Search for UHE photons and neutrinos using Telescope Array surface detector

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1 Search for UHE photons and neutrinos using Telescope Array surface detector G.I. Rubtsov, M. Fukushima, D. Ivanov, B. Stokes, G. Thomson, S.V. Troitsky for the Telescope Array Collaboration 32 th ICRC Beijing, August, 2011 Grigory I. Rubtsov for the Telescope Array collaboration Photon and neutrino search 1

2 Telescope Array surface detector 507 SD s, 3 m 2 each 680 km 2 area 3 years of operation Largest UHECR statistics in northern hemisphere Grigory I. Rubtsov for the Telescope Array collaboration Photon and neutrino search 2

3 Photon search strategy proton-induced EAS gamma-induced EAS Deep shower maximum and shortage of muons curved front Linsley s shower front curvature parameter a is used for photon/hadron separation Grigory I. Rubtsov for the Telescope Array collaboration Photon and neutrino search 3

4 Front curvature for typical event, θ = σ region Fit Photon MC data front delay [1200m]; core distance [1200m] Grigory I. Rubtsov for the Telescope Array collaboration Photon and neutrino search 4

5 Dataset Data collected by TA surface detector for three years: Cuts: 7 or more detectors triggered core distance to array boundary is larger than 1200m (one separation unit) χ 2 /d.o.f. < 5 45 < θ < 60 E γ > ev (E γ is estimated for every event using photon Monte-Carlo) 877 events after cuts Grigory I. Rubtsov for the Telescope Array collaboration Photon and neutrino search 5

6 Photon Monte-Carlo set CORSIKA with QGSJET-II, FLUKA and EGS4. PRESHOWER for geomagnetic field cascading Thinning with weight optimisation (ε = 10 6 ) Dethinning technique is used Kobal, Astropart.Phys.15: ,2001 Stokes et al, arxiv: Detector response is calculated with GEANT sampler E [ , ] ev, θ [0, 65 ] Exactly same cuts applied to data and Monte-Carlo sets Grigory I. Rubtsov for the Telescope Array collaboration Photon and neutrino search 6

7 Linsley curvature a : E > ev h_gm h_dt Entries Mean RMS Underflow Overflow h_gm h_dt Entries Mean RMS Underflow Overflow a h_gm h_dt Entries Mean RMS Underflow Overflow a a E γ > ev data photon MC, E 2 spectrum Grigory I. Rubtsov for the Telescope Array collaboration Photon and neutrino search 7

8 Event-by-event method For each event with curvature a obs we select photon MC events compatible by arrival direction and S 800. We calculate curvature distribution function f γ (a) for MC photons Let s define C = C is defined event-by-event a obs f γ (a)da For gamma events, C is uniformly distributed between 0 and 1 (independently of the photon primary spectrum). Gorbunov, GR, Troitsky, Astropart.Phys. 28:28-40 GR et al., AIP Conf.Proc Grigory I. Rubtsov for the Telescope Array collaboration Photon and neutrino search 8

9 C: E > ev < θ < 60 h_gm h_dt Entries Mean RMS Underflow 0 Overflow C data photon MC, E 2 spectrum Grigory I. Rubtsov for the Telescope Array collaboration Photon and neutrino search 9

10 Results Statistical test gives maximum expected number of photons in the set N γ Exposure A is calculated using photon MC conservatively assuming E 3 spectrum; E γ > ev, Nγ < 14.1, A = 643 km 2 sr yr E γ > ev, Nγ < 8.7, A = 887 km 2 sr yr E γ > ev, Nγ < 8.7, A = 1196 km 2 sr yr F γ = N γ /A E γ > ev, E γ > ev, E γ > ev, F γ < km 2 sr 1 yr 1 F γ < km 2 sr 1 yr 1 F γ < km 2 sr 1 yr 1 (95% CL) /PRELIMINARY/ Grigory I. Rubtsov for the Telescope Array collaboration Photon and neutrino search 10

11 Results Statistical test gives maximum expected number of photons in the set N γ Exposure A is calculated using photon MC conservatively assuming E 3 spectrum; E γ > ev, Nγ < 14.1, A = 643 km 2 sr yr E γ > ev, Nγ < 8.7, A = 887 km 2 sr yr E γ > ev, Nγ < 8.7, A = 1196 km 2 sr yr F γ = N γ /A E γ > ev, E γ > ev, E γ > ev, F γ < km 2 sr 1 yr 1 F γ < km 2 sr 1 yr 1 F γ < km 2 sr 1 yr 1 (95% CL) /PRELIMINARY/ Grigory I. Rubtsov for the Telescope Array collaboration Photon and neutrino search 11

12 Results Statistical test gives maximum expected number of photons in the set N γ Exposure A is calculated using photon MC conservatively assuming E 3 spectrum; E γ > ev, Nγ < 14.1, A = 643 km 2 sr yr E γ > ev, Nγ < 8.7, A = 887 km 2 sr yr E γ > ev, Nγ < 8.7, A = 1196 km 2 sr yr F γ = N γ /A E γ > ev, E γ > ev, E γ > ev, F γ < km 2 sr 1 yr 1 F γ < km 2 sr 1 yr 1 F γ < km 2 sr 1 yr 1 (95% CL) /PRELIMINARY/ Grigory I. Rubtsov for the Telescope Array collaboration Photon and neutrino search 12

13 Photon flux limits Log E 2 F Γ ev 2 km 2 yr 1 sr PRELIMINARY A Y TA PA Y PA Y A TA PA TA Log E min ev Grigory I. Rubtsov for the Telescope Array collaboration Photon and neutrino search 13

14 Photon fraction limits Ε Γ,% 100 A HP HP A A TA PA Y PF Y 10 TA PF YN PA PF PF PA AH AY YN YN PRELIMINARY Log E min ev Grigory I. Rubtsov for the Telescope Array collaboration Photon and neutrino search 14

15 Neutrino search strategy Neutrino produces very inclined young shower young shower, θ = 19.5 old shower, 78.3 long, indented wafeforms one peak Grigory I. Rubtsov for the Telescope Array collaboration Photon and neutrino search 15

16 Neutrino search We count waveform peaks per detector layer. peak FADC count higher than 3 right, 3 left neighbours and 0.2 VEM (separate on upper and lower layers) Dataset: TA surface detector, or more detectors triggered core distance to array boundary is larger than 1200m χ 2 /d.o.f. < 5 θ > 70 No energy (S 800 ) cut 785 events after cuts Grigory I. Rubtsov for the Telescope Array collaboration Photon and neutrino search 16

17 Number of peaks vs Zenith angle 7 data 6 5 peaks / layer 4 3 ν Zenith angle No young inclined showers in the dataset no neutrino candidates. Grigory I. Rubtsov for the Telescope Array collaboration Photon and neutrino search 17

18 Conclusions Photon flux limits are obtained above ev. Log E 2 F Γ ev 2 km 2 yr 1 sr PRELIMINARY Y Y Y Log E min ev A TA PA PA A TA PA TA Ε Γ,% YN A HP HP A A TA PA Y PF Y TA PF YN PF PA PF PA YN Log E min ev AH AY PRELIMINARY No down-going neutrino candidates, E ev. Grigory I. Rubtsov for the Telescope Array collaboration Photon and neutrino search 18

19 Backup slides Grigory I. Rubtsov for the Telescope Array collaboration Photon and neutrino search 19

20 Method details 1/2 For each event i we calculate curvature aobs i and curvature distribution fγ(a) i for MC photons. Then determine C i = a i obs f i γ(a)da For gamma events, C is uniformly distributed by definition. Let F γ be an integral flux of primary photons over a given energy range. Then we expect photons (A - exposure). N(F γ ) = F γ A Grigory I. Rubtsov for the Telescope Array collaboration Photon and neutrino search 20

21 Method details 2/2 Let P(N) be a conservative probability to have N photons in a dataset which is defined as a maximum over all subsets of N real events: P(N) = max P({i 1,..., i N }), i 1 <i 2 < <i N where P({i 1,..., i N }) is a statistical probability of the subset {i 1,..., i N } to be compatible with uniform distribution (100% photon events). We use Smirnov-Cramer-von Mises omega-square test. The constraint on the flux F γ at the confidence level of ξ follows from: P(N)W (N, N(F γ )) < 1 ξ. N Grigory I. Rubtsov for the Telescope Array collaboration Photon and neutrino search 21

22 Smirnov-Cramer-von Mises omega-square test Let F(x) be theoretical distribution and F n (x) observed distribution. We define the distance between distributions by: ω 2 = (F n (x) F(x)) 2 df(x). If x 1, x 2,..., x n is a set of observed values in increasing order, we have: nω 2 = 1 n ( ) 2i n + 2n F(x i). i=1 For this study any non-parametric statistical test may be used (e.g. KS test), but ω 2 test allows simple procedure for maximizing over all subsets of the dataset. Grigory I. Rubtsov for the Telescope Array collaboration Photon and neutrino search 22

23 Exposure calculation: E γ > ev We take MC photon set with E mc > ev conservatively assuming E 3 spectrum. We calculate the fraction of photons entering the search region. Geomertical exposure 45 < θ < 60 : A geom = 1286 km 2 sr yr 100% n det 7 67% χ 2 /d.o.f < 5 63% E γ > % A 19 total = 0.5 A geom = 643 km 2 sr yr Grigory I. Rubtsov for the Telescope Array collaboration Photon and neutrino search 23

24 Exposure calculation: E γ > ev We take MC photon set with E mc > ev conservatively assuming E 3 spectrum. We calculate the fraction of photons entering the search region. Geomertical exposure 45 < θ < 60 : A geom = 1286 km 2 sr yr 100% n det 7 95% χ 2 /d.o.f < 5 90% E γ > % A 19.5 total = 0.69 A geom = 887 km 2 sr yr Grigory I. Rubtsov for the Telescope Array collaboration Photon and neutrino search 24

25 Exposure calculation: E γ > ev We take MC photon set with E mc > ev conservatively assuming E 3 spectrum. We calculate the fraction of photons entering the search region. Geomertical exposure 45 < θ < 60 : A geom = 1286 km 2 sr yr 100% n det 7 99% χ 2 /d.o.f < 5 96% E γ > % A 20 total = 0.93 A geom = 1196 km 2 sr yr Grigory I. Rubtsov for the Telescope Array collaboration Photon and neutrino search 25

26 Comparison to median method Statistical method: E γ ev ev ev Events 45 < θ < N γ < A stat F γ < km 2 sr 1 yr 1 (95% CL) /PRELIMINARY/ Median method: E γ ev ev ev Events 45 < θ < Events C > Poisson 95% upper limit: A median = A stat / F γ < km 2 sr 1 yr 1 (95% CL) /PRELIMINARY/ Grigory I. Rubtsov for the Telescope Array collaboration Photon and neutrino search 26

27 Event reconstruction: fit functions Joint 7-parametric fit: x core, y core, θ, φ, S 800, t 0, a ( r f (r) = R m LDF (r) = f (r)/f (800 m) ) 1.2 ( 1 + r ) (η 1.2) (1 + r 2 ) 0.6 R m R1 2 S(r) = S 800 LDF (r) t 0 (r) = t 0 + t plane + a 0.67 (1 + r/r L ) 1.5 LDF (r) 0.5 R m = 90.0 m, R 1 = 1000 m, R L = 30 m η = (sec(θ) 1) Grigory I. Rubtsov for the Telescope Array collaboration Photon and neutrino search 27

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