Infrared Space Observatory long wavelength spectrometer observations of a cold giant molecular cloud core near the Galactic center

We have used the Long Wavelength Spectrometer aboard the Infrared Space Obs ervatory in the grating mode to map the far-infrared continuum emission (45 -175 mu m) toward the massive giant molecular cloud core GCM 0.25+0.11 loca ted near the Galactic center. Graybody models of the observed far-infrared spectral energy distribution indicate that the bulk of the dust in the diff use component along the line of sight toward GC-M 0.25+0.11 has a mean temp erature of similar to 26 K and a 100 mu m optical depth of similar to 0.17. GCM 0.25+0.11 is observed in emission at far-infrared (FIR) wavelengths (g reater than or similar to 100 mu m). However at midinfrared wavelengths (le ss than or similar to 70 mu m) the core is seen in absorption against the g eneral Galactic center background. This indicates that GCM 0.25+0.11 is loc ated in front of the bulk of the dust responsible for the diffuse FIR emiss ion, most likely a few hundred parsecs from the Galactic center. By subtrac ting the spectrum of the diffuse component from the spectrum observed towar d GCM 0.25+0.11, we have been able to extract the intrinsic spectrum of thi s GMC core. Graybody fits to the resulting far-infrared spectrum combined w ith our previous submillimeter measurements (350-800 mu m) give a low tempe rature similar to 18 K for the bulk of the dust in the GCM 0.25+0.11 core. In addition, the grain emissivity is a very steep function of frequency (nu (2.8)). The high grain emissivity exponent is consistent with the presence of dust grains covered with thick ice mantles. We have complemented our ISO data with CO (2-1) and HCO+ (3-2) observations carried out with the Caltec h Submillimeter Observatory. The molecular emission shows a large velocity gradient across the southern part of the core indicative of streaming motio ns of the gas or of the presence of multiple, spatially overlapping velocit y components. The observed gas kinematics may indicate that GCM 0.25+0.11 i s in the process of being disrupted by the strong tidal forces caused by th e high mass concentration in the Galactic center region. This might explain why there is no evidence for ongoing high-mass star formation associated w ith this core, in spite of its large molecular mass. However, the mean H-2 density of GCM 0.25+0.11 is well above the tidal stability limit for a Gala ctocentric distance of a few hundred parsecs implied by our observations. A n alternative explanation is that we are witnessing the very early stage of a cloud-cloud collision that may result in a future star formation episode .