SiO outflow signatures toward massive young stellar objects  with linearly distributed methanol masers

Buizer, James M. De; Redman, R. O.; Longmore, S.; Caswell, J. L.; Feldman, P. A.

doi:10.1051/0004-6361:200810907

Cited by 38 publications

(43 citation statements)

References 44 publications

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“…One can speculate that the mid-infrared photons, required for pumping the 6.7 GHz masers (Cragg et al 2002), could more easily penetrate into the dense HMC gas in proximity of the outflows, taking advantage of the cavities induced by the outflowing gas. The proposed association of the 6.7 GHz masers with outflows, based on the similarity of the 3D velocities of the methanol and water masers, agrees with the results by De Buizer (2003) and De Buizer et al (2009), which find that in most cases the methanol masers are elongated parallel to jets traced by the H 2 and SiO emissions, suggesting a physical association of the 6.7 GHz masers with the corresponding outflows.…”

Section: Methanol and Oh Maser Dynamics: Jet-driven Expansion Of The Hmcsupporting

confidence: 89%

A double-jet system in the G31.41 + 0.31 hot molecular core

Moscadelli

Cesaroni

et al. 2013

A&A

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Context. Many aspects of massive star ( > ∼ 10 M ) formation are still unclear. In particular, the outflow properties at close distance (100-1000 AU) from a massive young stellar object (MYSO) are not yet well established. Aims. This work presents a detailed study of the gas kinematics toward the hot molecular core (HMC) G31.41+0.31. Methods. To study the HMC 3D kinematics at milli-arcsecond angular resolution, we performed multi-epoch VLBI observations of the H 2 O 22 GHz and CH 3 OH 6.7 GHz masers, and single-epoch VLBI of the OH 1.6 GHz masers. Results. Water masers present a symmetric spatial distribution with respect to the HMC center, where two nearby (0. 2 apart), compact, VLA sources (labeled "A" and "B") are previously detected. The spatial distribution of a first group of water masers, named "J1", is well fit with an elliptical profile, and the maser proper motions mainly diverge from the ellipse center, with average speed of 36 km s −1 . These findings strongly suggest that the "J1" water maser group traces the heads of a young (dynamical time of 1.3 × 10 3 yr), powerful (momentum rate of 0.2 M yr −1 km s −1 ), collimated (semi-opening angle 10 • ) jet emerging from a MYSO located close (within ≈0. 15) to the VLA source "B". Most of the water features not belonging to "J1" present an elongated (≈2 in size), NE-SW oriented (PA ≈ 70 • ), S-shape distribution, which we denote with the label "J2". The elongated distribution of the "J2" group and the direction of motion, approximately parallel to the direction of elongation, of most "J2" water masers suggests the presence of another collimated outflow, emitted from a MYSO placed near the VLA source "A". The proper motions of the CH 3 OH 6.7 GHz masers, mostly diverging from the HMC center, also witness the expansion of the HMC gas driven by the "J1" and "J2" jets. The orientation (PA ≈ 70 • ) of the "J2" jet agrees well with that (PA = 68 • ) of the well-defined V LSR gradient across the HMC revealed by previous interferometric, thermal line observations. Furthermore, the "J2" jet is powerful enough to sustain the large momentum rate, 0.3 M yr −1 km s −1 , estimated from the interferometric, molecular line data in the assumption that the V LSR gradient represents a collimated outflow. These two facts lead us to favor the interpretation of the V LSR gradient across the G31.41+0.31 HMC in terms of a compact and collimated outflow.

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Section: Methanol and Oh Maser Dynamics: Jet-driven Expansion Of The Hmcsupporting

confidence: 89%

A double-jet system in the G31.41 + 0.31 hot molecular core

Moscadelli

Cesaroni

et al. 2013

A&A

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“…In Table 5 we list the luminosities, the depth of the 10 μm silicate absorption feature, whether or not any compact H II region is present, and whether or not any outflows have been detected, which can be useful for independently constraining disk geometry. As previously noted, however, in the case of AFGL 4176, no outflow components have been detected (De Buizer 2003;De Buizer et al 2009). For a broader discussion of these and other sources, we refer to the work by Grellmann et al (2011).…”

Section: Comparison With Other Mysossupporting

confidence: 59%

“…3, AFGL 4176 shows evidence for deviations from spherical symmetry only at the scales probed by our mid-infrared interferometric observations, which correspond to scales of roughly 20 to 200 mas. Furthermore, no outflow component has been revealed in searches by De Buizer (2003) and De Buizer et al (2009), nor in the HCO+ data presented in this work (Fig. 8).…”

Section: One-dimensional Radiative Transfer Modelingcontrasting

confidence: 38%

“…Using both the velocity curve of Brand & Blitz (1993) with updated parameters from Levine et al (2008), and the velocity curve of Reid et al (2009), we find that the combination of the source's LSR velocity of ∼−51 km s −1 (e.g. Fontani et al 2005;De Buizer et al 2009) and galactic coordinates are forbidden 1 . Consequently, a kinematic distance cannot be determined for AFGL 4176 using these rotation curves.…”

Section: Introductionmentioning

confidence: 96%

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On the massive young stellar object AFGL 4176

Boley

Linz

Boekel

et al. 2012

A&A

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Deeply embedded and at distances of several kiloparsecs, massive young stellar objects (MYSOs) present numerous challenges for observation and study. In this work, we present spatially-resolved observations of one MYSO, AFGL 4176, together with survey and literature data, ranging from interferometric observations with VLTI/MIDI in the mid-infrared, to single-dish Herschel measurements in the far-infrared, and sub-millimeter data from APEX. We consider this spatially-resolved, multi-wavelength data set in terms of both radiative transfer and geometric models. We find that the observations are well described by one-dimensional models overall, but there are also substantial deviations from spherical symmetry at scales of tens to hundreds of astronomical units, which are revealed by the mid-infrared interferometric measurements. We use a multiple-component, geometric modeling approach to explain the mid-infrared emission on scales of tens to hundreds of astronomical units, and find the MIDI measurements are well described by a model consisting of a one-dimensional Gaussian halo and an inclined (θ = 60 • ) circumstellar disk extending out to several hundred astronomical units along a position angle of 160 • . Finally, we compare our results both with previous models of this source, and with those of other MYSOs, and discuss the present situation with mid-infrared interferometric observations of massive stars.

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“…Many interferometric observations show that thermal and maser SiO emission depicted the low-velocity outflow centered on source I in Orion KL (Blake et al 1996;Wright et al 1996;Beuther et al 2005;Plambeck et al 2009;Goddi et al 2009;Zapata et al 2009). In addition, SiO traces many other molecular outflows in different sources (Jiménez-Serra et al 2004;Gibb et al 2007;De Buizer et al 2009;Zapata et al 2009). Mookerjea et al (2007) have not found emission from SiO at the position of the hot molecular core in G34.26+0.15.…”

Section: Discussionmentioning

confidence: 99%

A line-confusion limited millimeter survey of Orion KL

Tercero

Vincent

Cernicharo

et al. 2011

A&A

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Aims. We present a study of the silicon-bearing species detected in a line-confusion limited survey towards Orion KL performed with the IRAM 30-m telescope. The analysis of the line survey is organized by families of molecules. Our aim is to derive physical and chemical conditions for each family taking all observed lines into account from all isotopologs of each species. The large number of transitions in different vibrationally excited states covered by our data, which range from 80 to 280 GHz, let us provide reliable source-average column densities (hence, isotopolog abundances and vibrational temperatures) for the detected molecules. In addition, we provide a wide study of the physical properties of the source based on the different spectral components found in the emission lines. Methods. We modeled the lines of the detected molecules using a radiative transfer code, which permit us to choose between large velocity gradient (LVG) and local thermodynamic equilibrium (LTE) approximations depending on the physical conditions of the gas. We used appropriate collisional rates for the LVG calculations. To qualitatively investigate the origin of the SiS and SiO emissions in Orion KL we ran a grid of chemical models.Results. For the v = 1 state of SiO, we detected the J = 2−1 line and, for the first time in this source, emission in the J = 4−3 transition, both of them showing a strong masering effect. For SiO v = 0, we detected 28 SiO, 29 SiO, and 30 SiO; in addition, we have mapped the J = 5−4 SiO line. For SiS, we have detected the main species, 29 SiS, and SiS v = 1. Unlikely other species detected in Orion KL (IRc2), the emission peak of SiS appears at a velocity of 15.5 km s −1 . A study of the 5−4 SiO line around IRc2 shows this feature as an extended component that probably arises from the interaction of the outflow with the ambient cloud. We derive an SiO/SiS column density ratio of 13 in the plateau component, four times lower than the cosmic O/S ratio 48. In addition, we provide upper limits to the column density of several non-detected silicon-bearing species. The results of our chemical models show that while it is possible to reproduce SiO in the gas phase (as well as on the grains), SiS is a product of surface reactions, most likely involving direct reactions of sulfur with silicon.

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SiO outflow signatures toward massive young stellar objects with linearly distributed methanol masers

Cited by 38 publications

References 44 publications

A double-jet system in the G31.41 + 0.31 hot molecular core

A double-jet system in the G31.41 + 0.31 hot molecular core

On the massive young stellar object AFGL 4176

A line-confusion limited millimeter survey of Orion KL

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