Difference between revisions of "RS Oph paper meetings"
| Line 21: | Line 21: | ||
* To be done: | * To be done: | ||
| − | :- Several checks | + | :- Several checks using the Crab. Using 3 different datasets: 20201120, September 2021 and March 2022. For the MC prod, use the same one that we use for RS Oph (parameters for dark conditions) |
| − | :- Compare sensitivity | + | :- Compare IRF/sensitivity for our MC prod with the standard MC prod. |
{{Date|2022-03-30}} | {{Date|2022-03-30}} | ||
Revision as of 13:29, 23 March 2022
2022-02-09
Kick off meeting, division of the work. We decided that we should To be done: LST analysis, Fermi analysis, we decided not to go for optical analysis => will use the data that will be published by MAGIC
2022-02-23
- To be done:
- - LST analysis
- - produce MC production with specific NSB parameters, zenith and azimuth angles for RS Oph observation conditions.
2022-03-09
- Discussion
- - Runs in dark conditions present similar pixel charge distribution. We exclude the ones with runs affected by moon or strange distribution.
- Presented
- - First results using the IRFs computed by lstmcpipe.
- - First result analysis RS Oph with Fermi data
- To be done:
- - Several checks using the Crab. Using 3 different datasets: 20201120, September 2021 and March 2022. For the MC prod, use the same one that we use for RS Oph (parameters for dark conditions)
- - Compare IRF/sensitivity for our MC prod with the standard MC prod.
2022-03-30
