Difference between revisions of "RS Oph paper meetings"
Misabelber (talk | contribs) |
|||
| Line 28: | Line 28: | ||
* Yukiho | * Yukiho | ||
[[Media:RSOphMeeting20220330Yukiho.pdf]] | [[Media:RSOphMeeting20220330Yukiho.pdf]] | ||
| + | * Mab | ||
| + | [[Media:13042022_RS_Ophiuchi_Analysis_update_MabBernardos_compressed.pdf]] | ||
Revision as of 12:17, 13 April 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
- Yukiho
Media:RSOphMeeting20220330Yukiho.pdf
- Mab
Media:13042022_RS_Ophiuchi_Analysis_update_MabBernardos_compressed.pdf
