Multiple outflows from the luminous YSO IRAS 07422-2001

Varricatt, W. P.

doi:10.1051/0004-6361/201118193

Cited by 2 publications

(6 citation statements)

References 33 publications

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“…3, bottomleft panel), the masers in the subset OG show an elongated spatial distribution, oriented at close angle with the direction of collimation of the maser PMs. These are the kinematic properties expected for jets, and, for G176.52+0.20 and G236.82+1.98, this interpretation is supported by the observation on scales of 10 4 au of a collimated molecular flow (Fontani et al 2009) and an elongated chain of H 2 2.2 µm knots (Varricatt 2012), respectively, about parallel to the maser jet (see Fig. 3).…”

Section: Subgroup N-g: Linear V Lsr Gradientssupporting

confidence: 64%

“…3 and B.5 (lower panels) and comparing the values of MA MD and PD PM of the maser subset OG with the value of MA MD of the corresponding maser subset IG in Table A.1, it is also evident that, in each of the three sources, the V LSR gradient traced by the subset IG is about perpendicular (within 10 • -20 • ) to the axis of the jet identified by the subset OG. The finding of a V LSR gradient directed perpendicular to a jet hints at a rotating disk seen almost edge-on, and, for G236.82+1.98, this interpretation is corroborated by the detection of an extinction lane in the J-band UKIRT image of Varricatt (2012) about parallel to the maser V LSR gradient (see Fig. 3, bottom-right panel).…”

Section: Subgroup N-g: Linear V Lsr Gradientsmentioning

confidence: 72%

“…13 and 14 give the PA of the major-axis of the circumstellar disk and the PA of the sky-projected jet axis, if a disk and/or a jet have been detected towards the YSO through high angular-resolution observations in thermal (continuum or line) emission; Col. 15 reports the reference index of the literature observations. (a) The elongated chain of H 2 2.2 µm knots (PA ≈ 53 • ) and the extinction lane in the J-band image (PA ≈127 • ) are associated with the bright NIR source #1 of Varricatt (2012), which could correspond with our POETS target G236.82+1.98 within the uncertainties in the astrometric calibration of the UKIRT Wide Field Camera NIR images. (b) In this target, the water maser emission comes from two nearby YSOs, resolved through subarcsecond VLA observations, named VLA 3A and VLA 3B.…”

Section: Discussionmentioning

confidence: 98%

“…The V LSR gradient traced by the water masers is indicated by a dashed line, using colors to denote the red-and blue-shifted side of the gradient. The black dotted arrows labeled LJ (left) and the black dotted line labeled LD (right) denote the orientations of the elongated chain of H 2 2.2 µm knots and the extinction lane in the J-band image, respectively, observed in proximity of G236.82+1.98 by Varricatt (2012) maser PMs, PD PM , in two steps. First, we have identified the 60 • range in PA that includes the largest fraction of measured PMs.…”

Section: Distribution Of Proper Motionsmentioning

confidence: 99%

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Protostellar Outflows at the EarliesT Stages (POETS)

Moscadelli

Sanna

Goddi

et al. 2019

A&A

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Context. Although recent observations and theoretical simulations have pointed out that accretion disks and jets can be essential for the formation of stars with a mass of up to at least 20 M⊙, the processes regulating mass accretion and ejection are still uncertain. Aims. The goal of the Protostellar Outflows at the EarliesT Stages (POETS) survey is to image the disk-outflow interface on scales of 10–100 au in a statistically significant sample (36) of luminous young stellar objects (YSO), targeting both the molecular and ionized components of the outflows. Methods. The outflow kinematics is studied at milliarcsecond scales through very long baseline interferometry (VLBI) observations of the 22 GHz water masers, which are ideal test particles to measure the three-dimensional (3D) motion of shocks owing to the interaction of winds and jets with ambient gas. We employed the Jansky Very Large Array (JVLA) at 6, 13, and 22 GHz in the A- and B-Array configurations to determine the spatial structure and the spectral index of the radio continuum emission, and address its nature. Results. In about half of the targets, the water masers observed at separation ≤1000 au from the YSOs trace either or both of these kinematic structures: (1) a spatially elongated distribution oriented at close angle with the direction of collimation of the maser proper motions (PM), and (2) a linear local standard of rest (LSR) velocity (VLSR) gradient across the YSO position. The kinematic structure (1) is readily interpreted in terms of a protostellar jet, as confirmed in some targets via the comparison with independent observations of the YSO jets, in thermal (continuum and line) emissions, reported in the literature. The kinematic structure (2) is interpreted in terms of a disk-wind (DW) seen almost edge-on on the basis of several pieces of evidence: first, it is invariably directed perpendicular to the YSO jet; second, it agrees in orientation and polarity with the VLSR gradient in thermal emissions (when reported in the literature) identifying the YSO disk at scales of ≤1000 au; third, the PMs of the masers delineating the VLSR gradients hint at flow motions at a speed of 10–20 km s−1 directed at large angles with the disk midplane. In the remaining targets, the maser PMs are not collimated but rather tend to align along two almost perpendicular directions. To explain this peculiar PM distribution, and in light of the observational bias strongly favoring masers moving close to the plane of sky, we propose that, in these sources, the maser emission could originate in DW-jet systems slightly inclined (≤30°) with respect to edge-on. Magneto-centrifugally driven DWs could in general account for the observed velocity patterns of water masers.

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Section: Subgroup N-g: Linear V Lsr Gradientssupporting

confidence: 64%

Section: Subgroup N-g: Linear V Lsr Gradientsmentioning

confidence: 72%

Section: Discussionmentioning

confidence: 98%

Section: Distribution Of Proper Motionsmentioning

confidence: 99%

See 2 more Smart Citations

Protostellar Outflows at the EarliesT Stages (POETS)

Moscadelli

Sanna

Goddi

et al. 2019

A&A

View full text Add to dashboard Cite

show abstract

“…The V LSR gradient traced by the water masers is indicated by a dashed line, using colors to denote the red-and blue-shifted side of the gradient. The black dotted arrows labeled LJ (left) and the black dotted line labeled LD (right) denote the orientations of the elongated chain of H 2 2.2 µm knots and the extinction lane in the J-band image, respectively, observed in proximity of G236.82+1.98 by Varricatt (2012), using the Wide Field Camera mounted on the 3.8 m UKIRT.…”

Section: Subgroup N-g: Linear V Lsr Gradientsmentioning

confidence: 99%

Protostellar Outflows at the EarliesT Stages (POETS). III. H2O masers tracing disk-winds and jets near luminous YSOs

Moscadelli,

Sanna,

Goddi

et al. 2019

Preprint

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Context. Although recent observations and theoretical simulations have pointed out that accretion disks and jets can be essential for the formation of stars with a mass of up to at least 20 M ⊙ , the processes regulating mass accretion and ejection are still uncertain. Aims. The goal of the Protostellar Outflows at the EarliesT Stages (POETS) survey is to image the disk-outflow interface on scales of 10-100 au in a statistically significant sample (36) of luminous young stellar objects (YSO), targeting both the molecular and ionized components of the outflows. Methods. The outflow kinematics is studied at milliarcsecond scales through very long baseline interferometry (VLBI) observations of the 22 GHz water masers, which are ideal test particles to measure the three-dimensional (3D) motion of shocks owing to the interaction of winds and jets with ambient gas. We employed the Jansky Very Large Array (JVLA) at 6, 13, and 22 GHz in the Aand B-Array configurations to determine the spatial structure and the spectral index of the radio continuum emission, and address its nature.Results. In about half of the targets, the water masers observed at separation ≤1000 au from the YSOs trace either or both of these kinematic structures: 1) a spatially elongated distribution oriented at close angle with the direction of collimation of the maser proper motions (PM), and 2) a linear local standard of rest (LSR) velocity (V LSR ) gradient across the YSO position. The kinematic structure (1) is readily interpreted in terms of a protostellar jet, as confirmed in some targets via the comparison with independent observations of the YSO jets, in thermal (continuum and line) emissions, reported in the literature. The kinematic structure (2) is interpreted in terms of a disk-wind (DW) seen almost edge-on on the basis of several pieces of evidence: first, it is invariably directed perpendicular to the YSO jet; second, it agrees in orientation and polarity with the V LSR gradient in thermal emissions (when reported in the literature) identifying the YSO disk at scales of ≤1000 au; third, the PMs of the masers delineating the V LSR gradients hint at flow motions at a speed of 10-20 km s −1 directed at large angles with the disk midplane. In the remaining targets, the maser PMs are not collimated but rather tend to align along two almost perpendicular directions. To explain this peculiar PM distribution, and in light of the observational bias strongly favoring masers moving close to the plane of sky, we propose that, in these sources, the maser emission could originate in DW-jet systems slightly inclined (≤30 • ) with respect to edge-on. Magneto-centrifugally driven DWs could in general account for the observed velocity patterns of water masers.

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Multiple outflows from the luminous YSO IRAS 07422-2001

Cited by 2 publications

References 33 publications

Protostellar Outflows at the EarliesT Stages (POETS)

Protostellar Outflows at the EarliesT Stages (POETS)

Protostellar Outflows at the EarliesT Stages (POETS). III. H2O masers tracing disk-winds and jets near luminous YSOs

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