Astronomy & Astrophysics

All Figures

$\begin{figure} \par\includegraphics[width=8.5cm,clip]{2189fig1.eps}\end{figure}$ Figure 1: Comparison between the true total infrared luminosity and the estimated luminosity of galaxies. Open triangles, open diamonds, open squares and filled squares represent the ratios $L_{\rm FIR}/L_{\rm IR}^{\rm total}$ , $L_{\rm TIR}/L_{\rm IR}^{\rm total}$ , $L_{\rm TIR2}/L_{\rm IR}^{\rm total}$ , and $L_{\rm IR}/L_{\rm IR}^{\rm total}$ , respectively.
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In the text

$\begin{figure} \par\includegraphics[width=7.5cm,clip]{2189fig2.eps}\end{figure}$ Figure 2: The relation between $12~\mu$ m luminosity $L(12~\mu\mbox{m})$ and ${L}_{{\rm IR}}$ , the estimate of the total infrared (IR) luminosity $L_{\rm IR}^{\rm total}$ proposed by Sanders & Mirabel (1996).
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In the text

$\begin{figure} \par\includegraphics[width=7.5cm,clip]{2189fig3.eps}\end{figure}$ Figure 3: The relation between $25~\mu$ m luminosity $L(25~\mu\mbox{m})$ and ${L}_{{\rm IR}}$ .
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In the text

$\begin{figure} \par\includegraphics[width=7.5cm,clip]{2189fig4.eps}\end{figure}$ Figure 4: The performance of the linear estimation formula obtained from the $L(12~\mu\mbox{m})$ - ${L}_{{\rm IR}}$ relation. Filled squares are the same as those in Fig. 1. The open squares are the estimates $L_{\rm IR}^{\rm linear}$ , obtained from the linear relation (Eq. (6)), normalized to ${L}_{{\rm IR}}$ . The vertical error bars correspond to the 95% confidence interval shown in Fig. 2. The linear relation gives reasonable values for normal galaxies.
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In the text

$\begin{figure} \par\includegraphics[width=7.5cm,clip]{2189fig5.eps}\end{figure}$ Figure 5: The performance of the linear estimation formula obtained from the $L(25~\mu\mbox{m})$ - ${L}_{{\rm IR}}$ relation. Symbols are as in Fig. 4, except that they are for $25~\mu$ m.
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In the text

$\begin{figure} \par\includegraphics[width=7.5cm,clip]{2189fig6.eps}\end{figure}$ Figure 6: The relation between $15~\mu$ m luminosity and ${L}_{{\rm IR}}$ for the quiescent galaxy sample of Boselli et al. (2003) with our formula for estimating ${L}_{{\rm IR}}$ . We also show the 95% confidence interval, which is the same as that obtained for the $L(12~\mu\mbox{m})$ - ${L}_{{\rm IR}}$ relation.
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In the text

$\begin{figure} \par\includegraphics[width=8.3cm,clip]{2189figa1.eps}\end{figure}$ Figure A.1: The galaxy sample with total IR luminosities, $L_{\rm IR}^{\rm total}= 10^{10}~L_\odot \mbox{--} 10^{11}~L_\odot$ .

In the text

$\begin{figure} \par\includegraphics[width=8.3cm,clip]{2189figa2.eps}\end{figure}$ Figure A.2: The IR-luminous galaxy sample, with $L_{\rm IR}^{\rm total}> 10^{11}~L_\odot$ .

In the text

$\begin{figure} \par\includegraphics[width=8.3cm,clip]{2189figa3.eps}\end{figure}$ Figure A.3: The dwarf galaxy sample, with $L_{\rm IR}^{\rm total}< 10^{10}~L_\odot$ . No observational data are available at FIR-submm for II Zw 40 and SBS 0335-052, we extrapolated the SEDs by the SED model for a young galaxy presented by Takeuchi et al. (2003). The extrapolated data are represented by filled squares.

In the text

$\begin{figure} \par\includegraphics[width=8.5cm,clip]{2189fig1.eps}\end{figure}$	Figure 1: Comparison between the true total infrared luminosity and the estimated luminosity of galaxies. Open triangles, open diamonds, open squares and filled squares represent the ratios $L_{\rm FIR}/L_{\rm IR}^{\rm total}$ , $L_{\rm TIR}/L_{\rm IR}^{\rm total}$ , $L_{\rm TIR2}/L_{\rm IR}^{\rm total}$ , and $L_{\rm IR}/L_{\rm IR}^{\rm total}$ , respectively.
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$\begin{figure} \par\includegraphics[width=7.5cm,clip]{2189fig2.eps}\end{figure}$	Figure 2: The relation between $12~\mu$ m luminosity $L(12~\mu\mbox{m})$ and ${L}_{{\rm IR}}$ , the estimate of the total infrared (IR) luminosity $L_{\rm IR}^{\rm total}$ proposed by Sanders & Mirabel (1996).
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$\begin{figure} \par\includegraphics[width=7.5cm,clip]{2189fig3.eps}\end{figure}$	Figure 3: The relation between $25~\mu$ m luminosity $L(25~\mu\mbox{m})$ and ${L}_{{\rm IR}}$ .
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$\begin{figure} \par\includegraphics[width=7.5cm,clip]{2189fig5.eps}\end{figure}$	Figure 5: The performance of the linear estimation formula obtained from the $L(25~\mu\mbox{m})$ - ${L}_{{\rm IR}}$ relation. Symbols are as in Fig. 4, except that they are for $25~\mu$ m.
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$\begin{figure} \par\includegraphics[width=7.5cm,clip]{2189fig6.eps}\end{figure}$	Figure 6: The relation between $15~\mu$ m luminosity and ${L}_{{\rm IR}}$ for the quiescent galaxy sample of Boselli et al. (2003) with our formula for estimating ${L}_{{\rm IR}}$ . We also show the 95% confidence interval, which is the same as that obtained for the $L(12~\mu\mbox{m})$ - ${L}_{{\rm IR}}$ relation.
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