Issue |
A&A
Volume 663, July 2022
|
|
---|---|---|
Article Number | A100 | |
Number of page(s) | 13 | |
Section | Planets and planetary systems | |
DOI | https://doi.org/10.1051/0004-6361/202243490 | |
Published online | 19 July 2022 |
Precision measurement of a brown dwarf mass in a binary system in the microlensing event
OGLE-2019-BLG-0033/MOA-2019-BLG-035★
1
Dipartimento di Fisica e Astronomia “Galileo Galilei”, Università di Padova,
Vicolo dell’Osservatorio 3,
Padova
35122, Italy
2
Observatory, University of Warsaw,
Al. Ujazdowskie 4,
00-478
Warszawa, Poland
3
Dipartimento di Fisica “E.R. Caianiello”, Università degli studi di Salerno,
Via Giovanni Paolo II 132,
84084
Fisciano (SA), Italy
e-mail: valboz@sa.infn.it
4
Istituto Nazionale di Fisica Nucleare, Sezione di Napoli,
Via Cintia,
80126
Napoli (NA), Italy
5
School of Mathematical and Computational Sciences, Massey University,
Auckland
0745, New Zealand
6
Center for Astrophysics, Harvard & Smithsonian,
60 Garden St.,
Cambridge, MA
02138, USA
7
Department of Physics, Isfahan University of Technology,
Isfahan, Iran
8
Department of Physics, University of Warwick,
Gibbet Hill Road,
Coventry
CV4 7AL, UK
9
Institute for Space-Earth Environmental Research, Nagoya University,
Nagoya
464-8601, Japan
10
Code 667,
NASA Goddard Space Flight Center,
Greenbelt, MD
20771, USA
11
Department of Astronomy, University of Maryland,
College Park, MD
20742, USA
12
Department of Earth and Planetary Science, Graduate School of Science, The University of Tokyo,
7-3-1 Hongo, Bunkyo-ku,
Tokyo
113-0033, Japan
13
Instituto de Astrofísica de Canarias,
Vía Láctea s/n,
38205
La Laguna, Tenerife, Spain
14
Department of Earth and Space Science, Graduate School of Science, Osaka University,
Toyonaka, Osaka
560-0043, Japan
15
Zentrum für Astronomie der Universität Heidelberg, Astronomisches Rechen-Institut,
Mönchhofstr. 12–14,
69120
Heidelberg, Germany
16
Department of Physics, University of Auckland,
Private Bag 92019,
Auckland, New Zealand
17
Department of Physics, The Catholic University of America,
Washington, DC
20064, USA
18
University of Canterbury Mt. John Observatory,
PO Box 56,
Lake Tekapo
8770, New Zealand
19
IPAC,
Mail Code 100-22, Caltech, 1200 E. California Blvd.,
Pasadena, CA
91125, USA
20
Jet Propulsion Laboratory, California Institute of Technology,
4800 Oak Grove Drive,
Pasadena, CA
91109, USA
21
Department of Astronomy, Ohio State University,
140 W. 18th Ave.,
Columbus, OH
43210, USA
22
Max-Planck-Institute for Astronomy,
Königstuhl 17,
69117
Heidelberg, Germany
23
Department of Particle Physics and Astrophysics, Weizmann Institute of Science,
Rehovot
76100, Israel
24
Department of Astronomy, Tsinghua University,
Beijing
100084, PR China
25
Centre for Exoplanet Science, SUPA, School of Physics & Astronomy, University of St Andrews,
North Haugh,
St Andrews
KY16 9SS, UK
26
Centre for ExoLife Sciences, Niels Bohr Institute,
Øster Voldgade 5,
1350
Copenhagen, Denmark
27
Unidad de Astronomía, Universidad de Antofagasta,
Av. Angamos 601,
Antofagasta, Chile
28
Centre for Electronic Imaging, Department of Physical Sciences, The Open University,
Milton Keynes
MK7 6AA, UK
29
Instituto de Astronomía y Ciencias Planetarias, Universidad de Atacama,
Avenida Copayapu 485,
Copiapó, Atacama, Chile
30
Universität Hamburg, Faculty of Mathematics, Informatics and Natural Sciences, Department of Earth Sciences, Meteorological Institute,
Bundesstrasse 55,
20146
Hamburg, Germany
31
Instituto de Astrofísica Pontificia Universidad Católica de Chile,
Avenida Vicuna Mackenna 4860,
Macul, Santiago, Chile
32
Department of Physics, Sharif University of Technology,
PO Box 11155-9161
Tehran, Iran
33
Institute for Astronomy, University of Edinburgh, Royal Observatory,
Edinburgh
EH9 3HJ, UK
34
Astrophysics Group, Keele University,
Staffordshire
ST5 5BG, UK
35
National Astronomical Observatories, Chinese Academy of Sciences,
Beijing
100101, PR China
36
Las Cumbres Observatory,
6740 Cortona Drive, suite 102,
Goleta, CA
93117, USA
37
School of Physics and Astronomy, Tel-Aviv University,
Tel-Aviv
6997801, Israel
38
Auckland Observatory,
Auckland, New Zealand
39
Kumeu Observatory,
Kumeu, New Zealand
40
Universidade Federal do Rio Grande do Norte (UFRN), Departamento de Fśica,
59078-970
Natal, RN, Brazil
41
Laboratório Nacional de Astrofísica,
Rua Estados Unidos 154,
37504-364
Itajubá - MG, Brazil
42
Department of Physics, Chungbuk National University,
Cheongju
28644, Republic of Korea
43
Farm Cove Observatory, Centre for Backyard Astrophysics,
Pakuranga, Auckland, New Zealand
44
Klein Karoo Observatory, Centre for Backyard Astrophysics,
Calitzdorp, South Africa
45
Institute for Radio Astronomy and Space Research (IRASR), AUT University,
Auckland, New Zealand
Received:
7
March
2022
Accepted:
3
April
2022
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.
Key words: gravitational lensing: micro / binaries: general / brown dwarfs / stars: low-mass
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
© ESO 2022
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