All Figures

$\begin{figure} \par\includegraphics[width=12.35cm,clip]{0611fig1.eps} \end{figure}$ Figure 1: $A_{\rm V}$ grayscale map of HCL2 with black contours from 2 mag by 2 mag based on the data of Padoan et al. (2002). Four objects with high peak extinction ( $A_{\rm V}({\rm peak})\ge 8$ mag) surround a low extinction region in the centre. These are in clockwise: (1) TMC-1, (2) HCL2-A, (3) HCL2-B and (4) HCL2-E and HCL2-ES, the main clouds of the Taurus Molecular Ring (TMR). The IRAS point sources (see Table 3) are marked with white symbols. The white frame borders the region of our ISOPHOT 200 $\mu$ m map.
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In the text

$\begin{figure} \par\includegraphics[width=7.35cm,clip]{0611fig2.eps} \end{figure}$ Figure 2: Roadmap of the TMR clouds. The outer frame corresponds roughly to the extent of HCL2. The shaded elliptical ring follows the $A_{\rm V}=4$ mag extinction contours. The subclouds inside TMR are marked with ellipses. The 3 clouds inside the ISO 200 $\mu$ m image frame (box) are drawn with solid, the clouds outside with dashed lines. The TMC-1NH₃ peak HCL2 and TMR are elongated parallel to the galactic plane, but not all the dense subclouds follow that orientation.
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In the text

$\begin{figure} \par\includegraphics[width=15cm,clip]{0611fig3.eps} \end{figure}$ Figure 3: The southern part of the Taurus Molecular Ring (TMR) with the 3 main clouds (black ellipses) and the TMR hole in the multiwavelengh data. a) ISOPHOT 200 $\mu$ m surface brightness I₂₀₀ ( HPBW = 2 $^\prime$ ), greyscale levels: from 100 MJy sr^-1 to 190 MJy sr^-1the NH₃(1, 1) maximum at HCL2E is marked with a red contour at HCL2-E ( HPBW = 2 $^\prime$ ); b) IRAS 100 $\mu$ m intensity I₁₀₀ ( HPBW = 4 $^\prime$ ) contours: from 25 MJy sr^-1 by 1.5 MJy sr^-1; c) IRAS 60 $\mu$ m intensity I₆₀ ( HPBW = 4 $^\prime$ ) contours: from 2.5 MJy sr^-1 by 0.3 MJy sr^-1; d) C¹⁸O line intensity W(C¹⁸O) ( HPBW = 2 $.\mkern -4mu^\prime$ 7), greyscale levels: from 1 K km s^-1 to 2 K km s^-1. The parameters of the marked regions are listed in Table 1.
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In the text

$\begin{figure} \par\includegraphics[width=8cm,clip]{0611fig4.eps} \end{figure}$ Figure 4: C¹⁸O(1-0) spectra at the 4 regions marked in Fig. 3. a) TMC-1 CP at $l=174.40\hbox{$^\circ$ }, ~ b=-13.49\hbox{$^\circ$ }$ . b) HCL2-E at $l=174.35\hbox{$^\circ$ }, ~ b=-13.77\hbox{$^\circ$ }$ . c) HCL2-ES at $l=174.60\hbox{$^\circ$ }, ~ b=-13.67\hbox{$^\circ$ }$ . d) TMR hole at $l=174.20\hbox{$^\circ$ }, ~ b=-13.60\hbox{$^\circ$ }$ .
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In the text

$\begin{figure} \par\includegraphics[width=7.5cm,clip]{0611fig5.eps} \end{figure}$ Figure 5: a) Effelsberg-100 m NH₃ (1, 1) and (2, 2) spectra at HCL2-Ea the (1, 1) main group line area peak of HCL2-E (see Fig. 3). b) Effelsberg-100 m NH₃ (1, 1) and (2, 2) spectra at the HCL2-Eb; the (2, 2) peak position of HCL2-E. (The middle part of the spectra is presented.)
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In the text

$\begin{figure} \par\includegraphics[width=17.6cm,clip]{0611fig6.eps}\par \end{figure}$ Figure 6: a) $H-K_{\rm S}$ vs. J-H colours of 2MASS sources of the region. Point sources falling inside the the locus of classical T Tauri stars (CTT, Meyer et al. 1997) and having a good photometry are marked with red $\times$ -es. The reddened MS and evolved stars (with good photometry) are marked with small blue pluses. Four extended 2MASS objects are marked with red triangles. b) Grayscale map of the ISOPHOT 200 $\mu$ m surface brightness with 2MASS sources overlaid. The 25 candidate classical T Tauris (CTTs) (marked with black $\times$ -es) are located around the density peaks of the cores. The reddened MS and evolved stars (with good photometry) are marked with small blue pluses. (This figure in available in colour in the electronic version.)
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In the text

$\begin{figure} \par\includegraphics[width=14cm,clip]{0611fig7.eps} \end{figure}$ Figure 7: a) I₆₀ vs. I₁₀₀ for all pixels of TMR (small dots). Different symbols were overlaid for the different parts of TMR and the hole, as indicated in the upper left corner. b) I₂₀₀ vs. I₁₀₀ with representative slopes fitted to the data points of TMC-1 and HCL2-E. c) I₂₀₀ vs. $A_{\rm V}$ with line fitted to all points. TMC-1 shows I₂₀₀ excess d) W(C¹⁸O) vs. $\Delta I_{200}/\Delta I_{100}$ , the high ratios occur only inside the molecular cloud. e) W(C¹⁸O) vs. I₂₀₀ correlation in TMR. The correlation coefficient is 73%.
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In the text

$\begin{figure} \par\includegraphics[width=8cm,clip]{0611fig8.eps} \end{figure}$ Figure 8: Grayscale map of NH₃ (1, 1) line area distribution at the I₂₀₀ peak in the HCL2-E cloud. The origin is at: RA(1950) = 4 $^{\rm h}$ 37 $^{\rm m}$ 42 $^{\rm s}$ , Dec(1950) = 25$^$25 $^\prime$ . The continuous contours are drawn from 0.4 K km s^-1 (3 $\sigma$ NH₃(1, 1) line area) by 0.2 K km s^-1. The beam-width ( HPBW = 40 $^{\prime \prime }$ ) of the Effelsberg-100 m telescope is shown in the upper right corner. The ISOPHOT 200 $\mu$ m surface brightness contours of 165 and 175 MJy sr^-1 are drawn with dashed lines indicating the location of the FIR peak in HCL2-E. The HPBW of ISOPHOT C200 is shown in the lower left corner. The central positions of the H¹³CO⁺ cores of 42a,b,c of Onishi (2002) are marked with black squares. The HCL2 SE-2 X-ray/IRAS pointsource and two more YSO candidates are marked with star and annotation.
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In the text

$\begin{figure} \par\includegraphics[width=8cm,clip]{0611fig9.eps} \end{figure}$ Figure 9: HCL2 with TMR and its main clouds. C¹⁸O line intensity W(C¹⁸O) distribution as observed by the Nagoya-4 m telescope ( HPBW = 2 $.\mkern -4mu^\prime$ 7 shown in the upper left corner) in a 2 $^\prime$ grid. The W(C¹⁸O) contours (thin continuous lines) are drawn from 0.33 K km^-1 by 0.1 K km s^-1. The apparent W(C¹⁸O) maxima are at TMC-1 ( top left), HCL2-E ( left), HCL2-B ( center down), HCL2-A ( center). The area of the ISOPHOT image is marked with a black frame. We represent the associated HI cloud with HI 21 cm line area contours of 341 K km s^-1 and 352 K km s^-1(red dashed line).
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In the text

$\begin{figure} \par\includegraphics[width=8cm,clip]{0611fig4.eps} \end{figure}$	Figure 4: C¹⁸O(1-0) spectra at the 4 regions marked in Fig. 3. a) TMC-1 CP at $l=174.40\hbox{$^\circ$ }, ~ b=-13.49\hbox{$^\circ$ }$ . b) HCL2-E at $l=174.35\hbox{$^\circ$ }, ~ b=-13.77\hbox{$^\circ$ }$ . c) HCL2-ES at $l=174.60\hbox{$^\circ$ }, ~ b=-13.67\hbox{$^\circ$ }$ . d) TMR hole at $l=174.20\hbox{$^\circ$ }, ~ b=-13.60\hbox{$^\circ$ }$ .
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$\begin{figure} \par\includegraphics[width=7.5cm,clip]{0611fig5.eps} \end{figure}$	Figure 5: a) Effelsberg-100 m NH₃ (1, 1) and (2, 2) spectra at HCL2-Ea the (1, 1) main group line area peak of HCL2-E (see Fig. 3). b) Effelsberg-100 m NH₃ (1, 1) and (2, 2) spectra at the HCL2-Eb; the (2, 2) peak position of HCL2-E. (The middle part of the spectra is presented.)
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