A LIBRARY OF THEORETICAL ULTRAVIOLET SPECTRA OF MASSIVE, HOT STARS FOR EVOLUTIONARY SYNTHESIS

By C. Leitherer, Paula A. Ortiz Otálvaro, F. Bresolin, R. Kudritzki, B. Lo Faro, A. Pauldrach, M. Pettini, S. Rix. 2010

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We computed a comprehensive set of theoretical ultraviolet spectra of hot, massive stars with the radiation-hydrodynamics code WM-Basic. This model atmosphere and spectral synthesis code is optimized for computing the strong P Cygni type lines originating in the winds of hot stars, which are the strongest features in the ultraviolet spectral region. The computed set is suitable as a spectral library for inclusion in evolutionary synthesis models of star clusters and star-forming galaxies. The chosen stellar parameters cover the upper left Hertzsprung–Russell diagram at L ≳ 102.75 L☉ and Teff ≳ 20,000 K. The adopted elemental abundances are 0.05 Z☉, 0.2 Z☉, 0.4 Z☉, Z☉, and 2 Z☉. The spectra cover the wavelength range from 900 to 3000 Å and have a resolution of 0.4 Å. We compared the theoretical spectra to data of individual hot stars in the Galaxy and the Magellanic Clouds obtained with the International Ultraviolet Explorer and Far Ultraviolet Spectroscopic Explorer satellites and found very good agreement. We built a library with the set of spectra and implemented it into the evolutionary synthesis code Starburst99 where it complements and extends the existing empirical library toward lower chemical abundances. Comparison of population synthesis models at solar and near-solar composition demonstrates consistency between synthetic spectra generated with either library. We discuss the potential of the new library for the interpretation of the rest-frame ultraviolet spectra of star-forming galaxies. Properties that can be addressed with the models include ages, initial mass function, and heavy-element abundance. The library can be obtained both individually or as part of the Starburst99 package.

Subfields: Astronomy and Astrophysics, Instrumentation

View Paper: https://www.semanticscholar.org/paper/2fba64feb2e1f325ad3d230d44950dfdaa4b7866

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Citations in the corpus

Dancing in the dark: galactic properties trace spin swings along the cosmic web (2014, methodology): “Specifically, the mechanical energy from Type II SNe and stellar winds is taken from STARBURST99 (Leitherer et al. 1999, 2010), and the frequency of Type Ia SN explosions is computed following Greggio & Renzini (1983).”
RECONCILING THE STELLAR AND NEBULAR SPECTRA OF HIGH-REDSHIFT GALAXIES (2016, background): “…wind feature has been discussed by many authors as a potential diagnostic because of its strength and its dependence on stellar metallicity (e.g., Pettini et al. 2000; Leitherer et al. 2001; Shapley et al. 2003; Rix et al. 2004; Steidel et al. 2004; Quider et al. 2009, 2010; Leitherer et al. 2010).”
AN ALMA SURVEY OF SUBMILLIMETER GALAXIES IN THE EXTENDED CHANDRA DEEP FIELD SOUTH: THE REDSHIFT DISTRIBUTION AND EVOLUTION OF SUBMILLIMETER GALAXIES (2013, methodology): “We then define the stellar mass as the total mass in stars and stellar remnants, using Starburst99 to determine the mass lost due to winds and supernovae (Leitherer et al. 1999; Vázquez & Leitherer 2005; Leitherer et al. 2010).”
CONSTRAINING THE LOW-MASS SLOPE OF THE STAR FORMATION SEQUENCE AT 0.5 < z < 2.5 (2014, methodology): “To test our assumption of solar metallicity, we compare spectra produced from the stellar synthesis code Starburst 99 (Leitherer et al. 1999; Vázquez & Leitherer 2005; Leitherer et al. 2010).”
Consistent modelling of the meta-galactic UV background and the thermal/ionization history of the intergalactic medium (2018, methodology): “(11), the function lν [τ, Z(t − τ)] is the specific luminosity per unit initial stellar mass radiated by a single stellar population (SSP) at age τ and metallicity Z(t − τ), that we compute using the code STARBURST99 (Leitherer et al. 1999; Vázquez & Leitherer 2005; Leitherer et al. 2010, 2014).”
The Herschel Dwarf Galaxy Survey - I. Properties of the low-metallicity ISM from PACS spectroscopy (2015, methodology): “The source of radiation is chosen as a young starburst that we simulate with Starburst99 (Leitherer et al. 2010).”
(Star)bursts of FIRE: observational signatures of bursty star formation in galaxies (2015, methodology): “The inputs for the feedback models (such as stellar luminosity and supernova rates) are taken directly from STARBURST99 (Leitherer et al. 1999; Vázquez & Leitherer 2005; Leitherer et al. 2010, 2014).”
Photodissociation and photoionisation of atoms and molecules of astrophysical interest (2017, background): “In reality, stellar spectra are not black bodies but contain many emission or absorption lines (e.g., Ardila et al. 2002a,b; Leitherer et al. 2010).”
Ultraluminous X-ray sources in the Chandra and XMM-Newton era (2011, background): “Invoking 10 to 100 ordinary SN explosions over the last 1 Myr would require a massive star cluster withM & a few 105M⊙ (e.g., from STARBURST99; Leitherer et al. 2010, 1999).”
CLASH: THREE STRONGLY LENSED IMAGES OF A CANDIDATE z ≈ 11 GALAXY (2012, methodology): “800Å even for extremely young stellar populations, according to models like Starburst9922 (Leitherer et al. 1999, 2010).”
Modelling the nebular emission from primeval to present-day star-forming galaxies (2016, background): “…Ekström et al. 2012; Georgy et al. 2013; Chen et al. 2015) and atmospheres (e.g., Hauschildt & Baron 1999; Hillier & Miller 1999; Pauldrach et al. 2001; Lanz & Hubeny 2003, 2007; Hamann & Gräfener 2004; Martins et al. 2005; Puls et al. 2005; Rodŕıguez-Merino et al. 2005; Leitherer et al. 2010).”
THE METALLICITY EVOLUTION OF INTERACTING GALAXIES (2011, methodology): “We calculate the mass return rate, dMgas/dt, directly from Starburst99 synthetic population models (Leitherer et al. 1999; Vázquez & Leitherer 2005; Leitherer et al. 2010).”
Strongly star forming galaxies in the local Universe with nebular He iiλ4686 emission (2012, methodology): “…the He II λ4686 emission and its dependence on the stellar models adopted, we use the latest version (6.0) of the spectral synthesis code STARBURST99 (hereafter STB99; Leitherer et al. 1999, 2010) to calculate spectral energy distribution (SED) predictions for a range of ages and metal abundances.”
THE EFFECTS OF STELLAR ROTATION. II. A COMPREHENSIVE SET OF STARBURST99 MODELS (2014, methodology): “Starburst99 uses the extended, expanding model atmospheres WM-Basic (Pauldrach et al. 1998), CMFGEN (Hillier & Miller 1998, 1999), and PoWR (Gräfener et al. 2002; Hamann & Gräfener 2003, 2004) for its various outputs.”
THE INCIDENCE OF STELLAR MERGERS AND MASS GAINERS AMONG MASSIVE STARS (2013, methodology): “Such properties are generally derived using population synthesis models such as GALAXEV (Bruzual & Charlot 2003), STARBURST99 (Leitherer et al. 2010) and FSPS (Conroy et al. 2009), in which all stars are in principle assumed to evolve in isolation.”
Delay-time distribution of core-collapse supernovae with late events resulting from binary interaction (2017, methodology): “We use the online interface of STARBURST99 (Leitherer et al. 1999; Vázquez & Leitherer 2005; Leitherer et al. 2010, 2014) to compute the DTD, using two sets of assumptions.”
Evolutionary stellar population synthesis with MILES – II. Scaled-solar and α-enhanced models (2015, background): “…al. 2003; Murphy & Meiksin 2004; Zwitter, Castelli & Munari 2004; Coelho et al. 2005; Martins et al. 2005; Munari et al. 2005; Rodrı́guez-Merino et al. 2005; Frémaux et al. 2006; Martins & Coelho 2007; Leitherer et al. 2010; Palacios et al. 2010; Kirby 2011; de Laverny et al. 2012; Coelho 2014).”