A library of high resolution synthetic stellar spectra from 300 nm to 1.8 μm with solar and α-enhanced composition

By Paula Coelho, B. Barbuy, Jorge Meléndez, R. Schiavon, B. Castilho. 2005

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Libraries of stellar spectra are fundamental tools for the study of stellar populations, and both empirical and synthetic libraries have been used for this purpose. In this paper, a new library of high resolution synthetic spectra is presented, ranging from the near-ultraviolet (300 nm) to the near-infrared (1.8 ${\rm \mu}$m). The library spans all the stellar types that are relevant to the integrated light of old and intermediate-age stellar populations in the involved spectral region (spectral types F through M and all luminosity classes). The grid was computed for metallicities ranging from [Fe/H] = –2.5 to +0.5, including both solar and α -enhanced ([ α /Fe] = 0.4) chemical compositions. The synthetic spectra are a good match to observations of stars throughout the stellar parameter space encompassed by the library and over the whole spectral region covered by the computations.

Subfields: Astronomy and Astrophysics, Atomic and Molecular Physics, and Optics, Instrumentation

View Paper: https://www.semanticscholar.org/paper/5e40f13c54e09ceec19cd1f6f03a01326bdb6ef3

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Citations in the corpus

Fitting the integrated spectral energy distributions of galaxies (2010, background): “…libraries have improved significantly in recent years, with both fully theoretical (e.g. Kurucz 1992; Westera et al. 2002; Smith et al. 2002; Coelho et al. 2005; Martins et al. 2005; Lançon et al. 2007) and empirical, e.g. STELIB (Le Borgne et al. 2003), MILES (SánchezBlázquez et al. 2006;…”
ULySS: a full spectrum fitting package (2009, background): “The reference spectra are either a grid of theoretical models (e. g.Munari et al. 2005; Coelho et al. 2005) or a set of observed stars whose parameters are known from the analysis of individual high resoluti n spectra (e. g.Soubiran et al. 1998).”
The California-Kepler Survey. I. High-resolution Spectroscopy of 1305 Stars Hosting Kepler Transiting Planets (2017, methodology): “The code creates a synthetic spectrum of arbitrary Teff , log g, [Fe/H], and V sin i by first interpolating between model spectra computed by Coelho et al. (2005) at discrete values of Teff , log g, and [Fe/H].”
The atmospheric parameters and spectral interpolator for the MILES stars (2011, methodology): “We also used the Coelho et al. (2005) library to add some low metallicity cool dwarfs at the locations Teff = 3500 K, log g = 4.5 and 5.0, [Fe/H] = −1.5,−2.0 and −2.5 using as reference Teff = 3500 K, log g = 4.5, [Fe/H] = −0.5.”
UV-extended E-MILES stellar population models: young components in massive early-type galaxies (2016, methodology): “Note that in Vazdekis et al. (2015) we computed self-consistent models in the optical range, which are scaled-solar or αenhanced for all metallicities, with the aid of the theoretical stellar spectra of Coelho et al. (2005, 2007).”
An updated MILES stellar library and stellar population models (2011, methodology): “Spectra were retrieved from http://www.cruzeirodosul.edu. br/nat/modelos.html, and are described in Coelho et al. (2005) and Coelho et al. (2007).”
Improving the full spectrum fitting method: accurate convolution with Gauss-Hermite functions (2016, background): “…(ii) individual empirical (e.g. Cenarro et al. 2001; Prugniel & Soubiran 2001; Valdes et al. 2004; Sánchez-Blázquez et al. 2006) or synthetic (e.g. Coelho et al. 2005; Munari et al. 2005; Gustafsson et al. 2008) stars; (iii) principal components derived from a library of spectra; (iv) weighted…”
Chemical similarities between Galactic bulge and local thick disk red giants: O, Na, Mg, Al, Si, Ca, and Ti (2010, background): “Completely avoiding blends is almost an impossible task in cool, relatively metal-rich giants as in our sample, since their spectra are heavily blended with many atomic and molecular lines (e.g. Coelho et al. 2005), in particular due to CN.”
Coudé-feed stellar spectral library – atmospheric parameters (2010, methodology): “The spectra from Coelho et al. (2005) were used to extend the interpolator for the warm stars to low metallicity (down to [Fe/H] = –2.5 dex), and those from Martins et al. (2005), to extend to high and low temperatures.”
Automatic determination of stellar atmospheric parameters and construction of stellar spectral templates of the Guoshoujing Telescope (LAMOST) (2011, methodology): “…synthesis (Martins et al. 2005); a library of high resolution synthetic stellar spectra from 300 nm to 1.8µm with solar andα-enhanced composition (Coelho et al. 2005); UVBLUE (Rodrı́guez-Merino et al. 2005); synthetic stellar and SSP libraries as templates for Gaia simulations (Sordo et…”
New constraints on the chemical evolution of the solar neighbourhood and galactic disc(s) - improved astrophysical parameters for the Geneva-Copenhagen Survey (2011, background): “Determining [α/Fe] becomes increasingly difficult for the hottest and most metal-poor stars, as expectedbecause both atomic and molecular lines get weaker in this regim (e.g. Coelho et al. 2005).”
The metal content of bulge field stars from FLAMES-GIRAFFE spectra - I. Stellar parameters and iron abundances (2008, methodology): “The damping constants, taken from Coelho et al. (2005) were computed where possible, and in particular for most of the FeI lines, using the collisional broadening theory (Barklem, Anstee & O’Mara 1998; Barklem, Piskunov & O’Mara 2000).”
Evolutionary stellar population synthesis with MILES – I. The base models and a new line index system (2010, background): “Alternatively, theoretical stellar libraries at high spectral resolutions have also been developed for this purpose (e.g., Murphy & Meiksin 2004; Zwitter et al. 2004; Rodŕıguez-Merino et al. 2005; Munari et al. 2005; Coelho et al. 2005; Martins & Coelho 2007).”
The APOGEE-2 Survey of the Orion Star-forming Complex. II. Six-dimensional Structure (2018, methodology): “(Chapman & Hall/CRC) Bayo, A., Barrado, D., Stauffer, J., et al. 2011, A&A, 536, A63 Beccari, G., Petr-Gotzens, M. G., Boffin, H. M. J., et al. 2017, A&A, 604, A22 Biazzo, K., Alcalá, J. M., Frasca, A., et al. 2014, A&A, 572, A84 Blaauw, A. 1964, ARA&A, 2, 213 Blanton, M. R., Bershady, M. A., Abolf”
KINEMATIC AND SPATIAL SUBSTRUCTURE IN NGC 2264 (2015, methodology): “The Coelho et al. (2005) templates are computed with a resolution of R ∼ 100,000, much higher resolution than the observed spectra.”
Evolutionary stellar population synthesis with MILES – II. Scaled-solar and α-enhanced models (2015, methodology): “…by guest on 05 M ay 2019 Finally, the very large residuals seen at wavelengths smaller than ∼3800 Å are artificial in the sense that they are a result of the stellar spectra calculations performed by Coelho et al. (2005) who only included the first 10 Hydrogen Balmer transitions.”
Modeling the Panchromatic Spectral Energy Distributions of Galaxies (2013, background): “There are several modern spectral libraries computed byMunari et al. (2005), Martins et al. (2005), and Coelho et al. (2005) that offer fairly wide coverage in parameter space and are at high spectral resolution.”