A search for diffuse bands in fullerene planetary nebulae: evidence of diffuse circumstellar bands

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Volume 573 (January 2015)

A&A, 573 (2015) A97

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Table A.2

Diffuse interstellar bands in M 1-20 and HR 6716.

M 1-20					HR 6716
λ _c	FWHM	EQW	S/N	EQW/E _{B − V}	λ ^c	FWHM	EQW	S/N	EQW/E _{B − V}
(Å)	(Å)	(mÅ)		(Å/mag)	(Å)	(Å)	(mÅ)		(Å/mag)

4426.56^a	19.94^b	2579.0^b	20^c	3.22	4429.27	22.25	595.8	233	2.71
5780.44	1.93	361.1	36	0.45	5780.41	2.01	164.5	792	0.75
5796.97	0.78	153.4	39	0.19	5796.95	0.74	37.2	661	0.17
5849.69	0.95	70.7	52	0.09	5849.69	0.84	9.3	639	0.04
6195.83	0.43	44.3	71	0.05	6195.82	0.41	13.2	612	0.06
6203.00	1.39	97.7	77	0.12	6203.02	1.25	28.9	688	0.13
6269.89	1.51	89.2	67	0.11	6269.70	1.02	12.4	684	0.06
6283.60	4.06	573.0	73	0.72	6283.51	4.29	474.4	641	2.16
6375.94	0.51	26.3	75	0.03	6375.89	0.65	6.3	656	0.03
6379.14	0.59	80.6	100	0.10	6379.12	0.63	22.5	687	0.10
6613.48	1.01	177.0	79	0.22	6613.41	0.86	37.5	581	0.17
6660.52	0.59	27.5	74	0.03	6660.55	0.41	5.0	531	0.02

Notes. The 3σ errors in the EQWs scale as ~3 ×FWHM/(S/N), while the FHWMs are less precise than 0.03 Å.

^(a)

The parameters of this DIB are estimated by adopting a Lorentzian profile (see, e.g., Snow et al. 2002). The central wavelength in M 1-20 is very uncertain.

^(b)

Best estimates found by clipping out the narrow emission lines and smoothing the spectrum with boxcar 15. The error in the quoted EQW is estimated to be ~786 mÅ.

^(c)

S/N in the original spectrum.

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