Astronomy and Astrophysics – Astronomy
Scientific paper
Aug 2000
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2000apj...538..698m&link_type=abstract
The Astrophysical Journal, Volume 538, Issue 2, pp. 698-709.
Astronomy and Astrophysics
Astronomy
30
Ism: Herbig-Haro Objects, Ism: Individual (Hh 7-11), Ism: Lines And Bands, Ism: Molecules, Stars: Formation
Scientific paper
We have used the two spectrometers on the Infrared Space Observatory to observe the HH 7-11 flow, its redshifted counterpart, and the candidate exciting source SVS 13 in the star formation region NGC 1333. We detect atomic ([O I] 63 μm, [O I] 145 μm, [Si II] 34.8 μm, [C II] 158 μm) and molecular (H2, CO, H2O) lines at various positions along the bipolar flow. Most of the observed lines can be explained in terms of shock-excited emission. In particular, our analysis shows that dissociative (J-type) and nondissociative (C-type) shocks are simultaneously present everywhere along both lobes of the flow. We confirm the low-excitation nature of the Herbig-Haro nebulosities, with shock velocities vs<~40-50 km s-1. Toward both lobes of the outflow, we find preshock densities of n0~104 cm-3 for both the J and C components, implying B0~100 μG for B0~n0.50. In the central region of the flow, close to the exciting source, the preshock density deduced for the C-shock component is n0~105 cm-3, suggesting a magnetic field ~3 times stronger. We propose that the deficiency of gas-phase water in the post-C-shock regions is caused by freezing onto warm grains processed through the J-shock front and traveling along the magnetic field lines. The total observed cooling from the dissociative shock components is consistent with the power lost by a slow molecular outflow accelerated by a fast neutral HI wind. Finally, the skin of the cloud seen in projection toward the flow appears to be weakly photoionized by BD +30°549, the dominant illuminating source of the NGC 1333 reflection nebula. Based on observations with the Infrared Space Observatory (ISO), an ESA project with instruments funded by ESA Member States (especially the PI countries: France, Germany, the Netherlands, and the United Kingdom) with the participation of ISAS and NASA.
Caux Emmanuel
Ceccarelli Cecilia
Giannini Teresa
Liseau Rene
Lorenzetti Dario
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