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dc.rights.license© ESO 2021es
dc.contributor.authorGuzmán Díaz, J.-
dc.contributor.authorMendigutía, I.-
dc.contributor.authorMontesinos, B.-
dc.contributor.authorOudmaijer, R. D.-
dc.contributor.authorVioque, M.-
dc.contributor.authorRodrigo, C.-
dc.contributor.authorSolano, E.-
dc.contributor.authorMeeus, G.-
dc.contributor.authorMarcos Arenal, P.-
dc.identifier.citationAstronomy and Astrophysics 650: A182(2021)es
dc.description.abstractContext. Herbig Ae/Be stars (HAeBes) have so far been studied based on relatively small samples that are scattered throughout the sky. Their fundamental stellar and circumstellar parameters and statistical properties were derived with heterogeneous approaches before Gaia. Aims. Our main goal is to contribute to the study of HAeBes from the largest sample of such sources to date, for which stellar and circumstellar properties have been determined homogeneously from the analysis of the spectral energy distributions (SEDs) and Gaia EDR3 parallaxes and photometry. Methods. Multiwavelength photometry was compiled for 209 bona fide HAeBes for which Gaia EDR3 distances were estimated. Using the Virtual Observatory SED Analyser (VOSA), photospheric models were fit to the optical SEDs to derive stellar parameters, and the excesses at infrared (IR) and longer wavelengths were characterized to derive several circumstellar properties. A statistical analysis was carried out to show the potential use of such a large dataset. Results. The stellar temperature, luminosity, radius, mass, and age were derived for each star based on optical photometry. In addition, their IR SEDs were classified according to two different schemes, and their mass accretion rates, disk masses, and the sizes of the inner dust holes were also estimated uniformly. The initial mass function fits the stellar mass distribution of the sample within 2 < M*∕M⊙ < 12. In this aspect, the sample is therefore representative of the HAeBe regime and can be used for statistical purposes when it is taken into account that the boundaries are not well probed. Our statistical study does not reveal any connection between the SED shape from the Meeus et al. (2001, A&A, 365, 476) classification and the presence of transitional disks, which are identified here based on the SEDs that show an IR excess starting at the K band or longer wavelengths. In contrast, only ~28% of the HAeBes have transitional disks, and the related dust disk holes are more frequent in HBes than in HAes (~34% vs. 15%). The relatively small inner disk holes and old stellar ages estimated for most transitional HAes indicate that photoevaporation cannot be the main mechanism driving disk dissipation in these sources. In contrast, the inner disk holes and ages of most transitional HBes are consistent with the photoevaporation scenario, although these results alone do not unambiguously discard other disk dissipation mechanisms.Conclusions. The complete dataset is available online through a Virtual Observatory-compliant archive, representing the most recent reference for statistical studies on the HAeBe regime. VOSA is a complementary tool for the future characterization of newly identified
dc.description.sponsorshipJGD, IM and PMA acknowledge the Government of Comunidad Autónoma de Madrid (Spain) for funding this research through a ‘Talento’ Fellowship (2016-T1/TIC-1890 PI I. Mendigutía). The research of IM, JGD, BM and GM is also partially funded by the Spanish “Ministerio de Ciencia, Innovación y Universidades” through the national project “On the Rocks II” (PGC2018-101950-B-100; PI E. Villaver). MV acknowledges the STARRY project, which has received funding from the European Union’s Horizon 2020 research and innovation programme under MSCA ITN-EID grant agreement No 676036. This publication makes use of VOSA, developed under the Spanish Virtual Observatory project supported by the Spanish MINECO through grant AyA2017-84089. VOSA has been partially updated by using funding from the European Union’s Horizon 2020 Research and Innovation Programme, under Grant Agreement n 776403 (EXOPLANETS-A). This work has made use of data from the European Space Agency (ESA) mission Gaia (, processed by the Gaia Data Processing and Analysis Consortium (DPAC, Funding for the DPAC has been provided by national institutions, in particular the institutions participating in the Gaia Multilateral Agreement. The authors also acknowledge the referee for her/his useful comments, which have served to improve the original
dc.publisherEDP Scienceses
dc.relationinfo:eu-repo/grantAgreement/AEI/Plan Estatal de Investigación Científica y Técnica y de Innovación 2017-2020/PGC2018-101950-B-I00/ES/ON THE ROCKS II/-
dc.relationinfo:eu-repo/grantAgreement/AEI/Plan Estatal de Investigación Científica y Técnica y de Innovación 2013-2016/AYA2017-84089-P/ES/EL OBSERVATORIO VIRTUAL ESPAÑOL. EXPLOTACION CIENTIFICO-TECNICA DE ARCHIVOS ASTRONOMICOS/-
dc.rightsAttribution-NonCommercial-NoDerivatives 4.0 Internationales
dc.subjectProtoplanetary diskes
dc.subjectStars: pre-main sequencees
dc.subjectStars: variables: T Tauries
dc.subjectHerbig Ae/Bees
dc.subjectVirtual observatory toolses
dc.subjectStars: fundamental parameterses
dc.subjectAstronomical databases: miscellaneouses
dc.titleHomogeneous study of Herbig Ae/Be stars from spectral energy distributions and Gaia EDR3es
dc.contributor.funderComunidad de Madrid-
dc.contributor.funderAgencia Estatal de Investigación (AEI)-
dc.contributor.funderEuropean Research Council (ERC)-
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