Astronomy and Astrophysics – Astrophysics
Scientific paper
2003-07-28
Astrophys.J.604:508-520,2004
Astronomy and Astrophysics
Astrophysics
Revised version, with a new figure and broader parameter range
Scientific paper
10.1086/382061
Gamma-ray bursts are promising tools for tracing the formation of high redshift stars, including the first generation. At very high redshifts the reverse shock emission lasts longer in the observer frame, and its importance for detection and analysis purposes relative to the forward shock increases. We consider two different models for the GRB environment, based on current ideas about the redshift dependence of gas properties in galaxies and primordial star formation. We calculate the observed flux as a function of the redshift and observer time for typical GRB afterglows, taking into account intergalactic photoionization and Lyman-$\alpha$ absorption opacity as well as extinction by the Milky Way Galaxy. The fluxes in the X-ray and near IR bands are compared with the sensitivity of different detectors such as Chandra, XMM, Swift XRT and JWST. Using standard assumptions, we find that Chandra, XMM and Swift XRT can potentially detect GRBs in the X-ray band out to very high redshifts $z\gtrsim$ 30. In the K and M bands, the JWST and ground-based telescopes are potentially able to detect GRBs even one day after the trigger out to $z\sim$ 16 and 33, if present. While the X-ray band is insensitive to the external density and to reverse shocks, the near IR bands provide a sensitive tool for diagnosing both the environment and the reverse shock component.
Abel Tom
Gou Li-Jun
Meszaros Peter
Zhang Baigang
No associations
LandOfFree
Detectability of Long GRB Afterglows from Very High Redshifts does not yet have a rating. At this time, there are no reviews or comments for this scientific paper.
If you have personal experience with Detectability of Long GRB Afterglows from Very High Redshifts, we encourage you to share that experience with our LandOfFree.com community. Your opinion is very important and Detectability of Long GRB Afterglows from Very High Redshifts will most certainly appreciate the feedback.
Profile ID: LFWR-SCP-O-42