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SCExAO AND GPI Y JH BAND PHOTOMETRY AND INTEGRAL FIELD SPECTROSCOPY OF THE YOUNG BROWN DWARF COMPANION TO HD 1160

2017; IOP Publishing; Volume: 834; Issue: 2 Linguagem: Inglês

10.3847/1538-4357/834/2/162

1538-4357

E. Victor Garcia, Thayne Currie, Olivier Guyon, Keivan G. Stassun, Nemanja Jovanović, Julien Lozi, Tomoyuki Kudo, D. Doughty, Josh Schlieder, Jungmi Kwon, Taichi Uyama, Masayuki Kuzuhara, J. Carson, Takao Nakagawa, Jun Hashimoto, Nobuhiko Kusakabe, L. Abe, W. Brandner, Timothy D. Brandt, M. Feldt, Miwa Goto, C. A. Grady, Yutaka Hayano, Masahiko Hayashi, Saeko S. Hayashi, Thomas Henning, K. W. Hodapp, Miki Ishii, Masanori Iye, M. Janson, Ryo Kandori, G. R. Knapp, Taro Matsuo, Michael W. McElwain, Shoken M. Miyama, J. I. Morino, Amaya Moro‐Martín, T. Nishimura, Tae‐Soo Pyo, Eugene Serabyn, Takuya Suenaga, Hiroshi Suto, Ryuji Suzuki, Yasuhiro Takahashi, Hideki Takami, M. Takami, N. Takato, Hiroshi Terada, C. Thalmann, Edwin L. Turner, Makoto Watanabe, John P. Wisniewski, Tōru Yamada, Tomonori Usuda, Motohide Tamura,

Astronomy and Astrophysical Research

We present high signal-to-noise ratio, precise $YJH$ photometry and $Y$ band (\gpiwave~$\mu$m) 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 having an effective temperature of 3000--3100 $K$, a surface gravity of log $g$ = 4--4.5, a radius of~\bestfitradius~$R_{\rm J}$, and a luminosity of log $L$/$L_{\odot} = -2.76 \pm 0.05$. Neither the primary's Hertzspring-Russell diagram position nor atmospheric modeling of HD 1160 B show evidence for a sub-solar metallicity. The interpretation of the HD 1160 B depends on which stellar system components are used to estimate an 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 $M_{\rm J}$). If we consider HD 1160 A alone, younger ages (20--125 Myr) and a brown dwarf-like mass (35--90 $M_{\rm J}$) 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.