Interferometric multi-wavelength (sub)millimeter continuum study of the young high-mass protocluster IRAS 05358+3543

Beuther, H.; Leurini, S.; Schilke, P.; Wyrowski, F.; Menten, K. M.; Zhang, Qizhou

doi:10.1051/0004-6361:20066742

Cited by 95 publications

(131 citation statements)

References 50 publications

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“…But only a few studies have been dedicated to the earliest phases of star formation and to regions of 0.1 pc or smaller. In IRAS 05358+3543, Beuther et al (2007) reported the detection of two cores potentially more massive than 8 M with masses of 5−10.5 and 2.7−18.5 M , respectively, inside sizes of the same order as in the present work. One of them can be further subdivided into two objects separated by only 1700 AU, and may contain an B1 star that excites a hyper-compact HII region.…”

Section: Envelope Masses Of the Proto-stellar Objectssupporting

confidence: 79%

Fragmentation and mass segregation in the massive dense cores of Cygnus X

Bontemps¹,

Motte²,

Csengeri³

et al. 2010

A&A

188

337

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Massive dense cores (MDCs) are the high-mass equivalent of the so-called dense cores in nearby star-forming regions. With typical sizes of 0.1 pc, they could form either a few high-mass stars, or a cluster of low-mass stars. We present high-angular resolution continuum observations obtained with the IRAM Plateau de Bure interferometer at 1.3 and 3.5 mm towards the six most massive and youngest (IR-quiet) dense cores in the Cygnus X complex. Located at only 1.7 kpc, the Cygnus X region offers the opportunity of reaching small enough scales (of the order of 1700 AU at 1.3 mm) to separate individual collapsing objects, and thus to observe and constrain the result of the fragmentation process. The cores are sub-fragmented with a total of 23 fragments inside 5 cores. Only the most compact MDC, CygX-N63, may host a single proto-stellar object with an envelope as massive as ∼60 M . The fragments in the other cores have sizes and separations similar to low-mass pre-stellar condensations and Class 0 young stellar objects in nearby protoclusters, and are most probably self-gravitating objects (M > M vir ). In addition to CygX-N63, a total of 8 objects are found to be probable precursors of OB stars with their envelope masses ranging from 8.4 to 30 M inside a FWHM of 4000 AU. The level of fragmentation is globally higher than in the turbulence regulated, monolithic collapse scenario, but it is also not as high as expected in a pure gravo-turbulent scenario where the distribution of mass is dominated by low-mass protostars/stars. Here, the fractions of the total MDC masses in the high-mass proto-stellar fragments are found to be as high as 37, 58, and 100% in CygX-N12, CygX-N53, and CygX-N63, respectively. These high fractions of mass in the proto-stellar fragments are also indicative of a high efficiency of core formation in the MDCs. The increase in the core formation efficiency as a function of average density in the MDCs is proposed to be caused by the increasing importance of self-gravity leading to gravitational collapse on the scale of the MDCs. At the same time, the observed MDCs tend to fragment into a few proto-stellar objects within their central regions. We are therefore probably witnessing the primordial mass segregation of clusters. The physical origin of the fragmentation into a few high-mass objects is not yet clear, and will be investigated in the future by studying the kinematics of the MDCs.

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Section: Envelope Masses Of the Proto-stellar Objectssupporting

confidence: 79%

Fragmentation and mass segregation in the massive dense cores of Cygnus X

Bontemps¹,

Motte²,

Csengeri³

et al. 2010

A&A

188

337

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“…Alternatively, the presence of winds/outflows (see Sect. 4.2) could mimic a low value of β (Beuther et al 2007). Here we adopt a β = 1.6 in the rest of the paper.…”

Section: Density Temperature and Spectral Indecesmentioning

confidence: 96%

High-angular resolution observations of methanol in the infrared dark cloud core G11.11-0.12P1

Gómez

Wyrowski

Pillai

et al. 2011

A&A

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Recent studies suggest that infrared dark clouds (IRDCs) have the potential of harboring the earliest stages of massive star formation and indeed evidence for this is found toward distinct regions within them. We present a study with the Plateau de Bure Interferometer of a core in the archetypal filamentary IRDC G11.11-0.12 of a few arcsecond resolution to determine its physical and chemical structures. The data consist of continuum and line observations covering the C 34 S 2 → 1 line and the methanol 2 k → 1 k v t = 0 lines at 3 mm and the methanol 5 k → 4 k v t = 0 lines at 1 mm. Our observations show extended emission in the continuum at 1 and 3 mm. The methanol 2 k → 1 k v t = 0 emission has three maxima extending over a 1 pc scale (when merged with single-dish short-spacing observations); one of the maxima is spatially coincident with the continuum emission. The fitting results show an enhanced methanol fractional abundance (∼3 × 10 −8 ) at the central peak with respect to the other two peaks, where it decreases by about an order of magnitude (∼4−6 × 10 −9 ). Evidence of extended 4.5 μm emission, "wings" in the CH 3 OH 2 k → 1 k spectra, and CH 3 OH abundance enhancements point to the presence of an outflow in the east-west direction. In addition, we find a gradient of ∼4 km s −1 in the same direction, which we interpret as being produced by an outflow(s)-cloud interaction.

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“…The CH 3 OH masers show a linear distribution that was suggested to trace an edge-on disk (PA CH 3 OH ≈ 25 • , Minier et al 2000), which is associated with one of the millimeter continuum sources identified by Beuther et al (2007), i.e. mm1a.…”

Section: S231mentioning

confidence: 97%

“…mm1a. Beuther et al (2007) suggested that mm1a, which is also associated with an hypercompact H ii region and a mid-infrared source, forms a binary system with mm1b (with a projected separation of 1700 AU). Ginsburg et al (2009) observed mm1a with the VLA and they determined a projected separation between mm1a and the CH 3 OH maser site of ∼400 AU suggesting that probably the binary system is formed by mm1a and the massive YSO associated with the CH 3 OH maser site.…”

Section: S231mentioning

confidence: 99%

EVN observations of 6.7 GHz methanol maser polarization in massive star-forming regions

Surcis

Vlemmings

Langevelde

et al. 2013

A&A

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Context. Magnetic fields have only recently been included in theoretical simulations of high-mass star formation. The simulations show that magnetic fields play an important role in the formation and dynamics of molecular outflows. Masers, in particular 6.7-GHz CH 3 OH masers, are the best probes of the magnetic field morphologies around massive young stellar objects on the smallest scales of 10-100 AU. Aims. Providing new observational measurements of the morphology of magnetic fields around massive young stellar objects by using 6.7-GHz CH 3 OH maser emission is very important for setting constraints on the numerical simulations of massive star formation. Methods. This paper focuses on 4 massive young stellar objects, IRAS 06058+2138-NIRS 1, IRAS 22272+6358A, S255-IR, and S231, which complement our previous 2012 sample (the first EVN group). From all these sources, molecular outflows have been detected in the past. Seven of the European VLBI Network antennas were used to measure the linear polarization and Zeeman-splitting of the 6.7-GHz CH 3 OH masers in the star-forming regions in this second EVN group. Results. We detected a total of 128 CH 3 OH masing cloudlets. Fractional linear polarization (0.8%-11.3%) was detected towards 18% of the CH 3 OH masers in our sample. The linear polarization vectors are well ordered in all the massive young stellar objects. We measured significant Zeeman-splitting in IRAS 06058+2138-NIRS 1 (ΔV Z = 3.8 ± 0.6 m s −1 ) and S255-IR (ΔV Z = 3.2 ± 0.7 m s −1 ). Conclusions. By considering the 20 massive young stellar objects towards which the morphology of magnetic fields was determined by observing 6.7-GHz CH 3 OH masers in both hemispheres, we find no evident correlation between the linear distributions of CH 3 OH masers and the outflows or the linear polarization vectors. On the other hand, we present first statistical evidence that the magnetic field (on scales 10-100 AU) is primarily oriented along the large-scale outflow direction. Moreover, we empirically find that the linear polarization fraction of unsaturated CH 3 OH masers is P l < 4.5%.

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Interferometric multi-wavelength (sub)millimeter continuum study of the young high-mass protocluster IRAS 05358+3543

Cited by 95 publications

References 50 publications

Fragmentation and mass segregation in the massive dense cores of Cygnus X

Fragmentation and mass segregation in the massive dense cores of Cygnus X

High-angular resolution observations of methanol in the infrared dark cloud core G11.11-0.12P1

EVN observations of 6.7 GHz methanol maser polarization in massive star-forming regions

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