Detecting stellar-wind bubbles through infrared arcs in H ii regions

Mackey, Jonathan; Haworth, Thomas J.; Gvaramadze, V. V.; Mohamed, S.; Langer, N.; Harries, Tim J.

doi:10.1051/0004-6361/201527569

Cited by 53 publications

(55 citation statements)

References 137 publications

Supporting

Mentioning

Contrasting

Order By: Relevance

“…Often, the detailed microphysical state of the system is determined in a post-processing step applied to a dynamical simulation with a more approximate model for the chemistry and for the thermal behaviour. In reality the dynamics, microphysics and radiative transfer (and magnetic fields) are all interlinked and modelling this inter-dependency is at the frontier of modern capabilities (Haworth et al, 2016). 3.…”

Section: Types Of Synthetic Observationmentioning

confidence: 99%

Synthetic observations of star formation and the interstellar medium

Haworth

Glover

Koepferl

et al. 2018

New Astronomy Reviews

Self Cite

View full text Add to dashboard Cite

Synthetic observations are playing an increasingly important role across astrophysics, both for interpreting real observations and also for making meaningful predictions from models. In this review, we provide an overview of methods and tools used for generating, manipulating and analysing synthetic observations and their application to problems involving star formation and the interstellar medium. We also discuss some possible directions for future research using synthetic observations.

show abstract

Section: Types Of Synthetic Observationmentioning

confidence: 99%

Synthetic observations of star formation and the interstellar medium

Haworth

Glover

Koepferl

et al. 2018

New Astronomy Reviews

Self Cite

View full text Add to dashboard Cite

show abstract

“…A bow-shock feature is also clearly seen at WISE-22 µm and Herschel-70 µm, underlining the asymmetry of the bubble. This feature can be produced by a runaway star moving at high relative velocity (Gvaramadze et al 2011) or by a stellar wind within the H ii region associated with such a rapidly moving star (Mackey et al 2016). Because the WISE-22 µm arc is well inside the Spitzer-8 µm bubble we favour the second hypothesis.…”

Section: Distance To Particular Regionsmentioning

confidence: 99%

NGC 6334 and NGC 6357

Russeil

Adami

Bouret

et al. 2017

A&A

View full text Add to dashboard Cite

Aims. The formation of high-mass stars is still debated. For this reason, several projects such as Herschel-HOBYS are focussed on the study of the earliest phases of massive star formation. As a result, massive star-forming complexes such as NGC 6334 and NGC 6357 have been observed in the far-infrared to study their massive dense cores where massive stars are expected to form. However, to better characterise the environments of these cores we need to understand the previous massive star formation history. To better characterise the environment of these massive dense cores we study the previous high-mass star formation and how these stars act on their environments. Methods. This study is based on the spectral classification of the OB stars identified towards NGC 6334 and NGC 6357 with spectra taken with the AAOmega spectrograph on the Anglo-Australian Telescope (AAT). From the subsequent spectral classification of 109 stars across these regions we were able to evaluate the following: distance, age, mass, global star-forming efficiency (SFE), and star formation rate (SFR) of the regions. The physical conditions of the ionised gas for both complexes was also derived. Results. We confirm that NGC 6334 and NGC 6357 belong to the Saggitarius-Carina arm which, in this direction, extends from 1 kpc to 2.2 kpc. From the location of the stars in Hertzprung-Russell diagram we show that stars older than ∼10 Myr are broadly spread across these complexes, while younger stars are mainly located in the H ii regions and stellar clusters. Our data also suggests that some of the young stars can be considered runaway stars. We evaluate a SFE of 0.019 +0.008 −0.007 and 0.021 +0.004 −0.003 and a SFR of 1.1 × 10 3 ± 300 M Myr −1 and 1.7 × 10 3 ± 400 M Myr −1 for NGC 6334 and NGC 6357, respectively. We note that 29 OB stars have X-ray counterparts, most of them belonging to NGC 6357. This suggests that molecular clouds in NGC 6357 are more impacted by X-ray flux and stellar winds than in NGC 6334. Finally, from the analysis of nebular lines (Hα, [NII], and [SII]) from spectra from several regions of ionised gas, we confirm that the filaments in NGC 6357 are shock heated.

show abstract

“…RCW 120 is a well-studied Galactic H II region because of its ovoid shape and its relatively close distance (1.34 kpc, Russeil 2003;Zavagno et al 2007). Thanks to these advantages, this region has received a lot of attention from observers and simulations, and has been studied in several papers (Zavagno et al 2007(Zavagno et al , 2010(Zavagno et al , 2020Deharveng et al 2009;Anderson et al 2012Anderson et al , 2015Tremblin et al 2014;Kirsanova et al 2014Kirsanova et al , 2019Torii et al 2015;Walch et al 2015;Mackey et al 2016;Figueira et al 2017Figueira et al , 2018Marsh & Whitworth 2019). Figueira et al (2017) showed that two clumps observed at millimeter wavelength host different kinds of sources with respect to their evolutionary stage.…”

Section: Introductionmentioning

confidence: 99%

APEX CO observations towards the photodissociation region of RCW 120

Figueira

Zavagno

Bronfman

et al. 2020

A&A

View full text Add to dashboard Cite

Context. The edges of ionized (H II) regions are important sites for the formation of (high-mass) stars. Indeed, at least 30% of the Galactic high-mass-star formation is observed there. The radiative and compressive impact of the H II region could induce star formation at the border following different mechanisms such as the collect and collapse or the radiation-driven implosion (RDI) models and change their properties. Aims. We aim to study the properties of two zones located in the photo dissociation region (PDR) of the Galactic H II region RCW 120 and discuss them as a function of the physical conditions and young star contents found in both clumps. Methods. Using the APEX telescope, we mapped two regions of size 1.5′ × 1.5′ toward the most massive clump of RCW 120 hosting young massive sources and toward a clump showing a protrusion inside the H II region and hosting more evolved low-mass sources. The 12CO (J = 3−2), 13CO (J = 3−2) and C18O (J = 3−2) lines observed, together with Herschel data, are used to derive the properties and dynamics of these clumps. We discuss their relation with the hosted star formation. Results. Assuming local thermodynamic equilibrium, the increase of velocity dispersion and Tex are found toward the center of the maps, where star-formation is observed with Herschel. Furthermore, both regions show supersonic Mach numbers (7 and 17 in average). No substantial information has been gathered about the impact of far ultraviolet radiation on C18O photodissociation at the edges of RCW 120. The fragmentation time needed for CC to be at work is equivalent to the dynamical age of RCW 120 and the properties of region B are in agreement with bright-rimmed clouds. Conclusions. Although conclusions from this fragmentation model should be taken with caution, it strengthens the fact that, together with evidence of compression, CC might be at work at the edges of RCW 120. Additionally, the clump located at the eastern part of the PDR is a good candidate pre-existing clump where star-formation may be induced by the RDI mechanism.

show abstract

Detecting stellar-wind bubbles through infrared arcs in H ii regions

Cited by 53 publications

References 137 publications

Synthetic observations of star formation and the interstellar medium

Synthetic observations of star formation and the interstellar medium

NGC 6334 and NGC 6357

APEX CO observations towards the photodissociation region of RCW 120

Contact Info

Product

Resources

About