Photometric Evolution of Elliptical Galaxies in the Color-Magnitude Diagram

Arimoto, N.; Yoshii, Yuzuru

doi:10.1007/978-94-009-4598-2_23

Cited by 405 publications

(610 citation statements)

References 9 publications

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“…Evolutionary population synthesis models, which are regarded nowadays as standard, take into account the contributions of all possible stars, in proportions prescribed by stellar evolution theory (e.g., Tinsley 1980). These models combine at least three main ingredients that determine the quality of the predictions: a prescription for the IMF, a set of stellar evolutionary isochrones and stellar spectral libraries to predict a variety of observables in several bands such as fluxes, colours, M/L, or low resolution spectra (e.g., Bruzual 1983;Arimoto & Yoshii 1986;Guiderdoni & Rocca-Volmerange 1987;Fritze-Von Alvensleben & Gerhard 1994;Worthey 1994;Vazdekis et al 1996;Fioc & Rocca-Volmerange 1997;Kodama & Arimoto 1997;Maraston 1998;Leitherer et al 1999;Maraston 2005;Conroy & Gunn 2010) and also surface brightness fluctuations (SBFs) (e.g., Liu, Charlot & Graham 2000;Blakeslee, Vazdekis & Ajhar 2001;Liu, Graham & Charlot 2002;Cantiello et al 2003).…”

Section: Introductionmentioning

confidence: 99%

Evolutionary stellar population synthesis with MILES – II. Scaled-solar and α-enhanced models

Vazdekis

Coelho

Cassisi

et al. 2015

Monthly Notices of the Royal Astronomical Society

332

394

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We present models that predict spectra of old-and intermediate-aged stellar populations at 2.51Å (FWHM) with varying [α/Fe] abundance. The models are based on the MILES library and on corrections from theoretical stellar spectra. The models employ recent [Mg/Fe] determinations for the MILES stars and BaSTI scaled-solar and α-enhanced isochrones. We compute models for a suite of IMF shapes and slopes, covering a wide age/metallicity range. Using BASTI, we also compute "base models" matching The Galactic abundance pattern. We confirm that the α-enhanced models show a flux excess with respect to the scaled-solar models blue-ward ∼4500Å, which increases with age and metallicity. We also confirm that both [MgFe] and [MgFe] ′ indices are [α/Fe]-insensitive. We show that the sensitivity of the higher order Balmer lines to [α/Fe] resides in their pseudo-continua, with narrower index definitions yielding lower sensitivity. We confirm that the α-enhanced models yield bluer (redder) colours in the blue (red) spectral range. To match optical colours of massive galaxies we require both α-enhancement and a bottom-heavy IMF. The comparison of Globular Cluster line-strengths with our predictions match the [Mg/Fe] determinations from their individual stars. We obtain good fits to both full spectra and indices of galaxies with varying [α/Fe]. Using thousands of SDSS galaxy spectra we obtain a linear relation between a proxy for the abundance,

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Section: Introductionmentioning

confidence: 99%

Evolutionary stellar population synthesis with MILES – II. Scaled-solar and α-enhanced models

Vazdekis

Coelho

Cassisi

et al. 2015

Monthly Notices of the Royal Astronomical Society

332

394

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“…The first attempts to account for non-solar abundances and their impact on the photometric evolution of galaxies go back to Arimoto & Yoshii (1986). Einsel et al (1995) used more recent and complete stellar evolutionary tracks and colour calibrations for initial stellar metallcities 10 −4 ...4 · 10 −2 to describe the photometric evolution of galaxy types E through Sd.…”

Section: Introductionmentioning

confidence: 99%

Untitled

Möller

Alvensleben

Fricke

et al. 2001

Astrophysics and Space Science

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Abstract.As a tool to interpret nearby and high redshift galaxy data from optical to K-band we present our chemically consistent spectrophotometric evolutionary synthesis models. These models take into account the increasing initial metallicity of successive stellar generations using recently published metallicity dependent stellar evolutionary tracks, stellar yields and model atmosphere spectra.The influence of the metallicity is analysed. Dust absorption is included on the basis of gas content and abundance as it varies with time and galaxy type. We compare our models with IUE template spectra and are able to predict UV fluxes for different spectral types. Combined with a cosmological model we obtain evolutionary and k-corrections for various galaxy types and show the differences to models using only solar metallicity input physics as a function of redshift, wavelength band and galaxy type.

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“…The model parameters for spiral galaxies are determined to reproduce the present-day gas fractions and B − V colors in various galaxy types at 15 Gyr after the formation. The model of elliptical galaxies is the so-called galactic wind model, in which star formation stops at about 1 Gyr after the formation by a supernova-driven galactic wind (Larson 1974;Arimoto & Yoshii 1987). We assume that gas fraction in a elliptical galaxy decreases exponentially after the galactic wind time (∼ 1 Gyr), with a time scale same as the galactic wind time.…”

Section: Evolution Of Galaxies and Type Ia Supernova Ratementioning

confidence: 99%

Dust versus Supernova Cosmology

Totani

2001

Sources and Detection of Dark Matter and Dark Energy in the Universe

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Abstract. Here we present some critical discussions about the systematic uncertainty by dust extinction in the recent cosmological results of high-redshift Type Ia supernovae. First we argue that the currently available data do not robustly exclude the cosmologically significant extinction either by the reddening check or the dispersion argument because of the observational uncertainties, even in the case of ordinary dust that reddens. Then we discuss two theoretical possibilities that high-z supernovae have larger extinction and hence they are fainter than local supernovae: the intergalactic dust and host galaxy evolution. Optical and near-infrared observations for a large number of supernovae with improved photometric accuracy are required to reject these possibilities and derive a compelling cosmological result.

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Photometric Evolution of Elliptical Galaxies in the Color-Magnitude Diagram

Cited by 405 publications

References 9 publications

Evolutionary stellar population synthesis with MILES – II. Scaled-solar and α-enhanced models

Evolutionary stellar population synthesis with MILES – II. Scaled-solar and α-enhanced models

Untitled

Dust versus Supernova Cosmology

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