All Figures

$\begin{figure} \par\includegraphics[width=7cm,clip]{8916fig1.eps} \end{figure}$ Figure 1: Positions of slits PA 90 $^\circ$ -270 $^\circ$ and 160 $^\circ$ -340 $^\circ$ superimposed on an HST narrow-band H $\alpha$ (F656N) image of ESO 338-IG04 taken from Hayes (2007). North is up and east to the left. The positions of prominent super star clusters are marked, numbered according to Östlin et al. (1998). All the clusters belong to their inner sample, except 21, 25 and 47, which belong to the outer sample. The bright object to the lower right is a foreground star. The field of view here is 22 $^{\prime \prime }$ by 18 $^{\prime \prime }$ , corresponding to 3.9 kpc by 3.25 kpc at the distance of ESO 338-IG04 (37.5 Mpc; Östlin et al. 1998).
Open with DEXTER

In the text

$\begin{figure} \par\includegraphics[angle=270,width=8.6cm,clip]{8916f2a.ps}\par\... ...ace*{2mm} \includegraphics[angle=270,width=8.6cm,clip]{8916f2c.ps} \end{figure}$ Figure 2: Three examples of Paschen-line subtraction from the spectrum of ESO 338-IG04 around the calcium triplet, for extractions with different signal to noise ratio and different quality of subtraction, using the less affected blue wing of each line as a guide. These subtractions, for the slit at PA 90-270 $^\circ$ , were classed as high ( top; position -2 $.\!\!^{\prime\prime}$ 7), medium ( middle; +1 $^{\prime \prime }$ ) and low ( bottom; -1 $.\!\!^{\prime\prime}$ 2). Positions are relative to the point where the two slits cross; see Sect. 3. The subtracted spectrum is plotted over the original spectrum (grey). Vertical dashed lines mark the approximate expected position of the centres of the three calcium triplet lines.
Open with DEXTER

In the text

$\begin{figure} \par\includegraphics[width=8.5cm,clip]{8916fig3.ps} \par\end{figure}$ Figure 3: Cross-correlation functions with respect to HD 164349 (blue/darker and grey/lighter profiles; first and third panels) and [S III] profiles (in red; second and fourth panels) for ESO 338-IG04. The left two boxes are for slit PA 90 $^\circ$ -270 $^\circ$ and those on the right are for PA 160 $^\circ$ -340 $^\circ$ . Positions in arcsec relative to the crossing point of the two slits are marked next to each profile. CCFs are plotted in grey where the Paschen subtraction quality is low, or where the peak of the CCF is less than 0.25. Units in each plot are (abscissae) velocity in km s^-1km s^-1 and (ordinates) CCF value or flux in units of 10^-17 erg s^-1 cmcm^-2erg s^-1 cmcm^-2.
Open with DEXTER

In the text

$\begin{figure} \par\includegraphics[angle=-90,width=16cm,clip]{8916fig4.ps} \par\end{figure}$ Figure 4: Variation along slit PA 90 $^\circ$ -270 $^\circ$ of ( from top to bottom) continuum/line flux, velocity dispersion $\sigma$ and heliocentric velocity, for the gas ( left) and stars ( right) in ESO 338-IG04. Zero on the abscissa is defined as the point where our two slits cross, 4 $^{\prime \prime }$ east of cluster #23. The left panel shows the emission lines [S III] $\lambda$ 9069 (red open circles), H I Paschen lines (weighted means of all measured lines; blue filled circles), and O I $\lambda$ 8446 (green squares). The flux scales show ( left) the normalised strengths of the emission lines and ( right) the [S III] line flux compared to the mean continuum value around the calcium triplet. The dotted vertical lines mark the positions along the slit of ( from left to right) clusters 6, 19, 23, 44 and 53 from the inner sample of Östlin et al. (1998) (see also Fig. 1). The right panel shows results of cross-correlation with the K0 bright giant HD 164349 (blue squares) and pPXF results (magenta open circles). Cross-correlation measurements of velocity dispersion and heliocentric velocity are only shown where the CCF peak is greater than 0.25. CCF and pPXF results are not shown where the Paschen-subtraction quality was deemed to be low (see Fig. 2). The thick dashed line in the right panel repeats the [S III] results from the left panel for comparison. At the distance of ESO 338-IG04, 10 $^{\prime \prime }$ corresponds to 1.8 kpc.
Open with DEXTER

In the text

$\begin{figure} \par\includegraphics[angle=-90,width=16cm,clip]{8916fig5.ps} \end{figure}$ Figure 5: Same as Fig. 4, but for ESO 338-IG04 at PA 160 $^\circ$ -340 $^\circ$ . The dotted vertical lines in this case mark the positions along the slit of clusters 25 ( left) and 21 from the outer sample of Östlin et al. (1998) (see Fig. 1).
Open with DEXTER

In the text

$\begin{figure} \par\includegraphics[width=8.4cm,clip]{8916fig6.eps} % \par\end{figure}$ Figure 6: Velocity field ( left) and velocity dispersion ( right) of ESO 338-IG04 from Fabry-Perot measurements of H $\alpha$ , as measured by Östlin et al. (1999). North is up and east to the left. The colour scales in km s^-1km s^-1 are indicated below each panel. The black contours correspond to the H $\alpha$ flux in arbitrary logarithmic units. Overlaid in grey are the positions of our slits (cf. Fig. 1). Each frame is 36.4 $^{\prime \prime }$ wide, and one pixel corresponds to 0.91 $^{\prime \prime }$ on the sky.
Open with DEXTER

In the text

$\begin{figure} \par\includegraphics[angle=-90,width=16cm,clip]{8916fig5.ps} \end{figure}$	Figure 5: Same as Fig. 4, but for ESO 338-IG04 at PA 160 $^\circ$ -340 $^\circ$ . The dotted vertical lines in this case mark the positions along the slit of clusters 25 ( left) and 21 from the outer sample of Östlin et al. (1998) (see Fig. 1).
Open with DEXTER