Difference between revisions of "Triggers:GRBs"
From Gaia Science Alerts Working Group
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| + | [[File:GRB-schematic_lightcurve.png|300px|right]] | ||
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Very short-lived optical transients associated with enormous gamma-ray outbursts. | Very short-lived optical transients associated with enormous gamma-ray outbursts. | ||
A catalogue of GRBs is available [http://grad40.as.utexas.edu here]. | A catalogue of GRBs is available [http://grad40.as.utexas.edu here]. | ||
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* host galaxy can be visible | * host galaxy can be visible | ||
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[[File:GRB06-RAPTOR.png|400px]] from [http://ukads.nottingham.ac.uk/abs/2006ApJ...642L..99W Wozniak et al. 2006] | [[File:GRB06-RAPTOR.png|400px]] from [http://ukads.nottingham.ac.uk/abs/2006ApJ...642L..99W Wozniak et al. 2006] | ||
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== Detecting GRBs with Gaia == | == Detecting GRBs with Gaia == | ||
| − | [[File:plot_grb_eff.png|400px|Thumb Gaia detection efficiency for GRBs in per cents.]] | + | [[File:plot_grb_eff.png|400px|Thumb|right|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. | 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). | ||
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| + | [[File:plot_grb_mag.png|200px|right]] | ||
[[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 16:27, 6 October 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 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
