Feedback in the Antennae Galaxies (NGC 4038/9). I. High‐Resolution Infrared Spectroscopy of Winds from Super Star Clusters

Gilbert, Andrea M.; Graham, James R.

doi:10.1086/520910

Cited by 68 publications

(112 citation statements)

References 103 publications

(267 reference statements)

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“…Silich et al (2010) determined the heating efficiency of 10 young massive clusters in M82 galaxy from their corresponding HII regions radii and found η he 10%. Widths of recombination lines associated with super star clusters in the Antennae galaxies observed by Gilbert & Graham (2007) also suggest that η he 10%. Tenorio-Tagle et al (2016) argue that the heating efficiency is effectively low if majority of massive stars end up as interacting binaries resulting in much lower stellar wind velocities.…”

Section: Introductionmentioning

confidence: 80%

The Formation of Secondary Stellar Generations in Massive Young Star Clusters From Rapidly Cooling Shocked Stellar Winds

Wünsch

Palouš

Tenorio-Tagle

et al. 2017

ApJ

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We study a model of rapidly cooling shocked stellar winds in young massive clusters and estimate the circumstances under which secondary star formation, out of the reinserted winds from a first stellar generation (1G), is possible. We have used two implementations of the model: a highly idealized computationally inexpensive spherically symmetric semi-analytic model, and a complex three-dimensional radiation-hydrodynamic simulations, and they are in a good mutual agreement. The results confirm our previous findings that in a cluster with 1G mass 10 7 M and half-mass radius 2.38 pc, the shocked stellar winds become thermally unstable, collapse into dense gaseous structures that partially accumulate inside the cluster, self-shield against ionizing stellar radiation and form the second generation (2G) of stars. We have used the semi-analytic model to explore a subset of the parameter space covering a wide range of the observationally poorly constrained parameters: the heating efficiency, η he , and the mass loading, η ml . The results show that the fraction of the 1G stellar winds accumulating inside the cluster can be larger than 50% if η he 10% which is suggested by the observations. Furthermore, for low η he , the model provides a self-consistent mechanism predicting 2G stars forming only in the central zones of the cluster. Finally, we have calculated the accumulated warm gas emission in the H30α recombination line, analyzed its velocity profile and estimated its intensity for super star clusters in interacting galaxies NGC4038/9 (Antennae) showing that the warm gas should be detectable with ALMA.

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Section: Introductionmentioning

confidence: 80%

The Formation of Secondary Stellar Generations in Massive Young Star Clusters From Rapidly Cooling Shocked Stellar Winds

Wünsch

Palouš

Tenorio-Tagle

et al. 2017

ApJ

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“…In fact, Gilbert & Graham (2007) conclude that the SSCs in the Antennae constitute a new class of massive H ii regions that is distinct from the Galactic and typical extragalactic population. In this paper, we examine the size-density relation in extragalactic H ii regions, and explore several mechanisms which have been proposed to explain it, including clumpiness, dust extinction, and stellar content.…”

Section: Article Published By Edp Sciencesmentioning

confidence: 94%

“…In this paper, we examine the size-density relation in extragalactic H ii regions, and explore several mechanisms which have been proposed to explain it, including clumpiness, dust extinction, and stellar content. In particular, we focus on the H ii regions in Blue Compact Dwarf galaxies (BCDs); following Gilbert & Graham (2007), we shall refer to such regions as Emission-Line Clusters (ELCs). In fact, most of the current star formation in many BCDs occurs in such ELCs, rather than in the underlying diffuse component.…”

Section: Article Published By Edp Sciencesmentioning

confidence: 99%

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The size-density relation of extragalactic H II regions

Hunt¹,

Hirashita²

2009

A&A

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Aims. We investigate the size-density relation in extragalactic H ii regions, with the aim of understanding the role of dust and different physical conditions in the ionized medium.Methods. First, we compiled several observational data sets for Galactic and extragalactic H ii regions and confirm that extragalactic H ii regions follow the same size (D)-density (n) relation as Galactic ones (n ∝ D −1 ), rather than a relation with constant luminosity (n ∝ D −1.5 ). Motivated by the inability of static models to explain this, we then modelled the evolution of the size-density relation of H ii regions by considering their star formation history, the effects of dust, and pressure-driven expansion. The results are compared with our sample data whose size and density span roughly six orders of magnitude. Results. The extragalactic samples cannot be understood as an evolutionary sequence with a single initial condition. Thus, the sizedensity relation does not result from an evolutionary sequence of H ii regions but rather reflects a sequence with different initial gas densities ("density hierarchy"). We also find that the size of many H ii regions is limited by dust absorption of ionizing photons, rather than consumption by ionizing neutral hydrogen. Dust extinction of ionizing photons is particularly severe over the entire lifetime of compact H ii regions with typical gas densities of > ∼ 10 3 cm −3 . Hence, as long as the number of ionizing photons is used to trace massive star formation, much star-formation activity could be missed. Such compact dense environments, the ones most profoundly obscured by dust, have properties similar to "maximum-intensity starbursts". This implies that submillimeter and infrared wavelengths may be necessary to accurately assess star formation in these extreme conditions both locally and at high redshift.

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“…In reality, at ages 3 Myr, the surrounding neutral gas and dust may strongly obscure optical and UV emission from the starburst (e.g. Kobulnicky & Johnson 1999;Gilbert & Graham 2007;Whitmore et al 2014;Sokal et al 2015), before feedback clears away some of this natal material. Therefore, the peak C iii] emission may occur instead at the slightly older ages corresponding to the Wolf-Rayet phase, consistent with the C iii] detections at low redshift (Rigby et al 2015).…”

Section: Effect Of Ionizing Sedmentioning

confidence: 99%

PHOTOIONIZATION MODELS FOR THE SEMI-FORBIDDEN C iii] 1909 EMISSION IN STAR-FORMING GALAXIES

Jaskot

Ravindranath

2016

ApJ

105

168

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The increasing neutrality of the intergalactic medium at z > 6 suppresses Lyα emission, and spectroscopic confirmation of galaxy redshifts requires detecting alternative UV lines. The strong [C iii] λ1907+C iii] λ1909 doublet frequently observed in low-metallicity, actively star-forming galaxies is a promising emission feature. We present CLOUDY photoionization model predictions for C iii] equivalent widths (EWs) and line ratios as a function of starburst age, metallicity, and ionization parameter. Our models include a range of C/O abundances, dust content, and gas density. We also examine the effects of varying the nebular geometry and optical depth. Only the stellar models that incorporate binary interaction effects reproduce the highest observed C iii] EWs. The spectral energy distributions from the binary stellar population models also generate observable C iii] over a longer timescale relative to single-star models. We show that diagnostics using C iii] and nebular He ii λ1640 can separate star-forming regions from shock-ionized gas. We also find that density-bounded systems should exhibit weaker C iii] EWs at a given ionization parameter, and C iii] EWs could therefore select candidate Lyman continuum-leaking systems. In almost all models, C iii] is the next strongest line at < 2700Å after Lyα, and C iii] reaches detectable levels for a wide range of conditions at low metallicity. C iii] may therefore serve as an important diagnostic for characterizing galaxies at z > 6.

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Feedback in the Antennae Galaxies (NGC 4038/9). I. High‐Resolution Infrared Spectroscopy of Winds from Super Star Clusters

Cited by 68 publications

References 103 publications

The Formation of Secondary Stellar Generations in Massive Young Star Clusters From Rapidly Cooling Shocked Stellar Winds

The Formation of Secondary Stellar Generations in Massive Young Star Clusters From Rapidly Cooling Shocked Stellar Winds

The size-density relation of extragalactic H II regions

PHOTOIONIZATION MODELS FOR THE SEMI-FORBIDDEN C iii] 1909 EMISSION IN STAR-FORMING GALAXIES

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