Physical parameters of late M-type members of Chamaeleon I and TW Hydrae Association: Dust settling, age dispersion and activity

Simple item page
dc.catalogadorjlo
dc.contributor.authorBayo A.
dc.contributor.authorBarrado, D.
dc.contributor.authorAllard, F.
dc.contributor.authorHenning, T.
dc.contributor.authorComerón, F.
dc.contributor.authorMorales-Calderón, M.
dc.contributor.authorRajpurohit, A.S.
dc.contributor.authorPeña Ramírez, Karla Yulien
dc.contributor.authorBeamín, J.C.
dc.contributor.otherBeamín, J.C.
dc.date.accessioned2024-03-13T19:54:26Z
dc.date.available2024-03-13T19:54:26Z
dc.date.issued2017
dc.description.abstractAlthough mid-to-late type M dwarfs are the most common stars in our stellar neighbourhood, our knowledge of these objects is still limited. Open questions include the evolution of their angular momentum, internal structures, dust settling in their atmospheres and age dispersion within populations. In addition, at young ages, late-type Ms have masses below the hydrogen burning limit and therefore are key objects in the debate on the brown dwarf mechanism of formation. In this work, we determine and study in detail the physical parameters of two samples of young, late M-type sources belonging to either the Chamaeleon I dark cloud or the TW Hydrae Association and compare them with the results obtained in the literature for other young clusters and also for older, field, dwarfs. We used multiwavelength photometry to construct and analyse SEDs to determine general properties of the photosphere and disc presence. We also used low-resolution optical and near-infrared spectroscopy to study activity, accretion, gravity and effective temperature sensitive indicators.We propose a Virtual Observatory-based spectral index that is both temperature and age sensitive.We derived physical parameters using independent techniques confirming the already common feature/problem of the age/luminosity spread. In particular, we highlight two brown dwarfs showing very similar temperatures but clearly different surface gravity (explained invoking extreme early accretion). We also show how, despite large improvement in the dust treatment in theoretical models, there is still room for further progress in the simultaneous reproduction of the optical and near-infrared features of these cold young objects.
dc.fuente.origenSIPA
dc.identifier.doi10.1093/mnras/stw2760
dc.identifier.eissn13652966
dc.identifier.issn13652966 00358711
dc.identifier.scopusidSCOPUS_ID:85014740847
dc.identifier.urihttps://doi.org/10.1093/mnras/stw2760
dc.identifier.urihttps://repositorio.uc.cl/handle/11534/84349
dc.information.autorucInstituto de Física; Peña Ramírez, Karla Yulien; 0000-0002-5855-401X; 183751
dc.issue.numero1
dc.language.isoen
dc.nota.accesoContenido completo
dc.pagina.final783
dc.pagina.inicio760
dc.revistaMonthly Notices of the Royal Astronomical Society
dc.rightsacceso abierto
dc.subjectBrown dwarfs
dc.subjectStars: formation
dc.subjectStars: fundamental parameters
dc.subjectStars: lowmass
dc.subjectStars: pre-main-sequence
dc.subject.ddc520
dc.subject.deweyAstronomíaes_ES
dc.titlePhysical parameters of late M-type members of Chamaeleon I and TW Hydrae Association: Dust settling, age dispersion and activity
dc.typeartículo
dc.volumen465
sipa.codpersvinculados183751
sipa.trazabilidadScopus;12-10-2021
Files
Collections
Artículos de revistas