Structure of the Dense Molecular Gas in the NGC 1333 IRAS 4 Region

Details Structure of the Dense Molecular Gas in the NGC 1333 IRAS 4 Region Structure of the Dense Molecular Gas in the NGC 1333 IRAS 4 Region

Dec 2004

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2004apj...617.1157c&link_type=abstract

The Astrophysical Journal, Volume 617, Issue 2, pp. 1157-1166.

Astronomy and Astrophysics

Astronomy

10

Ism: Individual: Ngc Number: Ngc 1333 Iras 4, Ism: Molecules, Ism: Structure, Line: Profiles, Stars: Formation

Scientific paper

The NGC 1333 IRAS 4 region was observed in the HCN and HCO+ J=1-->0 lines using a single-dish telescope and in the 2.1 mm continuum and the H2CO JK-1K+1=212-->111 line using an interferometer. The single-dish maps show that there are at least two velocity components in emission: one at VLSR=6.7 km s-1 associated with the IRAS 4 core, and the other at ~8 km s-1 associated with a cloud extended from the SVS 13 complex. In addition, there is a foreground cold layer at ~8 km s-1 that causes absorption over most of the mapped area. The cloud structure suggests that the blue-skewed line profile of IRAS 4A/B may not be a sign of protostellar collapse. Examinations of both single-dish and interferometric maps suggest that the dip previously seen in the interferometric spectra toward IRAS 4A/B may be caused mostly by the large-scale foreground layer and partly by missing short-spacing flux. Absorption by an infalling envelope with an unusual velocity profile cannot be ruled out. The HCO+ map revealed other molecular cores, one associated with SK 1, and the other with SK 10/14. They are probable sites of star formation.

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