Small-scale structure in the Rosette molecular cloud revealed by <i>Herschel</i>

Francesco, James Di; Sadavoy, Sarah; Motte, F.; Schneider, N.; Hennemann, M.; Csengeri, T.; Bontemps, Sylvain; Balog, Z.; Zavagno, A.; André, Ph.; Saraceno, P.; Griffin, Matthew Joseph; Men’shchikov, A.; Abergel, A.; Baluteau, J. P.; Bernard, J.-P.; Cox, P.; Deharveng, L.; Didelon, P.; Giorgio, A. M. Di; Hargrave, Peter Charles; Huang, M.; Kirk, J. M.; Leeks, S. J.; Li, J. Z.; Marston, A. P.; Martín, P. G.; Minier, V.; Molinari, S.; Olofsson, G.; Persi, P.; Pezzuto, S.; Russeil, D.; Sauvage, M.; Sibthorpe, B.; Spinoglio, L.; Testi, L.; Teyssier, D.; Vavrek, R.; Ward-Thompson, Derek; White, G. J.; Wilson, C. D.; Woodcraft, A.

doi:10.1051/0004-6361/201014598

Cited by 40 publications

(41 citation statements)

References 24 publications

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“…This is confirmed by Herschel observations that discovered protostars and protostellar clumps di Francesco et al 2010) in all the clusters they have mapped. NGC 2244, REFL 09, and CMFT 10 would be more likely to be about to stop their activity.…”

Section: Individual Memberssupporting

confidence: 78%

Young stellar clusters in the Rosette molecular cloud

Cambrésy

Márton

Fehér

et al. 2013

A&A

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Aims. We focus on characterizing the young stellar population in the Rosette complex to improve our understanding of the processes that regulate the star formation in this region. Methods. We propose an original method that relies on the joint analysis of the star color and density in the near-infrared. It leads to mapping the molecular cloud spatial distribution and detecting the embedded clusters with their characterization in terms of member number and age estimation. Results. We have identified 13 clusters, 2 of which are new discoveries, and we estimate that the total number of young stellar objects in the Rosette ranges between 4000 and 8000 members. We find that the age distribution of the young clusters is not consistent with a general triggered scenario for the star formation in this molecular cloud. Conclusions. This study proves that the Rosette complex evolution is not governed by the influence of its OB star population. It suggests that the simple morphological appearance of an active region is not sufficient to conclude much about the triggering role in the star formation process. Our method of constraining the cluster properties using UKIDSS and WISE data has proven efficient, and studies of other regions of the Galactic plane would definitely benefit from this approach.

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Section: Individual Memberssupporting

confidence: 78%

Young stellar clusters in the Rosette molecular cloud

Cambrésy

Márton

Fehér

et al. 2013

A&A

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“…7. For instance, di Francesco et al (2010) already used this procedure and combined maps of Herschel data with Spitzer ones to distinguish between prestellar and protostellar cores. Once FHSC candidates are identified from these flux examinations, the next step will be to target them with high-resolution interferometry such as ALMA (see Paper II) to constrain the physical properties (e.g., strength of the magnetic field).…”

Section: Example Of Methodology To Target First Corementioning

confidence: 99%

Synthetic observations of first hydrostatic cores in collapsing low-mass dense cores

Commerçon

Launhardt

Dullemond

et al. 2012

A&A

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Context. The low-mass star formation evolutionary sequence is relatively well-defined both from observations and theoretical considerations. The first hydrostatic core is the first protostellar equilibrium object that is formed during the star formation process. Aims. Using state-of-the-art radiation-magneto-hydrodynamic 3D adaptive mesh refinement calculations, we aim to provide predictions for the dust continuum emission from first hydrostatic cores. Methods. We investigated the collapse and the fragmentation of magnetized 1 M prestellar dense cores and the formation and evolution of first hydrostatic cores using the RAMSES code. We used three different magnetization levels for the initial conditions, which cover a wide variety of early evolutionary morphology, e.g., the formation of a disk or a pseudo-disk, outflow launching, and fragmentation. We post-processed the dynamical calculations using the 3D radiative transfer code RADMC-3D. We computed spectral energy distributions and usual evolutionary stage indicators such as bolometric luminosity and temperature. Results. We find that the first hydrostatic core lifetimes depend strongly on the initial magnetization level of the parent dense core. We derive, for the first time, spectral energy distribution evolutionary sequences from high-resolution radiation-magneto-hydrodynamic calculations. We show that under certain conditions, first hydrostatic cores can be identified from dust continuum emission at 24 μm and 70 μm. We also show that single spectral energy distributions cannot help in distinguishing between the formation scenarios of the first hydrostatic core, i.e., between the magnetized and non-magnetized models. Conclusions. Spectral energy distributions are a first useful and direct way to target first hydrostatic core candidates but highresolution interferometry is definitively needed to determine the evolutionary stage of the observed sources.

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“…Triggered star formation is thought to be at work in this region, owing to the ionizing radiation and powerful winds of the NGC 2244 O stars. Recent results obtained by the Herschel Space Observatory reveal the presence of younger objects farther away from the HII region center, as well as temperature gradients (di Francesco et al 2010;Motte et al 2010;Schneider et al 2010). Constraining the mechanical energy release and ionizing flux of the massive star population is thus important in order to quantitatively study the process of star formation triggering.…”

Section: Introductionmentioning

confidence: 98%

“…As such, this sample is well suited to investigating the effects of rotation on massive stars surface abundances. The Rosette nebula is also famous for the numerous young stellar objects and embedded clusters in the so-called Rosette molecular cloud (Phelps & Lada 1997;di Francesco et al 2010). Triggered star formation is thought to be at work in this region, owing to the ionizing radiation and powerful winds of the NGC 2244 O stars.…”

Section: Introductionmentioning

confidence: 99%

A quantitative study of O stars in NGC 2244 and the Monoceros OB2 association

Martins

Mahy

Hillier

et al. 2012

A&A

103

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Aims. Our goal is to determine the stellar and wind properties of seven O stars in the cluster NGC 2244 and three O stars in the OB association Mon OB2. These properties give us insight into the mass loss rates of O stars. They allow us to both check the validity of rotational mixing in massive stars and to better understand the effects of the ionizing flux and wind mechanical energy release on the surrounding interstellar medium and its influence on triggered star formation. Methods. We collected optical and UV spectra of the target stars that we analyzed by means of atmosphere models computed with the code CMFGEN. The spectra of binary stars were disentangled and the components studied separately. Results. All stars have an evolutionary age less than 5 million years, with the most massive stars being among the youngest. Nitrogen surface abundances show no clear relation with projected rotational velocities. Binaries and single stars show the same range of enrichment. This is attributed to the youth and/or wide separation of the binary systems in which the components have not (yet) experienced strong interaction. A clear trend toward greater enrichment in higher luminosity objects is observed, consistent with what evolutionary models with rotation predict for a population of O stars at any given age. We confirm the weakness of winds in late O dwarfs. In general, mass loss rates derived from UV lines are lower than mass loss rates obtained from Hα. The UV mass loss rates are even lower than the single-line driving limit in the latest type dwarfs. These issues are discussed in the context of the structure of massive stars winds. The evolutionary and spectroscopic masses are in agreement above 25 M , but the uncertainties are large. Below this threshold, the few late-type O stars studied here indicate that the mass discrepancy still seems to hold.

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Small-scale structure in the Rosette molecular cloud revealed by Herschel

Cited by 40 publications

References 24 publications

Young stellar clusters in the Rosette molecular cloud

Young stellar clusters in the Rosette molecular cloud

Synthetic observations of first hydrostatic cores in collapsing low-mass dense cores

A quantitative study of O stars in NGC 2244 and the Monoceros OB2 association

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