A SEARCH FOR NH IN THE LARGE MAGELLANIC CLOUD

Results

In Fig.1 we present the observed spectra towards positions chosen on the basis of our HI data. For every spectrum, we extracted the HI spectra out of our data cube at the corresponding position, except for Fig.1f where we instead extracted a CO spectrum out of the CfA 1.2m telescope CO survey as published in Cohen et al. (1988). No emission was detected with upper limits of 25 to 74 mK (, where is listed in Column 4 of Table 1). In all of the HI spectra there are features which correspond to the two major gas components at 260 km and 280 km \ (Luks and Rohlfs 1992), but a wide variety of other emission and absorption features which show the complex structure of the atomic gas in this region. Fig.2 shows the spectra towards the IRAS Sources LI-LMCÒš1501, LI-LMCÒš1541 and LI-LMCÒš1609. The ticks in these spectra indicate the velocities at which Israel et al. (1993) detected CO. Again, no emission is detected.

ÒšÒš
Figure 2: spectra towards IRAS point sources LI-LMCÒš1501, LI-LMCÒš1541, LI-LMCÒš1609. The ticks indicate the velocity of CO components detected with the SEST telescope by Israel et al. (1993).

Ò? Copyright Astronomical Society of Australia 1997