Astronomy & Astrophysics

All Figures

$\begin{figure} \par\includegraphics[angle=-0,width=8cm,clip]{0646fi1.ps} \end{figure}$ Figure 1: Morphology of HS 0837+4717 as seen in the Wise V-band image. North is up, East is to the left. The positions of MMT ( $\rm PA=16\hbox {$^\circ $ }$ ) and BTA ( $\rm PA=44\hbox {$^\circ $ }$ and 130 $^\circ$ ) long slits are shown. The isophotes sample the image at the brightness levels of 11, 20, 30, 50, 75, 100, 150, 200 and 220 units. The minimal level corresponds to $\sim$ 1.5 $\sigma$ of the noise. See Sect. 3.5.
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In the text

$\begin{figure} \par {\hspace*{1.2cm} \includegraphics[angle=-90,width=11.6cm,cli... ...ce*{2mm} \includegraphics[angle=0,width=6.9cm,clip]{0646fi2d.ps} \end{figure}$ Figure 2: Upper panel: the MMT 2D spectrum of HS 0837+4717 with $\rm PA=16\hbox {$^\circ $ }$ , plotted with the contrast level adjusted so as to show the distribution of the continuum intensity along the slit. SSW is up. While the intensity of strong lines decreases symmetrically relative to the continuum brightness peak, the continuum intensity at the lower level is skewed to the SSW direction, indicating a slightly non-central position of the starburst. Middle panel: de-redshifted MMT 1D spectrum of the bright H II region in HS 0837+4717, extracted with the aperture of $1\hbox{$.\!\!^{\prime\prime}$ }5\times3\hbox{$.\!\!^{\prime\prime}$ }0$ . Bottom panel: de-redshifted 1D blue and red BTA spectra. Note the good consistency between the MMT and BTA spectra.
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In the text

$\begin{figure} \par\includegraphics[angle=-90,width=6.5cm,clip=]{0646fi3a.ps}\pa... ...e*{2mm} \includegraphics[angle=-90,width=6.5cm,clip=]{0646fi3c.ps} \end{figure}$ Figure 3: Gaussian multicomponent fitting (solid lines) of the BTA spectra of HS 0837+4717 (dotted lines). Top panel: region of the blue bump; middle panel: region of H $\beta$ and [O III] $\lambda \lambda$ 4959,5007; bottom panel: region of H $\alpha$ , [N II] $\lambda \lambda$ 6548,6583.
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In the text

$\begin{figure} \par\includegraphics[angle=-0,width=8cm,clip]{0646fi4.ps} \end{figure}$ Figure 4: Distribution of $\log$ (N/O) ratio versus $12+\log$ (O/H) for the BCG sample from Izotov & Thuan (1999) with the value for HS 0837+4717 shown. Data for Haro 11 and Mkn 996 are from Bergvall & Östlin (2002) and Thuan et al. (1996), respectively. The three galaxies with $\log$ (N/O) in the range -1.1 to -1.0 are UM 420, UM 448 and Mkn 1089.
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In the text

$\begin{figure} \par\mbox{ \includegraphics[angle=-0,width=5.1cm,clip]{0646fi5a.p... ...2mm} \includegraphics[angle=-0,width=5.1cm,clip]{0646fi5c.ps} } \end{figure}$ Figure 5: Left panel: intensity distribution along the slit of the continuum between H $\delta$ and H $\gamma$ . The dashed line shows the PSF (point-spread function) fitted to the central peak (related to the starburst). The dotted line shows the difference between the observed full light and that of the central bright compact region. The additional component, centered at $\approx$ 2 $.\!\!^{\prime\prime}$ 2 to the SSW is $\sim$ 0.25 of the bright peak amplitude. Middle panel: same as in the left panel, but for continuum in the red. The relative flux of the fainter knot is 0.28, that is a factor of 1.13 larger than in the blue. This implies that this knot in (B-R) is $\sim$ 0 $.\!\!^{\rm m}$ 13 redder than the central starburst, which mainly defines the integrated colours of the BCG. Right panel: same as the left panel, but for intensity centered on the H $\alpha$ line. No significant signal is seen at the periphery besides the scattered light from the central bright region.
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In the text

$\begin{figure} \par\mbox{\includegraphics[angle=-0,width=7cm,clip]{0646fi6a.ps} \includegraphics[angle=-0,width=7cm,clip]{0646fi6b.ps} } \end{figure}$ Figure 6: Left panel: intensity distribution of H $\alpha$ along the slit at $\rm PA=44\hbox {$^\circ $ }$ and the respective P-V diagram (binned with 3 pixels, or 1 $.\!\!^{\prime\prime}$ 2, corresponding to the seeing). The radial velocity increases monotonously in the SW direction, resembling the receding branch of rotation curve with the amplitude of 50-70 km s^-1. However, the expected approaching branch for negative coordinates in the direction to NE is absent (see text for discussion). Right panel: same as in the left panel but at $\rm PA=130\hbox {$^\circ $ }$ . The velocity variations in the central part of this cross-section are significantly smaller than those at $\rm PA=44\hbox {$^\circ $ }$ . This would be expected due to the small projection of the rotation velocity onto the minor axis. There seems to be a large velocity disturbance at the NW edge, where radial velocity steeply raises to 60-70 ( $\pm 30$ ) km s^-1 in the two last points. The small velocity variations are also observed on the opposite side of the galaxy.
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In the text

$\begin{figure} \par\includegraphics[angle=-90,width=6.5cm,clip=]{0646fi3a.ps}\pa... ...e*{2mm} \includegraphics[angle=-90,width=6.5cm,clip=]{0646fi3c.ps} \end{figure}$	Figure 3: Gaussian multicomponent fitting (solid lines) of the BTA spectra of HS 0837+4717 (dotted lines). Top panel: region of the blue bump; middle panel: region of H $\beta$ and [O III] $\lambda \lambda$ 4959,5007; bottom panel: region of H $\alpha$ , [N II] $\lambda \lambda$ 6548,6583.
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$\begin{figure} \par\includegraphics[angle=-0,width=8cm,clip]{0646fi4.ps} \end{figure}$	Figure 4: Distribution of $\log$ (N/O) ratio versus $12+\log$ (O/H) for the BCG sample from Izotov & Thuan (1999) with the value for HS 0837+4717 shown. Data for Haro 11 and Mkn 996 are from Bergvall & Östlin (2002) and Thuan et al. (1996), respectively. The three galaxies with $\log$ (N/O) in the range -1.1 to -1.0 are UM 420, UM 448 and Mkn 1089.
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