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Home All issues Volume 550 (February 2013) A&A, 550 (2013) L6 Full HTML
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Table A.1

Diffuse interstellar bands in fullerene PNea.

Tc 1 M 1-20 Hobbs et al. Luna et al.
λ c FWHM EQW S/N EQW/EB − V λ c FWHM EQW S/N EQW/EB − V EQW/EB − V EQW/EB − V
(Å) (Å) (mÅ) (Å/mag) (Å) (Å) (mÅ) (Å/mag) (Å/mag) (Å/mag)
4428.10b 19.35 860 329 3.74 4426.56b 19.94c 2579c 20d 3.22 1.10 ...   
5780.40 2.06 105 416 0.46 5780.66 2.17 359 32 0.45 0.23 0.46
5796.88 0.99 42 357 0.18 5797.31 1.14 155 53 0.19 0.18 0.17
5849.60 1.35 11 346 0.047 5850.02 1.23 70 37 0.087 0.086 0.061
6195.85 1.17 13 549 0.056 6196.18 0.95 36 68 0.045 0.034 0.053
6269.77 1.93 9 548 0.037 6270.19 2.48 130 66 0.16 0.069 ...   
6283.93 4.91 316 579 1.38 6283.77 5.25 706 61 0.88 0.41 0.90
6308.90 2.98 42 530 0.18 ...    ...    ...    ...    ...    0.049 ...   
6379.08 1.39 12 513 0.050 6379.56 1.30 93 56 0.12 0.085 0.088
6525.15 4.79 173 522 0.75 ...    ...    ...    ...    ...    ...    ...   
6613.50 1.42 36 412 0.16 6613.78 1.23 167 77 0.21 0.149 0.21

Notes. 

(a)

The 3-σ errors in the EQWs scale like  ~3 ×  FWHM/(S/N) while we estimate that the FHWMs in Tc 1 are precise to the 0.03 Å level (less for M 1-20).

(b)

The characteristics of this DIB are estimated by adopting a Lorentzian profile (see e.g., Snow et al. 1992).

(c)

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.

(d)

S/N in the original spectrum.

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