Sun

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...)

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)

Data sets ~1321 days in total

Energy spectrum

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

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

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…

Sun: unblinded data

Sun: limits on flux

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:

Sun: limits on σSD (preliminary) G. Lambard