A candidate circumbinary Keplerian disk in G35.20–0.74 N: A study with ALMA

Sánchez-Monge, Á.; Cesaroni, R.; Beltrán, M. T.; Kumar, M. S. N.; Stanke, T.; Zinnecker, H.; Etoka, S.; Galli, Daniele; Hummel, C. A.; Moscadelli, L.; Preibisch, Thomas; Ratzka, Thorsten; Tak, van der Floris; Vig, S.; Walmsley, C. M.; Wang, K. S

doi:10.1051/0004-6361/201321134

Cited by 106 publications

(148 citation statements)

References 28 publications

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“…13) strongly favors the rotation scenario, because this is exactly what is expected in the case of a disk rotating about the axis of the associated outflow. This scenario closely resembles the one for core B in the 3 × 10 4 L high-mass star-forming region G35.20−0.74N (see Sánchez-Monge et al 2013), which is interpreted as a Keplerian disk rotating about the axis of a bipolar IR nebula. Finally, this velocity gradient might also be mimicked by two distinct cores with different V LSR that are too close to be resolved by our observations.…”

Section: Velocity Gradients In Core Asupporting

confidence: 68%

“…Contour levels, which start at 3σ, are a) 0.2 to 2.6 by 0. For IRAS 20126+4104 and G35.20−0.74N, the cores turn out to be Keplerian disks rotating about B-type (proto)stars Sánchez-Monge et al 2013). As discussed next, this could also be the case for core A in G35.03.…”

Section: Temperature and Mass Estimatesmentioning

confidence: 86%

“…The first results for G35.20−0.74N have revealed velocity gradients consistent with an almost edge-on Keplerian disk (Sánchez-Monge et al 2013).…”

Section: Introductionmentioning

confidence: 93%

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Filamentary structure and Keplerian rotation in the high-mass star-forming region G35.03+0.35 imaged with ALMA

Beltrán

Sánchez-Monge

Cesaroni

et al. 2014

A&A

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Context. Theoretical scenarios propose that high-mass stars are formed by disk-mediated accretion. Aims. To test the theoretical predictions on the formation of massive stars, we wish to make a thorough study at high-angular resolution of the structure and kinematics of the dust and gas emission toward the high-mass star-forming region G35.03+0.35, which harbors a disk candidate around a B-type (proto)star. Methods. We carried out ALMA Cycle 0 observations at 870 μm of dust of typical high-density, molecular outflow, and cloud tracers with resolutions of <0. 5. Complementary Subaru COMICS 25 μm observations were carried out to trace the mid-infrared emission toward this star-forming region. Results. The submillimeter continuum emission has revealed a filamentary structure fragmented into six cores, called A-F. The filament could be in quasi-equilibrium taking into account that the mass per unit length of the filament, 200-375 M /pc, is similar to the critical mass of a thermally and turbulently supported infinite cylinder, ∼335 M /pc. The cores, which are on average separated by ∼0.02 pc, have deconvolved sizes of 1300-3400 AU, temperatures of 35-240 K, H 2 densities >10 7 cm −3 , and masses in the range 1-5 M , and they are subcritical. Core A, which is associated with a hypercompact Hii region and could be the driving source of the molecular outflow observed in the region, is the most chemically rich source in G35.03+0.35 with strong emission of typical hot core tracers such as CH 3 CN. Tracers of high density and excitation show a clear velocity gradient along the major axis of the core, which is consistent with a disk rotating about the axis of the associated outflow. The PV plots along the SE-NW direction of the velocity gradient show clear signatures of Keplerian rotation, although infall could also be present, and they are consistent with the pattern of an edge-on Keplerian disk rotating about a star with a mass in the range 5-13 M . The high t ff /t rot ratio for core A suggests that the structure rotates fast and that the accreting material has time to settle into a centrifugally supported disk. Conclusions. G35.03+0.35 is one of the most convincing examples of Keplerian disks rotating about high-mass (proto)stars. This supports theoretical scenarios according to which high-mass stars, at least B-type stars, would form through disk-mediated accretion.

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Section: Velocity Gradients In Core Asupporting

confidence: 68%

Section: Temperature and Mass Estimatesmentioning

confidence: 86%

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Filamentary structure and Keplerian rotation in the high-mass star-forming region G35.03+0.35 imaged with ALMA

Beltrán

Sánchez-Monge

Cesaroni

et al. 2014

A&A

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“…Results on G35.03+0.35 are presented in a parallel paper by Beltrán et al (2014), while first results on G35.20−0.74 N have been already published in Sánchez-Monge et al (2013b). In this work, we present the ALMA results on G35.20−0.74 N in a more extensive and detailed way.…”

Section: Introductionmentioning

confidence: 76%

A necklace of dense cores in the high-mass star forming region G35.20−0.74 N: ALMA observations

Sánchez-Monge

Beltrán

Cesaroni

et al. 2014

A&A

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Context. The formation process of high-mass stars (with masses >8 M ) is still poorly understood, and represents a challenge from both the theoretical and observational points of view. The advent of the Atacama Large Millimeter Array (ALMA) is expected to provide observational evidence to better constrain the theoretical scenarios. Aims. The present study aims at characterizing the high-mass star forming region G35.20−0.74 N, which is found associated with at least one massive outflow and contains multiple dense cores, one of them recently found associated with a Keplerian rotating disk. Methods. We used the radio-interferometer ALMA to observe the G35.20−0.74 N region in the submillimeter continuum and line emission at 350 GHz. The observed frequency range covers tracers of dense gas (e.g., H 13 CO + , C 17 O), molecular outflows (e.g., SiO), and hot cores (e.g., CH 3 CN, CH 3 OH). These observations were complemented with infrared and centimeter data. Results. The ALMA 870 μm continuum emission map reveals an elongated dust structure (∼0.15 pc long and ∼0.013 pc wide; full width at half maximum) perpendicular to the large-scale molecular outflow detected in the region, and fragmented into a number of cores with masses ∼1-10 M and sizes ∼1600 AU (spatial resolution ∼960 AU). The cores appear regularly spaced with a separation of ∼0.023 pc. The emission of dense gas tracers such as H 13 CO + or C 17 O is extended and coincident with the dust elongated structure. The three strongest dust cores show emission of complex organic molecules characteristic of hot cores, with temperatures around 200 K, and relative abundances 0.2-2 × 10 −8 for CH 3 CN and 0.6-5 × 10 −6 for CH 3 OH. The two cores with highest mass (cores A and B) show coherent velocity fields, with gradients almost aligned with the dust elongated structure. Those velocity gradients are consistent with Keplerian disks rotating about central masses of 4-18 M . Perpendicular to the velocity gradients we have identified a large-scale precessing jet/outflow associated with core B, and hints of an east-west jet/outflow associated with core A. Conclusions. The elongated dust structure in G35.20−0.74 N is fragmented into a number of dense cores that may form high-mass stars. Based on the velocity field of the dense gas, the orientation of the magnetic field, and the regularly spaced fragmentation, we interpret this elongated structure as the densest part of a 1D filament fragmenting and forming high-mass stars.

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“…Outflows are frequently detected in high-mass star forming regions, but it is thought that high-mass star formation is not merely a scaled-up version of the low-mass star formation process characterized by larger outflow parameters (e. g., Wu et al 2004), poor collimation around massive young stars (e. g., Shepherd & Churchwell 1996;Zhang et al 2005) and higher accretion rates (see review by Zinnecker & Yorke 2007). Additionally, disks in high-mass young stellar objects are still elusive -only a few of them have been detected (Zhang ⋆ E-mail: slqin@bao.ac.cn Shepherd, Claussen & Kurtz 2001;Patel et al 2005;Jiang et al 2005;Sánchez-Monge et al 2013a -probably due to their short lifetimes, the necessity of achieving high angular resolution (not available in the observations prior to ALMA) and source confusion in dense clusters. Therefore, the study and characterization of the outflow and infall processes involved in the formation of high-mass stars need to be understood in more detail.…”

Section: Introductionmentioning

confidence: 99%

SMA observations of the W3(OH) complex: Dynamical differentiation between W3(H₂O) and W3(OH)

Qin¹,

Schilke²,

Wu³

et al. 2015

Mon. Not. R. Astron. Soc.

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We present Submillimeter Array (SMA) observations of the HCN (3-2) and HCO + (3-2) molecular lines toward the W3(H 2 O) and W3(OH) star-forming complexes. Infall and outflow motions in the W3(H 2 O) have been characterized by observing HCN and HCO + transitions. High-velocity blue/red-shifted emission, tracing the outflow, show multiple knots, which might originate in episodic and precessing outflows. 'Blue-peaked' line profiles indicate that gas is infalling onto the W3(H 2 O) dust core. The measured large mass accretion rate, 2.3×10 −3 M ⊙ yr −1 , together with the small free-fall time scale, 5×10 3 yr, suggest W3(H 2 O) is in an early evolutionary stage of the process of formation of high-mass stars. For the W3(OH), a two-layer model fit to the HCN and HCO + spectral lines and Spizter/IRAC images support that the W3(OH) Hii region is expanding and interacting with the ambient gas, with the shocked neutral gas being expanding with an expansion timescale of 6.4×10 3 yr. The observations suggest different kinematical timescales and dynamical states for the W3(H 2 O) and W3(OH).

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A candidate circumbinary Keplerian disk in G35.20–0.74 N: A study with ALMA

Cited by 106 publications

References 28 publications

Filamentary structure and Keplerian rotation in the high-mass star-forming region G35.03+0.35 imaged with ALMA

Filamentary structure and Keplerian rotation in the high-mass star-forming region G35.03+0.35 imaged with ALMA

A necklace of dense cores in the high-mass star forming region G35.20−0.74 N: ALMA observations

SMA observations of the W3(OH) complex: Dynamical differentiation between W3(H₂O) and W3(OH)

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A candidate circumbinary Keplerian disk in G35.20–0.74 N: A study with ALMA

Cited by 106 publications

References 28 publications

Filamentary structure and Keplerian rotation in the high-mass star-forming region G35.03+0.35 imaged with ALMA

Filamentary structure and Keplerian rotation in the high-mass star-forming region G35.03+0.35 imaged with ALMA

A necklace of dense cores in the high-mass star forming region G35.20−0.74 N: ALMA observations

SMA observations of the W3(OH) complex: Dynamical differentiation between W3(H2O) and W3(OH)

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SMA observations of the W3(OH) complex: Dynamical differentiation between W3(H₂O) and W3(OH)