Untitled

Pilyugin, V. S.; Chikisheva, G. E.; Valitov, R. B.; Sapozhnikov, Yu. E.

doi:10.1023/a:1021638231873

Cited by 5 publications

(4 citation statements)

References 1 publication

Supporting

Mentioning

Contrasting

Order By: Relevance

“…Shaver et al (1983) have found that their oxygen abundances are in agreement with the empirical R 23 -calibration. At the same time it has been found (Pilyugin 2000(Pilyugin , 2001a(Pilyugin ,b, 2003 that the oxygen abundances derived with the R 23 -calibration after Edmunds & Pagel (1984) involve a systematic error depending on the excitation parameter: the R 23 -method provides more or less realistic oxygen abundances in highexcitation H ii regions and yields an overestimated oxygen abundances in low-excitation H ii regions. Taking into Table 2.…”

Section: Shaver Et Al's Set Of H II Regionsmentioning

confidence: 97%

On the oxygen abundance in our Galaxy

Pilyugin

Ferrini²,

Shkvarun

2003

A&A

View full text Add to dashboard Cite

Abstract. The compilation of published spectra of Galactic H  regions with available diagnostic [OIII]λ4363 line information has been carried out. Our list contains 71 individual measurements of 13 H  regions in the range of galactocentric distances from 6.6 to 14.8 kpc. The oxygen abundances in all the H  regions were recomputed in the same way, using the classic T e -method. The oxygen abundance at the solar galactocentric distance traced by those H  regions is in agreement with the oxygen abundance in the interstellar medium in the solar vicinity derived with high precision from the interstellar absorption lines towards stars. The derived radial oxygen abundance distribution was compared with that for H  regions from the Shaver et al. (1983) sample which is the basis of many models for the chemical evolution of our Galaxy. It was found that the original Shaver et al.'s oxygen abundances are overestimated by 0.2-0.3 dex. Oxygen abundances in H  regions from the Shaver et al. sample have been redetermined with the recently suggested P-method. The radial distribution of oxygen abundances from the Shaver et al. sample redetermined with the P-method is in agreement with our radial distribution of (O/H) Te abundances.

show abstract

Section: Shaver Et Al's Set Of H II Regionsmentioning

confidence: 97%

On the oxygen abundance in our Galaxy

Pilyugin

Ferrini²,

Shkvarun

2003

A&A

View full text Add to dashboard Cite

show abstract

“…Lee et al 2003), late-type galaxies (e.g. Pilyugin & Ferrini 2000) and ellipticals (e.g. Brodie & Huchra 1991).…”

Section: U M I N O S I T Y -M E Ta L L I C I T Y R E L At I O Nmentioning

confidence: 99%

Oxygen abundances and chemical evolution in low surface brightness galaxies

Naray

McGaugh

Blok

2004

Monthly Notices of the Royal Astronomical Society

View full text Add to dashboard Cite

We report the oxygen abundances of the H ii regions of a sample of low surface brightness (LSB) galaxies. We provide analytic functions describing McGaugh's calibration of the R23 method. We use this and the equivalent width (EW) method to determine oxygen abundances, and also make direct estimates in a few cases where the temperature‐sensitive [O iii]λ4363 line is available. We find LSB galaxies to be metal‐poor, consistent with the luminosity–metallicity (L–Z) relation of other galaxies. The large gas mass fractions of these objects provide an interesting test of chemical evolution models. We find no obvious deviation from the closed‐box model of galactic chemical evolution. Based on our abundance and gas mass fraction measurements, we infer that LSB galaxies are not fundamentally different from other galaxy types but are perhaps at an early stage of evolution.

show abstract

“…This implies that there is a "spiral versus irregular dichotomy" in the sense that there is a sudden change from spiral (radial abundance gradients are usually present) to irregular galaxies (typically no gradients). However, other properties (e.g., gas fraction, global metallicity) vary smoothly in transition from spirals to irregulars (Zaritsky et al 1994;Pilyugin & Ferrini 2000;Garnett 2002;Pilyugin et al 2007, among others).…”

Section: Introductionmentioning

confidence: 99%

On the radial abundance gradients in discs of irregular galaxies

Pilyugin¹,

Grebel²,

Zinchenko³

2015

Monthly Notices of the Royal Astronomical Society

View full text Add to dashboard Cite

We determine the radial abundance distributions across the disks of fourteen irregular galaxies of the types Sm and Im (morphological T types T = 9 and T =10) as traced by their H ii regions. The oxygen and nitrogen abundances in H ii regions are estimated through the T e method or/and with the counterpart method (C method). Moreover, we examine the correspondence between the radial abundance gradient and the surface brightness profile. We find that irregular galaxies with a flat inner profile (flat or outwardly increasing surface brightness in the central region) show shallow (if any) radial abundance gradients. On the other hand, irregular galaxies with a steep inner profile (with or without a bulge or central star cluster) usually show rather steep radial abundance gradients. This is in contrast to the widely held belief that irregular galaxies do not usually show a radial abundance gradient.

show abstract

Untitled

Cited by 5 publications

References 1 publication

On the oxygen abundance in our Galaxy

On the oxygen abundance in our Galaxy

Oxygen abundances and chemical evolution in low surface brightness galaxies

On the radial abundance gradients in discs of irregular galaxies

Contact Info

Product

Resources

About