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OGLE-2013-BLG-0911Lb: A Secondary on the Brown-dwarf Planet Boundary around an M Dwarf

Miyazaki, Shota and Shvartzvald, Yossi and Mróz, P. and Calchi Novati, S. and D’Ago, G. (2020) OGLE-2013-BLG-0911Lb: A Secondary on the Brown-dwarf Planet Boundary around an M Dwarf. Astronomical Journal, 159 (2). Art. No. 76. ISSN 1538-3881. https://resolver.caltech.edu/CaltechAUTHORS:20200131-135216215

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Abstract

We present the analysis of the binary-lens microlensing event OGLE-2013-BLG-0911. The best-fit solutions indicate the binary mass ratio of q 0.03, which differs from that reported in Shvartzvald et al. The event suffers from the well-known close/wide degeneracy, resulting in two groups of solutions for the projected separation normalized by the Einstein radius of s ~ 0.15 or s ~ 7. The finite source and the parallax observations allow us to measure the lens physical parameters. The lens system is an M dwarf orbited by a massive Jupiter companion at very close (M_(host) = 0.30^(+0.08)_(-0.06)M⊙, M_(comp) = 10.1^(+2.9)_(-2.2)M_(Jup), a_(exp) = 0.40^(+0.05)_(-0.04) au) or wide (M_(host) = 0.28^(+0.10)_(-0.08) M⊙, M_(comp) = 9.9^(+3.8)_(-3.5)M_(Jup), a(exp) = 18.0^(+3.8)_(3.5) au) separation. Although the mass ratio is slightly above the planet-brown dwarf (BD) mass-ratio boundary of q = 0.03, which is generally used, the median physical mass of the companion is slightly below the planet-BD mass boundary of 13M_(Jup). It is likely that the formation mechanisms for BDs and planets are different and the objects near the boundaries could have been formed by either mechanism. It is important to probe the distribution of such companions with masses of ~13M_(Jup) in order to statistically constrain the formation theories for both BDs and massive planets. In particular, the microlensing method is able to probe the distribution around low-mass M dwarfs and even BDs, which is challenging for other exoplanet detection methods.


Item Type:Article
Related URLs:
URLURL TypeDescription
https://doi.org/10.3847/1538-3881/ab64deDOIArticle
https://arxiv.org/abs/1912.09613arXivDiscussion Paper
ORCID:
AuthorORCID
Miyazaki, Shota0000-0001-9818-1513
Shvartzvald, Yossi0000-0003-1525-5041
Mróz, P.0000-0001-7016-1692
Calchi Novati, S.0000-0002-7669-1069
Additional Information:© 2020 The American Astronomical Society. Received 2019 October 17; revised 2019 December 18; accepted 2019 December 19; published 2020 January 31. We would like to thank the anonymous referee who helped to greatly improve our paper. The OGLE project has received funding from the National Science Centre, Poland, grant MAESTRO 2014/14/A/ST9/00121 to A.U. CITEUC is funded by National Funds through FCT—Foundation for Science and Technology (project: UID/Multi/00611/2013) and FEDER—European Regional Development Fund through COMPETE 2020—Operational Programme Competitiveness and Internationalization (project: POCI-01-0145-FEDER-006922). D.P.B., A.B., and D.S. were supported by NASA through grant NASA-NNX12AF54G. Work by C.R. was supported by an appointment to the NASA Postdoctoral Program at the Goddard Space Flight Center, administered by USRA through a contract with NASA. Work by N.K. is supported by JSPS KAKENHI grant No. JP15J01676. Work by Y.H. is supported by JSPS KAKENHI grant No. JP1702146. N.J.R. is a Royal Society of New Zealand Rutherford Discovery Fellow. This work was supported by JSPS KAKENHI grant No. JP17H02871. This research was supported by the I-CORE program of the Planning and Budgeting Committee and the Israel Science Foundation, grant 1829/12. D.M. acknowledges support by the U.S.-Israel Binational Science Foundation. Work by C.H. was supported by the grant (2017R1A4A1015178) of National Research Foundation of Korea. Work by W.Z., Y.K.J., and A.G. was supported by AST1516842 from the US NSF. W.Z., I.G.S., and A.G. were supported by JPL grant 1500811. Y.T. acknowledges the support of DFG priority program SPP 1992 "Exploring the Diversity of Extrasolar Planets" (WA 1047/11-1). K.H. acknowledges support from STFC grant ST/R000824/1.
Group:Infrared Processing and Analysis Center (IPAC)
Funders:
Funding AgencyGrant Number
National Science Centre (Poland)MAESTRO 2014/14/A/ST9/00121
Fundação para a Ciência e a Tecnologia (FCT)UID/Multi/00611/2013
Fundação para a Ciência e a Tecnologia (FCT)COMPETE 2020
Fondo Europeo de Desarrollo Regional (FEDER)POCI-01-0145-FEDER-006922
NASANNX12AF54G
NASA Postdoctoral ProgramUNSPECIFIED
Japan Society for the Promotion of Science (JSPS)JP15J01676
Japan Society for the Promotion of Science (JSPS)JP1702146
Royal SocietyUNSPECIFIED
Japan Society for the Promotion of Science (JSPS)JP17H02871
I-CORE Program of the Planning and Budgeting CommitteeUNSPECIFIED
Israel Science Foundation1829/12
Binational Science Foundation (USA-Israel)UNSPECIFIED
National Research Foundation of Korea2017R1A4A1015178
NSFAST-1516842
JPL1500811
Deutsche Forschungsgemeinschaft (DFG)SPP 1992
Deutsche Forschungsgemeinschaft (DFG)WA 1047/11-1
Science and Technology Facilities Council (STFC)ST/R000824/1
Subject Keywords:Gravitational microlensing; Exoplanet astronomy; Brown dwarfs; Exoplanet systems; Exoplanets; Extrasolar gas giants; Exoplanet detection methods; M dwarf stars
Issue or Number:2
Classification Code:Unified Astronomy Thesaurus concepts: Gravitational microlensing (672); Exoplanet astronomy (486); Brown dwarfs (185); Exoplanet systems (484); Exoplanets (498); Extrasolar gas giants (509); Exoplanet detection methods (489); M dwarf stars (982)
Record Number:CaltechAUTHORS:20200131-135216215
Persistent URL:https://resolver.caltech.edu/CaltechAUTHORS:20200131-135216215
Official Citation:Shota Miyazaki et al 2020 AJ 159 76
Usage Policy:No commercial reproduction, distribution, display or performance rights in this work are provided.
ID Code:101039
Collection:CaltechAUTHORS
Deposited By: Tony Diaz
Deposited On:31 Jan 2020 22:13
Last Modified:07 Feb 2020 18:52

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