All Figures

$\begin{figure} \par\includegraphics[width=12cm,height=7cm,clip]{5373fig1.eps} \end{figure}$ Figure 1: General layout. The signal passes 11 mirrors before reaching the detector. The receiver IF ouput then goes to a common IF module where part of it is detected by a total power detector used for the continuum observations, and the rest is down-converted to the 0-1 GHz band before going to the backends.
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In the text

$\begin{figure} \par\includegraphics[width=7cm,clip]{5373fig2.eps} \end{figure}$ Figure 2: View of the inner part of the cryostat. The input beam is shown. The mixer, IF isolator, and IF amplifier are on the 4 K cold plate.
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In the text

$\begin{figure} \par\includegraphics[width=8cm,clip]{5373fig3.eps} \end{figure}$ Figure 3: Typical receiver and system temperatures measured throughout the observing season in May-December 2005.
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In the text

$\begin{figure} \par\includegraphics[angle=-90,width=7.5cm,clip]{5373fig4.ps} \end{figure}$ Figure 4: Cross-scan pointing on Uranus.
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In the text

$\begin{figure} \par\includegraphics[width=7.5cm,clip]{5373fig5.eps} \end{figure}$ Figure 5: Example of OCS measurement in Orion-KL. The rotational transitions $J = 25 \to 24$ and $J = 26 \to 25$ from different sidebands appear quite close in the final IF spectrum with similar line intensities. Note that the asymmetry of the $J = 26 \to 25$ line (coming from the USB around 316 GHz) is opposite that of the $J = 25 \to 24$ line.
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In the text

$\begin{figure} \par\includegraphics[angle=-90,width=7.5cm,clip]{5373fig6.ps} \end{figure}$ Figure 6: C¹⁸O( $J = 3 \to 2$ ) spectrum of the cold dark cloud L183.
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In the text

$\begin{figure} \par\includegraphics[width=8cm,clip]{5373fig7.eps} \end{figure}$ Figure 7: CO( $J = 3 \to 2$ ) and ¹³CO( $J = 3 \to 2$ ) in NGC 4945 at the velocity resolution of 10 km s^-1. Note that these data were taken in March 2006 with the new mixer using the optimized-tuning procedure.
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In the text

$\begin{figure} \par\includegraphics[width=12cm,height=7cm,clip]{5373fig1.eps} \end{figure}$	Figure 1: General layout. The signal passes 11 mirrors before reaching the detector. The receiver IF ouput then goes to a common IF module where part of it is detected by a total power detector used for the continuum observations, and the rest is down-converted to the 0-1 GHz band before going to the backends.
Open with DEXTER

$\begin{figure} \par\includegraphics[width=7cm,clip]{5373fig2.eps} \end{figure}$	Figure 2: View of the inner part of the cryostat. The input beam is shown. The mixer, IF isolator, and IF amplifier are on the 4 K cold plate.
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$\begin{figure} \par\includegraphics[width=8cm,clip]{5373fig3.eps} \end{figure}$	Figure 3: Typical receiver and system temperatures measured throughout the observing season in May-December 2005.
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$\begin{figure} \par\includegraphics[angle=-90,width=7.5cm,clip]{5373fig4.ps} \end{figure}$	Figure 4: Cross-scan pointing on Uranus.
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$\begin{figure} \par\includegraphics[width=7.5cm,clip]{5373fig5.eps} \end{figure}$	Figure 5: Example of OCS measurement in Orion-KL. The rotational transitions $J = 25 \to 24$ and $J = 26 \to 25$ from different sidebands appear quite close in the final IF spectrum with similar line intensities. Note that the asymmetry of the $J = 26 \to 25$ line (coming from the USB around 316 GHz) is opposite that of the $J = 25 \to 24$ line.
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$\begin{figure} \par\includegraphics[angle=-90,width=7.5cm,clip]{5373fig6.ps} \end{figure}$	Figure 6: C¹⁸O( $J = 3 \to 2$ ) spectrum of the cold dark cloud L183.
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$\begin{figure} \par\includegraphics[width=8cm,clip]{5373fig7.eps} \end{figure}$	Figure 7: CO( $J = 3 \to 2$ ) and ¹³CO( $J = 3 \to 2$ ) in NGC 4945 at the velocity resolution of 10 km s^-1. Note that these data were taken in March 2006 with the new mixer using the optimized-tuning procedure.
Open with DEXTER