Mini Workshop on neutrino indirect detection of Dark Matter
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Europe/Paris
Description
This workshop is organised by the Dark Matter working groups of the ANTARES and IceCube collaboration to discuss issues of common interest in the dark matter search efforts.
The workshop will also benefit from the presence of various experts :
- Yann Mambrini (Orsay), phenomenologist in Susy and other BSM models
- Emmanuel Nezri (LAM-Marseille), phenomenologist in halo model and neutrino/gamma
indirect detection
- Julien Lavalle (Montpellier), phenomenologist in CR indirect detection
- Steve Muanza (CPPM), specialized in SUSY searches in ATLAS.
A preliminary list of topics to discuss include:
Backgrounds:
- what MCs we use
- Atmospheric mu's: settings (E-range, angular range, atmosphere, seasonal
variations, primary spectrum composition), uncertainties
- Atmospheric nu's: settings (E-range, angular range, spectrum), uncertainites
Signal:
- What MCs we use
- Models to test: (x)MSSM, mUED, non-MSS models, Inert Higgs model...
- parametr scans: format and variables to save. Common scans?
Going beyond grid scans
Cosmological inputs:
- Omega, rho_local, v_local: which best values and uncertainties
- benchmark halo model (which one?)
detector/analysis related:
- Energy threshold to quote results
- reconstruction issues: Low-E reconstruction, cascade reconstruction
.Do we have everything in place to expand searches to other flavors than muons?
.How low in energy we can go? (Neutrino Telescopes are very efficient in constraining high mass WIMPS, but current models favour low masses)
- Search/analysis techniques
- From raw data to final results: how do we set limits.
limits on neutrino flux, muon flux and cross sections
- Systematic uncertainties: how to include them
General:
- Comparisons with direct, other indirect and LHC results.
What do we need? How to present our results so they are
useful to them (and we appear in their plots?)
- How present results in the most model-independent way ?
Hoping to see you in Marseille
Carlos de los Heros
Vincent Bertin
Discussion between the experiments: (backg. MCs, limit setting, systematics, plots...)
Which MCs are we using
How to set limits
How to convert muon fluxes to other quantities
How to compare with other experiments
How to present plots
How to include systematic uncertainties
09:30
SUSY scans in IceCUbe20m
Transparents
10:30
→
11:00
Coffee break
30m
11:00
→
13:00
Discussion between the experiments: (cont.)
Which MCs are we using
How to set limits
How to convert muon fluxes to other quantities
How to compare with other experiments
How to present plots
How to include systematic uncertainties
11:00
Systematics in ANTARES DM analysis20m
Orateur:
M.Sotiris Loucatos(IRFU CEA-Saclay)
Slides
13:00
→
14:15
Lunch
1h 15m
14:15
→
16:15
Galactic analyses: (discussion with E. Nezri and J. Lavalle)
14:15
Relic density, indirect detection on Gamma Rays and Cosmic Rays20m
Orateur:
DrJulien Lavalle(CNRS - LUPM)
Slides
15:00
Dark Matter Halos20m
Orateur:
DrEmmanuel NEZRI(LAM CNRS)
Slides
16:15
→
16:45
Coffee break
30m
16:45
→
18:30
Galactic analyses: (discussion between experiments)
Models and Signal MCs: (discussion with Y. Mambrini)
Flavours of the MSSM
non-MSSM models
MCs: Superbayes, DarkSusy, MicrOmegas
10:30
→
11:00
Coffee break
30m
11:00
→
13:00
Models and Signal MCs: (signal MCs used, models tested, settings, sources...)
Flavours of the MSSM
non-MSSM models
MCs: Superbayes, DarkSusy, MicrOmegas
13:00
→
14:15
Lunch
1h 15m
14:15
→
16:15
Discussion between the experiments: (common issues: parameter scans, limits...)
Which MCs are we using
How to set limits
How to convert muon fluxes to other quantities
How to compare with other experiments
How to present plots
How to include systematic uncertainties
16:15
→
16:35
Coffee break
20m
16:35
→
18:00
Discussion between the experiments: (comparison with other experiments. Discussion with S. Muanza, ATLAS)
Which MCs are we using
How to set limits
How to convert muon fluxes to other quantities
How to compare with other experiments
How to present plots
How to include systematic uncertainties