Excitation temperature of and broadening of the 6196 Å diffuse interstellar band

M. Kaźmierczak; P. Gnaciński; M. R. Schmidt; G. Galazutdinov; A. Bondar; J. Krełowski

doi:10.1051/0004-6361/200811558

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Volume 498 / No 3 (May II 2009)

A&A, 498 3 (2009) 785-791

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Table 1:

Basic data of our program stars, columns ``DIB'' and ``C₂'' identify sources of the 6196 Å DIB profile and of the C₂ band, ``S/N'' determines the signal-to-noise ratio in the range of the spectrum near to a 6196 Å feature.
Object	Name	Sp/L*	E(B-V)*	DIB	S/N	C₂
HD 23 180	o Per	B1III	0.27	GECKO	600	BOES
HD 110 432		B2pe	0.48	FEROS	300	^a
HD 147 888	$\rho$ Oph D	B5V	0.47	FEROS	500	^b
HD 147 889		B2V	1.07	HARPS	500	UVES
HD 148 184	$\chi$ Oph	B2Vn,el	0.52	HARPS	600	UVES
HD 149 757	$\zeta$ Oph	O9.5V	0.32	CES	1000	^c
HD 154 368		O9.5Iab	0.73	UVES	300	UVES
HD 163 800		O7IIIf	0.60	HARPS	500	UVES
HD 169 454	V430 SCT	B1Ia	0.93	UVES	400	UVES
HD 179 406	20 Aql	B3V	0.33	HARPS	600	UVES
HD 204 827		B0V	1.11	BOES	300	^d

* Thorburn et al. (2003), Hunter et al. (2006); ^a calculated by Sonnentrucker et al. (2007) using the equivalent widths of van Dishoeck & Black (1989) (Phillips system); ^b Sonnentrucker et al. (2007) (Mulliken system); ^c calculated by Sonnentrucker et al. (2007) using the equivalent widths of Hobbs & Campbell (1982) (Phillips system); ^d calculated in this work using the equivalent widths of Ádámkovics et al. (2003) (Phillips system).

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