The California-Kepler Survey. I. High-resolution Spectroscopy of 1305 Stars Hosting Kepler Transiting Planets

By E. Petigura, Andrew W. Howard, G. Marcy, J. Johnson, H. Isaacson, Phillip Cargile, L. Hebb, B. Fulton, L. Weiss, Timothy Morton and 5 more. 2017

260 citations recorded by the source corpus.

The California-Kepler Survey (CKS) is an observational program developed to improve our knowledge of the properties of stars found to host transiting planets by NASA’s Kepler Mission. The improvement stems from new high-resolution optical spectra obtained using HIRES at the W. M. Keck Observatory. The CKS stellar sample comprises 1305 stars classified as Kepler objects of interest, hosting a total of 2075 transiting planets. The primary sample is magnitude-limited ( ) and contains 960 stars with 1385 planets. The sample was extended to include some fainter stars that host multiple planets, ultra-short period planets, or habitable zone planets. The spectroscopic parameters were determined with two different codes, one based on template matching and the other on direct spectral synthesis using radiative transfer. We demonstrate a precision of 60 K in , 0.10 dex in , 0.04 dex in , and 1.0 in . In this paper, we describe the CKS project and present a uniform catalog of spectroscopic parameters. Subsequent papers in this series present catalogs of derived stellar properties such as mass, radius, and age; revised planet properties; and statistical explorations of the ensemble. CKS is the largest survey to determine the properties of Kepler stars using a uniform set of high-resolution, high signal-to-noise ratio spectra. The HIRES spectra are available to the community for independent analyses.

Subfields: Astronomy and Astrophysics, Instrumentation

View Paper: https://www.semanticscholar.org/paper/bcf249b1e8ece9c10ff68050187a01c6d015732a

How researchers see this paper

The researchers whose trusted networks rank it highest, strongest advocate first. Every researcher gets a different order.

In Astronomy and Astrophysics

1. J. Owen
2. E. Petigura
3. B. Fulton
4. Timothy Morton
5. Yanqin Wu
6. Andrew W. Howard
7. E. Gaidos
8. D. Huber

In Instrumentation

1. J. Owen
2. Timothy Morton
3. E. Petigura
4. B. Fulton
5. E. Gaidos
6. Andrew W. Howard
7. G. Marcy
8. J. Johnson

Citations in the corpus

• About 30% of Sun-like Stars Have Kepler-like Planetary Systems: A Study of Their Intrinsic Architecture (2018, background): “Sun-like stars from the California Kepler Survey (Petigura et al. 2017), which give us 150 planet pairs to constrain the inclination dispersion σi,5.”
• An asteroseismic view of the radius valley: stripped cores, not born rocky (2017, unknown): “Recently, Fulton et al. (2017) provided clear evidence of the valley by using a spectroscopic sample from the CaliforniaKepler Survey (CKS), with better-constrained stellar parameters (Petigura et al. 2017; Johnson et al. 2017).”
• The California-Kepler Survey. IV. Metal-rich Stars Host a Greater Diversity of Planets (2017, background): “Around 20 sub-Saturns have well-measured masses from either RVs or TTVs (see Petigura et al. 2017a for a recent compilation).”
• Identifying Exoplanets with Deep Learning: A Five-planet Resonant Chain around Kepler-80 and an Eighth Planet around Kepler-90 (2017, methodology): “We imposed Gaussian priors on the two limb-darkening coefficients, centered at values predicted by Claret & Bloemen (2011) for the host stars (using spectroscopic parameters from MacDonald et al. 2016 for Kepler-80, and parameters from Petigura et al. 2017 for Kepler-90).”
• The Evaporation Valley in the Kepler Planets (2017, methodology): “Recently, the California-Kepler Survey (CKS), using spectroscopic follow-up of a large (1305) sample of planet hosting Kepler stars (Petigura et al. 2017) refined the planet parameters for 2025 Kepler planets, and reduced the typical planetary radius error to ∼ 10% (Johnson et al. 2017).”
• The California-Kepler Survey. II. Precise Physical Properties of 2025 Kepler Planets and Their Host Stars (2017, methodology): “The CKS project and goals are described in detail in Paper I of this series (Petigura et al. 2017).”
• Core-powered mass-loss and the radius distribution of small exoplanets (2017, methodology): “E-mail: sivan.ginzburg@mail.huji.ac.il Recently, refined radius measurements by the California-Kepler Survey (Johnson et al. 2017; Petigura et al. 2017) allowed Fulton et al. (2017) to identify a distinct valley in the radius distribution of short-period planets.”
• Atmospheric Escape and the Evolution of Close-In Exoplanets (2018, methodology): “The California-Kepler-Survey used spectroscopic follow-up of exoplanet host stars to reduce the uncertainty in the stellar radius and associated planetary radii (Petigura et al. 2017; Johnson et al. 2017) to ∼ 10%.”
• The California-Kepler Survey. III. A Gap in the Radius Distribution of Small Planets (2017, methodology): “Here, we examine a sample of planets orbiting stars with precisely measured radii from the California-Kepler Survey (CKS; see Petigura et al. (2017) and Johnson et al. (2017)).”
• Revised Radii of Kepler Stars and Planets Using Gaia Data Release 2 (2018, methodology): “These uncertainties contained Teff offsets between different methods, which are typically less than 150 K (see Table 7 and Teff comparison plots in Petigura et al. 2017).”