2022A&A...663A.100H

Query : 2022A&A...663A.100H

2022A&A...663A.100H - Astronomy and Astrophysics, volume 663A100-100 (2022/7-1)

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. (The OGLE Collaboration), 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., ISHITANI SILVA S., TODA T., TRISTRAM P.J., VANDOROU A., YAMA H. (The MOA Collaboration), BEICHMAN C.A., BRYDEN G., CALCHI NOVATI S., CAREY S., GAUDI B.S., GOULD A., HENDERSON C.B., JOHNSON S., SHVARTZVALD Y., ZHU W. (The Spitzer Team), DOMINIK M., HUNDERTMARK M., JORGENSEN U.G., LONGA-PENA P., SKOTTFELT J., TREGLOAN-REED J., BACH-MOLLER N., BURGDORF M., D'AGO G., HAIKALA L., HITCHCOCK J., KHALOUEI E., PEIXINHO N., RAHVAR S., SNODGRASS C., SOUTHWORTH J., SPYRATOS P. (The MiNDSTEp Consortium), ZANG W., YANG H., MAO S., BACHELET E., MAOZ D., STREET R.A., TSAPRAS Y., CHRISTIE G.W., COOPER T., DE ALMEIDA L., DO NASCIMENTO J.-D., GREEN J., HAN C., HENNERLEY S., MARMONT A., McCORMICK J., MONARD L.A.G., NATUSCH T., POGGE R. (The LCO and {mu}FUN Collaboration)

Abstract (from CDS):


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 M1 = 0.149 ± 0.010 M☉ and a brown dwarf with a mass of M2 = 0.0463 ± 0.0031 M☉ at a projected separation of a⊥ = 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.

Abstract Copyright: © ESO 2022

Journal keyword(s): gravitational lensing: micro - binaries: general - brown dwarfs - stars: low-mass

VizieR on-line data: <Available at CDS (J/A+A/663/A100): auckr.dat ctioi.dat danishr.dat farmu.dat kkou.dat kumeur.dat lcogthi.dat lcogtri.dat moar.dat moav.dat oglei.dat opdi.dat spitzerl.dat>

Simbad objects: 9

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Number of rows : 9
N Identifier Otype ICRS (J2000)
RA 		ICRS (J2000)
DEC 		Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2026 		#notes
1 OGLE-2007-BLG-224 * 08 05 41.0 -28 45 36           FV 28 0
2 OGLE-2012-BLG-0358 BD? 17 42 46.7641762656 -24 15 39.605456196           ~ 16 1
3 NAME Galactic Center reg 17 45 39.60213 -29 00 22.0000           ~ 16269 0
4 OGLE-2011-BLG-0420 * 17 50 56.1715170240 -29 49 30.216419616           ~ 11 1
5 OGLE-2016-BLG-1266 BD? 17 51 24.86 -29 44 32.1           ~ 7 0
6 MOA 2009-BLG-232 * 17 54 22.3539093816 -29 03 21.146804712           ~ 13 1
7 MOA 2011-BLG-149 * 17 56 47.690 -31 16 04.71           ~ 6 0
8 MOA 2007-BLG-197 * 18 07 04.729 -31 56 46.77           ~ 10 0
9 2MASS J18083825-3003386 ** 18 08 38.2563956550 -30 03 38.728877436         15.711 ~ 3 0

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