Astronomy & Astrophysics

All Figures

$\begin{figure} \par\resizebox{8.8cm}{!}{\rotatebox{270}{\includegraphics*{SMCN12... ...zebox{8.8cm}{!}{\rotatebox{270}{\includegraphics*{LMCN83B_iso2.ps}}}\end{figure}$ Figure 1: Comparison of $~{\rm ^{12}CO}$ and $~{\rm ^{13}CO}$ profiles in the clouds associated with various HII regions. Temperature scales are in $T_{\rm A}^{*} = 0.72 T_{\rm mb}$ . The offset positions refer to the integrated emission maps as in Figs. 2, 3 and 5.
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In the text

$\begin{figure} \par\includegraphics[width=12cm,clip]{3791f2.eps}\par \end{figure}$ Figure 2: Maps of CO clouds associated with SMC HII regions N 12, N 27, N 83 and N 84. Linear contours are at multiples of $\int$ $T_{\rm mb}{\rm d}V = 1~~{\rm {K~km~s^{-1}}}$ for N 12 (both transitions), 1.25 $~{\rm {K~km~s^{-1}}}$ (J=1-0) and 1 $~{\rm {K~km~s^{-1}}}$ (J=2-1) for N 27 and 0.75 $~{\rm {K~km~s^{-1}}}$ for N 83 and N 84. For all four objects, position-velocity cuts are in declination. Linear contours are at multiples of $T_{\rm mb} = 0.3$ K for N 12, at 0.40 K and 0.75 K respectively for N 27 and at 0.20 K for N 83 and N 84. Gray scales are labelled in $T_{\rm A}^{*}$ rather than $T_{\rm mb}$ .
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In the text

$\begin{figure} \par\includegraphics[width=12cm,clip]{3791f3.eps} \end{figure}$ Figure 3: Maps of CO cloud associated with SMC HII region N 88. Linear contours are at multiples of $\int$ $T_{\rm mb}{\rm d} V = 0.40~~{\rm {K~km~s^{-1}}}$ (J=1-0) and 0.75 $~{\rm {K~km~s^{-1}}}$ (J=2-1). Position velocity cuts are in right ascension. Linear contours are at multiples of $T_{\rm mb} = 0.10$ K and 0.25 K respectively. Gray scales are labelled in $T_{\rm A}^{*}$ rather than $T_{\rm mb}$ .
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In the text

$\begin{figure} \par\includegraphics[width=12cm,clip]{3791f4.eps}\par \end{figure}$ Figure 4: Maps of CO clouds associated with LMC HII regions N 57 and N 59. Linear contours are at multiples of $\int$ $T_{\rm mb}$ dV = 1.4 (J=1-0) and 2.0 ( $J=2{-}1)~~{\rm {K~km~s^{-1}}}$ for N 57 and 1.00 $~{\rm {K~km~s^{-1}}}$ for N 59. Position-velocity cut for LMC-N 59 is in declination, whereas the cuts for N 57 are diagonal from southwest to northeast. Linear contours are at multiples of $T_{\rm mb} = 0.70$ K (J=1-0) and 1.0 K (J=2-1) for N 57 and at 0.30 K for N 59. Gray scales are labelled in $T_{\rm A}^{*}$ rather than $T_{\rm mb}$ .
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In the text

$\begin{figure} \par\includegraphics[width=12cm,clip]{3791f5.eps}\par \end{figure}$ Figure 5: Maps of CO clouds associated with LMC HII regions N 55 and N 83. Linear contours are at multiples of $\int$ $T_{\rm mb}$ d $V = 2.0~~{\rm {K~km~s^{-1}}}$ for both N 55 and N 83. For both objects position-velocity cuts in right ascension are shown and for N 83 also a cut in declination. The right-ascension cut through N 83 is at a declination offset +1.3 for right-ascension offsets below +0.5 and jumps to a declination offset +0.3 for RA offsets above +0.5. Linear contours are at multiples of $T_{\rm mb} = 0.5$ K for N 55 and at 0.4 and 0.30 K respectively for N 83. Gray scales are labelled in $T_{\rm A}^{*}$ rather than $T_{\rm mb}$ .
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In the text

$\begin{figure} \par\resizebox{18cm}{!}{\rotatebox{270}{\includegraphics*{isotop.... ...r\resizebox{18cm}{!}{\rotatebox{270}{\includegraphics*{isobot.ps}}} \end{figure}$ Figure 6: The isotopic ratio $I(~{\rm ^{12}CO})/I(~{\rm ^{13}CO})$ as a function of velocity integrated intensity $I(~{\rm ^{12}CO}) = \int$ $T_{\rm mb}({\rm CO}){\rm d}V$ for $~{\rm ^{13}CO}$ pointings in various LMC fields. The observed source is identified in each panel, together with a Roman numeral referring to Key programme paper in which source maps are presented.
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In the text

$\begin{figure} \par\resizebox{14cm}{!}{\rotatebox{270}{\includegraphics*{isoall.ps}}} \end{figure}$ Figure 7: The isotopic ratio $I(~{\rm ^{12}CO})/I(~{\rm ^{13}CO})$ as a function of velocity integrated intensity $I(~{\rm ^{12}CO}) = \int$ $T_{\rm mb}({\rm CO}){\rm d}V$ for all $~{\rm ^{13}CO}$ pointings in the SMC and the LMC.
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In the text

$\begin{figure} \par\resizebox{8cm}{!}{\rotatebox{270}{\includegraphics*{isomap.ps}}} \end{figure}$ Figure 8: The distribution of points in the densely populated lower left part of Fig. 7 is shown here as an iso-density contour map.
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In the text

$\begin{figure} \par\resizebox{8.cm}{!}{\rotatebox{270}{\includegraphics*{highrat.ps}}} \end{figure}$ Figure 9: Plot of $J=1{-}0/J=2{-}1~~{\rm ^{12}CO}$ transition ratios as a function of (the higher) $J=1{-}0~~{\rm ^{12}CO}/~{\rm ^{13}CO}$ isotopic ratios. The transition ratios on average slightly exceed unity.
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In the text

$\begin{figure} \par\resizebox{7.5cm}{!}{\rotatebox{0}{\includegraphics*{lebfig.eps}}} \end{figure}$ Figure 10: Plots showing $~{\rm ^{12}CO}$ and $~{\rm ^{13}CO}$ line ratios as a result of LTE modelling of various conditions representing the Magellanic Clouds environment.
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In the text

$\begin{figure} \par\resizebox{8.8cm}{!}{\rotatebox{270}{\includegraphics{SMCN12... ...zebox{8.8cm}{!}{\rotatebox{270}{\includegraphics{LMCN83B_iso2.ps}}}\end{figure}$	Figure 1: Comparison of $~{\rm ^{12}CO}$ and $~{\rm ^{13}CO}$ profiles in the clouds associated with various HII regions. Temperature scales are in $T_{\rm A}^{*} = 0.72 T_{\rm mb}$ . The offset positions refer to the integrated emission maps as in Figs. 2, 3 and 5.
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$\begin{figure} \par\resizebox{18cm}{!}{\rotatebox{270}{\includegraphics{isotop.... ...r\resizebox{18cm}{!}{\rotatebox{270}{\includegraphics{isobot.ps}}} \end{figure}$	Figure 6: The isotopic ratio $I(~{\rm ^{12}CO})/I(~{\rm ^{13}CO})$ as a function of velocity integrated intensity $I(~{\rm ^{12}CO}) = \int$ $T_{\rm mb}({\rm CO}){\rm d}V$ for $~{\rm ^{13}CO}$ pointings in various LMC fields. The observed source is identified in each panel, together with a Roman numeral referring to Key programme paper in which source maps are presented.
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$\begin{figure} \par\resizebox{14cm}{!}{\rotatebox{270}{\includegraphics*{isoall.ps}}} \end{figure}$	Figure 7: The isotopic ratio $I(~{\rm ^{12}CO})/I(~{\rm ^{13}CO})$ as a function of velocity integrated intensity $I(~{\rm ^{12}CO}) = \int$ $T_{\rm mb}({\rm CO}){\rm d}V$ for all $~{\rm ^{13}CO}$ pointings in the SMC and the LMC.
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$\begin{figure} \par\resizebox{8cm}{!}{\rotatebox{270}{\includegraphics*{isomap.ps}}} \end{figure}$	Figure 8: The distribution of points in the densely populated lower left part of Fig. 7 is shown here as an iso-density contour map.
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$\begin{figure} \par\resizebox{8.cm}{!}{\rotatebox{270}{\includegraphics*{highrat.ps}}} \end{figure}$	Figure 9: Plot of $J=1{-}0/J=2{-}1~~{\rm ^{12}CO}$ transition ratios as a function of (the higher) $J=1{-}0~~{\rm ^{12}CO}/~{\rm ^{13}CO}$ isotopic ratios. The transition ratios on average slightly exceed unity.
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$\begin{figure} \par\resizebox{7.5cm}{!}{\rotatebox{0}{\includegraphics*{lebfig.eps}}} \end{figure}$	Figure 10: Plots showing $~{\rm ^{12}CO}$ and $~{\rm ^{13}CO}$ line ratios as a result of LTE modelling of various conditions representing the Magellanic Clouds environment.
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