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Spectral characterization of newly detected young substellar binaries with SINFONI
Stockholm University, Faculty of Science, Department of Astronomy.
Stockholm University, Faculty of Science, Department of Astronomy.
Stockholm University, Faculty of Science, Department of Astronomy.
Number of Authors: 42019 (English)In: Astronomy and Astrophysics, ISSN 0004-6361, E-ISSN 1432-0746, Vol. 627, article id A167Article in journal (Refereed) Published
Abstract [en]

We observe 14 young low-mass substellar objects using the VLT/SINFONI integral field spectrograph with laser guide star adaptive optics to detect and characterize three candidate binary systems. All three binary candidates show strong signs of youth, with two of them likely belonging to young moving groups. Together with the adopted young-moving-group ages we employ isochrones from the BT-Settle CIFIST substellar evolutionary models to estimate individual masses for the binary components. We find 2MASS J15104786-2818174 to be part of the approximate to 30-50 Myr Argus moving group and to be composed of a 34-48 M-Jup primary brown dwarf with spectral type M9 gamma and a fainter 15 22 MJup companion, separated by approximate to 100 mas. 2MASS J22025794-5605087 is identified as an almost equal-mass binary in the AB Dor moving group, with a projected separation of approximate to 60 mas. Both components share spectral type M9 gamma/beta, which with the adopted age of 120 200 Myr yields masses in the range of 50 68 M-Jup for each component individually. The observations of 2MASS J15474719-2423493 are of lower quality and we obtain no spectral characterization for the target, but resolve two components separated by approximate to 170 mas which with the predicted young field age of 30 50 Myr yields individual masses below 20 M-Jup. Out of the three candidate binary systems, 2MASS J22025794-5605087 has unambiguous spectroscopic signs of being a bona-fide binary, while the other two will require second-epoch confirmation. The small projected separations between the binary components correspond to physical separations of approximate to 4-7AU, meaning that astrometric monitoring of just a few years would be adequate to generate constrained orbital fits and dynamical masses for the systems. In combination with their young ages, these binaries will prove to be excellent benchmarks for calibrating substellar evolutionary models down to a very low-mass regime.

Place, publisher, year, edition, pages
2019. Vol. 627, article id A167
Keywords [en]
astrometry, brown dwarfs, binaries: close
National Category
Astronomy, Astrophysics and Cosmology
Identifiers
URN: urn:nbn:se:su:diva-171656DOI: 10.1051/0004-6361/201935319ISI: 000475840500004OAI: oai:DiVA.org:su-171656DiVA, id: diva2:1344669
Available from: 2019-08-21 Created: 2019-08-21 Last updated: 2019-08-21Bibliographically approved

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