All Figures

$\begin{figure} \par\includegraphics[angle=90,width=18cm,clip]{MS2937f1.eps} \end{figure}$ Figure 1: Successive observations by the Nobeyama Radioheliograph of an eruptive prominence that occurred on 31 July 1992 above the east solar limb. a) is a partial image of the whole Sun at 01:15:41 (UT) processed by the Steer algorithm. The FOV is $16\times 21$ arcmin. b) is an image obtained from the same data as a), however is processed by the classical Högbom algorithm. c) is the same prominence as a) in H $\alpha$ at the same time with almost the same FOV observed by the Norikura 10 cm-diameter Coronagraph. d-1)- d-9) are successive images processed by the Steer algorithm. The FOV is the same as a). d-1) is 00:15 (UT). d-2) is 00:45 (UT). d-3) is 00:50 (UT). d-4) is 00:55 (UT). d-5) is 01:00 (UT). d-6) is 01:05 (UT). d-7) is 01:10 (UT). d-8) is 01:15 (UT). d-9) is 01:20 (UT).
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In the text

$\begin{figure} \par\includegraphics[angle=90,width=8.8cm,clip]{MS2937f2.eps} \end{figure}$ Figure 2: The rms noise level, and the rms level in the sky region excluding CLEAN points in the simulated image and in the observed image of the Nobeyama Radioheliograph at each CLEAN criterion.
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In the text

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{MS2937f3.eps} \end{figure}$ Figure 3: Noise concentration and image smoothing in the observed image of the Nobeyama Radioheliograph with two CLEAN criteria. CLEAN criterion of a) is 3 $\times$ rms noise level. CLEAN criterion of b) is 0.5 $\times$ rms noise level.
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In the text

$\begin{figure} \par\includegraphics[angle=90,width=18cm,clip]{MS2937f4.eps}\par \end{figure}$ Figure 4: Consecutive observations of 17-GHz enhanced emissions associated with soft X-ray coronal holes, which are indicated by blue arrows. Color-scaled images are the soft X-ray emission observed by the Soft X-ray Telescope. Blue contours with stripes are the 17-GHz enhanced emissions of 500 K or more from the quiet disk brightness of 10 000 K observed by the Nobeyama Radioheliograph. a)- d) are 4-day consecutive images around noon from 4 March 1993 through 7 March 1993, and are processed by the Steer algorithm. e) is obtained from the same data as c), however is processed by the classical Högbom algorithm.
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In the text

$\begin{figure} \par\includegraphics[angle=90,width=8.8cm,clip]{MS2937fa1.eps} \end{figure}$ Figure A.1: The array configuration of the Nobeyama Radioheliograph.

In the text

$\begin{figure} \par\includegraphics[angle=90,width=8.8cm,clip]{MS2937fa2.eps} \end{figure}$ Figure A.2: The observing points (UV pattern) in the Fourier domain (UV plane) of the Nobeyama Radioheliograph.

In the text

$\begin{figure} \par\includegraphics[angle=90,width=8.8cm,clip]{MS2937fa3.eps} \end{figure}$ Figure A.3: The rms noise level in images due to major hardware error sources, and the rms differential level between the model image and the restored image at each CLEAN criterion in the simulation. The error sources are unequal bandpass characteristics, antenna-pointing errors, delay errors, and noise at correlator outputs.

In the text

$\begin{figure} \par\includegraphics[angle=90,width=8.8cm,height=7.2cm,clip]{MS2937fa4.eps} \end{figure}$ Figure A.4: Increase of the rms noise (error) level assuming the disk component and a single Gaussian source with various sizes in the simulation. One pixel corresponds to 4.91 arcsec in images.

In the text

$\begin{figure} \par\includegraphics[angle=90,width=18cm,clip]{MS2937fa5.eps} \end{figure}$ Figure A.5: a-1)-a-4) are successive images of the Nobeyama Radioheliograph at 90-min intervals without the disk component, i.e. 17-GHz enhanced emissions in the south polar region. The FOV is $10\times 20$ arcmin. Stripes flow from left to right through the FOV with time. b-1)-b-4) are successive images obtained from the same data as a-1)-a-4). Components outside the FOV are, however, restored beforehand using the NON-CLEAN BOX.

In the text

$\begin{figure} \par\includegraphics[angle=90,width=8.8cm,clip]{MS2937f2.eps} \end{figure}$	Figure 2: The rms noise level, and the rms level in the sky region excluding CLEAN points in the simulated image and in the observed image of the Nobeyama Radioheliograph at each CLEAN criterion.
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$\begin{figure} \par\includegraphics[width=8.8cm,clip]{MS2937f3.eps} \end{figure}$	Figure 3: Noise concentration and image smoothing in the observed image of the Nobeyama Radioheliograph with two CLEAN criteria. CLEAN criterion of a) is 3 $\times$ rms noise level. CLEAN criterion of b) is 0.5 $\times$ rms noise level.
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