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Detection of Water Vapor in the Thermal Spectrum of the Non-transiting Hot Jupiter Upsilon Andromedae 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 Carr, John S. and Johnson, John A. (2017) Detection of Water Vapor in the Thermal Spectrum of the Non-transiting Hot Jupiter Upsilon Andromedae b. Astronomical Journal, 154 (2). Art. No. 78. ISSN 1538-3881.

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The Upsilon Andromedae system was the first multi-planet system discovered orbiting a main-sequence star. We describe the detection of water vapor in the atmosphere of the innermost non-transiting gas giant ups And b by treating the star–planet system as a spectroscopic binary with high-resolution, ground-based spectroscopy. We resolve the signal of the planet's motion and break the mass-inclination degeneracy for this non-transiting planet via deep combined flux observations of the star and the planet. In total, seven epochs of Keck NIRSPEC L band observations, three epochs of Keck NIRSPEC short-wavelength K band observations, and three epochs of Keck NIRSPEC long wavelength K band observations of the ups And system were obtained. We perform a multi-epoch cross-correlation of the full data set with an atmospheric model. We measure the radial projection of the Keplerian velocity (K_P = 55 ± 9 km s−1), true mass (M_b = 1.7^(+0.33)_(-0.24) M_J), and orbital inclination (i_b 24° ± 4°), and determine that the planet's opacity structure is dominated by water vapor at the probed wavelengths. Dynamical simulations of the planets in the ups And system with these orbital elements for ups And b show that stable, long-term (100 Myr) orbital configurations exist. These measurements will inform future studies of the stability and evolution of the ups And system, as well as the atmospheric structure and composition of the hot Jupiter.

Item Type:Article
Related URLs:
URLURL TypeDescription Paper
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
Carr, John S.0000-0002-6695-3977
Johnson, John A.0000-0001-9808-7172
Additional Information:© 2017 The American Astronomical Society. Received 2017 February 22; revised 2017 June 16; accepted 2017 July 2; published 2017 August 1. The authors thank an anonymous reviewer for useful comments and suggestions on this paper. The authors also thank Konstantin Batygin for guidance and insight into the stability of this planetary system and 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 WM 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 WM 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 PI). Basic research in infrared astrophysics at the Naval Research Laboratory is supported by 6.1 base funding.
Group:Astronomy Department
Funding AgencyGrant Number
W. M. Keck FoundationUNSPECIFIED
Naval Research Laboratory6.1 Base funding
Issue or Number:2
Record Number:CaltechAUTHORS:20170801-091325018
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Usage Policy:No commercial reproduction, distribution, display or performance rights in this work are provided.
ID Code:79664
Deposited By: Tony Diaz
Deposited On:01 Aug 2017 17:07
Last Modified:20 Apr 2020 08:47

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