A Large High Altitude Air Shower Observatory : the LHAASO Project

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1 A Large High Altitude Air Shower Observatory : the LHAASO Project Olivier Deligny CNRS/IN2P3 - IPN Orsay on behalf the LHAASO Collaboration Contact Person: Zhen CAO, IHEP Rencontres de Moriond, 9/16 March

2 Origin of Cosmic Rays? Because of their amazing spectrum extreme regularity over 13 decades in energy spanning 32 decades in flux Non-thermal spectrum, with few breaks Usual suspect in the Galaxy : supernova remnants (taking 10% of the kinetic energy converted into accelerated particles through diffusive shock) Difficulty to accelerate 17 above 10 ev in SNRs Usual suspects above 10 ev : extragalactic objects such as Active Galactic Nuclei or Gamma Ray Bursts 17 Scientific Motivation for LHAASO : track back to the origin of CRs with - High Energy Gamma Rays - Cosmic Ray Studies 2

3 cosmic ray anisotropy in arrival direction al Journal Supplement Series, 203:34 (20pp), 2012 December Sky Maps of Cosmic Rays 1<E[EeV]<2 Tibet-III 2<E[EeV]<4 equatorial coordinates 5 TeV courtesy Kazuoki Munakata At The Pierre Auger Collaboration IceCube-59 anisotropy vs energy 20 TeV Abreu et al.,e[eev]>8 Astrop. Phys., 34, 627, [%] EAS-TOP Aglietta et al., ApJ, 692, L130, relative intensity IceCube-22 Abbasi et al., ApJ, 718, L194, IceCube <E[EeV]<8 Tibet AS! Amenomori et al., ApJ. 626, L29, low energies, significant dipoles and higher order 0 multipoles have been observed At higher energies, the statistics is more limited : upper limits have been set ! Energy [GeV] 300 3,000 pc -3 ance sky maps in four independent energy bins. The maps are smoothed using an angular window with radius Θ = 1 rad to exhibit any dipolar-like ections of the reconstructed dipoles are shown with the associated uncertainties. The Galactic plane and Galactic center are also depicted as the (3 µg) star. At the-3 highest energies, some 3!10 3!10 3! gyro-radius (pc) f this figure is-5available in -4the online journal.) 3!10-2 correlations with nearby 700 7,000 70,000 gyro-radius (AU) extragalactic matter beensince found influence in the28rightheliospheric panel ofinfluence Figure 6, galactic restricted to the havefinally, some consistency is observed both in declinaonsidered here. Though the phase and tion and right but havebetween not 4allowed yet theascension as a function of energy, the use of larger y determined due to the corresponding direction energy intervals and/or energy thresholds may help to pick up identification of sources pointing close to the equatorial South Pole, it is a significant signal above the background level. The amplitudes 7 70 t a consistent smooth behavior is observed using esented here and applied to a data set containing of the dipole are shown in Figure 8 for two energy intervals (1 < E/[EeV] < 4 and E > 4 EeV) and as a function of en- 3

4 High-Energy Gamma Rays Counterpart of accelerated electrons (inverse Compton scattering, Bremsstrahlung) Is there a counterpart of accelerated hadrons? Few evidences with current data At TeV energies, ~120 sources discovered Crucial to get more sources (spectral index, cut-off above 100 TeV?,...) 4

5 Probing GCRs Acceleration with High-Energy Gamma Rays? Crab Nebula The Universe is opaque to gamma rays at high energy... (interactions with Extragalactic Background Light) Difficult to produce HE gamma rays with electrons above 100 TeV : smoking guns for CRs acceleration could be found there. 5

6 Transient Sources and XGal CRs What fraction of GRBs emit GeV or TeV gamma rays? How much energy is available in these objects to accelerate CRs? Observations at the highest photon energies are necessary to understand the acceleration processes and energy budgets in GRBs Since GRBs are located at cosmological distances, the highest energies of gamma rays are likely to be in the 50 to 300 GeV range, depending on the redshift Need for an observatory with a wide f.o.v. and high duty cycle to observe transient sources at >100 GeV 6

7 XGal variables - AGN Flares continuously monitor flares notify multi-wavelengths observers discover orphan TeV flares 7

8 Science Goals of a Wide-Field Instrument - Galactic Cosmic Ray Origins - Highest Energies in Gamma Rays - Galactic Diffuse Emission - Particle Acceleration in Jets - Gamma Ray Bursts at Highest Energies - AGN Flaring - Multi-wavelengths and multi-messenger campaigns - Complete Survey 8

9 LHAASO Objectives - All sky survey γ-ray astronomy in the ~100 GeV-~1 PeV range - high sensitivity and energy resolution sources and energy spectrum - full duty cycle, wide FOV and sensitivity transient - as good as possible γ-hadron discrimination power, - high angular resolution - Cosmic ray detection between 10 TeV and 100 PeV - Bridge between space/balloon borne measurements and ground based UHECR measurements - Unprecedented statistics for anisotropy studies in the knee region 9

10 Survey of the Gamma Sky 2 possible techniques Cerenkov imaging of gamma-ray showers (IACT) Detection at ground of gamma-ray showers Ex: HESS, MAGIC, VERITAS then CTA Ex: ARGO, MILAGRO, Tibet-ASγ, HAWC - High sensitivity (γ hadron separation) - Good spatial resolution BUT - Low duty cycle - Limited field of view - 100% duty cycle - Large field of View BUT Lower rejection power LHAASO : Detection at ground of gamma-ray showers optimizing the rejection power with large collection surface and multiparameter measures 10

11 LHAASO - General Design 4300 m a.s.l. Yunnan province (China) WCDA m 2 water Cerenkov detector for γ>100gev 4 ponds of Water Cerenkov + μ detectors under water Cerenkov detectors KM2A 1km 2 complex array covering m 2 for γ >30TeV and CRs Array of 5000 scintillation detectors Array of 1200 μdetectors buried water Cerenkov detectors WFCTA - Array of 24 WFV Cerenkov-telescopes for CRs 11

12 Water Cerenkov Detectors MILAGRO-like pools ~4 times HAWC in surface 12

13 '#(4$5256/((("(("(! 01%2$&,'*+$,$-./)!!"#$%&'(&)$#'*+$,$-./)! LHAASO - KM2A SIMULATION "#!$!%"&&'!()*+,'!-".+/)&!01!,/)2!!! "#!$!(+L)*.B!01!%)M,2!! *34560! :81;!!!!!!!!!!!! <687=38>85418?5!*)(()@%)A.BCD2! E?550!3;7?:F18?5!7G4184:02!!! J?5=18?550!NOO!P!6F!10>G72!!!"#$%!! *3456!=H4>G!60!IF0!<QF::R7STD2!!!!!!2(! KM2A: Array of scintillators! (Ne) and buried muon detectors (Nmu) " " " 3405'!! U?FI?83!60!687=38>85418?5!!!!!!!!! *)(()!@!%)A.BC!68QV8=8:0!W!!! */* 3405'!,H4>G!60!IF0!:8>81;2! J?5=18?550!F58KF0>051!60!5F812!! :%;9:%:<=>8=??489@5:%%1% % #! >)1+*:)$*:!A!B!C!DEFGH!C!IJ!1! #! K,-)::+&#!:')*()55-(+&#!A!G!'1! #! "5-6&+!%+!,5$1L!A!H!11! #! M)L#+:!$,()6&+:!3N!"9! #!3! O')*()55-(+&#!A!P*(2#-'Q*+!D0IBRIEJ!! Journées DR 23 janvier !! " " " "!! 3# " " " Journées DR 23 janvier 20 13

14 Sensitivity to Gamma-Ray Sources Detection of gamma rays in an overwhelming background of CRs... Excess of gamma-ray showers in a target window : S(> E) = N γ(> E) NCR (> E) Q, hadrons/gamma discrimination power (Nmu vs Ne) : r ɛ γ / 1 ɛ CR. N γ (> E) = n 1y T N CR (> E) = n 1y dt T dt E de A γ eff E (E,θ(t)) cosθ(t) Φcrab γ (E) ξ(δω), de A CR eff (E,θ(t)) cosθ(t) I CR(E) δω, Requirements : large acceptance and good angular resolution 14

15 Angular Resolution Shower front = bulk of particles grouped in a thick nearly spherical pancake The thickness of this spherical cap depends on the distance to the shower axis Non-weighted fit : Iterations of a planar fit, removing tails in the residual distribution New iterations with conical corrections χ 2 (ns 2 )= 1 c 2 {lx i + my i + nz i + c(t i t 0 )} 2 i Events x plane fit 3 plane fit 5 plane fit M. Iacovacci et al Residuals(ns) 15

16 Survey of the Gamma Sky > 100 GeV A few hundred extra-galactic sources are expected WCDA : 4 ponds of water Cerenkov detectors covering m 2 Sensitivity expected : 2% of the Crab luminosity 16

17 Survey of the Gamma Sky > 10 TeV KM2A : shower array of muon and electron detectors (MD and ED) covering m 2 Expected performances: angular resolution - Energy resolution< 20% - Sensitivity of 1% of I crab 17

18 Cosmic Ray Measurements HYBRID detection with KM2A and WFCTA Array of 24 WFV Cerenkov-telescopes Combining Nmu+Xmax on an event by event basis is crucial to distinguish between light/heavy CRs Possible outcomes : - Individual energy spectra - Anisotropy studies as a function of the primary species 18

19 Observatory Construction It is planned for a construction of 5-6 years yrs Detector R/D 1.5 FEE R/D: 2 FEE Production: 1.5 DAQ & installation: 0.5 Detector deployment: 4 1% array test run: 1 now 6 yrs The total budget is about US$140M (financed by China) 19

20 International Collaboration ARGO upgrading for low energy extension IPNO / Omega ASIC electronics for LHAASO TUNKA on top of LHAASO-KM2A for high energy extension (>10 16 ev) Current and potential Collaborators 20

21 The LHAASO Project A ground based large and complex γ and CR observatory at high altitude Complementary to CTA for γ-ray astronomy Investigate detailed energy spectra for Galactic sources above 30 TeV Survey the whole sky for γ sources above 100 GeV CR measurements at the «knees» Engineering prototypes running at ARGO site 21

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