Hot molecular cores in young stellar objects of different luminosities

Details Hot molecular cores in young stellar objects of different luminosities Hot molecular cores in young stellar objects of different luminosities

May 2011

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2011iaus..280p.328s&link_type=abstract

The Molecular Universe, Posters from the proceedings of the 280th Symposium of the International Astronomical Union held in Tole

Astronomy and Astrophysics

Astronomy

Scientific paper

First discovered in the vicinity of massive protostars, hot molecular cores (HMCs) are compact (≲0.1 pc) and dense (≳107 cm-3) objects with relatively high temperatures (≳100 K) that show a very rich chemistry in complex organic molecules (e. g., CH_3CN, CH_3OH). They are considered to be one of the first evolutionary signposts of massive star formation. However, many questions remain still open regarding HMCs. Must all the (massive) protostars undergo the HMC stage? Which is the lifetime of HMCs? Are the HMCs specifically associated with a dominant star formation phenomena? In this work, we present interferometric observations toward two young stellar objects (YSOs) of different luminosities (102 {L}&sun; and 105 {L}&sun;) in order to compare the properties of their hot molecular cores, simultaneously to their outflow, dense gas and radiocontinuum emission. The hot core emission for these two YSOs appears associated with faint ionized gas emission likely tracing radiojets, molecular outflows and dense gas, suggesting that HMCs are associated with outflowing activity. The possibility that hot cores are heated not only directly from the embedded YSO but also from shocks of the outflow/jet is explored.

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