All Figures

$\begin{figure} \par\includegraphics[angle=-90,width=8.2cm,clip]{8560fig1.ps}\end{figure}$ Figure 1: The distribution of absolute blue magnitudes within the parent sample of 863 galaxies, as a function of distance in Mpc. The solid line corresponds to the apparent magnitude limit of B= 15.5 mag used in selecting the galaxies. Black/filled symbols denote the observed subsample, and red/open symbols the remaining unobserved galaxies.
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In the text

$\begin{figure} \par\includegraphics[angle=-90,width=8.2cm,clip]{8560fg2a.ps}\vspace*{1mm} \includegraphics[angle=-90,width=8.2cm,clip]{8560fg2b.ps}\end{figure}$ Figure 2: a) The luminosity function for the entire parent sample, types S0a - Im, plotted as points with error bars; the solid line shows the luminosity function from the SDSS blue sequence. b) Luminosity functions including all galaxy types: SDSS (solid line); this study with all Virgo galaxies included (dashed line); and this study with galaxies excluded out to 10 $^\circ$ from the centre of the Virgo cluster (dot-dashed line).
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In the text

$\begin{figure} \par\includegraphics[angle=-90,width=8.2cm,clip]{8560fig3.ps}\end{figure}$ Figure 3: The log of the SFR to B-band luminosity ratio, plotted against the log of the B-band luminosity, for the observed galaxies. Circled points denote early types, T= 0-2; stars are intermediate types, T= 3-7; and filled circles are late types, T = 8-10.
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In the text

$\begin{figure} \par\includegraphics[angle=-90,width=8.2cm,clip]{8560fg4a.ps}\vspace*{2mm} \includegraphics[angle=-90,width=8.2cm,clip]{8560fg4b.ps}\end{figure}$ Figure 4: The distribution of absolute magnitudes amongst each galaxy T-type for both the parent a) and the observed b) samples.
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In the text

$\begin{figure} \par\includegraphics[angle=-90,width=8.2cm,clip]{8560fig5.ps}\end{figure}$ Figure 5: The H $\alpha$ luminosity function derived from our parent sample, with type-dependent extinction corrections. The dashed line shows H $\alpha$ luminosity function of Gallego et al. (1995). The horizontal scale is given both in terms of Log (H $\alpha$ ) luminosity, in Watts ( bottom scale), and Log (SFR), in solar masses per year ( top scale).
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In the text

$\begin{figure} \par\includegraphics[angle=-90,width=8.2cm,clip]{8560fg6a.ps}\vspace*{1mm} \includegraphics[angle=-90,width=8.2cm,clip]{8560fg6b.ps}\end{figure}$ Figure 6: SFR density as a function of absolute blue magnitude found using the points in the B-band luminosity function shown in Fig. 2 ( top); and using the SDSS B-band luminosity function ( bottom). The cumulative fraction of the SFR density is shown by the dot-dashed line in each plot; the scale for this fraction is marked along the right-hand axis.
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In the text

$\begin{figure} \par\includegraphics[angle=-90,width=8.2cm,clip]{8560fig7.ps}\end{figure}$ Figure 7: SFR density as a function of galaxy morphological type, with galaxy numbers drawn from our B-band luminosity function.
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In the text

$\begin{figure} \par\includegraphics[width=8.1cm,clip]{8560fga1.ps}\hspace*{0.45cm} \includegraphics[width=8.1cm,clip]{8560fga2.ps}\end{figure}$ Figure A.1: Morphological classifications in the CMD for galaxies. Left: NFGS sample. Right: a subset of the JPG sample. The dashed line in both plots represents an optimal divider between the red and blue sequences determined from a larger SDSS sample.
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In the text

$\begin{figure} \par\includegraphics[width=8.3cm,clip]{8560fga3.ps}\end{figure}$ Figure A.2: Morphological classifications in the CMD for galaxies. As per Fig. A.1 ( right) except using g-r Petrosian colours instead of u-r model colours. The dashed line represents an optimal divider determined by eye from a larger SDSS sample: $(g-r)_{\rm divide} = 0.65 - 0.023 (M_{\rm b} + 20)$ .
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In the text

$\begin{figure} \par\includegraphics[angle=-90,width=8.2cm,clip]{8560fig1.ps}\end{figure}$	Figure 1: The distribution of absolute blue magnitudes within the parent sample of 863 galaxies, as a function of distance in Mpc. The solid line corresponds to the apparent magnitude limit of B= 15.5 mag used in selecting the galaxies. Black/filled symbols denote the observed subsample, and red/open symbols the remaining unobserved galaxies.
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$\begin{figure} \par\includegraphics[angle=-90,width=8.2cm,clip]{8560fig3.ps}\end{figure}$	Figure 3: The log of the SFR to B-band luminosity ratio, plotted against the log of the B-band luminosity, for the observed galaxies. Circled points denote early types, T= 0-2; stars are intermediate types, T= 3-7; and filled circles are late types, T = 8-10.
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$\begin{figure} \par\includegraphics[angle=-90,width=8.2cm,clip]{8560fg4a.ps}\vspace*{2mm} \includegraphics[angle=-90,width=8.2cm,clip]{8560fg4b.ps}\end{figure}$	Figure 4: The distribution of absolute magnitudes amongst each galaxy T-type for both the parent a) and the observed b) samples.
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$\begin{figure} \par\includegraphics[angle=-90,width=8.2cm,clip]{8560fig5.ps}\end{figure}$	Figure 5: The H $\alpha$ luminosity function derived from our parent sample, with type-dependent extinction corrections. The dashed line shows H $\alpha$ luminosity function of Gallego et al. (1995). The horizontal scale is given both in terms of Log (H $\alpha$ ) luminosity, in Watts ( bottom scale), and Log (SFR), in solar masses per year ( top scale).
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$\begin{figure} \par\includegraphics[angle=-90,width=8.2cm,clip]{8560fg6a.ps}\vspace*{1mm} \includegraphics[angle=-90,width=8.2cm,clip]{8560fg6b.ps}\end{figure}$	Figure 6: SFR density as a function of absolute blue magnitude found using the points in the B-band luminosity function shown in Fig. 2 ( top); and using the SDSS B-band luminosity function ( bottom). The cumulative fraction of the SFR density is shown by the dot-dashed line in each plot; the scale for this fraction is marked along the right-hand axis.
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$\begin{figure} \par\includegraphics[angle=-90,width=8.2cm,clip]{8560fig7.ps}\end{figure}$	Figure 7: SFR density as a function of galaxy morphological type, with galaxy numbers drawn from our B-band luminosity function.
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$\begin{figure} \par\includegraphics[width=8.1cm,clip]{8560fga1.ps}\hspace*{0.45cm} \includegraphics[width=8.1cm,clip]{8560fga2.ps}\end{figure}$	Figure A.1: Morphological classifications in the CMD for galaxies. Left: NFGS sample. Right: a subset of the JPG sample. The dashed line in both plots represents an optimal divider between the red and blue sequences determined from a larger SDSS sample.
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$\begin{figure} \par\includegraphics[width=8.3cm,clip]{8560fga3.ps}\end{figure}$	Figure A.2: Morphological classifications in the CMD for galaxies. As per Fig. A.1 ( right) except using g-r Petrosian colours instead of u-r model colours. The dashed line represents an optimal divider determined by eye from a larger SDSS sample: $(g-r)_{\rm divide} = 0.65 - 0.023 (M_{\rm b} + 20)$ .
Open with DEXTER