Galactic Plane H2O Masers: A Southern Survey

Batchelor, R.; Caswell, J. L.; Goss, W. M.; Haynes, R. F.; Knowles, SH; Wellington, K. J.

doi:10.1071/ph800139

Cited by 62 publications

(79 citation statements)

References 4 publications

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“…From observations with the VLT MIR VISIR camera, Grave et al (2014) found indications that this region consists of two main luminous sources (O4V and O5V) which account for at least half of the luminosity from this region. As well as being proximate to the Hii region G333.6-0.22, this molecular outflow source is also associated with MSX and 1.2-mm dust sources (Mookerjea et al 2004) and masers of H 2 O and OH (Batchelor et al 1980;Caswell 1998).…”

Section: G333 Outflow/infall Sourcesmentioning

confidence: 88%

Infall, outflow, and turbulence in massive star-forming cores in the G333 giant molecular cloud

Wiles

Redman

et al. 2015

Mon. Not. R. Astron. Soc.

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We present molecular line imaging observations of three massive molecular outflow sources, G333.6-0.2, G333.1-0.4, and G332.8-0.5, all of which also show evidence for infall, within the G333 giant molecular cloud (GMC). All three are within a beam size (36 arcseconds) of IRAS sources, 1.2-mm dust clumps, various masing species and radio continuum-detected Hii regions and hence are associated with high-mass star formation. We present the molecular line data and derive the physical properties of the outflows including the mass, kinematics, and energetics and discuss the inferred characteristics of their driving sources. Outflow masses are of 10 to 40 M ⊙ in each lobe, with core masses of order 10 3 M ⊙ . outflow size scales are a few tenth of a parsec, timescales are of several ×10 4 years, mass loss rates a few ×10 −4 M ⊙ /yr. We also find the cores are turbulent and highly supersonic.

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Section: G333 Outflow/infall Sourcesmentioning

confidence: 88%

Infall, outflow, and turbulence in massive star-forming cores in the G333 giant molecular cloud

Wiles

Redman

et al. 2015

Mon. Not. R. Astron. Soc.

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“…Both X-ray point sources and extended emission have been reported. RCW 49 has also been observed in molecular and atomic line surveys of OH (Caswell 1997(Caswell , 1998, CH 3 OH (Caswell 1997), H 2 O (Batchelor et al 1980), H 2 CO (Caswell & Haynes 1987;Whiteoak & Gardner 1974), and H109 and/or H110 lines (Wilson et al 1970;Caswell & Haynes 1987). It has also been imaged in the radio continuum by , , Haynes et al (1978Haynes et al ( , 1979, and Whiteoak & Uchida (1997, hereafter WU97).…”

Section: Introductionmentioning

confidence: 90%

RCW 49 at Mid‐Infrared Wavelengths: A GLIMPSE from the Spitzer Space Telescope

Churchwell¹,

Whitney

Babler³

et al. 2004

ASTROPHYS J SUPPL S

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The luminous, massive star formation region RCW 49, located in the southern Galactic plane, was imaged with the Infrared Array Camera (IRAC) on the Spitzer Space Telescope as part of the Galactic Legacy Infrared Mid-Plane Survey Extraordinaire (GLIMPSE) program. The IRAC bands contain polycyclic aromatic hydrocarbon (PAH) features at 3.3, 6.2, 7.7, and 8.6 m, as well as the Br line. These features are the major contributors to the diffuse emission from RCW 49 in the IRAC bands. The Spitzer IRAC images show that the dust in RCW 49 is distributed in a network of fine filaments, pillars, knots, sharply defined boundaries, bubbles, and bow shocks. The regions immediately surrounding the ionizing star cluster and W-R stars are evacuated of dust by stellar winds and radiation. The IRAC images of RCW 49 suggest that the dust in RCW 49 has been sculpted by the winds and radiation from the embedded luminous stars in the inner 5 0 (inner $6 pc) of the nebula. At projected angular radii > 5 0 from the central ionizing cluster, the azimuthally averaged infrared intensity falls off as $ À3 . Both high-resolution radio and mid-IR images suggest that the nebula is density bounded along its western boundary. The filamentary structure of the dust in RCW 49 suggests that the nebula has a small dust filling factor and, as a consequence, the entire nebula may be slightly density bounded to H-ionizing photons. Subject headingg s: astrochemistry -dust, extinction -H ii regions -infrared: ISM -ISM: lines and bands

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“…Also Garay et al observed a strong signature of large-scale infall motions and derived an infall speed of ∼1 km s −1 and a mass infall rate of ∼1 × 10 −2 M yr −1 at a radius of ∼0.2 pc. Water masers were detected toward IRAS 16547−4247 by Batchelor et al (1980) with the Parkes radio telescope. They reported a flux of 100 Jy and a v LSR = −34 km s −1 for the maser emission.…”

Section: Introductionmentioning

confidence: 99%

The Rotating Molecular Structures and the Ionized Outflow Associated With Iras 16547–4247

Franco-Hernández

Moran

Rodrı́guez³

et al. 2009

ApJ

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We present Very Large Array 1.3 cm radio continuum and water maser observations as well as Submillimeter Array SO 2 (226.300 GHz) and 1.3 mm dust continuum observations toward the massive star formation region IRAS 16547−4247. We find evidence of multiple sources in the central part of the region. There is evidence of a rotating structure associated with the most massive of these sources, traced at small scales (∼50 AU) by the water masers. At large scales (∼1000 AU), we find a velocity gradient in the SO 2 molecular emission with a barely resolved structure that can be modeled as a rotating ring or two separate objects. The velocity gradients of the masers and of the molecular emission have the same sense and may trace the same structure at different size scales. The position angles of the structures associated with the velocity gradients are roughly perpendicular to the outflow axis observed in radio continuum and several molecular tracers. We estimate the mass of the most massive central source to be around 30 solar masses from the velocity gradient in the water maser emission. The main source of error in this estimate is the radius of the rotating structure. We also find water masers that are associated with the large-scale molecular outflow of the system, as well as water masers that are associated with other sources in the region. Our results suggest that the formation of this source, one of the most luminous protostars or protostellar clusters known, is taking place with the presence of ionized jets and disk-like structures.

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Galactic Plane H2O Masers: A Southern Survey

Cited by 62 publications

References 4 publications

Infall, outflow, and turbulence in massive star-forming cores in the G333 giant molecular cloud

Infall, outflow, and turbulence in massive star-forming cores in the G333 giant molecular cloud

RCW 49 at Mid‐Infrared Wavelengths: A GLIMPSE from the Spitzer Space Telescope

The Rotating Molecular Structures and the Ionized Outflow Associated With Iras 16547–4247

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