Astronomy & Astrophysics

All Figures

$\begin{figure} \par\includegraphics[angle=-90,width=7.8cm,clip]{2393fig1a.eps}\vspace*{3mm} \includegraphics[angle=-90,width=7.8cm,clip]{2393fig1b.eps}\end{figure}$ Figure 1: Top: coupling optics for telescope use. A mirror mounted to a scanner motor selects either one of the calibration sources (black body at 400 $^{\circ }$ C, ambient absorber) or one of two positions on the sky. Bottom: to scale model of the receiver. The size of the aluminum cube is roughly $80\times 60\times 42$ cm³ weighing about 80 kg. The different parts of the optical path are marked in colours and described in the text.
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In the text

$\begin{figure} \par\includegraphics[angle=-90,width=8cm,clip]{2393fig2a.eps}\vsp... ...ce*{3mm} \includegraphics[angle=-90,width=7.3cm,clip]{2393fig2c.eps}\end{figure}$ Figure 2: Top: CO₂ P(30) absorption and emission line at 1037.4 cm^-1. The spectra are double sideband, binned to a 4 MHz resolution and highly contaminated by telluric ozone absorption. The combined fit (black line) yields the telluric and Mars spectra shown seperated in the center and bottom respectively. The width of the emission peak was determined to be $42~{\rm MHz}\pm4.0$ MHz ( FWHM) suggesting an altitude of 60-80 km as the origin of the line. The offset of the emission peak from the center of the absorption line of 7.5 MHz is most likely caused by zonal wind in the higher atmosphere.
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In the text