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Characterizing 51 Eri b from 1 to 5 μm: A Partly Cloudy Exoplanet

Rajan, Abhijith and Patel, Rahul I. (2017) Characterizing 51 Eri b from 1 to 5 μm: A Partly Cloudy Exoplanet. Astronomical Journal, 10 (1). Art. No. 10. ISSN 0004-6256. https://resolver.caltech.edu/CaltechAUTHORS:20170616-120657567

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Abstract

We present spectrophotometry spanning 1–5 μm of 51 Eridani b, a 2–10 M_(Jup) planet discovered by the Gemini Planet Imager Exoplanet Survey. In this study, we present new K1 (1.90–2.19 μm) and K2 (2.10–2.40 μm) spectra taken with the Gemini Planet Imager as well as an updated L_P (3.76 μm) and new M_S (4.67 μm) photometry from the NIRC2 Narrow camera. The new data were combined with J (1.13–1.35 μm) and H (1.50–1.80 μm) spectra from the discovery epoch with the goal of better characterizing the planet properties. The 51 Eri b photometry is redder than field brown dwarfs as well as known young T-dwarfs with similar spectral type (between T4 and T8), and we propose that 51 Eri b might be in the process of undergoing the transition from L-type to T-type. We used two complementary atmosphere model grids including either deep iron/silicate clouds or sulfide/salt clouds in the photosphere, spanning a range of cloud properties, including fully cloudy, cloud-free, and patchy/intermediate-opacity clouds. The model fits suggest that 51 Eri b has an effective temperature ranging between 605 and 737 K, a solar metallicity, and a surface gravity of log(g) = 3.5–4.0 dex, and the atmosphere requires a patchy cloud atmosphere to model the spectral energy distribution (SED). From the model atmospheres, we infer a luminosity for the planet of −5.83 to −5.93 (log L/L_⊙), leaving 51 Eri b in the unique position of being one of the only directly imaged planets consistent with having formed via a cold-start scenario. Comparisons of the planet SED against warm-start models indicate that the planet luminosity is best reproduced by a planet formed via core accretion with a core mass between 15 and 127 M_⊕.


Item Type:Article
Related URLs:
URLURL TypeDescription
https://doi.org/10.3847/1538-3881/aa74dbDOIArticle
http://iopscience.iop.org/article/10.3847/1538-3881/aa74dbPublisherArticle
https://arxiv.org/abs/1705.03887arXivDiscussion Paper
ORCID:
AuthorORCID
Patel, Rahul I.0000-0002-5025-6827
Additional Information:© 2017 American Astronomical Society. Received 2017 March 24. Accepted 2017 May 8. Published 2017 June 16. The authors thank Gabriel Marleau for the discussion on warm-start models. The Gemini Observatory is operated by the AURA under a cooperative agreement with the NSF on behalf of the Gemini partnership: the National Science Foundation (United States), the National Research Council (Canada), CONICYT (Chile), the Australian Research Council (Australia), Ministério da Ciéncia, Tecnologia e Inovaçao (Brazil), and Ministerio de Ciencia, Tecnología e Innovación Productiva (Argentina). This work was supported by NSF grants AST-1411868 (A.R., J.L.P., B.M.), AST-1518332 (R.J.D.R.), and DGE-1311230 (K.W.D.). F.M. and E.N. are supported by NASA Grant NNX14AJ80G. This work was supported by Fonds de Recherche du Québec (J.R., R.D., D.L.). K.M.M. and T.S.B. are supported by the NASA Exoplanets Research Program (XRP) by cooperative agreement NNX16AD44G. G.V. and J.K.W. acknowledge JPL's ESI program for GPI-related funding. The results reported herein benefited from collaborations or information exchange within NASA's Nexus for Exoplanet System Science (NExSS) research coordination network sponsored by NASA's Science Mission Directorate and the NExSS grant NNX15AD95G. Portions of this work were performed under the auspices of the U.S. Department of Energy by Lawrence Livermore National Laboratory under Contract DE-AC52-07NA27344. This research has benefited from the SpeX Prism Library (or SpeX Prism Library Analysis Toolkit) maintained by Adam Burgasser at http://www.browndwarfs.org/spexprism, the IRTF Spectral Library maintained by Michael Cushing, and the Montreal Brown Dwarf and Exoplanet Spectral Library maintained by Jonathan Gagné. Facilities: Gemini:South (GPI), Keck:II (NIRC2). Software: GPI Data Reduction Pipeline (v1.3.0; Perrin et al. 2014), pyKLIP (Wang et al. 2015).
Group:Infrared Processing and Analysis Center (IPAC)
Funders:
Funding AgencyGrant Number
National Research Council of CanadaUNSPECIFIED
Comisión Nacional de Investigación Científica y Tecnológica (CONICYT)UNSPECIFIED
Australian Research CouncilUNSPECIFIED
Ministério da Ciéncia, Tecnologia e InovaçaoUNSPECIFIED
Ministerio de Ciencia, Tecnología e Innovación ProductivaUNSPECIFIED
NSFAST-1411868
NSFAST-1518332
NSFDGE-1311230
NASANNX14AJ80G
Fonds de Recherche du QuébecUNSPECIFIED
NASANNX16AD44G
NASANNX15AD95G
Department of Energy (DOE)DE-AC52-07NA27344
Subject Keywords:instrumentation: adaptive optics; planets and satellites: atmospheres; planets and satellites: composition; planets and satellites: gaseous planets; stars: individual (51 Eridani)
Issue or Number:1
Record Number:CaltechAUTHORS:20170616-120657567
Persistent URL:https://resolver.caltech.edu/CaltechAUTHORS:20170616-120657567
Official Citation:Abhijith Rajan et al 2017 AJ 154 10
Usage Policy:No commercial reproduction, distribution, display or performance rights in this work are provided.
ID Code:78283
Collection:CaltechAUTHORS
Deposited By: Ruth Sustaita
Deposited On:16 Jun 2017 20:29
Last Modified:03 Oct 2019 18:07

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