Near-infrared spectroscopy of the Y0 WISEP J173835.52+273258.9 and the Y1 WISE J035000.32–565830.2: The importance of non-equilibrium chemistry
Abstract
Here, we present new near-infrared spectra, obtained at Gemini Observatory, for two Y dwarfs: WISE J035000.32–565830.2 (W0350) and WISEP J173835.52+273258.9 (W1738). A FLAMINGOS-2 R = 540 spectrum was obtained for W0350, covering $$1.0\lt \lambda \;\mu {\rm{m}}$$ $$\lt \;1.7$$, and a cross-dispersed Gemini near-infrared spectrograph R = 2800 spectrum was obtained for W1738, covering 0.993–1.087 μm, 1.191–1.305 μm, 1.589–1.631 μm, and 1.985–2.175 μm, in four orders. We also present revised YJH photometry for W1738, using new NIRI Y and J imaging, and a re-analysis of the previously published NIRI H-band images. We compare these data, together with previously published data for late-T and Y dwarfs, to cloud-free models of solar metallicity, calculated both in chemical equilibrium and with disequilibrium driven by vertical transport. We find that for the Y dwarfs, the non-equilibrium models reproduce the near-infrared data better than the equilibrium models. The remaining discrepancies suggest that fine-tuning the CH4/CO and NH3/N2 balance is needed. Improved trigonometric parallaxes would improve the analysis. Despite the uncertainties and discrepancies, the models reproduce the observed near-infrared spectra well. We find that for the Y0, W1738, $${T}_{{\rm{eff}}}=425\pm 25\;{\rm{K}}$$, and log $$g=4.0\pm 0.25$$, and for the Y1, W0350, $${T}_{{\rm{eff}}}=350\pm 25\;{\rm{K}}$$, and log $$g=4.0\pm 0.25$$. W1738 may be metal-rich. Based on evolutionary models, these temperatures and gravities correspond to a mass range for both Y dwarfs of 3–9 Jupiter masses, with W0350 being a cooler, slightly older, version of W1738; the age of W0350 is 0.3–3 Gyr, and the age of W1738 is 0.15–1 Gyr.
- Authors:
-
- Gemini Observatory, Hilo, HI (United States)
- Maison de la Simulation, CEA-CNRS-INRIA-UPS-UVSQ, USR, Gif-Sur-Yvette (France); Univ. of Exeter, Exeter (United Kingdom)
- Los Alamos National Lab. (LANL), Los Alamos, NM (United States)
- NASA Ames Research Center, Moffett Field, CA (United States)
- Univ. of California, Santa Cruz, CA (United States)
- Univ. of Exeter, Exeter (United Kingdom)
- Univ. of Exeter, Exeter (United Kingdom); Ecole Normale Superieure de Lyon, CRAL, UMR, CNRS, Lyon Cedex (France)
- Publication Date:
- Research Org.:
- Los Alamos National Lab. (LANL), Los Alamos, NM (United States)
- Sponsoring Org.:
- National Aeronautics and Space Administration (NASA); USDOE
- OSTI Identifier:
- 1296684
- Report Number(s):
- LA-UR-16-21256
Journal ID: ISSN 1538-4357
- Grant/Contract Number:
- AC52-06NA25396
- Resource Type:
- Accepted Manuscript
- Journal Name:
- The Astrophysical Journal (Online)
- Additional Journal Information:
- Journal Name: The Astrophysical Journal (Online); Journal Volume: 824; Journal Issue: 1; Journal ID: ISSN 1538-4357
- Publisher:
- Institute of Physics (IOP)
- Country of Publication:
- United States
- Language:
- English
- Subject:
- 79 ASTRONOMY AND ASTROPHYSICS; molecular processes; stars: brown dwarfs; stars: atmospheres; stars: individual (WISE J035000.32-565830.2, WISEP J173835.52+273258.9)
Citation Formats
Leggett, Sandy K., Tremblin, Patrick, Saumon, Didier, Marley, Mark S., Morley, Caroline V., Amundsen, David S., Baraffe, Isabelle, and Chabrier, Gilles. Near-infrared spectroscopy of the Y0 WISEP J173835.52+273258.9 and the Y1 WISE J035000.32–565830.2: The importance of non-equilibrium chemistry. United States: N. p., 2016.
Web. doi:10.3847/0004-637X/824/1/2.
Leggett, Sandy K., Tremblin, Patrick, Saumon, Didier, Marley, Mark S., Morley, Caroline V., Amundsen, David S., Baraffe, Isabelle, & Chabrier, Gilles. Near-infrared spectroscopy of the Y0 WISEP J173835.52+273258.9 and the Y1 WISE J035000.32–565830.2: The importance of non-equilibrium chemistry. United States. https://doi.org/10.3847/0004-637X/824/1/2
Leggett, Sandy K., Tremblin, Patrick, Saumon, Didier, Marley, Mark S., Morley, Caroline V., Amundsen, David S., Baraffe, Isabelle, and Chabrier, Gilles. Fri .
"Near-infrared spectroscopy of the Y0 WISEP J173835.52+273258.9 and the Y1 WISE J035000.32–565830.2: The importance of non-equilibrium chemistry". United States. https://doi.org/10.3847/0004-637X/824/1/2. https://www.osti.gov/servlets/purl/1296684.
@article{osti_1296684,
title = {Near-infrared spectroscopy of the Y0 WISEP J173835.52+273258.9 and the Y1 WISE J035000.32–565830.2: The importance of non-equilibrium chemistry},
author = {Leggett, Sandy K. and Tremblin, Patrick and Saumon, Didier and Marley, Mark S. and Morley, Caroline V. and Amundsen, David S. and Baraffe, Isabelle and Chabrier, Gilles},
abstractNote = {Here, we present new near-infrared spectra, obtained at Gemini Observatory, for two Y dwarfs: WISE J035000.32–565830.2 (W0350) and WISEP J173835.52+273258.9 (W1738). A FLAMINGOS-2 R = 540 spectrum was obtained for W0350, covering $1.0\lt \lambda \;\mu {\rm{m}}$ $\lt \;1.7$, and a cross-dispersed Gemini near-infrared spectrograph R = 2800 spectrum was obtained for W1738, covering 0.993–1.087 μm, 1.191–1.305 μm, 1.589–1.631 μm, and 1.985–2.175 μm, in four orders. We also present revised YJH photometry for W1738, using new NIRI Y and J imaging, and a re-analysis of the previously published NIRI H-band images. We compare these data, together with previously published data for late-T and Y dwarfs, to cloud-free models of solar metallicity, calculated both in chemical equilibrium and with disequilibrium driven by vertical transport. We find that for the Y dwarfs, the non-equilibrium models reproduce the near-infrared data better than the equilibrium models. The remaining discrepancies suggest that fine-tuning the CH4/CO and NH3/N2 balance is needed. Improved trigonometric parallaxes would improve the analysis. Despite the uncertainties and discrepancies, the models reproduce the observed near-infrared spectra well. We find that for the Y0, W1738, ${T}_{{\rm{eff}}}=425\pm 25\;{\rm{K}}$, and log $g=4.0\pm 0.25$, and for the Y1, W0350, ${T}_{{\rm{eff}}}=350\pm 25\;{\rm{K}}$, and log $g=4.0\pm 0.25$. W1738 may be metal-rich. Based on evolutionary models, these temperatures and gravities correspond to a mass range for both Y dwarfs of 3–9 Jupiter masses, with W0350 being a cooler, slightly older, version of W1738; the age of W0350 is 0.3–3 Gyr, and the age of W1738 is 0.15–1 Gyr.},
doi = {10.3847/0004-637X/824/1/2},
journal = {The Astrophysical Journal (Online)},
number = 1,
volume = 824,
place = {United States},
year = {Fri Jun 03 00:00:00 EDT 2016},
month = {Fri Jun 03 00:00:00 EDT 2016}
}
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