All Figures

Figure 1: Objects in the CRL 2136 region: the upper panel shows the positions of radio sources 3 and 4 (filled circles), infrared source 1 (filled square), and the class II CH3OH maser (filled pentagon). The three little stars mark the positions from which of 1665 MHz RCP maser emission arises and the circles mark LCP emission. For the OH emission, the symbol sizes reflect the position uncertainties. The (at this scale) unresolved dot at the (0, 0) position represents the Q-band map of RS 4, an enlarged image of which is shown in Fig. 2. The square around it indicates its position uncertainty. The dotted rectangle outlines the region containing H2O maser emission shown in detail in Fig. 4 and the dashed rectangle outlines an enlarged region shown in the lower panel.

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In the text

Figure 2: Radio source 4 at 43.3 GHz: the contours represent 5, 7, 9, and 11 times the 2.7 mJy beam-1 rms noise in our 43.3 GHz map. The dotted ellipse in the lower left corner represents the FWHM size of the Gaussian restoring beam, while the full line ellipses represent the maximum and nominal FWHM source size from JMFIT (see discussion in text). Angular offsets are relative to the position given in Table 1.

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In the text

Figure 3: Top panel: H2O spectrum taken at the Effelsberg 100 m telescope on 2002 December 26. Second panel from top: VLA H2O spectrum made from our 1992 May 19 data at the pixel with maximum emission. In the third panel from top the intensity axis is expanded to show the extremely weak emission at the lowest and highest velocities. The arrows show the velocity ranges over which maps of integrated emission, marked by the rectangles in Fig. 4 were produced. The lower panel shows the RCP and LCP emission of the OH 1665 MHz line published by Argon et al. (2000). For details of how the spectrum was formed see this reference. The dotted vertical lines mark the FWHM linewidths of various molecular species mapped by van der Tak et al. (2000b), who determine a centroid LSR velocity of 22.8(0.1) km s-1. The solid line marks the velocity of the single, narrow 6.7 GHz CH3OH maser feature (Caswell et al. 1995).

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In the text

Figure 4: Area containing the H2O maser emission, indicated by the dashed rectangle in Fig. 1. The error bars in the upper panel give the positions of H2O masers determined from channel by channel fitting of the H2O data cube. The centers of the full line rectangles are the positions of the centroid positions of maps integrated over the velocity ranges given (and indicated in Fig. 3); the sizes corresponds to the errors of the fitted position. The dotted rectangle encloses the two regions of strongest emission, whose velocity ranges are given. This area is shown in more detail in the lower panel, in which the emission in the dotted rectangles spreads over the indicated velocities. Position offsets are relative to the position of RS 4 given in Table 1. Note that the relative registration of the H2O and RS 4 have an estimated error of 0.3 arcsec.

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In the text

	Figure 5: The radio-to-submillimeter-wavelength spectral energy distributions of CRL 2136 IRS 1/RS 4 ( full dots) and Orion source I ( open dots). The full line represents a fit to our 4.9 to 43.3 GHz data for RS 4, while the dashed line is a fit to the submillimeter data of Kastner et al. (1994). Error bars of flux densities are smaller than or comparable to the symbol sizes.
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In the text