Oxygen abundances in nearby dwarf irregular galaxies

Skillman, Evan D.; Kennicutt, R. C.; Hodge, P. W.

doi:10.1086/168178

Cited by 510 publications

(616 citation statements)

References 0 publications

Supporting

Mentioning

555

Contrasting

Order By: Relevance

“…Direct spectroscopic observations of individual stars in more dIs are much needed. Skillman et al (1989) confirmed in a seminal paper a strong correlation between absolute magnitude and metallicity for local dIs in the sense that the fainter systems have lower metallicities. This was hinted already in some earlier papers: e.g.…”

Section: Chemical Abundances Of Dwarf Irregular Galaxiesmentioning

confidence: 75%

“…Richer and McCall (1995) made a spectroscopic study of planetary nebulae (PNe) in local dEs, including data from the literature on the Fornax dwarf. They also revisit the metallicity-luminosity relation for dwarf irregulars by Skillman et al (1989), using new determinations of the distance and metallicity. Their PN spectra have rather low signal to noise requiring empirical relations between [OIII]λ5007 and Hβ to estimate lower bounds on the oxygen abundances in the three dEs, from which they make a transformation to a "mean oxygen abundance".…”

Section: Chemical Abundances Of Local Group De/dsph Galaxiesmentioning

confidence: 99%

See 1 more Smart Citation

The most metal-poor galaxies

Kunth

Östlin

2000

Astronomy and Astrophysics Review

376

428

View full text Add to dashboard Cite

Metallicity is a key parameter that controls many aspects in the formation and evolution of stars and galaxies. In this review we focus on the metal deficient galaxies, in particular the most metal-poor ones, because they play a crucial rôle in the cosmic scenery. We first set the stage by discussing the difficult problem of defining a global metallicity and how this quantity can be measured for a given galaxy. The mechanisms that control the metallicity in a galaxy are reviewed in detail and involve many aspects of modern astrophysics: galaxy formation and evolution, massive star formation, stellar winds, chemical yields, outflows and inflows etc. Because metallicity roughly scales as the galactic mass, it is among the dwarfs that the most metalpoor galaxies are found. The core of our paper reviews the considerable progress made in our understanding of the properties and the physical processes that are at work in these objects. The question on how they are related and may evolve from one class of objects to another is discussed. While discussing metal-poor galaxies in general, we present a more detailed discussion of a few very metal-poor blue compact dwarf galaxies like IZw18. Although most of what is known relates to our local universe, we show that it pertains to our quest for primeval galaxies and is connected to the question of the origin of structure in the universe. We discuss what QSO absorption lines and known distant galaxies tell us already? We illustrate the importance of star-forming metal-poor galaxies for the determination of the primordial helium abundance, their use as distance indicator and discuss the possibility to detect nearly metal-free galaxies at high redshift from Lyα emission.

show abstract

Section: Chemical Abundances Of Dwarf Irregular Galaxiesmentioning

confidence: 75%

Section: Chemical Abundances Of Local Group De/dsph Galaxiesmentioning

confidence: 99%

The most metal-poor galaxies

Kunth

Östlin

2000

Astronomy and Astrophysics Review

376

428

View full text Add to dashboard Cite

show abstract

“…In H II regions, O/H varies from ∼3% solar to about half solar (using the solar oxygen abundance from Asplund [2]) for the most massive SFDGs [36]. As shown by Skillman et al [147], there is a correlation between luminosity and metallicity among local SFDGs. As more data are added though, the scatter increases, in particular if the luminosities are based on emission in the blue part of the spectrum, dominated by young stars [e.g 44].…”

Section: Chemical Abundancesmentioning

confidence: 96%

Star Forming Dwarf Galaxies

Bergvall¹

2011

Astrophysics and Space Science Proceedings

View full text Add to dashboard Cite

Star forming dwarf galaxies (SFDGs) have a high gas content and low metallicities, reminiscent of the basic entities in hierarchical galaxy formation scenarios. In the young universe they probably also played a major role in the cosmic reionization. Their abundant presence in the local volume and their youthful character make them ideal objects for detailed studies of the initial stellar mass function (IMF), fundamental star formation processes and its feedback to the interstellar medium. Occasionally we witness SFDGs involved in extreme starbursts, giving rise to strongly elevated production of super star clusters and global superwinds, mechanisms yet to be explored in more detail. SFDGs is the initial state of all dwarf galaxies and the relation to the environment provides us with a key to how different types of dwarf galaxies are emerging. In this review we will put the emphasis on the exotic starburst phase, as it seems less important for present day galaxy evolution but perhaps fundamental in the initial phase of galaxy formation.

show abstract

“…Galaxies are known to follow a mass-metallicity relationship, where the larger the stellar mass the higher the metallicity (e.g., Skillman et al 1989;Tremonti et al 2004;Gallazzi et al 2005). The relationship presents a significant scatter that has been recently found to be associated with the present SFR in the galaxy Lara-López et al 2010;Yates et al 2012;Pérez-Montero et al 2013;Andrews and Martini 2013;Zahid et al 2013).…”

Section: The Stellar Mass-metallicity-sfr Relationshipmentioning

confidence: 99%

Star formation sustained by gas accretion

Alméida

Elmegreen

Muñoz–Tuñón

et al. 2014

Astron Astrophys Rev

177

130

View full text Add to dashboard Cite

Numerical simulations predict that metal-poor gas accretion from the cosmic web fuels the formation of disk galaxies. This paper discusses how cosmic gas accretion controls star formation, and summarizes the physical properties expected for the cosmic gas accreted by galaxies. The paper also collects observational evidence for gas accretion sustaining star formation. It reviews evidence inferred from neutral and ionized hydrogen, as well as from stars. A number of properties characterizing large samples of star-forming galaxies can be explained by metal-poor gas accretion, in particular, the relationship among stellar mass, metallicity, and star-formation rate (the so-called fundamental metallicity relationship). They are put forward and analyzed. Theory predicts gas accretion to be particularly important at high redshift, so indications based on distant objects are reviewed, including the global star-formation history of the universe, and the gas around galaxies as inferred from absorption features in the spectra of background sources.

show abstract

Oxygen abundances in nearby dwarf irregular galaxies

Cited by 510 publications

References 0 publications

The most metal-poor galaxies

The most metal-poor galaxies

Star Forming Dwarf Galaxies

Star formation sustained by gas accretion

Contact Info

Product

Resources

About