The Bubbling Galactic Disk

Churchwell, E.; Povich, Matthew S.; Allen, David A.; Taylor, M. Susan; Meade, M. R.; Babler, B.; Indebetouw, R.; Watson, C.; Whitney, B. A.; Wolfire, M. G.; Bania, T. M.; Benjamin, Robert A.; Clemens, D. P.; Cohen, Martin; Cyganowski, C. J.; Jackson, James M.; Kobulnicky, Henry A.; Mathis, J. S.; Mercer, E. P.; Stolovy, S.; Uzpen, B.; Watson, Dorothy; Wolff, Michael

doi:10.1086/507015

Cited by 517 publications

(855 citation statements)

References 35 publications

(40 reference statements)

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“…However, this does not mean that processes we discuss operate on this spatial scale. What we observe is actually a merged result of dust evolution in many separate regions, which are, probably, observed in our Galaxy as infrared bubbles (Churchwell et al 2006). A correlation between the F8/F24 ratio and metallicity for our entire sample is presented in Fig.…”

Section: Relations Between Various Parameterssupporting

confidence: 54%

Optical and infrared emission of H ii complexes as a clue to the PAH life cycle

Khramtsova¹,

Wiebe²,

Lozinskaya³

et al. 2014

Monthly Notices of the Royal Astronomical Society

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We present an analysis of optical spectroscopy and infrared aperture photometry of more than 100 H ii complexes in nine galaxies. Spectra obtained with the 6-m telescope of SAO RAS are used along with archival data from Spitzer and several ground-based telescopes to infer a strength of polycyclic aromatic hydrocarbon (PAH) emission, age, properties of the UV radiation field, and metallicity of studied H ii complexes. Physical properties (age, radiation field parameters, metallicity) are related to the F 8 /F 24 ratio used as a proxy for the PAH abundance in order to reveal factors that may influence the PAH evolution in H ii complexes. The well-known correlation between the F 8 /F 24 ratio and metallicity is confirmed in the studied complexes. The infrared flux ratio also correlates with the [O iii]λ5007/Hβ ratio which is often considered as an indicator of the radiation field hardness, but this correlation seems to be a mere reflection of a correlation between [O iii]λ5007/Hβ and metallicity. In separate metallicity bins, the F 8 /F 24 ratio is found to correlate with an age of an H ii complex, which is estimated from the equivalent width of Hβ line. The correlation is positive for low metallicity complexes and negative for high metallicity complexes. Analysing various mechanisms of PAH formation and destruction in the context of found correlations, we suggest that PAH abundance is likely altered by the UV radiation within H ii complexes, but this is not necessarily due to their destruction. If PAHs can also form in H ii complexes due to some processes like aromatisation, photodestruction, shattering and sputtering of very small grains, the net F 8 /F 24 ratio is determined by a balance between all these processes that can be different at different metallicities.

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Section: Relations Between Various Parameterssupporting

confidence: 54%

Optical and infrared emission of H ii complexes as a clue to the PAH life cycle

Khramtsova¹,

Wiebe²,

Lozinskaya³

et al. 2014

Monthly Notices of the Royal Astronomical Society

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“…With GLIMPSE, Churchwell et al (2006) detected 322 partial and closed rings. They argue that the bubbles are primarily formed by hot young stars in massive star-formation regions and about 13% enclose known star clusters.…”

Section: Introductionmentioning

confidence: 99%

First stars of theρOphiuchi dark cloud

Pillitteri

Wolk

Chen

et al. 2016

A&A

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Star formation in molecular clouds can be triggered by the dynamical action of winds from massive stars. Furthermore, X-ray and UV fluxes from massive stars can influence the life time of surrounding circumstellar disks. We present the results of a 53 ks XMMNewton observation centered on the ρ Ophiuchi A+B binary system. ρ Ophiuchi lies in the center of a ring of dust, likely formed by the action of its winds. This region is different from the dense core of the cloud (L1688 Core F) where star formation is at work. X-rays are detected from ρ Ophiuchi as well as a group of surrounding X-ray sources. We detected 89 X-ray sources, 47 of them have at least one counterpart in 2MASS+All-WISE catalogs. Based on IR and X-ray properties, we can distinguish between young stellar objects (YSOs) belonging to the cloud and background objects. Among the cloud members, we detect three debris-disk objects and 22 disk-less − Class III young stars. We show that these stars have ages in 5−10 Myr, and are significantly older than the YSOs in L1688. We speculate that they are the result of an early burst of star formation in the cloud. An X-ray energy of ≥5 × 10 44 erg has been injected into the surrounding medium over the past 5 Myr, we discuss the effects of such energy budget in relation to the cloud properties and dynamics.

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“…Churchwell et al 2006). Given the small separations in GCs, they should soon unite and thus form a superbubble (e.g.…”

Section: Introductionmentioning

confidence: 99%

Superbubble dynamics in globular cluster infancy

Krause¹,

Charbonnel²,

Decressin³

et al. 2012

A&A

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The picture of the early evolution of globular clusters has been significantly revised in recent years. Current scenarios require at least two generations of stars of which the first generation (1G), and therefore also the protocluster cloud, has been much more massive than the currently predominating second generation (2G). Fast gas expulsion is thought to unbind the majority of the 1G stars. Gas expulsion is also mandatory to remove metal-enriched supernova ejecta, which are not found in the 2G stars. It has long been thought that the supernovae themselves are the agent of the gas expulsion, based on crude energetics arguments. Here, we assume that gas expulsion happens via the formation of a superbubble, and describe the kinematics by a thin-shell model. We find that supernovadriven shells are destroyed by the Rayleigh-Taylor instability before they reach escape speed for all but perhaps the least massive and most extended clusters. More power is required to expel the gas, which might plausibly be provided by a coherent onset of accretion onto the stellar remnants. The resulting kpc-sized bubbles might be observable in Faraday rotation maps with the planned Square Kilometre Array radio telescope against polarised background radio lobes if a globular cluster would happen to form in front of such a radio lobe.

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The Bubbling Galactic Disk

Cited by 517 publications

References 35 publications

Optical and infrared emission of H ii complexes as a clue to the PAH life cycle

Optical and infrared emission of H ii complexes as a clue to the PAH life cycle

First stars of theρOphiuchi dark cloud

Superbubble dynamics in globular cluster infancy

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