First 450 $\sf \mu$m dust continuum mapping of the massive star-forming region NGC 3576 with 
the P-ArTéMiS bolometer camera

André, P.; Minier, V.; Gallais, P.; Revéret, V.; Pennec, J. Le; Rodriguez, L.; Boulade, O.; Doumayrou, E.; Dubreuil, Didier; Lortholary, M.; Martignac, J.; Talvard, M.; Breuck, C. De; Hamon, G.; Schneider, N.; Bontemps, Sylvain; Lagage, Pierre-Olivier; Pantin, É.; Roussel, Hervé; Miller, M.; Purcell, Cormac; Hill, T.; Stützki, J.

doi:10.1051/0004-6361:200810957

Cited by 44 publications

(74 citation statements)

References 24 publications

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“…4 are similar to the tracks used by André et al (2008) and were computed assuming each protostar forms from a prestellar core of finite initial mass M core ≡ M env (0) and has L bol = GM (t)Ṁ acc (t)/R (t) + L (t), where R (M ) is the protostellar radius (mass) and L the PMS birthline luminosity (Stahler 1988). The mass accretion rate and the envelope mass were assumed to be related bẏ M acc (t) = M env (t)/τ, where = 50% is the typical SFE for individual cores (cf.…”

Section: Evolutionary Classification Of Protostellar Sourcesmentioning

confidence: 64%

The formation of active protoclusters in the Aquila rift: a millimeter continuum view

Maury¹,

André²,

Men’shchikov³

et al. 2011

A&A

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While most stars are believed to form in stellar clusters, the formation and early evolution of young stellar clusters is still largely unknown. Improving our knowledge of the earliest phases of clustered star formation is crucial for understanding the origin of the stellar initial mass function and the efficiency of the star formation process, which both play a key role in the evolution of galaxies. Here, we present an analysis of the Aquila rift complex which addresses the questions of the star formation rate (SFR), star formation efficiency (SFE) and typical lifetime of the Class 0 protostellar phase in two nearby cluster-forming clumps: the Serpens South and W40 protoclusters. We carried out a 1.2 mm dust continuum mapping of the Aquila rift complex with the MAMBO bolometer array on the IRAM 30 m telescope. Using a multi-scale source extraction method, we perform a systematic source extraction in our millimeter continuum map. Based on complementary data from the Herschel Gould Belt survey and Spitzer maps, we characterize the spectral energy distributions (SEDs) of the 77 mm continuum sources detected with MAMBO and estimate their evolutionary stages. Taking advantage of the comprehensive dataset available for the Serpens South region, spanning wavelengths from 2 μm to 1.2 mm, we estimate the numbers of young stellar objects (YSOs) at different evolutionary stages and find a ratio of Class 0 to Class I protostars N(0)/N(I) = 0.19−0.27. This low ratio supports a scenario of relatively fast accretion at the beginning of the protostellar phase, and leads to a Class 0 lifetime of ∼4−9 × 10 4 yr. We also show that both the Serpens South and W40 protoclusters are characterized by large fractions of protostars and high SFRs ∼ 20−50 M Myr −1 pc −2 , in agreement with the idea that these two nearby clumps are active sites of clustered star formation currently undergoing bursts of star formation, and have the potential ability to form bound star clusters. While the formation of these two protoclusters is likely to have been initiated in a very different manner, the resulting protostellar populations are observed to be very similar. This suggests that after the onset of gravitational collapse, the detailed manner in which the collapse has been initiated does not affect much the ability of a clump to form stars.

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Section: Evolutionary Classification Of Protostellar Sourcesmentioning

confidence: 64%

The formation of active protoclusters in the Aquila rift: a millimeter continuum view

Maury¹,

André²,

Men’shchikov³

et al. 2011

A&A

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128

244

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“…Core masses range from 5 to 516 M and most appear to be gravitationally bound. Complementary results by André et al (2008) imply that seven cores will go on to form massive stars between 15 and 50 M . The large scale velocity structure of the filament is smooth, but at least one clump shows the signature of inward gas motions via asymmetries in the NH 3 (1,1) line profiles.…”

Section: Introductionmentioning

confidence: 77%

Multi-generation massive star-formation in NGC 3576

Purcell

Minier

Longmore

et al. 2009

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Context. Recent 1.2-mm continuum observations have shown the giant H II region NGC 3576 to be embedded in the centre of an extended filamentary dust-cloud. The bulk of the filament away from the H II region contains a number of clumps seen only at (sub-)millimetre wavelengths. Infrared and radio observations of the central star cluster have uncovered evidence of sequential starformation leading us to believe that the adjacent clumps may host massive protostellar objects at a very early stage of evolution. Aims. We have investigated the physical and chemical conditions in the dusty clumps with the goal of characterising their star-forming content. Methods. We have used the Australia Telescope Compact Array (ATCA) to image the cloud for the NH 3 (1,1), (2,2) and (4,4) transitions, 22 GHz H 2 O masers, and 23 GHz continuum emission. The 70-m Tidbinbilla dish was used to estimate the total integrated intensity of NH 3 . We also utilised the 22-m Mopra antenna to map the region for the molecular lines 13 CO (1 -0), C 18 O (1 -0), HCO + (1 -0), H 13 CO + (1 -0), CS (1 -0) and N 2 H + (1 -0). Results. Emission from dense molecular gas follows the morphology of the 1.2-mm dust emission, except towards the central ionised region. The H II region is observed to be expanding into the molecular cloud, sweeping up a clumpy shell of gas, while the central star cluster is dispersing the molecular gas to the east. Analysis of the NH 3 data indicates that temperature and linewidth gradients exist in the western arm of the filament. Temperatures are highest adjacent to the central H II region, indicating that the embedded cluster of young stars there is heating the gas. Six new H 2 O masers were detected in the arms of the filament, all associated with NH 3 emission peaks, confirming that star-formation has begun within these cores. Core masses range from 5 to 516 M and most appear to be gravitationally bound. Complementary results by André et al. (2008) imply that seven cores will go on to form massive stars between 15 and 50 M . The large scale velocity structure of the filament is smooth, but at least one clump shows the signature of inward gas motions via asymmetries in the NH 3 (1,1) line profiles. The same clump exhibits an enhanced abundance of N 2 H + , which coupled with an absence of CO indicates depletion onto the dust grain surface. Conclusions. The HII region at the heart of NGC 3576 is potentially triggering the formation of massive stars in the bulk of the associated cloud.

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“…The location of these four sources on the M env -L bol evolutionary diagram for protostars is shown in Fig. 20, and their comparison with the evolutionary tracks of (André et al 2008, and references therein), suggests that these objects will evolve The slanted red line corresponds to the location where 50% of the initial core mass is converted into stellar mass (see Bontemps et al 1996;André et al 2000).…”

Section: Evolutionary Status Of Massive Sourcesmentioning

confidence: 96%

The molecular complex associated with the Galactic H II region Sh2-90: a possible site of triggered star formation

Samal

Zavagno

Deharveng

et al. 2014

A&A

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Aims. We investigate the star formation activity in the molecular complex associated with the Galactic H ii region Sh2-90.Methods. We obtain the distribution of the ionized and cold neutral gas using radio-continuum and Herschel observations. We use near-infrared and Spitzer data to investigate the stellar content of the complex. We discuss the evolutionary status of embedded massive young stellar objects (MYSOs) using their spectral energy distribution.Results. The Sh2-90 region presents a bubble morphology in the mid-infrared. Radio observations suggest it is an evolved H ii region with an electron density ∼144 cm −3 , emission measure ∼6.7 × 10 4 cm −6 pc and an ionized mass ∼55 M . From Herschel and CO (J = 3−2) observations we found that the H ii region is part of an elongated extended molecular cloud (H 2 column density ≥3 × 10 21 cm −2 and dust temperature 18−27 K) of total mass ≥1 × 10 4 M . We identify the ionizing cluster of Sh2-90, the main exciting star being an O8-O9 V star. Five cold dust clumps, four mid-IR blobs around B stars, and a compact H ii region are found at the edge of the bubble. The velocity information derived from CO data cubes suggest that most of them are associated with the Sh2-90 region. One hundred and twenty-nine low mass (≤3 M ) YSOs have been identified, and they are found to be distributed mostly in the regions of high column density. Four candidate Class 0/I MYSOs have been found. We suggest that multi-generation star formation is present in the complex. From evidence of interaction, time scales involved, and evolutionary status of stellar/protostellar sources, we argue that the star formation at the edges of Sh2-90 might have been triggered. However, several young sources in this complex are probably formed by some other processes.

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First 450 $\sf \mu$m dust continuum mapping of the massive star-forming region NGC 3576 with the P-ArTéMiS bolometer camera

Cited by 44 publications

References 24 publications

The formation of active protoclusters in the Aquila rift: a millimeter continuum view

The formation of active protoclusters in the Aquila rift: a millimeter continuum view

Multi-generation massive star-formation in NGC 3576

The molecular complex associated with the Galactic H II region Sh2-90: a possible site of triggered star formation

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