Table 2: Diffuse interstellar bands investigated in this study. Equivalent widths ( EW) and associated statistical errors $\sigma _{\it EW}$ are quoted in mÅ. For non-detected DIBs upper limits are given; EW $_{\rm upper\ limit} = 3 \times \sigma _{\rm continuum} \times {\it FWHM}_{\rm DIB}$, with $\sigma _{\rm continuum}$ the noise on the adjacent continuum, and FWHM $_{\rm DIB}$ the expected full width at half maximum of the respective DIB. The \ensuremath {E_{B-V}} values were derived by subtracting the Milky Way foreground contamination from the line of sight reddening (see Sect. 4.1 and Tables 1 and 3). The "$\times $'' signifies DIBs that were not covered by the spectral setting, and the (B) indicates possible blending with stellar or instrumental features. We have derived upper limits for DIB strengths towards the low reddened target Sk -67 5. Sk -70 120 has been used as the reference star ( \ensuremath {E_{B-V}} = 0.0 mag).
    LMC
    Sk -69 223 Sk -69 243 Sk -67 2 Sk -68 135 Sk -67 5
\ensuremath {E_{B-V}} $_{\rm , LMC}$   0.20 0.29 0.12 0.14 0.04
DIB $\lambda_{\rm LMC}$ EW ( $\sigma _{\it EW}$) EW ( $\sigma _{\it EW}$) EW ( $\sigma _{\it EW}$) EW ( $\sigma _{\it EW}$) EW ( $\sigma _{\it EW}$)
4428 4431.95 <180 150 (180) <247 <200 <200
5705 5710.23 20 (9) 25 (21) <32 <23 <28 (B)
5780 5785.57 145 (2) $\times $ $\times $ $\times $ $\times $
5797 5802.21 28 (6) $\times $ $\times $ $\times $ $\times $
5849 5855.08 <8 11 (6) 10 (5) 5 (5) <15
6196 6201.57 12 (3) 7 (3) 5 (3) <7 <7
6203(B) 6208.67 50 (20) 25 (14) 19 (14) 17 (17) <17
6284 6289.51 240 (21) 335 (47) 150 (29) 30 (30) <163
6376 6381.71 5 (6) <28 <23 <20 (B) <17
6379 6384.96 12 (4) 15 (4) <10 <10 (B) <7
6613 6619.51 20 (8) 50 (14) 13 (8) 5 (3) (B) <13


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