An updated MILES stellar library and stellar population models

By J. Falc'on-Barroso, P. Sánchez-Blázquez, A. Vazdekis, E. Ricciardelli, N. Cardiel, A. Cenarro, J. Gorgas, Reynier Peletier. 2011

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Aims: We present a number of improvements to the MILES library and stellar population models. We correct some small errors in the radial velocities of the stars, measure the spectral resolution of the library and models more accurately, and give a better absolute flux calibration of the models. Methods: We use cross-correlation techniques to correct the radial velocities of the offset stars and the penalised pixel-fitting method, together with different sets of stellar templates, to re-assess the spectral resolution of the MILES stellar library and models. We have also re-calibrated the zero-point flux level of the models using a new calibration scheme. Results: The end result is an even more homogeneously calibrated stellar library than the originally released one, with a measured spectral resolution of ~2.5 A, almost constant with wavelength, for both the MILES stellar library and models. Furthermore, the new absolute flux calibration for the spectra excellently agrees with predictions based on independent photometric libraries. Conclusions: This improved version of the MILES library and models (version 9.1) is available at the project's website (http://miles.iac.es).

Subfields: Astronomy and Astrophysics, Instrumentation

View Paper: https://www.semanticscholar.org/paper/3db853e47c56cfe818fe800c58b1c94ddff5526b

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Citations in the corpus

New fully empirical calibrations of strong-line metallicity indicators in star forming galaxies (2016, methodology): “(0000) CAT library of spectral templates (Vazdekis et al. 2012; Ricciardelli et al. 2012), an extension of the previous MILES library (Falcón-Barroso et al. 2011; Cenarro et al. 2001; Vazdekis et al. 2010; Sánchez-Blázquez et al. 2006) in which both Indo-U.”
UV-extended E-MILES stellar population models: young components in massive early-type galaxies (2016, methodology): “To obtain the absolute flux in the V-band we follow the method described in Falcón-Barroso et al. (2011), which is based on the calibration of Fukugita, Shimasaku & Ichikawa (1995).”
Three Hypervelocity White Dwarfs in Gaia DR2: Evidence for Dynamically Driven Double-degenerate Double-detonation Type Ia Supernovae (2018, methodology): “Radial velocities (RVs) were measured via crosscorrelation against the MILES library, comprising nearly 1000 stellar templates (Sánchez-Blázquez et al. 2006; Falcón-Barroso et al. 2011).”
Toward a Better Understanding of Cosmic Chronometers: A New Measurement of H(z) at z ∼ 0.7 (2021, methodology): “…to TMJ11, they are generated with variable age, [Z/H], [α/Fe] parameters, and use an updated version of the same empirical stellar library (MILES, Falcón-Barroso et al. 2011), but are based on corrections from theoretical stellar spectra and assume different stellar isochrones (BaSTI,…”
MIUSCAT: extended MILES spectral coverage – I. Stellar population synthesis models (2012, methodology): “MILES includes 985 stars covering the range 3525- 7500 Å with a spectral resolution of 2.5 Å(FWHM), as recently shown in Falcón-Barroso et al. (2011).”
The Fifteenth Data Release of the Sloan Digital Sky Surveys: First Release of MaNGA-derived Quantities, Data Visualization Tools, and Stellar Library (2018, background): “…to be Gaussian, and the 42 templates resulting from a hierarchical clustering analysis of the MILES stellar library (SánchezBlázquez et al. 2006; Falcón-Barroso et al. 2011) are always used for the continuum templates; details regarding the latter is discussed in K. Westfall et al., (in…”
COUNTING LOW-MASS STARS IN INTEGRATED LIGHT (2011, background): “1 (Falcón-Barroso et al. 2011), which corrects several smallerrors in previous releases.”
Inferring the star formation histories of massive quiescent galaxies with bagpipes: evidence for multiple quenching mechanisms (2017, methodology): “These differ from earlier versions by their use of the Medium-resolution Isaac Newton Telescope library of empirical spectra (MILES; Falcón-Barroso et al. 2011) in the UV-optical spectral region.”
A characteristic oxygen abundance gradient in galaxy disks unveiled with CALIFA (2013, methodology): “The models were extracted from the SSP template library provided by the MILES project (Vazdekis et al. 2010; Falcón-Barroso et al. 2011).”
The star formation history of CALIFA galaxies: Radial structures (2013, methodology): “(b) Base CB is an updated version of the Bruzual & Charlot (2003) models that replaces STELIB (Le Borgne et al. 2003) with a combination of the MILES (Sánchez-Blázquez et al. 2006; Falcón-Barroso et al. 2011) and granada (Martins et al. 2005) spectral libraries.”
Improved constraints on the expansion rate of the Universe up to z ∼ 1.1 from the spectroscopic evolution of cosmic chronometers (2012, methodology): “The two models are also based on independent libraries of stellar spectra, with MaStro using the latest MILES models [77] and BC03 using STELIB [78].”
Stellar population gradients in galaxy discs from the CALIFA survey - The influence of bars (2014, methodology): “…line spectrum is fitted with the penalised pixel-fitting pPXF (Cappellari & Emsellem 2004), using as templates the stellar population models of Vazdekis et al. (2010, V10 hereafter) based on the MILES stellar library (Sánchez-Blázquez et al. 2006; Cenarro et al. 2007; Falcón-Barroso et al. 2011)2.”
THE MASS–METALLICITY RELATION WITH THE DIRECT METHOD ON STACKED SPECTRA OF SDSS GALAXIES (2012, methodology): “The synthetic spectra were created from a library of 300 empirical miles spectral templates (Sánchez-Blázquez et al. 2006; Cenarro et al. 2007; Vazdekis et al. 2010; Falcón-Barroso et al. 2011, data as obtained from the miles Web site2).”
Evolutionary stellar population synthesis with MILES – II. Scaled-solar and α-enhanced models (2015, methodology): “To derive the synthetic colours, we adopt Vega magnitudes for the Johnson bands, B and V (Buser & Kurucz 1978; see also Falcón-Barroso et al. 2011 for further details on our definition of Vega magnitudes) and the AB system for the SDSS filters: u, g, r and i. MNRAS 449, 1177–1214 (2015) D ow…”