On Measuring Nebular Chemical Abundances in Distant Galaxies Using Global Emission‐Line Spectra

Kobulnicky, Henry A.; Kennicutt, Robert C.; Pizagno, James

doi:10.1086/306987

Cited by 385 publications

(515 citation statements)

References 58 publications

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“…The correlation for small, metal-deficient galaxies is even better. These findings provide confidence that chemical properties do provide reliable information on the chemical content [9].…”

Section: Obtaining Nebular Chemical Abundances From Global Galaxy Spesupporting

confidence: 54%

Chemical constraints on the star formation history in high redshift galaxies

Kobulnicky¹,

Zaritsky²,

Kennicutt³

et al. 1999

The 9th Astrophysics Conference: After the Dark Ages, When Galaxies Were Young (The Universe at 2Self Cite

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Abstract.It is now possible to study the chemical properties of distant galaxies through emission line diagnostics which have long been used in local H II regions. Initial results from a sample of compact, narrow emission line galaxies at z = 0.2 to z = 0.5 show a range of metallicities from metal-poor like the SMC to super solar. The oxygen abundances correlate strongly with optical luminosity just like local galaxies. This suggests that the chemical production and retention in individual galaxies is determined predominantly by local characteristics, such as the integrated star formation activity and the depth of the gravitational potential rather than the cosmic star formation history. The ratios of specific elements like nitrogen-to-oxygen can constrain the evolutionary descendants of hi-z galaxies.

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“…The correlation for small, metal-deficient galaxies is even better. These findings provide confidence that chemical properties do provide reliable information on the chemical content [9].…”

Section: Obtaining Nebular Chemical Abundances From Global Galaxy Spesupporting
confidence: 54%

Chemical constraints on the star formation history in high redshift galaxies
Kobulnicky¹,
Zaritsky²,
Kennicutt³
et al. 1999
The 9th Astrophysics Conference: After the Dark Ages, When Galaxies Were Young (The Universe at 2Self Cite
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0
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“…1 are H  regions with oxygen abundances determined through the T e -method (compilation of data from Pilyugin 2000Pilyugin , 2001a. Figure 2 shows the two-dimensional theoretical calibration reported by Kobulnicky et al (1999). This calibration is based on the grid of the models of H  regions after McGaugh (1991).…”

Section: Oxygen Abundances In H II Regions: Model Fitting Versus T E mentioning
confidence: 99%

“…The grids of photoionization models are often used to establish the relation between strong oxygen line intensities and oxygen abundances (Edmunds & Pagel 1984;McCall et al 1985;Dopita & Evans 1986;Kobulnicky et al 1999;Kewley & Dopita 2002, among others). The relation (between strong oxygen line intensities and oxygen abundances) established on the basis of the grids of the photoionization models for H  regions will be referred to as theoretical or model calibration.…”

Section: Introductionmentioning
confidence: 99%

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Abundance determinations in H II regions
Pilyugin
¹

2003
A&A
60
3
58
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Abstract. The discrepancy between the oxygen abundances in high-metallicity H  regions determined through the T e -method (and/or through the corresponding "strong lines -oxygen abundance" calibration) and that determined through the model fitting (and/or through the corresponding "strong lines -oxygen abundance" calibration) is discussed. It is suggested to use the interstellar oxygen abundance in the solar vicinity, derived with very high precision from the high-resolution observations of the weak interstellar OIλ1356 absorption lines towards the stars, as a "Rosetta stone" to verify the validity of the oxygen abundances derived in H  regions with the T e -method at high abundances. The agreement between the value of the oxygen abundance at the solar galactocentric distance traced by the abundances derived in H  regions through the T e -method and that derived from the interstellar absorption lines towards the stars is strong evidence in favor of that i) the two-zone model for T e seems to be a realistic interpretation of the temperature structure within H  regions, and ii) the classic T e -method provides accurate oxygen abundances in H  regions. It has been concluded that the "strong lines -oxygen abundance" calibrations must be based on the H  regions with the oxygen abundances derived with the T e -method but not on the existing grids of the models for H  regions.
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“…• 8.6 > log O H + 12 ≥ 8.5 : As a second step, the average of the R 23 calibrations from and its parameterisation in Kobulnicky et al (1999) and Zaritsky et al (1994) can be used to estimate the abundance. Zaritsky et al (1994) give the relation:…”

Section: Optical Emission Linesmentioning
confidence: 99%

The Structure and Interaction History of Moderate Luminosity Mergers
Hüttemeister¹,
Manthey²
2006
Proc. IAU
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Interaction and merging are the two most important driving forces of galaxy evolution. In contrast to the well studied major mergers of two large gas-rich disk galaxies, which may lead to Ultraluminous Infrared Galaxies (ULIRGs, LFIR>1012 L⊙), mergers between galaxies of unequal mass or a spiral and an elliptical (S+E mergers) are still poorly understood. These moderate luminosity mergers typically have LFIR > 1011 L⊙. Here, we present the results of our multiwavelength study of a sample of such kind of mergers, including interferometric HI and single-dish CO observations, optical and near-infrared imaging as well as optical spectroscopy.

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On Measuring Nebular Chemical Abundances in Distant Galaxies Using Global Emission‐Line Spectra

Cited by 385 publications

References 58 publications

Chemical constraints on the star formation history in high redshift galaxies

Chemical constraints on the star formation history in high redshift galaxies

Abundance determinations in H II regions

The Structure and Interaction History of Moderate Luminosity Mergers

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