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

A. Herald; A. Udalski; V. Bozza; P. Rota; I. A. Bond; J. C. Yee; S. Sajadian; P. Mróz; R. Poleski; J. Skowron; M. K. Szymanski; I. Soszynski; P. Pietrukowicz; S. Kozlowski; K. Ulaczyk; K. A. Rybicki; P. Iwanek; M. Wrona; M. Gromadzki; F. Abe; R. Barry; D. P. Bennett; A. Bhattacharya; A. Fukui; H. Fujii; Y. Hirao; Y. Itow; R. Kirikawa; I. Kondo; N. Koshimoto; Y. Matsubara; S. Matsumoto; S. Miyazaki; Y. Muraki; G. Olmschenk; C. Ranc; A. Okamura; N. J. Rattenbury; Y. Satoh; T. Sumi; D. Suzuki; S. Ishitani Silva; T. Toda; P. J. Tristram; A. Vandorou; H. Yama; C. A. Beichman; G. Bryden; S. Calchi Novati; S. Carey; B. S. Gaudi; A. Gould; C. B. Henderson; S. Johnson; Y. Shvartzvald; W. Zhu; M. Dominik; M. Hundertmark; U. G. Jørgensen; P. Longa-Peña; J. Skottfelt; J. Tregloan-Reed; N. Bach-Møller; M. Burgdorf; G. D'Ago; L. Haikala; J. Hitchcock; E. Khalouei; N. Peixinho; S. Rahvar; C. Snodgrass; J. Southworth; P. Spyratos; W. Zang; H. Yang; S. Mao; E. Bachelet; D. Maoz; R. A. Street; Y. Tsapras; G. W. Christie; T. Cooper; L. De Almeida; J. D. Do Nascimento; J. Green; C. Han; S. Hennerley; A. Marmont; J. McCormick; L. A.G. Monard; T. Natusch; R. Pogge

doi:10.1051/0004-6361/202243490

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

A. Herald, A. Udalski, V. Bozza^*, P. Rota, I. A. Bond, J. C. Yee, S. Sajadian, P. Mróz, R. Poleski, J. Skowron, M. K. Szymanski, I. Soszynski, P. Pietrukowicz, S. Kozlowski, K. Ulaczyk, K. A. Rybicki, P. Iwanek, M. Wrona, M. Gromadzki, F. AbeR. Barry, D. P. Bennett, A. Bhattacharya, A. Fukui, H. Fujii, Y. Hirao, Y. Itow, R. Kirikawa, I. Kondo, N. Koshimoto, Y. Matsubara, S. Matsumoto, S. Miyazaki, Y. Muraki, G. Olmschenk, C. Ranc, A. Okamura, N. J. Rattenbury, Y. Satoh, T. Sumi, D. Suzuki, S. Ishitani Silva, T. Toda, P. J. Tristram, A. Vandorou, H. Yama, C. A. Beichman, G. Bryden, S. Calchi Novati, S. Carey, B. S. Gaudi, A. Gould, C. B. Henderson, S. Johnson, Y. Shvartzvald, W. Zhu, M. Dominik, M. Hundertmark, U. G. Jørgensen, P. Longa-Peña, J. Skottfelt, J. Tregloan-Reed, N. Bach-Møller, M. Burgdorf, G. D'Ago, L. Haikala, J. Hitchcock, E. Khalouei, N. Peixinho, S. Rahvar, C. Snodgrass, J. Southworth, P. Spyratos, W. Zang, H. Yang, S. Mao, E. Bachelet, D. Maoz, R. A. Street, Y. Tsapras, G. W. Christie, T. Cooper, L. De Almeida, J. D. Do Nascimento, J. Green, C. Han, S. Hennerley, A. Marmont, J. McCormick, L. A.G. Monard, T. Natusch, R. Pogge

^*Corresponding author for this work

School of Physics and Astronomy

Research output: Contribution to journal › Article › peer-review

4 Scopus citations

Abstract

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.

Original language	English
Article number	A100
Journal	Astronomy and Astrophysics
Volume	663
DOIs	https://doi.org/10.1051/0004-6361/202243490
State	Published - 1 Jul 2022

Funding

Funders	Funder number
Japan Society for the Promotion of Science	20J20633
Japan Society for the Promotion of Science

Keywords

Binaries: general
Brown dwarfs
Gravitational lensing: micro
Stars: low-mass

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10.1051/0004-6361/202243490

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Herald, A., Udalski, A., Bozza, V., Rota, P., Bond, I. A., Yee, J. C., Sajadian, S., Mróz, 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., ... Pogge, R. (2022). Precision measurement of a brown dwarf mass in a binary system in the microlensing event: OGLE-2019-BLG-0033/MOA-2019-BLG-035. Astronomy and Astrophysics, 663, Article A100. https://doi.org/10.1051/0004-6361/202243490

@article{427f1a3b32ee44ac85b7432eaf1a63bb,

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

abstract = "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.",

keywords = "Binaries: general, Brown dwarfs, Gravitational lensing: micro, Stars: low-mass",

author = "A. Herald and A. Udalski and V. Bozza and P. Rota and Bond, {I. A.} and Yee, {J. C.} and S. Sajadian and P. Mr{\'o}z and R. Poleski and J. Skowron and Szymanski, {M. K.} and I. Soszynski and P. Pietrukowicz and S. Kozlowski and K. Ulaczyk and Rybicki, {K. A.} and P. Iwanek and M. Wrona and M. Gromadzki and F. Abe and R. Barry and Bennett, {D. P.} and A. Bhattacharya and A. Fukui and H. Fujii and Y. Hirao and Y. Itow and R. Kirikawa and I. Kondo and N. Koshimoto and Y. Matsubara and S. Matsumoto and S. Miyazaki and Y. Muraki and G. Olmschenk and C. Ranc and A. Okamura and Rattenbury, {N. J.} and Y. Satoh and T. Sumi and D. Suzuki and Silva, {S. Ishitani} and T. Toda and Tristram, {P. J.} and A. Vandorou and H. Yama and Beichman, {C. A.} and G. Bryden and Novati, {S. Calchi} and S. Carey and Gaudi, {B. S.} and A. Gould and Henderson, {C. B.} and S. Johnson and Y. Shvartzvald and W. Zhu and M. Dominik and M. Hundertmark and J{\o}rgensen, {U. G.} and P. Longa-Pe{\~n}a and J. Skottfelt and J. Tregloan-Reed and N. Bach-M{\o}ller and M. Burgdorf and G. D'Ago and L. Haikala and J. Hitchcock and E. Khalouei and N. Peixinho and S. Rahvar and C. Snodgrass and J. Southworth and P. Spyratos and W. Zang and H. Yang and S. Mao and E. Bachelet and D. Maoz and Street, {R. A.} and Y. Tsapras and Christie, {G. W.} and T. Cooper and {De Almeida}, L. and {Do Nascimento}, {J. D.} and J. Green and C. Han and S. Hennerley and A. Marmont and J. McCormick and Monard, {L. A.G.} and T. Natusch and R. Pogge",

note = "Publisher Copyright: {\textcopyright} ",

year = "2022",

month = jul,

day = "1",

doi = "10.1051/0004-6361/202243490",

language = "אנגלית",

volume = "663",

journal = "Astronomy and Astrophysics",

issn = "0004-6361",

publisher = "EDP Sciences",

}

Herald, A, Udalski, A, Bozza, V, Rota, P, Bond, IA, Yee, JC, Sajadian, S, Mróz, P, Poleski, R, Skowron, J, Szymanski, MK, Soszynski, I, Pietrukowicz, P, Kozlowski, S, Ulaczyk, K, Rybicki, KA, Iwanek, P, Wrona, M, Gromadzki, M, Abe, F, Barry, R, Bennett, DP, 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, NJ, Satoh, Y, Sumi, T, Suzuki, D, Silva, SI, Toda, T, Tristram, PJ, Vandorou, A, Yama, H, Beichman, CA, Bryden, G, Novati, SC, Carey, S, Gaudi, BS, Gould, A, Henderson, CB, Johnson, S, Shvartzvald, Y, Zhu, W, Dominik, M, Hundertmark, M, Jørgensen, UG, Longa-Peña, P, Skottfelt, J, Tregloan-Reed, J, Bach-Møller, N, Burgdorf, M, D'Ago, G, Haikala, L, Hitchcock, J, Khalouei, E, Peixinho, N, Rahvar, S, Snodgrass, C, Southworth, J, Spyratos, P, Zang, W, Yang, H, Mao, S, Bachelet, E, Maoz, D, Street, RA, Tsapras, Y, Christie, GW, Cooper, T, De Almeida, L, Do Nascimento, JD, Green, J, Han, C, Hennerley, S, Marmont, A, McCormick, J, Monard, LAG, Natusch, T & Pogge, R 2022, 'Precision measurement of a brown dwarf mass in a binary system in the microlensing event: OGLE-2019-BLG-0033/MOA-2019-BLG-035', Astronomy and Astrophysics, vol. 663, A100. https://doi.org/10.1051/0004-6361/202243490

TY - JOUR

T1 - Precision measurement of a brown dwarf mass in a binary system in the microlensing event

T2 - 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 - Mróz, 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 - Novati, S. Calchi

AU - Carey, S.

AU - Gaudi, B. S.

AU - Gould, A.

AU - Henderson, C. B.

AU - Johnson, S.

AU - Shvartzvald, Y.

AU - Zhu, W.

AU - Dominik, M.

AU - Hundertmark, M.

AU - Jørgensen, U. G.

AU - Longa-Peña, P.

AU - Skottfelt, J.

AU - Tregloan-Reed, J.

AU - Bach-Møller, N.

AU - Burgdorf, M.

AU - D'Ago, G.

AU - Haikala, L.

AU - Hitchcock, J.

AU - Khalouei, E.

AU - Peixinho, N.

AU - Rahvar, S.

AU - Snodgrass, C.

AU - Southworth, J.

AU - Spyratos, P.

AU - Zang, W.

AU - Yang, H.

AU - Mao, S.

AU - Bachelet, E.

AU - Maoz, D.

AU - Street, R. A.

AU - Tsapras, Y.

AU - Christie, G. W.

AU - Cooper, T.

AU - De Almeida, L.

AU - Do Nascimento, J. D.

AU - Green, J.

AU - Han, C.

AU - Hennerley, S.

AU - Marmont, A.

AU - McCormick, J.

AU - Monard, L. A.G.

AU - Natusch, T.

AU - Pogge, R.

PY - 2022/7/1

Y1 - 2022/7/1

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 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.

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 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.

KW - Binaries: general

KW - Brown dwarfs

KW - Gravitational lensing: micro

KW - Stars: low-mass

UR - http://www.scopus.com/inward/record.url?scp=85134703427&partnerID=8YFLogxK

U2 - 10.1051/0004-6361/202243490

DO - 10.1051/0004-6361/202243490

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AN - SCOPUS:85134703427

SN - 0004-6361

VL - 663

JO - Astronomy and Astrophysics

JF - Astronomy and Astrophysics

M1 - A100

ER -

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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