HE2: Muons and Neutrinos

Transcription

1 HE2: Muons and Neutrinos 2.1 Muon observations Solar & atmospheric neutrinos Astrophysical neutrinos Calculations New experiments, instrumentation 18 Merida, July 11, 2007 Tom Gaisser 1

2 Searching for possible hidden chambers in the Pyramid of the Sun Muon tomography ICRC-2007, Mérida 2

3 Searching for possible hidden chambers in the Pyramid of the Sun Muon tomography ICRC-2007, Mérida 2

4 Muons, the gold standard of cosmic-ray physics Muon tomography works because the spectrum of muons is very well-measured up to several hundred GeV Genetic relation to neutrinos constrains neutrino flux: π + µ + + ν µ ; µ + e + + ν e + ν µ, K + µ + + ν µ ; etc. Major uncertainties in µ and ν fluxes: E > TeV: K component E > 100 TeV: charm component Overall normalization Merida, July 11, 2007 Tom Gaisser 3 J. Kempa

5 MINOS far detector µ + /µ - with MINOS 10 < E µ < 250 GeV at 2 < X cosθ < 4 km w. e. Equivalent to 1 < E µ < 7 TeV at surface First high-statistics measurement of muon charge ratio in TeV energy range Realize goal of Zatsepin & Kuz min (1960)* in the energy range of x10 12 ev the µ-meson angular distributions depend significantly on their production mechanism (*JETP 39, , 1960) Merida, July 11, 2007 Tom Gaisser 4

6 Charge Ratio Model Results x x MINOS measure µ+ / µ - and fit to formulas best fit values: f π+ = A π+ /A π - = 0.55; f K+ = A K+ /A K - = 0.67 Merida, July 11, 2007 Tom Gaisser 5

7 π / K ratio Critical energy for interaction vs decay: ε π = m π c 2 / cτ π ~ 115 GeV ε K = m K c 2 / cτ K ~ 850 GeV Effect bigger for K by kinematics: 1 - m µ /m K ~1 1 - m µ /m π << 1 Steep spectrum K contribution increases when E > ε π vertical 60 degrees Merida, July 11, 2007 Tom Gaisser 6

8 Implications for > TeV atmospheric ν f K+ = 0.67 A N K + / A N K - = 2 Substantial contribution of associated production ( p Λ K + ) Effect is amplified for ν s: ν µ / ν µ 2 Important for atmospheric neutrino background in neutrino telescopes MINOS measurement will lead to improved calculation of >TeV φ ν Merida, July 11, 2007 Tom Gaisser 7

9 Super-Kamiokande and status of neutrino oscillations SK-III operating since July 12, 2006 Hardware and software upgrades Full complement of >11 thousand 20 PMTs plus outer (veto) detector Recalibration finished and first year data in good agreement with SK-I + SK-II Potential for lower threshold for solar neutrino analysis Merida, July 11, 2007 Tom Gaisser 8

10 SK- I SK- II 1. Introduction: History of Super-Kamiokande Started data taking (SK- I) Evidence of Atm. ν ocsillation(98 ) K2K started Evidence of Solar ν oscillation(01 ) 39m Stopped data taking for detector upgrade Accident partial reconstruction of the detector Resumed data taking (SK- II) Resumed K2K beam (K2K-II) ν C Scientific American K2K finished Confirm ν oscillation by accelerator ν Stopped data taking for full reconstruction 42m M. Miura Water Cherenkov detector 1000 m underground 50,000 ton (22,500 ton fid.) 11, inch PMTs 1,885 anti-counter PMTs E > 5 MeV E resolution: 14 5, inch PMTs E > 7 MeV E resolution: 21 9

11 SK-I, SK-II combined analysis Yumiko Takenaga Merida, July 11, 2007 Tom Gaisser 10

12 SK extension to low energy Reconstruction algorithms were refined during SK-II to overcome loss of PMTs Potential to extend threshold to ~3 MeV Solar neutrinos in transition region Reactor anti-neutrinos Detection of low-energy ν e + p n + e + requires addition of Gd to detect recoil n Bonus: this will allow improved search for relic supernova ν e Merida, July 11, 2007 Tom Gaisser 11

13 oscillated/unoscillated 1.0 Why Study Low Energy Events? after simple cuts (vertex correl., fiducial volume,...) expected spectrum from one year of SK ν data (15 reactors) with Gd (current best-fit oscillation parameters) Reconstructed Total Positron Energy (MeV) P(ν e ν e ) Michael Smy SSM ν spectrum p 0.8 p 0.8 Vacuum osc. 7Be dominant Expected P(ν e ν e ) pep B precision measurement of solar neutrino oscillation parameters with reactor neutrinos need 0.1% GdCl 3 to tag neutrons in delayed coincidence MSW transition for solar neutrinos oscillations 0.2 matter osc. dominant ν e both require very low energy threshold & precise energy 12calibration Courtesy K. Bays, UC Irvine & M. Nakahata, ICRR Gd 0.2 γ s with ΣE=8MeV

14 Neutrino oscillation status L/E dip seen at first oscillation minimum No evidence yet for any non-standard oscillations, only upper limits for sterile neutrinos oscillations increasing with energy No sign yet of possible second-order oscillation effects three-neutrino effects θ 13 MINOS in NuMi beam results consistent with SK Merida, July 11, 2007 Tom Gaisser 13

15 14 p Predicting Unoscillated FD Spectrum Targe t MINOS in NuMi neutrino beam, Alexandre Sousa π + Decay Pipe Start with Near Detector data and perform extrapolation to the Far Detector Use knowledge of pion decay kinematics and beamline geometry to construct a beam transport matrix and predict FD spectrum from measured ND spectrum The Beam Matrix method is the primary method used in the MINOS CC analysis ND FD =

16 15 MINOS Best Fit Spectrum PRL 97, (2006) Best fit energy spectrum and Data/MC Ratio for POT Sample Observed Expected (Unoscillated) ν µ (<30 GeV) ±14.4 ν µ (<10 GeV) ±10.7 ν µ (<5 GeV) ±8.8

17 Atmospheric neutrinos in MINOS First detector with ability to determine sign of atmospheric neutrinos Too small to obtain good statistics Note reversal of muon charge ratio: muon neutrino / muon anti-neutrino > 1 therefore µ - / µ+ > 1 Merida, July 11, 2007 Tom Gaisser 16

18 Atmospheric ν as background Plot shows sum of neutrinos + antineutrinos ν e ν µ Solar ν Prompt ν RPQM for prompt ν Bugaev et al., PRD58 (1998) Slope = 2.7 Slope = 3.7 Merida, July 11, 2007 Tom Gaisser 17

19 Atmospheric ν as background Expected flux of relic supernova neutrinos Plot shows sum of neutrinos + antineutrinos ν e ν µ Solar ν Prompt ν RPQM for prompt ν Bugaev et al., PRD58 (1998) Slope = 2.7 Slope = 3.7 Merida, July 11, 2007 Tom Gaisser 17

20 Atmospheric ν as background Expected flux of relic supernova neutrinos ν e Plot shows sum of neutrinos + antineutrinos ν µ Possible E -2 diffuse astrophysical spectrum (WB bound / 2 for osc) Solar ν Prompt ν RPQM for prompt ν Bugaev et al., PRD58 (1998) Slope = 2.7 Slope = 3.7 Merida, July 11, 2007 Tom Gaisser 17

21 Atmospheric ν as background Expected flux of relic supernova neutrinos ν e Plot shows sum of neutrinos + antineutrinos ν µ Possible E -2 diffuse astrophysical spectrum (WB bound / 2 for osc) Solar ν Refined calculations in GeV range: M.Honda, G. Barr Prompt ν RPQM for prompt ν Bugaev et al., PRD58 (1998) Slope = 2.7 Slope = 3.7 Merida, July 11, 2007 Tom Gaisser 17

22 Atmospheric vs astrophysical ν Atmospheric ν µ : ν e : ν τ ~ 2:1:0 Steady flux sec(θ) distribution Steep spectrum ν e very steep prompt neutrinos ν µ : ν e = 1:1 normalization uncertain harder spectrum Astrophysical ν µ : ν e : ν τ ~ 1:1:1 Flux may be variable Point sources expected Harder spectrum All flavors similar spectra Charm decay is important background for search for astrophysical neutrinos Merida, July 11, 2007 Tom Gaisser 18

23 T. Iida, HE2.3 Merida, July 11, 2007 Tom Gaisser 19

24 Diffuse, relic supernova neutrinos Super-K limit is from ν e + p n + e + Neutron not detected in current Super-K Backgrounds: atmospheric ν e and ν e solar ν e and reactor ν e atmospheric ν µ µ (E µ < 50 MeV) Stopped µ below threshold atmosphere ν e interactions Merida, July 11, 2007 Tom Gaisser 20

25 Improvement with tagged neutron Beacom & Vagins, PRL 93 (2004) Prescribe gadolinium additive to detect neutrons and eliminate background and select anti-ν e only Merida, July 11, 2007 Tom Gaisser 21

26 Improvement with tagged neutron Beacom & Vagins, PRL 93 (2004) Prescribe gadolinium additive to detect neutrons and eliminate background and select anti-ν e only Current limits close to expectation! Merida, July 11, 2007 Tom Gaisser 21

27 Time Information: Sliding Window Search Livermore simulation (Totani et.al. 1998) sec Time Profile of SN burst Sliding Time window search M. Ikeda, Super-K Time duration of main burst is about 10 sec. Prompt burst of ν e is so called neutronization burst whose time duration is expected as ~10msec. 1. Set timewindow (Δt) and multiplicity threshold (M thr. ) M thr. events/δt Δt Event time 22

28 Time Information: Sliding Window Search Livermore simulation (Totani et.al. 1998) sec Time Profile of SN burst Sliding Time window search M. Ikeda, Super-K Time duration of main burst is about 10 sec. Prompt burst of ν e is so called neutronization burst whose time duration is expected as ~10msec. 1. Set timewindow (Δt) and multiplicity threshold (M thr. ) M thr. events/δt Δt Multiplicity threshold Event time 22

29 S-K Summary (SN burst search) Using data from Super-K, 3 methods of supernova searches with newly installed criteria was conducted. Data set : from May 1996 to Oct 2005 Total livetime: days (Livetime for 3rd analysis : days) No candidate was observed 100% detection probability up to 100 kpc SN rate within 100kpc(LMC,SMC,our Galaxy) is estimated < % C.L. Detection probability is maintained at a level of 7% for SN at Andromeda. No candidate of neutronization burst observed 23

30 RUN Since: To: Uptime [days] Duty Cycle Mass [tonn] PUBLISHED RUN 1 Jun 6 th 92 May 31 st % rd ICRC 1993 RUN 2 Aug 4 th 93 Mar 11 th % th ICRC 1995 RUN 3 Mar 11 th 95 Apr 30 th % th ICRC 1997 RUN 4 Apr 30 th 97 Mar 15 th % th ICRC 1999 RUN 5 Mar 16 th 99 Dec 11 th % th ICRC 2001 RUN 6 Dec 12 th 00 Mar 24 th % th ICRC 2003 RUN 7 Mar 25 th 03 Feb 4 th >99% th ICRC 2005 RUN 8 Feb 5 th 05 May 31 st >99% th ICRC 2007 Total 4919 days Upper Limit to SN event in the Milky Way 0.17 /year (90% c.l.) 30 th International Cosmic Ray Conference Merida, Mexico C.Vigorito, University & INFN Torino, Italy

31 Detectors sensitive to high-energy neutrinos Neutrino telescopes Primarily aimed at >TeV, upward ν µ -induced ν e.g. IceCube/AMANDA, Baikal, Antares, Nestor, KM3net Also sensitive to PeV, EeV ν, but limited area Radio, acoustic detection Threshold in EeV range Giant EAS detectors sensitive to ~EeV ν e.g. Auger, HiRes, CRTNT Merida, July 11, 2007 Tom Gaisser 25

32 IceCube : 13 strings deployed : 8 strings 1450m : 1 string 2450m 26

33 IceCube IceTop Air shower detector 80 pairs of ice Cherenkov tanks Threshold ~ 300 TeV : 13 strings deployed Current configuration - 22 strings - 52 surface tanks : 8 strings InIce Planned 80 strings of 60 optical modules each 17 m between modules 125 m string separation 1450m 2450m : 1 string AMANDA-II 19 strings 677 modules 26

34 IceCube IceTop Air shower detector 80 pairs of ice Cherenkov tanks Threshold ~ 300 TeV : 13 strings deployed Current configuration - 22 strings - 52 surface tanks : 8 strings InIce Planned 80 strings of 60 optical modules each 17 m between modules 125 m string separation 1450m 2450m : 1 string AMANDA-II 19 strings 677 modules 2007/08: add 14 to 18 strings and tank stations 26 Completion by 2011.

35 IceCube IceTop Air shower detector 80 pairs of ice Cherenkov tanks Threshold ~ 300 TeV : 13 strings deployed Current configuration - 22 strings - 52 surface tanks : 8 strings InIce Planned 80 strings of 60 optical modules each 1450m : 1 string AMANDA-II 19 strings 677 modules 17 m between modules 125 m string separation 2450m 2007/08: add 14 to 18 strings and tank stations AMANDA now operating as part of IceCube -talk of A. Gross 26 Completion by 2011.

36 Atmospheric neutrinos in IceCube Paolo Desiati, John Pretz Merida, July 11, 2007 Tom Gaisser 27

37 Goals for neutrino astronomy Point source searches Unbinned search improves sensitivity (Braun, Aguilar) Search for clusters in time and space (E. Bernardini, R. Porrata) Search for neutrinos from identified GRB (I. Taboada) Multi-messenger Target of Opportunity in coincidence with gamma-ray telescope see Gavin Rowell s rapporteur talk for details of the ν/γ connection Atmospheric ν and search for diffuse astrophysical ν covered here Merida, July 11, 2007 Tom Gaisser 28

38 Neutrino effective area for ANTARES S. Escoffier, ANTARES background sources and effects ICRC 07, Merida

39 Neutrino effective area for ANTARES S. Escoffier, ANTARES background sources and effects ICRC 07, Merida

40 Neutrino effective area for ANTARES 10 cm 2 S. Escoffier, ANTARES background sources and effects ICRC 07, Merida

41 Point source search with IceCube-9 Chad Finley IC9 point source limit IC9: Neutrino effective area Merida, July 11, 2007 Tom Gaisser 30

42 Expected ν flux from galactic point sources, example: RXJ Christian Stegmann et al. Merida, July 11, 2007 Tom Gaisser 31

43 Note importance of background of atmospheric ν in a km 3 detector Merida, July 11, 2007 Tom Gaisser 32

44 Note importance of background of atmospheric ν in a km 3 detector Merida, July 11, 2007 Tom Gaisser 32

45 Search for diffuse ν with hard spectrum Gary Hill et al. Merida, July 11, 2007 Tom Gaisser 33

46 AMANDA 4 yrs atmospheric ν preliminary [1] Achterberg et al., astro-ph/ Kirsten Münich 30th ICRC, Mexico July 2007

47 AMANDA cascade searches (>PeV) Lisa Gerhardt Merida, July 11, 2007 Tom Gaisser 35

48 AMANDA cascade searches Merida, July 11, 2007 Tom Gaisser 36

49 AMANDA cascade searches Similar cascade search with different energy-dependent variable in paper by Oxana Tarasova for AMANDA Merida, July 11, 2007 Tom Gaisser 36

50 BAIKAL, Ralf Wischnewski NT200+ = NT long outer R.Wischnewski ICRC, Merida, 2007 Km 3 planned - Height = 210m - = 200m - Geom.Volume ~ 5 Mton 37

51 Atmospheric Muon-Neutrinos E_thr ~ 15GeV Skyplot of NT200 neutrino events / 5 years (galactic coordinates) Galactic center visible 18 hours per day R.Wischnewski ICRC, Merida, Data: 372 upward ν events ( ). ( N µ (>15GeV)/N µ (>1GeV)~1/7 ) - MC: 385 ev. expected (15%BG). A high statistics neutrino sample for Point-Source Search, incl. GalCenter. No evidence for non-atmosph. ν s. 38

52 ICRC/ H.E.2.3/ ANTARES: Conclusions and Outlook Antoine Kouchner Major step forward during the last year Detector working well within design specifications: Junction Box in operation since Dec lines delivering data on the site All technical problems solved 12 lines detector complete early 2008: Operation for science 5 years Milestone towards a KM 3 underwater detector

53 ICRC/ H.E.2.3/ ANTARES: Conclusions and Outlook Antoine Kouchner Major step forward during the last year Detector working well within design specifications: Junction Box in operation since Dec lines delivering data on the site All technical problems solved 12 lines detector complete early 2008: Operation for science 5 years Milestone towards a KM 3 underwater detector Candidates for first undersea neutrino!!

54 ICRC/ H.E.2.3/ 2007 Zenith angle distribution 40 number of events After quality cuts 5 lines 2007 data No alignement ANTARES PRELIMINARY µ cos θ

55 ICRC/ H.E.2.3/ 2007 Zenith angle distribution 40 number of events After quality cuts 5 lines 2007 data No alignement ANTARES PRELIMINARY µ Indicates good angular resolution cos θ

56 ICRC/ H.E.2.3/ line detector displays 41 µ

57 NEMO km 3 Conceptual Design NEMO 3600 /17

58 Toward the ν-telescope EU funded the joint activity for a European-scale Design Study for a km 3 ν-telescope in the Mediterranean Sea KM3NeT: ANTARES-NEMO-NESTOR consortium The 2000 experience gained will contribute to the advancement of the 3000 KM3NeT activities NEMO 3600 /17

59 Region of sky observable by Neutrino Telescopes John Carr AMANDA (South Pole) ANTARES (43 North) Mkn 421 Mkn 501 Mkn 501 CRAB RX J CRAB SS433 SS433 GX339-4 VELA Galactic Centre 44

60 Quest for cosmogenic ν Motivated by indication of GZK feature in UHE cosmic-ray spectrum Cosmogenic ν (from p + γ 2.7 n + π + ν) Probe evolution, composition, spectra of extragalactic cosmic-ray sources Goal: >1000 km 3 sr, > 100 events/yr, E >10 18 ev RICE, AURA, ANITA, ARIANNA at this conference Acoustic detection in Ice another possibility Merida, July 11, 2007 Tom Gaisser 45

61 Model dependence of cosmogenic ν N. Busca Pure protons Mixed Cosmic rays Neutrinos

62 >PeV ν absorbed in the Earth Earth-skimming ν E. Bernardini Merida, July 11, 2007 Tom Gaisser 47

63 Neutrinos: important bi-product in Auger ν h Karl-Heinz Kampert em µ ~30 atm 1 atm h

64 Neutrinos: important bi-product in Auger ν h A neutrino can induce a young horizontal shower! Karl-Heinz Kampert em µ ~30 atm h 1 atm

65 EeV ν τ detection with Auger et al. D. Gora <~ 1 GZK ν τ / year in Auger Γcτ ~ 100 km for E τ ~ 2 x ev followed by τ-decay shower T. Weiler, D. Fargion Merida, July 11, 2007 Tom Gaisser 49

66 Current upper limit from Auger Oscar Blanch-Bigas Merida, July 11, 2007 Tom Gaisser 50

67 Current upper limit from Auger Oscar Blanch-Bigas HiRes limit < E n < ev slightly above Auger limit --Kai Martens Merida, July 11, 2007 Tom Gaisser 50

68 Km 3 telescopes can also do ν τ G. Miele --talk describes how to unfold neutrino Cross section Merida, July 11, 2007 Tom Gaisser 51

69 The radio technique Jaime Alvarez-Muniz Conditions for coherent radio emission 1. Net excess charge MOON REGOLITH 2. λ obs > shower dimensions L Δθ Diffraction by a slit Δθ ~ (νl) -1 J. Alvarez-Muñiz et al. ICRC 2007, Mérida (México)

70 Merida, July 11, 2007 Tom Gaisser 53

71 Detector was tested in pulsed electron beam at SLAC Jeff Kowalski Merida, July 11, 2007 Tom Gaisser 53

72 Merida, July 11, 2007 Tom Gaisser 54

73 Merida, July 11, 2007 Tom Gaisser 55

74 Proposed detectors AURA at South Pole digitize signal at antenna cluster --Hagar Landsman ARIANNA Steve Barwick Merida, July 11, 2007 Tom Gaisser 56

75 SPATS Geometry Vertical Testing acoustic detection at the South Pole --Justin Vandenbroucke 80 m Horizontal

76 Simulated hybrid array geometry J. Vandenbroucke astro-ph/

77 Calibrate radio technique with Askaryan pulses from air Askaryan pulses from air shower cores, Merida, 30 th ICRC, July (Seckel) 59

78 Calibrate radio technique with Askaryan pulses from air 1 cm 1 m 100 m Askaryan pulses from air shower cores, Merida, 30 th ICRC, July (Seckel) 59

79 Sensitivity and limits S. Barwick, ARIANNA N. Busca Merida, July 11, 2007 Tom Gaisser 60

80 Concluding comments TeV muon charge ratio important new result from MINOS Implications for >TeV atmospheric neutrinos SK-III fully operational for one-year Expect lower threshold, doping with Gd Expect to find Supernova relic neutrinos IceCube running with 22 strings, completion by 2011 Antares progressing well; Km3net plan km-scale neutrino telescope in the Mediterranean Intense interest in detecting GZK neutrinos Goal should be 1000 km 3 for 100 GZK ν per year Need to calibrate the technique use EAS cores? Merida, July 11, 2007 Tom Gaisser 61

81 Late news July 10, 2007 The National Science Foundation (NSF) today announced selection of a University of California-Berkeley proposal to produce a technical design for a Deep Underground Science and Engineering Laboratory (DUSEL) at the former Homestake gold mine near Lead, S.D. The Homestake team, headed by Kevin Lesko, could receive up to $5 million per year for up to three years. Merida, July 11, 2007 Tom Gaisser 62

82 Extras Merida, July 11, 2007 Tom Gaisser 63

83 Calculations of anti-ν e background MeV Note dependence on phase of solar cycle: 10 20% variation a signature of background, not of signal similar to response of neutron monitors FLUKA MeV Battistoni et al.(2004): 64

84 All flavor limits by AMANDA Ignacio Taboada Cascade (Rolling) Cascade (Trig & Roll) R03b WB03 MN06 n m search R03a Merida, July 11, 2007 Tom Gaisser