacted significantly the accuracy and precision of the results. Interestingly, only a few frequencies were required to achieve accurate results on the mass and radius. For the age the same was true when at least one l = 2 mode was considered.

KW - asteroseismology

KW - methods: statistical

KW - stars: evolution

KW - stars: fundamental parameters

KW - stars: oscillations

UR - http://www.scopus.com/inward/record.url?scp=85119486369&partnerID=8YFLogxK

U2 - 10.1093/mnras/stab2886

DO - 10.1093/mnras/stab2886

M3 - Journal article

SN - 0035-8711

VL - 508

SP - 5864

EP - 5885

JO - Monthly Notices of the Royal Astronomical Society

JF - Monthly Notices of the Royal Astronomical Society

IS - 4

ER -

PLATO hare-and-hounds exercise: asteroseismic model fitting of main-sequence solar-like pulsators

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