All Figures

$\begin{figure} \par\mbox{\includegraphics[width=5.6cm,clip]{0309fig5_a.eps} \inc... ...fig5_e.eps} \includegraphics[width=5.6cm,clip]{0309fig5_f.eps} } \end{figure}$ Figure 5: Results of the time series analysis for 6 regular variables in our sample. This figure provides information only on the variability periods in optical and SiO (both peak and integrated area in v=1 and v=2). The complete information obtained from this analysis for all suitable objects, including delays between SiO and optical or NIR maxima is provided in Table 2.
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In the text

$\begin{figure} \par\includegraphics[angle=-90,width=16.5cm,clip]{0309fig6.eps} \end{figure}$ Figure 6: SiO versus NIR and Optical phase lag histograms for a sample that consists on the four SiO delays listed in Cols. 4 and 7 of Table 2 for those objects where suitable optical (from the AAVSO) and/or NIR (from LeB93) data exist.
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In the text

$\begin{figure} \par\mbox{\includegraphics[angle=270,width=3.72cm,clip]{0309fig7_... ...s} \includegraphics[angle=270,width=3.3cm,clip]{0309fig7_j.eps} } \end{figure}$ Figure 7: Comparison of optical, SiO, and NIR (Smith et al. 2002, 2003) light curves in a subset of objects from our sample. The cases of o Cet, R Aqr and R Cas are of particular interest (see text). Dates of optical maxima are indicated by vertical lines unless otherwise indicated.
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In the text

$\begin{figure} \par\includegraphics[angle=270,width=17cm,clip]{NEW_FIG/0309fig8_grey.eps} \end{figure}$ Figure 8: Left: optical and ²⁸SiO v=1,2 J=1-0 light curves of o Cet (Mira) between mid 1984 and mid 1995. The v=2 curves have been shifted by 600 Jy (peak) and 2000 Jy km s^-1 (area) for clarity. Right: time evolution of the monitored SiO lines as a function of LSR velocity. The contours mark the following flux levels (in Jy): 20, 40, 60, 100, 200, 400, 600, 1000, and 2000 for both v=1 and v=2. Dates of optical maxima are indicated by vertical lines. The solid horizontal line in the right panels represents the velocity of the CO J=2-1 peak emission, the dashed horizontal lines are the velocities at which the CO emission is half of the peak, and the dotted horizontal lines represent the terminal velocities at which CO emission disappears (from Cernicharo et al. 1997). The small vertical ticks mark the dates of observations.
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In the text

$\begin{figure} \par\includegraphics[angle=270,width=17.5cm,clip]{NEW_FIG/0309fig9_grey.eps} \end{figure}$ Figure 9: Same as Fig. 8 but for GY Aql. The CO velocities are not shown in this case. The v=2 curves on the left panel have been shifted by 50 Jy (peak) and 200 Jy km s^-1 (area) for clarity. The contour levels for SiO are: 10, 20, 40, 60, 90, 120, 160, 200, and 250 Jy for both v=1 and v=2.
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In the text

$\begin{figure} \par\includegraphics[width=17.7cm]{0309fig10_grey.eps} \end{figure}$ Figure 10: Left: near-Infrared (3.79 $\mu$ m, dots connected by a black solid line, and 4.64 $\mu$ m, dots connected by a blue solid line) and ²⁸SiO v=1, 2 J=1-0 light curves of IK Tau. The v=2 curves on the left panel have been shifted by 300 Jy (peak) and 1000 Jy km s^-1 (area) for clarity. From the time series analysis of optical, NIR and SiO light curves the periods have been determined (see Table 2) and they all are in remarkable agreement. This object, together with R Aqr, is a good example for showing that NIR and ²⁸SiO light curves have very little phase lag. The right panels show the time evolution of the monitored SiO lines as a function of LSR velocity. The contours mark the following levels (in Jy): 20, 40, 60, 80, 100, 200, 400, 600, and 900 for both v=1 and v=2 in IK Tau.
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In the text

$\begin{figure} \par\includegraphics[width=18cm,clip]{0309fig1.eps} \end{figure}$ Figure 1: SiO data of the young stellar object Orion Irc2. For clarity, we have introduced shifts in the lower left pannels for v=2 data with respect to v=1 data: 200 Jy (peak) and 500 Jy km s^-1 (area). The contours correspond to the following levels (in Jy): and 50, 100, 150, 200, 400, 700, 1000, 1500, and 2000 for both v=1 and v=2.
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In the text

$\begin{figure} \par\includegraphics[width=18cm,clip]{0309fig2.eps} \end{figure}$ Figure 2: This figure and the following two display the optical and SiO data of the three objects of our sample classified as supergiant stars (VY CMa, VX Sgr and $\mu$ Cep). For each object, the upper left panel shows the optical (dots) light curves from the AAVSO database. In the case of VY CMa there are in addition two infrared curves from LeB93: 3.79 $\mu$ m (M_L, dots connected by a black solid line) and 4.64 $\mu$ m (M_M, dots connected by a blue solid line). The lower left panel shows the ²⁸SiO v=1, 2 J=1-0 light curves from the Yebes monitoring. Vertical lines mark the epochs of optical maxima (if there is optical periodicity). The right panel shows for each object the time evolution of the monitored SiO lines as a function of LSR velocity. The contours for VY CMa correspond to the following levels (in Jy): 50, 100, 200, 400, 600, 1000, 1500, 2000, and 2500 for both v=1 and v=2. The small vertical ticks mark the dates of observations.
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In the text

$\begin{figure} \par\includegraphics[width=18cm,clip]{0309fig3.eps} \end{figure}$ Figure 3: Analogous curves to those displayed in Fig. 2 but for VX Sgr. The shifts introduced in the lower left panels are the following: 300 Jy (peak) and 3000 Jy km s^-1 (area). The contours correspond to the following levels (in Jy): 25, 50, 75, 100, 150, 200, 300, 400, and 500 for v=1, and 15, 25, 50, 75, 100, 150, 200, 250, and 300 for v=2.
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In the text

$\begin{figure} \par\includegraphics[width=18cm,clip]{0309fig4.eps} \end{figure}$ Figure 4: Analogous curves to those displayed in Fig. 2 but for $\mu$ Cep. The shifts introduced in the lower left pannels have been the following: 200 Jy (peak) and 500 Jy km s^-1 (area). The contours correspond to the following levels (in Jy): 20, 50, 80, 120, 150, 200, 300, 400, and 500 for both v=1 and v=2.
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In the text

$\begin{figure} \par\includegraphics[angle=0,width=18cm,clip]{0309fig11.eps} \end{figure}$ Figure 11: Left: near-Infrared (3.79 $\mu$ m, dots connected by a black solid line, and 4.64 $\mu$ m, dots connected by a blue solid line) and ²⁸SiO v=1,2 J=1-0 light curves of R Aqr. For R Aqr we have applied shifts to the v=2 curves of 200 Jy (peak) and 1000 Jy km s^-1 (area) for clarity. In addition, optical light curves are also available and shown. From the time series analysis of optical, NIR and SiO light curves the periods have been determined (see Table 2) and they all are in remarkable agreement. This object, together with IK Tau, is a very good example for showing that NIR and ²⁸SiO light curves have very little phase lag. The right panels show the time evolution of the monitored SiO lines as a function of LSR velocity. The contours mark the following levels (in Jy): and 20, 50, 100, 150, 200, 300, 500, 750, and 1000 in both v=1 and v=2.
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In the text

$\begin{figure} \par\includegraphics[angle=0,width=18cm,clip]{0309fig12.eps} \end{figure}$ Figure 12: Left: near-Infrared (3.79 $\mu$ m, dots connected by a black solid line, and 4.64, $\mu$ m dots connected by a blue solid line) and ²⁸SiO v=1,2 J=1-0 light curves of IRC+10011 between 1988 and mid 1995. The v=2 curves on the left panel have been shifted by 100 Jy (peak) and 300 Jy km s^-1 (area) for clarity. From the NIR and SiO data the corresponding periods have been determined (see Table 2) with the result of a remarkable agreement and almost no phase lag at the maxima. The right panels show the time evolution of the monitored SiO lines as a function of LSR velocity. The contours mark the following levels (in Jy): 20, 40, 60, 90, 120, 180, 250, 350, and 400 for both v=1 and v=2.
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In the text

$\begin{figure} \par\includegraphics[angle=0,width=18cm,clip]{0309fig13.eps} \end{figure}$ Figure 13: Same as Fig. 9 but for OH26.5+0.6. The contour levels for SiO are: 10, 25, 50, 75, 100, 150, 200, 300, and 400 Jy for both v=1 and v=2.
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In the text

$\begin{figure} \par\includegraphics[angle=0,width=18cm,clip]{0309fig14.eps} \end{figure}$ Figure 14: Same as Fig. 9 but for R Leo. The contour levels for SiO are: 20, 40, 60, 100, 200, 400, 600, 1000, and 1400 Jy for both v=1 and v=2. For clarity, the v=2 peak and area curves have been shifted by 500 Jy (peak) and 2000 Jy km s^-1 respectively.
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In the text

$\begin{figure} \par\includegraphics[angle=0,width=18cm,clip]{0309fig15.eps} \end{figure}$ Figure 15: Same as Fig. 9 but for R Cas. The contour levels for SiO are: 20, 40, 60, 100, 200, 400, 600, 800, and 1000 for both v=1 and v=2. For clarity, the v=2 peak and area curves have been shifted by 500 Jy (peak) and 2000 Jy km s^-1 respectively.
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In the text

$\begin{figure} \par\includegraphics[angle=0,width=18cm,clip]{0309fig16.eps} \end{figure}$ Figure 16: Same as Fig. 9 but for R LMi. The contour levels for SiO are: 10, 20, 40, 75, 100, 150, 200, 300 and 400 Jy (v=1), and 10, 20, 30, 50, 75, 100, 150, 200 and 300 (v=2). For clarity, the v=2 peak and area curves have been shifted by 400 Jy (peak) and 1000 Jy km s^-1 respectively.
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In the text

$\begin{figure} \par\includegraphics[angle=0,width=18cm,clip]{0309fig17.eps} \end{figure}$ Figure 17: Same as Fig. 9 but for R Aql. The contour levels for SiO are: 5, 10, 20, 30, 50, 100, 150, 200, and 250 for both v=1 and v=2. For clarity, the v=2 peak and area curves have been shifted by 100 Jy (peak) and 300 Jy km s^-1 respectively.
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In the text

$\begin{figure} \par\includegraphics[angle=0,width=18cm,clip]{0309fig18.eps} \end{figure}$ Figure 18: Same as Fig. 9 but for W Hya. The contour levels for SiO are 25, 50, 100, 200, 500, 1000, 1500, 2000, and 3000 Jy for both v=1 and v=2. For clarity, the v=2 peak and area curves have been shifted with respect to v=1 by 1000 Jy and 5000 Jy km s^-1 respectively.
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In the text

$\begin{figure} \par\includegraphics[angle=0,width=18cm,clip]{0309fig19.eps} \end{figure}$ Figure 19: Same as Fig. 9 but for R Cnc. The contour levels for SiO are 10, 20, 40, 60, 75, 100, 150, 200, and 250 Jy in both v=1 and v=2. For clarity, the v=2 peak and area curves have been shifted with respect to v=1 by 100 Jy and 200 Jy km s^-1 respectively.
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In the text

$\begin{figure} \par\includegraphics[angle=0,width=18cm,clip]{0309fig20.eps} \end{figure}$ Figure 20: Same as Fig. 9 but for TX Cam. The contour levels for SiO are 10, 20, 40, 60, 100, 200, 300, 500, and 750 Jy in both v=1 and v=2. For clarity, the v=2 peak and area curves have been shifted with respect to v=1 by 500 Jy and 1000 Jy km s^-1 respectively.
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In the text

$\begin{figure} \par\includegraphics[angle=0,width=18cm,clip]{0309fig21.eps} \end{figure}$ Figure 21: Same as Fig. 9 but for U Her. The contour levels for SiO are 10, 20, 40, 60, 80, 100, 150, 250, and 350 Jy in both v=1 and v=2. For clarity, the v=2 peak and area curves have been shifted with respect to v=1 by 200 Jy and 500 Jy km s^-1 respectively.
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In the text

$\begin{figure} \par\mbox{\includegraphics[width=5.6cm,clip]{0309fig5_a.eps} \inc... ...fig5_e.eps} \includegraphics[width=5.6cm,clip]{0309fig5_f.eps} } \end{figure}$	Figure 5: Results of the time series analysis for 6 regular variables in our sample. This figure provides information only on the variability periods in optical and SiO (both peak and integrated area in v=1 and v=2). The complete information obtained from this analysis for all suitable objects, including delays between SiO and optical or NIR maxima is provided in Table 2.
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$\begin{figure} \par\includegraphics[angle=-90,width=16.5cm,clip]{0309fig6.eps} \end{figure}$	Figure 6: SiO versus NIR and Optical phase lag histograms for a sample that consists on the four SiO delays listed in Cols. 4 and 7 of Table 2 for those objects where suitable optical (from the AAVSO) and/or NIR (from LeB93) data exist.
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$\begin{figure} \par\mbox{\includegraphics[angle=270,width=3.72cm,clip]{0309fig7_... ...s} \includegraphics[angle=270,width=3.3cm,clip]{0309fig7_j.eps} } \end{figure}$	Figure 7: Comparison of optical, SiO, and NIR (Smith et al. 2002, 2003) light curves in a subset of objects from our sample. The cases of o Cet, R Aqr and R Cas are of particular interest (see text). Dates of optical maxima are indicated by vertical lines unless otherwise indicated.
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$\begin{figure} \par\includegraphics[angle=270,width=17.5cm,clip]{NEW_FIG/0309fig9_grey.eps} \end{figure}$	Figure 9: Same as Fig. 8 but for GY Aql. The CO velocities are not shown in this case. The v=2 curves on the left panel have been shifted by 50 Jy (peak) and 200 Jy km s^-1 (area) for clarity. The contour levels for SiO are: 10, 20, 40, 60, 90, 120, 160, 200, and 250 Jy for both v=1 and v=2.
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$\begin{figure} \par\includegraphics[width=18cm,clip]{0309fig1.eps} \end{figure}$	Figure 1: SiO data of the young stellar object Orion Irc2. For clarity, we have introduced shifts in the lower left pannels for v=2 data with respect to v=1 data: 200 Jy (peak) and 500 Jy km s^-1 (area). The contours correspond to the following levels (in Jy): and 50, 100, 150, 200, 400, 700, 1000, 1500, and 2000 for both v=1 and v=2.
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$\begin{figure} \par\includegraphics[width=18cm,clip]{0309fig3.eps} \end{figure}$	Figure 3: Analogous curves to those displayed in Fig. 2 but for VX Sgr. The shifts introduced in the lower left panels are the following: 300 Jy (peak) and 3000 Jy km s^-1 (area). The contours correspond to the following levels (in Jy): 25, 50, 75, 100, 150, 200, 300, 400, and 500 for v=1, and 15, 25, 50, 75, 100, 150, 200, 250, and 300 for v=2.
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$\begin{figure} \par\includegraphics[width=18cm,clip]{0309fig4.eps} \end{figure}$	Figure 4: Analogous curves to those displayed in Fig. 2 but for $\mu$ Cep. The shifts introduced in the lower left pannels have been the following: 200 Jy (peak) and 500 Jy km s^-1 (area). The contours correspond to the following levels (in Jy): 20, 50, 80, 120, 150, 200, 300, 400, and 500 for both v=1 and v=2.
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$\begin{figure} \par\includegraphics[angle=0,width=18cm,clip]{0309fig13.eps} \end{figure}$	Figure 13: Same as Fig. 9 but for OH26.5+0.6. The contour levels for SiO are: 10, 25, 50, 75, 100, 150, 200, 300, and 400 Jy for both v=1 and v=2.
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$\begin{figure} \par\includegraphics[angle=0,width=18cm,clip]{0309fig14.eps} \end{figure}$	Figure 14: Same as Fig. 9 but for R Leo. The contour levels for SiO are: 20, 40, 60, 100, 200, 400, 600, 1000, and 1400 Jy for both v=1 and v=2. For clarity, the v=2 peak and area curves have been shifted by 500 Jy (peak) and 2000 Jy km s^-1 respectively.
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$\begin{figure} \par\includegraphics[angle=0,width=18cm,clip]{0309fig15.eps} \end{figure}$	Figure 15: Same as Fig. 9 but for R Cas. The contour levels for SiO are: 20, 40, 60, 100, 200, 400, 600, 800, and 1000 for both v=1 and v=2. For clarity, the v=2 peak and area curves have been shifted by 500 Jy (peak) and 2000 Jy km s^-1 respectively.
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$\begin{figure} \par\includegraphics[angle=0,width=18cm,clip]{0309fig16.eps} \end{figure}$	Figure 16: Same as Fig. 9 but for R LMi. The contour levels for SiO are: 10, 20, 40, 75, 100, 150, 200, 300 and 400 Jy (v=1), and 10, 20, 30, 50, 75, 100, 150, 200 and 300 (v=2). For clarity, the v=2 peak and area curves have been shifted by 400 Jy (peak) and 1000 Jy km s^-1 respectively.
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$\begin{figure} \par\includegraphics[angle=0,width=18cm,clip]{0309fig17.eps} \end{figure}$	Figure 17: Same as Fig. 9 but for R Aql. The contour levels for SiO are: 5, 10, 20, 30, 50, 100, 150, 200, and 250 for both v=1 and v=2. For clarity, the v=2 peak and area curves have been shifted by 100 Jy (peak) and 300 Jy km s^-1 respectively.
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$\begin{figure} \par\includegraphics[angle=0,width=18cm,clip]{0309fig18.eps} \end{figure}$	Figure 18: Same as Fig. 9 but for W Hya. The contour levels for SiO are 25, 50, 100, 200, 500, 1000, 1500, 2000, and 3000 Jy for both v=1 and v=2. For clarity, the v=2 peak and area curves have been shifted with respect to v=1 by 1000 Jy and 5000 Jy km s^-1 respectively.
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$\begin{figure} \par\includegraphics[angle=0,width=18cm,clip]{0309fig19.eps} \end{figure}$	Figure 19: Same as Fig. 9 but for R Cnc. The contour levels for SiO are 10, 20, 40, 60, 75, 100, 150, 200, and 250 Jy in both v=1 and v=2. For clarity, the v=2 peak and area curves have been shifted with respect to v=1 by 100 Jy and 200 Jy km s^-1 respectively.
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$\begin{figure} \par\includegraphics[angle=0,width=18cm,clip]{0309fig20.eps} \end{figure}$	Figure 20: Same as Fig. 9 but for TX Cam. The contour levels for SiO are 10, 20, 40, 60, 100, 200, 300, 500, and 750 Jy in both v=1 and v=2. For clarity, the v=2 peak and area curves have been shifted with respect to v=1 by 500 Jy and 1000 Jy km s^-1 respectively.
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$\begin{figure} \par\includegraphics[angle=0,width=18cm,clip]{0309fig21.eps} \end{figure}$	Figure 21: Same as Fig. 9 but for U Her. The contour levels for SiO are 10, 20, 40, 60, 80, 100, 150, 250, and 350 Jy in both v=1 and v=2. For clarity, the v=2 peak and area curves have been shifted with respect to v=1 by 200 Jy and 500 Jy km s^-1 respectively.
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