High signal-to-noise spectral characterization of the planetary-mass object HD 106906 b *, **

Daemgen, Sebastian; Todorov, Kamen; Quanz, Sascha P.; Meyer, Michael R.; Mordasini, Christoph; Marleau, Gabriel-Dominique; Fortney, Jonathan J. (2017). High signal-to-noise spectral characterization of the planetary-mass object HD 106906 b *, **. Astronomy and astrophysics, 608(A71), A71. EDP Sciences 10.1051/0004-6361/201731527

Preview

Text Mordasini_High signal-to-noise spectral characterization of the planetary-mass object HD 106906 b.pdf - Published Version Available under License Publisher holds Copyright. Download (2MB) | Preview

Context.
Directly imaged planets are ideal candidates for spectroscopic characterization of their atmospheres. The angular separations that are typically close to their host stars, however, reduce the achievable contrast and thus signal-to-noise ratios (S/N).
Aims.
We spectroscopically characterize the atmosphere of HD 106906 b, which is a young low-mass companion near the deuterium burning limit. The wide separation from its host star of 7.1′′ makes it an ideal candidate for high S/N and high-resolution spectroscopy.
We aim to derive new constraints on the spectral type, effective temperature, and luminosity of HD 106906 b and also to provide a high S/N template spectrum for future characterization of extrasolar planets.
Methods. We obtained 1.1–2.5μm integral field spectroscopy with the VLT/SINFONI instrument with a spectral resolution of R≈2000–4000. New estimates of the parameters of HD 106906 b are derived by analyzing spectral features, comparing the extracted
spectra to spectral catalogs of other low-mass objects, and fitting with theoretical isochrones.
Results. We identify several spectral absorption lines that are consistent with a low mass for HD 106906 b. We derive a new spectral type of L1.5±1.0, which is one subclass earlier than previous estimates. Through comparison with other young low-mass objects, this translates to a luminosity of log(L/L⊙)=−3.65±0.08 and an effective temperature of Teff=
1820±240 K. Our new mass estimates range between M=11.9+1.7−0.8MJup (hot start) and M=14.0+0.2−0.5 MJup (cold start). These limits take into account a possibly finite
formation time, i.e., HD 106906 b is allowed to be 0–3 Myr younger than its host star. We exclude accretion onto HD 106906 b at rates M>4.8×10⁻¹⁰ MJup yr⁻¹ based on the fact that we observe no hydrogen (Paschen-β, Brackett-γ) emission. This is indicative of little or no circumplanetary gas. With our new observations , HD 106906 b is the planetary-mass object with one of the highest S/N spectra yet. We make the spectrum available for future comparison with data from existing and next-generation (e.g., ELT and JWST) spectrographs.

Interest & Impact

Downloads

178 since deposited on 18 Apr 2018
12 in the past 12 months

Citations

5 Citations in Web of Science ®
6 Citations in Scopus

Search

in Google Scholar™

Services

Actions (login required)

Edit item

Actions (login required)

Edit item