All Figures

$\begin{figure} \par\resizebox{\hsize}{!}{\rotatebox{90}{\includegraphics{odin9_1... ...esizebox{\hsize}{!}{\rotatebox{90}{\includegraphics{odin9_3.ps}}} \end{figure}$ Figure 1: Correction for frequency drift during the observation. Upper: the plus-signs denote the channel number of the center of the telluric O₃ line during the Orion observations, expressed as Odin revolutions. The upper curve (solid line) depicts the behaviour of the reciprocal LO-temperature. Middle: the plus-signs designate the difference between the values shown above. The full-drawn curve is a polynomial fit to these points. This curve describes the average behaviour of the temperature measured at the main reflector. Lower: the rms-spread of the residuals to the polynomial fit corresponds to 0.7 of the AC-channel width (=0.36 km s^-1).
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In the text

$\begin{figure} \par\resizebox{\hsize}{!}{\rotatebox{90}{\includegraphics{odin9_4... ...resizebox{\hsize}{!}{\rotatebox{0}{\includegraphics{odin9_5.ps}}} \end{figure}$ Figure 2: NH₃ $(J,K) = (1,0) \rightarrow (0,0)$ spectra toward Orion A. Upper: the reduced spectra for the three positions discussed in the text (antenna temperature vs. correlator channel) are shown together with the adopted polynomial fits to their baselines. Lower: same as above, but with the baselines subtracted ( $T_{\rm mb}$ vs. $v_{\rm LSR}$ ). The data are displayed as histograms. Uppermost, the KAO observation (2 $^{\prime }$ FWHM) by Keene et al. (1983) (thin line) is shown together with the Odin spectrum toward (0, 0). The much higher S/N of the Odin data aside, the agreement between these two observations is strikingly good. Following below, the spectra toward the three positions observed with Odin are displayed, together with Gaussian fits to the line profiles as thin lines (cf. Table 1). For reference, a vertical dashed line is drawn at $v_{\rm LSR}$ = 9.1 km s^-1.
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In the text