Astronomy and Astrophysics, volume 595A, 76-76 (2016/11-1)
The small-scale HH34 IRS jet as seen by X-shooter.
NISINI B., GIANNINI T., ANTONIUCCI S., ALCALA J.M., BACCIOTTI F. and PODIO L.
Abstract (from CDS):
Context. Atomic jets are a common phenomenon among young stars, being intimately related to disk accretion. Most studies have been performed on jets from pre-main sequence stars. However, to date very little detailed information has been gathered on jets from young embedded low mass sources (the so-called classI stars), especially in the inner jet region.
Aims. We exploit a diagnostic analysis based on multiwave spectroscopic observations to infer kinematics and physical conditions of the inner region of the prototypical classI jet from HH34IRS.
Methods. We use a deep X-shooter spectrum covering the wavelength range 350-2300 nm at resolution between ∼8000 and ∼18 000 (i.e., ΔV∼17-27km/s), which allows us to detect lines in a wide range of excitation conditions (from Eup∼8000 to ∼31000cm–1 ) and to study their kinematics. Statistical equilibrium and ionization models are adopted to derive the jet main physical parameters.
Results. We separately derive the physical conditions for the extended high velocity jet (HVC, Vr~-100km/s) and for the low velocity and compact gas (LVC, Vr~-20-50km/s) located on-source. Close to the jet base (<200AU from source) the HVC gas is mostly neutral (xe<0.1) and very dense (nH>5x105cm–3). The LVC gas has the same density and AV as the HVC, but it is at least a factor of two colder.Iron abundance in the HVC is consistent with the solar value, while it is a factor of 3 subsolar in the LVC, suggesting an origin of the LVC gas from a dusty disk. From the derived total density we infer that the jet mass flux rate is >5x10–7M☉/yr. We find that the relationships between accretion luminosity and permitted line luminosity derived for T Tauri stars cannot be directly extended to classI sources embedded in reflection nebulae since the permitted lines are seen through scattered light. An accretion rate of ∼7x10–6M☉/yr is instead derived from an empirical relationship connecting Macc with L([OI])(HVC).
Conclusions. The classI HH34IRS jet at small scale shares many kinematical and physical properties with the jets from the most active classical T Tauri (CTT) stars. However, the HH34IRS jet is denser as a consequence of the larger mass ejection rate with respect to typical values in CTTs jets. These findings suggests that the acceleration and excitation mechanisms in collimated jets are not influenced by evolution and are similar in CTTs and in still embedded sources with high accretion rates.
© ESO, 2016
stars: formation - stars: protostars - ISM: jets and outflows - ISM: individual objects: HH34
Fig.1, Table 2 : Knots AN not in SIMBAD.
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