Evolutionary population synthesis in stellar systems. I - A global approach

Buzzoni, A.

doi:10.1086/191399

Cited by 201 publications

(237 citation statements)

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“…It may be interesting to note that except for B350, their estimates based on the BC03 SPSS models are not compatible (too young) with the observed CMDs, even taking into account the reported uncertainties; on the other hand, the estimates obtained from the T03 models are similar to those by P05, and, in particular, the old age reported for B350 fully agrees with our results. The sensitivity of colors and/or spectral indices generally used as age diagnostics (like, for example, Hβ) to the morphology of the horizontal branch is known for long time: for example, it was already taken into account in the models of the integrated light of SSPs by Buzzoni (1989). Bright and hot BHB stars typical of an old population may mimic the effect of a hotter MSTO, i.e., of a younger age (see Lee et al 2000, for a thorough discussion; and Percival & Salaris 2011, for a very recent investigation in the context of SPSS modeling).…”

Section: Summary and Discussionmentioning

confidence: 99%

HST/ACS color-magnitude diagrams of candidate intermediate-age M 31 globular clusters

Perina¹,

Galleti²,

Pecci³

et al. 2011

A&A

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We present deep (V 28.0) BV photometry obtained with the wide field channel of the Advanced Camera for Surveys on board HST for four M 31 globular clusters that were identified as candidate intermediate-age (age ∼ 1−9 Gyr) by various authors, based on their integrated spectra and/or broad/intermediate-band colors. Two of them (B292 and B350) display an obvious blue horizontal branch, indicating that they are as old as the oldest Galactic globulars. On the other hand, for the other two (B058 and B337), which display red horizontal branches, it was not possible either to confirm or disconfirm the age estimate from integrated spectra. The analysis of the distribution in the spectral indices Mg2 and Hβ of the M 31 and Milky Way clusters whose horizontal branch can be classified as red or blue based on existing CMDs, strongly suggests that classical age diagnostics from integrated spectra may be significantly influenced by the HB morphology of the clusters and can lead to erroneous age-classifications. We also provide the CMD for another two clusters that fall into the field of the main targets, B336, an old and metal-poor globular with a significant population of RR Lyrae variables, and the newly discovered B531, a cluster with a very red red giant branch.

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Section: Summary and Discussionmentioning

confidence: 99%

HST/ACS color-magnitude diagrams of candidate intermediate-age M 31 globular clusters

Perina¹,

Galleti²,

Pecci³

et al. 2011

A&A

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“…The downside is that they are an agglomeration of a large number of absorption lines from various chemical elements, so that their use for the derivation of individual element abundances is nontrivial. While the 1990s have seen the advent of a number of stellar population models produced for the aim of analysing galaxy spectra (Buzzoni 1989;Bruzual & Charlot 1993;Vazdekis et al 1996;Worthey 1994;Maraston 1998), it was also recognised that Mg and Fe absorption features in early-type galaxies could not be reproduced by these models (Peletier 1989;Worthey et al 1992;Davies et al 1993;Carollo & Danziger 1994;Bender & Paquet 1995;Greggio 1997) as shown in Fig. 1.…”

Section: Brief History Of Element Ratio Modellingmentioning

confidence: 99%

Element abundance ratios in stellar population modelling

Thomas

2014

Proc. IAU

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Abstract. I review the implementation of the effects from varying chemical element abundance ratios in stellar population modelling, focusing on α-and Fe-peak elements. A brief overview of the development of such models over the past 30 years is provided, starting with early work on the identification of relevant absorption features in the spectra of early-type galaxies in the 1980s leading to the most recent developments of the past years. Recent highlights include the adoption of new flux calibrated libraries, the inclusion of a wide range of chemical elements, the calculation of error estimates on the model, and the consideration of element variation effects on full spectra. The calibration of such models with globular clusters and some key results on the element ratios measured in early-type galaxies are presented.

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“…The Miller-Scalo IMF implies z=0.25, and κ « 1.2. Recent studies indicate that the value of κ depend on passband and metallicity (Buzzoni 1989, Worthey 1994. These authors find 0.6 < κ < 0.95 for the V band.…”

Section: Models For the Evolution Of The M/l Ratiomentioning

confidence: 99%

Measuring the Evolution of the M/L ratio from the Fundamental Plane in Cl 0024+16 atz=0.39

Franx¹,

VanDokkum²

1996

Symp. - Int. Astron. Union

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Abstract. The existence of the Fundamental Plane of early-type galaxies implies that the M/L ratios of early-types are well behaved. It provides therefore an important tool to measure the evolution of the M/L ratio with redshift. These measurements, in combination with measurements of the evolution of the luminosity function, can be used to constrain the mass evolution of galaxies.We present the Fundamental Plane relation measured for galaxies in the rich cluster CL 0024+16 at z=0.391. The galaxies satisfy a tight Fundamental Plane, with relatively low scatter (15 %).,The M/L is 31 ± 12 % lower than the M/L measured in Coma, which is consistent with simple evolutionary models. Hence, galaxies with very similar dynamical properties existed at a ζ=0Λ.More, and deeper data are needed to measure the evolution of the slope and the scatter of the Fundamental Plane to higher accuracy. Furthermore, data on the richest nearby clusters would be valuable to test the hypothesis that the Fundamental Plane is independent of cluster environment.

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Evolutionary population synthesis in stellar systems. I - A global approach

Cited by 201 publications

References 0 publications

HST/ACS color-magnitude diagrams of candidate intermediate-age M 31 globular clusters

HST/ACS color-magnitude diagrams of candidate intermediate-age M 31 globular clusters

Element abundance ratios in stellar population modelling

Measuring the Evolution of the M/L ratio from the Fundamental Plane in Cl 0024+16 atz=0.39

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