Analysis of Galactic late-type O dwarfs: more constraints on the weak wind problem

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Table 1:

Observational data of the program stars.
			Far-UV		UV		Optical
star	spectral type^a	V	data set^b	date	data set	date	instrument	date
HD 216898	O9IV, O8.5V	8.04	F-A0510303	2000-08-03	SWP43934	1992-02-05	OHP/ELODIE	2004-08-29
HD 326329	O9V	8.76	F-B0250501	2001-08-09	SWP48698	1993-09-21	ESO/FEROS	2005-06-25
HD 66788	O8V, O9V	9.43	F-P1011801	2000-04-06	SWP49080	1993-11-03	ESO/FEROS	2004-12-22
${\zeta }$ Oph	O9.5Vnn	2.56	C-C002	1972-08-29 $^{{\dagger}}$	SWP36162	1989-04-29	OHP/ELODIE	1998-06-11
HD 216532	O8.5V((n))	8.03	F-A0510202	2000-08-02	SWP34226	1988-09-11	OHP/ELODIE	2005-11-10

^a Spectral types come from Lesh (1968), Schild et al. (1969), Garrison (1970), Walborn (1973), and MacConnell & Bidelman (1976).
^b Satellite used to obtain spectra: F = FUSE and C = Copernicus.
$^{{\dagger}}$ Orbits #115-247 (Snow et al. 1977).

Source LaTeX | All tables | In the text

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