Spyros Tzamarias School of Science and Technology Hellenic Open University Neutrino Telescopy a1er the new developments in Par8cle and Astropar8cle Physics
Sky view of a Mediterranean UnderSea Neutrino Telescope FOV for up going neutrinos shown From Mediterranean 24h per day visibility up to declination ~ 50 >25% >75% KM3NeT coverage of most of the sky (87%) including the Galactic Centre 2
KM3NeT consoraum consists of 40 European insatutes, including those in Antares, Nemo and Nestor, from 10 countries (Cyprus, France, Germany, Greece, Ireland, Italy, The Netherlands, Rumania, Spain, U.K) KM3NeT is included in the ESFRI and ASPERA roadmaps KM3NeT Design Study (2006 2009) defined telescope design and outlined main technological opaons Approved and funded under the 6 EU Frame Program Conceptual Design Report published in 2008 h\p://www.km3net.org/public.php Technical Design Report (TDR) completed => outline technology opaons for the construcaon, deployment and maintenance of a deep sea neutrino telescope h\p://www.km3net.org/km3net TDR.pdf KM3NeT Preparatory Phase (2008 2012) defines final design, producaon planes for the detector elements and infrastructure features. Prototype validaaonis under way. Legal, governance and funding aspects are also under study. ScienAfic Standing Commi\ee: External ScienAfic EvaluaAon Approved and funded by EU under the 7 EU Frame Program
General KM3NeT lay out DetecAon Units Primary JuncAon box Secondary JuncAon boxes Electro opacal cable OpticalModule (OM) = pressure resistant/tight sphere cointaining photo multpliers Detection Unit (DU) = mechanical structure holding OMs, enviromenta lsensors, electronics, DU is the building block of the telescope 4
Design Study TDR DetecAon Unit and OpAcal Module Concepts Two different opaons for OMs and Dus reported in TDR Flexible tower with horizontal bars equipped with large PMT OMs Slender string Vertical sequence of multi PMT OMs Preparatory Phase =>Convergence i.e. DU=Flexible tower, OM=MulA PMT Prototype and validaaon acaviaes crucial for final choice 5 GOLDEN ROOL: Maximize the Discovery Poten8al 5
DOMBAR Prototype Storey Bar Frame Rope Storage Rope & Cable Storage Mechanical Cable ConnecAon OpAcal Module Mechanical Interface 2 DOM + 1 BAR = 1 DOMBAR 20 DOMBARS = DOMTOWER The Ver8cal String Structure IS NOT ROOLED OUT 6
Fermi LAT ObservaAon Fermi Bubbles From Meng Su, Tracy R. Slatyer, Douglas P. Finkbeiner Astrophys.J. 724:1044 1082,2010 Large extension (50 lat. 40 long.) no spaaal variaaon in the spectrum
From M. Crocker and F. Haronian Phys. Rev. Le\. 106 (2011) 101102 We show below that a cosmic ray populaaon can explain these structures Finally, we predict that there should be a region of extended, TeV radiaaon surrounding the GalacAc nucleus on similar size scales to the GeV bubbles with an intensity up to E 2 F (TeV) ~10 9 TeV cm 1 s 1 sr 1 which should make an interesang target for future ray studies. Likewise, the region is a promising source for future, Northern Hemiphere, km3 volume neutrino telescope: we esamate (assuming a =2.0 proton spectrum cut off 1 PeV). The expected neutrino flux for one bubble is E 2 F (TeV) ~ 10 6 GeV cm 1 s 1 sr 1 * 0.34 sr / 2.5 ~ 1.3 10 7 GeV cm 1 s 1 Gamma flux From spectrum to spectrum Single bubble solid angle
Neutrino genera8on Rosa Coniglione homogeneous in a circular region around fixed points North = 15 RA = 243 R =19 South = 44 RA = 298 R =19 one block of 154 DU
In Meng Su et al. bubbles are due to relaavisac CR electrons that produce gamma through IC process
GalacAc Candidate Sources SNRs Origin of CosmicRays SNR paradigm, VHE but no conclusive evidence about CR accelera8on RXJ1713 39.43 and Vela JR best candidates RXJ1713 39.43 IF hadronic mechanisms => spectrum can be calculated from VHE spectrum ( solid redline Vissani) Hess RXJ1713 39.43 Observation at 5 within about 5ys with KM3NeT
Gamma Ray Bursts
The spaaal distribuaon of the photosensiave area is a criacal parameter that affects the discovery potenaal of the telescope NIM A 626 627 (2011) S188 S190
Environmental Parameters & Early Discovery Driven Scenario doi:10.1016/j.nima.2010.09.040
Detector Geometrical Layout 154 Towers or 77 Towers Each Tower consists of 20 bars, 6m in length and 40m apart One MulAPMT OM at each end of the bar. 29% QE Detectors Footprint
Use WISELY the whole Experimental Informa8on ReconstrucAon ResoluAon on a track by track basis Energy EsAmaAon (θ, φ) z ψ (θ m, φ m ) x y
Eν<10 TeV 100TeV<Eν<1 PeV 10TeV<Eν<100 TeV 1PeV<Eν
A Neutrino Telescope CAN Measure Energy NIM A 626 627 (2011) S185 S187
0.5<cos(θ)<0.55 Reconstructed Energy (log of GeV)
N=0 N=4 N=6 N=8
Discovery Poten8al (50% Discovery Probability) preliminary 3σ This Method: 1.2x 10 9 E 2 flux for 50% discovery This Method without Energy: 1.6x10 9 Binned method: >2.4x10 9 4σ This Method: 1.6x 10 9 This Method without Energy: 2.6x10 9
Atmospheric γ=2 γ=1.8 (re weighted)) Log(E/GeV)
Signal Events Signal Events 24 Signal Events on Top of Background 15 Signal Events on Top of Background Spectral Index Spectral Index
Spectral Index esamaaon accuracy Signal events on top of Background
Final Remarks We gain a factor of 2 in discovery potenaal by using more of the informaaon offered by the data! We can make it be\er The Design of KM3 is not finished yet OpAmize the layout for fast discovery GalacAc Extended Sources GRBs, AGN, GKZ Dark Ma\er? UHE Atmospheric Showers?