Evolutionary synthesis of galaxies at high spectral resolution with the code PEGASE-HR. Metallicity and age tracers

By D. L. Borgne, B. Rocca-Volmerange, P. Prugniel, Ariane Lançon, M. Fioc, Caroline Paris, U. Toronto, Cral, O. Strasbourg, O. Bordeaux. 2004

278 citations recorded by the source corpus.

We present PEGASE-HR, a new stellar population synthesis program generating high resolution spectra (R = 10 000) over the optical range λλ = 400-680 nm. It links the spectro-photometric model of galaxy evolution PEGASE.2 (Fioc & Rocca-Volmerange 1997) to an updated version of the ELODIE library of stellar spectra observed with the 193 cm telescope at the Observatoire de Haute-Provence (Prugniel & Soubiran 2001a). The ELODIE star set gives a fairly complete coverage of the Hertzprung-Russell (HR) diagram and makes it possible to synthesize populations in the range (Fe/H) = − 2t o+0.4. This code is an exceptional tool for exploring signatures of metallicity, age, and kinematics. We focus on a detailed study of the sensitivity to age and metallicity of the high-resolution stellar absorption lines and of the classical metallic indices proposed until now to solve the age-metallicity degeneracy. Validity tests on several stellar lines are performed by comparing our predictions for Lick indices to the models of other groups. The comparison with the lower resolution library BaSeL (Lejeune et al. 1997) confirms the quality of the ELODIE library when used for single stellar populations (SSPs) from 10 7 to 2 × 10 10 yr. Predictions for the evolved populations of globular clusters and elliptical galaxies are given and compared to observational data. Two new high- resolution indices are proposed around the Hγ line. They should prove useful in the analysis of spectra from the new generation of telescopes and spectrographs.

Subfields: Astronomy and Astrophysics, Instrumentation

View Paper: https://www.semanticscholar.org/paper/a044d45462b703e98c45ef6ec643409c9d8b34b7

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Citations in the corpus

Evolution of Stars and Stellar Populations (2005, methodology): “[124], [140]) one can determine the SSP integrated spectrum by applying Equation (11.”
Medium-resolution Isaac Newton Telescope library of empirical spectra - II. The stellar atmospheric parameters (2006, background): “Recently, an updated version of ELODIE stellar library (hereafter ELODIE.3, Prugniel & Soubiran 2004) has been also incorporated into a new population-synthesis model (Le Borgne et al. 2004).”
UV-extended E-MILES stellar population models: young components in massive early-type galaxies (2016, background): “…dynamics (as a result of the smearing due to their velocity dispersion), have opened new means to further improve these studies (e.g. Vazdekis 1999; Schiavon et al. 2002; Bruzual & Charlot 2003; Le Borgne et al. 2004; Vazdekis et al. 2010; Maraston & Strömbäck 2011; Conroy & van Dokkum 2012a).”
Automatic determination of stellar atmospheric parameters and construction of stellar spectral templates of the Guoshoujing Telescope (LAMOST) (2011, background): “Spectral synthesis of stellar populations of galaxies, e.g. Le Borgne et al. (2004), Percival & Salaris (2009), Prugneil et al. (2007a), Koleva et al. (2007), Vazdekis t al.”
Stellar Population Inference with Prospector (2020, background): “…pop- ∗ Banting Fellow ulation synthesis codes which treat these elements with varying degrees of complexity, including GALAXEV (Bruzual & Charlot 2003), PÉGASE Fioc & RoccaVolmerange (1997); Le Borgne et al. (2004), Maraston (2005), FSPS (Conroy et al. 2009), and BPASS (Eldridge et al. 2017).”
PRIMUS: CONSTRAINTS ON STAR FORMATION QUENCHING AND GALAXY MERGING, AND THE EVOLUTION OF THE STELLAR MASS FUNCTION FROM z = 0–1 (2013, background): “3; Conroy et al. 2009; Conroy & Gunn 2010); Bruzual & Charlot (2003, hereafter BC03); the SPS models of Maraston (2005, hereafter Ma05)44; and pegase45 (Fioc & Rocca-Volmerange 1997, 1999; Le Borgne et al. 2004).”
STECMAP: STEllar Content from high-resolution galactic spectra via Maximum A Posteriori (2005, unknown): “The library used in Pégase-HR is known to be deficient in high metallicity, high α-element abundance red giants (Le Borgne et al. 2004), which may lead to an over-estimate of age or metallicity in observed galaxies2.”
ULySS: a full spectrum fitting package (2009, unknown): “HR (Le Borgne et al. 2004) and Vazdekis-Miles (Vazdekis 1999; Sánchez-Blázquez et al. 2006).”
Population Synthesis in the Blue. IV. Accurate Model Predictions for Lick Indices and UBV Colors in Single Stellar Populations (2007, background): “In fact, other well-known stellar population synthesis models in the literature (e.g., Worthey 1994, Vazdekis 1999, Bruzual & Charlot 2003, Le Borgne et al. 2004, Lee & Worthey 2005), which are based on similar combinations of theoretical isochrones and empirical stellar libraries, are afflicted by…”
New fully empirical calibrations of strong-line metallicity indicators in star forming galaxies (2016, methodology): “The stellar continuum subtraction in the [Sii] λ4069 spectral window (close to Hδ) has been performed using a different kind of stellar templates, the PÉGASE HR3(Le Borgne et al. 2004), a library which covers a wavelength range of 4000-6800 Å with a spectral resolution of R = 10000 at λ = 5500 Å;”
STECKMAP: STEllar Content and Kinematics from high resolution galactic spectra via Maximum A Posteriori (2005, methodology): “In the whole paper we use the Pégase-HR SSP models (Le Borgne et al. 2004) in order to illustrate and investigate the behaviour of the problems through simulations and inversions of mock data.”
Coudé-feed stellar spectral library – atmospheric parameters (2010, background): “The library is also available at a resolution of 0.55 Å (R ∼ 10 000) for the population synthesis in PegaseHR (Le Borgne et al. 2004).”
ISM properties in low-metallicity environments. III. The dust spectral energy distributions of II Zw 40, He 2-10 and NGC 1140 (2005, background): “Hence, the initial metallicity is not of great concern, due to the age-metallicity degeneracy (e.g. Le Borgne et al. 2004).”
Rates and Properties of Type Ia Supernovae as a Function of Mass and Star Formation in Their Host Galaxies (2006, methodology): “Our set of synthetic templates is computed with the PÉGASE.2 galaxy spectral evolution code (Fioc & Rocca-Volmerange 1997; Le Borgne & Rocca-Volmerange 2002; Le Borgne et al. 2004).”
Stellar populations of early-type galaxies in different environments - II. Ages and metallicities (2006, background): “The new generation of stellar population models do not only predict individual features as a function of the age and metallicity, but synthesise full spectral energy distributions(SEDs) (Vazdekis 1999; Vazdekis et al. 2003; Bruzual & Charlot 2003; Le Borgne et al. 2004).”
A primer on hierarchical galaxy formation: the semi-analytical approach (2006, background): “Vazdekis (1999) produced models with even higher resolution over a limited range of wavelengths (see also Le Borgne et al. 2004).”
Age-dating luminous red galaxies observed with the Southern African Large Telescope (2016, methodology): “We also tested other models such as Pegase–HR/ELODIE 3.1 (Le Borgne et al. 2004, PE), Vazdekis/MILES (Vazdekis et al. 2010, VM) and the latest Maraston/MILES models (Maraston & Strömbäck 2011, M11), in order to check any systematic differences.”