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Evidence for the Direct Detection of the Thermal Spectrum of the Non-Transiting Hot Gas Giant HD 88133 b

Piskorz, Danielle and Benneke, Björn and Crockett, Nathan R. and Lockwood, Alexandra C. and Blake, Geoffrey A. and Barman, Travis S. and Bender, Chad F. and Bryan, Marta L. and Carr, John S. and Fischer, Debra A. and Howard, Andrew W. and Isaacson, Howard and Johnson, John A. (2016) Evidence for the Direct Detection of the Thermal Spectrum of the Non-Transiting Hot Gas Giant HD 88133 b. Astrophysical Journal, 832 (2). Art. No. 131. ISSN 0004-637X. https://resolver.caltech.edu/CaltechAUTHORS:20161123-092049528

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Abstract

We target the thermal emission spectrum of the non-transiting gas giant HD 88133 b with high-resolution near-infrared spectroscopy, by treating the planet and its host star as a spectroscopic binary. For sufficiently deep summed flux observations of the star and planet across multiple epochs, it is possible to resolve the signal of the hot gas giant's atmosphere compared to the brighter stellar spectrum, at a level consistent with the aggregate shot noise of the full data set. To do this, we first perform a principal component analysis to remove the contribution of the Earth's atmosphere to the observed spectra. Then, we use a cross-correlation analysis to tease out the spectra of the host star and HD 88133 b to determine its orbit and identify key sources of atmospheric opacity. In total, six epochs of Keck NIRSPEC L-band observations and three epochs of Keck NIRSPEC K-band observations of the HD 88133 system were obtained. Based on an analysis of the maximum likelihood curves calculated from the multi-epoch cross-correlation of the full data set with two atmospheric models, we report the direct detection of the emission spectrum of the non-transiting exoplanet HD 88133 b and measure a radial projection of the Keplerian orbital velocity of 40 ± 15 km s^(−1), a true mass of 1.02^(+0.61)_(-0.28)M_J, a nearly face-on orbital inclination of 15^(+6o)_(-5), and an atmosphere opacity structure at high dispersion dominated by water vapor. This, combined with 11 years of radial velocity measurements of the system, provides the most up-to-date ephemeris for HD 88133.


Item Type:Article
Related URLs:
URLURL TypeDescription
http://dx.doi.org/10.3847/0004-637X/832/2/131DOIArticle
http://iopscience.iop.org/article/10.3847/0004-637X/832/2/131/metaPublisherArticle
https://arxiv.org/abs/1609.09074arXivDiscussion Paper
ORCID:
AuthorORCID
Piskorz, Danielle0000-0003-4451-2342
Benneke, Björn0000-0001-5578-1498
Crockett, Nathan R.0000-0002-6586-7591
Blake, Geoffrey A.0000-0003-0787-1610
Barman, Travis S.0000-0002-7129-3002
Bender, Chad F.0000-0003-4384-7220
Bryan, Marta L.0000-0002-6076-5967
Carr, John S.0000-0002-6695-3977
Fischer, Debra A.0000-0003-2221-0861
Howard, Andrew W.0000-0001-8638-0320
Isaacson, Howard0000-0002-0531-1073
Additional Information:© 2016 The American Astronomical Society. Received 2016 May 20; revised 2016 September 9; accepted 2016 September 27; published 2016 November 23. The authors would like to thank Heather Knutson for helpful discussions throughout the preparation of this manuscript. The authors wish to recognize and acknowledge the very significant cultural role and reverence that the summit of Maunakea has always had within the indigenous Hawaiian community. We are most fortunate to have the opportunity to conduct observations from this mountain. The data presented herein were obtained at the W.M. Keck Observatory, which is operated as a scientific partnership among the California Institute of Technology, the University of California, and the National Aeronautics and Space Administration. The Observatory was made possible by the generous financial support of the W.M. Keck Foundation. This work was partially supported by funding from the NSF Astronomy & Astrophysics and NASA Exoplanets Research Programs (grants AST-1109857 and NNX16AI14G, G.A. Blake P.I.), and the Center for Exoplanets and Habitable Worlds, which is supported by the Pennsylvania State Unviersity, the Eberly College of Science, and the Pennsylvania Space Grant Consortium. Basic research in infrared astrophysics at the Naval Research Laboratory is supported by 6.1 base funding. Finally, we thank an anonymous reviewer for helpful insights which improved the content of this paper.
Funders:
Funding AgencyGrant Number
W. M. Keck FoundationUNSPECIFIED
NSFAST-1109857
NASANNX16AI14G
Pennsylvania State UnviersityUNSPECIFIED
Eberly College of ScienceUNSPECIFIED
Pennsylvania Space Grant ConsortiumUNSPECIFIED
Naval Research Laboratory6.1 Base funding
Subject Keywords:planets and satellites: atmospheres – techniques: spectroscopic
Issue or Number:2
Record Number:CaltechAUTHORS:20161123-092049528
Persistent URL:https://resolver.caltech.edu/CaltechAUTHORS:20161123-092049528
Official Citation:Danielle Piskorz et al 2016 ApJ 832 131
Usage Policy:No commercial reproduction, distribution, display or performance rights in this work are provided.
ID Code:72276
Collection:CaltechAUTHORS
Deposited By: Tony Diaz
Deposited On:23 Nov 2016 18:29
Last Modified:14 Oct 2019 22:45

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