TY - JOUR
T1 - Surveying nearby brown dwarfs with HGCA: direct imaging discovery of a faint, high-mass brown dwarf orbiting HD 176535 A
AU - Li, Yiting
AU - Brandt, Timothy D.
AU - Brandt, G. Mirek
AU - An, Qier
AU - Franson, Kyle
AU - Dupuy, Trent J.
AU - Chen, Minghan
AU - Bowens-Rubin, Rachel
AU - Lewis, Briley L.
AU - Bowler, Brendan P.
AU - Gibbs, Aidan
AU - Kiman, Rocio
AU - Faherty, Jacqueline
AU - Currie, Thayne
AU - Jensen-Clem, Rebecca
AU - Zhang, Hengyue
AU - Contreras-Martinez, Ezequiel
AU - Fitzgerald, Michael P.
AU - Mazin, Benjamin A.
AU - Millar-Blanchaer, Maxwell
N1 - Funding Information:
This research has made use of the KOA, which is operated by the WMKO and the NExScI, under contract with the National Aeronautics and Space Administration. This work presents results from the European Space Agency (ESA) space mission Gaia. Gaia data are being processed by the Gaia Data Processing and Analysis Consortium (DPAC). Funding for the DPAC is provided by national institutions, in particular the institutions participating in the Gaia MultiLateral Agreement (MLA). The Gaia mission website is https://www.cosmos.esa.int/gaia . The Gaia archive website is https://archives.esac.esa.int/gaia . TDB gratefully acknowledges support from the Alfred P. Sloan Foundation and from the NASA Exoplanet Research Program under grant #80NSSC18K0439. BLL acknowledges support from the National Science Foundation Graduate Research Fellowship under Grant No. 2021-25 DGE-2034835. Any opinions, findings, and conclusions or recommendations expressed in this material are those of the authors(s) and do not necessarily reflect the views of the National Science Foundation. BPB acknowledges support from the NASA Exoplanet Research Program grant 20-XRP20_2-0119 and the Alfred P. Sloan Foundation. RK acknowledges the support by the National Science Foundation under Grant No. NSF PHY-1748958. We thank the Heising Simons Foundation for the support.
Funding Information:
This research has made use of the KOA, which is operated by the WMKO and the NExScI, under contract with the National Aeronautics and Space Administration. This work presents results from the European Space Agency (ESA) space mission Gaia. Gaia data are being processed by the Gaia Data Processing and Analysis Consortium (DPAC). Funding for the DPAC is provided by national institutions, in particular the institutions participating in the Gaia MultiLateral Agreement (MLA). The Gaia mission website is https://www.cosmos.esa.int/gaia. The Gaia archive website is https://archives.esac.esa.int/gaia. TDB gratefully acknowledges support from the Alfred P. Sloan Foundation and from the NASA Exoplanet Research Program under grant #80NSSC18K0439. BLL acknowledges support from the National Science Foundation Graduate Research Fellowship under Grant No. 2021-25 DGE-2034835. Any opinions, findings, and conclusions or recommendations expressed in this material are those of the authors(s) and do not necessarily reflect the views of the National Science Foundation. BPB acknowledges support from the NASA Exoplanet Research Program grant 20-XRP20 2-0119 and the Alfred P. Sloan Foundation. RK acknowledges the support by the National Science Foundation under Grant No. NSF PHY-1748958. We thank the Heising Simons Foundation for the support.
Publisher Copyright:
© 2023 The Author(s) Published by Oxford University Press on behalf of Royal Astronomical Society.
PY - 2023/7/1
Y1 - 2023/7/1
N2 - Brown dwarfs with well-measured masses, ages, and luminosities provide direct benchmark tests of substellar formation and evolutionary models. We report the first results from a direct imaging survey aiming to find and characterize substellar companions to nearby accelerating stars with the assistance of the Hipparcos-Gaia Catalog of Accelerations (HGCA). In this paper, we present a joint high-contrast imaging and astrometric discovery of a substellar companion to HD 176535 A, a K3.5V main-sequence star aged approximately 3.59+−10.8715s Gyr at a distance of 36.99 ± 0.03 pc. In advance of our high-contrast imaging observations, we combined precision High Accuracy Radial velocity Planet Searcher (HARPS) Radial Velocities (RVs) and HGCA astrometry to predict the potential companion's location and mass. We thereafter acquired two nights of KeckAO/NIRC2 direct imaging observations in the L' band, which revealed a companion with a contrast of ΔL'p = 9.20 ± 0.06 mag at a projected separation of ≈0.35 arcsec (≈13 au) from the host star. We revise our orbital fit by incorporating our dual-epoch relative astrometry using the open-source Markov chain Monte Carlo orbit fitting code ORVARA. We obtain a dynamical mass of 65.9+−12.07MJup that places HD 176535 B firmly in the brown dwarf regime. HD 176535 B is a new benchmark dwarf useful for constraining the evolutionary and atmospheric models of high-mass brown dwarfs. We found a luminosity of log(Lbol/L⊙) = −5.26 ± 0.07 and a model-dependent effective temperature of 980 ± 35 K for HD 176535 B. We infer HD 176535 B to be a T dwarf from its mass, age, and luminosity. Our dynamical mass suggests that some substellar evolutionary models may be underestimating luminosity for high-mass T dwarfs. Given its angular separation and luminosity, HD 176535 B would make a promising candidate for Aperture Masking Interferometry with JWST and GRAVITY/Keck Planet Imager and Characterizer, and further spectroscopic characterization with instruments like the CHARIS/SCExAO/Subaru integral field spectrograph.
AB - Brown dwarfs with well-measured masses, ages, and luminosities provide direct benchmark tests of substellar formation and evolutionary models. We report the first results from a direct imaging survey aiming to find and characterize substellar companions to nearby accelerating stars with the assistance of the Hipparcos-Gaia Catalog of Accelerations (HGCA). In this paper, we present a joint high-contrast imaging and astrometric discovery of a substellar companion to HD 176535 A, a K3.5V main-sequence star aged approximately 3.59+−10.8715s Gyr at a distance of 36.99 ± 0.03 pc. In advance of our high-contrast imaging observations, we combined precision High Accuracy Radial velocity Planet Searcher (HARPS) Radial Velocities (RVs) and HGCA astrometry to predict the potential companion's location and mass. We thereafter acquired two nights of KeckAO/NIRC2 direct imaging observations in the L' band, which revealed a companion with a contrast of ΔL'p = 9.20 ± 0.06 mag at a projected separation of ≈0.35 arcsec (≈13 au) from the host star. We revise our orbital fit by incorporating our dual-epoch relative astrometry using the open-source Markov chain Monte Carlo orbit fitting code ORVARA. We obtain a dynamical mass of 65.9+−12.07MJup that places HD 176535 B firmly in the brown dwarf regime. HD 176535 B is a new benchmark dwarf useful for constraining the evolutionary and atmospheric models of high-mass brown dwarfs. We found a luminosity of log(Lbol/L⊙) = −5.26 ± 0.07 and a model-dependent effective temperature of 980 ± 35 K for HD 176535 B. We infer HD 176535 B to be a T dwarf from its mass, age, and luminosity. Our dynamical mass suggests that some substellar evolutionary models may be underestimating luminosity for high-mass T dwarfs. Given its angular separation and luminosity, HD 176535 B would make a promising candidate for Aperture Masking Interferometry with JWST and GRAVITY/Keck Planet Imager and Characterizer, and further spectroscopic characterization with instruments like the CHARIS/SCExAO/Subaru integral field spectrograph.
KW - astrometry
KW - methods: data analysis
KW - techniques: high angular resolution
KW - techniques: image processing
UR - http://www.scopus.com/inward/record.url?scp=85161536308&partnerID=8YFLogxK
U2 - 10.1093/mnras/stad1315
DO - 10.1093/mnras/stad1315
M3 - Article
AN - SCOPUS:85161536308
SN - 0035-8711
VL - 522
SP - 5622
EP - 5637
JO - Monthly Notices of the Royal Astronomical Society
JF - Monthly Notices of the Royal Astronomical Society
IS - 4
ER -