Difference between revisions of "Verification phase"

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Main aim of the Verification Phase is to verify the robustness of the issued alerts and confirm them with the dedicated set of follow-up telescopes. This should reveal all necessary  adjustments to be done in the detection algorithm to assure the best and the most robust performance later on.
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Main aim of the Verification Phase is to verify the robustness of the issued alerts and confirm them with the dedicated set of follow-up telescopes available for ''Target of Opportunity'' (ToO) mode. This should reveal all necessary  adjustments to be done in the detection algorithm to assure the best and the most robust performance later on.
 
   
 
   
 
Verification Phase will last for 2-3 months and is planned to take place as early in the mission as possible, as soon as the alerting system is ready to perform.  
 
Verification Phase will last for 2-3 months and is planned to take place as early in the mission as possible, as soon as the alerting system is ready to perform.  
 
Currently, it seems it will happen only after the first cycle (half a year, i.e. late 2012/early 2013), as the accumulated data ("baseline flux") will not be available before.
 
Currently, it seems it will happen only after the first cycle (half a year, i.e. late 2012/early 2013), as the accumulated data ("baseline flux") will not be available before.
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== Preliminary list of telescopes and people involved ==
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{| border="1" style="width:85%;"
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!Telescope/Observatory || Contact person (with email) || Details
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|-
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|Swiss Euler || Laurent Eyer (laurent.eyer@unige.ch) || 1.2m, La Silla, Chile
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|-
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|Belgian Mecatore || Laurent Eyer || 1.2m, La Palma (Swiss Time)
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|-
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|Loiano || Gisella Clementini (gisella.clementini@oabo.inaf.it) || 1.5m, Bologna, Italy
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|-
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|Konkoly || Laszlo Szabados (szabados@szombat.konkoly.hu) ||
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|-
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|}

Revision as of 11:48, 23 March 2010

Main aim of the Verification Phase is to verify the robustness of the issued alerts and confirm them with the dedicated set of follow-up telescopes available for Target of Opportunity (ToO) mode. This should reveal all necessary adjustments to be done in the detection algorithm to assure the best and the most robust performance later on.

Verification Phase will last for 2-3 months and is planned to take place as early in the mission as possible, as soon as the alerting system is ready to perform. Currently, it seems it will happen only after the first cycle (half a year, i.e. late 2012/early 2013), as the accumulated data ("baseline flux") will not be available before.

Preliminary list of telescopes and people involved

Telescope/Observatory Contact person (with email) Details
Swiss Euler Laurent Eyer (laurent.eyer@unige.ch) 1.2m, La Silla, Chile
Belgian Mecatore Laurent Eyer 1.2m, La Palma (Swiss Time)
Loiano Gisella Clementini (gisella.clementini@oabo.inaf.it) 1.5m, Bologna, Italy
Konkoly Laszlo Szabados (szabados@szombat.konkoly.hu)