NGC 6334 and NGC 6357: H<i>α</i>kinematics and the nature of the H II regions

Russeil, D.; Tigé, J.; Adami, C.; Schneider, N.; Zavagno, A.; Samal, M. R.; Amram, P.; Guennou, L.; Coarer, E. Le; Walsh, A. J.; Longmore, Steven N.; Purcell, Cormac

doi:10.1051/0004-6361/201424484

Cited by 24 publications

(42 citation statements)

References 81 publications

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“…However, the values obtained from the integrated flux densities are indicative of non-thermal emission (Rosero et al 2016;Kobulnicky & Johnson 1999;Rodriguez et al 1993). Thus a scenario of co-existing free-free and non-thermal emission can be visualized for the H II regions as has been addressed by several authors (Russeil et al 2016;Veena et al 2016;Nandakumar et al 2016;Mücke et al 2002;Das et al 2017). The above interpretation should be taken with caution because GMRT is not a scaled array between the observed frequencies and the observed visibilities span different uv ranges.…”

Section: Emission From Ionized Gasmentioning

confidence: 99%

Radio and infrared study of southern H II regions G346.056−0.021 and G346.077−0.056

Das

Tej

Vig

et al. 2018

A&A

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Aims. We present a multiwavelength study of two southern Galactic H II regions G346.056−0.021 and G346.077−0.056 which are located at a distance of 10.9 kpc. The distribution of ionized gas, cold and warm dust and the stellar population associated with the two H II regions are studied in detail using measurements at near-infrared, mid-infrared, far-infrared, submillimeter and radio wavelengths. Methods. The radio continuum maps at 1280 and 610 MHz were obtained using the Giant Metrewave Radio Telescope to probe the ionized gas. The dust temperature, column density and dust emissivity maps were generated by using modified blackbody fits in the far-infrared wavelength range 160 -500 µm. Various near-and mid-infrared colour and magnitude criteria were adopted to identify candidate ionizing star(s) and the population of young stellar objects in the associated field. Results. The radio maps reveal the presence diffuse ionized emission displaying distinct cometary morphologies. The 1280 MHz flux densities translate to ZAMS spectral types in the range O7.5V -O7V and O8.5V -O8V for the ionizing stars of G346.056−0.021 and G346.077−0.056, respectively. A few promising candidate ionizing star(s) are identified using near-infrared photometric data. The column density map shows the presence of a large, dense dust clump enveloping G346.077−0.056. The dust temperature map shows peaks towards the two H II regions. The submillimetre image shows the presence of two additional clumps one being associated with G346.056−0.021. The masses of the clumps are estimated to range between ∼ 1400 to 15250 M . Based on simple analytic calculations and the correlation seen between the ionized gas distribution and the local density structure, the observed cometary morphology in the radio maps is better explained invoking the champagne-flow model. Conclusions.

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Section: Emission From Ionized Gasmentioning

confidence: 99%

Radio and infrared study of southern H II regions G346.056−0.021 and G346.077−0.056

Das

Tej

Vig

et al. 2018

A&A

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“…NGC 6334 is located at a distance of 1.61 kpc (PT08), and consists of a dense molecular gas filament extended along the Galactic plane over 10 pc and extended H II regions outside the filament. The filamentary molecular ridge is dense and consists of six active sub-regions identified by McBreen et al (1979) and Loughran et al (1978) as far-infrared sources which are denominated I-V and I(N) (see Table 3 in TP08, and recent papers Tigé et al 2017;Andŕe et al 2016;Russeil et al 2010Russeil et al , 2012Russeil et al , 2013Russeil et al , 2016Willis et al 2013, Zernickel et al 2013Feigelson et al 2009). There are molecular outflows associated with I(N) and I (Megeath & Tieftrunk,1999, McCutcheon et al 2000, Leurini et al 2006, Qiu et al 2011.…”

Section: Twin Starbursts In the Carina-sagittarius Armmentioning

confidence: 99%

Molecular clouds in the NGC 6334 and NGC 6357 region: Evidence for a 100 pc-scale cloud–cloud collision triggering the Galactic mini-starbursts

Fukui

Kohno

Yokoyama

et al. 2018

Publications of the Astronomical Society of Japan

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We carried out new CO (J =1-0, 2-1 and 3-2) observations with NANTEN2 and ASTE in the region of the twin Galactic mini-starbursts NGC 6334 and NGC 6357. We detected two velocity molecular components of 12 km s −1 velocity separation, which is continuous over 3 degrees along the plane. In NGC 6334 the two components show similar two-peaked intensity distributions toward the young H II regions and are linked by a bridge feature. In NGC 6357 we found spatially complementary distribution between the two velocity components as well as a bridge feature in velocity. Based on these results we hypothesize that the two clouds in the two regions collided with each other in the past few Myr and triggered formation of the starbursts over ∼100 pc. We suggest that the formation of the starbursts happened toward the collisional region of ∼ 10-pc extents with initial high molecular column densities. For NGC 6334 we present a scenario which includes spatial variation of the colliding epoch due to non-uniform cloud separation. The scenario possibly explains the apparent age difference among the young O stars in NGC 6334 raging from 10 4 yrs to 10 6 yrs; the latest collision happened within 10 5 yrs toward the youngest stars in NGC 6334 I(N) and I which exhibit molecular outflows without H II regions. For NGC 6357 the O stars were formed a few Myrs ago, and the cloud dispersal by the O stars is significant. We conclude that cloud-cloud collision offers a possible explanation of the min-starburst over a 100-pc scale.

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“…From the above estimates we infer thermal free-free emission to be associated with components A and C whereas the emission from component B shows spectral signature for non-thermal emission. Compact radio sources exhibiting such large negative spectral index have been discussed in Russeil et al (2016) and Rodríguez et al (2014) where the latter study puts forth a viable scenario of colliding winds of a massive binary system which produces a shocked region between the components where electrons can reach relativistic speeds by Fermi acceleration thus producing synchrotron emission. Similar interpretation has been discussed by Luque-Escamilla et al (2011) for the extended non-thermal radio emission detected towards the W43 cluster.…”

Section: Spectral Index Mapsmentioning

confidence: 99%

Infrared dust bubble CS51 and its interaction with the surrounding interstellar medium

Das

Tej

Vig

et al. 2017

Monthly Notices of the Royal Astronomical Society

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A multiwavelength investigation of the southern infrared dust bubble CS51 is presented in this paper. We probe the associated ionized, cold dust, molecular and stellar components. Radio continuum emission mapped at 610 and 1300 MHz, using the Giant Metrewave Radio Telescope, India, reveal the presence of three compact emission components (A, B, and C) apart from large-scale diffuse emission within the bubble interior. Radio spectral index map show the coexistence of thermal and non-thermal emission components. Modified blackbody fits to the thermal dust emission using Herschel PACS and SPIRE data is performed to generate dust temperature and column density maps. We identify five dust clumps associated with CS51 with masses and radius in the range 810 -4600 M and 1.0 -1.9 pc, respectively. We further construct the column density probability distribution functions of the surrounding cold dust which display the impact of ionization feedback from high-mass stars. The estimated dynamical and fragmentation timescales indicate the possibility of collect and collapse mechanism in play at the bubble border. Molecular line emission from the MALT90 survey is used to understand the nature of two clumps which show signatures of expansion of CS51.

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NGC 6334 and NGC 6357: Hαkinematics and the nature of the H II regions

Cited by 24 publications

References 81 publications

Radio and infrared study of southern H II regions G346.056−0.021 and G346.077−0.056

Radio and infrared study of southern H II regions G346.056−0.021 and G346.077−0.056

Molecular clouds in the NGC 6334 and NGC 6357 region: Evidence for a 100 pc-scale cloud–cloud collision triggering the Galactic mini-starbursts

Infrared dust bubble CS51 and its interaction with the surrounding interstellar medium

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