Properties of H II region populations in galaxies. II - The H II region luminosity function

Kennicutt, Robert C.; Edgar, B. K.; Hodge, P. W.

doi:10.1086/167147

Cited by 341 publications

(422 citation statements)

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“…Our best fit slope for IC 1613 gives a = −1.54 ± 0.1. This value is similar to the value (a = −1.6 ± 0.2) found by HLG, and is within the mean values found for a sample of irregular galaxies studied by Kennicutt et al (1989), Strobel et al (1991), Kingsburgh & McCall (1998) and Youngblood & Hunter (1999).…”

Section: The H II Region Luminosity Functionsupporting

confidence: 90%

Kinematics of the ionized gas in the Local Group irregular galaxy IC 1613

Valdez-Gutiérrez

Rosado

Георгиев

et al. 2001

A&A

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Abstract. We present Hα and [S ii] observations for the Local Group irregular galaxy IC 1613 using the PUMA scanning Fabry-Perot interferometer. Our goal is to analyze the kinematics of the ionized gas in the complex sample of superbubbles located in the whole extension of our field (10 ), which includes most of the optical emission of this galaxy, and to study the inter-relationship between young stellar associations and nebulae based on a previous study that we have made on the stellar associations of the central region of this galaxy. The ionized gas in this galaxy is distributed in classical H ii regions and in a series of superbubbles (also called giant shells) covering a large fraction of the optical extent of the galaxy. We present a catalog of kinematical properties of both the H ii regions of this galaxy and the superbubbles. We have also compared the kinematics of the ionized gas in H ii regions to search for possible dynamic differences between neutral and ionized gas.

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Section: The H II Region Luminosity Functionsupporting

confidence: 90%

Kinematics of the ionized gas in the Local Group irregular galaxy IC 1613

Valdez-Gutiérrez

Rosado

Георгиев

et al. 2001

A&A

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“…Of course the problem of identifying compact blobs against a background is a long studied one in astronomy and there has been considerable borrowing of well-established algorithms. In local galaxies, flux isophotes in Hα are often used to identify the numerous HII regions in nearby galaxies (Kennicutt, Edgar, & Hodge 1989); this has also been applied at high-redshift Wuyts et al 2012). More sophisticated techniques allow for a variable background, e.g.…”

Section: Properties Of Substructuresmentioning

confidence: 99%

The Dawes Review 1: Kinematic Studies of Star-Forming Galaxies Across Cosmic Time

Glazebrook

2013

Publ. Astron. Soc. Aust.

132

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The last seven years have seen an explosion in the number of Integral Field galaxy surveys, obtaining resolved 2D spectroscopy, especially at high-redshift. These have taken advantage of the mature capabilities of 8-10 m class telescopes and the development of associated technology such as AO. Surveys have leveraged both high spectroscopic resolution enabling internal velocity measurements and high spatial resolution from AO techniques and sites with excellent natural seeing. For the first time, we have been able to glimpse the kinematic state of matter in young, assembling starforming galaxies and learn detailed astrophysical information about the physical processes and compare their kinematic scaling relations with those in the local Universe. Observers have measured disc galaxy rotation, merger signatures, and turbulence-enhanced velocity dispersions of gas-rich discs. Theorists have interpreted kinematic signatures of galaxies in a variety of ways (rotation, merging, outflows, and feedback) and attempted to discuss evolution vs. theoretical models and relate it to the evolution in galaxy morphology. A key point that has emerged from this activity is that substantial fractions of high-redshift galaxies have regular kinematic morphologies despite irregular photometric morphologies and this is likely due to the presence of a large number of highly gas-rich discs. There has not yet been a review of this burgeoning topic. In this first Dawes review, I will discuss the extensive kinematic surveys that have been done and the physical models that have arisen for young galaxies at high-redshift.

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“…6, SF can occur in different locations within galaxy disks, namely in circumnuclear starbursts and in giant H H regions further out in the disks. Individual H n regions can be very powerful, like for example 30 Dor in the Large Magellanic Cloud, with L(Ha) -6.7X 10 39 ergs s -1 (Kennicutt et al 1989). Therefore, both circumnuclear starbursts and widespread SF activity must be considered as potential energy sources for diskhalo interactions.…”

Section: Which Spiral Galaxies Have Halos?mentioning

confidence: 99%

“…The gas disks are more relaxed, enabling the condensation of gas into giant molecular clouds (GMCs; Kennicutt and Chu 1988), which are the birthplaces of massive stars. Thus, only galaxies of type Sb or later host giant extragalactic H H regions (GEHRs; Kennicutt 1984;Kennicutt et al 1989). As noted above, the distribution of these GEHRs can vary (starburst vs. widespread SF).…”

Section: Why Only Late-type Spirals?mentioning

confidence: 99%

Gaseous Halos of Late-Type Spiral Galaxies

Dahlem¹

1997

PASP

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ABSTRACT. This article reviews the most recent observational results on disk-halo interactions in nearby galaxies. The implications of these results on our understanding of the structure of the interstellar medium (ISM) in our Galaxy and external spiral galaxies, with particular emphasis on the halo ISM, are discussed. Disk-halo interactions occur only above the brightest HII regions, which are found almost exclusively in late-type spirals and dwarf and irregular galaxies. Circumnuclear starbursts are the most energetic flavor of this phenomenon. The existence, the shapes, and the properties of gaseous halos depend on the level of energy input into the disk ISM per unit surface area, i.e., on the feedback of mass, momentum, and energy produced by vigorous star formation. Thus, current theoretical models of the ISM take into account that gaseous halos are natural extensions of disk ISMs and are heated by the winds and ionizing radiation of massive stars, and by the shock waves of Supernovae and their remnants. Observationally, this is reflected by the fact that all phases of the ISM known to exist in galaxy disks have also been detected in halos. Disk-halo interactions are a very effective way of redistributing energy, metals, and magnetic fields in galaxies and of expelling them into intergalactic space when outflows reach escape velocity. MOTIVATION AND OUTLINESpiral galaxies consist of three spatially and dynamically dinstinct components, namely bulge, disk, and halo. Of these, the central bulge consists primarily of old stars and has a low gas fraction. The disk and halo consist of stars plus gas, dust, and in many cases "dark matter." Here I want to concentrate on the interstellar medium (ISM) in the disks and halos of galaxies, with emphasis on late-type spirals. Massive dark halos will not be described (see, e.g., Ashman 1992; Holt and Bennett 1995). In the current context "latetype" stands for disk-dominated spirals with rather inconspicuous bulges (Hubble types Sb -Sdm). The ISM of elliptical galaxies and early-type spirals (S0-Sab) will also not be presented here (cf. Walsh et al. 1989;and Fabbiano 1989).Studies of the ISM contribute significantly to our understanding of the structure, kinematics, and evolution of galaxies. The level of star formation (SF), its spatial distribution, and its temporal changes depend strongly on the properties of the interstellar gas from which stars can form. Stars feed energy and metal-enriched matter back into the ambient medium via stellar winds and supernovae (SNe), thereby distributing processed material throughout the ISM. Hence, through this gas-star-gas cycle, the ISM becomes a mediator of SF.In Sec. 2, the different phases of the ISM in galaxies will be introduced, and Sec. 3 presents observations of the ISM in the Milky Way. Section 4 will show that the Galactic ISM is l A\\ correspondence should be directed to this address. not confined to the thin disk, but extends to high distances (z) above the plane, forming a gaseous halo. However, being located within the...

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Properties of H II region populations in galaxies. II - The H II region luminosity function

Cited by 341 publications

References 0 publications

Kinematics of the ionized gas in the Local Group irregular galaxy IC 1613

Kinematics of the ionized gas in the Local Group irregular galaxy IC 1613

The Dawes Review 1: Kinematic Studies of Star-Forming Galaxies Across Cosmic Time

Gaseous Halos of Late-Type Spiral Galaxies

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