ISO Spectroscopy of the HH 7-11 Flow and its red-shifted Counterpart

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dc.creatorMolinari, S.
dc.creatorNoriega-Crespo, A.
dc.creatorCeccarelli, C.
dc.creatorNisini, B.
dc.creatorGiannini, T.
dc.creatorLorenzetti, D.
dc.creatorCaux, E.
dc.creatorLiseau, R.
dc.creatorSaraceno, P.
dc.creatorWhite, G. J.
dc.date2000-03-02
dc.date.accessioned2026-07-07T06:28:07Z
dc.date.available2026-07-07T06:28:07Z
dc.descriptionWe have used the two spectrometers on the Infrared Space Observatory to observe the HH 7-11 flow, its red-shifted counterpart, and the candidate exciting source SVS 13, in the star formation region NGC 1333. We detect atomic ([OI]63um and 145um, [SiII]34.8um, [CII]158um) and molecular (H_2, CO, H_2O) 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 non-dissociative (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 <40-50 km/s. Toward both lobes of the outflow we find pre-shock densities of n_0~10^4 cm-3 for both the J and C components, implying B_0~100uG. In the central region of the flow, close to the exciting source, the pre-shock density deduced for the C-shock component is n_0~10^5 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 due to 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 photo-ionised by BD +30 549, the dominant illuminating source of the NGC 1333 reflection nebula.
dc.description16 pages, Fig. 1 is in color, accepted by The Astrophysical Journal
dc.identifierhttps://arxiv.org/abs/astro-ph/0003031
dc.identifierhttp://arxiv.org/abs/astro-ph/0003031
dc.identifier.urihttp://salesiana.dossiersoluciones.com/handle/123456789/97622
dc.subjectAstrophysics
dc.titleISO Spectroscopy of the HH 7-11 Flow and its red-shifted Counterpart
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