 |
Figure 1: Examples of the observed spectra of NGC 346-11 from UVES. These sample spectral regions include important lines such as Si IV b), Si III c) and C III d). Notice the lack of an obvious N II line at 3995 Å in a). |
| Open with DEXTER | |
In the text
 |
Figure 2: Observed and theoretical spectra for the He II line at 4541 Å in NGC 346-11. The latter are for effective temperatures of 30 000 K, 32 500 K and 35 000 K ( upper, middle and lower smooth curvesrespectively) and imply an estimate of approximately 33 500 K. |
| Open with DEXTER | |
In the text
 |
Figure 3: Examples of the agreement between observed and theoretical (generated using the atmospheric parameters listed in Table 2) Balmer line profiles. |
| Open with DEXTER | |
In the text
 |
Figure 4: The observed interstellar gas components towards NGC 346-11 and AV 304, together with the Gaussian fits used to deduce the velocities listed in Table 4. |
| Open with DEXTER | |
In the text