Detectability of the first cosmic explosions
We present a fully self-consistent simulation of a synthetic survey of the furthermost cosmic explosions. The appearance of the first generation of stars (Population III) in the Universe represents a critical point during cosmic evolution, signalling the end of the dark ages, a period of absence of...
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| Hauptverfasser: | , , , , |
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| Dokumenttyp: | Article (Journal) |
| Sprache: | Englisch |
| Veröffentlicht: |
2013 October 16
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| In: |
Monthly notices of the Royal Astronomical Society
Year: 2013, Jahrgang: 436, Heft: 2, Pages: 1555-1563 |
| ISSN: | 1365-2966 |
| DOI: | 10.1093/mnras/stt1680 |
| Online-Zugang: | Verlag, lizenzpflichtig, Volltext: https://doi.org/10.1093/mnras/stt1680
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| Verfasserangaben: | R.S. de Souza, E.E.O. Ishida, J.L. Johnson, D.J. Whalen and A. Mesinger |
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| 100 | 1 | |a Souza, Rafael S. de |e VerfasserIn |0 (DE-588)1134896271 |0 (DE-627)889772681 |0 (DE-576)486417379 |4 aut | |
| 245 | 1 | 0 | |a Detectability of the first cosmic explosions |c R.S. de Souza, E.E.O. Ishida, J.L. Johnson, D.J. Whalen and A. Mesinger |
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| 520 | |a We present a fully self-consistent simulation of a synthetic survey of the furthermost cosmic explosions. The appearance of the first generation of stars (Population III) in the Universe represents a critical point during cosmic evolution, signalling the end of the dark ages, a period of absence of light sources. Despite their importance, there is no confirmed detection of Population III stars so far. A fraction of these primordial stars are expected to die as pair-instability supernovae (PISNe), and should be bright enough to be observed up to a few hundred million years after the big bang. While the quest for Population III stars continues, detailed theoretical models and computer simulations serve as a testbed for their observability. With the upcoming near-infrared missions, estimates of the feasibility of detecting PISNe are not only timely but imperative. To address this problem, we combine state-of-the-art cosmological and radiative simulations into a complete and self-consistent framework, which includes detailed features of the observational process. We show that a dedicated observational strategy using ≲ 8 per cent of the total allocation time of the James Webb Space Telescope mission can provide us with up to ∼9-15 detectable PISNe per year. | ||
| 700 | 1 | |a Ishida, E. E. O. |e VerfasserIn |4 aut | |
| 700 | 1 | |a Johnson, J. L. |e VerfasserIn |4 aut | |
| 700 | 1 | |a Whalen, Daniel J. |e VerfasserIn |0 (DE-588)1078317976 |0 (DE-627)83831421X |0 (DE-576)450461009 |4 aut | |
| 700 | 1 | |a Mesinger, A. |e VerfasserIn |4 aut | |
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