Impact of the Primordial Stellar Initial Mass Function on the 21-cm Signal
| Autor: | T Gessey-Jones, N S Sartorio, A Fialkov, G M Mirouh, M Magg, R G Izzard, E de Lera Acedo, W J Handley, R Barkana |
|---|---|
| Jazyk: | angličtina |
| Rok vydání: | 2022 |
| Předmět: |
Cosmology and Nongalactic Astrophysics (astro-ph.CO)
FOS: Physical sciences Astronomy and Astrophysics Astrophysics::Cosmology and Extragalactic Astrophysics Early Universe Astrophysics - Astrophysics of Galaxies Dark ages reionization first stars Population III [Stars] Astrophysics - Solar and Stellar Astrophysics Space and Planetary Science Astrophysics of Galaxies (astro-ph.GA) Astrophysics::Solar and Stellar Astrophysics Astrophysics::Earth and Planetary Astrophysics Solar and Stellar Astrophysics (astro-ph.SR) Astrophysics::Galaxy Astrophysics Astrophysics - Cosmology and Nongalactic Astrophysics |
| Popis: | Properties of the first generation of stars [referred to as the Population III (Pop III) stars], such as their initial mass function (IMF), are poorly constrained by observations and have yet to converge between simulations. The cosmological 21-cm signal of neutral hydrogen is predicted to be sensitive to Lyman-band photons produced by these stars, thus providing a unique way to probe the first stellar population. In this paper, we investigate the impacts of the Pop III IMF on the cosmic-dawn 21-cm signal via the Wouthuysen-Field effect, Lyman-Werner feedback, Ly alpha heating, and cosmic microwave background heating. We calculate the emission spectra of star-forming haloes for different IMFs by integrating over individual metal-free stellar spectra, computed from a set of stellar evolution histories and stellar atmospheres, and taking into account variability of the spectra with stellar age. Through this study, we therefore relax two common assumptions: that the zero-age main-sequence emission rate of a Pop III star is representative of its lifetime mean emission rate, and that Pop III emission can be treated as instantaneous. Exploring bottom-heavy, top-heavy, and intermediate IMFs, we show that variations in the 21-cm signal are driven by stars lighter than 20 M-circle dot. For the explored models, we find maximum relative differences of 59 per cent in the cosmic-dawn global 21-cm signal, and 131 per cent between power spectra. Although this impact is modest, precise modelling of the first stars and their evolution is necessary for accurate prediction and interpretation of the 21-cm signal. UK Research & Innovation (UKRI) Science & Technology Facilities Council (STFC) Science and Technology Development Fund (STDF) ST/V506606/1 AF's Royal Society University Research Fellowship 181073 180523 Science & Technology Facilities Council (STFC) ST/R000603/1 Max-Planck-Gesellschaft via the fellowship of the International Max Planck Research School for Astronomy and Cosmic Physics at the University of Heidelberg (IMPRS-HD) Science & Technology Facilities Council (STFC) ST/R000603/1 ST/L003910/1 Royal Society of London Israel Science Foundation 2359/20 Ambrose Monell Foundation Institute for Advanced Study Vera Rubin Presidential Chair in Astronomy The David & Lucile Packard Foundation |
| Databáze: | OpenAIRE |
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