EDP Sciences
Free Access
Issue
A&A
Volume 508, Number 2, December III 2009
Page(s) 615 - 640
Section Extragalactic astronomy
DOI https://doi.org/10.1051/0004-6361/200912042
Published online 04 November 2009

Online Material

Table 1:  Journal of the intermediate-resolution long-slit spectroscopy observations, carried out using the 2.5 m INT, 2.56 m NOT and 4.2 m WHT telescopes and with the instrumentation as explained in text.

\begin{figure}
\par\includegraphics[width=8.8cm,clip]{12042f01.eps}
\end{figure} Figure 1:

IDS INT spectra for regions C, A, and B of Haro 15. Fluxes are not corrected for reddening. The most important emission lines have been labeled. See Fig. 3 in Paper I for the identification of the regions.

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\begin{figure}
\par\includegraphics[width=8.8cm,clip]{12042f02.eps}
\end{figure} Figure 2:

Lower panels: zoom of the spectra of regions C ( center), A, and B of Haro 15 ( bottom). Fluxes are not corrected for reddening. Upper panels: spatial distribution of the relative flux of [O II] $\lambda $3727 ( upper, right) and [O III] $\lambda $5007 ( upper, left) emission lines along the slit of PA 117$^{\circ }$.

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\begin{figure}
\par\includegraphics[width=8.8cm]{12042f03.eps}
\end{figure} Figure 3:

Position-velocity diagrams for the two slit positions observed in Haro 15. Both the H$\alpha $ and the [O III] $\lambda $5007 profiles have been analyzed. East is at the top in both diagrams. See Fig. 3 in Paper I for the identification of the regions.

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\begin{figure}
\par\includegraphics[width=8.8cm]{12042f04.eps}
\end{figure} Figure 4:

IDS INT spectra for the center of Mkn 1199 and the dwarf companion galaxy at its NE. Fluxes are not corrected for reddening. The most important emission lines have been labeled. See Fig. 5 in Paper I for the identification of the regions.

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\begin{figure}
\par\includegraphics[width=8.8cm]{12042f06.eps}
\end{figure} Figure 6:

Position-velocity diagrams for the two slit positions observed in Mkn 1199 using the H$\alpha $ profiles. NE is up in both diagrams. See Fig. 5 in Paper I for the identification of the regions.

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\begin{figure}
\par\includegraphics[width=8.8cm]{12042f07.eps}
\end{figure} Figure 7:

Spectra for the region A of Mkn 5 obtained using IDS at the INT (PA $349^{\circ }$) and ISIS at the WHT (PA $354^{\circ }$). Fluxes are not corrected for reddening. The most important emission lines have been labeled. See Fig. 7 in Paper I for the identification of the regions.

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\begin{figure}
\par\includegraphics[width=8.8cm,clip]{12042f08.eps}
\end{figure} Figure 8:

Position-velocity diagrams for the slit positions observed in Mkn 5 using the [O III] $\lambda $5007 profile. N is up in all diagrams. See Fig. 7 in Paper I for the identification of the regions.

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\begin{figure}
\par\includegraphics[width=8.8cm]{12042f09.eps}
\end{figure} Figure 9:

IDS INT spectra for the center of IRAS 0828+2816 and knot #8. Fluxes are not corrected for reddening. The most important emission lines have been labeled. See Fig. 9 in Paper I for the identification of the regions.

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\begin{figure}
\par\includegraphics[width=8.8cm]{12042f10.eps}
\end{figure} Figure 10:

Position-velocity diagrams for the three slit positions observed of IRAS 08208+2816 using the [O III] $\lambda $5007 profile. N is up in all diagrams. We have included the position of the regions (see Fig. 9 in Paper I for their identification), emphasizing those analyzed by spectroscopy. Notice that the lacking of data at the southern edge of the southern tail in the diagrams with PA 345$^{\circ }$ and 355$^{\circ }$ is because of the contamination by a bright star.

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\begin{figure}
\par\includegraphics[width=8.8cm]{12042f12.eps}
\end{figure} Figure 12:

Position-velocity diagram for the slit position observed in POX 4 using the [O III] $\lambda $5007 profile. NE is up. See Fig. 11 in Paper I for the identification of the regions.

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\begin{figure}
\par\includegraphics[width=8.8cm]{12042f13.eps}
\end{figure} Figure 13:

ISIS 4.2 m WHT spectrum for the center of UM 420 (top) and the galaxy UGC 1809 (bottom). Fluxes are not corrected for reddening. The most important emission lines have been labeled.

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\begin{figure}
\par\includegraphics[width=8.8cm]{12042f15.eps}
\end{figure} Figure 15:

Position-velocity diagram for the slit position observed in UM 420 using both the H$\alpha $ and H$\beta $ profiles. W is up.

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\begin{figure}
\par\includegraphics[width=8.8cm]{12042f16.eps}
\end{figure} Figure 16:

ISIS 4.2 m WHT spectrum for SBS 0926+606 A. Fluxes are not corrected for reddening. The most important emission lines have been labeled. See Fig. 15 in Paper I for the identification of this region.

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\begin{figure}
\par\includegraphics[width=8.8cm]{12042f17.eps}
\end{figure} Figure 17:

Position-velocity diagram for the slit position with PA 14$^{\circ }$ observed in SBS 0926+606 using the H$\alpha $ profile. Notice that the y-axis is broken. NE is up. See Fig. 15 in Paper I for the identification of the regions.

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\begin{figure}
\par\includegraphics[width=8.8cm]{12042f18.eps}
\end{figure} Figure 18:

ISIS 4.2 m WHT spectrum for SBS 0948+532 using a slit with PA 114$^{\circ }$. Fluxes are not corrected for reddening. The most important emission lines have been labeled.

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\begin{figure}
\par\includegraphics[width=8.8cm]{12042f19.eps}
\end{figure} Figure 19:

Position-velocity diagram for the slit position with PA 114$^{\circ }$ observed in SBS 0948+532 using the [O III] $\lambda $5007 profile. NW is up (see Fig. 17 in Paper I).

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\begin{figure}
\par\includegraphics[width=8.8cm,clip]{12042f20.eps}
\end{figure} Figure 20:

IDS 2.5 m INT spectrum for SBS 1054+364 using a slit with PA 55$^{\circ }$. Fluxes are not corrected for reddening. The most important emission lines have been labeled. See Fig. 19 in Paper I for identification of the region.

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\begin{figure}
\par\includegraphics[width=8.8cm]{12042f21.eps}
\end{figure} Figure 21:

Position-velocity diagram for the slit position observed in SBS 1054+365 using the H$\alpha $ profile. NE is up. See Fig. 19 in Paper I for identification of the regions.

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\begin{figure}
\par\includegraphics[width=8.8cm]{12042f22.eps}
\end{figure} Figure 22:

ISIS 4.2 m WHT spectrum for SBS 1211+540 using a slit with PA 138$^{\circ }$. Fluxes are not corrected for reddening. The most important emission lines have been labeled. See Fig. 21 in Paper I for identification of the region.

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\begin{figure}
\par\includegraphics[width=8.8cm]{12042f23.eps}
\end{figure} Figure 23:

Position-velocity diagram for the slit position with PA 138$^{\circ }$ observed in SBS 1211+532 using the [O III] $\lambda $5007 profile. NW is up. See Fig. 21 in Paper I for identification of the regions.

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\begin{figure}
\par\includegraphics[width=8.8cm]{12042f24.eps}
\end{figure} Figure 24:

ISIS 4.2 m WHT spectrum for regions A (top) and C (bottom) of SBS 1319+579 obtained with a slit with PA 49$^{\circ }$. Fluxes are not corrected for reddening. The most important emission lines have been labeled. See Fig. 23 in Paper I for identification of the regions.

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\begin{figure}
\par\includegraphics[width=8.8cm]{12042f25.eps}
\end{figure} Figure 25:

Position-velocity diagram for the slit position observed in SBS 1319+579 using the H$\alpha $ profile. The relative intensity of the H$\alpha $ emission along the spatial direction is also shown, identifying all observed regions. NE is up. See Fig. 23 in Paper I for identification of the regions.

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\begin{figure}
\par\includegraphics[width=8.8cm]{12042f26.eps}
\end{figure} Figure 26:

ISIS 4.2 m WHT spectrum for regions C (top) and A (bottom) of SBS 1415+437 using a slit with PA 20$^{\circ }$. Fluxes are not corrected for reddening. The most important emission lines have been labeled. See Fig. 25 in Paper I for identification of the regions.

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\begin{figure}
\par\includegraphics[width=8.8cm]{12042f27.eps}
\end{figure} Figure 27:

Position-velocity diagram for the slit position with PA 20$^{\circ }$ observed in SBS 1415+437 using the H$\alpha $ profile. NE is up. See Fig. 25 in Paper I for identification of the regions.

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\begin{figure}
\par\includegraphics[width=8.8cm]{12042f28.eps}
\end{figure} Figure 28:

IDS INT spectra for the regions A (bottom) and B (top) of IRAS III Zw 107. Fluxes are not corrected for reddening. The most important emission lines have been labeled. See Fig. 27 in Paper I for identification of the regions.

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\begin{figure}
\par\includegraphics[width=8.8cm]{12042f29.eps}
\end{figure} Figure 29:

Position-velocity diagram for the slit position with PA 0$^{\circ }$ observed in III Zw 107 using the H$\alpha $ profile. N is up. See Fig. 27 in Paper I for identification of the regions.

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\begin{figure}
\par\includegraphics[width=8.8cm]{12042f30.eps}
\end{figure} Figure 30:

IDS INT spectrum (bottom) using a slit with PA 49$^{\circ }$ and ALFOSC 2.56 m NOT spectrum (top) using a slit of PA 109$^{\circ }$ of Tol 9. Fluxes are not been corrected for reddening. The most important emission lines have been labeled. See Figs. 29 and 30 in Paper I for identification of the regions.

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\begin{figure}
\par\includegraphics[width=8.8cm]{12042f32.eps}
\end{figure} Figure 32:

ALFOSC 2.56 m NOT spectra of the regions analyzed in Tol 1457-262. Fluxes are not corrected for reddening. The most important emission lines have been labeled. See Fig. 31 in Paper I for identification of the regions.

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\begin{figure}
\par\includegraphics[width=8.8cm]{12042f33.eps}
\end{figure} Figure 33:

Position-velocity diagram for the slit position observed in Object 1 of Tol 1457-262 using the H$\alpha $ profile. The relative intensity of the H$\alpha $ emission along the spatial direction is also shown, identifying all observed regions. NW is up. See Fig. 31 in Paper I for identification of the regions.

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\begin{figure}
\par\includegraphics[width=8.8cm]{12042f34.eps}
\end{figure} Figure 34:

ALFOSC 2.56 m NOT spectra for the galaxy pair ESO 566-8 (top) and ESO 566-7 (bottom) that constitute Arp 256. Fluxes are not been corrected for reddening. The most important emission lines have been labeled. See Fig. 34 in Paper I for identification of the galaxies.

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\begin{figure}
\par\includegraphics[width=8.8cm]{12042f35.eps}
\end{figure} Figure 35:

Position-velocity diagram for the slit position observed in Arp 252 using the H$\alpha $ profile. Notice that the y-axis is broken in two parts. N is up. See Fig. 34 in Paper I for identification of the galaxies.

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Appendix A: Tables

Table A.1:   Dereddened line intensity ratios with respect to I(H$\beta $) = 100 for knots analyzed in Haro 15.

Table A.2:   Physical conditions and chemical abundances of the ionized gas of the regions analyzed in Haro 15.

Table A.3:   Dereddened line intensity ratios with respect to I(H$\beta $)=100 for knots analyzed in Mkn 1199.

Table A.4:   Physical conditions and chemical abundances of the ionized gas of the regions analyzed in Mkn 1199.

Table A.5:   Dereddened line intensity ratios with respect to I(H$\beta $)=100 for knots analyzed in Mkn 5. Region A was observed using three slit positions with a PA of 0$^{\circ }$ (INT-1), 349$^{\circ }$ = -11$^{\circ }$ (INT-2), and 354$^{\circ }$ = -6$^{\circ }$ (WHT).

Table A.6:   Physical conditions and chemical abundances of the ionized gas of the regions analyzed in Mkn 5.

Table A.7:   Dereddened line intensity ratios with respect to I(H$\beta $) = 100 for regions analyzed in IRAS 08208+2816. The slit positions that we used for each knot are: PA 345$^{\circ }$ for C, PA 355$^{\circ }$ for #8 and #10, and PA 10$^{\circ }$ for #3 y #5.

Table A.8:   Physical conditions and chemical abundances of the ionized gas of the regions analyzed in IRAS 08208+2816.

Table A.9:   Dereddened line intensity ratios with respect to I(H$\beta $)=100 for regions analyzed in POX 4, UM 420, and SBS 0926+606.

Table A.10:   Physical conditions and chemical abundances of the ionized gas in POX 4, UM 420, and SBS 0926+606.

Table A.11:   Dereddened line intensity ratios with respect to I(H$\beta $) = 100 for regions analyzed in SBS 0948+532, SBS 1054+365, and SBS 1211+540.

Table A.12:   Physical conditions and chemical abundances of the ionized gas in SBS 0948+532, SBS 1054+365, and SBS 1211+540.

Table A.13:   Dereddened line intensity ratios with respect to I(H$\beta $) = 100 for knots analyzed in SBS 1319+579 (regions A, B, and C) and SBS 1415+457 (regions C and A).

Table A.14:   Physical conditions and chemical abundances of the ionized gas for the regions analyzed in SBS 1319+579 and SBS 1415+437.

Table A.15:   Dereddened line intensity ratios with respect to I(H$\beta $) = 100 for knots analyzed in III Zw 107 (regions A, B, and C) and Tol 9 (spectra obtained with 2.5 m INT and 2.56 m NOT).

Table A.16:   Physical conditions and chemical abundances of the ionized gas for the regions analyzed in III Zw 107 and Tol 9.

Table A.17:   Dereddened line intensity ratios with respect to I(H$\beta $) = 100 for knots analyzed in Tol 1457-262 (regions A, B, and C) and Arp 252 (galaxy A, ESO 566-8, and galaxy B, ESO 566-7).

Table A.18:   Physical conditions and chemical abundances of the ionized gas for the regions analyzed in Tol 1457-262 and Arp 252 (galaxy A, ESO 566-8, and galaxy B, ESO 566-7).

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