The potential for detecting gamma-ray burst afterglows from population III stars with the next generation of infrared telescopes
We investigate the detectability of a proposed population of gamma-ray bursts (GRBs) from the collapse of Population III (Pop III) stars. The James Webb Space Telescope (JWST) and Space Infrared Telescope for Cosmology and Astrophysics (SPICA) will be able to observe the late time infrared afterglow...
| Main Authors: | , , |
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| Format: | Journal Article |
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IOP Publishing Ltd.
2013
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| Online Access: | http://hdl.handle.net/20.500.11937/18737 |
| _version_ | 1848749830365511680 |
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| author | Macpherson, D. Coward, D. Zadnik, Marjan |
| author_facet | Macpherson, D. Coward, D. Zadnik, Marjan |
| author_sort | Macpherson, D. |
| building | Curtin Institutional Repository |
| collection | Online Access |
| description | We investigate the detectability of a proposed population of gamma-ray bursts (GRBs) from the collapse of Population III (Pop III) stars. The James Webb Space Telescope (JWST) and Space Infrared Telescope for Cosmology and Astrophysics (SPICA) will be able to observe the late time infrared afterglows. We have developed a new method to calculate their detectability, which takes into account the fundamental initial mass function and formation rates of Pop III stars, from which we find the temporal variability of the afterglows and ultimately the length of time JWST and SPICA can detect them. In the range of plausible Pop III GRB parameters, the afterglows are always detectable by these instruments during the isotropic emission, for a minimum of 55 days and a maximum of 3.7 yr. The average number of detectable afterglows will be 2.96× 10–5 per SPICA field of view (FOV) and 2.78× 10–6 per JWST FOV. These are lower limits, using a pessimistic estimate of Pop III star formation. An optimal observing strategy with SPICA could identify a candidate orphan afterglow in ~1.3 yr, with a 90% probability of confirmation with further detailed observations. A beamed GRB will align with the FOV of the planned GRB detector Energetic X-ray Imaging Survey Telescope once every 9 yr. Pop III GRBs will be more easily detected by their isotropic emissions (i.e., orphan afterglows) rather than by their prompt emissions. |
| first_indexed | 2025-11-14T07:27:10Z |
| format | Journal Article |
| id | curtin-20.500.11937-18737 |
| institution | Curtin University Malaysia |
| institution_category | Local University |
| last_indexed | 2025-11-14T07:27:10Z |
| publishDate | 2013 |
| publisher | IOP Publishing Ltd. |
| recordtype | eprints |
| repository_type | Digital Repository |
| spelling | curtin-20.500.11937-187372017-09-13T13:46:48Z The potential for detecting gamma-ray burst afterglows from population III stars with the next generation of infrared telescopes Macpherson, D. Coward, D. Zadnik, Marjan stars gamma-ray burst Population III general We investigate the detectability of a proposed population of gamma-ray bursts (GRBs) from the collapse of Population III (Pop III) stars. The James Webb Space Telescope (JWST) and Space Infrared Telescope for Cosmology and Astrophysics (SPICA) will be able to observe the late time infrared afterglows. We have developed a new method to calculate their detectability, which takes into account the fundamental initial mass function and formation rates of Pop III stars, from which we find the temporal variability of the afterglows and ultimately the length of time JWST and SPICA can detect them. In the range of plausible Pop III GRB parameters, the afterglows are always detectable by these instruments during the isotropic emission, for a minimum of 55 days and a maximum of 3.7 yr. The average number of detectable afterglows will be 2.96× 10–5 per SPICA field of view (FOV) and 2.78× 10–6 per JWST FOV. These are lower limits, using a pessimistic estimate of Pop III star formation. An optimal observing strategy with SPICA could identify a candidate orphan afterglow in ~1.3 yr, with a 90% probability of confirmation with further detailed observations. A beamed GRB will align with the FOV of the planned GRB detector Energetic X-ray Imaging Survey Telescope once every 9 yr. Pop III GRBs will be more easily detected by their isotropic emissions (i.e., orphan afterglows) rather than by their prompt emissions. 2013 Journal Article http://hdl.handle.net/20.500.11937/18737 10.1088/0004-637X/779/1/73 IOP Publishing Ltd. fulltext |
| spellingShingle | stars gamma-ray burst Population III general Macpherson, D. Coward, D. Zadnik, Marjan The potential for detecting gamma-ray burst afterglows from population III stars with the next generation of infrared telescopes |
| title | The potential for detecting gamma-ray burst afterglows from population III stars with the next generation of infrared telescopes |
| title_full | The potential for detecting gamma-ray burst afterglows from population III stars with the next generation of infrared telescopes |
| title_fullStr | The potential for detecting gamma-ray burst afterglows from population III stars with the next generation of infrared telescopes |
| title_full_unstemmed | The potential for detecting gamma-ray burst afterglows from population III stars with the next generation of infrared telescopes |
| title_short | The potential for detecting gamma-ray burst afterglows from population III stars with the next generation of infrared telescopes |
| title_sort | potential for detecting gamma-ray burst afterglows from population iii stars with the next generation of infrared telescopes |
| topic | stars gamma-ray burst Population III general |
| url | http://hdl.handle.net/20.500.11937/18737 |