SOPHIE velocimetry of Kepler transit candidates - VII. A false-positive rate of 35% for Kepler close-in giant candidates

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Volume 545 (September 2012)

A&A, 545 (2012) A76

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Issue		A&A Volume 545, September 2012


Article Number		A76
Number of page(s)		16
Section		Planets and planetary systems
DOI		https://doi.org/10.1051/0004-6361/201219608
Published online		10 September 2012

Online material

Table 2

SOPHIE measurements of KOI-12.

Table 3

SOPHIE measurements of KOI-131.

Table 4

SOPHIE measurements of KOI-190.

Table 5

SOPHIE measurements of KOI-192.

Table 6

SOPHIE measurements of KOI-197.

Table 7

SOPHIE measurements of KOI-201.

Table 8

SOPHIE measurements of KOI-340.

Table 9

SOPHIE measurements of KOI-418.

Table 10

SOPHIE measurements of KOI-419.

Table 11

SOPHIE measurements of KOI-425.

Table 12

SOPHIE measurements of KOI-607.

Table 13

SOPHIE measurements of KOI-609.

Table 14

SOPHIE measurements of KOI-611.

Table 15

SOPHIE measurements of KOI-698.

Table 16

SOPHIE measurements of KOI-1786.

Table 17

Parameters for KOI-419.

Table 18

Parameters for KOI-698.

Table 19

Occurrence of hot Jupiter per thousand of stars.

	Fig. 7 KOI-419 light-curve (top panel), radial velocities (middle panel) and spectral energy distribution (bottom panel) with the best-combined fit (red or black line). The phase zero corresponds to the periastron epoch. The open circles in the bottom panel correspond to the best model integrated toward the same band-passes as the photometric measurements (red dots).
Open with DEXTER

Fig. 8

KOI-698 light-curve (top panel), radial velocities (middle panel) and spectral energy distribution (bottom panel) with the best-combined fit (red or black line). The phase zero corresponds to the periastron epoch. The open circles in the bottom panel correspond to the best model integrated toward the same band-passes as the photometric measurements (red dots). The Rossiter-McLaughlin-like effect seen around phase 0.3 and 0.9 is due to the expected variation when the primary and secondary spectra are blended.

Open with DEXTER

© ESO, 2012

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