Multiwavelength Study of the Powering Sources of the Double H<sub>2</sub>Bipolar Jet in L1634

Beltrán, M. T.; Estalella, R.; Ho, Paul T. P.; Calvet, Nuria; Anglada, Guillem; Sepúlveda, Inma

doi:10.1086/324683

Cited by 17 publications

(39 citation statements)

References 42 publications

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“…L 1157-mm region may thus be indicative of physical differences between the properties of the material toward the embedded source and those of the more extended region. This effect was already observed in other young embedded sources (Visser et al 1998;Johnstone & Bally 1999;Smith et al 2000;Beltrán et al 2002).…”

Section: Spectral Index Mapsupporting

confidence: 72%

L1157: Interaction of the molecular outflow with the Class 0 environment

Beltrán

Gueth

Guilloteau

et al. 2004

A&A

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Abstract. We present high angular resolution interferometric observations [ ] of the dust continuum at 2.7 and 1.3 mm, and of the HC 3 N (J = 12 → 11) and C 18 O (J = 2 → 1) emission around L1157-mm, a Class 0 object that drives a spectacular molecular outflow. The millimeter dust emission is clearly resolved into two components, a flattened compact source of ∼450 × 250 AU at 1.3 mm, and mass ∼0.1 M , plus an extended envelope of ∼3000 AU at 1.3 mm, and mass ∼1.1 M . The millimeter spectral index varies throughout the region, with the lower value found toward the compact protostar, possibly indicating grain growth in the denser regions. A strong interaction between the molecular outflow and the close protostellar environment is taking place and affects the structure of the innermost parts of the envelope. This is shown by the spatial coincidence between the molecular outflow and the dust (1.3 mm continuum) and HC 3 N emission: both tracers show structures associated to the edges of the outflow lobes. Basically, the global picture sketched for the Class 0 object L1157-mm by Gueth et al. (1997) is supported. We find possible evidence of infall, but we do not detect any velocity gradient indicative of a rotating circumstellar disk.

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Section: Spectral Index Mapsupporting

confidence: 72%

L1157: Interaction of the molecular outflow with the Class 0 environment

Beltrán

Gueth

Guilloteau

et al. 2004

A&A

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“…This can be compared to the model-dependent infall rate derived by Beltrán et al (2002) ofṀ in = 2.6−8.0 × 10 −5 M yr −1 which implies that well under 10% of the inflowing mass is ejected.…”

Section: Hh 240cmentioning

confidence: 93%

“…The outflow is driven from IRAS 05173-0555 (Davis et al 1997), a protostar with an estimated mass infall rate of 2−8 × 10 −5 M yr −1 (Beltrán et al 2002), bolometric luminosity Send offprint requests to: B. O'Connell, e-mail: boc@arm.ac.uk of 17 L (Reipurth et al 1993) and bolometric temperature of 77 K (Mardones et al 1997), classifying it as undergoing a transition phase from Class 0 to Class I. In addition to this east-west outflow there is a weaker northwest-southeast outflow driven from IRS 7, 40 to the east (Hodapp & Ladd 1995;Davis et al 1997).…”

Section: Introductionmentioning

confidence: 99%

A near-infrared study of the bow shocks within the L1634 protostellar outflow

O’Connell

Smith

Davis

et al. 2004

A&A

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Abstract. The L1634 bright-rimmed globule contains an intriguing arrangement of shock structures: two series of aligned molecular shock waves associated with the Herbig-Haro flows HH 240 and HH 241. We present near-infrared spectroscopy and narrow-band imaging in the (1, 0) S(1) and (2, 1) S(1) emission lines of molecular hydrogen. These observations yield the spatial distributions of both the molecular excitation and velocity, which demonstrate distinct properties for the individual bow shocks. Bow shock models are applied, varying the shock physics, geometry, speed, density and magnetic field properties to fit two prominent bow shocks. The models predict that both bows move at 60 • to the plane of the sky. High magnetic fields and low molecular fractions are implied. The advancing compact bow HH 240C is interpreted as a J-type bow (frozen-in magnetic field) with the flanks in transition to C-type (field diffusion). It is a paraboloidal bow of speed ∼42 km s −1 entering a medium of quite high density (2 × 10 4 cm −3 ). The following bow HH 240A is faster despite a lower excitation, moving through a lower density medium. We find a C-type bow shock model to fit all the data for HH 240A. The favoured bow models are then tested comprehensively against published H 2 emission line fluxes and CO spectroscopy. We conclude that, while the CO emission originates from cloud gas directly set in motion, the H 2 emission is generated from shocks sweeping through an outflow. Also considering optical data, we arrive at a global outflow model involving episodic slow-precessing twin jets.

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“…The other bipolar jet only has two knotty bow shocks (knots 9 and 4; Hodapp & Ladd 1995), and the near-infrared source found near the center, IRS 7 (Davis et al 1997), is probably the powering source of this second outflow. The continuum emission towards the core of L1634 has been mapped at centimeter, millimeter, and submillimeter wavelengths (Reipurth et al 1993;Chini et al 1997;Beltrán et al 2002;Morgan et al 2008). Beltrán et al (2002) model the circumstellar dust emission around IRAS 05173−0555, and conclude that the infrared source traces an embedded young stellar object still in its infall phase.…”

Section: Introductionmentioning

confidence: 99%

“…The synthesized beam is drawn in the bottom left corner of the bottom left panel. The crosses mark the submillimeter continuum positions of IRAS 05173−0555 (right cross) and IRS 7 (left cross) (Beltrán et al 2002). Froebrich (2005), the source would be better classify as a bordeline Class 0/I object, or maybe a Class I object.…”

Section: Introductionmentioning

confidence: 99%

Dissection of the protostellar envelope surrounding IRAS 05173-0555 in L1634

Beltrán¹,

Wiseman

et al. 2008

A&A

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Context. The youngest protostars that power energetic outflows are surrounded by infalling and rotating envelopes that contain most of the mass of the system. Aims. We study the properties and kinematics of the protostellar envelope surrounding the embedded source IRAS 05173−0555 in L1634. Methods. We carried out VLA ammonia observations at 1.3 cm with the VLA in the D configuration to map the gas towards the core of L1634. Results. The NH 3 emission towards IRAS 05173−0555 is resolved and shows two components that are clearly distinguishable morphologically: a cross-like structure, roughly elongated in the direction of the HH 240/241 outflow and associated with IRAS 05173−0555, plus an arc-like stream elongated towards the north. The properties and kinematics of the gas suggest that the origin of the cross-like morphology could be the interaction between the outflow and the envelope. A more compact and flattened structure, which could be undergoing rotation about the axis of the outflow, has been detected towards the center of the cross-like envelope. The northern stream, which has properties and velocity that are different from those of the cross-like envelope, is likely part of the original cloud envelope, and could be a quiescent core that may never form stars, or instead be in a prestellar phase.

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Multiwavelength Study of the Powering Sources of the Double H₂Bipolar Jet in L1634

Cited by 17 publications

References 42 publications

L1157: Interaction of the molecular outflow with the Class 0 environment

L1157: Interaction of the molecular outflow with the Class 0 environment

A near-infrared study of the bow shocks within the L1634 protostellar outflow

Dissection of the protostellar envelope surrounding IRAS 05173-0555 in L1634

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Multiwavelength Study of the Powering Sources of the Double H2Bipolar Jet in L1634

Cited by 17 publications

References 42 publications

L1157: Interaction of the molecular outflow with the Class 0 environment

L1157: Interaction of the molecular outflow with the Class 0 environment

A near-infrared study of the bow shocks within the L1634 protostellar outflow

Dissection of the protostellar envelope surrounding IRAS 05173-0555 in L1634

Contact Info

Product

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Multiwavelength Study of the Powering Sources of the Double H₂Bipolar Jet in L1634