Difference between revisions of "Triggers:GRBs"
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[[File:plot_grb_eff.png|400px|Thumb Gaia detection efficiency for GRBs in per cents.]] | [[File:plot_grb_eff.png|400px|Thumb Gaia detection efficiency for GRBs in per cents.]] | ||
| − | + | About 5% of GRBs is detectable by Gaia, with the highest efficiency close to the nodes. The main feature visible in the data is steady and rapid decline over AF CCDs. Time sampling at AF CCDs level is 4.4s per CCD. | |
We also demand the transient to be visible in the second FOV (after 105 min). | We also demand the transient to be visible in the second FOV (after 105 min). | ||
[[File:GRB-fraction.png|300px]] from [http://prola.aps.org/abstract/RMP/v76/i4/p1143_1 Piran,2005] | [[File:GRB-fraction.png|300px]] from [http://prola.aps.org/abstract/RMP/v76/i4/p1143_1 Piran,2005] | ||
Revision as of 09:29, 10 September 2009
Very short-lived optical transients associated with enormous gamma-ray outbursts. A catalogue of GRBs is available here. Comprehensive recent review on GRBs and their physics can be found in Piran,2005
- time-scales from seconds to minutes
- in maximum can reach up to few mag, but the whole range observed
- host galaxy can be visible
from Piran, 2005.
from Wozniak et al. 2006
Detecting GRBs with Gaia
About 5% of GRBs is detectable by Gaia, with the highest efficiency close to the nodes. The main feature visible in the data is steady and rapid decline over AF CCDs. Time sampling at AF CCDs level is 4.4s per CCD. We also demand the transient to be visible in the second FOV (after 105 min).
from Piran,2005
