All Figures

$\begin{figure} \par\includegraphics[angle=-90,width=13cm,clip]{1836c1at.eps}\\ \includegraphics[angle=-90,width=13cm,clip]{1836c1ab.eps} \end{figure}$ Figure 1: a) The eastern part of the Perseus molecular cloud complex. Top: SCUBA 850 $\mu {\rm m}$ map. The colourscale (greyscale) is from 0 to 2281 mJy/beam on a square root (flux density) scale to bring out the low intensity features. Bottom: contours of C¹⁸O 1-0 integrated intensity at 1' resolution overlaid on 850 $\mu {\rm m}$ colourscale (greyscale). Contours are 1, 2, 4, 8, 16 K km s^-1. In both maps the black boundary marks the area mapped with SCUBA and the grey boundary marks the area mapped in C¹⁸O (note, B5 was not mapped in C¹⁸O). Some well-known clusters and IRAS sources are marked.
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In the text

$\begin{figure} \par\includegraphics[angle=-90,width=17.3cm,clip]{1836c1bt.eps}\\ \includegraphics[angle=-90,width=17.3cm,clip]{1836c1bb.eps} \end{figure}$ Figure 1: b) The western part of the Perseus molecular cloud complex. Top: SCUBA 850 $\mu {\rm m}$ map. The colourscale (greyscale) is from 0 to 2281 mJy/beam on a square root (flux density) scale to bring out the low intensity features. Bottom: contours of C¹⁸O 1-0 integrated intensity at 1' resolution overlaid on 850 $\mu {\rm m}$ colourscale (greyscale). Contours are 1, 2, 4, 8, 16 K km s^-1. In both maps the black boundary marks the area mapped with SCUBA and the grey boundary marks the area mapped in C¹⁸O (note, B5 was not mapped in C¹⁸O). Some well-known clusters and IRAS sources are marked.
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In the text

$\begin{figure} \includegraphics[width=17.3cm,angle=0]{1836c2.eps} \end{figure}$ Figure 2: SCUBA 850 $\mu {\rm m}$ maps of the a) B5, b) HH211, c) B1, d) L1448, e) NGC 1333, f) L1455, g) IRAS 03292+3039, h) IRAS 03282+3035 and i) IRAS 03271+3213 regions. Colourscale (greyscale) is 850 $\mu {\rm m}$ continuum from 0 (white) to 2281 mJy/beam (black) on a square root (flux density) scale to bring out the low intensity features. Black contours are 850 $\mu {\rm m}$ 100, 200, 400, 800, 1600, 3200 mJy/beam. White contours are 450 $\mu {\rm m}$ 2, 4, 8 Jy/beam. Dark green contours (thick grey contours) are where the C¹⁸O integrated intensity = 1 K km s^-1.
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In the text

$\begin{figure} \par\includegraphics[angle=-90,width=8.8cm,clip]{1836f3.eps} \end{figure}$ Figure 3: Probability of finding a submm core in a 22'' square pixel with a given 1' beam-averaged C¹⁸O integrated intensity: observed (thin black line) and probability distribution of $\log_{10}({P}(\hbox{core})) = N_{\rm cores}(I_i)/N_{\rm pixels}(I_i)$ for each integrated intensity bin I_i (greyscale), and best-fit power law (thick black line). To convert the probabilities to another pixel size use $P' = P(\hbox {core})\times {\hbox {(pixel area)}\over 22^2}\cdot$
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In the text

$\begin{figure} \par\includegraphics[scale=0.35,angle=-90]{1836fa1.eps} \end{figure}$ Figure A.1: Probability density function for the power law index $\alpha$ , $\log({P}(\alpha\vert x,y))$ . Verticals are 68.3%, 95.4% and 99.7% confidence limits.

In the text