Gamma-Ray Bursts as Cosmological Tools
2009 (English)Article in journal (Refereed) Submitted
In recent years there has been considerable activity in using gamma-ray bursts as cosmological probes for determining global cosmological parameters complementing results from type Ia supernovae and other methods. This requires a characteristics of the source to be a standard candle. We show that contrary to earlier indications the accumulated data speak against this possibility. Another method would be to use correlation between a distance dependent and a distance independent variable to measure distance and determine cosmological parameters as is done using Cepheid variables and to some extent Type Ia supernovae. Many papers have dealt with the use of so called Amati relation, first predicted by Lloyd, Petrosian and Mallozzi, or the Ghirlanda relation for this purpose. We have argued that these procedure involve many unjustified assumptions which if not true could invalidate the results. In particular, we point out that many evolutionary effects can affect the final outcome. In particular, we demonstrate that the existing data from Swift and other earlier satellites show that the gamma-ray burst may have undergone luminosity evolution. Similar evolution may be present for other variables such as the peak photon energy of the total radiated energy. Another out come of our analysis is determination of the luminosity function and the comoving rate evolution of gamma-ray bursts which does not seem to agree with the cosmic star formation rate. We caution however, that the above result are preliminary and includes primarily the effect of detection threshold. Other selection effects, perhaps less important than this, are also known to be present and must be accounted for. We intend to address these issues in future publications.
Place, publisher, year, edition, pages
Astrophysics - High Energy Astrophysical Phenomena
Astronomy, Astrophysics and Cosmology
IdentifiersURN: urn:nbn:se:kth:diva-81243OAI: oai:DiVA.org:kth-81243DiVA: diva2:497510
QS 2012 QS 201203152012-02-102012-02-102012-03-15Bibliographically approved