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J/other/Nat/486.375   Stellar parameters of KOI stars          (Buchhave+, 2012)

An abundance of small exoplanets around stars with a wide range of metallicities. Buchhave L.A., Latham D.W., Johansen A., Bizzarro M., Torres G., Rowe J.F., Batalha N.M., Borucki W.J., Brugamyer E., Caldwell C., Bryson S.T., Ciardi D.R., Cochran W.D., Endi M., Esquerdo G.A., Ford E.B., Geray J.C., Gilliland R.L., Hansen T., Isaacson H., Laird J.B., Lucas P.W., Marcy G.W., Morse J.A., Robertson P., Shporer A., Stefanik R.P., Still M., Quinn S.N. <Nature, 485, 375-377 (2012)> =2012Natur.486..375B
ADC_Keywords: Stars, double and multiple ; Planets Abstract: The abundance of heavy elements (metallicity) in the photospheres of stars similar to the Sun provides a "fossil" record of the chemical composition of the initial protoplanetary disk. Metal-rich stars are much more likely to harbour gas giant planets, supporting the model that planets form by accumulation of dust and ice particles5. Recent ground-based surveys suggest that this correlation is weakened for Neptunian-sized planets. However, how the relationship between size and metallicity extends into the regime of terrestrial-sized exoplanets is unknown. Here we report spectroscopic metallicities of the host stars of 226 small exoplanet candidates discovered by NASA's Kepler mission, including objects that are comparable in size to the terrestrial planets in the Solar System. Description: In February 2011, the Kepler mission announced its discovery of 1,235 planet candidates, of which more than half have radii smaller than that of Neptune: RP<4R{earth}, where R{earth} plus is the Earth radius. We used reconnaissance spectra obtained by the Kepler Follow-up Observing Program (FOP) to derive metallicities for several hundred of the brighter planet candidates, and used the results to explore the relationship between planet size and host-star metallicity. File Summary:
FileName Lrecl Records Explanations
ReadMe 80 . This file tables.dat 103 226 Stellar parameters of Kepler Objects of Interest
See also: V/133 : Kepler Input Catalog (Kepler Mission Team, 2009) J/ApJ/728/117 : Kepler planetary candidates. I. (Borucki+, 2011) Byte-by-byte Description of file: tables.dat
Bytes Format Units Label Explanations
1- 2 A2 --- --- [K0] 3- 9 F7.2 --- KOI [1/1607[ Kepler Object of Interest (NNNN.NN) 11- 14 I4 K Teff Effective temperature 16- 18 I3 K e_Teff rms uncertainty on Teff 20- 23 F4.2 [cm/s2] logg Surfacre gravity 25- 28 F4.2 [cm/s2] e_logg rms uncertainty on logg 30- 34 F5.2 [-] [m/H] Star metallicity 36- 39 F4.2 [-] e_[m/H] rms uncertainty on [m/H] 41- 44 F4.1 km/s vsini Rotational velocity 46- 48 F3.1 km/s e_vsini rms uncertainty on vsini 50- 54 F5.3 Rsun R* Stellar radius 56- 60 F5.3 Rsun E_R* Error on R* (upper value) 62- 66 F5.3 Rsun e_R* Error on R* (lower value) 68- 72 F5.3 Msun M* Stellar mass 74- 78 F5.3 Msun E_M* Error on R* (upper value) 80- 84 F5.3 Msun e_M* Error on R* (lower value) 86- 91 F6.3 Rgeo Rp Planet radius in Earth radii 93- 97 F5.3 Rgeo e_Rp rms uncertainty in Rp, in Earth radii 99-103 F5.1 --- S/N Signal-to-noise ratio per resolution element
History: From electronic version of the journal
(End) Patricia Vannier [CDS] 23-Jul-2012
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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