THE EFFECTS OF STELLAR ROTATION. II. A COMPREHENSIVE SET OF STARBURST99 MODELS

By C. Leitherer, S. Ekström, G. Meynet, Daniel Schaerer, K. B. Agienko, Emily M. Levesque. 2014

345 citations recorded by the source corpus.

We present a new set of synthesis models for stellar populations obtained with Starburst99 and based on new stellar evolutionary tracks with rotation. We discuss models with zero rotation velocity and with velocities of 40% of the break-up velocity on the zero-age main-sequence. These values are expected to bracket realistic rotation velocity distributions in stellar populations. The new rotating models for massive stars are more luminous and hotter due to a larger convective core and enhanced surface abundances. This results in pronounced changes in the integrated spectral energy distribution of a population containing massive stars. The changes are most significant at the shortest wavelengths where an increase of the ionizing luminosity by up to a factor of five is predicted. We also show that high equivalent widths of recombination lines may not necessarily indicate a very young age but can be achieved at ages as late as ∼107 yr. Comparison of these two boundary cases (0% and 40% of the break-up velocity) will allow users to evaluate the effects of rotation and provide guidance for calibrating the stellar evolution models. We also introduce a new theoretical ultraviolet spectral library built from the Potsdam Wolf–Rayet atmospheres. Its purpose is to help identify signatures of Wolf–Rayet stars in the ultraviolet whose strength is sensitive to the particulars of the evolution models. The new models are available for solar and one-seventh solar metallicities. A complete suite of models can be generated on the Starburst99 Web site. The updated Starburst99 package can be retrieved from that Web site as well.

Subfields: Astronomy and Astrophysics, Education, Instrumentation

View Paper: https://www.semanticscholar.org/paper/57c3afdec8001a59082ab9775d80e37f8feb17b4

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Citations in the corpus

Detection of high Lyman continuum leakage from four low-redshift compact star-forming galaxies (2016, methodology): “These relations were calculated with Starburst99 models (Leitherer et al. 1999, 2014) adopting a Salpeter (1955) IMF, a combination of stellar atmosphere models by Lejeune et al. (1997) and Schmutz et al. (1992), and various Geneva evolutionary tracks for non-rotating and rotating stars.”
Binary Population and Spectral Synthesis Version 2.1: Construction, Observational Verification, and New Results (2017, background): “Perhaps, the most direct comparison is between BPASS and the STARBURST99 models (Leitherer et al. 1999; Leitherer et al. 2014, hereafter S99), both of which were originally designed and optimised for young starbursts.”
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 lifecycle of molecular clouds in nearby star-forming disc galaxies (2019, methodology): “…a Chabrier (2005) initial mass function (IMF) and use Geneva stellar evolutionary tracks (Schaller et al. 1992) with STARBURST99 spectral synthesis (Leitherer et al. 2014).8 Haydon et al. (2018) calibrate tstar,ref using an SPS model describing an instantaneous burst of star formation, to avoid…”
De re metallica: the cosmic chemical evolution of galaxies (2018, background): “These have been extensively used to investigate the chemical enrichment of the circumgalactic/intergalactic medium and in the interstellar medium of galaxies (e.g. Le Brun et al., 1997; Rauch, 1998; Pettini et al., 2002a; Noterdaeme et al., 2008; Lehnert et al., 2009; Steidel et al., 2010; Rafelski ”
Lyα EMISSION FROM GREEN PEAS: THE ROLE OF CIRCUMGALACTIC GAS DENSITY, COVERING, AND KINEMATICS (2015, methodology): “In the top left panel of Figures 6–8, we show a 50Myr old, continuous star-forming model spectrum, with Z = 0.002 (Leitherer et al. 2014).”
The First Billion Years project: the escape fraction of ionizing photons in the epoch of reionization (2015, methodology): “Depending on the physics included in the stellar synthesis models, this could vary by a factor of ∼ 2 − 5 (Eldridge & Stanway 2009; Leitherer et al. 2014).”
Stellar population effects on the inferred photon density at reionization (2015, background): “…combine theoretical (atmosphere and evolution) models or empirical spectra of individual stars, assuming some initial mass function (IMF) and stellar population age, and process the resultant emission through dust and gas screens to calculate an ‘observed’ spectrum (Leitherer et al. 1999, 2014).”
J1154+2443: a low-redshift compact star-forming galaxy with a 46 per cent leakage of Lyman continuum photons (2017, methodology): “A grid of instantaneous burst SEDs with a wide range of ages from 0 Myr to 15 Gyr was calculated with starburst99 (Leitherer et al. 1999, 2014) to derive the SED of the galaxy stellar component.”
ALMA SPECTROSCOPIC SURVEY IN THE HUBBLE ULTRA DEEP FIELD: THE INFRARED EXCESS OF UV-SELECTED z = 2–10 GALAXIES AS A FUNCTION OF UV-CONTINUUM SLOPE AND STELLAR MASS (2016, background): “…to output large amounts of ionizing radiation tens of million of years after an initial burst of star formation (e.g., Yoon et al. 2006; Eldridge & Stanway 2009, 2012; Levesque et al. 2012; de Mink et al. 2013; Kewley et al. 2013; Leitherer et al. 2014; Szécsi et al. 2015; Gräfener et al. 2015).”
Double neutron stars: merger rates revisited (2017, methodology): “Klencki et al. (in prep.) with the use of the Starburst99 code (Leitherer et al. 1999, 2014) calculated the correction factor KIMF=0.51 which can be used as a multiplicative factor in equation B1 to calculate the rate density in a more consistent manner (see section 2 and appendix therein).”
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.”
THE MOSDEF SURVEY: ELECTRON DENSITY AND IONIZATION PARAMETER AT z ∼ 2.3 (2015, methodology): “…for the existence of the metallicity-ionization parameter anti-correlation The argument for an anti-correlation between O/H and ionization parameter arises from the fact that lowmetallicity stars produce more ionizing photons in total and have harder ionizing spectrum (Leitherer et al. 2014).”
The HDUV Survey: A Revised Assessment of the Relationship between UV Slope and Dust Attenuation for High-redshift Galaxies (2017, background): “A secondary effect that will boost ξion above the predictions from single star solar metallicity stellar population models is the higher ionizing photon output associated with lower metallicity and rotating massive stars (Eldridge & Stanway 2009; Leitherer et al. 2014).”
(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).”
RECONCILING THE STELLAR AND NEBULAR SPECTRA OF HIGH-REDSHIFT GALAXIES (2016, methodology): “15 For direct comparison to the KBSS-LM1 far-UV spectrum, we used the high-resolution WM-Basic spectra covering the wavelength range 900-3000 Å spectral resolution of 0.4 Å provided by Starburst99, which we smoothed and re-sampled to match the wavelength scale and spectral resolution of the LM1 comp”