Detection of Water Vapor in the Thermal Spectrum of the Non-transiting Hot Jupiter Upsilon Andromedae b
Abstract
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.
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.Attached Files
Published - Piskorz_2017_AJ_154_78.pdf
Submitted - 1707.01534.pdf
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Additional details
- Eprint ID
- 79664
- Resolver ID
- CaltechAUTHORS:20170801-091325018
- W. M. Keck Foundation
- AST-1109857
- NSF
- NNX16AI14G
- NASA
- 6.1 Base funding
- Naval Research Laboratory
- Created
-
2017-08-01Created from EPrint's datestamp field
- Updated
-
2021-11-15Created from EPrint's last_modified field
- Caltech groups
- Astronomy Department, Division of Geological and Planetary Sciences