Other
Scientific paper
Jul 2011
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2011yera.confe..39r&link_type=abstract
The 41st Young European Radio Astronomers Conference, held at University of Manchester/Jodrell Bank Observatory, 18-20 July 2011
Other
Scientific paper
Since hot molecular cores are considered the cradle of massive stars, the study of their gas kinematics is key to better understand the physical processes leading to massive star formation. Previous observations of rotational transitions from vibrationally excited levels of HC3N (hereafter HC3N*) towards the Sgr B2M and Sgr B2N hot cores, revealed the existence of two systematic trends in these high-mass star forming regions: i) a decrease of the linewidth with increasing energy of the vibrational levels involved in the transition; and ii) an increase of the linewidth with the size of the HC3N* emitting region. Since these systematic trends may be related to the global processes of high-mass star formation, it is necessary to clearly establish whether these trends are also found toward other hot cores with different total luminosities or gas masses. Here, we present observations of several rotational transitions of HC3N* toward a sample of 10 hot cores whose luminosities span from several 103 to ~108 solar luminosities. Our results show that the systematic trends for the HC3N* linewidths to decrease with increasing energy of the transition, and to decrease with the size of the emitting region, are preserved toward the observed hot cores. This is explained by the fact that the emission from the lower energy transitions of HC3N* likely shows a contribution from high-velocity shocked gas arising from molecular outflows. This suggests that molecular outflows are the major agent, over collapse and/or rotation, affecting the global kinematics in massive star forming regions. In addition, our HC3N* data reveals a clear correlation between the linewidths of the HC3N* 1v6 and 1v7 lines and the total luminosity measured in these regions, suggesting that HC3N* is an excellent tool to link the gas kinematics of hot cores with their global properties such as total luminosity or mass.
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