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

2. 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 Marseille

3. 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 Marseille

4. 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 Marseille

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

6. 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 Marseille

7. Gamma spectra N (GeV-1s-1cm-2) G Ecut (TeV) F>1TeV (s-1cm-2)
RXJ1713
2.04
17.9
VelaX 2006*
1.45
13.8
VelaX 2012 total
1.32
14.0
VelaX 2012 inner
1.36
13.9
* F. Aharonian et al.,
Astronomy & Astrophysics L (2006)
R. Coniglione
29-31 January Marseille

8. 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 Marseille

9. Neutrino spectra
R. Coniglione
29-31 January Marseille

10. Neutrino spectra N (GeV-1s-1cm-2) G Ecut (TeV) F>1TeV (s-1cm-2) *
Vela X 2006 Kappes (Ref. 1)*
0.98
0.84
VelaX 2006 Vissani (Ref. 2)**
1.45
7.22
VelaX 2012 total Vissani (Ref. 2)**
1.32 8
VelaX 2012 inner Vissani ( Ref. 2)**
1.36 7 *
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) ;
F. Vissani and F.L. Villante, Nucl. Inst. Meth. A588 (2008) 123;
F. Vissani, Astropart. Phys. 26 (2006) 310 **
R. Coniglione
29-31 January Marseille

11. 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 Marseille

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

13. 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=
R. Coniglione
29-31 January Marseille

14. 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 *
2.24 -
VelaJ ICRC 2011 single region *
2.11
VelaJ ICRC 2011 whole *
2.22
R. Coniglione
29-31 January Marseille

15. Vela Junior neutrino spectrum* ** N
(GeV-1s-1cm-2) G
Ecut
(TeV)
F>1TeV (s-1cm-2)
VelaJ Vissani 2007**
2.24 -
VelaJ Vissani ICRC 2011 single region**
2.11
VelaJ Kappes*
1.72
1.19
R. Coniglione
29-31 January Marseille

16. 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 Marseille

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

18. 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 Marseille

19. 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
Discovery for E-2 with a TeV spectrum in about 1 ÷1 ½ year
Discovery for E-2 with a TeV spectrum in about 5 ÷6 years
strings+multipmt
(no muatm)
Discovery for E-2 with a TeV spectrum in about 1 ÷1 ½ year
Discovery for E-2 with a TeV spectrum in about 3÷4 years
To be confirmed
R. Coniglione
29-31 January Marseille

20. 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 Marseille

21. Spare
R. Coniglione
29-31 January Marseille

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

23. Neutrino spectra N (GeV-1s-1cm-2) G Ecut (TeV) F>1TeV (s-1cm-2) *
RXJ1713 Kelner (Ref.1)*
1.72
2.1
RXJ1713 Kappes (Ref. 2)*
1.35
RXJ1713 Vissani (Ref. 3)
2.04
13.1
Vela X 2006 Kappes (Ref. 2)*
0.98
0.84
VelaX 2006 Vissani ( Ref. 3)
1.45
7.22
VelaX 2012 total Vissani (Ref. 3)
1.32 8
VelaX 2012 inner Vissani ( Ref. 3)
1.36 7
Ref. 1S.R. Kelner et al. Phys. Rev. D (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) ;
F. Vissani and F.L. Villante, Nucl. Inst. Meth. A588 (2008) 123;
F. Vissani, Astropart. Phys. 26 (2006) 310 *
R. Coniglione
29-31 January Marseille