All Figures

$\begin{figure} \par\includegraphics[width=8cm]{2779f1.ps}\end{figure}$ Figure 1: Diagram of the GOLF nominal working mode. The sunlight traverses a vapour cell containing a Na gas and placed inside a magnetic field that splits the measurements in both wings at $\pm$ 108 Å from the reference wavelength.
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In the text

$\begin{figure} \par\includegraphics[width=8cm,clip]{2779f2.eps}\end{figure}$ Figure 2: Time evolution of the phase difference between low-degree p modes simultaneously measured from GOLF and MDI instruments before correcting for the July 14, 2003 time lag ( right arrow). The re-synchronization made on February 8, 2002 is also visible ( left arrow). The vertical dashed lines correspond to the dates of the changes in the GOLF working cycle.
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In the text

$\begin{figure} \par\includegraphics[width=8cm,clip]{2779f3.ps}\end{figure}$ Figure 3: Counting rate (automatically corrected of SEUs) of both GOLF photomultipliers for the low magnetic modulation starting on July 13, 2000 (plotted only 1 point every 100 s).
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In the text

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{2779f4.eps} \end{figure}$ Figure 4: GOLF PMs electron spectrum of the main channel for October 20, 1997. The optimal counting rate for the PMs is reached when the average impulse amplitude is $\sim$ 250 mV.
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In the text

$\begin{figure} \par\includegraphics[width=7.5cm,clip]{2779f5.eps} \end{figure}$ Figure 5: Effects of the high voltage perturbation over the PM1 counting rate. PM2 has no such perturbations. The time axis origin is August 20, 2000. During this period, a SoHO off-pointing event was visible in both tubes.
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In the text

$\begin{figure} \par {\includegraphics[angle=90,width=8cm,clip]{2779f6.ps} } \end{figure}$ Figure 6: Time evolution of the GOLF resonance cell stem temperature ( top) and the two photocathodes temperatures ( bottom. Black for PM1 and light gray for PM2). The time scale starts on April 11, 1996.
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In the text

$\begin{figure} \par {\includegraphics[angle=90,width=8cm,clip]{2779f7.ps} } \end{figure}$ Figure 7: Resonance cell stem temperature scan of January 17, 1996 for the PM1 in the four points of the sodium profile. The reference temperature is 171 $\hbox {$^\circ $ }$ C.
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In the text

$\begin{figure} \par {\includegraphics[angle=90,width=8.4cm,clip]{2779f8.ps} } \end{figure}$ Figure 8: Corrected photometric rates P⁺ and P^- starting on April 11, 1996 and up to June 2, 2004.
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In the text

$\begin{figure} \par {\includegraphics[angle=90,width=8.5cm]{2779f9.ps} } \end{figure}$ Figure 9: Example of 72 days of GOLF PM1 counting rates against PM2 for I^- in arbitrary units before ( top figure) and after ( bottom figure) applying all the corrections and scaling it into velocity (m/s).
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In the text

$\begin{figure} \par {\includegraphics[angle=90,width=8.2cm,clip]{2779f10.ps} } \end{figure}$ Figure 10: X magnitude (see text) as a function of time (starting April 11, 1996) in the top and as a function of the radial component of the orbital velocity in the bottom. The dashed lines in both panels describe the ideal linear response of the system to this radial orbital velocity.
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In the text

$\begin{figure} \par\includegraphics[angle=90,width=7.8cm]{2779f11.ps}\end{figure}$ Figure 11: Velocity residuals as a function of time for PM2 ( top), and after removing a low-frequency trend ( bottom). The signals have been undersampled to 2 h for display purposes only.
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In the text

$\begin{figure} \par\includegraphics[angle=90,width=8cm]{2779f12.ps}\end{figure}$ Figure 12: Three samples of one hour long time series from the V_X ( top and middle panels) and the V_S ( bottom panel) GOLF signal. The V_S is the calibrated velocity for PM2 following Ulrich et al. (2000).
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In the text

$\begin{figure} \par {\includegraphics[angle=90,width=12cm]{2779f13.ps} } \end{figure}$ Figure 13: From top to bottom: time evolution of the MPSI (Magnetic Plage Strength Index), the sum of the SoHO orbital velocity and the gravitational red shift velocity in km s^-1, the photon noise, the low-order p-modes region (from 0.9 to 1.2 mHz) called #1 and the high-order g-modes region (from 150 to 350 $\mu$ Hz) called #2 (the last three variables in units of ${\rm (m/s)^2/Hz}$ ). The photon noise level has been subtracted in these two last regions.
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In the text

$\begin{figure} \par\includegraphics[width=7.8cm,clip]{2779f14.eps}\end{figure}$ Figure 14: First ( top) and last ( bottom) 100-day PSD (in black) of GOLF velocity measurements (in ${\rm (m/s)^2/Hz}$ units). An estimator of the detector chain noise is computed by subtracting the signal of both PMs (see text).
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In the text

$\begin{figure} \par\mbox{\includegraphics[width=8.cm]{2779f15a.ps}\qquad \includegraphics[width=8.3cm]{2779f15b.ps} } \end{figure}$ Figure 15: Left: comparison of the blue- and red-wing power spectrum measured using the first 74 days of GOLF data. Right: evolution with time of the integrated p-mode power between 2.4 and 3.4 mHz using 100-day series shifted every 25 d. See the text for details.
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In the text

$\begin{figure} \par\includegraphics[width=8cm]{2779f1.ps}\end{figure}$	Figure 1: Diagram of the GOLF nominal working mode. The sunlight traverses a vapour cell containing a Na gas and placed inside a magnetic field that splits the measurements in both wings at $\pm$ 108 Å from the reference wavelength.
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$\begin{figure} \par\includegraphics[width=8cm,clip]{2779f2.eps}\end{figure}$	Figure 2: Time evolution of the phase difference between low-degree p modes simultaneously measured from GOLF and MDI instruments before correcting for the July 14, 2003 time lag ( right arrow). The re-synchronization made on February 8, 2002 is also visible ( left arrow). The vertical dashed lines correspond to the dates of the changes in the GOLF working cycle.
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$\begin{figure} \par\includegraphics[width=8cm,clip]{2779f3.ps}\end{figure}$	Figure 3: Counting rate (automatically corrected of SEUs) of both GOLF photomultipliers for the low magnetic modulation starting on July 13, 2000 (plotted only 1 point every 100 s).
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$\begin{figure} \par\includegraphics[width=8.8cm,clip]{2779f4.eps} \end{figure}$	Figure 4: GOLF PMs electron spectrum of the main channel for October 20, 1997. The optimal counting rate for the PMs is reached when the average impulse amplitude is $\sim$ 250 mV.
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$\begin{figure} \par\includegraphics[width=7.5cm,clip]{2779f5.eps} \end{figure}$	Figure 5: Effects of the high voltage perturbation over the PM1 counting rate. PM2 has no such perturbations. The time axis origin is August 20, 2000. During this period, a SoHO off-pointing event was visible in both tubes.
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$\begin{figure} \par {\includegraphics[angle=90,width=8cm,clip]{2779f6.ps} } \end{figure}$	Figure 6: Time evolution of the GOLF resonance cell stem temperature ( top) and the two photocathodes temperatures ( bottom. Black for PM1 and light gray for PM2). The time scale starts on April 11, 1996.
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$\begin{figure} \par {\includegraphics[angle=90,width=8cm,clip]{2779f7.ps} } \end{figure}$	Figure 7: Resonance cell stem temperature scan of January 17, 1996 for the PM1 in the four points of the sodium profile. The reference temperature is 171 $\hbox {$^\circ $ }$ C.
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$\begin{figure} \par {\includegraphics[angle=90,width=8.4cm,clip]{2779f8.ps} } \end{figure}$	Figure 8: Corrected photometric rates P⁺ and P^- starting on April 11, 1996 and up to June 2, 2004.
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$\begin{figure} \par {\includegraphics[angle=90,width=8.5cm]{2779f9.ps} } \end{figure}$	Figure 9: Example of 72 days of GOLF PM1 counting rates against PM2 for I^- in arbitrary units before ( top figure) and after ( bottom figure) applying all the corrections and scaling it into velocity (m/s).
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$\begin{figure} \par {\includegraphics[angle=90,width=8.2cm,clip]{2779f10.ps} } \end{figure}$	Figure 10: X magnitude (see text) as a function of time (starting April 11, 1996) in the top and as a function of the radial component of the orbital velocity in the bottom. The dashed lines in both panels describe the ideal linear response of the system to this radial orbital velocity.
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$\begin{figure} \par\includegraphics[angle=90,width=7.8cm]{2779f11.ps}\end{figure}$	Figure 11: Velocity residuals as a function of time for PM2 ( top), and after removing a low-frequency trend ( bottom). The signals have been undersampled to 2 h for display purposes only.
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$\begin{figure} \par\includegraphics[angle=90,width=8cm]{2779f12.ps}\end{figure}$	Figure 12: Three samples of one hour long time series from the V_X ( top and middle panels) and the V_S ( bottom panel) GOLF signal. The V_S is the calibrated velocity for PM2 following Ulrich et al. (2000).
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$\begin{figure} \par\includegraphics[width=7.8cm,clip]{2779f14.eps}\end{figure}$	Figure 14: First ( top) and last ( bottom) 100-day PSD (in black) of GOLF velocity measurements (in ${\rm (m/s)^2/Hz}$ units). An estimator of the detector chain noise is computed by subtracting the signal of both PMs (see text).
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$\begin{figure} \par\mbox{\includegraphics[width=8.cm]{2779f15a.ps}\qquad \includegraphics[width=8.3cm]{2779f15b.ps} } \end{figure}$	Figure 15: Left: comparison of the blue- and red-wing power spectrum measured using the first 74 days of GOLF data. Right: evolution with time of the integrated p-mode power between 2.4 and 3.4 mHz using 100-day series shifted every 25 d. See the text for details.
Open with DEXTER