Herald, A. and Udalski, A. and Bozza, V. and Rota, P. and Bond, I. A. and Yee, J. C. and Sajadian, S. and Mróz, P. and Poleski, R. and Skowron, J. and Szymanski, M. K. and Soszyński, I. and Pietrukowicz, P. and Kozłowski, S. and Ulaczyk, K. and Rybicki, K. A. and Iwanek, P. and Wrona, M. and Gromadzki, M. and Abe, F. and Barry, R. and Bennett, D. P. and Bhattacharya, A. and Fukui, A. and Fujii, H. and Hirao, Y. and Itow, Y. and Kirikawa, R. and Kondo, I. and Koshimoto, N. and Matsubara, Y. and Matsumoto, S. and Miyazaki, S. and Muraki, Y. and Olmschenk, G. and Ranc, C. and Okamura, A. and Rattenbury, N. J. and Satoh, Y. and Sumi, T. and Suzuki, D. and Ishitani Silva, S. and Toda, T. and Tristram, P. J. and Vandorou, A. and Yamamoto, H. and Beichman, C. A. and Bryden, G. and Calchi Novati, S. and Carey, S. and Gaudi, B. S. and Gould, A. and Henderson, C. B. and Johnson, S. and Shvartzvald, Y. and Zhu, W. and Dominik, M. and Hundertmark, M. and Jørgensen, U. G. and Longa-Peña, P. and Skottfelt, J. and Tregloan-Reed, J. and Bach-Møller, N. and Burgdorf, M. and D’Ago, G. and Haikala, L. and Hitchcock, J. and Khalouei, E. and Peixinho, N. and Rahvar, S. and Snodgrass, C. and Southworth, J. and Spyratos, P. and Zang, W. and Yang, H. and Mao, S. and Bachelet, E. and Maoz, D. and Street, R. A. and Tsapras, Y. and Christie, G. W. and Cooper, T. and de Almeida, L. and do Nascimento, J.-D. and Green, J. and Han, C. and Hennerley, S. and Marmont, A. and McCormick, J. and Monard, L. A. G. and Natusch, T. and 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 . Art. No. A100. ISSN 0004-6361. doi:10.1051/0004-6361/202243490. https://resolver.caltech.edu/CaltechAUTHORS:20220721-8768000
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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.
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| Alternate Title: | Precision measurement of a brown dwarf mass in a binary system in the microlensing event OGLE-2019-BLG-0033/MOA-2019-BLG-035 | ||||||||||||||||||||||||||||||||||||
| Additional Information: | © ESO 2022. Received: 7 March 2022 Accepted: 3 April 2022. 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 J.C.Y. was supported by JPL grant 1571564. This work has made use of data from the European Space Agency (ESA) mission Gaia (https://www. cosmos.esa.int/gaia), processed by the Gaia Data Processing and Analysis Consortium (DPAC, https://www.cosmos.esa.int/web/gaia/dpac/consortium). Funding for the DPAC has been provided by national institutions, in particular the institutions participating in the Gaia Multilateral Agreement. This work uses observations made at the Observatorio do Pico dos Dias/LNA (Brazil). The lightcurves are only available at the CDS via anonymous ftp to cdsarc.u-strasbg.fr (130.79.128.5) or via http://cdsarc.u-strasbg.fr/viz-bin/cat/J/A+A/663/A100 | ||||||||||||||||||||||||||||||||||||
| Group: | Infrared Processing and Analysis Center (IPAC) | ||||||||||||||||||||||||||||||||||||
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| Subject Keywords: | gravitational lensing: micro / binaries: general / brown dwarfs / stars: low-mass | ||||||||||||||||||||||||||||||||||||
| DOI: | 10.1051/0004-6361/202243490 | ||||||||||||||||||||||||||||||||||||
| Record Number: | CaltechAUTHORS:20220721-8768000 | ||||||||||||||||||||||||||||||||||||
| Persistent URL: | https://resolver.caltech.edu/CaltechAUTHORS:20220721-8768000 | ||||||||||||||||||||||||||||||||||||
| Official Citation: | 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. Szymański, I. Soszyński, P. Pietrukowicz, S. Kozłowski, K. Ulaczyk, K. A. Rybicki, P. Iwanek, M. Wrona, M. Gromadzki, (The OGLE collaboration), 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, (The MOA collaboration), C. A. Beichman, G. Bryden, S. Calchi Novati, S. Carey, B. S. Gaudi, A. Gould, C. B. Henderson, S. Johnson, Y. Shvartzvald, W. Zhu, (The Spitzer team), 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, (The MiNDSTEp consortium), 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 and (The LCO & μFUN collaboration) A&A, 663 (2022) A100 DOI: https://doi.org/10.1051/0004-6361/202243490 | ||||||||||||||||||||||||||||||||||||
| Usage Policy: | No commercial reproduction, distribution, display or performance rights in this work are provided. | ||||||||||||||||||||||||||||||||||||
| ID Code: | 115742 | ||||||||||||||||||||||||||||||||||||
| Collection: | CaltechAUTHORS | ||||||||||||||||||||||||||||||||||||
| Deposited By: | George Porter | ||||||||||||||||||||||||||||||||||||
| Deposited On: | 22 Jul 2022 19:49 | ||||||||||||||||||||||||||||||||||||
| Last Modified: | 08 Aug 2022 20:46 |
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