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Kepler-15b: A Hot Jupiter Enriched in Heavy Elements and the First Kepler Mission Planet Confirmed with the Hobby-Eberly Telescope

Endl, Michael and Ciardi, David R. (2011) Kepler-15b: A Hot Jupiter Enriched in Heavy Elements and the First Kepler Mission Planet Confirmed with the Hobby-Eberly Telescope. Astrophysical Journal Supplement Series, 197 (1). p. 13. ISSN 0067-0049. https://resolver.caltech.edu/CaltechAUTHORS:20111212-121337008

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Abstract

We report the discovery of Kepler-15b (KOI-128), a new transiting exoplanet detected by NASA's Kepler mission. The transit signal with a period of 4.94 days was detected in the quarter 1 (Q1) Kepler photometry. For the first time, we have used the High Resolution Spectrograph (HRS) at the Hobby-Eberly Telescope (HET) to determine the mass of a Kepler planet via precise radial velocity (RV) measurements. The 24 HET/HRS RVs and 6 additional measurements from the Fibre-fed Échelle Spectrograph spectrograph at the Nordic Optical Telescope reveal a Doppler signal with the same period and phase as the transit ephemeris. We used one HET/HRS spectrum of Kepler-15 taken without the iodine cell to determine accurate stellar parameters. The host star is a metal-rich ([Fe/H] = 0.36 ± 0.07) G-type main-sequence star with T_eff = 5515 ± 124 K. The semi-amplitude K of the RV orbit is 78.7^(+8.5)_(–9.5) m s^(–1), which yields a planet mass of 0.66 ± 0.1 M_Jup. The planet has a radius of 0.96 ± 0.06 R_Jup and a mean bulk density of 0.9 ± 0.2 g cm^(–3). The radius of Kepler-15b is smaller than the majority of transiting planets with similar mass and irradiation level. This suggests that the planet is more enriched in heavy elements than most other transiting giant planets. For Kepler-15b we estimate a heavy element mass of 30-40 M_⊕.


Item Type:Article
Related URLs:
URLURL TypeDescription
http://dx.doi.org/10.1088/0067-0049/197/1/13DOIArticle
http://iopscience.iop.org/0067-0049/197/1/13PublisherArticle
ORCID:
AuthorORCID
Ciardi, David R.0000-0002-5741-3047
Additional Information:© 2011 American Astronomical Society. Received 2011 July 8; accepted 2011 October 18; published 2011 November 4. Based on observations obtained with the Hobby–Eberly Telescope, which is a joint project of the University of Texas at Austin, the Pennsylvania State University, Stanford University, Ludwig-Maximilians-Universität München, and Georg-August-Universität Göttingen. Funding for this Discovery mission is provided by NASA’s Science Mission Directorate. We thank the hundreds of people who make this mission successful. The Hobby–Eberly Telescope (HET) is a joint project of the University of Texas at Austin, the Pennsylvania State University, Stanford University, Ludwig-Maximilians-Universität München, and Georg-August-Universität Göttingen. The HET is named in honor of its principal benefactors, William P. Hobby and Robert E. Eberly. Based in part on observations made with the Nordic Optical Telescope, operated on the island of La Palma jointly by Denmark, Finland, Iceland, Norway, and Sweden, in the Spanish Observatorio del Roque de los Muchachos of the Instituto de Astrofisica de Canarias. We also thank the anonymous referee for many helpful suggestions to improve the manuscript.
Group:Infrared Processing and Analysis Center (IPAC)
Funders:
Funding AgencyGrant Number
NASAUNSPECIFIED
Subject Keywords:planetary systems; stars: individual (Kepler-15, KOI-128, KIC 11359879, 2MASS J19444814+4908244); techniques: image processing; techniques: photometric; techniques: radial velocities; techniques: spectroscopic
Issue or Number:1
Record Number:CaltechAUTHORS:20111212-121337008
Persistent URL:https://resolver.caltech.edu/CaltechAUTHORS:20111212-121337008
Official Citation:Kepler-15b: A Hot Jupiter Enriched in Heavy Elements and the First Kepler Mission Planet Confirmed with the Hobby-Eberly Telescope Michael Endl et al. 2011 ApJS 197 13
Usage Policy:No commercial reproduction, distribution, display or performance rights in this work are provided.
ID Code:28423
Collection:CaltechAUTHORS
Deposited By: Jason Perez
Deposited On:22 Dec 2011 15:27
Last Modified:03 Oct 2019 03:32

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