Precision measurement of a brown dwarf mass in a binary system in the microlensing event OGLE-2019-BLG-0033/MOA-2019-BLG-035

Simple item page
dc.contributor.authorHerald, A.
dc.contributor.authorUdalski, A.
dc.contributor.authorBozza, V.
dc.contributor.authorRota, P.
dc.contributor.authorBond, I. A.
dc.contributor.authorYee, J. C.
dc.contributor.authorSajadian, S.
dc.contributor.authorMroz, P.
dc.contributor.authorPoleski, R.
dc.contributor.authorSkowron, J.
dc.contributor.authorSzymanski, M. K.
dc.contributor.authorSoszynski, I.
dc.contributor.authorPietrukowicz, P.
dc.contributor.authorKozlowski, S.
dc.contributor.authorUlaczyk, K.
dc.contributor.authorRybicki, K. A.
dc.contributor.authorIwanek, P.
dc.contributor.authorWrona, M.
dc.contributor.authorGromadzki, M.
dc.contributor.authorAbe, F.
dc.contributor.authorBarry, R.
dc.contributor.authorBennett, D. P.
dc.contributor.authorBhattacharya, A.
dc.contributor.authorFukui, A.
dc.contributor.authorFujii, H.
dc.contributor.authorHirao, Y.
dc.contributor.authorItow, Y.
dc.contributor.authorKirikawa, R.
dc.contributor.authorKondo, I.
dc.contributor.authorKoshimoto, N.
dc.contributor.authorMatsubara, Y.
dc.contributor.authorMatsumoto, S.
dc.contributor.authorMiyazaki, S.
dc.contributor.authorMuraki, Y.
dc.contributor.authorOlmschenk, G.
dc.contributor.authorRanc, C.
dc.contributor.authorOkamura, A.
dc.contributor.authorRattenbury, N. J.
dc.contributor.authorSatoh, Y.
dc.contributor.authorSumi, T.
dc.contributor.authorSuzuki, D.
dc.contributor.authorSilva, S. Ishitani
dc.contributor.authorToda, T.
dc.contributor.authorTristram, P. J.
dc.contributor.authorVandorou, A.
dc.contributor.authorYama, H.
dc.contributor.authorBeichman, C. A.
dc.contributor.authorBryden, G.
dc.contributor.authorNovati, S. Calchi
dc.contributor.authorCarey, S.
dc.contributor.authorGaudi, B. S.
dc.contributor.authorGould, A.
dc.contributor.authorHenderson, C. B.
dc.contributor.authorJohnson, S.
dc.contributor.authorShvartzvald, Y.
dc.contributor.authorZhu, W.
dc.contributor.authorDominik, M.
dc.contributor.authorHundertmark, M.
dc.contributor.authorJorgensen, U. G.
dc.contributor.authorLonga-Pena, P.
dc.contributor.authorSkottfelt, J.
dc.contributor.authorTregloan-Reed, J.
dc.contributor.authorBach-Moller, N.
dc.contributor.authorBurgdorf, M.
dc.contributor.authorD'Ago, G.
dc.contributor.authorHaikala, L.
dc.contributor.authorHitchcock, J.
dc.contributor.authorKhalouei, E.
dc.contributor.authorPeixinho, N.
dc.contributor.authorRahvar, S.
dc.contributor.authorSnodgrass, C.
dc.contributor.authorSouthworth, J.
dc.contributor.authorSpyratos, P.
dc.contributor.authorZang, W.
dc.contributor.authorYang, H.
dc.contributor.authorMao, S.
dc.contributor.authorBachelet, E.
dc.contributor.authorMaoz, D.
dc.contributor.authorStreet, R. A.
dc.contributor.authorTsapras, Y.
dc.contributor.authorChristie, G. W.
dc.contributor.authorCooper, T.
dc.contributor.authorde Almeida, L.
dc.contributor.authordo Nascimento, J. -D., Jr.
dc.contributor.authorGreen, J.
dc.contributor.authorHan, C.
dc.contributor.authorHennerley, S.
dc.contributor.authorMarmont, A.
dc.contributor.authorMcCormick, J.
dc.contributor.authorMonard, L. A. G.
dc.contributor.authorNatusch, T.
dc.contributor.authorPogge, R.
dc.date.accessioned2025-01-20T21:04:10Z
dc.date.available2025-01-20T21:04:10Z
dc.date.issued2022
dc.description.abstractContext. Brown dwarfs are transition objects between stars and planets that are still poorly understood, for which several competing mechanisms have been proposed to describe their formation. Mass measurements are generally difficult to carry out for isolated objects as well as for brown dwarfs orbiting low-mass stars, which are often too faint for a spectroscopic follow-up.
dc.description.abstractAims. Microlensing provides an alternative tool for the discovery and investigation of such faint systems. Here, we present an analysis of the microlensing event OGLE-2019-BLG-0033/MOA-2019-BLG-035, which is caused by a binary system composed of a brown dwarf orbiting a red dwarf.
dc.description.abstractMethods. Thanks to extensive ground observations and the availability of space observations from Spitzer, it has been possible to obtain accurate estimates of all microlensing parameters, including the parallax, source radius, and orbital motion of the binary lens.
dc.description.abstractResults. Following an accurate modeling process, we found that the lens is composed of a red dwarf with a mass of M-1 = 0.149 +/- 0.010 M-circle dot and a brown dwarf with a mass of M-2 = 0.0463 +/- 0.0031 M-circle dot at a projected separation of a(perpendicular to) = 0.585 au. The system has a peculiar velocity that is typical of old metal-poor populations in the thick disk. A percent-level precision in the mass measurement of brown dwarfs has been achieved only in a few microlensing events up to now, but will likely become more common in the future thanks to the Roman space telescope.
dc.fuente.origenWOS
dc.identifier.doi10.1051/0004-6361/202243490
dc.identifier.eissn1432-0746
dc.identifier.issn0004-6361
dc.identifier.urihttps://doi.org/10.1051/0004-6361/202243490
dc.identifier.urihttps://repositorio.uc.cl/handle/11534/93217
dc.identifier.wosidWOS:000827180900006
dc.language.isoen
dc.revistaAstronomy & astrophysics
dc.rightsacceso restringido
dc.subjectgravitational lensing: micro
dc.subjectbinaries: general
dc.subjectbrown dwarfs
dc.subjectstars: low-mass
dc.subject.ods13 Climate Action
dc.subject.odspa13 Acción por el clima
dc.titlePrecision measurement of a brown dwarf mass in a binary system in the microlensing event OGLE-2019-BLG-0033/MOA-2019-BLG-035
dc.typeartículo
dc.volumen663
sipa.indexWOS
sipa.trazabilidadWOS;2025-01-12
Files
Collections
Artículos de revistas