Computer Science
Scientific paper
Jan 2001
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2001iaus..205..220t&link_type=abstract
Galaxies and their Constituents at the Highest Angular Resolutions, Proceedings of IAU Symposium #205, held 15-18 August 2000 at
Computer Science
Scientific paper
We present results from sub-arcsecond NIR integral field spectroscopy and mm-interferometry of the merging galaxy NGC 6240. Using stellar absorption features in the NIR we determined the stellar velocity field in NGC 6240 which shows a prograde encounter of two progenitor galaxies. Rotation velocities of up to 250 km s-1 indicate that the two compact NIR emission peaks are indeed the nuclei of massive progenitor galaxies. Using the velocity dispersion as a mass tracer an excess mass between the two nuclei is detected. This mass can be attributed to a massive rotating disk of cold CO gas located between the nuclei which is seen with mm-interferometry in the CO J=2rightarrow1 line. The collision of the two galaxies causes shock-heating of the interstellar medium in the interaction zone between the nuclei. This is detected through rovibrational emission lines of H2. The line profiles of the cold and hot molecular gas reveal very high velocities (up to 1000 km s-1) and the gas motions appear chaotic with a complex morphology and velocity structure. Even though there is a large gas reservoir in the interaction zone, the Brackett γ map shows little star formation in this region. The turbulent gas motions keep the gas clouds stable and prevent star formation. After the gas kinetic energy is dissipated and the turbulence has subsided the gas clouds can collapse and star formation, most likely in the form of a major starburst, can set in.
Genzel Reinhard
Tacconi Linda
Tecza Matthias
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