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Published January 10, 2017 | Published + Accepted Version
Journal Article Open

SCExAO and GPI YJH Band Photometry and Integral Field Spectroscopy of the Young Brown Dwarf Companion to HD 1160


We present high signal-to-noise ratio, precise Y JH photometry and Y band (0.957–1.120 μm) spectroscopy of HD 1160 B, a young substellar companion discovered from the Gemini NICI Planet Finding Campaign using the Subaru Coronagraphic Extreme Adaptive Optics instrument and the Gemini Planet Imager. HD 1160 B has typical mid-M dwarf-like infrared colors and a spectral type of M5.5^(+1.0)_(-0.5), where the blue edge of our Y band spectrum rules out earlier spectral types. Atmospheric modeling suggests HD 1160 B has an effective temperature of 3000–3100 K, a surface gravity of log g = 4–4.5, a radius of 1.55 ± 0.10 R_J, and a luminosity of log L/L⊙ = −2.76 ± 0.05. Neither the primary's Hertzspring–Russell diagram position nor atmospheric modeling of HD 1160 B show evidence for a subsolar metallicity. Interpretation of the HD 1160 B spectroscopy depends on which stellar system components are used to estimate the age. Considering HD 1160 A, B and C jointly, we derive an age of 80–125 Myr, implying that HD 1160 B straddles the hydrogen-burning limit (70–90 M_J). If we consider HD 1160 A alone, younger ages (20–125 Myr) and a brown dwarf-like mass (35–90 MJ) are possible. Interferometric measurements of the primary, a precise Gaia parallax, and moderate-resolution spectroscopy can better constrain the system's age and how HD 1160 B fits within the context of (sub)stellar evolution.

Additional Information

© 2017 The American Astronomical Society. Received 2016 June 24; revised 2016 October 12; accepted 2016 October 16; published 2017 January 11. We thank Anna-Lise Marie for detailed, helpful discussions about and access to SPHERE HD 1160 B spectra. We thank Eric Mamajek for discussions about the metallicity of nearby, young stars. We thank Davy Kirkpatrick for providing NIR spectra of M-dwarf spectral standards. We thank Federico Spada for discussions and tests of the Yonsei-Yale models. EVG would like to acknowledge the gracious support of his Lowell Pre-doctoral Fellowship by the BF foundation and the excellent support of Fisk-Vanderbilt Bridge Program. This research has made use of the SIMBAD database, operated at CDS, Strasbourg, France. This research has made use of the Keck Observatory Archive (KOA), which is operated by the W. M. Keck Observatory and the NASA Exoplanet Science Institute (NExScI), under contract with the National Aeronautics and Space Administration. The authors acknowledge support from the JSPS (Grant-in-Aid for Research #23103002, #23340051, and #26220704). This work was partially supported by the Grant-in-Aid for JSPS fellows (Grant Number 25-8826). M.J. acknowledges support of the U.S. National Science Foundation, under Award No. 1009203. This work performed under the auspices of the U.S. Department of Energy by Lawrence Livermore National Laboratory under Contract DE-AC52-07NA27344 with document release number LLNL-JRNL-701012-DRAFT. We wish to acknowledge the pivotal cultural role and reverence that the summit of Maunakea has always had within the indigenous Hawaiian community. We are most fortunate to have the privilege to conduct scientific observations from this mountain.

Attached Files

Published - Garcia_2017_ApJ_834_162.pdf

Accepted Version - 1610.05786.pdf


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