Description of source "NGC 6334I (N)" from Beuther et al. (2005)

We do not detect any compact thermal NH3 or CH3OH emis-sion toward NGC 6334I(N) (Fig. 2). However, the extended NH3 emission has about the same peak intensities as NGC 6334I but is distributed over a large area (>10) without a distinct peak position. The millimeter peak detected by T. R. Hunter et al. (2005, in preparation) is located approximately at the center of the large-scale NH3 core. The NH3 (1, 1) and (2, 2) emission has a spatial distribution similar to that of the NH3 (3, 3) emission previously reported by Kraemer & Jackson (1999).

While we do not detect any thermal CH3OH emission, we find Class I CH3OH maser emission from the CH3OH (32,1–31,2) E and CH3OH (42,2–41,3) E lines . Both lines show a maser component at ap-proximately ~3 km s~1, but the CH3OH (42,2~41,3) E line ex-hibits another maser component at approximately 5 km s~1 (Fig. 3). The spatial positions of the ~3 km s~1 components are approximately 700 northeast of the millimeter peak in the direc-tion of the collimated SiO outflow, whereas the ~5 km s~1 com-ponent is located about 1000 south of the millimeter peak (the exact positions are given in Table 2). The observed peak bright-ness temperature of the ~3 km s~1 line is 7000 K (Fig. 3). The ~5 km s~1 component is less clearly associated with one of the two outflow axes, but both components are spatially close to pre-viously detected Class I CH3OH (70–61) A+ 44 GHz maser posi-tions (Kogan & Slysh 1998). We note that there are significantly fewer, just two, 25 GHz maser components detected than 44 GHz components. The 23 maser spots observed in the latter line are spread over an area of 2300 ; 3200, which is somewhat larger but comparable to the 1500 separation of the 25 GHz components.

The positional offsets between the 44 and 25 GHz maser posi-tions may be due to the loss of absolute positional information during self-calibration of the 44 GHz data by Kogan & Slysh (1998). Performing Gaussian fits to the CH3OH data in the image plane, we get slightly extended features compared to the beam size. This indicates unresolved spatial blending of different ma-ser components within each channel width of 0.2 km s~1.