All Figures

$\begin{figure} \par\includegraphics[width=7.25cm,clip]{8699f1a.eps}\par\includegraphics[width=7.25cm,clip]{8699f1b.eps}\end{figure}$ Figure 1: Continuum visibilities (crosses) and uniform brightness temperature models (line). Top: leading side. Bottom: trailing side.
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In the text

$\begin{figure} \par\includegraphics[width=8.35cm,clip]{8699f2.eps}\end{figure}$ Figure 2: Real part of trailing side continuum visibilities near zero-crossing, compared to various models. See text for details.
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In the text

$\begin{figure} \par\includegraphics[angle=-90,width=7.4cm,clip]{8699f3a.eps}\par... ...3b.eps}\par\includegraphics[angle=-90,width=7.4cm,clip]{8699f3c.eps}\end{figure}$ Figure 3: Maps of SO₂ 216.643 GHz line emission and continuum after phase self-calibration. Top: leading side line emission. Center: trailing side line emission. Bottom: continuum map. Contour step is 50 mJy/beam for the line data, 100 mJy/beam for the continuum data. The circle indicates the size of Io. The synthesized beam is shown in the inset.
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In the text

$\begin{figure} \par\includegraphics[angle=-90,width=8.4cm,clip]{8699f4a.eps}\par\includegraphics[angle=-90,width=8.4cm,clip]{8699f4b.eps}\end{figure}$ Figure 4: Spectral maps in the SO₂ line at 216.643 GHz. Top: leading size. Bottom: trailing side. RA, Dec offsets (in '') are indicated for each beam position. The spectral resolution is 120 kHz. The surface of Io and the synthesized beam are indicated.
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In the text

$\begin{figure} \par\includegraphics[width=5.1cm,clip]{8699f5.eps}\end{figure}$ Figure 5: SO₂ line spectra observed at five beam positions along Io's Equator on Io leading side. Gaussian fits are superimposed and Doppler shifts from rest frequency (km s^-1) are indicated, with their 1 $\sigma$ error bar.
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In the text

$\begin{figure} \par\includegraphics[width=8.2cm,clip]{8699f6.eps}\end{figure}$ Figure 6: Map of the Doppler shifts (m/s) on the SO₂ 216.643 GHz line on the leading side, from PdBI data. Positive velocities are indicated by solid black lines and negative velocities by dashed black lines. Contour level is 50 m/s.
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In the text

$\begin{figure} \par\includegraphics[width=8.2cm,clip]{8699f7.eps}\end{figure}$ Figure 7: Map of the 216.643 GHz line width ( FWHM, in m/s) on the leading side, from PdBI data. Contour level is 100 m/s.
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In the text

$\begin{figure} \par\includegraphics[width=8.2cm,clip]{aa8699f8.eps}\end{figure}$ Figure 8: Fit of IRAM-30 m October 9 (lead, bottom) and 10 (trail, top), 1999 observations, with models derived from the Spencer et al. (2005) SO₂ distribution. Data are shown as black histograms. Green lines: original Spencer distribution. Pink lines: rescaled Spencer distribution (identical to original on leading side). Blue lines: rescaled distribution, with horizontal winds. See text and Table 4 for details and parameters.
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In the text

$\begin{figure} \par\includegraphics[width=8.2cm,clip]{aa8699f9.eps}\end{figure}$ Figure 9: Fit of IRAM-30 m October 9 (lead, bottom) and 10 (trail, top), 1999 observations, with models derived from the Feaga et al. (2008) SO₂ distribution. Data are shown as black histograms. Green lines: original Feaga distribution. Pink lines: rescaled Feaga distribution. Blue lines: rescaled distribution, with horizontal winds. See text and Table 4 for details and parameters.
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In the text

$\begin{figure} \par\includegraphics[width=8.2cm,clip]{8699f10.eps}\end{figure}$ Figure 10: Fit of IRAM-30 m November 26, 1999 (trail) observations. Data are shown as black histograms. Green: rescaled Spencer distribution. Blue: rescaled Feaga distribution. Red: rescaled Spencer distribution with winds. Black line: rescaled Feaga distribution with winds. See text and Table 4 for details and parameters.
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In the text

$\begin{figure} \par\includegraphics[width=8.2cm,clip]{8699f11.eps}\end{figure}$ Figure 11: Fit of 216.643 GHz leading side disk-average spectrum. Left: IRAM-30 m (Nov. 25, 1999). Right: PdBI (Jan. 28, 2005). Data are shown as black histograms. The spectral resolution is 100 kHz for IRAM 30-m and 120 kHz for PdBI. Green: rescaled Spencer distribution. Blue: rescaled Feaga distribution. Red: rescaled Spencer distribution with winds. Black line: rescaled Feaga distribution with winds. See text and Table 4 for details and parameters.
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In the text

$\begin{figure} \par\includegraphics[width=8.4cm,clip]{8699f12.eps}\end{figure}$ Figure 12: Doppler shifts for a hydrostatic model with a direct wind speed of 200 m/s.
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In the text

$\begin{figure} \par\includegraphics[angle=-90,width=7.4cm,clip]{8699f13a.eps}\pa... ...cs[angle=-90,width=7.4cm,clip]{8699f13c.eps} \end{figure}$ Figure 13: Model emission maps on the leading side. Top: rescaled Spencer distribution, Center: rescaled Feaga distribution, Bottom: rescaled Spencer distribution, restricted to SZA < 70 $^{\circ }$ . Gas temperature is adjusted so as to reproduce the observed total flux (see Table 5). Contour step is 50 mJy/beam.
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In the text

$\begin{figure} \par\includegraphics[width=8.2cm,clip]{8699f14.eps}\end{figure}$ Figure 14: 217 GHz emission line, rescaled to Io radius, produced by 1 nightside Pele or Prometheus plume located 40 $^{\circ }$ away from disk center. Assumed fluxes are 2 $\times$ 10²⁹and 1.1 $\times$ 10²⁹ SO₂ molecules s^-1, respectively. Also shown are synthetic spectra calculated for isothermal plumes.
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In the text

$\begin{figure} \par\includegraphics[width=7.25cm,clip]{8699f1a.eps}\par\includegraphics[width=7.25cm,clip]{8699f1b.eps}\end{figure}$	Figure 1: Continuum visibilities (crosses) and uniform brightness temperature models (line). Top: leading side. Bottom: trailing side.
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$\begin{figure} \par\includegraphics[width=8.35cm,clip]{8699f2.eps}\end{figure}$	Figure 2: Real part of trailing side continuum visibilities near zero-crossing, compared to various models. See text for details.
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$\begin{figure} \par\includegraphics[angle=-90,width=7.4cm,clip]{8699f3a.eps}\par... ...3b.eps}\par\includegraphics[angle=-90,width=7.4cm,clip]{8699f3c.eps}\end{figure}$	Figure 3: Maps of SO₂ 216.643 GHz line emission and continuum after phase self-calibration. Top: leading side line emission. Center: trailing side line emission. Bottom: continuum map. Contour step is 50 mJy/beam for the line data, 100 mJy/beam for the continuum data. The circle indicates the size of Io. The synthesized beam is shown in the inset.
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$\begin{figure} \par\includegraphics[angle=-90,width=8.4cm,clip]{8699f4a.eps}\par\includegraphics[angle=-90,width=8.4cm,clip]{8699f4b.eps}\end{figure}$	Figure 4: Spectral maps in the SO₂ line at 216.643 GHz. Top: leading size. Bottom: trailing side. RA, Dec offsets (in '') are indicated for each beam position. The spectral resolution is 120 kHz. The surface of Io and the synthesized beam are indicated.
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$\begin{figure} \par\includegraphics[width=5.1cm,clip]{8699f5.eps}\end{figure}$	Figure 5: SO₂ line spectra observed at five beam positions along Io's Equator on Io leading side. Gaussian fits are superimposed and Doppler shifts from rest frequency (km s^-1) are indicated, with their 1 $\sigma$ error bar.
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$\begin{figure} \par\includegraphics[width=8.2cm,clip]{8699f6.eps}\end{figure}$	Figure 6: Map of the Doppler shifts (m/s) on the SO₂ 216.643 GHz line on the leading side, from PdBI data. Positive velocities are indicated by solid black lines and negative velocities by dashed black lines. Contour level is 50 m/s.
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$\begin{figure} \par\includegraphics[width=8.2cm,clip]{8699f7.eps}\end{figure}$	Figure 7: Map of the 216.643 GHz line width ( FWHM, in m/s) on the leading side, from PdBI data. Contour level is 100 m/s.
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$\begin{figure} \par\includegraphics[width=8.2cm,clip]{aa8699f9.eps}\end{figure}$	Figure 9: Fit of IRAM-30 m October 9 (lead, bottom) and 10 (trail, top), 1999 observations, with models derived from the Feaga et al. (2008) SO₂ distribution. Data are shown as black histograms. Green lines: original Feaga distribution. Pink lines: rescaled Feaga distribution. Blue lines: rescaled distribution, with horizontal winds. See text and Table 4 for details and parameters.
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$\begin{figure} \par\includegraphics[width=8.2cm,clip]{8699f10.eps}\end{figure}$	Figure 10: Fit of IRAM-30 m November 26, 1999 (trail) observations. Data are shown as black histograms. Green: rescaled Spencer distribution. Blue: rescaled Feaga distribution. Red: rescaled Spencer distribution with winds. Black line: rescaled Feaga distribution with winds. See text and Table 4 for details and parameters.
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$\begin{figure} \par\includegraphics[width=8.4cm,clip]{8699f12.eps}\end{figure}$	Figure 12: Doppler shifts for a hydrostatic model with a direct wind speed of 200 m/s.
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$\begin{figure} \par\includegraphics[angle=-90,width=7.4cm,clip]{8699f13a.eps}\pa... ...cs[angle=-90,width=7.4cm,clip]{8699f13c.eps} \end{figure}$	Figure 13: Model emission maps on the leading side. Top: rescaled Spencer distribution, Center: rescaled Feaga distribution, Bottom: rescaled Spencer distribution, restricted to SZA < 70 $^{\circ }$ . Gas temperature is adjusted so as to reproduce the observed total flux (see Table 5). Contour step is 50 mJy/beam.
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$\begin{figure} \par\includegraphics[width=8.2cm,clip]{8699f14.eps}\end{figure}$	Figure 14: 217 GHz emission line, rescaled to Io radius, produced by 1 nightside Pele or Prometheus plume located 40 $^{\circ }$ away from disk center. Assumed fluxes are 2 $\times$ 10²⁹and 1.1 $\times$ 10²⁹ SO₂ molecules s^-1, respectively. Also shown are synthetic spectra calculated for isothermal plumes.
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