English (United Kingdom)

https://curated-unify.zendy.io/wp-json/zendy-region/v1/featured_content/oa?rat=en

https://curated-unify.zendy.io/wp-json/zendy-region/v1/highlighted_journal/

Global: Zendy Plus annual

Presents the access of premium content as premium feature

Premium Content

Presents the keyphrase highlighting as premium feature

Keyphrase Highlighting

Presents the summarisation as premium feature

Summarisation

Insights

Presents the pdf analysis as premium feature

PDF Analysis

Presents the zaia usage as premium feature

ZAIA

Global: Zendy Tools annual

Global: Zendy Free Plan

Global: Zendy Tools monthly

Global: Zendy Plus monthly

We investigate the detectability of a proposed population of Gamma-Ray Bursts(GRBs) from the collapse of Population III (Pop III) stars. The James WebbSpace Telescope (JWST) and Space Infrared telescope for Cosmology andAstrophysics (SPICA) will be able to observe the late time infrared afterglows.We have developed a new method to calculate their detectability, which takesinto account the fundamental initial mass function (IMF) and formation rates ofPop III stars, from which we find the temporal variability of the afterglowsand ultimately the length of time JWST and SPICA can detect them. In the rangeof plausible Pop III GRB parameters, the afterglows are always detectable bythese instruments during the isotropic emission, for a minimum of 55 days and amaximum of 3.7 years. The average number of detectable afterglows will be2.96$\times 10^{-5}$ per SPICA field of view (FOV) and 2.78$\times 10^{-6}$ perJWST FOV. These are lower limits, using a pessimistic estimate of Pop III starformation. An optimal observing strategy with SPICA could identify a candidateorphan afterglow in $\sim 1.3$ years, with a 90 percent probability ofconfirmation with further detailed observations. A beamed GRB will align withthe FOV of the planned GRB detector Energetic X-ray Imaging Survey Telescopeonce every 9 years. Pop III GRBs will be more easily detected by theirisotropic emissions (i.e. orphan afterglows) rather than by their promptemissions.

The Potential for Detecting Gamma-Ray Burst Afterglows from Population III Stars with the Next Generation of Infrared Telescopes