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|Title:||Perspectives on Gamma-Ray Burst Physics and Cosmology with Next Generation Facilities|
Cannizzo, John K.
Tanvir, Nial R.
|Citation:||Space Science Reviews, 2016, in press|
|Abstract:||High-redshift Gamma-Ray Bursts (GRBs) beyond redshift (Formula presented.) are potentially powerful tools to probe the distant early Universe. Their detections in large numbers and at truly high redshifts call for the next generation of high-energy wide-field instruments with unprecedented sensitivity at least one order of magnitude higher than the ones currently in orbit. On the other hand, follow-up observations of the afterglows of high-redshift GRBs and identification of their host galaxies, which would be difficult for the currently operating telescopes, require new, extremely large facilities of at multi-wavelengths. This chapter describes future experiments that are expected to advance this exciting field, both being currently built and being proposed. The legacy of Swift will be continued by SVOM, which is equipped with a set of space-based multi-wavelength instruments as well as and a ground segment including a wide angle camera and two follow-up telescopes. The established Lobster-eye X-ray focusing optics provides a promising technology for the detection of faint GRBs at very large distances, based on which the THESEUS, Einstein Probe and other mission concepts have been proposed. Follow-up observations and exploration of the reionization era will be enabled by large facilities such as SKA in the radio, the 30 m class telescopes in the optical/near-IR, and the space-borne WFIRST and JWST in the optical/near-IR/mid-IR. In addition, the X-ray and (Formula presented.)-ray polarization experiment POLAR is also introduced.|
|Embargo on file until:||21-Jul-2017|
|Rights:||Copyright © 2016 Springer Verlag. Deposited with reference to the publisher’s open access archiving policy.|
|Description:||The file associated with this record is under a 12 month embargo from publication in accordance with the publisher's self-archiving policy. The full text may be available through the publisher links provided above.|
|Appears in Collections:||Published Articles, Dept. of Physics and Astronomy|
Files in This Item:
|1606.09536v1.pdf||Post-review (final submitted author manuscript)||7.13 MB||Adobe PDF||View/Open|
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