Detection of the Winds from the Exciting Sources of Shell H [CSC]ii[/CSC] Regions in NGC 6334

Carral, P.; Kurtz, S.; Rodrı́guez, Luis F.; Menten, K. M.; Cantó, J.; Arceo, R.

doi:10.1086/339701

Cited by 45 publications

(90 citation statements)

References 48 publications

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“…IRAS HIRES maps show some indication of a source in the 100 m band but not in the 12, 25, or 60 m bands (Kraemer et al 1999). Furthermore, no UC H ii region has been detected toward this source, although Carral et al (2002) detected a weak radio continuum source in I(N) with a size of only 400 AU. There is also no sign of clustering in the K-band map, although several red stars have been detected that may be embedded, lower mass stars.…”

Section: Discussionmentioning

confidence: 91%

“…This confusion must arise from the fact that these regions contain entire clusters of sources (see x 4.3). In the remaining core, NGC 6334 I(N), 3.6 cm continuum emission has been detected by Carral et al (2002) at the level of 0.34 mJy over roughly 400 AU; this is both much weaker and much smaller than a typical UC H ii region (Wood & Churchwell 1989). …”

Section: The Location Of Iras Sources and H II Reg Gionsmentioning

confidence: 92%

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A Near-Infrared/Millimeter-Wave Study of Six Fourth-Quadrant High-Mass Star Formation Regions

Sollins

Megeath

2004

Astron J

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We present near-infrared and millimeter-wave observations of six high-mass star-forming regions in the fourth quadrant: RCW 108, G333.6, RCW 117, RCW 122, NGC 6334 I, and G351.6. These regions have heliocentric distances of 1.3-3.0 kpc and total luminosities ranging from 0.5 to 3 ; 10 5 L . Millimeter maps taken in transitions of C 18 O, HC 3 N, 12 C 16 O, and SiO with the Swedish-ESO Submillimetre Telescope 15 m telescope detail the structure and kinematics of the clouds. Near-infrared K-band images of the same regions obtained with the MPG/ESO 2.2 m telescope are used to map the stellar surface density. The C 18 O (1 ! 0) line shows extended high column density gas, with column densities ranging from 10 22 to 3 ; 10 23 cm À2 ; in contrast, the HC 3 N (15 ! 14) emission shows eight sharply peaked dense cores. We examine these cores for recent and ongoing star formation by searching for high-velocity, non-Gaussian wings on the CO (1 ! 0) and SiO (2 ! 1) lines, peaks in the surface density of stars, and positional coincidences with IRAS point sources, as well as masers and H ii regions reported in the literature. All of the cores show evidence of ongoing star formation. NGC 6334 I(N) stands out as a unique case in which an outflow has formed and masers have appeared, but no IRAS source, K-band cluster, or UC H ii region has yet appeared; our data support previous claims that this is a rare example of a core in the earliest stages of forming a cluster of high-and low-mass stars.

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Section: Discussionmentioning

confidence: 91%

Section: The Location Of Iras Sources and H II Reg Gionsmentioning

confidence: 92%

A Near-Infrared/Millimeter-Wave Study of Six Fourth-Quadrant High-Mass Star Formation Regions

Sollins

Megeath

2004

Astron J

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“…At sub-millimetre wavelengths, the central part of NGC 6334 consists of a 10-pc long filament that is also associated with strong extinction (Russeil et al 2010). Several sites of high-mass star formation have been identified (e.g., Loughran et al 1986), by the presence of water masers, UC H ii regions (e.g., Rodriguez et al 1982;Carral et al 2002), molecular outflows, and H ii regions (GUM 61, 62, 63, and 64 (Gum 1955), and GM1-24, indicated in Fig. 1).…”

Section: The Ngc 6334 Star-formation Complexmentioning

confidence: 99%

TheHerschelview of the massive star-forming region NGC 6334

Russeil

Schneider

Anderson

et al. 2013

A&A

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Aims. Fundamental to any theory of high-mass star formation are gravity and turbulence. Their relative importance, which probably changes during cloud evolution, is not known. By investigating the spatial and density structure of the high-mass star-forming complex NGC 6334 we aim to disentangle the contributions of turbulence and gravity. Methods. We used Herschel PACS and SPIRE imaging observations from the HOBYS key programme at wavelengths of 160, 250, 350, and 500 μm to construct dust temperature and column density maps. Using probability distribution functions (PDFs) of the column density determined for the whole complex and for four distinct sub-regions (distinguished on the basis of differences in the column density, temperature, and radiation field), we characterize the density structure of the complex. We investigate the spatial structure using the Δ-variance, which probes the relative amount of structure on different size scales and traces possible energy injection mechanisms into the molecular cloud. Results. The Δ-variance analysis suggests that the significant scales of a few parsec that were found are caused by energy injection due to expanding H ii regions, which are numerous, and by the lengths of filaments seen everywhere in the complex. The column density PDFs have a lognormal shape at low densities and a clearly defined power law at high densities for all sub-regions whose slope is linked to the exponent α of an equivalent spherical density distribution. In particular with α = 2.37, the central sub-region is largly dominated by gravity, caused by individual collapsing dense cores and global collapse of a larger region. The collapse is faster than free-fall (which would lead only to α = 2) and thus requires a more dynamic scenario (external compression, flows). The column density PDFs suggest that the different sub-regions are at different evolutionary stages, especially the central sub-region, which seems to be in a more evolved stage.

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“…At the northeastern end of the region, the deeply-embedded source "I" was first identified in farinfrared images (Emerson et al 1973;McBreen et al 1979;Gezari 1982). NGC6334I contains an embedded cluster of stars in near-infrared images (Tapia et al 1996;Seifahrt et al 2008;Persi & Tapia 2008) and a cometary ultracompact HII (UCHII) region (De Pree et al 1995;Carral et al 2002). The UCHII region is detected in the mid-infrared along with a few other sources (Kraemer et al 1999;Harvey & Gatley 1983).…”

Section: Introductionmentioning

confidence: 99%

THE MASSIVE PROTOSTELLAR CLUSTER NGC 6334I AT 220 au RESOLUTION: DISCOVERY OF FURTHER MULTIPLICITY, DIVERSITY, AND A HOT MULTI-CORE

Brogan

Hunter

Cyganowski

et al. 2016

ApJ

122

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We present VLA and ALMA imaging of the deeply-embedded protostellar cluster NGC6334I from 5 cm to 1.3 mm at angular resolutions as fine as 0.′′ 17 (220 AU). The dominant hot core MM1 is resolved into seven components at 1.3 mm, clustered within a radius of 1000 AU. Four of the components have brightness temperatures > 200 K, radii ∼ 300 AU, minimum luminosities ∼ 10 4 L ⊙ , and must be centrally heated. We term this new phenomenon a "hot multi-core". Two of these objects also exhibit compact free-free emission at longer wavelengths, consistent with a hypercompact HII region (MM1B) and a jet (MM1D). The spatial kinematics of the water maser emission centered on MM1D are consistent with it being the origin of the highvelocity bipolar molecular outflow seen in CO. The close proximity of MM1B and MM1D (440 AU) suggests a proto-binary or a transient bound system. Several components of MM1 exhibit steep millimeter SEDs indicative of either unusual dust spectral properties or time variability. In addition to resolving MM1 and the other hot core (MM2) into multiple components, we detect five new millimeter and two new centimeter sources. Water masers are detected for the first time toward MM4A, confirming its membership in the protocluster. With a 1.3 mm brightness temperature of 97 K coupled with a lack of thermal molecular line emission, MM4A appears to be a highly optically-thick 240 L ⊙ dust core, possibly tracing a transient stage of massive protostellar evolution. The nature of the strongest water maser source CM2 remains unclear due to its combination of non-thermal radio continuum and lack of dust emission.

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Detection of the Winds from the Exciting Sources of Shell H [CSC]ii[/CSC] Regions in NGC 6334

Cited by 45 publications

References 48 publications

A Near-Infrared/Millimeter-Wave Study of Six Fourth-Quadrant High-Mass Star Formation Regions

A Near-Infrared/Millimeter-Wave Study of Six Fourth-Quadrant High-Mass Star Formation Regions

TheHerschelview of the massive star-forming region NGC 6334

THE MASSIVE PROTOSTELLAR CLUSTER NGC 6334I AT 220 au RESOLUTION: DISCOVERY OF FURTHER MULTIPLICITY, DIVERSITY, AND A HOT MULTI-CORE

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