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

By A. Vazdekis, Paula Coelho, Santi Cassisi, E. Ricciardelli, J. Falc'on-Barroso, P. Sánchez-Blázquez, F. Barbera, M. Beasley, Adriano Pietrinferni. 2015

206 citations recorded by the source corpus.

We are indebted to the Padova group for making their isochrone calculations available to us. We are grateful to A. de C. Milone for providing us with his [Mg/Fe] estimates for the stars of the MILES library before publication. We also are grateful to H.-S. Kim, J. Cho, R. M. Sharples and S.-J. Yoon, who provided us with GGC line-strength measurements prior to publication. We are grateful to B. Barbuy, J. L. Cervantes, I. G. de la Rosa, M. Koleva, R. Peletier and A. Sansom for very useful discussions. We thank the referee H.-C. Lee for a careful reading of the manuscript and for very valuable clarifications that helped us to improve the manuscript. We also would like to thank J. A. Perez Prieto for helping us in the construction of the web page for the models. The MILES library was observed at the INT on the island of La Palma, operated by the Isaac Newton Group at the Observatorio del Roque de los Muchachos of the Instituto de Astrofisica de Canarias. This research has made an extensive use of the SIMBAD data base and VizieR catalogue access tool (both operated at CDS, Strasbourg, France), the NASA's Astrophysics Data System Article Service. We made use of data retrieved from the Sloan Digital Sky Survey archives ( http://www.sdss.org ). Funding for the SDSS and SDSS-II has been provided by the Alfred P. Sloan Foundation, the Participating Institutions, the National Science Foundation, the US Department of Energy, the National Aeronautics and Space Administration, the Japanese Monbukagakusho, the Max Planck Society and the Higher Education Funding Council for England. PC acknowledges the financial support by FAPESP via project 2008/58406-4 and fellowship 2009/09465-0. JFB acknowledges support from the Ramon y Cajal programme by the Spanish Ministry of Economy and Competitiveness (MINECO). This work has been supported by the Programa Nacional de Astronomia y Astrofisica of MINECO, under grants AYA2013-48226-C3-1-P, AYA2013-48226-C3-2-P, AYA2013-48226-C3-3-P and by the Generalitat Valenciana under grant PROMETEOII2014-069.

Subfields: Astronomy and Astrophysics, Instrumentation

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Citations in the corpus

An Older, More Quiescent Universe from Panchromatic SED Fitting of the 3D-HST Survey (2018, background): “Vazdekis et al. (2015) generate α-enhanced models with [α/Fe]=+0.4 and show that the resulting optical fluxes change by 10%–40% and the optical colors change by ∼0.1 mag, depending on the age and metallicity of the stars.”
A unified multiwavelength model of galaxy formation (2015, background): “There are several libraries available which provide L (SSP) λ (t, Z; Φ) for different ages, metallicities and IMFs (e.g. Bruzual & Charlot 1993; Bressan et al. 1998; Bruzual & Charlot 2003; Maraston 2005; Conroy et al. 2009; Vazdekis et al. 2015).”
Modelling and interpreting spectral energy distributions of galaxies with BEAGLE (2016, methodology): “Following Walcher et al. (2009, see also Vazdekis et al. 2015), we account for the dependence of the function Sλ on α/Fe ratio in equation (1) by writing Sλ(t ′, Z, [α/Fe]) = S theor λ (t ′, Z, [α/Fe]) S theorλ (t ′, Z) Sλ(t ′, Z), (5) where Sλ(t′, Z) is the luminosity per unit wavelength of an SSP…”
Toward a Better Understanding of Cosmic Chronometers: A New Measurement of H(z) at z ∼ 0.7 (2021, methodology): “Differences as a function of redshift between stellar ages and metallicities [Z/H] of 140 LEGA-C passive galaxies obtained with Vazdekis et al. (2015) single-burst (SSP, upper panels) and exponentially declining (τ -decl., lower panels) star formation histories versus Thomas et al. (2011) SSP…”
Age-dating luminous red galaxies observed with the Southern African Large Telescope (2016, background): “However, most of the absorption features (e.g. high–order Balmer lines) present in our wavelength ranges are sensitive to the age determination but insensitive to the metallicity and α–elements (the detailed discussion about the absorption features sensitivity is given in Vazdekis et al. (2015)).”
Ultra-diffuse galaxies outside clusters: clues to their formation and evolution (2016, methodology): “As a further test, we have reestimated the stellar masses of our UDGs using the stellar population predictions provided by (Vazdekis et al. 2015) using a universal Kroupa IMF (Kroupa 2001).”
UV-extended E-MILES stellar population models: young components in massive early-type galaxies (2016, methodology): “We refer the interested reader to Cassisi et al. (2004), Pietrinferni et al. (2004) and Vazdekis et al. (2015) for a more detailed comparison of these two sets of isochrones.”