2017A&A...598A..14B


C.D.S. - SIMBAD4 rel 1.7 - 2020.07.11CEST18:16:38

2017A&A...598A..14B - Astronomy and Astrophysics, volume 598A, 14-14 (2017/2-1)

The shocked gas of the BHR71 outflow observed by Herschel: indirect evidence for an atomic jet.

BENEDETTINI M., GUSDORF A., NISINI B., LEFLOCH B., ANDERL S., BUSQUET G., CECCARELLI C., CODELLA C., LEURINI S. and PODIO L.

Abstract (from CDS):

Context.In the BHR71 region, two low-mass protostarsIRS1 andIRS2 drive two distinguishable outflows. They constitute an ideal laboratory to investigate both the effects of shock chemistry and the mechanisms that led to their formation.
Aims. We aim to define the global morphology of the warm gas component of the BHR71 outflow and at modelling its shocked component.
Methods. We present the first far infrared Herschel images of the BHR71 outflows system in the CO (14-13), H2O (221-110), H2O (212-101) and [OI] 145µm transitions, revealing the presence of several knots of warm, shocked gas associated with the fast outflowing gas.In two of these knots we performed a detailed study of the physical conditions by comparing a large set of transitions from several molecules to a grid of shock models.
Results. The Herschel lines ratios in the outflow knots are quite similar, showing that the excitation conditions of the fast moving gas do not change significantly within the first ∼0.068pc of the outflow, apart at the extremity of the southern blue-shifted lobe that is expanding outside the parental molecular cloud. Rotational diagram, spectral line profile and LVG analysis of the CO lines in knot A show the presence of two gas components: one extended, cold (T∼80K) and dense (n(H2)=3x105-4x106cm–3) and another compact (18''), warm (T=1700-2200K) with slightly lower density (n(H2)=2x104-6x104cm–3).In the two brightest knots (where we performed shock modelling) we found that H2 and CO are well fitted with non-stationary (young) shocks. These models, however, significantly underestimate the observed fluxes of [OI] and OH lines, but are not too far off those of H2O, calling for an additional, possibly dissociative, J-type shock component.
Conclusions. Our modelling indirectly suggests that an additional shock component exists, possibly a remnant of the primary jet. Direct, observational evidence for such a jet must be searched for.

Abstract Copyright: © ESO, 2017

Journal keyword(s): stars: formation - ISM: jets and outflows - ISM: individual objects: BHR71 - infrared: ISM

CDS comments: Table 2, fig.2 knots A-E not in SIMBAD.

Simbad objects: 9

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Number of rows : 9

N Identifier Otype ICRS (J2000)
RA
ICRS (J2000)
DEC
Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2020
#notes
1 HH 320 HH 12 01 32.7 -65 08 11           ~ 15 0
2 [B2001b] IRS 2 Y*O 12 01 34.0 -65 08 44           ~ 24 0
3 HH 321 HH 12 01 36.3 -65 09 34           ~ 12 0
4 BHR 71 MoC 12 01 36.810 -65 08 49.22           ~ 119 0
5 HH 54 HH 12 55 49.5 -76 56 08           ~ 118 0
6 LDN 1157 DNe 20 39 06.4 +68 02 13           ~ 484 0
7 [DE95] LDN 1157 B1 out 20 39 11 +68 01.3           ~ 180 0
8 LDN 1148 DNe 20 40 31.6 +67 21 45           ~ 59 0
9 NAME Cep E HII 23 03 12.779 +61 42 25.75           ~ 153 0

    Equat.    Gal    SGal    Ecl

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2020.07.11-18:16:38

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