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 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:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
tables.dat 103 226 Stellar parameters of Kepler Objects of Interest
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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
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Bytes Format Units Label Explanations
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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
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History:
From electronic version of the journal
(End) Patricia Vannier [CDS] 23-Jul-2012