Neutrino Astronomy with Antares and KM3NeT

Transcription

1 Neutrino Astronomy with Antares and KM3NeT (and (and IceCube) IceCube) aart aart heijboer heijboer -- nikhef nikhef 1

2 -astronomy protons are deflected by magnetic fields in the universe ph ot on high energy neutrinos: travel in straight lines point to their source are tell-tale signs of proton acceleration are not absorbed on their way here 2

3 -astronomy Supernova Remnants Micro quasars protons are deflected by magnetic fields in the universe Active Galactic Nuclei Gamma Ray bursts Dark Matter ph ot on Fermi Bubbles Diffuse Fluxes Atmospheric neutrinos & oscillations Cosmic ray physics Monopoles & Nuclearites Neutrino physics (mass hierarchy)? 3

4 on u m ino r t neu Uppsala 2000 Ivo van Vulpen 4 4

5 neutrino telescopes Antares 2007-now Lake Baikal, NT200+ KM3NeT Uppsala 2000 Amanda Ivo van Vulpen IceCube 2007-now 5 5

6 View of the sky subtlety: -telescopes can look upward somewhat, at high energies. RX J1713 Vela X All results are for 'phase-2': overlap: change of independent confirmation 6

7 Antares results data Uppsala 2000 Ivo van Vulpen 7 7

8 Antares results limits computed for 51 astrophysical objects most significant spot in the sky: 2.3s (p=2.1%) data Uppsala 2000 Ivo van Vulpen 8 8

9 Antares results limits on E-2 flux - limits improved 40% compared to publication APj 760 (2012) 53 - Careful when comparing to IceCube. Uppsala 2000 Ivo van Vulpen 9 9

10 Antares results - limits improved 40% compared to publication APj 760 (2012) 53 - Careful when comparing - Cut-off expected for to IceCube. Galactic Sources - Antares rules the Southern Hemisphere below 10 TeV Uppsala 2000 Ivo van Vulpen 10 10

11 Antares results 3C279 p=10% Fermi-bubbles (1.2 excess) coincidence with flairing sources PRELIMINARY neutrinos coincident with GRB (none found) Uppsala 2000 dark matter annihilation in the Sun (very competitive limits) Ivo van Vulpen 11 11

12 12 Multi-messenger program Many multi-messenger programs being pursued, both online and offline. 12

13 KM3NeT Building Block KM3NeT - next generation neutrino telescope (and infrastructure for earth and sea science) - ambition for full project ('phase-2'): - 6 blocks of 115 strings - distributed over multiple sites (fr,it,gr) (good for funding, not bad for science) - costs 220 Meuro - 'phase-1': - Have some funding now in NL, Fr, It - Fr + It need to spend it before ~ Building fraction of the detector (31 strings) + seabed infrastructure in Fr+It working very hard to build and deploy phase-1 in next two years 13

14 KM3NeT Building Block KM3NeT 'recent' news - Jan 2013 : collaboration formed - 40 institutes, 180 members, MOU drafted - NL spokesperson - MOU drafted 14

15 String Deployment String Launching Fast mounting of optical modules Multiple deployments / cruise Autonomous unfurling from seabed Recovery of launcher vehicle 15

16 Mechanical 2-12String April 2013: 5 deployments Deployment at a depth of 1000mTests (NIOZ boat) 20 miles off the coast of Motril, Spain Spain in-house designed cable (huge cost saving) Successful demonstration of deployment concept DOMs are horizontal Some issues with penetrators (understood and fixed) 16

17 The Multi-PMT Digital Optical Module 17 inch > Digital photon counting Directional information Wide angle of view Robust against bioluminescence Cost reduction cf ANTARES Most cm2 PMT for the $ ANTARES Storey 17

18 The Multi-PMT Digital Optical Module 31 x 3 PMTs Hamamatsu, ETL, HZC Light collection ring 20 40% gain in PC for free Low power (<10 W / DOM) FPGA readout sub-ns time stamping time over threshold all data to shore White Rabbit time synchronisation Calibration LED & acoustic piezo in sphere Optical fibre data transmission DWDM with 80 wavelengths Gb/s readout 18

19 Prototype Optical Module Final integration tests in dedicated dark box Connected to Antares Instrumentation Line 19

20 Prototype Optical Module - results Atm. muons data (M 6) preliminary Rate [a.u.] Atm. muons K40 bioluminescence data Rate [Hz] preliminary Number of coincident hits in DOM >6 coincidences within 20ns reduces K40 contribution dominated by atmospheric muons Participation to events with Ncoinc>6 Upper PMTs more events directional information from single floor enormously rich data from single OM. Publication in preparation 20

21 science focus : galactic SNR HESS TeV gamma rays - SNR standard candidate for bulk of Cosmic Rays (but hard to prove). - High Energy Gamma Rays: - energies up to 100 TeV - power law spectra (expected from particle acceleration). - Is this proof of CR acceleration? hadronic scenario distinguish - try by means of gamma-ray spectrum - model-dependency makes it hard - IC 433 & W44 claimed hadronic [ Science 339 ( )] - by detecting neutrinos experimentally hard, but if then CRs (no need for models) leptonic scenario: produced by bremstrahlung or inverse-compton of electrons 21

22 KM3NeT reach for RXJ1713 KM3NeT discovery potential flux model derived directly from TeV -ray observations Kappes et al., ApJ 656 (2007) 870 Vissani, Phys. Rev. D 78 (2008) current best limit (Antares) factor 9 above model. Years Nsource Nbg 5 sigma sigma or : limit hadron fraction to <30% at 90% CL after 5.8 years. Antares , ApJ, 760, 53 Full fase-2 detector (620 strings) full simulation & reconstruction: resolution = 0.2 deg Background is atmospheric antares RXJ limit antares E-2 limit - - ν flux model only (working to include e ) KM3NeT (phase-2) will: determine without any whether RXJ is dominated by hadrons or electrons if hadrons: discover the (first) source and prove SNR accelerate CRs 22

23 23

24 IceCube Signal (starting track analysis) 4 evidence of cosmic neutrinos! - publication (excepted by Science) and results from muon analysis expected soon 24

25 Diffuse Neutrino Flux IceCube signal: (dominated by cascades) muon nu flux of ~1.2 *10-8 GeV/cm2/s/sr (E-2, cutoff at 2 PeV) KM3NeT: muon neutrino 5σ discovery ANTARES: current sensitivity: GeV/cm2/s/sr (no cutoff, muon, 3 yrs) ANTARES cascade resolution: 100TeV) KM3NeT (phase-2): 5σ confirmation of IceCube signal in 2.5 years (µ only with simple analysis) nb in -channel KM3NeT 0.1o resolution full phase-2 detector (700 strings) Will improve if KM3NeT optimized for HE signal Phase-1(+X) might be enough to confirm and study the signal.. with excellent angular resolution. possibility under study exciting (since phase 1 will happen... soon) 25

26 Conclusions Antares working well since 2007 and producing high quality science competing with IceCube in Southern Hemisphere and other niches large multi-messenger program KM3NeT Collaboration formed, management in place, many issues (site) settled NL has huge role in design and construction. Testing and prototyping well underway prototype optical module in Antares provides rich data 'Phase-1' is funded and will be built in the next year(s) There is growing evidence from IceCube for a High energy flux of cosmic neutrinos Can we study the signal with Phase-1?? (or a little more) 26

27 Sites Events (yr-1) with 600 strings Strong case for distributed research infrastructure. Agreement that France, Italy and Greece host part of the observatory strings per building block Advantages: Access to regional funding (ERDF) Retain manpower Neutrino astronomy does not suffer If size exceeds a certain minimum Additional overhead small e.g: need multiple cables anyway Associated sciences benefit 27

28 Earth and sea sciences rare infrastructure for continuous and long-term measurements example from Antares [Deep-Sea Research 58 (2011) ] count rate in OMs France A ADCP 'particle content' ADCP vertical current increased counting rate correlates with downward current & suspended particles (i.e. food) Sudden eddy currents transport surface water to the deep short-lived events drive deep sea live permanent observator y 28

29 PhotoMultiplier Development Specifications QE: / TTS: 4.5(5.0)ns FWHM Gain for 900V<HV<1300 V Prepulses <1% Delayed pulses <3.5% Afterpulses late<10%; early<2% Dark rate <1500 Hz Cost/PC area cheaper than 10 inch ETL ETL D792KFL Aart Heijboer9cm APP symposium, diameterleiden, Okt 2013 Hamamatsu R cm diameter tender has been placed for 15,000 3 PMTs 29

30 Strings Mooring line: Buoy 2 Dyneema ropes (4 mm diameter, prestretched) 18 storeys (one DOM each), 36m spacing, 100m anchor-first storey Electro-optical backbone: Oil filled flexible hose ~6mm diameter 18 fibres and 2 copper wires At each storey: 1 fibre+2 wires Break out box with fuses at each storey 30

31 Origin of CRs is key topic - HESS LOI, page 2 of science case (similar on CTA website) Identifying and studying hadron (CR) acceleration is a main topic of all TeV astronomy. everyone agrees that if 's can be detected, it's the best way to answer the question....it's not just us from wc eend that think wc eend is interesting... 31

32 Hadronic SNR Science 339 ( ) TeV gamma data cannot distinguish between models - Fermi-LAT (GeV) in this case - still: very dependent on models This detection provides direct evidence that cosmic-ray protons are accelerated in SNRs. Fermi-LAT IC 433 & W44 : Both have Molecular Clouds which can serve as 'beam dumps' 32

33 SNR RX J 'poster child' for KM3NeT intense shell-type SNR (first one in TeV) TeV emission up to 100 TeV Origin of 's debated extensively (next slide) Molecular cloud (beam target) Viable that the observed TeV gamma's are hadronic: newest Fermi-LAT data can be accommodated in 3D MHD simulations [Inoue et al. ApJ (2012)] TeV gamma's correlate with the molecular cloud suggestive of hadronic scenario (nnext slide) [Y. Fukui, arxiv: ] 33

34 SNR RX J TeV gamma ray emission corresponds to target density as expected in hadronic scenario of production [Y. Fukui, arxiv: ] 34

35 SNR RX J A statistical study of Galactic SNR source spectra detected at >GeV energies Mandelartz, M. and Becker Tjus, J., ArXiv e-prints p (2013) - Acceleration of cosmic rays and gamma-ray emission from supernova remnants in the Galaxy Cristofari, P. et al., ArXiv e-prints p (2013) - Molecular and atomic gas in the young TeV gamma-ray SNRs RX J and RX J : evidence for the hadronic production of gamma rays Fukui, Y., ArXiv e-prints p (2013) -3 to 12 millimetre studies of dense gas towards the western rim of supernova remnant RX J Maxted, N.I. et al., ArXiv e-prints p (2012) - Cosmic Ray Electron Evolution in the Supernova Remnant RX J Finke, J.D. and Dermer, C.D., ArXiv e-prints p (2012) - Gamma Rays from Cosmic Rays in Supernova Remnants Dermer, C.D. and Powale, G., ArXiv e-prints p (2012) - Unified model for the gamma-ray emission of supernova remnants Yuan, Q. et al., ArXiv e-prints p (2012) - Observations of the young supernova remnant RX J with the Fermi Large Area Telescope Abdo, A.A. and Fermi LAT Collaboration, ArXiv e-prints p (2011) - Core-collapse model of broadband emission from SNR RX J with therm al X-rays and Gamma-rays from escaping cosmic rays Ellison, D.C. et al., ArXiv e-prints p (2011) - Derivation of the Electron Distribution in SNR RX J via a Spectral Inversion Method Li, H. et al., ArXiv e-prints p (2011) - Galactic Sources of High-Energy Neutrinos: Highlights Vissani, F. and Aharonian, F., ArXiv e-prints p (2011) - Stochastic Electron Acceleration in SNR RX J Fan, Z. and Liu, S., ArXiv e-prints p (2011) - Star-forming Dense Cloud Cores in the TeV Gamma-ray SNR RX J Sano, H. et al., ApJ 724 p59-68 (2010) - Efficient Cosmic Ray Acceleration, Hydrodynamics, and Self-Consistent Thermal X-Ray Emission Applied to Supernova Remnant RX J Ellison, D.C. et al., ApJ 712 p (2010) - Nonthermal and thermal emission from the supernova remnant RX J Berezhko, E.G. and Volk, H.J., A&A 511 pa34+ (2010) - Stochastic electron acceleration in the TeV supernova remnant RX J : the high-energy cut-off Fan, Z. et al., MNRAS 406 p (2010) - Nonthermal Radiation of Young Supernova Remnants: The Case of RX J Zirakashvili, V.N. and Aharonian, F.A., ApJ 708 p (2010) - Lepton models for TeV emission from SNR RX J Fan, Z.H. et al., A&A 517 pl4+ (2010) - Modeling the Multi-Wavelength Emission of Shell-Type Supernova Remnant RX J Yuan, Q. et al., ArXiv e-prints p (2010) source : TevCat -Modeling the Gamma-Ray Emission Produced by Runaway Cosmic Rays in the Environment of RX J Casanova, S. et al., PASJ 62 p (2010) -A joint spectro-imaging analysis of the XMM-Newton and HESS observations of the supernova remnant RX J Acero, F. et al., A&A 505 p (2009) -Gamma-ray emission from SNR RX J and the origin of galactic cosmic rays Morlino, G. et al., MNRAS 392 p (2009) -Gamma rays and neutrinos from SNR RX J Morlino, G. et al., Astroparticle Physics 31 p (2009) -Reanalysis of Data Taken by the Cangaroo 3.8 Meter Imaging Atmospheric Cherenkov Telescope: PSR B , SN 1006, and Vela Yoshikoshi, T. et al., ApJ 702 p (2009) -The multi-band non-thermal emission from the supernova remnant RX J Fang, J. et al., MNRAS 392 p (2009) -Arguments against a dominantly hadronic origin of the VHE radiation from the supernova remnant RX J Plaga, R., New Astronomy 13 p73-76 (2008) -On the Very-High-Energy Gamma Ray Spectra from Typical Supernovae Remnants Shurtleff, R., ArXiv e-prints 807 p (2008) -Study of Nonthermal Emission from SNR RX J with Suzaku Tanaka, T. et al., ApJ 685 p (2008) -Hadronic versus leptonic origin of the gamma-ray emission from supernova remnant RX J Berezhko, E.G. and Volk, H.J., A&A 492 p (2008) -Sub-mm/mm studies of the molecular gas in the Galactic disk: the TeV gamma ray SNR RXJ and the W28 high mass star forming region Fukui, Y., 1085 p (2008) -Magnetic Field Amplification and Rapid Time Variations in SNR RX J Ellison, D.C. and Vladimirov, A., ApJ 673 pl47-l50 (2008) -Primary particle acceleration above 100 TeV in the shell-type supernova remnant RX J with deep HESS observations Aharonian, F. et al., A&A 464 p (2007) -Extremely fast acceleration of cosmic rays in a supernova remnant Uchiyama, Y. et al., Nature 449 p (2007) -A detailed spectral and morphological study of the gamma-ray supernova remnant RX J with HESS Aharonian, F. et al., A&A 449 p (2006) -High-energy particle acceleration in the shell of a supernova remnant Aharonian, F.A. et al., Nature 432 p75-77 (2004) -Evidence for TeV gamma-ray emission from the shell type SNR RX J Muraishi, H. et al., A&A 354 pl57-l61 (2000) 35

36 Vela-x and Vela jr x-ray image (rosat) Vela X : pulsar wind nebula usually assumed leptonic, but see e.g. L.Zhang and X.C.Yang in ApJ 699 L153-L156, 2009 up to 50 TeV Vela Jr. (a.k.a. SNR RX J ) young SNR pure power-law measured up to 20 TeV molecular cloud vele jr spectrum 36

37 neutrino mass hierarchy measurement?? 37

38 ORCA Following the measurement of , it has been suggested to determine the neutrino mass hierarchy using atmospheric neutrinos, measured in multi-megaton detectors: JHEP 02 (2013) 082 very optimistic paper Matter effect differs depending on Hierarchy at <10 GeV energies KM3NeT community is conducting a feasibility study (under the acronym ORCA) should report by end of the year. Similar interest in IceCube (PINGU) Initial Idea: investigate if it's worth it to devote part of KM3NeT infrastructure to low energies Tev Gev : factor 1000 requires much denser detector shifting towards: investigate if km3net-like technology is useful for building low-energy -detector for atmospheric neutrinos beams: arxiv: , arxiv: oscillation probability neutrino energy (GeV) 38

39 ORCA sensitivity event rate NH IH NH NH = after applying the (assumed) resolutions and acceptance, max ~10% difference remains between in IH and NH 39

40 ORCA sensitivity event rate NH IH NH NH = after applying the (assumed) resolutions and acceptance, max ~10% difference remains between in IH and NH after resolutions, effect is small hard measurement! 40

41 Mass hierarchy significance 5 years with 1.75 Mton Seems not easy to reach 5 volume = money, but also systematics will be important Performance assumed in this plot is better than current results of full simulation & reconstruction that can (and will have to) change. Some issues not considered yet atm background confusion ( tagging) e/ systematics So to be very clear: 1) We will not do it unless 5 can be reached in reasonalbe time 2) This plot, which does not reach 5 fast, is IMHO optimistic (but feasibility study may still surprise us) 41

42 Results of parameter fit generated m2large σ( m2large) (ev2) fitted value fitted value fitted value 1 Mton*year ( NHtrue, NHfit ) generated generated σ(θ23) (deg) σ(θ13) (deg) Fit working well. Good sensitivity to m2large & 23! 42

43 Angular resolution Effective neutrino area 43

44 Shock acceleration u > Vs in the rest frame of the shock, the situation is analogous to this. at every bounce, kinetic energy is transferred from the racket to the ball 44

45 Fermi-LAT on RXJ ApJ, 734, 28, Data more compatible with the leptonic models tested than the hadronic ones. - See however Inoue et al,

46 both are 1 PeV within the errors 2.8 sigma (expect atm. nu, observe 2) 46