All Tables

Table 1: Properties of the observed target 4U 1907+09 and the telluric standards HD 165470 and HD 166934. The listed values were obtained from the SIMBAD database, except $\ensuremath {{E}_{(B-V)}}$ , $v_r \sin i$ and spectral type of the optical companion to 4U 1907+09 which were taken from Cox et al. (2005). The intrinsic colours for the quoted spectral types are adopted from Schmidt-Kaler (1982). The total exposure time for 4U 1907+09 is 9000 s; 6300 and 2700 s in the 346+580 and 437+860 settings, respectively. The instrument settings are indicated by the central wavelength (in Å) of the red and blue arm of the UVES spectrograph, respectively. The former setting covers the spectral range up to 6640 Å, while the latter covers the spectral range, with gaps, from 6700 to 10390 Å (shown in Fig. 1).
Table 2: Central wavelength $\lambda$ (Å), full width at half maxium F (Å), equivalent width W (mÅ) and the error on the equivalent width $\sigma W$ (mÅ) for a selection of the strongest DIBs observed towards 4U 1907+09 and the comparison targets BD +63 1964 and HD 183143 (Tuairisg et al. 2000). The full table is available as on-line material only.
Table 3: Relative strength of 4U 1907+09 DIBs compared to BD +63 1964 and HD 183143 DIBs. The DIBs in 4U 1907+09 are stronger and broader compared to the reference targets. The 9577 and 9632 Å DIBs for BD +63 1964 have been observed tentatively by Vuong (private communication) and are weakened by about a factor of three with respect to HD 183143.
Table 4: Sightlines towards five reddened HMXBs. The name of the X-ray source, colour excess $\ensuremath {{E}_{(B-V)}}$ , visual extinction $A_{\rm V}$ , total to selective visual extinction $R_{\rm V}$ , H I column density, distance and the 5797, 6613, 5780 Å DIB and K I equivalent widths are tabulated.
Table 5: Line of sight comparison. To illustrate how the line of sight towards 4U 1907+09 relates to the other well studied lines of sight in our Galaxy, we summarise dust, gas and DIB properties. DIB strengths for Cyg OB2-41 (VI Cyg 12) from Chlewicki et al. 1986 (except for $\lambda$ 6613 taken from Rawlings et al. 2003 and $\lambda$ 6379 taken from Bromage & Nandy 1973). DIB strengths for HD 144217 and HD 149757 are from Sollerman et al. (2005). For HD 183143, BD +63 1964 and Cyg OB2-41 the N(H₂) is inferred from N(CH) (Jenniskens et al. 1992), and N(H I) from N(H)=5.8 $\times$ 10²¹ $\ensuremath {{E}_{(B-V)}}$ and N(H) = N(H I) + 2 N(H₂). N(CH) via EW(CH) (Kreowski et al. 1999) for HD 183143 and BD +63 1964, and from Scappini et al. (2000) for Cyg OB2-41.
Full version
Table 2: Observed wavelength ( $\lambda$ in Å) (in heliocentric rest frame), full width at half maximum (F in Å), equivalent width (W in mÅ) and the statistical error on equivalent width ( $\sigma$ in mÅ) of the DIBs detected towards 4U 1907+09 are given in Cols. 1 to 4, respectively. Corresponding values for the comparison targets BD +63 1964 ( $\lambda$ < 6650 Å; Tuairisg et al. 2000) and HD 183143 ( $\lambda$ > 6650 Å; Jenniskens & Desert 1994, JD94) are given in Cols. 5 to 8. 4U 1907+09 features that are only tentative are put into parenthesises. For spectral regions not covered by our observations we use "x''. Parameters for all DIBs (both for 4U 1907+09 and reference targets) are determined by fitting Gaussians. For 4U 1907+09 it is not always possible, due to broadening and/or limited signal-to-noise, to decompose the DIB spectrum in a similar way as has been done for the reference spectra. Where possible we indicate with curly brackets how different DIB complexes are related to each other. A large number of the very weak DIBs ( $\leq$ 10 mÅ) are not detected, especially those in regions contaminated with telluric lines, or regions affected by small scale fringing (above 7000 Å). Column 10 (N) lists a "+'' for the positive identification of a hitherto tentative DIB. A non-detection of a tentative DIB is indicated with "-''. And a "G'' refers to a new DIB from the Galazutdinov et al. (2000) survey. A "?'' points out a unidentified feature. The expected stellar contamination is very small, and mostly negligible in deriving the EW. We indicate also in Col. 10 the possible stellar line contamination as predicted by the Lanz & Hubeny (2003) O-star model atmosphere with T = 30,000 K and log g = 3.00 (see also the main text).