(high-energy) Multi-messenger astronomy with neutrinos, cosmic rays and gravitational waves - an experimental review - Véronique Van Elewyck (APC & Université Paris Diderot) 1 Multi-messenger astronomy: why and how Galac'c Extragalac'c GC engine PWN AGN μquasars SNR GRB Iden'fy the sources of high-energy cosmic radiaon and characterize the produc'on/acceleraon/interac'on mechanisms at play Multi-messenger astronomy: why and how HE photons: neutral, absorbed and interact with CMB/IRB What are we looking for ? Discover and understand the most violent phenomena in the universe Astrophysical sources of cosmic radiaon: galac'c/extragalac'c Multi-messenger astronomy: why and how HE photons: neutral, absorbed and interact with CMB/IRB Cosmic rays: deflected and interact with CMB What are we looking for ? Discover and understand the most violent phenomena in the universe Astrophysical sources of cosmic radiaon: galac'c/extragalac'c Multi-messenger astronomy: why and how HE photons: neutral, absorbed and interact with CMB/IRB Cosmic rays: deflected and interact with CMB Neutrinos: neutral,interact weakly, point to the source …and trace hadronic interac'ons What are we looking for ? Discover and understand the most violent phenomena in the universe Astrophysical sources of cosmic radiaon: galac'c/extragalac'c also hadronuclear (p-p) interac'ons at source at Earth Multi-messenger astronomy: why and how HE photons: neutral, absorbed and interact with CMB/IRB Cosmic rays: deflected and interact with CMB Neutrinos: neutral,interact weakly, point to the source …and trace hadronic interac'ons Gravitaonal waves: travel undisturbed by maer/EM fields …and trace source progenitors What are we looking for ? Discover and understand the most violent phenomena in the universe Astrophysical sources of cosmic radiaon: galac'c/extragalac'c ν GW CR γ Neutrino telescopes today KM3NeT 12 lines, completed 2008 ~ 0,02 km3 instrumented volume Prototype for a km3-sized detector in the Mediterranean: KM3NeT (ARCA & ORCA) under construction InIce: 86 lines, completed 2010 ~ 1 km3 instrumented volume DeepCore: 8 lines, dense infill IceTop: air shower array 7 Detection principle MUON (TRACK) TOPOLOGY: • νµ charged current • golden channel for astronomy: angular resolution < 0.2° - 0.4° in water < 1° in ice • interaction vertex can be outside of the detector: increased effective volume μ • ~30% resolu'on on log10(Eµ) time, position & amplitude of hits νμ energy & arrival direction of 8 ν Detection principle MUON (TRACK) TOPOLOGY: • νµ charged current • golden channel for astronomy: angular resolution < 0.2° - 0.4° in water < 1° in ice • interaction vertex can be outside of the detector: increased effective volume μ • ~30% resolu'on on log10(Eµ) … But large background from atmospheric muons: go deep look downwards νμ apply veto 9 Detection principle CASCADE (shower) TOPOLOGY: • νe ντ charged current + all flavors neutral current • mostly contained events, ~spherical topology: energy resolution ~5% • angular resolution strongly affected by optical properties of the medium (water vs ice): ~ 3° ANTARES (2° for KM3NeT) ~ 10° IceCube 10 TeV – 1 PeV e νe 10 Status of neutrino astronomy See A. Capone: ANTARES/KM3NeT – Astropar'cle Physics Session Wed 12:00 See D. Grant: IceCube results – Plenary session Fri The IceCube signal is robust… and challenging ! Discovery channel: signal also observed in other channels: HESE, now 4-year sample e.g. upgoing νμ (tracks) from all-sky, all-flavour (tracks+cascades) Northern sky only best fit (E > 30 TeV): bestBest fit (190 fit (190 TeVTeV – 8 – 8 PeVPeV) ): ? ~ E-2.6 ~ E-2.1 Status of neutrino astronomy Different energy thresholds… Different sky coverages… Spectral index inferred from samples with Different flavour content… - different energy thresholds… E>25 TeV - different sky coverages… - different flavour content… Indicaon of spectral break ? Indicaon of Galac'c + extragalac'c components ? E>190 TeV −6 ] 10 -2 Atmospheric neutrinos cm -1 PRELIMINARY IceCube flux sr -1 ANTARES sensitivity (2007-2015) …Latest ANTARES results 10−7 Γ = 2.5 ANTARES upper limit (this analysis) compable with IceCube signal, but no significant excess yet: /dE [GeV s 1f Φ Γ = 2 d 2 10−8 E 2007-2015 combined (tracks +cascades) 10−9 4 4.5 5 5.5 6 6.5 7 log (E /GeV) 10 ν Status of neutrino astronomy & PoS ICRC 2015 (2016) & ApJ 809 (2015) Different energy thresholds… The Astrophysical Journal 809 (2015) 98 Different sky coverages… Different flavour content… Different energy thresholds… Different sky coverages… Indicaon of spectral break ? Different flavour content… Indicaon of Galac'c + extragalac'c components ? Signal consistent with an isotropic diffuse flux (> 100 sources) Event flavour distribu'on consistent with standard oscillaons; excludes No source idenfied No electromagne'c counterpart observed neutron decay scenario at 3.6 σ WHERE AND WHICH ARE THE SOURCES ? ? main observables: spectrum – composi'on – anisotropies (same as for UHE cosmic rays !) no evidence for anisotropies so far… but: need good angular/energy accuracy all-flavour astronomy Limited angular resolu'on (~10° for cascades) mul-messenger programs (TIME and SPACE coincidences) Status of neutrino astronomy & ApJ 809 (2015) Different energy thresholds… The Astrophysical Journal 809 (2015) 98 Different sky coverages… Different flavour content… Different energy thresholds… Different sky coverages… Indicaon of spectral break ? Different flavour content… Indicaon of Galac'c + extragalac'c components ? & Moharana et al., PoS ICRC 2015 (2016) Signal consistent with an isotropic diffuse flux (> 100 sources) Event flavour distribu'on consistent with standard oscillaons; excludes No source idenfied No electromagne'c counterpart observed neutron decay scenario at 3.6 σ WHERE AND WHICH ARE THE SOURCES ? ? main observables: spectrum – composi'on – anisotropies (same as for UHE cosmic rays !) no evidence for anisotropies so far… but: need good angular/energy accuracy all-flavour astronomy Limited angular resolu'on (~10° for cascades) mul-messenger programs (TIME and SPACE coincidences) Searches for neutrinos from the Galactic Plane Most recent analysis tes'ng KRAγ model of & arXiv 1705.00497 CR diffusion in the Galaxy: radial dependance of the slope of the diffusion coefficient & the advec've wind ANTARES 90% UL 2016 IceCube HESE New ANTARES 90% UL, ν 50 PeV cutoff IceCube prelim (IPA 2017) v Up to 19% of IceCube HESE sample KRAγ 50PeV cut-off for CR can originate from Galac'c CR KRAγ 5PeV cut-off for CR diffusion v Galac'c CR interac'on with gas cannot explain the spectral anomaly … combined study ANTARES+IceCube underway à increase in sensi'vity expected Searches for neutrino point sources ground.IceCube: 2008-2015, > 700 000 events 2 Candidatethrough-going list search. In the second + star'ng approach, the tracks directions of a pre-defined list of known All-sky + candidate sources: objects which are neutrino source candidates are investigated to look for an excess or (in No significant excess found so far the case & of ApJ null observation) 835 (2017) to determine an upper limit on their neutrino fluxes. 3 Galactic Centre region. The third search is similar to the full sky search but restricted to a in the data region centred in the origin of the galactic coordinate system (↵, δ)=(266.40◦,–28.94◦)and defined by an ellipse with a semi-axis of 15◦ in the direction of the galactic latitude and a −5 ] 10 Latest searches ANTARES (paper PS) & IC (which paper ?) -1 ANTARES 2007-15 sensitivity semi-axis of 20◦ in galactic longitude. The motivation relies on the number of high-energy s ANTARES 2007-15 sensitivity (E < 100 TeV) ν neutrino events observed by the IceCube (IC) detector [19, 20] that appear to cluster in -2 ANTARES 2007-15 limits (candidate list) ANTARES 2007-15 limits (candidate list for HESE events) this region. Furthermore, the HESS Collaboration recently discovered an accelerator of ANTARES 2007-15 limits (1 declination bands) −6 ° PeV protons in the Galactic Centre [21] that could produce high-energy neutrinos. 10 IceCube 7 years sensitivity [ApJ 835(2017)2 151] Advantag of combining ANTARES+IC samples IceCube 3 years MESE sensitivity (E < 100 TeV) [ApJ 824(2016)2 L28] ν [GeV cm IceCube 7 years limits [ApJ 835(2017)2 151] 4 Sagittarius A*. Finally, the fourth approach tests the location of Sagittarius A* as an extended (à backup) source by assuming a Gaussian emission profile of various widths. 90%CL −7 Φ 10 2 Figure 6 represents the event sample in equatorial coordinates in the ANTARES visible sky. E The considered neutrino source candidates and the search region around the Galactic Centre are 10−8 also indicated. ANTARES: 2007-2015 10−9 7629 tracks + 180 showers 10−10 −1 −0.8 −0.6 −0.4 −0.2 0 0.2 0.4 0.6 0.8 1 sinδ Figure 9: Upper limits at a 90 % C.L. on the signal flux from the investigated candidates assuming 2 an E− spectrum (red circles). The dashed red line shows the ANTARES sensitivity and the blue dashedComplementarity line the sensitivity of the seven ANTARES - years point-like sourceIceCube analysis by the IceCube Collaboration for comparison [24]. The upper-limits obtained in this analysis are also included (blue dots).at E < 100 The ANTARES 5TeVσ pre-trial discovery flux is a factor 2.5 to 2.9 larger than the sensitivity. The curve for the sensitivity for neutrino energies under 100 TeV is also included (solid red line). The IceCube curve for energies under 100 TeV (solid blue line) is obtained from the 3 yearsCombined MESE analysis [25]. analysis The limits of the 2007-2012 most significant cluster obtained in bands of 1◦ in declination (dark red squares) are also shown. à Further improvement in sensi'vity GC region Candidate Sources 4.2 CandidateA new listcombined study underway… IC HESE tracks The candidate list used in the last ANTARES point-like source analysis [15] contained neutrino & arXiv 1706.01857 source candidates both from Galactic and extra-Galactic origin listed in the TeVCat catalogue [26].