Neutrino Telescopy a1er the new developments in Par8cle and Astropar8cle Physics

Transcription

1 Spyros Tzamarias School of Science and Technology Hellenic Open University Neutrino Telescopy a1er the new developments in Par8cle and Astropar8cle Physics

2 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

3 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 ( ) 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:// Technical Design Report (TDR) completed => outline technology opaons for the construcaon, deployment and maintenance of a deep sea neutrino telescope h\p:// TDR.pdf KM3NeT Preparatory Phase ( ) 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

4 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

5 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

6 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

7 Fermi LAT ObservaAon Fermi Bubbles From Meng Su, Tracy R. Slatyer, Douglas P. Finkbeiner Astrophys.J. 724: ,2010 Large extension (50 lat. 40 long.) no spaaal variaaon in the spectrum

8 From M. Crocker and F. Haronian Phys. Rev. Le\. 106 (2011) 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 ~ GeV cm 1 s 1 Gamma flux From spectrum to spectrum Single bubble solid angle

9 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

10 In Meng Su et al. bubbles are due to relaavisac CR electrons that produce gamma through IC process

11 GalacAc Candidate Sources SNRs Origin of CosmicRays SNR paradigm, VHE but no conclusive evidence about CR accelera8on RXJ and Vela JR best candidates RXJ IF hadronic mechanisms => spectrum can be calculated from VHE spectrum ( solid redline Vissani) Hess RXJ Observation at 5 within about 5ys with KM3NeT

12

13

14

15 Gamma Ray Bursts

16

17 The spaaal distribuaon of the photosensiave area is a criacal parameter that affects the discovery potenaal of the telescope NIM A (2011) S188 S190

18 Environmental Parameters & Early Discovery Driven Scenario doi: /j.nima

19 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

20 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

21 Eν<10 TeV 100TeV<Eν<1 PeV 10TeV<Eν<100 TeV 1PeV<Eν

22 A Neutrino Telescope CAN Measure Energy NIM A (2011) S185 S187

23 0.5<cos(θ)<0.55 Reconstructed Energy (log of GeV)

24 N=0 N=4 N=6 N=8

25 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

26 Atmospheric γ=2 γ=1.8 (re weighted)) Log(E/GeV)

27 Signal Events Signal Events 24 Signal Events on Top of Background 15 Signal Events on Top of Background Spectral Index Spectral Index

28 Spectral Index esamaaon accuracy Signal events on top of Background

29 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?