Oxygen abundances in diffuse ellipticals and the metallicity-luminosity relations for dwarf galaxies

Richer, M. G.; McCall, Marshall L.

doi:10.1086/175727

Cited by 249 publications

(403 citation statements)

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“…In summary, many Local Group dEs are very metal poor, which probably is related to their intrinsic faintness. Taking the average offset between [Fe/H] and [O/H] into account, Mateo (1998) concludes that dEs appear to be more metal rich in view of their luminosities, in agreement with Richer and McCall (1995).…”

Section: Chemical Abundances Of Local Group De/dsph Galaxiessupporting

confidence: 60%

“…7.1. More recent work in this area include that of Richer and McCall (1995) and Hidalgo-Gámez and Olofsson (1998). The comparison of dIs and dEs is not straightforward, as will be discussed in next section, since different chemical elements are sampled in general.…”

Section: Chemical Abundances Of Dwarf Irregular Galaxiesmentioning

confidence: 99%

“…If there is no classification in the literature, but published images are available, we classified the galaxies according to this scheme. The solid line shows the M B − Z relation for dIs by Richer and McCall (1995), while the short and long dashed lines shows the relation for dEs (see caption).…”

Section: Global Relations and Evolutionary Links 71 The Metallicity-mentioning

confidence: 99%

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The most metal-poor galaxies

Kunth

Östlin

2000

Astronomy and Astrophysics Review

381

428

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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.

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Section: Chemical Abundances Of Local Group De/dsph Galaxiessupporting

confidence: 60%

Section: Chemical Abundances Of Dwarf Irregular Galaxiesmentioning

confidence: 99%

Section: Global Relations and Evolutionary Links 71 The Metallicity-mentioning

confidence: 99%

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The most metal-poor galaxies

Kunth

Östlin

2000

Astronomy and Astrophysics Review

381

428

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“…We compare our detections with other literature surveys in NGC 205 also interested in emission-line populations, in particular PNe: Ford et al (1973), Ciardullo et al (1989), Richer & McCall (1995), Corradi et al (2005), Merrett et al (2006) and Richer & McCall (2008). All these surveys studied this galaxy using narrow-band imaging and/or optical spectroscopy.…”

Section: The Systems' Discoverymentioning

confidence: 73%

“…All these surveys studied this galaxy using narrow-band imaging and/or optical spectroscopy. From these works, only the spectroscopic survey of McCall (1995 and could had found out our symbiotics. However, targets in Table 1 are not included among theirs.…”

Section: The Systems' Discoverymentioning

confidence: 99%

Discovery of true, likely and possible symbiotic stars in the dwarf spheroidal NGC 205★

Gonçalves

Magrini

Rosa

et al. 2014

Monthly Notices of the Royal Astronomical Society

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In this paper we discuss the photometric and spectroscopic observations of newly discovered (symbiotic) systems in the dwarf spheroidal galaxy NGC 205. The Gemini Multi-Object Spectrograph on-off band [O iii] 5007Å emission imaging highlighted several [O iii] line emitters, for which optical spectra were then obtained (Gonçalves et al. 2014). The detailed study of the spectra of three objects allow us to identify them as true, likely and possible symbiotic systems (SySts), the first ones discovered in this galaxy. SySt-1 is unambiguously classified as a symbiotic star, because of the presence of unique emission lines which belong only to symbiotic spectra, the well known O vi Raman scattered lines. SySt-2 is only possibly a SySt because the Ne vii (Gutierrez-Moreno et al. 1995). It is worth mentioning that at least another two confirmed symbiotics, one of the Local Group dwarf spheroidal IC 10 and the other of the Galaxy, are also misplaced in this diagram.

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A Panchromatic View of Galaxies

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Oxygen abundances in diffuse ellipticals and the metallicity-luminosity relations for dwarf galaxies

Cited by 249 publications

References 0 publications

The most metal-poor galaxies

The most metal-poor galaxies

Discovery of true, likely and possible symbiotic stars in the dwarf spheroidal NGC 205★

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