RS Oph paper meetings
Revision as of 10:43, 29 April 2022 by AAguascaCabot (talk | contribs)
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
- Discussion
- - Use new MC production for the RS Oph analysis
- To be done:
- - Use the best spectral model for each day to plot the daily flux.
- - Cross-check Jakub's UL implementation using gammapy.
- Slides
2022-04-13
- Discussion
- - Optimised cuts using Crab data may not be optimal because of the different spectral index between RS Oph and Crab Nebula. Maybe it is better to obtain the best quality cuts using MC simulations weighted to the spectral index of RS Oph.
- - Analysis of ULs for the data after moon break using gammapy is complicated because we do not have significant detection (\sim 2 sig).
- To be done:
- - Castro's plots.
- - Investigate how to implement UL calculation.
- Slides
