All Figures

$\begin{figure} \par {\hspace*{3mm} \includegraphics[width=7.8cm,clip]{Gc161_f1.e... ...}}\vspace*{1.2cm} \includegraphics[width=8.35cm,clip]{Gc161_f2.eps}\end{figure}$ Figure 1: The 95 ${\mu }$ m map of the Lockman Hole LHEX ( upper panel) and LHNW ( lower panel) areas. The circles indicate our detected sources with signal-to-noise ratio >4. Each map is ${\sim }44'\times 44'$ .
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In the text

$\begin{figure} \par\includegraphics[width=5.4cm,clip]{Gc161_f3.eps} \end{figure}$ Figure 2: Example of a pair of ISOPHOT complex sources. The figure shows the optical R band image (Fadda et al. 2004, in prep.) with overlayed the 95 $~\mu$ m contours. The ISOPHOT positions are marked with open squares, the triangles indicate the ISOCAM 15 ${\mu }$ m detections (Fadda et al. 2004).
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In the text

$\begin{figure} \par\includegraphics[width=8.7cm,clip]{Gc161_f4.eps} \end{figure}$ Figure 3: Integral counts at 95 ${\mu }$ m. Our estimated values (starred filled symbols) are compared with data from a variety of other surveys (see text for references and details). The counts are expected to be dominated by extragalactic sources, for which some model predictions are also reported.
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In the text

$\begin{figure} \par\includegraphics[width=8.2cm,clip]{Gc161_f5.eps}\end{figure}$ Figure 4: Differential 95 ${\mu }$ m counts ${\rm d}N/{\rm d}S$ normalized to the Euclidean law ( $N \propto S^{-2.5}$ ). Symbols are the same as in Fig. 3. Our results are compared with those from the preliminary analysis of the ISOPHOT ELAIS survey (Efstathiou et al. 2000, open circles) and with those from Kawara et al. (2004, filled triangles). We also show as a long-dashed line the expected contribution of non-evolving spirals as in the model of Franceschini et al. (2001).
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In the text

$\begin{figure} \par {\hspace{3mm} \includegraphics[width=7.8cm,clip]{Gc161_f1.e... ...}}\vspace{1.2cm} \includegraphics[width=8.35cm,clip]{Gc161_f2.eps}\end{figure}$	Figure 1: The 95 ${\mu }$ m map of the Lockman Hole LHEX ( upper panel) and LHNW ( lower panel) areas. The circles indicate our detected sources with signal-to-noise ratio >4. Each map is ${\sim }44'\times 44'$ .
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$\begin{figure} \par\includegraphics[width=5.4cm,clip]{Gc161_f3.eps} \end{figure}$	Figure 2: Example of a pair of ISOPHOT complex sources. The figure shows the optical R band image (Fadda et al. 2004, in prep.) with overlayed the 95 $~\mu$ m contours. The ISOPHOT positions are marked with open squares, the triangles indicate the ISOCAM 15 ${\mu }$ m detections (Fadda et al. 2004).
Open with DEXTER

$\begin{figure} \par\includegraphics[width=8.7cm,clip]{Gc161_f4.eps} \end{figure}$	Figure 3: Integral counts at 95 ${\mu }$ m. Our estimated values (starred filled symbols) are compared with data from a variety of other surveys (see text for references and details). The counts are expected to be dominated by extragalactic sources, for which some model predictions are also reported.
Open with DEXTER