Johnson, John Asher and Petigura, Erik A. and Fulton, Benjamin J. and Marcy, Geoffrey W. and Howard, Andrew W. and Isaacson, Howard and Hebb, Leslie and Cargile, Phillip A. and Morton, Timothy D. and Weiss, Lauren M. and Winn, Joshua N. and Rogers, Leslie A. and Sinukoff, Evan and Hirsch, Lea A. (2017) The California-Kepler Survey. II. Precise Physical Properties of 2025 Kepler Planets and Their Host Stars. Astronomical Journal, 154 (3). Art. No. 108. ISSN 1538-3881. doi:10.3847/1538-3881/aa80e7. https://resolver.caltech.edu/CaltechAUTHORS:20170621-093412676
![[img]](https://authors.library.caltech.edu/style/images/fileicons/application_pdf.png) |
PDF
- Published Version
See Usage Policy. 2MB |
|
PDF
- Submitted Version
See Usage Policy. 3MB |
Use this Persistent URL to link to this item: https://resolver.caltech.edu/CaltechAUTHORS:20170621-093412676
Abstract
We present stellar and planetary properties for 1305 Kepler Objects of Interest (KOIs) hosting 2025 planet candidates observed as part of the California-Kepler Survey. We combine spectroscopic constraints, presented in Paper I, with stellar interior modeling to estimate stellar masses, radii, and ages. Stellar radii are typically constrained to 11%, compared to 40% when only photometric constraints are used. Stellar masses are constrained to 4%, and ages are constrained to 30%. We verify the integrity of the stellar parameters through comparisons with asteroseismic studies and Gaia parallaxes. We also recompute planetary radii for 2025 planet candidates. Because knowledge of planetary radii is often limited by uncertainties in stellar size, we improve the uncertainties in planet radii from typically 42% to 12%. We also leverage improved knowledge of stellar effective temperature to recompute incident stellar fluxes for the planets, now precise to 21%, compared to a factor of two when derived from photometry.
| Item Type: | Article | ||||||||||||||||||||||||||||
|---|---|---|---|---|---|---|---|---|---|---|---|---|---|---|---|---|---|---|---|---|---|---|---|---|---|---|---|---|---|
| Related URLs: |
| ||||||||||||||||||||||||||||
| ORCID: |
| ||||||||||||||||||||||||||||
| Additional Information: | © 2017 American Astronomical Society. Received 2017 March 30; revised 2017 June 2; accepted 2017 June 14; published 2017 August 24. The CKS project was conceived, planned, and initiated by AWH, GWM, JAJ, HTI, and TDM. AWH, GWM, JAJ acquired Keck telescope time to conduct the magnitude-limited survey. Keck time for the other stellar samples was acquired by JNW, LAR, and GWM. The observations were coordinated by HTI and AWH and carried out by AWH, HTI, GWM, JAJ, TDM, BJF, LMW, EAP, ES, and LAH. AWH secured CKS project funding. SpecMatch was developed and run by EAP and SME@XSEDE was developed and run by LH and PAC. EAP computed derived planetary and stellar properties with assistance from BJF. This manuscript was largely written by EAP with significant assistance from AWH, GWM, and BJF. We thank Jason Rowe, Dan Huber, and Jeff Valenti for helpful conversations and Roberto Sanchis-Ojeda for his work on the Ultra-Short Period planet sample. We thank the many observers who contributed to the measurements reported here. We gratefully acknowledge the efforts and dedication of the Keck Observatory staff, especially Randy Campbell, Scott Dahm, Greg Doppmann, Marc Kassis, Jim Lyke, Hien Tran, Josh Walawender, Greg Wirth for support of HIRES and of remote observing. Most of the data presented here are based on spectra 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 NASA. We are grateful to the time assignment committees of the University of Hawaii, the University of California, the California Institute of Technology, and NASA for their generous allocations of observing time that enabled this large project. Kepler was competitively selected as the tenth NASA Discovery mission. Funding for this mission is provided by the NASA Science Mission Directorate. We thank the, the Kepler Science Office, the Science Operations Center, Threshold Crossing Event Review Team (TCERT), and the Followup Observations Program (FOP) Working Group for their work on all steps in the planet discovery process ranging from selecting target stars and pointing the Kepler telescope to developing and running the photometric pipeline to curating and refining the catalogs of Kepler planets. E. A. P. acknowledges support from Hubble Fellowship grant HST-HF2-51365.001-A awarded by the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Inc. for NASA under contract NAS 5-26555. A. W. H. acknowledges NASA grant NNX12AJ23G. P. A. C. acknowledges National Science Foundation grant AST-1109612. T. D. M. acknowledges NASA grant NNX14AE11G. P. A. C. acknowledges National Science Foundation grant AST-1109612. L. H. acknowledges National Science Foundation grant AST-1009810. L. M. W. acknowledges support from Gloria and Ken Levy and from the the Trottier Family. E. S. is supported by a post-graduate scholarship from the Natural Sciences and Engineering Research Council of Canada. This work made use of the SIMBAD database (operated at CDS, Strasbourg, France), NASA’s Astrophysics Data System Bibliographic Services, and the NASA Exoplanet Archive, which is operated by the California Institute of Technology, under contract with the National Aeronautics and Space Administration under the Exoplanet Exploration Program. Finally, 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. Facilities: Keck:I (HIRES), Kepler. | ||||||||||||||||||||||||||||
| Group: | Infrared Processing and Analysis Center (IPAC), Astronomy Department | ||||||||||||||||||||||||||||
| Funders: |
| ||||||||||||||||||||||||||||
| Subject Keywords: | planets and satellites: fundamental parameters – planets and satellites: general – stars: abundances – stars: fundamental parameters – techniques: spectroscopic | ||||||||||||||||||||||||||||
| Issue or Number: | 3 | ||||||||||||||||||||||||||||
| DOI: | 10.3847/1538-3881/aa80e7 | ||||||||||||||||||||||||||||
| Record Number: | CaltechAUTHORS:20170621-093412676 | ||||||||||||||||||||||||||||
| Persistent URL: | https://resolver.caltech.edu/CaltechAUTHORS:20170621-093412676 | ||||||||||||||||||||||||||||
| Official Citation: | John Asher Johnson et al 2017 AJ 154 108 | ||||||||||||||||||||||||||||
| Usage Policy: | No commercial reproduction, distribution, display or performance rights in this work are provided. | ||||||||||||||||||||||||||||
| ID Code: | 78401 | ||||||||||||||||||||||||||||
| Collection: | CaltechAUTHORS | ||||||||||||||||||||||||||||
| Deposited By: | Ruth Sustaita | ||||||||||||||||||||||||||||
| Deposited On: | 21 Jun 2017 17:44 | ||||||||||||||||||||||||||||
| Last Modified: | 15 Nov 2021 17:39 |
Repository Staff Only: item control page
