Impact of the Primordial Stellar Initial Mass Function on the 21-cm Signal
| Autor: | Gessey-Jones, T., Sartorio, N. S., Fialkov, A., Mirouh, G. M., Magg, M., Izzard, R. G., Acedo, E. de Lera, Handley, W. J., Barkana, R. |
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| Rok vydání: | 2022 |
| Předmět: | |
| Zdroj: | Monthly Notices of the Royal Astronomical Society, Volume 516, Issue 1, October 2022, Pages 841-860 |
| Druh dokumentu: | Working Paper |
| DOI: | 10.1093/mnras/stac2049 |
| Popis: | Properties of the first generation of stars (Pop III), 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 CMB heating. We calculate the emission spectra of star-forming halos 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 a bottom-heavy, a top-heavy, and intermediate IMFs, we show that variations in the 21-cm signal are driven by stars lighter than 20 solar masses. For the explored models we find maximum relative differences of 59% in the cosmic dawn global 21-cm signal, and 131% 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. Comment: 20 pages, 16 figures. Accepted for publication in MNRAS, updated to accepted version |
| Databáze: | arXiv |
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