Metallicity gradients in early-type galaxies

Carollo, C. M.; Danziger, I. J.; Buson, L. M.

doi:10.1093/mnras/265.3.553

Cited by 227 publications

(351 citation statements)

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“…Incidentally, the Mg 2 gradients of the most luminous bulges as well as the slope of the gradient-luminosity relation are similar to those among low-luminosity ellipticals in the Carollo et al (1993) sample.…”

Section: Radial Line-strength Gradientssupporting

confidence: 55%

“…Symbols are shown in the inset (where T is the RC3 morphological type). The dotted lines depict the extremes of the ∆Mg2/∆log(r) vs. MV relation among low-and intermediate-luminosity E and S0 galaxies from Carollo et al (1993).…”

Section: Radial Line-strength Gradientsmentioning

confidence: 99%

“…Evidence in favor of this scenario has been presented by means of spectroscopic studies of ellipticals : Carollo, Danziger & Buson (1993) reported the presence of a correlation between radial Mg 2 absorptionline-strength gradients and galaxy mass, velocity dispersion, and central line strength for low-to intermediate-mass (i.e., M < ∼ 10 11 M ⊙ ) ellipticals, as opposed to giant ellipticals (but see different results by Gorgas 1996 andKobayashi &Arimoto 1999). The gradients may thus be driven mostly by dissipation in smallish ellipticals, whereas merging and violent relaxation play a more important role for giant ellipticals.…”

Section: Introduction: the Formation Of Bulges Of Spiralsmentioning

confidence: 99%

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Goudfrooij

Gorgas

Jablonka

1999

Astrophysics and Space Science

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Abstract. We present first results of a comprehensive survey of deep long-slit spectra along the minor axis of bulges of edge-on spiral galaxies. Our results indicate that stellar populations in bulges are fairly old and encompass a range of metallicities. The luminosity-weighted ages of bulges range from those found for cluster ellipticals to slightly "younger" (by up to only a few Gyr, however). Their α/Fe element ratio is typically supersolar, consistent with those found in giant ellipticals. The radial line-strength gradients in bulges correlate with bulge luminosity. Generally, these findings are more compatible with predictions of the "dissipative collapse" model than with those of the "secular evolution" model.

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Section: Radial Line-strength Gradientssupporting

confidence: 55%

Section: Radial Line-strength Gradientsmentioning

confidence: 99%

Section: Introduction: the Formation Of Bulges Of Spiralsmentioning

confidence: 99%

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Goudfrooij

Gorgas

Jablonka

1999

Astrophysics and Space Science

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“…Carollo et al 1993;Gonzalez 1993;Davies et al 1993;Trager et al 1998Trager et al , 2000 and a reddening of the stellar light (colour−magnitude relation, e.g. Bower et al 1992) with the velocity dispersion of the galaxies.…”

Section: Introductionmentioning

confidence: 99%

Cosmological formation and chemical evolution of an elliptical galaxy

Colavitti

Pipino

Matteuccí

2009

A&A

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Aims. We aim to study the effect of a cosmologically motivated gas infall law for the formation of a massive elliptical galaxy in order to understand its impact on the formation of spheroids. Methods. We replace the empirical infall law of the model by Pipino & Matteucci with a cosmologically derived infall law for the formation of an elliptical galaxy. We compare our predictions with observations. We also compare the obtained results with those of Pipino & Matteucci.Results. We computed models with and without galactic winds; we found that models without wind predict a too large current SNIa rate. In particular, the cosmological model produces a current SNIa value which is about ten times higher than the observed values. Moreover models without wind predict a high current SNII rate, too large even if compared with the recent GALEX data. The predicted SNII rate for the model with wind, on the other hand, is too low if compared with the star formation histories given by GALEX. The mean value for the [Mg/Fe] ratio in the dominant stellar population of the simulated galaxy, as predicted by the cosmological model, is too low if compared to observations. This is a very important result indicating that the cosmological infall law is in contradiction to the chemical evolution. Conclusions. A cosmologically derived infall law for an elliptical galaxy cannot reproduce all the chemical constraints given by observations. The problem resides in the fact that the cosmologically derived infall law implies a slow gas accretion with a consequent star formation rate active for a long period. In this situation low [Mg/Fe] ratios are produced for the dominant stellar population in a typical elliptical, at variance with observations.

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“…The relation of radial B − R color gradients with radial gradients of the stellar line-strength indices Mg2 (left panel) and <Fe> (right panel) for all ellipticals for which both pairs of quantities have been measured to date. Data taken from Peletier (1989), Carollo et al (1993), Davies et al (1993), Carollo & Danziger (1994), and Paper I.…”

Section: The "Dust Mass Discrepancy" Among Elliptical Galaxiesmentioning

confidence: 99%

The Distribution of Dust and Gas in Elliptical Galaxies

Goudfrooij

1996

New Extragalactic Perspectives in the New South Africa

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Abstract.Results from IRAS and recent optical CCD surveys are examined to discuss the distribution and origin of dust and ionized gas in elliptical galaxies. In strong contrast with the situation among spiral galaxies, masses of dust in elliptical galaxies as derived from optical extinction are an order of magnitude lower than those derived from IRAS data. I find that this dilemma can be resolved by a diffusely distributed component of dust which is not detectable in optical data.The morphology of dust lanes and their association with ionized gas in elliptical galaxies argues for an external origin of both components of the ISM.

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Metallicity gradients in early-type galaxies

Cited by 227 publications

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Cosmological formation and chemical evolution of an elliptical galaxy

The Distribution of Dust and Gas in Elliptical Galaxies

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