Precision measurement of a brown dwarf mass in a binary system in the microlensing event OGLE-2019-BLG-0033/MOA-2019-BLG-035
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Precision measurement of a brown dwarf mass in a binary system in the microlensing event OGLE-2019-BLG-0033/MOA-2019-BLG-035. / Herald, A.; Udalski, A.; Bozza, V.; Rota, P.; Bond, I. A.; Yee, J. C.; Sajadian, S.; Mroz, P.; Poleski, R.; Skowron, J.; Szymanski, M. K.; Soszynski, I.; Pietrukowicz, P.; Kozlowski, S.; Ulaczyk, K.; Rybicki, K. A.; Iwanek, P.; Wrona, M.; Gromadzki, M.; Abe, F.; Barry, R.; Bennett, D. P.; Bhattacharya, A.; Fukui, A.; Fujii, H.; Hirao, Y.; Itow, Y.; Kirikawa, R.; Kondo, I.; Koshimoto, N.; Matsubara, Y.; Matsumoto, S.; Miyazaki, S.; Muraki, Y.; Olmschenk, G.; Ranc, C.; Okamura, A.; Rattenbury, N. J.; Satoh, Y.; Sumi, T.; Suzuki, D.; Silva, S. Ishitani; Toda, T.; Tristram, P. J.; Vandorou, A.; Yama, H.; Beichman, C. A.; Bryden, G.; Jorgensen, U. G.; Bach-Moller, N.; OGLE Collaboration; MOA Collaboration; Spitzer Team; MINDSTEp Consortium; LCO & FUN Collaboration.
I: Astronomy & Astrophysics, Bind 663, 100, 19.07.2022.Publikation: Bidrag til tidsskrift › Tidsskriftartikel › Forskning › fagfællebedømt
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TY - JOUR
T1 - Precision measurement of a brown dwarf mass in a binary system in the microlensing event OGLE-2019-BLG-0033/MOA-2019-BLG-035
AU - Herald, A.
AU - Udalski, A.
AU - Bozza, V.
AU - Rota, P.
AU - Bond, I. A.
AU - Yee, J. C.
AU - Sajadian, S.
AU - Mroz, P.
AU - Poleski, R.
AU - Skowron, J.
AU - Szymanski, M. K.
AU - Soszynski, I.
AU - Pietrukowicz, P.
AU - Kozlowski, S.
AU - Ulaczyk, K.
AU - Rybicki, K. A.
AU - Iwanek, P.
AU - Wrona, M.
AU - Gromadzki, M.
AU - Abe, F.
AU - Barry, R.
AU - Bennett, D. P.
AU - Bhattacharya, A.
AU - Fukui, A.
AU - Fujii, H.
AU - Hirao, Y.
AU - Itow, Y.
AU - Kirikawa, R.
AU - Kondo, I.
AU - Koshimoto, N.
AU - Matsubara, Y.
AU - Matsumoto, S.
AU - Miyazaki, S.
AU - Muraki, Y.
AU - Olmschenk, G.
AU - Ranc, C.
AU - Okamura, A.
AU - Rattenbury, N. J.
AU - Satoh, Y.
AU - Sumi, T.
AU - Suzuki, D.
AU - Silva, S. Ishitani
AU - Toda, T.
AU - Tristram, P. J.
AU - Vandorou, A.
AU - Yama, H.
AU - Beichman, C. A.
AU - Bryden, G.
AU - Jorgensen, U. G.
AU - Bach-Moller, N.
AU - OGLE Collaboration
AU - MOA Collaboration
AU - Spitzer Team
AU - MINDSTEp Consortium
AU - LCO & FUN Collaboration
PY - 2022/7/19
Y1 - 2022/7/19
N2 - Context. 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.Aims. 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.Methods. 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.Results. 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.
AB - Context. 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.Aims. 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.Methods. 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.Results. 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.
KW - gravitational lensing: micro
KW - binaries: general
KW - brown dwarfs
KW - stars: low-mass
KW - DIFFERENCE IMAGE-ANALYSIS
KW - GALACTIC BULGE
KW - GRAVITATIONAL LENS
KW - CHEMICAL EVOLUTION
KW - PLANET CANDIDATE
KW - OPTICAL DEPTH
KW - GIANT PLANETS
KW - PHOTOMETRY
KW - DISCOVERY
KW - SPITZER
U2 - 10.1051/0004-6361/202243490
DO - 10.1051/0004-6361/202243490
M3 - Journal article
VL - 663
JO - Astronomy & Astrophysics
JF - Astronomy & Astrophysics
SN - 0004-6361
M1 - 100
ER -
ID: 315254593