All Figures

$\begin{figure} \par\includegraphics[angle=0,width=8cm]{1872fi1a.eps}\vspace*{2mm} \includegraphics[angle=-90,width=8cm]{1872fi1b.eps}\end{figure}$ Figure 1: Top panel: OH maser emission from IRAS 20126+4104 (black contours) superimposed on an image of the 3.6-cm continuum emission (greyscale and white contours) from Hofner et al. (2004), aligned in J2000 coordinates. The OH masers peak flux is 13.3 Jy/beam and the contour levels of the map are 1, 3, 5, 7 and 9 Jy/beam. The straight lines refer to the jet/outflow directions (C99), while the box shows the location of the bottom panel. Bottom panel: positions and velocities of the OH, H₂O and methanol maser components and the position of the 3.6 cm peak with accuracy bar (Hofner priv. comm.). The cross bars in the bottom right corner show OH masers position uncertainty. Note the close association of the three masers species and particularly between the OH and methanol masers.
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In the text

$\begin{figure} \par\includegraphics[angle=0,width=5.7cm]{1872fig2.eps}\end{figure}$ Figure 2: H₂O masers spectra towards IRAS 20126+4104 from the MERLIN observations in March 2002 (solid line) compared with that of Medicina single dish observations in Nov. 1997 (dashed line) from MCR. MERLIN detected no emission between velocities 10 to 16 km s^-1 while the component centred at -7.1 km s^-1 became very bright. The axis on the left side shows the MERLIN intensity and the axis on the right side shows the Medicina intensity
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In the text

$\begin{figure} \par\includegraphics[angle=270,width=8cm]{1872fig3.eps}\end{figure}$ Figure 3: Comparison between the water masers positions from our MERLIN and the VLBA observations towards IRAS 20126+4104. Between these observations the masers spots have either changed almost completely or perhaps have moved to the south west. MCR maser spots located very far from the MERLIN spots are not shown.
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In the text

$\begin{figure} \par\includegraphics[angle=0,width=5.7cm]{1872fig4.eps}\end{figure}$ Figure 4: CH₃OH maser spectrum towards IRAS 20126+4104 from MERLIN (solid line) compared with spectrum of Onsala-Effelsberg baseline (dashed line) from Minier et al. (2001).
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In the text

$\begin{figure} \par\includegraphics[angle=0,width=6cm]{1872fig5}\end{figure}$ Figure 5: The integrated OH maser emission (white contours) superimposed on the K (2.2- $\mu$ m) image of the source (inverted greyscale and black contours), from Sridharan et al. (2004). The OH masers clearly arise from the material giving rise to the dark extinction lane between the two lobes of the nebula. The extinction lane is due to the material in a circumstellar disk around the central source. The positional uncertainty in the IR image is estimated to be 0.1''.
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In the text

$\begin{figure} \par\includegraphics[angle=270,width=8.8cm]{1872fig6.ps}\end{figure}$ Figure 6: The OH (open symbols) and methanol (filled symbols) maser velocities against the corresponding offset from the direction of the jet axis. The offset is computed with respect to the position of the centre of the OH masers cluster. The curves represent the velocities for Keplerian motion around a central mass of 1, 5, 10, 15 20 and 30 $M_\odot$ as indicated. The systemic velocity is taken to be -4.5 km s^-1 (Cesaroni, priv. comm.).
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In the text

$\begin{figure} \par\includegraphics[angle=270,width=8cm]{1872fig3.eps}\end{figure}$	Figure 3: Comparison between the water masers positions from our MERLIN and the VLBA observations towards IRAS 20126+4104. Between these observations the masers spots have either changed almost completely or perhaps have moved to the south west. MCR maser spots located very far from the MERLIN spots are not shown.
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$\begin{figure} \par\includegraphics[angle=0,width=5.7cm]{1872fig4.eps}\end{figure}$	Figure 4: CH₃OH maser spectrum towards IRAS 20126+4104 from MERLIN (solid line) compared with spectrum of Onsala-Effelsberg baseline (dashed line) from Minier et al. (2001).
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