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J/ApJ/838/25     Hectochelle spectroscopy for 776 Kepler stars     (Guo+, 2017)

The metallicity distribution and hot Jupiter rate of the Kepler field: Hectochelle high-resolution spectroscopy for 776 Kepler target stars. Guo X., Johnson J.A., Mann A.W., Kraus A.L., Curtis J.L., Latham D.W. <Astrophys. J., 838, 25-25 (2017)> =2017ApJ...838...25G (SIMBAD/NED BibCode)
ADC_Keywords: Abundances ; Spectroscopy ; Effective temperatures ; Photometry ; Stars, double and multiple Keywords: catalogs; methods: statistical; planets and satellites: detection; stars: abundances; stars: fundamental parameters; techniques: imaging spectroscopy Abstract: The occurrence rate of hot Jupiters from the Kepler transit survey is roughly half that of radial velocity surveys targeting solar neighborhood stars. One hypothesis to explain this difference is that the two surveys target stars with different stellar metallicity distributions. To test this hypothesis, we measure the metallicity distribution of the Kepler targets using the Hectochelle multi-fiber, high-resolution spectrograph. Limiting our spectroscopic analysis to 610 dwarf stars in our sample with logg>3.5, we measure a metallicity distribution characterized by a mean of [M/H]mean=-0.045±0.009, in agreement with previous studies of the Kepler field target stars. In comparison, the metallicity distribution of the California Planet Search radial velocity sample has a mean of [M/H]CPS,mean=-0.005±0.006, and the samples come from different parent populations according to a Kolmogorov-Smirnov test. We refit the exponential relation between the fraction of stars hosting a close-in giant planet and the host star metallicity using a sample of dwarf stars from the California Planet Search with updated metallicities. The best-fit relation tells us that the difference in metallicity between the two samples is insufficient to explain the discrepant hot Jupiter occurrence rates; the metallicity difference would need to be ∼0.2-0.3dex for perfect agreement. We also show that (sub)giant contamination in the Kepler sample cannot reconcile the two occurrence calculations. We conclude that other factors, such as binary contamination and imperfect stellar properties, must also be at play. Description: We measure the metallicity distribution of Kepler target stars through a sample of 835 high-resolution spectra taken with the Hectochelle multi-fiber spectrograph (R∼34000). Four observations pointing at four different fields within the Kepler field were obtained (wavelength range from 5145 to 5300Å) in 2014 Jul 15. File Summary:
FileName Lrecl Records Explanations
ReadMe 80 . This file table2.dat 53 776 Stellar parameters of 776 Kepler stars
See also: V/137 : Extended Hipparcos Compilation (XHIP) (Anderson+, 2012) V/133 : Kepler Input Catalog (Kepler Mission Team, 2009) VI/120 : High-resolution synthetic stellar library (Coelho+, 2005) J/ApJ/348/557 : X-ray studies of stars in the Pleiades (Micela+, 1990) J/A+A/420/183 : Spectrosc. survey in solar neighborhood (Allende Prieto+ 2004) J/A+A/415/1153 : [Fe/H] for 98 extra-solar planet-host stars (Santos+, 2004) J/ApJ/622/1102 : The planet-metallicity correlation. (Fischer+, 2005) J/ApJS/159/141 : Spectroscopic properties of cool stars. I. (Valenti+, 2005) J/ApJS/169/430 : Atmospheric param. of 1907 metal-rich stars (Robinson+, 2007) J/A+A/487/373 : Spectroscopic parameters of 451 HARPS-GTO stars (Sousa+, 2008) J/ApJS/190/1 : A survey of stellar families (Raghavan+, 2010) J/A+A/535/A30 : Abundances of 12 stars in open clusters (Carrera+, 2011) J/ApJ/742/54 : CASH project II. 14 extremely metal-poor stars (Hollek+, 2011) J/other/Nat/486.375 : Stellar parameters of KOI stars (Buchhave+, 2012) J/ApJ/753/90 : Stellar param. of K5 and later type Kepler stars (Mann+, 2012) J/A+A/538/A76 : Automatic stellar spectral classification (Navarro+, 2012) J/ApJ/771/107 : Spectroscopy of faint KOI stars (Everett+, 2013) J/ApJ/769/57 : Equivalent widths of metal-poor stars (Frebel+, 2013) J/ApJ/795/64 : A catalog of exoplanet physical param. (Foreman-Mackey+, 2014) J/ApJS/211/2 : Revised properties of Q1-16 Kepler targets (Huber+, 2014) J/ApJ/807/45 : Potentially habitable planets orbiting M dwarfs (Dressing+, 2015) J/AJ/150/134 : uvbyCaHβ photometry of NGC 752 (Twarog+, 2015) J/ApJS/225/32 : Extended abundance analysis of cool stars (Brewer+, 2016) J/ApJS/224/12 : Kepler planetary candidates. VII. 48-month (Coughlin+, 2016) J/AJ/152/8 : Impact of stellar multiplicity on planetary systems I. (Kraus+, 2016) J/ApJ/822/86 : False positive proba. for Q1-Q17 DR24 KOIs (Morton+, 2016) J/A+A/587/A64 : Physical properties of giant exoplanets (Santerne+, 2016) http://exoplanetarchive.ipac.caltech.edu/ : NASA exoplanet archive Byte-by-byte Description of file: table2.dat
Bytes Format Units Label Explanations
1- 7 I7 --- KIC Kepler identifier 9- 10 I2 h RAh [19] Hour of Right Ascension (J2000) 12- 13 I2 min RAm [9/34] Minute of Right Ascension (J2000) 15- 18 F4.1 s RAs Second of Right Ascension (J2000) 20 A1 --- DE- [+] Sign of the Declination (J2000) 21- 22 I2 deg DEd [42/46] Degree of Declination (J2000) 24- 25 I2 arcmin DEm Arcminute of Declination (J2000) 27- 30 F4.1 arcsec DEs Arcsecond of Declination (J2000) 32- 35 F4.1 mag Kpmag [8.8/15] Apparent Kepler magnitude 37- 40 I4 K Teff [3980/7370] Effective temperature (1) 42- 45 F4.2 [cm/s2] log(g) [1.2/5] Log surface gravity (1) 47- 51 F5.2 [Sun] [M/H] [-2.5/0.5] Metallicity by number density (1) 53 A1 --- Bin Binary code (N=not a binary; P=Potential binary, 46 occurrences)
Note (1): All stars have uniform empirical uncertainties on Teff of 100K, log(g) of 0.1, and [M/H]=0.1dex. The uncertainties are estimated in section 4 by picking out stars with multiple measurements and comparing the best-fit parameters for each observation of the same stars.
History: From electronic version of the journal
(End) Prepared by [AAS], Emmanuelle Perret [CDS] 26-Oct-2017
The document above follows the rules of the Standard Description for Astronomical Catalogues.From this documentation it is possible to generate f77 program to load files into arrays or line by line

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