Evolutionary stellar population synthesis at high spectral resolution: optical wavelengths

By R. Delgado, M. Cerviño, L. Martins, C. Leitherer, P. A. I. D. A. D. Andalucia, Spain. 2005

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We present the single stellar population (SSP) synthesis results of our new synthetic stellar atmosphere models library with a spectral sampling of 0.3 A, covering the wavelength range from 3000 to 7000 A for a wide range of metallicities (twice solar, solar, half solar and 1/10 solar). The stellar library is composed of 1650 spectra computed with the latest improvements in stellar atmospheres. In particular, it incorporates non-local thermodynamic equilibrium (LTE) line-blanketed models for hot (T eff ≥ 27 500 K), and LTE line-blanketed models (Phoenix) for cool (3000 ≤ T eff ≤ 4500 K) stars. Because of the high spectral resolution of this library, evolutionary synthesis models can be used to predict the strength of numerous weak absorption lines and the evolution of the profiles of the strongest lines over a wide range of ages. The SSP results have been calculated for ages from 1 Myr to 17 Gyr using the stellar evolutionary tracks provided by the Geneva and Padova groups. For young stellar populations, our results have a very detailed coverage of high-temperature stars with similar results for the Padova and Geneva isochrones. For intermediate and old stellar populations, our results, once degraded to a lower resolution, are similar to the ones obtained by other groups (limitations imposed by the stellar evolutionary physics notwidthstanding). The limitations and advantages of our models for the analysis of integrated populations are described. The full set of the stellar library and the evolutionary models are available for retrieval at the websites http://www.iaa.csic.es/∼rosa and http://www.iaa.csic.es/∼mcs/sed@, or on request from the first two authors.

Subfields: Astronomy and Astrophysics, Instrumentation

View Paper: https://www.semanticscholar.org/paper/29c8cae723b13f4d80f485167687ad94f3c51a0d

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Citations in the corpus

A LIBRARY OF THEORETICAL ULTRAVIOLET SPECTRA OF MASSIVE, HOT STARS FOR EVOLUTIONARY SYNTHESIS (2010, methodology): “This follows the approach we took for the generation of the optical high-resolution library in Starburst99 (González Delgado et al. 2005; Martins et al. 2005b).”
Bursty stellar populations and obscured active galactic nuclei in galaxy bulges (2007, background): “In future papers it will be important to consider comparison between different spectral synthesis models, such as those based on synthetic stellar libraries (González Delgado et al. 2005).”
Fitting the integrated spectral energy distributions of galaxies (2010, background): “Currently less frequently used are fully theoretical stellar population models such as González Delgado et al. (2005); Coelho et al. (2007).”
MIUSCAT: extended MILES spectral coverage – I. Stellar population synthesis models (2012, background): “There are models that are fed with theoretical stellar atmospheres (e.g., Schiavon et al. 2000; González-Delgado et al. 2005; Coelho et al. 2007), whereas other models employ empirical libraries, mostly in the visible (e.g., Vazdekis 1999; Bruzual & Charlot 2003; Le Borgne et al. 2004; Conroy &…”
Revised Primordial Helium Abundance Based on New Atomic Data (2007, methodology): “For samples including a large fraction of objects with EWem(H ) 1508we expect the error for this concept to be larger than ours; moreover, to agree with the models by González Delgado et al. (1999, 2005), the average EWab(H ) for any given sample has to be equal to or larger than 2 8.”
Outflows in Infrared-Luminous Starbursts at z < 0.5. I. Sample, Na I D Spectra, and Profile Fitting (2005, result): “1996, ApJ, 462, 651 Lilly, S. J., Eales, S. A., Gear, W. K. P., Hammer, F., Le Fèvre, O., Crampton, D., Bond, J. R., & Dunne, L. 1999, ApJ, 518, 641 Lutz, D., Veilleux, S., & Genzel, R. 1999, ApJ, 517, L13 Madau, P., Ferrara, A., & Rees, M. J. 2001, ApJ, 555, 92 Marsh, T. 1989, PASP, 100, 1032 Mart”
Stellar Population Diagnostics of Elliptical Galaxy Formation (2006, unknown): “Trager SC, Faber SM, Worthey G, Gonzales JJ. 2000.”
The CALIFA survey across the Hubble sequence: Spatially resolved stellar population properties in galaxies (2015, background): “Base GMe is a combination of the SSP spectra provided by Vazdekis et al. (2010) for populations older than t = 63 Myr and the González Delgado et al. (2005) models for younger ages.”
SDSS IV MaNGA – spatially resolved diagnostic diagrams: a proof that many galaxies are LIERs (2016, background): “…(defined by Worthey & Ottaviani 1997) is primarily sensitive to stars of intermediate spectral type (A to early F) and thus increases until about 300-400 Myr after the burst (post-starburst population) and then decreases again at later times (Kauffmann et al. 2003a; González Delgado et al. 2005).”
THEORETICAL EVOLUTION OF OPTICAL STRONG LINES ACROSS COSMIC TIME (2013, background): “Optical and X-ray studies suggest that nuclear LINERs (< 1 kpc) are predominantly inefficiently accreting AGN, analogous to the ”low” state of black hole binary systems (Ho 2005; Satyapal et al. 2005; Kewley et al. 2006b; González-Mart́ın et al. 2009; Gu & Cao 2009; Ho 2009).”
The SAMI Galaxy Survey: shocks and outflows in a normal star-forming galaxy (2014, methodology): “In this application, we adopt theoretical SSP models, assuming Padova isochrones, of 18 ages4 and solar metallicity from González Delgado et al. (2005).”
Modeling the Panchromatic Spectral Energy Distributions of Galaxies (2013, methodology): “The Martins et al. (2005) library has even been incorporated into a fully theoretical high resolution SPS model (González Delgado et al. 2005).”
GAS-PHASE OXYGEN GRADIENTS IN STRONGLY INTERACTING GALAXIES. I. EARLY-STAGE INTERACTIONS (2010, methodology): “To fit these relatively high-resolution data, we used the stellar population synthesis models of González Delgado et al. (2005) as our stellar continuum templates.”
A library of high resolution synthetic stellar spectra from 300 nm to 1.8 μm with solar and α-enhanced composition (2005, background): “…Cerviño & Mas-Hesse 1994; Fioc & Rocca-Volmerange 1997; Leitherer et al. 1999; Vazdekis 1999; Buzzoni 2002; Schulz et al. 2002; Jimenez et al. 2004; Gonzalez Delgado et al. 2005; Maraston 2005; Schiavon 2005) and both empirical and theoretical libraries have improved dramatically in recent years.”
METALLICITY GRADIENTS AND GAS FLOWS IN GALAXY PAIRS (2010, methodology): “For continuum fitting, UHSPECFIT utilizes code from Moustakas (2006) and the González Delgado et al. (2005) evolutionary stellar population synthesis models.”
CALIFA, the Calar Alto Legacy Integral Field Area survey - III. Second public data release (2012, methodology): “Details of these measurements will be presented in González Delgado et al. (in prep.).”
Evolutionary stellar population synthesis with MILES – I. The base models and a new line index system (2010, methodology): “However, as pointed out in Section 2.3.1, we do not find a strong physical reason to use the González-Hernández & Bonifacio (2009) temperature scale, particularly for metal-rich objects.”
A new approach to systematic uncertainties and self-consistency in helium abundance determinations (2010, methodology): “The code used the input models from González Delgado et al. (2005) and Martins et al. (2005), and He I absorption line strengths as a function of stellar population age were examined.”