Interstellar Abundance Gradients In NGC 2403: Comparison To M33

Garnett, D. R.; Shields, G. A.; Skillman, Evan D.; Sagan, Sławomir; Dufour, R. J.

doi:10.1086/304775

Cited by 276 publications

(374 citation statements)

References 73 publications

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“…As suggested by Combes (1998), a ''universal'' slope per disk scale length might be explained by the viscous disk models of Lin & Pringle (1987), although model predictions are not conclusive as of yet. The Garnett et al (1997) compilation of O/H gradients shows a similar signature, where abundance gradients in dex per kpc are steeper and exhibit greater scatter for lower luminosity disks, but this trend goes away when gradients are expressed in dex/h. Note, however, that the abundance gradients compiled in van Zee et al (1998) and reported in PB00 do show a clear increase with magnitude when plotted as dex/h, thus thwarting the interpretation of a universal abundance gradient per scale length.…”

Section: Discussionmentioning

confidence: 81%

Structure of Disk‐dominated Galaxies. II. Color Gradients and Stellar Population Models

MacArthur

Courteau

Bell

et al. 2004

ASTROPHYS J SUPPL S

210

260

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We investigate optical and near-IR color gradients in a sample of 172 low-inclination galaxies spanning Hubble types S0-Irr. The colors are compared with stellar population synthesis models from which luminosityweighted average ages and metallicities are determined. We explore the effects of different underlying star formation histories and additional bursts of star formation. Our results are robust in a relative sense under the assumption that our galaxies shared a similar underlying star formation history and that no bursts involving more than $10% of the galaxy mass have occurred in the past 1-2 Gyr. Because the observed gradients show radial structure, we measure ''inner'' and ''outer'' disk age and metallicity gradients. Trends in age and metallicity and their gradients are explored as a function of Hubble type, rotational velocity, total near-IR galaxy magnitude, central surface brightness, and scale length. We find strong correlations in age and metallicity with Hubble type, rotational velocity, total magnitude, and central surface brightness in the sense that earlier-type, faster rotating, more luminous, and higher surface brightness galaxies are older and more metal-rich, suggesting an early and more rapid star formation history for these galaxies. The increasing trends with rotational velocity and total magnitude level off for V rot k120 km s À1 and M K P À23 mag, respectively. This effect is stronger for metallicity (than age), which could reflect a threshold potential above which all metals are retained and thus metallicity saturates at the yield. Outer disk gradients are found to be weaker than the inner gradients as expected for a slower variation of the potential and surface brightness in the outer parts. We find that stronger age gradients are associated with weaker metallicity gradients. Trends in gradients with galaxy parameters are compared with model predictions: these trends do not agree with predictions of semianalytic models of hierarchical galaxy formation, possibly owing to the effect of bar-induced radial flows. The observed trends are in agreement with chemo-spectrophotometric models of spiral galaxy evolution based on CDM-motivated scaling laws but none of the hierarchical merging characteristics, implying a strong dependence of the star formation history of spiral galaxies on the galaxy potential and halo spin parameter.

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Section: Discussionmentioning

confidence: 81%

Structure of Disk‐dominated Galaxies. II. Color Gradients and Stellar Population Models

MacArthur

Courteau

Bell

et al. 2004

ASTROPHYS J SUPPL S

210

260

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“…Inspection of Fig. 3 shows that there is no possibility of large central (intersect) oxygen abundances (as large as 12 + log O/H ∼ 9.50 and higher) derived with theoretical (model) calibrations (Zaritsky et al 1994;Garnett et al 1997). On the contrary, the low central oxygen abundances predicted by the empirical calibration (Pilyugin et al 2002) fit this picture well.…”

Section: Verification Of the Validity Of The T E -Methods At High Metamentioning

confidence: 83%

Abundance determinations in H II regions

Pilyugin

2003

A&A

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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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“…This is the regime where nitrogen is predominantly secondary (Alloin et al 1979;Considère et al 2000;Pettini et al 2008). The fact that the N/O ratio is relatively flat at low metallicities indicates that production of nitrogen is dominated by primary processes at low metallicities, and by secondary processes at high metallicities (Garnett et al 1997;Ferguson et al 1998;Henry & Worthey 1999).…”

Section: Nitrogen and Oxygen Abundancesmentioning

confidence: 99%

Study of star-forming galaxies in SDSS up to redshift 0.4

Lara-López¹,

Cepa

Bongiovanni³

et al. 2009

A&A

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Context. The chemical composition of the gas in galaxies over cosmic time provides a very important tool for understanding galaxy evolution. Although there are many studies at high redshift, they are rather scarce at lower redshifts. However, low redshift studies can provide important clues about the evolution of galaxies, furnishing the required link between the local and high redshift universe. In this work, we focus on the metallicity of the gas of star-forming galaxies at low redshift, looking for signs of chemical evolution.Aims. We aim to analyze the metallicity contents star-forming galaxies of similar luminosities and masses at different redshifts. With this purpose, we present a study of the metallicity of relatively massive (log(M star /M ) 10.5) star forming galaxies from SDSS-DR5 (Sloan Digital Sky Survey-data release 5), using different redshift intervals from 0.04 to 0.4. Methods. We used data processed with the STARLIGHT spectral synthesis code, correcting the fluxes for dust extinction, estimating metallicities using the R 23 method, and segregating the samples with respect to the value of the [N ii] λ6583/[O ii] λ3727 line ratio in order to break the R 23 degeneracy selecting the upper branch. We analyze the luminosity and mass-metallicity relations, and the effect of the Sloan fiber diameter looking for possible biases. Results. By dividing our redshift samples in intervals of similar magnitude and comparing them, significant signs of metallicity evolution are found. Metallicity correlates inversely with redshift: from redshift 0 to 0.4 a decrement of ∼0.1 dex in 12 + log(O/H) is found.

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Interstellar Abundance Gradients In NGC 2403: Comparison To M33

Cited by 276 publications

References 73 publications

Structure of Disk‐dominated Galaxies. II. Color Gradients and Stellar Population Models

Structure of Disk‐dominated Galaxies. II. Color Gradients and Stellar Population Models

Abundance determinations in H II regions

Study of star-forming galaxies in SDSS up to redshift 0.4

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