The real voyage is not to travel to new landscapes, but to see with new eyes... Marcel Proust

Transcription

1 Francis Halzen University of Wisconsin The real voyage is not to travel to new landscapes, but to see with new eyes... Marcel Proust

2 ν GeV γ-rays Visible CMB Radio Flux Energy (ev) / / / / / / / TeV sources! / / cosmic / rays / / / / / / /

3 Multi-Messenger Astronomy protons, γ-rays, neutrinos, gravitational waves as probes of the high-energy Universe protons: directions scrambled by magnetic fields γ-rays : straight-line propagation but reprocessed in the sources, extragalactic backgrounds absorb Eγ > TeV neutrinos: straight-line propagation, unabsorbed, but difficult to detect

4 ν astronomy ν astronomy requires kilometer- scale detectors AMANDA: proof of concept IceCube: : a kilometer-scale ν observatory

5 cosmic neutrinos associated with cosmic rays

6 Galactic and Extragalactic Cosmic Rays Knee New component with hard spectrum? Ankle

7 >>> energy in extra-galactic cosmic rays: ~ 3x10-19 erg/cm 3 or ~ erg/yr per (Mpc) 3 for years 3x10 39 erg/s per galaxy 3x10 44 erg/s per active galaxy 2x10 52 erg per gamma ray burst >>> energy in cosmic rays ~ equal to the energy in light! 1 TeV = 1.6 erg

8 Neutrino Beams: Heaven & Earth NEUTRINO BEAMS: HEAVEN & EARTH Black Hole Radiation Enveloping Black Hole p + γ -> n + π + ~ cosmic ray + neutrino -> p + π 0 ~ cosmic ray + gamma

9 Neutrinos Associated With the Source of the Cosmic Rays? neutrino flux AMANDA II sensitivity(!) ~50 events per kilometer square per year

10 why km 2 telescope area? neutrinos associated with the observed sources of cosmic rays (and gamma rays) models of cosmic ray accelerators: an example guaranteed" cosmic neutrino fluxes cosmic ray interactions with CMBR cosmic ray interactions in galactic plane, in galaxy clusters, in the sun decaying EeV neutrons gamma ray burst RXJ 1713!!!

11 Active Galaxy Radiation Field: Ask Astronomers energy in protons ~ energy in electrons photon target observed in lines >> few events per year km 2

12 GZK Cosmic Rays & Neutrinos cosmogenic neutrinos are guaranteed 0.1 few events per year in IceCube p + γ CMB π + n

13 Gamma Ray Bursts Fireball: Rapidly expanding collimated ball of photons, electrons and positrons becoming optically thin during expansion Shocks: external collisions with interstellar material (e.g. remnant guaranteed TeV neutrinos!!!) or internal collisions when slower material is overtaken by faster in the fireball. Protons and photons coexist in the fireball

14 Models of Cosmic Ray Accelerators: Same Conclusion! neutrino flux AMANDA II sensitivity(!) ~ 50 events per kilometer square per year

15 First-Generation Neutrino Telescopes

16 equires ilometer-scale eutrino etectors

17 Infrequently, a cosmic neutrino is captured in the ice, i.e. the neutrino interacts with an ice nucleus Cerenkov light cone In the crash a muon (or electron, or tau) ) is produced γ muon or tau Detector interaction The muon radiates blue light in its wake Optical sensors capture (and map) the light neutrino

18 10 PMT Hamatsu- 70

19 ANTARES 12 lines 25 storeys / line 3 PMT / storey ANTARES Layout 14.5 m 350 m ~60-75 m 100 m Junction box 40 km to shore Readout cables

20 Northern hemisphere detectors Baikal NT200 Antares Nestor 1100 m deep data taking since 1998 new: 3 distant strings March 17, strings connected 2400 m deep completion: start 2006 March 29, of 12 floors deployed 4000 m deep completion: 2006

21 Infrequently, a cosmic neutrino is captured in the ice, i.e. the neutrino interacts with an ice nucleus Cerenkov light cone In the crash a muon (or electron, or tau) ) is produced muon or tau detector interaction The muon radiates blue light in its wake Optical sensors capture (and map) the light neutrino

22 North AMANDA South Pole road to 1500 m 2000 m [not to scale] work Dome Summer camp Amundsen-Scott South Pole station

23 AMANDA II up-going muon 61 modules hit t i m e > 7 neutrinos/day on-line Size ~Number of Photons

24 AMANDA Event Signature: Muon CC muon neutrino interaction track ν µ + N µ + X

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26 Skyplot Amanda-II, events below horizon above horizon: mostly fake events

27 Detection of φ ν (E ν ) dn/de = A ν φ ν = {P earth P µ A µ }φ ν with P µ = n R µ σ ν 10 6 Ε Τev A ν = P earth P µ A µ

28 Infrequently, a cosmic neutrino is captured in the ice, i.e. the neutrino interacts with an ice nucleus Cerenkov light cone In the crash a muon (or electron, or tau) ) is produced muon or tau detector interaction The muon radiates blue light in its wake Optical sensors capture (and map) the light neutrino

29 at TeV energy Neutrino area: 10~100 cm 2 Muon area: ~ 10,000 m 2 (geometric area km 2 ) a The AMANDA Detector

30 AMANDA effective area

31 1968 OSO-3 (Kraushaar et al. 1972) effective area 4 cm photons sources seen in next mission! SAS cm 2

32 Skyplot Amanda-II, events below horizon above horizon: mostly fake events

33 AMANDA skyplot optimized for best sensitivity to E -3 E -2 sources α Preliminary 3369 events

34 AMANDA: proof of concept

35 Atmospheric Neutrinos Cosmic Ray e + µ + π + ν e ν µ ν µ 15 Km

36 Atmospheric ν s as Test Beam 100 TeV 100 GeV Neutrino Energy in GeV

37 Optimized 2002 analysis zenith distribution data atmo > < > normalization not final yet, assumed lifetime is 208 days

38 Diffuse muon neutrino fluxes Model predictions and AMANDA (E -2 ) limits _ ν µ + ν µ Excluded predictions diffuse (B10) cascades/3 unfolded UHE/3 Integral limits (cover 90% of final energy spectrum): diffuse (B10) cascades UHE Quasidifferential limit: unfolded

39 Astronomy

40 Fireball Phenomenology & The Gamma-Ray Burst (GRB) Neutrino Connection Electron --- Progenitor (Massive star) Magnetic Field γ- ray 6 Hours 3 Days e - p + γ-ray Optical X-ray (2-10 kev) Radio p E ergs ( n) + π ν µ + µ ν µ + e + ν e ν µ + γ + Shock variability is reflected in the complexity of the GRB time profile. over 500 GRB searched! R < 10 8 cm R cm, T 3 x 10 3 seconds R cm, T 3 x seconds

41 Skyplot Amanda-II, events below horizon above horizon: mostly fake events

42 AMANDA 2000

43 Sensitivities Single years & Combination.03 Sensitivity / 10-6 GeV E -2 cm -2 s Sin(δ)

44 : scrambled (top) and unblinded (bottom)

45 Significance map for

46 Preliminary Cas A Mk421 Mk501 Cyg Crab M87 SS433

47 90% C.L. upper limits (in units of 10-8 cm -2 s -1 ) for selected sources for an E -2 spectral shape integrated above E ν =10 GeV Φ limit limit limit Source Declination ν Φ ν N obs / N bgr Φ ν N obs / N bgr SS o / / 1.69 M o / / 1.10 Crab 22.0 o / / 1.10 Mkn o / / 0.65 Mkn o / / 0.69 Cyg. X o / / 0.67 Cas. A 58.8 o / / 1.03 PRELIMINARY

48 Selected Source Analysis Stacking Source Analysis Galactic Plane Transient Sources Burst Search Correlation Analysis Multi-Pole Analysis Lower energy threshold (optimize to steeper spectra)

49 µ cm -2 s southern sky 4 years Super-Kamiokande northern sky 170 days AMANDA-B years MACRO Expected sensitivity for AMANDA SS-433 Mk-501 ν/γ ~ 1 Measured sensitivity days AMANDA-II declination (degrees)

50 Neutrino Beams: Heaven & Earth γ ν

51 Intrinsic source γ spectrum (corrected for IR absorption) Measured γ spectrum AMANDA average flux limit for two assumed spectral indices α, compared to the average gamma flux of Markarian 501 as observed in 1997 by HEGRA. AMANDA-II has reached the sensitivity needed to search from neutrino fluxes from TeV gamma sources of similar strength to the instrinsic gamma flux. This Plot 2000 data only!

52 (Hess/ Cangaroo) γ-rays from π 0 decay discovered E ν N ν (E ν ) = ε E γ N γ (E γ ) transparent source π 0 = π + = π - 1 < ε < 8 accelerator beam dump (hidden source) ν flux predicted observed γ-ray flux RX J per year (galactic center) ~40 per km2 RX J1713

53 Supernova Beam Dump RX J

54 leaving the 3 σ club IceCube AMANDA-II** ANTARES # OF PMTS 4800/10 INCH 600/8 INCH 900/10 INCH point source sensitivity (muons per year) cm -2 s cm -2 s -1 weakly dependent on declination x cm -2 s -1 depending on declination diffuse limit* (ν µ per year) 10-9 GeV cm -2 s -1 sr GeV cm x 10-7 GeV cm -2 s -1 sr -1 s -1 sr -1 * depends on assumption for background from atmospheric neutrinos from charm ** includes systematic errors

55 Water or Ice?

56 Kilometer-Scale Neutrino Telescopes

57 0 m 50 m Ice Top Snow Layer 300 m 1400 m IceCube 2400 m

58 Size Perspective AMANDAII 300 m 1500 m 50 m 2500 m

59 0 m 50 m 1400 m 2400 m 300 m Runway South Pole IceCube 80 Strings 4800 PMT Instrumented volume: 1 km3 (1 Gigaton) IceCube is designed to detect neutrinos of all flavors at energies from 10 7 ev (SN) to ev

60 µ-event in IceCube 300 atmospheric neutrinos per day AMANDA II IceCube: Larger Telescope Superior Detector 1 km

61 2 x ev event in AMANDA and IceCube

62 enhanced role of tau neutrinos: cosmic beam: ν e = ν µ = ν τ because of oscillations ν τ not absorbed by the Earth (regeneration) pile-up near 1 PeV where ideal sensitivity

63 PeV τ (300m) ν τ τ τ decays

64 IceCube Start 2002 First strings 2004 Completed 2010

65 µ cm -2 s -1 Super-K, MACRO SS-433 Achieved and expected sensitivities to steady point sources AMANDA Antares Nestor? GX Mk-501 ν/γ ~ KM3 in Mediterr. IceCube km year aperture by 2007 for A II+IceCube

66 conclusions AMANDA collected > 5,000 ν s ~ 10 (7) more every day on-line neutrino sensitivity has reached ν = γ > 300,000 per year from IceCube from 1 Crab to < 0.01 Crab sensitivity

67 Bartol Bartol Research Research Institute, Institute, Delaware, Delaware, USA USA Univ. Univ. of of Alabama, Alabama, USA USA Pennsylvania Pennsylvania State State University, University, USA USA UC UC Berkeley, Berkeley, USA USA Clark-Atlanta Clark-Atlanta University, University, USA USA Univ. Univ. of of Maryland, Maryland, USA USA IAS, IAS, Princeton, Princeton, USA USA University University of of Wisconsin-Madison, Wisconsin-Madison, USA USA University University of of Wisconsin-River Wisconsin-River Falls, Falls, USA USA LBNL, LBNL, Berkeley, Berkeley, USA USA University University of of Kansas, Kansas, USA USA Southern Southern Univ. Univ. and and A&M A&M College, College, Baton Baton Rouge Rouge USA USA (12) (12) Venezuela Venezuela Universidad Simon Bolivar, Caracas, Venezuela Europe Europe (11) (11) Japan Japan Chiba Chiba University, University, Japan Japan University University of of Canterbury, Canterbury, Christchurch, Christchurch, NZ NZ Universite UniversiteLibre Librede de Bruxelles, Bruxelles, Belgium Belgium Vrije Vrije Universiteit Universiteit Brussel, Brussel, Belgium Belgium Université Universitéde de Mons-Hainaut, Mons-Hainaut, Belgium Belgium Universität UniversitätMainz, Germany Germany DESY-Zeuthen, DESY-Zeuthen, Germany Germany Universität UniversitätWuppertal, Germany Germany Uppsala Uppsala University, University, Sweden Sweden Stockholm Stockholm university, university, Sweden Sweden Imperial Imperial College, College, London, London, UK UK University University of of Oxford, Oxford, UK UK NIKHEF, NIKHEF, Utrecht, Utrecht, Netherlands Netherlands New New Zealand Zealand

68 IceCube effective area for muons Galactic center - after quality cuts and atm µ reduction by ~ averaged over E 2 spectrum Northern sky - at trigger level - after quality cuts and atm m red. - after additional energy cuts optimized for point source search For E > 1 TeV, A eff >A geom non-contained events

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