discovery potential of Galactic sources R. Coniglione discovery potential of Galactic sources 29-31 January 2013 Marseille R. Coniglione, P. Sapienza and A. Trovato INFN - Laboratori Nazionali del Sud

Estimate of FoM (time needed to make a 5s discovery with 50% probability) for Galactic sources RXJ1713 (Piera talk) Vela X Vela Junior Fermi bubbles R. Coniglione 29-31 January 2013 Marseille

The simulations The codes: ANTARES codes modified for KM3NeT with multi-PMT (details in Annarita’s talk) The detector: 2 blocks of 310 strings (20 floors/string 40m distant) with MultiPMT. Distance between strings 100m. Total volume 3.8 km3 (String distance optimization in Piera’s talk) Genhen Neutrino generator KM3 Light & hits GENDET geometry MODK40 40K Background hits Running on Lyon clusters RECO Reconstruction code I/O format -> ASCII files R. Coniglione 29-31 January 2013 Marseille

The method Best flux value from the minimization of MDP Na is the number of signal events that exceed the background with a significance a with a 50% of probability Minimization on L (good reconstructed tracks)and Nhit (related to muon energy) and Rbin (search cone) R. Coniglione 29-31 January 2013 Marseille

The Pulsar Wind Nebula Vela X R. Coniglione 29-31 January 2013 Marseille

VelaX Gamma spectrum d=-45.6° Extension: Inner region 0.8° Total 1.2° New HESS paper appeared on ArXiv in October 2012 and now on Astronomy and Astrophysics 548 (2012) A38 with a higher flux measurement. (53h 2012/ 12h 2006 of observation) Observation up to 50 TeV d=-45.6° Extension: Inner region 0.8° Total 1.2° R. Coniglione 29-31 January 2013 Marseille

Gamma spectra N (GeV-1s-1cm-2) G Ecut (TeV) F>1TeV (s-1cm-2) RXJ1713 2.13 10-14 2.04 17.9 1.68 10-11 VelaX 2006* 1.03 10-14 1.45 13.8 1.28 10-11 VelaX 2012 total 1.46 10-14 1.32 14.0 2.10 10-11 VelaX 2012 inner 1.16 10-14 1.36 13.9 1.6 10-11 * F. Aharonian et al., Astronomy & Astrophysics L43 448 (2006) R. Coniglione 29-31 January 2013 Marseille

Neutrino spectra Main hypothesis are: Full hadronic mechanism and source transparent to gamma In the Vissani prescription neutrino flux is estimated from Gamma yield Gamma from h and neutrino oscillations taken into account with In Kappes et al., ApJ 656 (2007) 870 a parameterization of pion production and decay in hadronic interaction is used to evaluate the relationship between g-ray, p and n spectra in the hypothesis that the proton spectrum is a power law. From the fit of observed gamma spectra the neutrino spectra parameters are evaluated. Oscillations are taken into account with R. Coniglione 29-31 January 2013 Marseille

Neutrino spectra R. Coniglione 29-31 January 2013 Marseille

Neutrino spectra N (GeV-1s-1cm-2) G Ecut (TeV) F>1TeV (s-1cm-2) * Vela X 2006 Kappes (Ref. 1)* 11.75 10-15 0.98 0.84 4.32 10-12 VelaX 2006 Vissani (Ref. 2)** 0.60 10-14 1.45 7.22 5.76 10-12 VelaX 2012 total Vissani (Ref. 2)** 0.93 10-14 1.32 8 10.3 10-11 VelaX 2012 inner Vissani ( Ref. 2)** 0.72 10-14 1.36 7 7.36 10-11 * Ref. 1 Kappes et al., ApJ 656 (2007) 870. Ref. 2 From gamma to neutrino spectra following Vissani prescription F.L. Villante and F. Vissani, Phys. Rev. D 78 (2008) 103007; F. Vissani and F.L. Villante, Nucl. Inst. Meth. A588 (2008) 123; F. Vissani, Astropart. Phys. 26 (2006) 310 ** R. Coniglione 29-31 January 2013 Marseille

Simulation results Years for discovery 5s 50% 3s 50% 7.5 2.6 5.2 1.8 Source at d=-45.6° with a flat disk distribution of 0.8° (inner part of VelaX) Reconstruction with scanning 3°x3° no morphology in simulation no atmospheric muons Years for discovery 5s 50% 3s 50% Vela X 2006 Kappes 7.5 2.6 VelaX 2006 Vissani 5.2 1.8 VelaX 2012 inner Vissani 2.8 1.1 R. Coniglione 29-31 January 2013 Marseille

The SuperNova Remnant Vela junior R. Coniglione 29-31 January 2013 Marseille

Vela Junior gamma spectrum SNR Vela Junior d=-46.37° F. Aharonian et al., Astrophys. Journal (2007) 236 data from December 2004 to May 2005 (33h of ON-source run) Observation up to ≈20 TeV no cut off observed Radial profile G=2.24 N=1.9 10-14 R. Coniglione 29-31 January 2013 Marseille

Vela Junior gamma spectrum SNR Vela Junior d=-46.37° Manuel Paz Arribas et al., ICRC 2011 Amount of data increased of a factor 2 data from 2004 to 2009 (72h of live time after data quality selection) Morphology analysis -> NO absolute flux values -> *N extracted from 2007 values N (GeV-1s-1cm-2) G Ecut (TeV) F>1TeV (s-1cm-2) VelaJ 2007 *1.89 10-14 2.24 - 1.52 10-11 VelaJ ICRC 2011 single region *1.69 10-14 2.11 VelaJ ICRC 2011 whole *1.86 10-14 2.22 R. Coniglione 29-31 January 2013 Marseille

Vela Junior neutrino spectrum * ** N (GeV-1s-1cm-2) G Ecut (TeV) F>1TeV (s-1cm-2) VelaJ Vissani 2007** 6.6 10-15 2.24 - 5.30 10-12 VelaJ Vissani ICRC 2011 single region** 2.64 10-15 2.11 5.71 10-12 VelaJ Kappes* 1.67 10-14 1.72 1.19 4.84 10-12 R. Coniglione 29-31 January 2013 Marseille

Simulation results Vela Junior Source at d=-46.37° with a flat disk distribution of 1° Reconstruction with scanning 3°x3° no morphology no atmospheric muons Years for discovery 5s 50% Vela Junior Vissani 2007 >10 VelaJ Vissani ICRC 2011 2.9 + cutoff 13 TeV 6 VelaJ Kappes >>10 R. Coniglione 29-31 January 2013 Marseille

The Fermi bubbles R. Coniglione 29-31 January 2013 Marseille

homogeneous in a circular region around fixed points Neutrino generation homogeneous in a circular region around fixed points Visibility for a detector at Capo Passero North d = -15° RA = 243° R =19° South d = -44° RA = 298° R. Coniglione 29-31 January 2013 Marseille

The Fermi bubble To be confirmed In the paper simulation for 2 x154 towers with multiPMT 180m spaced (≈6km3) Paper appeared in Astroparticle Physics Vol. 42 (feb 2013) 7-14. tower+multipmt detector @180m Discovery for E-2 with a cutoff@100 TeV spectrum in about 1 ÷1 ½ year Discovery for E-2 with a cutoff@30 TeV spectrum in about 5 ÷6 years strings+multipmt detector @100m (no muatm) Discovery for E-2 with a cutoff@100 TeV spectrum in about 1 ÷1 ½ year Discovery for E-2 with a cutoff@30 TeV spectrum in about 3÷4 years To be confirmed R. Coniglione 29-31 January 2013 Marseille

Good FoM for VelaX and Bubbles (about 3 years) Resume Good FoM for VelaX and Bubbles (about 3 years) FoM strongly dependent on the neutrino spectrum prediction measured high energy gamma spectra. To be done Include the atmospheric muon background Include the morphology Unbinned analysis R. Coniglione 29-31 January 2013 Marseille

Spare R. Coniglione 29-31 January 2013 Marseille

Neutrino spectra Kappes et al. Kelner et al. Morlino et al. Astrop. Phys. 31 (2009) 376 R. Coniglione 29-31 January 2013 Marseille

Neutrino spectra N (GeV-1s-1cm-2) G Ecut (TeV) F>1TeV (s-1cm-2) * RXJ1713 Kelner (Ref.1)* 1.68 10-14 1.72 2.1 6.62 10-12 RXJ1713 Kappes (Ref. 2)* 15.52 10-14 1.35 4.80 10-12 RXJ1713 Vissani (Ref. 3) 8.35 10-15 2.04 13.1 6.12 10-12 Vela X 2006 Kappes (Ref. 2)* 11.75 10-15 0.98 0.84 4.32 10-12 VelaX 2006 Vissani ( Ref. 3) 0.60 10-14 1.45 7.22 5.76 10-12 VelaX 2012 total Vissani (Ref. 3) 0.93 10-14 1.32 8 10.3 10-11 VelaX 2012 inner Vissani ( Ref. 3) 0.72 10-14 1.36 7 7.36 10-11 Ref. 1S.R. Kelner et al. Phys. Rev. D 74 034018 (2006) Ref. 2 Kappes et al., ApJ 656 (2007) 870. Ref. 3 From gamma to neutrino spectra following Vissani prescription F.L.Villante and F.Vissani, Phys. Rev. D 78 (2008) 103007; F. Vissani and F.L. Villante, Nucl. Inst. Meth. A588 (2008) 123; F. Vissani, Astropart. Phys. 26 (2006) 310 * R. Coniglione 29-31 January 2013 Marseille