Population Synthesis in the Blue. IV. Accurate Model Predictions for Lick Indices and UBV Colors in Single Stellar Populations

By R. Schiavon. 2007

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Subfields: Astronomy and Astrophysics, Instrumentation

View Paper: https://www.semanticscholar.org/paper/a065382de3eb993292e6c0e08099859e23a0fac8

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Citations in the corpus

Modeling the Panchromatic Spectral Energy Distributions of Galaxies (2013, methodology): “In principle then, the consideration of multiple Balmer lines should provide constraints on multiple age components, and/or allow for the separation of age and blue HB effects (Schiavon et al. 2004, Schiavon 2007, Serra & Trager 2007).”
Age-dating luminous red galaxies observed with the Southern African Large Telescope (2016, methodology): “…(ii) techniques that fit features in the spectra such as Lick– index fitting (e.g. Worthey & Ottaviani 1997; Bruzual & Charlot 2003; Thomas, Maraston, & Bender 2003; Lee & Worthey 2005; Annibali et al. 2007; Schiavon 2007; Lee et al. 2009; Vazdekis et al. 2010; Thomas, Maraston, & Johansson 2011).”
Re-evaluating old stellar populations (2018, methodology): “6 We use table 1 of Schiavon (2007) to define the wavelength dependence of the resolution.”
COUNTING LOW-MASS STARS IN INTEGRATED LIGHT (2011, methodology): “…be contrasted with models such as Bruzual & Charlot (2003), which model spectral energy distributions at solar abundance patterns, and models that consider the effect of age, metallicity, and abundance patterns on the Lick index system (e.g., Trager et al. 2000; Thomas et al. 2003b; Schiavon 2007).”
The SAURON project – XVII. Stellar population analysis of the absorption line strength maps of 48 early-type galaxies (2010, methodology): “This diagram provides a convenient overview of our line 1 [MgFe] = √ Mg b × (Fe5270+Fe5335) 2 2 [MgFe]′ = √ Mg b × (0.72 × Fe5270 + 0.28× Fe5335) 3 We use here the “base” models from Schiavon (2007) with solarabundance ratios, where the abundance ratio bias of the stellar libr y has been removed.”
Evolutionary stellar population synthesis with MILES – II. Scaled-solar and α-enhanced models (2015, methodology): “(e.g. Rose 1985, 1994; Trager et al. 1998, 2000; Proctor & Sansom 2002; Sánchez-Blázquez et al. 2003; Carretero et al. 2004; Thomas et al. 2005; Schiavon 2007; Conroy & van Dokkum 2012b).”
MIUSCAT: extended MILES spectral coverage – I. Stellar population synthesis models (2012, methodology): “In the low metallicity regime, however, our models combine scaled-solar isochrones with stellar spectra that do not show this abundance ratio pattern (e.g., Edvardsson et al. 1993; Schiavon 2007).”
De re metallica: the cosmic chemical evolution of galaxies (2018, background): “…in the 1970s and later refined and re-calibrated, and are still widely used, especially when only low-resolution spectra are available (e.g., Faber, 1973; Worthey et al., 1994; Worthey & Ottaviani, 1997; Trager et al., 1998, 2000a; Thomas et al., 2003; Schiavon, 2007; Thomas et al., 2011).”
EARLY-TYPE GALAXY ARCHEOLOGY: AGES, ABUNDANCE RATIOS, AND EFFECTIVE TEMPERATURES FROM FULL-SPECTRUM FITTING (2013, methodology): “TheEZ_Ages code fits 7 Lick indices with the SPS models of Schiavon (2007) in order to derive the age, [Fe/H], [C/Fe], [N/Fe], [Mg/Fe], and [Ca/Fe].”
Deriving Physical Properties from Broadband Photometry with Prospector: Description of the Model and a Demonstration of its Accuracy Using 129 Galaxies in the Local Universe (2016, methodology): “ATLAS-3D simultaneously estimates metallicities, ages, and alpha abundances using Schiavon (2007) simple stellar populations matched to observed measurements of the Lick indices (Worthey et al. 1994) for Hβ, Fe5015, and Mg b.”
Nuclear star clusters (2009, background): “This trend with galaxy mass is not as evident in the photometric measurements alone, but we regard the spectroscopic results as more reliable, given the near independence of the Lick index-based metallicities on age (e.g., Schiavon 2007).”
The ATLAS3D Project – XXX. Star formation histories and stellar population scaling relations of early-type galaxies (2015, methodology): “Abundance ratio dependences are small for the Schiavon (2007) models used here.”
Evolutionary stellar population synthesis with MILES – I. The base models and a new line index system (2010, methodology): “…al. 1984; Gorgas et al. 1993; Worthey et al. 1994) There are, however, alternative fitting functions in the optical range (e.g., Buzzoni 1995; Gorgas et al. 1999; Tantalo, Chiosi & Piovan 2007; Schiavon 2007) and in other spectral ranges (e.g., Cenarro et al. 2002; Mármol-Queraltó et al. 2008).”
THE STELLAR INITIAL MASS FUNCTION IN EARLY-TYPE GALAXIES FROM ABSORPTION LINE SPECTROSCOPY. II. RESULTS (2012, background): “The latter are based on the SPS model of Schiavon (2007).”
Stellar population models at high spectral resolution (2011, background): “…Davies et al. 1993; Surma & Bender 1995; Tripicco & Bell 1995; Greggio 1997; Trager et al. 2000; Maraston et al. 2003; Thomas et al. 2003, 2004; Schiavon 2007; Thomas et al. 2011, ,just to name a few among the most relevant works on the topic, see the latter paper for full referencing and…”
Erratum: Recovering galaxy stellar population properties from broad-band spectral energy distribution fitting (2012, methodology): “…line indices and comparing to element-ratio sensitive models (e.g. Worthey et al. 1992; Trager et al. 2000; Kuntschner 2000; Thomas et al. 2005; Schiavon 2007; Thomas et al. 2010), the high S/N that is required made this method practical only for a limited number of galaxies at limited…”