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dc.contributor.authorMoro-Martín, Amaya-
dc.contributor.authorNoriega-Crespo, A.-
dc.contributor.authorCesarsky, D.-
dc.contributor.authorCabrit, S.-
dc.contributor.authorCernicharo, José-
dc.contributor.authorLefloch, Bertrand-
dc.date.accessioned2008-01-02T13:19:10Z-
dc.date.available2008-01-02T13:19:10Z-
dc.date.issued2003-05-07-
dc.identifier.citationarXiv:astro-ph/0305108v1en_US
dc.identifier.citationThe Astrophysical Journal Letters, 590:L41–L44, 2003 June 10en_US
dc.identifier.issn1538-4357-
dc.identifier.urihttp://hdl.handle.net/10261/2646-
dc.description.abstractWe report on spectro-imaging observations of the Herbig-Haro 2 outflow with the ISOCAM camera onboard the Infrared Space Observatory (ISO). The [Ne II}] 12.81 microns and [Ne III]15.55 microns lines are detected only towards the jet working surface (HH 2H), consistent with the high excitation of this knot in the optical range, while H2 pure rotational emission is found all over the shocked region HH 2. The low energy transition S(2) traces warm gas (T approx. 400K) peaked towards knots E-F and extended ejecta (T approx. 250-380) with masses of a few 0.001 solar mass in the high-velocity CO outflow extending between the powering source and HH 2. Such emission could arise from low-velocity C-type shocks (v= 10-15 km/s). The higher transitions S(3)-S(7) trace the emission of hot shocked gas (T= 1000-1400K) from individual optical knots in the HH 2 region. The ortho to para (OTP) ratio exhibits large spatial variations between 1.2 (E) and 2.5 (H), well below its value at LTE. The emission of the S(3)-S(7) lines is well accounted for by planar C-shock models with a typical velocity V= 20-30 km/s propagating into a medium of density 10^4-10^5 cm-3 with an initial OTP ratio close to 1 in the pre-shock gas. In the leading edge of the jet, where the geometry of the emission allows a simple modelling, a good agreement is found with velocities derived from the optical proper motions measured in the ionized gas.en_US
dc.format.extent376326 bytes-
dc.format.mimetypeapplication/pdf-
dc.language.isoengen_US
dc.publisherAmerican Astronomical Societyen_US
dc.relation.isversionofPreprint-
dc.rightsopenAccessen_US
dc.subjectStars: formationen_US
dc.subjectISM: Herbig‐Haro objectsen_US
dc.subjectISM: individual (HH 1–2)en_US
dc.subjectISM: jets and outflowsen_US
dc.subjectISM: moleculesen_US
dc.titleWarm Molecular Hydrogen and Ionized Neon in the HH2 Outflowen_US
dc.typepreprinten_US
dc.identifier.doi10.1086/376673-
dc.description.peerreviewedPeer revieweden_US
dc.type.coarhttp://purl.org/coar/resource_type/c_816bes_ES
item.openairetypepreprint-
item.cerifentitytypePublications-
item.languageiso639-1en-
item.grantfulltextopen-
item.openairecristypehttp://purl.org/coar/resource_type/c_816b-
item.fulltextWith Fulltext-
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