All Figures

$\begin{figure} \par\includegraphics[width=7cm,clip]{7677fig1.eps}\end{figure}$ Figure 1: VLT/FORS2 spectroscopy of three new WR stars. Narrow emission lines in the spectrum of #33 are from an associated H II region.
Open with DEXTER

In the text

$\begin{figure} \par\includegraphics[width=7.8cm,clip]{7677fig2.eps}\end{figure}$ Figure 2: Comparison between the $\lambda 4781$ continuum magnitudes of WR candidates in NGC 300 and the $\lambda$ 4684 excess (stars), updated from Schild et al. (2003). Spectroscopically confirmed WR stars are presented - see key. Approximate absolute magnitudes and line equivalent widths are indicated. Three WR candidates, #1 (WC4), #37 and #51, for which reliable photometry was not feasible are omitted from this figure.
Open with DEXTER

In the text

$\begin{figure} \par\includegraphics[width=5.85cm,clip]{7677fig3.eps}\end{figure}$ Figure 3: Spectroscopically confirmed N(WC)/N(WN) ratio for NGC 300, together with other nearby spiral (filled squares) and irregular (filled circles) galaxies from Crowther (2007) and references therein, plus Hadfield & Crowther (2007) for NGC 1313. Open symbols for NGC 300 and NGC 1313 are corrected for candidate WR sources, as outlined in the text. Predictions from Meynet & Maeder (2005, solid) and Eldridge & Vink (2006, dotted) are also shown.
Open with DEXTER

In the text

$\begin{figure} \par\includegraphics[width=7.8cm,clip]{7677fig4.eps}\end{figure}$ Figure 4: Spectroscopic comparison between NGC 300 #41, a candidate for the optical counterpart of NGC 300 X-1, and [MAC92] 17-A, alias IC 10 X-1 (Clark & Crowther 2004; Prestwich et al. 2007).
Open with DEXTER

In the text

$\begin{figure} \par\includegraphics[angle=-90,width=7.9cm,clip]{7677fig5.eps}\end{figure}$ Figure 5: Spectroscopic comparison between the de-reddened VLT/FORS2 spectrum of NGC 300 #41 and the theoretical non-LTE model (dotted-lines) discussed in the text.
Open with DEXTER

In the text

$\begin{figure} \par\includegraphics[width=7cm,clip]{7677fig1.eps}\end{figure}$	Figure 1: VLT/FORS2 spectroscopy of three new WR stars. Narrow emission lines in the spectrum of #33 are from an associated H II region.
Open with DEXTER

$\begin{figure} \par\includegraphics[width=7.8cm,clip]{7677fig4.eps}\end{figure}$	Figure 4: Spectroscopic comparison between NGC 300 #41, a candidate for the optical counterpart of NGC 300 X-1, and [MAC92] 17-A, alias IC 10 X-1 (Clark & Crowther 2004; Prestwich et al. 2007).
Open with DEXTER

$\begin{figure} \par\includegraphics[angle=-90,width=7.9cm,clip]{7677fig5.eps}\end{figure}$	Figure 5: Spectroscopic comparison between the de-reddened VLT/FORS2 spectrum of NGC 300 #41 and the theoretical non-LTE model (dotted-lines) discussed in the text.
Open with DEXTER