1. Sun

2. Sun: simulation with WIMPSIM
νe, νμ, ντ
Sun
Earth
Blennow, Edsjö, Ohlsson (03/2008): “WIMPSIM” model-independent production
Great statistics with 12×106 WIMPs annihilations
Capture rate and annihilations in equilibrium at the Sun core
Annihilations in c,b and t quarks, τ leptons and direct channels
Interactions taken into account in the Sun medium
Three flavors oscillations, regeneration of τ leptons in the Sun medium (Bahcall et al.) available parameters (WIMPs mass, oscillations parameters...)

3. Some jargon Reconstruction strategies: Cuts:
BBFit  low energies/masses (<250 GeV)
Single line (only hits in one line, no azimuth information)  very low energies
Multiline
AAFit (likelihood based)  high energies/masses (>250 GeV)
Cuts used:
lambda (quality parameter, basically the likelihood value)
beta: angular error estimation
Cuts:
tchi2: ~ χ2 (BBFit)
lambda: Quality reconstruction parameter ~ likelihood (AAFit)
beta: angular error estimate (AAFit)

4. Data sets
~1321 days in total

5. Energy spectrum

6. Sun: detector response
DM analyses are in the “low energy” range of neutrino telescopes
12 lines
Angular resolution
5 lines
9 lines
12 lines
kinematic

7. Sun: background estimation
The background is estimated by scrambling the data in time
The effect of the visibility of the Sun is taken into account

8. Sun: cut optimization
Neutrino flux at the Earth x Detector Efficiency x Visibility  Signal
Data in the Sun direction time scrambled  Background
Cuts on the angular window size and on the track quality cut are chosen to optimize the flux sensitivity
Once the optimum quality cuts are chosen we proceed to unblind…

9. Sun: unblinded data

10. Sun: limits on flux

11. Cross section calculation
Differential neutrino flux is related
with the annihilation rate as:
If we assume equilibrium between capture and annihilation in the Sun:
where the capture rate can be expressed as:

12. Sun: limits on σSD
(preliminary)
G. Lambard