All Figures

$\begin{figure} \par\includegraphics[width=17.5cm,clip]{a522f01.eps} \end{figure}$ Figure 1: Oxygen and nitrogen abundances, and nitrogen-to-oxygen abundance ratios versus galactocentric distance for late-type galaxies. The oxygen abundances are shown by filled circles, the linear least-squares fits to these data are presented by solid lines. The nitrogen abundances are shown by open squares, the linear least-squares fits to these data are presented by dashed lines. The nitrogen-to-oxygen abundance ratios are shown by open circles, the linear least-squares fits to these data are presented by solid lines. The galactocentric distances are normalized to the isophotal radius.
Open with DEXTER

In the text

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{a522f06.eps} \end{figure}$ Figure 6: The characteristic oxygen abundance as a function of absolute blue magnitude M_B for our sample of spiral galaxies. The solid line is the ${\rm O/H} - M_B$ relationship (best fit derived through the least squares method). The dashed lines correspond to the lines shifted by -0.2 dex and +0.2 dex along the vertical axes relatively to the derived ${\rm O/H} - M_B$ relationship. The dotted line is the ${\rm O/H} - M_B$ relationship for our sample of irregular galaxies extrapolated to the luminosity range of spiral galaxies. The line presented by the plus signs is the extrapolated ${\rm O/H} - M_B$ relationship for irregular galaxies derived by Richer & McCall (1995).
Open with DEXTER

In the text

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{a522f07.eps} \end{figure}$ Figure 7: The characteristic oxygen abundance as a function of rotation velocity for our sample of spiral galaxies. The solid line is the ${\rm O/H} -V_{\rm rot}$ relationship (best fit derived through the least squares method). The dashed lines correspond to the lines shifted by -0.2 dex and +0.2 dex relatively to the derived ${\rm O/H} -V_{\rm rot}$ relationship.
Open with DEXTER

In the text

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{a522f08.eps} \end{figure}$ Figure 8: The characteristic oxygen abundance as a function of Hubble type, expressed in the terms of T-type, for our sample of spiral galaxies. The solid line is the O/H-T relationship derived through the least squares method. The dashed lines correspond to the lines shifted by -0.2 dex and +0.2 dex relatively to the derived O/H-T relationship.
Open with DEXTER

In the text

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{a522f09.eps} \end{figure}$ Figure 9: The characteristic oxygen abundance as a function of absolute blue magnitude M_B for our sample of spiral galaxies (the filled circles). The solid line is the best (linear least-squares) fit to these data. The open squares are oxygen abundances in irregular galaxies, the dashed line is the metallicity-luminosity relationship for our sample of irregular galaxies. The dotted line is the O/H - M_B relationship for irregular galaxies derived by Lee et al. (2003). The O/H - M_B relationship for irregular galaxies derived by Richer & McCall (1995) is presented by the plus signs.
Open with DEXTER

In the text

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{a522f10.eps} \end{figure}$ Figure 10: The characteristic oxygen abundance as a function of rotation velocity $V_{\rm rot}$ for our sample of spiral galaxies (the filled circles). The solid line is the best (linear least-squares) fit to these data. The open squares are oxygen abundances in irregular galaxies, the dashed line is the linear least-squares fit to these data.
Open with DEXTER

In the text

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{a522f11.eps} \end{figure}$ Figure 11: The absolute blue magnitude M_B as a function of the rotation velocity. The filled circles are spiral galaxies, the open squares are irregular galaxies.
Open with DEXTER

In the text

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{a522f12.eps} \end{figure}$ Figure 12: Gas mass fraction as a function of the absolute blue magnitude M_B. The filled circles are spiral galaxies, the open squares are irregular galaxies. The solid line is the $\mu - M_B$ relationship for spiral galaxies, the dashed line is the $\mu - M_B$ relationship for irregular galaxies.
Open with DEXTER

In the text

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{a522f13.eps} \end{figure}$ Figure 13: a) Effective oxygen yield as a function of the absolute blue magnitude M_B. The filled circles are spiral galaxies, the open circles are irregular galaxies. The solid line is the $y_{\rm eff} - M_{B}$ relation for spiral galaxies (best fit). The dashed line corresponds to the mean $y_{\rm eff} = 0.00268$ for spiral galaxies. b) Effective oxygen yield as a function of the rotation velocity. Symbols are the same as in panel a).
Open with DEXTER

In the text

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{a522f14.eps} \end{figure}$ Figure 14: a) The positions of spiral (filled circles) and irregular (open squares) galaxies in the $\mu$ - O/H diagram together with the predictions of the closed-box models. The solid curve is the prediction of the closed-box model with oxygen yield y₀ = 0.00268(the mean value of the effective oxygen yields derived for spiral galaxies). The dashed curves correspond to the predictions of the closed-box models with oxygen yields $y=1.5\times y_0$ and y=y₀/1.5. The dotted curve is the prediction of the closed-box models with oxygen yields y=y₀/4. b) The oxygen abundances extrapolated to zero radius (open triangles) and extrapolated to the isophotal radius $R_{\rm 25}$ (filled triangles) in spiral galaxies with well defined radial oxygen abundance gradients together with the $\mu - {\rm O/H}$ track predicted by the closed-box model with oxygen yield y₀ = 0.00268. The large plus sign is the position of the solar vicinity region.
Open with DEXTER

In the text

$\begin{figure} \par\includegraphics[width=8cm,clip]{a522f15.eps} % \end{figure}$ Figure 15: Comparison of temperature-based oxygen abundances O/H $_{T_{\rm e}}$ with those derived with different calibrations for high-metallicity H II regions. a) The O/H_P - O/H $_{T_{\rm e}}$ diagram. The filled circles represent the O/H $_{T_{\rm e}}$ abundances for H II regions in the galaxy NGC 5457 from Kennicutt et al. (2003), the filled triangles are the O/H $_{T_{\rm e}}$ abundances for H II regions in this galaxy from other authors. The open squares are the O/H $_{T_{\rm e}}$ abundances for H II regions in other galaxies. The O/H_P abundances are derived through the high-metallicity P-calibration. The solid line is the equal-value line, the dashed lines are shifted by +0.15 dex and -0.15 dex. b) The O/H $_{\rm ZKH}$ - O/H $_{T_{\rm e}}$ diagram for the same H II regions. The O/H $_{\rm ZKH}$ abundances are derived using the high-metallicity calibration from Zaritsky et al. (1994). c) The O/H $_{\rm KKP}$ - O/H $_{T_{\rm e}}$ diagram for the same H II regions. The O/H $_{\rm KKP}$ abundances are derived using the high-metallicity calibration from Kobulnicky et al. (1999).
Open with DEXTER

In the text

$\begin{figure} \par\includegraphics[width=8cm,clip]{a522f16.eps} \end{figure}$ Figure 16: The oxygen abundance versus galactocentric distance for the galaxy NGC 5457. a) The filled circles are temperature-based abundances from Kennicutt et al. (2003). The solid line is the least squares fit to these data. The open circles are temperature-based abundances from other authors (compilation from Pilyugin 2001b). The dashed line is the least squares fit to all the temperature-based abundances. b) The filled circles are oxygen abundances derived through the high-metallicity P-calibration for a large sample of H II regions with $R_{\rm g} < 0.60 R_{\rm 25}$ . The best fit to these data is presented by the dashed line. The solid line is the same as in a). c) The filled circles are abundances derived using the calibration from Kobulnicky et al. (1999) for the same H II regions. The least squares fit to these data is presented by the dashed line.
Open with DEXTER

In the text

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{a522f17.eps} \end{figure}$ Figure 17: The characteristic oxygen abundance as a function of absolute blue magnitude M_B for our sample of spiral galaxies (the filled circles). The solid line is the O/H - M_B relationship (best fit derived through the least squares method). The dashed lines correspond to the lines shifted by -0.2 dex and +0.2 dex along the vertical axes relatively to the derived ${\rm O/H} - M_B$ relationship. The oxygen abundances in the galaxy NGC 5457 are presented by the open circle (O/H at $R=0.4R_{\rm 25}$ ) and open square (O/H at the disk half-light radius). The ${\rm O/H} - M_B$ relationship from Garnett (2002) is shown by plus signs.
Open with DEXTER

In the text

$\begin{figure} \par\includegraphics[width=17.5cm,clip]{a522f02.eps} \end{figure}$ Figure 2: Oxygen and nitrogen abundances and nitrogen-to-oxygen abundance ratio versus galactocentric distance for late-type galaxies. The oxygen abundances are shown by filled circles, the linear least-squares fits to these data are presented by solid lines. The nitrogen abundances are shown by open squares, the linear least-squares fits to these data are presented by dashed lines. The nitrogen-to-oxygen abundance ratios are shown by open circles, the linear least-squares fits to these data are presented by solid lines. The galactocentric distances are normalized to the isophotal radius. The H II regions with depleted oxygen abundances in NGC 2903 are shown by pluses.
Open with DEXTER

In the text

$\begin{figure} \par\includegraphics[width=17.5cm,clip]{a522f03.eps} \end{figure}$ Figure 3: Oxygen and nitrogen abundances and nitrogen-to-oxygen abundance ratio versus galactocentric distance for late-type galaxies. The oxygen abundances are shown by filled circles, the linear least-squares fits to these data are presented by solid lines. The nitrogen abundances are shown by open squares, the linear least-squares fits to these data are presented by dashed lines. The nitrogen-to-oxygen abundance ratios are shown by open circles, the linear least-squares fits to these data are presented by solid lines. The galactocentric distances are normalized to the isophotal radius.
Open with DEXTER

In the text

$\begin{figure} \par\includegraphics[width=17.5cm,clip]{a522f04.eps} \end{figure}$ Figure 4: Oxygen and nitrogen abundances and nitrogen-to-oxygen abundance ratio versus galactocentric distance for late-type galaxies. The oxygen abundances are shown by filled circles, the linear least-squares fits to these data are presented by solid lines. The nitrogen abundances are shown by open squares, the linear least-squares fits to these data are presented by dashed lines. The nitrogen-to-oxygen abundance ratios are shown by open circles, the linear least-squares fits to these data are presented by solid lines. The galactocentric distances are normalized to the isophotal radius.
Open with DEXTER

In the text

$\begin{figure} \par\includegraphics[width=17.5cm,clip]{a522f05.eps} \end{figure}$ Figure 5: Oxygen and nitrogen abundances and nitrogen-to-oxygen abundance ratio versus galactocentric distance for late-type galaxies. The oxygen abundances are shown by filled circles, the linear least-squares fits to these data are presented by solid lines. The nitrogen abundances are shown by open squares, the linear least-squares fits to these data are presented by dashed lines. The nitrogen-to-oxygen abundance ratios are shown by open circles, the linear least-squares fits to these data are presented by solid lines. The galactocentric distances are normalized to the isophotal radius.
Open with DEXTER

In the text

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{a522f07.eps} \end{figure}$	Figure 7: The characteristic oxygen abundance as a function of rotation velocity for our sample of spiral galaxies. The solid line is the ${\rm O/H} -V_{\rm rot}$ relationship (best fit derived through the least squares method). The dashed lines correspond to the lines shifted by -0.2 dex and +0.2 dex relatively to the derived ${\rm O/H} -V_{\rm rot}$ relationship.
Open with DEXTER

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{a522f08.eps} \end{figure}$	Figure 8: The characteristic oxygen abundance as a function of Hubble type, expressed in the terms of T-type, for our sample of spiral galaxies. The solid line is the O/H-T relationship derived through the least squares method. The dashed lines correspond to the lines shifted by -0.2 dex and +0.2 dex relatively to the derived O/H-T relationship.
Open with DEXTER

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{a522f10.eps} \end{figure}$	Figure 10: The characteristic oxygen abundance as a function of rotation velocity $V_{\rm rot}$ for our sample of spiral galaxies (the filled circles). The solid line is the best (linear least-squares) fit to these data. The open squares are oxygen abundances in irregular galaxies, the dashed line is the linear least-squares fit to these data.
Open with DEXTER

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{a522f11.eps} \end{figure}$	Figure 11: The absolute blue magnitude M_B as a function of the rotation velocity. The filled circles are spiral galaxies, the open squares are irregular galaxies.
Open with DEXTER

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{a522f12.eps} \end{figure}$	Figure 12: Gas mass fraction as a function of the absolute blue magnitude M_B. The filled circles are spiral galaxies, the open squares are irregular galaxies. The solid line is the $\mu - M_B$ relationship for spiral galaxies, the dashed line is the $\mu - M_B$ relationship for irregular galaxies.
Open with DEXTER