All Figures

$\begin{figure} \par\hspace*{1.0cm}\psfig{figure=5622f1.ps,angle=0,width=6.0cm} % \end{figure}$ Figure 1: Archival HST/ACS UV image of SBS 0335-052E with thelabelled compact clusters. North is up and East is to the left.
Open with DEXTER

In the text

$\begin{figure} \par\mbox{\psfig{figure=5622f2a.ps,angle=0,width=9.0cm}\psfig{fig... ...0,width=9.0cm}\psfig{figure=5622f2d.ps,angle=0,width=9.0cm,clip=} } \end{figure}$ Figure 2: Spectrum of the brightest part of SBS 0335-052E shown in Fig. 7a as a rectangular region delineated by the thick solid line.
Open with DEXTER

In the text

$\begin{figure} \par\mbox{\psfig{figure=5622f3a.ps,angle=0,width=9.0cm}\psfig{fig... ...0,width=9.0cm}\psfig{figure=5622f3d.ps,angle=0,width=9.0cm,clip=} } \end{figure}$ Figure 3: Spectrum of a region centered on clusters 4 and 5 and shown in Fig. 7a as a square region delineated by a thick dashed line.
Open with DEXTER

In the text

$\begin{figure} \mbox{\psfig{figure=5622f4a.ps,angle=0,width=3.5cm}\psfig{figure=... ...0,width=3.5cm}\psfig{figure=5622f4i.ps,angle=0,width=3.5cm,clip=} } \end{figure}$ Figure 4: Images in the continuum near H $\beta$ emission line a) and in emission lines [O II] $\lambda$ 3727 Å b), [O III] $\lambda$ 4363 Å c), He II $\lambda$ 4686 Å d), [Ar IV] $\lambda$ 4740 Å e), H $\beta$ $\lambda$ 4861 Å f), [O III] $\lambda$ 5007 Å g), He I $\lambda$ 5876 Å h) and H $\alpha$ $\lambda$ 6563 Å i). All images are shown in the logarithmic flux scale. Positions of stellar clusters are labelled in panel (a). White cross in each panel shows the location of the region with maximum flux of the H $\alpha$ $\lambda$ 6563 Å emission line.
Open with DEXTER

In the text

$\begin{figure} \par\mbox{\psfig{figure=5622f5a.ps,angle=0,width=6.0cm}\hspace*{1.0cm}\psfig{figure=5622f5b.ps,angle=0,width=6.0cm,clip=} } \end{figure}$ Figure 5: Distribution of the H $\beta$ $\lambda$ 4861 Å equivalent width a) and of the H $\alpha$ $\lambda$ 6563 Å equivalent width b) in Å, with errors indicated in parentheses. Each square region corresponds to $0\hbox{$.\!\!^{\prime\prime}$ }52\times0\hbox{$.\!\!^{\prime\prime}$ }52$ . Only regions in which both EW(H $\beta$ ) and EW(H $\alpha$ ) could be measured are shown. Dark squares indicate the locations of clusters 1+2 with the maximum flux of the H $\alpha$ emission line, grey squares the locations of clusters 4+5.
Open with DEXTER

In the text

$\begin{figure} \par\hspace*{1.0cm}\psfig{figure=5622f6.ps,angle=0,width=6.0cm,clip=}\end{figure}$ Figure 6: He II $\lambda$ 4686/H $\beta$ relative intensity distribution (in percent). Only regions with a strong enough He II $\lambda$ 4686 emission line are shown. The dark square is the location of clusters 1+2, while the grey square is the location of clusters 4+5.
Open with DEXTER

In the text

$\begin{figure} \par\mbox{\psfig{figure=5622f7a.ps,angle=0,width=4.4cm}\hspace*{0... ...ce*{0.1cm}\psfig{figure=5622f7d.ps,angle=0,width=4.4cm,clip=} } \par\end{figure}$ Figure 7: Profiles of the emission lines: a) H $\alpha$ $\lambda$ 6563 Å, b) He II $\lambda$ 4686 Å, c) [O II] $\lambda$ 3726,3729 Å and d) [O III] $\lambda$ 4363 Å. All $0\hbox{$.\!\!^{\prime\prime}$ }52\times0\hbox{$.\!\!^{\prime\prime}$ }52$ regions are shown. Dark squares mark the location of clusters 1+2, grey squares the location of clusters 4+5. Thick solid and thick dashed lines in (a) delineate the brightest rectangular region and the second brightest square region for which the spectra are shown in Figs. 2 and 3.
Open with DEXTER

In the text

$\begin{figure} \par\hspace*{1.5cm}\psfig{figure=5622f8.ps,angle=0,width=5.3cm} % \end{figure}$ Figure 8: Schematic H $\alpha$ kinematic model of SBS 0335-052E. Clusters 1, 2 and 4, 5 are shown by dark and grey circles respectively. The region with narrow H $\alpha$ profiles is shown by a grey rectangle. Its orientation is close to the orientation of the H I cloud discussed by Pustilnik et al. (2001). Two regions with the ionised gas outflow are located to the north and south of the region with a narrow H $\alpha$ emission line.
Open with DEXTER

In the text

$\begin{figure} \par\mbox{\psfig{figure=5622f9a.ps,angle=0,width=5.0cm}\hspace*{0... ...hspace*{0.1cm}\psfig{figure=5622f9d.ps,angle=0,width=5.0cm,clip=} } \end{figure}$ Figure 9: Macroscopic/turbulent velocity dispersion at the FWHM (in km s^-1) derived from the a) H $\alpha$ $\lambda$ 6563 Å, b) He II $\lambda$ 4686 Å, (c) [O II] $\lambda$ 3729 Å and d) [O III] $\lambda$ 4363 Å emission lines. The errors of the velocity dispersion are shown in parentheses. Only regions with the detected lines are shown. The dark square shows the location of clusters 1+2 with a maximum flux of the H $\alpha$ 6563 Å emission line. The grey square shows the location of clusters 4+5.
Open with DEXTER

In the text

$\begin{figure} \par\mbox{\psfig{figure=5622f10a.ps,angle=0,width=5.0cm}\hspace*{... ...psfig{figure=5622f10e.ps,angle=0,width=5.0cm,clip=}\hspace*{1.5cm}} \end{figure}$ Figure 10: a) Electron temperature distribution (in 10⁴ K) from the [O III] $\lambda$ 4363/( $\lambda$ 4959+ $\lambda$ 5007) line ratio. b) Electron number density distribution (in cm^-3) from the [S II] $\lambda$ 6717/ $\lambda$ 6731 line ratio. c) Oxygen abundance 12+log O/H distribution. d) Distribution of the nitrogen-to-oxygen abundance ratio. e) Distribution of the neon-to-oxygen abundance ratio. The dark region is the region with maximum intensity of H $\alpha$ 6563 Å emission line coincident with the location of clusters 1 and 2. The grey region corresponds to clusters 4 and 5.
Open with DEXTER

In the text

$\begin{figure} \par\hspace*{0.0cm}\psfig{figure=5622f11.ps,angle=0,width=8.5cm} % \end{figure}$ Figure 11: Part of the spectrum of cluster 3 showing the probable broad Wolf-Rayet emission lines N III $\lambda$ 4640 and C IV $\lambda$ 4658 labelled "WR''.
Open with DEXTER

In the text

$\begin{figure} \par\hspace*{1.0cm}\psfig{figure=5622f1.ps,angle=0,width=6.0cm} % \end{figure}$	Figure 1: Archival HST/ACS UV image of SBS 0335-052E with thelabelled compact clusters. North is up and East is to the left.
Open with DEXTER

$\begin{figure} \par\mbox{\psfig{figure=5622f2a.ps,angle=0,width=9.0cm}\psfig{fig... ...0,width=9.0cm}\psfig{figure=5622f2d.ps,angle=0,width=9.0cm,clip=} } \end{figure}$	Figure 2: Spectrum of the brightest part of SBS 0335-052E shown in Fig. 7a as a rectangular region delineated by the thick solid line.
Open with DEXTER

$\begin{figure} \par\mbox{\psfig{figure=5622f3a.ps,angle=0,width=9.0cm}\psfig{fig... ...0,width=9.0cm}\psfig{figure=5622f3d.ps,angle=0,width=9.0cm,clip=} } \end{figure}$	Figure 3: Spectrum of a region centered on clusters 4 and 5 and shown in Fig. 7a as a square region delineated by a thick dashed line.
Open with DEXTER

$\begin{figure} \par\hspace*{1.0cm}\psfig{figure=5622f6.ps,angle=0,width=6.0cm,clip=}\end{figure}$	Figure 6: He II $\lambda$ 4686/H $\beta$ relative intensity distribution (in percent). Only regions with a strong enough He II $\lambda$ 4686 emission line are shown. The dark square is the location of clusters 1+2, while the grey square is the location of clusters 4+5.
Open with DEXTER

$\begin{figure} \par\hspace*{0.0cm}\psfig{figure=5622f11.ps,angle=0,width=8.5cm} % \end{figure}$	Figure 11: Part of the spectrum of cluster 3 showing the probable broad Wolf-Rayet emission lines N III $\lambda$ 4640 and C IV $\lambda$ 4658 labelled "WR''.
Open with DEXTER