Astronomy & Astrophysics

All Figures

$\begin{figure} \par\includegraphics[width=16cm,clip]{0179-fig1.eps} \end{figure}$ Figure 1: HERA optical scheme. The mechanical drive of the K-mirror has been omitted for clarity.
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In the text

$\begin{figure} \par\includegraphics[angle=-90,width=8cm,clip]{0179-fig2.ps} \end{figure}$ Figure 2: Single sideband receiver noise temperatures of the 9 receiver elements, measured at the telescope reference plane (Nasmyth Focus).
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In the text

$\begin{figure} \par {\includegraphics[width=8cm,clip]{0179fi3a.ps}\hspace*{9mm}} \par\vspace*{3mm} \includegraphics[width=8.8cm,clip]{0179fi3b.eps} \end{figure}$ Figure 3: Upper panel: continuum beam map of Mars with active derotation and observing in the beam-chopped, on-the-fly mode. Contours are 15% to 90% of the peak power in 25% steps. Lower panel: beam profiles derived from scans across the limb of the moon.
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In the text

$\begin{figure} \par\includegraphics[angle=-90,width=8cm,clip]{0179fig4.eps} \end{figure}$ Figure 4: Pointing toward Uranus with the central pixel; K-mirror in its vertical position (filled points) and from $-80^{\circ }$ to $+80^{\circ }$ in $20^{\circ }$ steps ( $320^{\circ }$ on sky, empty squares), relative to the 230 GHz beam size.
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In the text

$\begin{figure} \par\includegraphics[width=8.5cm,clip]{0179fig5.ps} \end{figure}$ Figure 5: Example of inclined scanning (Azimuth) with equidistant sampling. The telescope and derotator control allow any other scanning direction. The scanned band has a total width of 68''.
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In the text

$\begin{figure} \par\includegraphics[angle=0,width=8cm,clip]{0179fig6.ps} \end{figure}$ Figure 6: Spectroscopic baseline ripple. Upper panel: Fourier transform of a position-switched observation (the reference position was offset by $-1^\circ$ in elevation), with the central pixel connected to a 1 GHz-wide filter bank. The three ripple components (arrows) have inverse frequencies $\tilde\nu$ corresponding to separations d between the reflecting surfaces. Lower panel: frequency-switched observations of the dark cloud B133 in the ¹²CO line at 230.5 GHz, a 5 min integration. The frequency throw was set equal to the dominant ripple frequency (6.9 MHz). The narrow features at 2 and 11 km s^-1 are mesospheric, the broader features show the opacity and velocity structure of the source. As expected, the baselines are flattest for off-axis pixels.
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In the text

$\begin{figure} \par\includegraphics[angle=-90,width=8cm,clip]{0179fig7.eps} \end{figure}$ Figure 7: a) ¹²CO(2-1) spectra of Orion A, obtained with the nine pixels as a relative calibration check. The array was shifted on a rectangular 24'' grid aligned with the sky coordinates with active field derotation. b) Spectra after calibration correction with individual factors obtained from the integrated line fluxes. The identical line shapes mean that pointing errors are negligible. c) rms deviation of the temperatures as measured by the different pixels after gain correction.
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In the text

$\begin{figure} \par\includegraphics[angle=-90,width=8.8cm,clip]{0179fig8.eps} \end{figure}$ Figure 8: Velocity integrated CO(2-1) emission in M 51, from on-the-fly mapping with an inclined array, scanning in the RA (horizontal) direction. In the vertical direction, the area with Dec offsets -370'' to 0'' was scanned twice (rms 1.4 ${\rm K}~ {\rm km~s^{-1}}$ ), while the area above Dec offset 0'' was scanned only once (rms 1.8 ${\rm K}~ {\rm km~s^{-1}}$ ). The total integration time (on and off source) is $\sim$ 4 h. The data were corrected for gain drifts with a correlation algorithm. The grey scale shows $\int {T}_a^* \ {\rm d}v$ .
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In the text

$\begin{figure} \par\includegraphics[width=16cm,clip]{0179-fig1.eps} \end{figure}$	Figure 1: HERA optical scheme. The mechanical drive of the K-mirror has been omitted for clarity.
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$\begin{figure} \par\includegraphics[angle=-90,width=8cm,clip]{0179-fig2.ps} \end{figure}$	Figure 2: Single sideband receiver noise temperatures of the 9 receiver elements, measured at the telescope reference plane (Nasmyth Focus).
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$\begin{figure} \par {\includegraphics[width=8cm,clip]{0179fi3a.ps}\hspace{9mm}} \par\vspace{3mm} \includegraphics[width=8.8cm,clip]{0179fi3b.eps} \end{figure}$	Figure 3: Upper panel: continuum beam map of Mars with active derotation and observing in the beam-chopped, on-the-fly mode. Contours are 15% to 90% of the peak power in 25% steps. Lower panel: beam profiles derived from scans across the limb of the moon.
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$\begin{figure} \par\includegraphics[angle=-90,width=8cm,clip]{0179fig4.eps} \end{figure}$	Figure 4: Pointing toward Uranus with the central pixel; K-mirror in its vertical position (filled points) and from $-80^{\circ }$ to $+80^{\circ }$ in $20^{\circ }$ steps ( $320^{\circ }$ on sky, empty squares), relative to the 230 GHz beam size.
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$\begin{figure} \par\includegraphics[width=8.5cm,clip]{0179fig5.ps} \end{figure}$	Figure 5: Example of inclined scanning (Azimuth) with equidistant sampling. The telescope and derotator control allow any other scanning direction. The scanned band has a total width of 68''.
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