The effects of binaries on the evolution of UV spectral features in massive starbursts

Belkus, Houria; Bever, J. Van; Vanbeveren, D.

doi:10.1051/0004-6361:20030037

Cited by 28 publications

(33 citation statements)

References 21 publications

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“…The impact of these stars on stellar populations has been studied by multiple authors (e.g. Belkus et al 2003;Zhang et al 2015;Götberg et al 2018). We defer discussion of the ultraviolet upturn behaviour of BPASS v2.2 models to a future paper (in prep).…”

Section: Comparison With Other Stellar Population Synthesis Modelsmentioning

confidence: 99%

“…Other stellar population synthesis codes have begun to consider the effects of binary evolution (e.g. Belkus et al 2003;Zhang et al 2015;Götberg et al 2017Götberg et al , 2018. Amongst these are our Binary Population and Spectral Synthesis (BPASS, Eldridge & Stanway 2009Eldridge et al 2017) models, which have proven remarkably successful at matching the properties of young stellar populations (<100 Myr) across a broad range of environments and redshifts (e.g.…”

Section: Introductionmentioning

confidence: 99%

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Re-evaluating old stellar populations

Stanway

Eldridge

2018

Monthly Notices of the Royal Astronomical Society

468

361

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Determining the properties of old stellar populations (those with age >1 Gyr) has long involved the comparison of their integrated light, either in the form of photometry or spectroscopic indexes, with empirical or synthetic templates. Here we reevaluate the properties of old stellar populations using a new set of stellar population synthesis models, designed to incorporate the effects of binary stellar evolution pathways as a function of stellar mass and age. We find that single-aged stellar population models incorporating binary stars, as well as new stellar evolution and atmosphere models, can reproduce the colours and spectral indices observed in both globular clusters and quiescent galaxies. The best fitting model populations are often younger than those derived from older spectral synthesis models, and may also lie at slightly higher metallicities.

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Section: Comparison With Other Stellar Population Synthesis Modelsmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

Re-evaluating old stellar populations

Stanway

Eldridge

2018

Monthly Notices of the Royal Astronomical Society

468

361

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“…the importance of thermally-pulsating asymptotic giant branch (TP-AGB) stars, whose contribution to the integrated light is being debated (see Maraston 2005Maraston , 2011b, and references therein), and the recurrent question of the importance of binary stars (cf. Vanbeveren et al 1998;Schaerer & Vacca 1998;Belkus et al 2003;Dionne & Robert 2006;Eldridge 2011) For our present objective, first galaxies, uncertainties related to TP-AGB stars are not a major concern, since we are dealing with young stellar populations and focussing on the UV to optical (rest-frame) domain, where these stars can safely be neglected. The evolution of close massive binary stars can alter the predicted spectra of young stellar populations, as illustrated e.g.…”

Section: Stellar Evolutionmentioning

confidence: 99%

Evolutionary Synthesis Models as a Tool and Guide Towards the First Galaxies

Schaerer

2012

The First Galaxies

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We summarize the principles and fundamental ingredients of evolutionary synthesis models, which are stellar evolution, stellar atmospheres, the IMF, starformation histories, nebular emission, and also attenuation from the ISM and IGM. The chapter focusses in particular on issues of importance for predictions of metalpoor and Population III dominated galaxies. We review recent predictions for the main physical properties and related observables of star-forming galaxies based on up-to-date inputs. The predicted metallicity dependence of these quantities and their physical causes are discussed. The predicted observables include in particular the restframe UV-to-optical domain with continuum emission from stars and the ionized ISM, as well as emission lines from H, He, and metals. Based on these predictions we summarize the main observational signatures (emission line strengths, colors etc.), which can be used to distinguish "normal" stellar populations from very metal-poor objects or even Pop III. Evolutionary synthesis models provide an important and fundamental tool for studies of galaxy formation and evolution, from the nearby Universe back to first galaxies. They are used in many applications to interpret existing observations, to predict and guide future missions/instruments, and to allow direct comparisons between state-of-the-art galaxy simulations and observations.

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“…Examples include the evolution of massive-star spectral features in starburst galaxies (Van Bever & Vanbeveren 1998Belkus et al 2003;Brinchmann et al 2008), the ultraviolet upturn in elliptical galaxies (Han et al 2007), the X-ray binary population in galaxies (Van Bever & Vanbeveren 2000), the population of double pulsars (De Donder & Vanbeveren 1998Belczynski et al 2002), the population of carbon-enhanced IAUS266. Close pairs: keys to comprehension of star cluster evolution 297 metal-poor stars (Pols et al 2009) O'Shaughnessy et al 2009); the population of long γ-ray bursts (Detmers et al 2008) and, last but not least, the SNe Ia (see Section 4) which are responsible for some 70% of all iron in the Universe.…”

Section: Vanbeverenmentioning

confidence: 99%

Close pairs: keys to comprehension of star cluster evolution

Vanbeveren

2009

Proc. IAU

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Abstract. In this review I first summarize why binaries are key objects in the study of stellar populations, to understand the evolution of star clusters and galaxies, and thus to understand the universe. I then focus on four specific topics:(i) the formation (through binaries) and evolution of very massive stars in dense clusters and the importance of stellar-wind mass loss. I discuss preliminary computations of wind mass-loss rates of very massive stars performed with the Munich hydrodynamical code and the influence of these new rates on the possible formation of an intermediate-mass black hole in the cluster MGG 11 in M82;(ii) the evolution of intermediate-mass binaries in a starburst with special emphasis on the variation of the supernova (SN) Ia rate (i.e., on the delayed time distribution of SNe Ia). A comparison with SN Ia rates in elliptical galaxies may provide important clues to SN Ia models as well as to the evolution of SN Ia progenitors; (iii) the evolution of double-neutron-star mergers in a starburst (i.e., the delayed time distribution of these mergers) and what this tells us about the suggestion that these mergers may be important production sites of r-process elements; (iv) the possible effect of massive binaries on the self-enrichment of globular clusters.

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The effects of binaries on the evolution of UV spectral features in massive starbursts

Cited by 28 publications

References 21 publications

Re-evaluating old stellar populations

Re-evaluating old stellar populations

Evolutionary Synthesis Models as a Tool and Guide Towards the First Galaxies

Close pairs: keys to comprehension of star cluster evolution

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