Hot subdwarf stars in close-up view - I. Rotational properties of subdwarf B stars in close binary systems and nature of their unseen companions

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Volume 519 (September 2010)

A&A, 519 (2010) A25

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Table 3:

Projected rotational velocities of radial velocity variable sdBs, for which orbital parameters are unavailable or uncertain.
System	$T_{\rm eff}$	m_B	S/N	seeing	$N_{\rm lines}$	${v_{\rm rot}~\sin~i}$	Instrument
	[K]	[mag]		[arcsec]		[ ${\rm km~s^{-1}}$ ]
HE 2208+0126	24 300	15.6	24	0.8	15	<5.0	UVES
TON S 135	25 000	13.1	47		35	6.6 $\pm$ 1.0	FEROS
HE 2322-4559^c	25 500	15.5	23	0.7	16	10.9 $\pm$ 1.1	UVES
HS 2043+0615	26 200	16.0	22	1.3	26	12.3 $\pm$ 1.1	UVES
HE 1309-1102^c	27 100	16.1	7	0.6	7	7.6 $\pm$ 2.3	UVES
HS 2357+2201	27 600	13.3	29	0.7	26	6.1 $\pm$ 1.1	UVES
HS 2359+1942	31 400	14.4	14	0.6	26	< 5.0	UVES
PG 1032+406	31 600	10.8	20		H/He	<34	Palomar
HE 1140-0500^c	34 500	14.8	18	0.9	5	5.2 $\pm$ 2.7	UVES
HS 1536+0944^c	35 100	15.6	19	1.1	15	12.2 $\pm$ 1.6	UVES
HE 1033-2353	36 200	16.0	13	0.6	7	9.3 $\pm$ 2.3	UVES

Notes. The average seeing is only given if the spectra were obtained with a wide slit in the course of the SPY survey. In all other cases the seeing should not influence the measurements. Atmospheric parameters are taken from Lisker et al. (2005) except TON S 135 (Heber 1986) and PG 1032+406 (Maxted et al. 2001). ^c Companion visible in the spectrum.

Source LaTeX | All tables | In the text

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