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$\begin{figure} \par\includegraphics[width=16.5cm,clip]{6467f1.ps} \end{figure}$ Figure 1: ¹²CO 3-2 outflow maps. Colourscale: 850 $\mu {\rm m}$ SCUBA map with black contours at 100, 200, 400, 800, 1600 mJy/beam. The area observed in ¹²CO 3-2 is outlined in green. Outflows are displayed as a renzogram, equivalent to superimposing a series of channel maps each with one contour at a fixed intensity level (e.g. Kregel et al. 2004). a) Region to the SE of IC 348 The renzogram intensity level is 3 K km s^-1 and included channels from -5-7 km s^-1 (blue) and 11-15 km s^-1 (red). b) IC 348 including HH211 (12) and IC 348 mms (13): 2 K km s^-1 from -5-6 km s^-1 (blue) and 11-15 km s^-1 (red). c) B1 including B1-c (1), B1-bN/S (2), b1-d (4) and IRAS 03301+3057 (7): 3 K km s^-1, from -5-4 km s^-1 (blue) and 9-15 km s^-1 (red). d) B5 IRS1 (78) and (79) 2.5 K km s^-1, -5-8 (blue) and 12-15 km s^-1 (red). e) IRAS 03235+3004 (80) 2.0 K km s^-1, -5-3 (blue) and 6-15 km s^-1 (red). f) L1455 including RNO15 (35), PP9 (37), and L1455 FIR2 (39): 1.8 K km s^-1 from -5-2 km s^-1 (blue) and 11-18 km s^-1 (red). g) L1448 including L1448 N/NW (27), L1448 C (28) and L1448 IRS2 (30): 3.0 K km s^-1 from -5-0 km s^-1 (blue) and 8-15 km s^-1 (red). h) IRAS 03292+3039 (76): 2.0 K km s^-1, -5-4 (blue) and 9-15 km s^-1 (red). i) IRAS 03282+3035 (77): 3.0 K km s^-1, -5-5 (blue) and 7-15 km s^-1 (red). j) Region in the N of NGC 1333. 2 K km s^-1 from -5-1 km s^-1 (blue) and 12-15 km s^-1 (red). k) 03271+3013 (81) 1.0 K km s^-1, -5-6 (blue) and 8-15 km s^-1 (red).
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In the text

$\begin{figure} \par\includegraphics[width=9.4cm,clip]{6467f2.eps} \end{figure}$ Figure 1: continued. NGC 1333 from data first published in Knee & Sandell (2000). The renzogram intensity level is 3 K km s^-1 and included channels from -5-3 km s^-1 (blue) and 12-18 km s^-1 (red). 850 $\mu {\rm m}$ contours and colourscale are as before.
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In the text

$\begin{figure} \par\includegraphics[angle=-90,width=12cm,clip,origin=rb]{6467f3.ps}\end{figure}$ Figure 2: $L_{\rm bol}$ vs. $M_{\rm env}$ for all submm cores in Perseus (Paper I; Paper II) with ¹²CO targets marked by small black circles and outflow detections additionally marked by large black circles. Class 0 sources are marked as asterisks ( $\ast$ , red) and Class I by open stars (blue). The remaining sources (dots) are assumed starless. The horizontal line at 0.25 $L_{\odot }$ marks the lower luminosity limit for the outflow sample, and the vertical dashed line at 0.3 $M_{\odot }$ marks the $3\sigma$ detection limit for the SCUBA survey.
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In the text

$\begin{figure} \par\includegraphics[width=7.8cm,clip]{6467f4.ps}\end{figure}$ Figure 3: Top: fraction of outflow sources as a function of core mass for sources with definite outflows (solid thick line). The thin line shows the number of Class I sources as classified in Paper II. The ratio of protostars to starless cores decreases with decreasing mass. Bottom: as above with the fraction of protostars corrected for the outflow detection statistics in that mass bin. The greyscale gives the probability distribution of the fraction of protostars (see Appendix).
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In the text

$\begin{figure} \par\includegraphics[width=6.6cm,clip]{6467f5.ps}\end{figure}$ Figure 4: Relationships between momentum flux and ( top to bottom) bolometric luminosity $L_{\rm bol}$ , core mass $M_{\rm env}$ , and bolometric temperature $T_{\rm bol}$ . Sources marked by open stars (blue) and asterisks (red) are Class I and Class 0 respectively based on the SED (Paper II). The top two panels show best fits corresponding to $F_{\rm CO} \propto \mbox{$L_{\rm bol}$ }^{1.5}$ and $F_{\rm CO} \propto \mbox{$M_{\rm env}$ }^{1.5}$ respectively. Uncertainties on $F_{\rm CO}$ (see Sect. 4) are shown; uncertainties on $L_{\rm bol}$ are typically 30%, $M_{\rm env}$ at least a factor 2, and $T_{\rm bol}$ a few Kelvin.
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In the text

$\begin{figure} \par\includegraphics[width=6.75cm,clip]{6467f6.ps}\end{figure}$ Figure 5: Histograms of momentum flux for Class 0 (solid) and Class I (dotted) protostars.
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In the text

$\begin{figure} \par\includegraphics[width=8.3cm,clip]{6467f7.ps}\end{figure}$ Figure 6: $F_{\rm CO}~ c / \mbox{$L_{\rm bol}$ }$ (dimensionless) vs. $\mbox{$M_{\rm env}$ }/\mbox{$L_{\rm bol}$ }^{0.5}$ (in $\mbox{$M_{\odot}$ }$ nd $\mbox{$L_{\odot}$ }$ respectively). See also Bontemps et al. (1996, Fig. 7#. Sources marked by open stars (blue) and asterisks (red) are Class I and Class 0 respectively based on the SED (Paper II).
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In the text

$\begin{figure} \par\includegraphics[angle=-90,width=12cm,clip,origin=rb]{6467f8.ps}\end{figure}$ Figure 7: Core destruction timescales at current outflow mass loss rate, vs. left bolometric temperature; right current core mass. Class I sources (Hatchell et al. 2007, based on the SED), are marked by (blue) open stars and Class 0 sources by (red) asterisks.
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In the text

$\begin{figure} \par\includegraphics[width=6.8cm,clip]{6467f9.ps}\end{figure}$ Figure 8: Histograms of core destruction timescales for Class 0 (solid) and Class I (dotted) protostars. Sources with upper limits on the lifetime are excluded.
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In the text

$\begin{figure} \par\includegraphics[width=17cm,clip]{6467f10.ps}\end{figure}$ Figure 9: ¹²CO 3-2 spectra for outflow sources showing linewings at the 1.5 K ( $3\sigma$ ) level at least 3 km s^-1 from the ambient velocity (marked by inner solid and vertical lines). The outer vertical lines mark the range of velocities included in the momentum flux calculation.
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In the text

$\begin{figure} \par\includegraphics[width=17cm,clip]{6467f11.ps} \end{figure}$ Figure 9: continued.
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In the text

$\begin{figure} \par\includegraphics[width=17cm,clip]{6467f12.ps} \end{figure}$ Figure 9: continued.
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In the text

$\begin{figure} \par\includegraphics[width=17cm,clip]{6467f13.ps} \end{figure}$ Figure 9: continued.
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In the text

$\begin{figure} \par\includegraphics[width=17cm,clip]{6467f14.ps} \end{figure}$ Figure 9: continued.
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In the text

$\begin{figure} \par\includegraphics[width=17cm,clip]{6467f15.ps} \end{figure}$ Figure 9: continued.
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In the text

$\begin{figure} \par\includegraphics[width=17cm,clip]{6467f16.ps} \end{figure}$ Figure 9: continued.
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In the text

$\begin{figure} \par\includegraphics[width=17cm,clip]{6467f17.ps} \end{figure}$ Figure 9: continued.
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In the text

$\begin{figure} \par\includegraphics[width=17cm,clip]{6467f18.ps}\end{figure}$ Figure 10: ¹²CO 3-2 spectra for sources with no outflow, showing no linewings above the 1.5 K ( $3\sigma$ ) level (upper horizontal solid line) at 3 km s^-1 from the ambient velocity (inner solid and vertical lines).
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In the text

$\begin{figure} \par\includegraphics[width=9.4cm,clip]{6467f2.eps} \end{figure}$	Figure 1: continued. NGC 1333 from data first published in Knee & Sandell (2000). The renzogram intensity level is 3 K km s^-1 and included channels from -5-3 km s^-1 (blue) and 12-18 km s^-1 (red). 850 $\mu {\rm m}$ contours and colourscale are as before.
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$\begin{figure} \par\includegraphics[width=6.75cm,clip]{6467f6.ps}\end{figure}$	Figure 5: Histograms of momentum flux for Class 0 (solid) and Class I (dotted) protostars.
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$\begin{figure} \par\includegraphics[width=8.3cm,clip]{6467f7.ps}\end{figure}$	Figure 6: $F_{\rm CO}~ c / \mbox{$L_{\rm bol}$ }$ (dimensionless) vs. $\mbox{$M_{\rm env}$ }/\mbox{$L_{\rm bol}$ }^{0.5}$ (in $\mbox{$M_{\odot}$ }$ nd $\mbox{$L_{\odot}$ }$ respectively). See also Bontemps et al. (1996, Fig. 7#. Sources marked by open stars (blue) and asterisks (red) are Class I and Class 0 respectively based on the SED (Paper II).
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$\begin{figure} \par\includegraphics[angle=-90,width=12cm,clip,origin=rb]{6467f8.ps}\end{figure}$	Figure 7: Core destruction timescales at current outflow mass loss rate, vs. left bolometric temperature; right current core mass. Class I sources (Hatchell et al. 2007, based on the SED), are marked by (blue) open stars and Class 0 sources by (red) asterisks.
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$\begin{figure} \par\includegraphics[width=6.8cm,clip]{6467f9.ps}\end{figure}$	Figure 8: Histograms of core destruction timescales for Class 0 (solid) and Class I (dotted) protostars. Sources with upper limits on the lifetime are excluded.
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$\begin{figure} \par\includegraphics[width=17cm,clip]{6467f10.ps}\end{figure}$	Figure 9: ¹²CO 3-2 spectra for outflow sources showing linewings at the 1.5 K ( $3\sigma$ ) level at least 3 km s^-1 from the ambient velocity (marked by inner solid and vertical lines). The outer vertical lines mark the range of velocities included in the momentum flux calculation.
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$\begin{figure} \par\includegraphics[width=17cm,clip]{6467f11.ps} \end{figure}$	Figure 9: continued.
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$\begin{figure} \par\includegraphics[width=17cm,clip]{6467f18.ps}\end{figure}$	Figure 10: ¹²CO 3-2 spectra for sources with no outflow, showing no linewings above the 1.5 K ( $3\sigma$ ) level (upper horizontal solid line) at 3 km s^-1 from the ambient velocity (inner solid and vertical lines).
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