$\begin{figure} \par\rotatebox{-90}{\resizebox{10.1cm}{15cm}{\includegraphics{h1366f2.ps}}} \end{figure}$

Figure 2: Results of the SiO monitoring for the red supergiant VY CMa. On the left, optical (dots) and SiO (lines) variability curves. On the right, spectra (contours) and variability of the centroid (thick line) for the v=1 (bottom) and v=2 (top) J=1-0 maser lines. Contours for v=1 are: -25, 25, 50, 100, 200, 400, 600, 1000, 2000, and 3500 Jy. For v=2: -25, 25, 50, 100, 200, 300, 500, 1000, 1500, and 2500 Jy. In addition to the optical variability, we have also displayed an available IR monitoring of this object in L' (big black dots) and M (big grey dots) bands

$\begin{figure} \par\rotatebox{-90}{\resizebox{10.1cm}{15cm}{\includegraphics{h1366f3.ps}}}\end{figure}$

Figure 3: Same as Fig. 2 for the red supergiant $\mu$ Cep. The contours for both v=1 and v=2are: -15, 20, 40, 60, 80, 120, 150, 200, 400 and 600 Jy

$\begin{figure}\par\rotatebox{-90}{\resizebox{10.1cm}{15cm}{\includegraphics{h1366f4.ps}}}\end{figure}$

Figure 4: Same as Fig. 2 for the supergiant regular variable VX Sgr. v=1 contours: -10, 10, 25, 50, 100, 150, 200, 300, 400, and 500 Jy. v=2 contours: -10, 10, 25, 50, 75, 100, 150, 200, 250, and 300 Jy

$\begin{figure}\par\rotatebox{-90}{\resizebox{10.1cm}{15cm}{\includegraphics{h1366f5.ps}}}\end{figure}$

Figure 5: Same as Fig. 2 for the semiregular variable GY Aql. v=1 contours: -10, 10, 20, 40, 60, 90, 120, 160, 200, and 250 Jy. v=2 contours: -10, 10, 20, 40, 60, 90, 120, 160, and 200 Jy

$\begin{figure}\par\rotatebox{-90}{\resizebox{10.1cm}{15cm}{\includegraphics{h1366f6.ps}}}\end{figure}$

Figure 6: Same as Fig. 2 for the semiregular variable RT Vir. v=1 contours: -10, 5, 10, 15, 20, 30, 40, 50, 75, and 100 Jy. v=2 contours: -10, 5, 10, 20, 30, 50, 75, 100, 125, and 150 Jy

$\begin{figure}\par\rotatebox{-90}{\resizebox{10.1cm}{15cm}{\includegraphics{h1366f7.ps}}}\end{figure}$

Figure 7: Same as Fig. 2 for the Mira variable R Aqr. v=1 contours: -20, 20, 40, 60, 80, 100, 150, 200, 300, and 500 Jy. v=2 contours: -20, 20, 40, 60, 80, 100, 200, 400, 600, and 800 Jy. As for the case of VY CMa, we have also displayed IR monitorings of this object in L' and M bands

$\begin{figure}\par\rotatebox{-90}{\resizebox{10.1cm}{15cm}{\includegraphics{h1366f8.ps}}}\end{figure}$

Figure 8: Same as Fig. 2 for the Mira variable R Aql. v=1 contours: -5, 5, 10, 20, 30, 50, 100, 150, 200, and 250 Jy. v=2 contours: -5, 5, 10, 20, 30, 50, 75, 100, 140, and 180 Jy

$\begin{figure}\par\rotatebox{-90}{\resizebox{10.1cm}{15cm}{\includegraphics{h1366f9.ps}}}\end{figure}$

Figure 9: Same as Fig. 2 for the Mira variable TX Cam. v=1 contours: -15, 10, 20, 40, 60, 100, 200, 400, and 600 Jy. v=2 contours: -15, 10, 20, 40, 60, 100, 200, 300, 450, and 600 Jy

$\begin{figure}\par\rotatebox{-90}{\resizebox{10.1cm}{15cm}{\includegraphics{h1366f10.ps}}}\end{figure}$

Figure 10: Same as Fig. 2 for the Mira variable R Cnc. v=1 and v=2 contours: -10, 5, 10, 20, 30, 50, 75, 100, 125, and 150 Jy

$\begin{figure}\par\rotatebox{-90}{\resizebox{10.1cm}{15cm}{\includegraphics{h1366f11.ps}}}\end{figure}$

Figure 11: Same as Fig. 2 for the Mira variable R Cas. v=1 and v=2 contours: -20, 20, 40, 60, 100, 200, 400, 600, 800, and 1000 Jy

$\begin{figure}\par\rotatebox{-90}{\resizebox{10.1cm}{15cm}{\includegraphics{h1366f12.ps}}}\end{figure}$

Figure 12: Same as Fig. 2 for the Mira variable o Cet (Mira). v=1 and v=2 contours: -20, 20, 40, 60, 100, 200, 400, 600, 1000, and 2000 Jy

$\begin{figure}\par\rotatebox{-90}{\resizebox{10.1cm}{15cm}{\includegraphics{h1366f13.ps}}}\end{figure}$

Figure 13: Same as Fig. 2 for the S-type Mira variable $\chi$ Cyg. v=1 and v=2 contours: -2, 2, 5, 10, 20, 30, 40, and 55 Jy

$\begin{figure}\par\rotatebox{-90}{\resizebox{10.1cm}{15cm}{\includegraphics{h1366f14.ps}}}\end{figure}$

Figure 14: Same as Fig. 2 for the Mira variable U Her. v=1 and v=2 contours: -10, 10, 20, 40, 60, 80, 100, 150, 250, and 350 Jy

$\begin{figure}\par\rotatebox{-90}{\resizebox{10.1cm}{15cm}{\includegraphics{h1366f15.ps}}}\end{figure}$

Figure 15: Same as Fig. 2 for the Mira variable W Hya. v=1 contours: -20, 25, 50, 100, 200, 500, 1000, 1500, 2000, and 3000 Jy. v=2 contours: -20, 25, 50, 100, 200, 500, 1000, 2000, 3000, and 4000 Jy

$\begin{figure}\par\rotatebox{-90}{\resizebox{10.1cm}{15cm}{\includegraphics{h1366f16.ps}}}\end{figure}$

Figure 16: Same as Fig. 2 for the Mira variable X Hya. v=1 and v=2 contours: -2, 2, 5, 10, 15, 20, 30, and 45 Jy

$\begin{figure}\par\rotatebox{-90}{\resizebox{10.1cm}{15cm}{\includegraphics{h1366f17.ps}}}\end{figure}$

Figure 17: Same as Fig. 2 for the Mira variable R Leo. v=1 and v=2 contours: -20, 20, 40, 60, 100, 200, 400, 600, 1000, and 1400 Jy

$\begin{figure}\par\rotatebox{-90}{\resizebox{10.1cm}{15cm}{\includegraphics{h1366f18.ps}}}\end{figure}$

Figure 18: Same as Fig. 2 for the Mira variable R LMi. v=1 contours: -15, 10, 20, 40, 75, 100, 150, 200, 300, and 400 Jy. v=2 contours: -15, 5, 10, 20, 30, 50, 75, 100, 140, and 180 Jy

$\begin{figure}\par\rotatebox{-90}{\resizebox{10.1cm}{15cm}{\includegraphics{h1366f19.ps}}}\end{figure}$

Figure 19: Same as Fig. 22 for the Mira variable IK Tau (NML Tau). v=1 and v=2 contours: -20, 20, 40, 60, 80, 100, 200, 400, 700, and 900 Jy. The optical magnitude of this star is very weak resulting on poor visible light curves. Thus, the plot includes NIR light curves instead of optical data

$\begin{figure}\par\rotatebox{-90}{\resizebox{10.1cm}{15cm}{\includegraphics{h1366f20.ps}}}\end{figure}$

Figure 20: Same as Fig. 2 for the infrared source IRC +10011 (WX Psc). v=1 and v=2 contours: -10, 10, 20, 40, 60, 90, 120, 180, 250, and 350 Jy. No optical data are available for this star in the AAVSO international data base. NIR light curves corresponding to our observing period are plotted instead

$\begin{figure}\par\rotatebox{-90}{\resizebox{10.1cm}{15cm}{\includegraphics{h1366f21.ps}}}\end{figure}$

Figure 21: Same as Fig. 2 for the OH/IR star OH 26.5+0.6. v=1 contours: -3, 5, 10, 15, 20, 30, 40, and 55 Jy. v=2 contours: -3, 5, 10, 20, 30, 40, 60, and 90 Jy. No optical neither NIR variability curves are available for this object

$\begin{figure}\rotatebox{-90}{\resizebox{10.1cm}{15cm}{\includegraphics{h1366f22.ps}}}\end{figure}$

Figure 22: Same as Fig. 2 for the young stellar source Orion IRc2. v=1 and v=2 contours: -20, 20, 40, 60, 100, 200, 500, 1000, 1500, and 2000 Jy. No velocity centroid curve is shown in this case

7. Figures 2-22