Extrasolar planets and brown dwarfs around A–F type stars - VII. θ Cygni radial velocity variations: planets or stellar phenomenon?

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Table 1:

$\theta$ Cygni stellar properties.
Parameter		$\theta$ Cygni
Spectral type		F4V
$v\sin i$	[km s $^{\rm -1}$ ]	7
V		4.49
B-V		$0.395 \pm 0.015$
$\pi$	[mas]	$54.54 \pm 0.15$
Distance	[pc]	$18.33\pm0.05$
M_V		3.14
[Fe/H]		-0.08
$T_{\rm eff}$	[K]	6745
$\log{g}$		4.2
M₁	[ $M_{\odot}$ ]	$1.38 \pm 0.05$
Age	[Gyr]	1.5_-0.7^+0.6
ppm ( $\alpha$ ) $^\dagger$	[mas yr $^{\rm -1}$ ]	-8.15
ppm ( $\delta$ ) $^\dagger$	[mas yr $^{\rm -1}$ ]	-262.99

$^\dagger$ The proper motion is affected from the orbital motion that we discuss in Sect. 2.2.
Note: photometric and astrometric data from the H IPPARCOS catalogue (ESA 1997; van Leeuwen 2007); spectroscopic data from Nordström et al. (2004) and Erspamer & North (2003).

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