The EBLM project - VIII. First results for M-dwarf mass, radius, and effective temperature measurements using <i>CHEOPS</i> light curves

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dc.contributor.authorSwayne, M., I
dc.contributor.authorMaxted, P. F. L.
dc.contributor.authorTriaud, A. H. M. J.
dc.contributor.authorSousa, S. G.
dc.contributor.authorBroeg, C.
dc.contributor.authorFloren, H-G
dc.contributor.authorGuterman, P.
dc.contributor.authorSimon, A. E.
dc.contributor.authorBoisse, I
dc.contributor.authorBonfanti, A.
dc.contributor.authorMartin, D.
dc.contributor.authorSanterne, A.
dc.contributor.authorSalmon, S.
dc.contributor.authorStanding, M. R.
dc.contributor.authorVan Grootel, V.
dc.contributor.authorWilson, T. G.
dc.contributor.authorAlibert, Y.
dc.contributor.authorAlonso, R.
dc.contributor.authorAnglada Escude, G.
dc.contributor.authorAsquier, J.
dc.contributor.authorBarczy, T.
dc.contributor.authorBarrado, D.
dc.contributor.authorBarros, S. C. C.
dc.contributor.authorBattley, M.
dc.contributor.authorBaumjohann, W.
dc.contributor.authorBeck, M.
dc.contributor.authorBeck, T.
dc.contributor.authorBekkelien, A.
dc.contributor.authorBenz, W.
dc.contributor.authorBillot, N.
dc.contributor.authorBonfils, X.
dc.contributor.authorBrandeker, A.
dc.contributor.authorBusch, M-D
dc.contributor.authorCabrera, J.
dc.contributor.authorCharnoz, S.
dc.contributor.authorCameron, A. Collier
dc.contributor.authorCsizmadia, Sz
dc.contributor.authorDavies, M. B.
dc.contributor.authorDeleuil, M.
dc.contributor.authorDeline, A.
dc.contributor.authorDelrez, L.
dc.contributor.authorDemangeon, O. D. S.
dc.contributor.authorDemory, B-O
dc.contributor.authorDransfield, G.
dc.contributor.authorEhrenreich, D.
dc.contributor.authorErikson, A.
dc.contributor.authorFortier, A.
dc.contributor.authorFossati, L.
dc.contributor.authorFridlund, M.
dc.contributor.authorFutyan, D.
dc.contributor.authorGandolfi, D.
dc.contributor.authorGillon, M.
dc.contributor.authorGuedel, M.
dc.contributor.authorHebrard, G.
dc.contributor.authorHeidari, N.
dc.contributor.authorHellier, C.
dc.contributor.authorHeng, K.
dc.contributor.authorHobson, M.
dc.contributor.authorHoyer, S.
dc.contributor.authorIsaak, K. G.
dc.contributor.authorKiss, L.
dc.contributor.authorHodzic, V. Kunovac
dc.contributor.authorLalitha, S.
dc.contributor.authorLaskar, J.
dc.contributor.authordes Etangs, A. Lecavelier
dc.contributor.authorLendl, M.
dc.contributor.authorLovis, C.
dc.contributor.authorMagrin, D.
dc.contributor.authorMarafatto, L.
dc.contributor.authorMcCormac, J.
dc.contributor.authorMiller, N.
dc.contributor.authorNascimbeni, V
dc.contributor.authorOlofsson, G.
dc.contributor.authorOttensamer, R.
dc.contributor.authorPagano, I
dc.contributor.authorPalle, E.
dc.contributor.authorPeter, G.
dc.contributor.authorPiotto, G.
dc.contributor.authorPollacco, D.
dc.contributor.authorQueloz, D.
dc.contributor.authorRagazzoni, R.
dc.contributor.authorRando, N.
dc.contributor.authorRauer, H.
dc.contributor.authorRibas, I
dc.contributor.authorSantos, N. C.
dc.contributor.authorScandariato, G.
dc.contributor.authorSegransan, D.
dc.contributor.authorSmith, A. M. S.
dc.contributor.authorSteinberger, M.
dc.contributor.authorSteller, M.
dc.contributor.authorSzabo, Gy M.
dc.contributor.authorThomas, N.
dc.contributor.authorUdry, S.
dc.contributor.authorWalter, I
dc.contributor.authorWalton, N. A.
dc.contributor.authorWillett, E.
dc.date.accessioned2025-01-20T22:02:21Z
dc.date.available2025-01-20T22:02:21Z
dc.date.issued2021
dc.description.abstractThe accuracy of theoretical mass, radius, and effective temperature values for M-dwarf stars is an active topic of debate. Differences between observed and theoretical values have raised the possibility that current theoretical stellar structure and evolution models are inaccurate towards the low-mass end of the main sequence. To explore this issue, we use the CHEOPS satellite to obtain high-precision light curves of eclipsing binaries with low-mass stellar companions. We use these light curves combined with the spectroscopic orbit for the solar-type companion to measure the mass, radius, and effective temperature of the M-dwarf star. Here, we present the analysis of three eclipsing binaries. We use the pycheops data analysis software to fit the observed transit and eclipse events of each system. Two of our systems were also observed by the TESS satellite - we similarly analyse these light curves for comparison. We find consistent results between CHEOPS and TESS, presenting three stellar radii and two stellar effective temperature values of low-mass stellar objects. These initial results from our on-going observing programme with CHEOPS show that we can expect to have similar to 24 new mass, radius, and effective temperature measurements for very low-mass stars within the next few years.
dc.fuente.origenWOS
dc.identifier.doi10.1093/mnras/stab1687
dc.identifier.eissn1365-2966
dc.identifier.issn0035-8711
dc.identifier.urihttps://doi.org/10.1093/mnras/stab1687
dc.identifier.urihttps://repositorio.uc.cl/handle/11534/93971
dc.identifier.wosidWOS:000703918800019
dc.issue.numero1
dc.language.isoen
dc.pagina.final322
dc.pagina.inicio306
dc.revistaMonthly notices of the royal astronomical society
dc.rightsacceso restringido
dc.subjecttechniques: photometric
dc.subjecttechniques: spectroscopic
dc.subjectbinaries: eclipsing
dc.subjectstars: fundamental parameters
dc.subjectstars: low-mass
dc.subject.ods13 Climate Action
dc.subject.odspa13 Acción por el clima
dc.titleThe EBLM project - VIII. First results for M-dwarf mass, radius, and effective temperature measurements using <i>CHEOPS</i> light curves
dc.typeartículo
dc.volumen506
sipa.indexWOS
sipa.trazabilidadWOS;2025-01-12
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