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Authordc.contributor.authorTrahin, B.
Authordc.contributor.authorBreuval, L.
Authordc.contributor.authorKervella, P.
Authordc.contributor.authorMerand, A.
Authordc.contributor.authorNardetto, N.
Authordc.contributor.authorGallenne, Alexandre
Authordc.contributor.authorHocde, V.
Authordc.contributor.authorGieren, W.
Admission datedc.date.accessioned2022-04-28T15:14:06Z
Available datedc.date.available2022-04-28T15:14:06Z
Publication datedc.date.issued2021
Cita de ítemdc.identifier.citationA&A 656, A102 (2021)es_ES
Identifierdc.identifier.other10.1051/0004-6361/202141680
Identifierdc.identifier.urihttps://repositorio.uchile.cl/handle/2250/185153
Abstractdc.description.abstractContext. As primary anchors of the distance scale, Cepheid stars play a crucial role in our understanding of the distance scale of the Universe because of their period-luminosity relation. Determining precise and consistent parameters (radius, temperature, color excess, and projection factor) of Cepheid pulsating stars is therefore very important. Aims. With the high-precision parallaxes delivered by the early third Gaia data release (EDR3), we aim to derive various parameters of Cepheid stars in order to calibrate the period-luminosity and period-radius relations and to investigate the relation of period to p-factor. Methods. We applied an implementation of the parallax-of-pulsation method through the algorithm called spectro-photointerferometry of pulsating stars (SPIPS), which combines all types of available data for a variable star (multiband and multicolor photometry, radial velocity, effective temperature, and interferometry measurements) in a global modeling of its pulsation. Results. We present the SPIPS modeling of a sample of 63 Galactic Cepheids. Adopting Gaia EDR3 parallaxes as an input associated with the best available dataset, we derive consistent values of parameters for these stars such as the radius, multiband apparent magnitudes, effective temperatures, color excesses, period changes, Fourier parameters, and the projection factor. Conclusions. Using the best set of data and the most precise distances for Milky Way Cepheids, we derive new calibrations of the period-luminosity and period-radius relations: MKS = −5.529±0.015 − 3.141±0.050(log P − 0.9) and log R = 1.763±0.003 + 0.653±0.012(log P − 0.9). After investigating the dependences of the projection factor on the parameters of the stars, we find a high dispersion of its values and no evidence of its correlation with the period or with any other parameters such as radial velocity, temperature, or metallicity. Statistically, the p-factor has an average value of p = 1.26±0.07, but with an unsatisfactory agreement (σ = 0.15). In absence of any clear correlation between the p-factor and other quantities, the best agreement is obtained under the assumption that the p-factor can take any value in a band with a width of 0.15. This result highlights the need for a further examination of the physics behind the p-factor.es_ES
Patrocinadordc.description.sponsorshipEuropean Research Council (ERC) 695099 French National Research Agency (ANR) ANR-15-CE31-0012-01 Spanish Government AYA2017-84089es_ES
Lenguagedc.language.isoenes_ES
Publisherdc.publisherEDPes_ES
Type of licensedc.rightsAttribution-NonCommercial-NoDerivs 3.0 United States*
Link to Licensedc.rights.urihttp://creativecommons.org/licenses/by-nc-nd/3.0/us/*
Sourcedc.sourceAstronomy & Astrophysicses_ES
Keywordsdc.subjectStars: variables: Cepheidses_ES
Keywordsdc.subjectStars: fundamental parameterses_ES
Keywordsdc.subjectDistance scalees_ES
Títulodc.titleInspecting the Cepheid parallax of pulsation using Gaia EDR3 parallaxes Projection factor and period-luminosity and period-radius relationses_ES
Document typedc.typeArtículo de revistaes_ES
dc.description.versiondc.description.versionVersión publicada - versión final del editores_ES
dcterms.accessRightsdcterms.accessRightsAcceso abiertoes_ES
Catalogueruchile.catalogadorcrbes_ES
Indexationuchile.indexArtículo de publícación WoSes_ES


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Attribution-NonCommercial-NoDerivs 3.0 United States
Except where otherwise noted, this item's license is described as Attribution-NonCommercial-NoDerivs 3.0 United States