Volume 449, Number 3, April III 2006
|Page(s)||1089 - 1100|
|Section||Interstellar and circumstellar matter|
|Published online||24 March 2006|
An observational survey of molecular emission ahead of Herbig-Haro objects
Department of Physics and Astronomy, UCL, Gower St., London, WC1E 6BT, UK e-mail: firstname.lastname@example.org
2 Institut de Ciències de l'Espai (CSIC), Gran Capità 2, 08034 Barcelona, Catalunya, Spain
3 Institut d'Estudis Espacial de Catalunya, Spain
4 School of Physics, University of Exeter, Stocker Road, Exeter, EX4 4QL, UK
Accepted: 16 December 2005
Context.A molecular survey recently performed ahead of HH 2 supports the idea that the observed molecular enhancement is due to UV radiation from the HH object.Aims.The aim of the present work is to determine whether all HH objects with enhanced HCO+ emission ahead of them also exhibit the same enhanced chemistry as HH 2. We thus observed several molecular lines at several positions ahead of five Herbig-Haro objects where enhanced HCO+ emission was previously observed.Methods.We mapped the five Herbig-Haro objects using the IRAM-30 m. For each position we searched for more than one molecular species, and where possible for more than one transition per species. We then estimated the averaged beam column densities for all species observed and also performed LVG analyses to constrain the physical properties of the gas.Results.The chemically richest quiescent gas is found ahead of the HH 7–11 complex, in particular at the HH 7–11 A position. In some regions we also detected a high velocity gas component. We find that the gas densities are always higher than those typical of a molecular cloud while the derived temperatures are always quite low, ranging from 10 to 25 K. The emission of most species seems to be enhanced with respect to that of a typical dense clump, probably due to the exposure to a high UV radiation from the HH objects. Chemical differentiation among the positions is also observed. We attempt a very simple chemical analysis to explain such differentiation.
© ESO, 2006
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