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. Mroz; 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. Jorgensen; P. Longa-Pena; 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., Jr 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. Mroz, 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. Jorgensen, P. Longa-Pena, 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., Jr do Nascimento, J. Green, C. Han, S. Hennerley, A. Marmont, J. McCormick, L. A. G. Monard, T. Natusch, R. Pogge

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

Abstract

Context. Brown dwarfs are poorly understood transition objects between stars and planets, with several competing mechanisms having been proposed for their formation. Mass measurements are generally difficult for isolated objects but also for brown dwarfs orbiting low-mass stars, which are often too faint for spectroscopic follow-up. Aims. Microlensing provides an alternative tool for the discovery and investigation of such faint systems. Here we present the analysis of the microlensing event OGLE-2019-BLG-0033/MOA-2019-BLG-035, which is due to 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 parallax, source radius and orbital motion of the binary lens. Results. After accurate modeling, we find that the lens is composed of a red dwarf with mass M₁ = 0.149 ± 0.010M⊙ and a brown dwarf with mass M₂ = 0.0463 ± 0.0031M⊙, 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. Percent precision in the mass measurement of brown dwarfs has been achieved only in a few microlensing events up to now, but will likely become common with the Roman space telescope.

Original language	English
Article number	A100
Number of pages	13
Journal	Astronomy & Astrophysics
Volume	633
Early online date	19 Jul 2022
DOIs	https://doi.org/10.1051/0004-6361/202243490
Publication status	Published - Jul 2022

Keywords

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

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10.1051/0004-6361/202243490

Herald-2022-Precision-measurement-of-A&A-633-A100
Copyright © ESO 2022. This work has been made available online in accordance with publisher policies or with permission. Permission for further reuse of this content should be sought from the publisher or the rights holder. This is the author created accepted manuscript following peer review and may differ slightly from the final published version. The final published version of this work is available at https://doi.org/10.1051/0004-6361/202243490.
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H2020 MSCA ITN EJD 2019: H2020 MSCA ITN EJD 2019 CHAMELEON
Helling, C. (PI)
European Commission
1/06/20 → 31/05/24
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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., ... 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 & Astrophysics, 633, Article A100. https://doi.org/10.1051/0004-6361/202243490

@article{268d2c9fad69450696585f3518be8def,

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 poorly understood transition objects between stars and planets, with several competing mechanisms having been proposed for their formation. Mass measurements are generally difficult for isolated objects but also for brown dwarfs orbiting low-mass stars, which are often too faint for spectroscopic follow-up. Aims. Microlensing provides an alternative tool for the discovery and investigation of such faint systems. Here we present the analysis of the microlensing event OGLE-2019-BLG-0033/MOA-2019-BLG-035, which is due to 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 parallax, source radius and orbital motion of the binary lens. Results. After accurate modeling, we find that the lens is composed of a red dwarf with mass M1 = 0.149 ± 0.010M⊙ and a brown dwarf with mass M2 = 0.0463 ± 0.0031M⊙, 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. Percent precision in the mass measurement of brown dwarfs has been achieved only in a few microlensing events up to now, but will likely become common with the Roman space telescope.",

keywords = "Gravitational lensing: micro, Binaries: general, Brown dwarfs, 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. Mroz 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 {Ishitani Silva}, S. and T. Toda and Tristram, {P. J.} and A. Vandorou and H. Yama and Beichman, {C. A.} and G. Bryden and {Calchi Novati}, S. 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 Jorgensen, {U. G.} and P. Longa-Pena 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., Jr} 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 = "Funding: The MOA project is supported by JSPS KAK-ENHI Grant Number JSPS24253004, JSPS26247023, JSPS23340064, JSPS15H00781, JP16H06287,17H02871 and 19KK0082 and a Royal Society of New Zealand Marsden Grant MFP-MAU1901. U.G.J. acknowledges funding from the European Union H2020-MSCA-ITN-2019 under Grant no. 860470 (CHAMELEON) and from the Novo Nordisk Foundation Interdisciplinary Synergy Program grant no. NNF19OC0057374. W.Zang, W.Zhu, H.Y. and S.M. acknowledge support by the National Science Foundation of China (Grant No. 12133005). This research uses data obtained through the Telescope Access Program (TAP), which has been funded by the TAP member institutes. Work by C.R. was supported by a Research Fellowship of the Alexander von Humboldt Foundation. Work by C.H. was supported by the grants of National Research Foundation of Korea (2020R1A4A2002885 and 2019R1A2C2085965). Work by JCY was supported by JPL grant 1571564. ",

year = "2022",

month = jul,

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

language = "English",

volume = "633",

journal = "Astronomy & Astrophysics",

issn = "0004-6361",

publisher = "EDP SCIENCES S A",

}

Herald, A, Udalski, A, Bozza, V, Rota, P, Bond, IA, Yee, JC, Sajadian, S, Mroz, 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, Ishitani Silva, S, Toda, T, Tristram, PJ, Vandorou, A, Yama, H, Beichman, CA, Bryden, G, Calchi Novati, S, Carey, S, Gaudi, BS, Gould, A, Henderson, CB, Johnson, S, Shvartzvald, Y, Zhu, W, Dominik, M, Hundertmark, M, Jorgensen, UG, Longa-Pena, 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, J-DJ, 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 & Astrophysics, vol. 633, 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 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 - Ishitani Silva, S.

AU - Toda, T.

AU - Tristram, P. J.

AU - Vandorou, A.

AU - Yama, H.

AU - Beichman, C. A.

AU - Bryden, G.

AU - Calchi Novati, S.

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 - Jorgensen, U. G.

AU - Longa-Pena, 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., Jr

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.

N1 - Funding: The MOA project is supported by JSPS KAK-ENHI Grant Number JSPS24253004, JSPS26247023, JSPS23340064, JSPS15H00781, JP16H06287,17H02871 and 19KK0082 and a Royal Society of New Zealand Marsden Grant MFP-MAU1901. U.G.J. acknowledges funding from the European Union H2020-MSCA-ITN-2019 under Grant no. 860470 (CHAMELEON) and from the Novo Nordisk Foundation Interdisciplinary Synergy Program grant no. NNF19OC0057374. W.Zang, W.Zhu, H.Y. and S.M. acknowledge support by the National Science Foundation of China (Grant No. 12133005). This research uses data obtained through the Telescope Access Program (TAP), which has been funded by the TAP member institutes. Work by C.R. was supported by a Research Fellowship of the Alexander von Humboldt Foundation. Work by C.H. was supported by the grants of National Research Foundation of Korea (2020R1A4A2002885 and 2019R1A2C2085965). Work by JCY was supported by JPL grant 1571564.

PY - 2022/7

Y1 - 2022/7

N2 - Context. Brown dwarfs are poorly understood transition objects between stars and planets, with several competing mechanisms having been proposed for their formation. Mass measurements are generally difficult for isolated objects but also for brown dwarfs orbiting low-mass stars, which are often too faint for spectroscopic follow-up. Aims. Microlensing provides an alternative tool for the discovery and investigation of such faint systems. Here we present the analysis of the microlensing event OGLE-2019-BLG-0033/MOA-2019-BLG-035, which is due to 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 parallax, source radius and orbital motion of the binary lens. Results. After accurate modeling, we find that the lens is composed of a red dwarf with mass M1 = 0.149 ± 0.010M⊙ and a brown dwarf with mass M2 = 0.0463 ± 0.0031M⊙, 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. Percent precision in the mass measurement of brown dwarfs has been achieved only in a few microlensing events up to now, but will likely become common with the Roman space telescope.

AB - Context. Brown dwarfs are poorly understood transition objects between stars and planets, with several competing mechanisms having been proposed for their formation. Mass measurements are generally difficult for isolated objects but also for brown dwarfs orbiting low-mass stars, which are often too faint for spectroscopic follow-up. Aims. Microlensing provides an alternative tool for the discovery and investigation of such faint systems. Here we present the analysis of the microlensing event OGLE-2019-BLG-0033/MOA-2019-BLG-035, which is due to 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 parallax, source radius and orbital motion of the binary lens. Results. After accurate modeling, we find that the lens is composed of a red dwarf with mass M1 = 0.149 ± 0.010M⊙ and a brown dwarf with mass M2 = 0.0463 ± 0.0031M⊙, 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. Percent precision in the mass measurement of brown dwarfs has been achieved only in a few microlensing events up to now, but will likely become common with the Roman space telescope.

KW - Gravitational lensing: micro

KW - Binaries: general

KW - Brown dwarfs

KW - Stars: low mass

U2 - 10.1051/0004-6361/202243490

DO - 10.1051/0004-6361/202243490

M3 - Article

SN - 0004-6361

VL - 633

JO - Astronomy & Astrophysics

JF - Astronomy & 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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Keywords

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H2020 MSCA ITN EJD 2019: H2020 MSCA ITN EJD 2019 CHAMELEON

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