Evolutionary synthesis of simple stellar populations

Kurth, Oliver; Alvensleben, Uta Fritze v.; Fricke, K. J.

doi:10.1051/aas:1999499

Cited by 57 publications

(88 citation statements)

References 28 publications

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“…This effect is strongest in (V − K) and can amount to more than 1 mag in (V − K) at solar metallicity as seen in Fig. 1, where we plot the (V − K) color evolution for an SSP based on isochrones including the TP-AGB in comparison with an SSP from Kurth et al (1999) based on the Padova stellar evolutionary tracks that did not include the TP-AGB phase. The effect is weaker at lower metallicities and for colors at shorter wavelengths.…”

Section: Input Physics: Padova Isochrones With Tp-agbmentioning

confidence: 95%

“…We supplemented these Padova isochrones by low mass stars in the mass range from 0.15−0.45 M from the calculations of Chabrier & Baraffe (1997) that include a new description of the interior of low mass objects and use non-grey atmospheres (see Kurth et al 1999 for details). The Padova group recently added low mass-stars to their isochrones themselves (Girardi et al 2000) but did not compare their low mass stars to those of Chabrier & Baraffe.…”

Section: Input Physics: Padova Isochrones With Tp-agbmentioning

confidence: 99%

“…A second possibility to start from a discrete set of stellar tracks and obtain a reasonably smooth photometric evolution is the use of a Monte Carlo method as described e.g. by Kurth et al (1999). This method works very well for a photometric description but requires a huge number of Monte Carlo stars and timesteps to yield a smooth spectral evolution.…”

Section: Introductionmentioning

confidence: 99%

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Spectral and photometric evolution of simple stellar populations at various metallicities

Schulz¹,

Alvensleben²,

Möller³

et al. 2002

A&A

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128

209

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Abstract.A new set of evolutionary synthesis spectra are presented for Simple Stellar Populations (SSPs) covering ranges in metallicity from 0.02 ≤ Z/Z ≤ 2.5 and ages from 4 × 10 6 yr ≤ t ≤ 16 Gyr. They are based on the most recent isochrones from the Padova group that extend earlier models by the inclusion of the thermal pulsing AGB phase for stars in the mass range 2 M ≤ m ≤ 7 M in accordance with the fuel consumption theorem. We show that with respect to earlier models, inclusion of the TP-AGB phase leads to significant changes in the (V − I) and (V − K) colors of SSPs in the age range from 10 8 to ∼ > 10 9 yr. Using model atmosphere spectra from Lejeune et al. (1997Lejeune et al. ( , 1998, we calculate the spectral evolution of single burst populations of various metallicities covering the wavelength range from 90 Å through 160 µm. Isochrone spectra are convolved with filter response functions to describe the time evolution of luminosities and colors in Johnson, Thuan & Gunn, Koo, HST, Washington and Strömgren filters. The models and their results are not only intended for use in the interpretation of star clusters but also for combination with any kind of dynamical galaxy formation and/or evolution model that contains a star formation criterion. Moreover, the evolution of these single burst single metallicity stellar populations is readily folded with any kind of star formation -and eventually chemical enrichment -history to describe the evolutionary spectral synthesis of composite stellar populations like galaxies of any type with continuous or discontinuous star formation. For these latter purposes we also present the time evolution of ejection rates for gas and metals for two different Initial Mass Functions (IMFs) as well as cosmological and evolutionary corrections for all the filters as a function of redshift for 0 ≤ z ≤ 5 and two different cosmologies. Extensive data files are provided in the electronic version, at CDS, and at our above www-address.

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Section: Input Physics: Padova Isochrones With Tp-agbmentioning

confidence: 95%

Section: Input Physics: Padova Isochrones With Tp-agbmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

See 1 more Smart Citation

Spectral and photometric evolution of simple stellar populations at various metallicities

Schulz¹,

Alvensleben²,

Möller³

et al. 2002

A&A

Self Cite

128

209

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show abstract

“…For example, compared the integrated colours of globular clusters in the Milky Way and M31 with population synthesis models of Bruzual & Charlot (as reported in Leitherer et al 1996), and Kurth, Fritze-von Alvensleben & Fricke (1999), as well as updated versions of Corresponding author: graeme@ucolick.org the Worthey (1994) models. They concluded that an age difference of 4 Gyr or more was needed between metal-rich and metal-poor clusters in order to provide the best model fits to their colours, with the metal-rich clusters being systematically younger.…”

Section: Introductionmentioning

confidence: 99%

Integrated colours of Milky Way globular clusters and horizontal branch morphology

Smith

Strader

2007

Astron Nachr

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Broadband colours are often used as metallicity proxies in the study of extragalactic globular clusters. A common concern is the effect of variations in horizontal branch (HB) morphology -the second-parameter effect -on such colours. We have used UBVI, Washington, and DDO photometry for a compilation of over 80 Milky Way globular clusters to address this question. Our method is to fit linear relations between colour and [Fe/H], and study the correlations between the residuals about these fits and two quantitative measures of HB morphology. While there is a significant HB effect seen in U − B, for the commonly used colours B − V , V − I, and C − T1, the deviations from the baseline colour-[Fe/H] relations are less strongly related to HB morphology. There may be weak signatures in B − V and C − T1, but these are at the limit of observational uncertainties. The results may favour the use of B − I in studies of extragalactic globular clusters, especially when its high [Fe/H]-sensitivity is considered.

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“…continue to be improved. Successive generations of modelers have combined the best available knowledge on the ingredients of population synthesis models to predict the appearance of the combined light of generations of stars (Tinsley 1980;Bruzual 1983;Arimoto & Yoshii 1987;Charlot & Bruzual 1991;Bertelli et al 1994;Lançon & Rocca-Volmerange 1996;Fioc & Rocca-Volmerange 1997;Kurth et al 1999;Leitherer et al 1999;Girardi et al 2000). Nevertheless the actual understanding of near-infrared properties has remained a subject of debate, in particular at intermediate ages, between 0.1 and 2-3 Gyr (Girardi & Bertelli 1998;Maraston 1998).…”

Section: Introductionmentioning

confidence: 99%

Photometric properties of single stellar populations: FromZ/Z$\mathsf{_{\odot}=1/50}$ toZ/Z$\mathsf{_{\odot}=2.5}$

Mouhcine

Lançon

2003

A&A

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Abstract. We describe a large grid of photometric properties of single stellar populations that focuses on the near infrared properties of intermediate age populations. The underlying model was presented in recent articles, where we compared its predictions with observations of properties of star clusters and of asymptotic giant branch populations of Local Group galaxies. The grid is made available in tabular form. We present the time evolution of optical and near-infrared broadband colours in the

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Evolutionary synthesis of simple stellar populations

Cited by 57 publications

References 28 publications

Spectral and photometric evolution of simple stellar populations at various metallicities

Spectral and photometric evolution of simple stellar populations at various metallicities

Integrated colours of Milky Way globular clusters and horizontal branch morphology

Photometric properties of single stellar populations: FromZ/Z$\mathsf{_{\odot}=1/50}$ toZ/Z$\mathsf{_{\odot}=2.5}$

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