Search for neutrinos from Fast Radio Bursts with the ANTARES telescope M. Sanguineti (INFN Genova) D. Turpin (IRAP/CPPM), D. Dornic (CPPM), A. Coleiro (APC, IFIC), E. Petroff, S. Bhandari, E. Keane (SUPERB) on behalf the ANTARES and SUPERB Collaborations ICRC 2017 @ Busan - 17/07/17
Fast Radio Burst Short transient : 1-10 ms and Very bright : 1-10 Jy ms (<S/N> = 22) → The brightest FRB 150807 reached S max = 128 Jy and S = 44.8 Jy ms ! Detected in : GHz energy band (typically close to 1.4 GHz) Frequency dependent delay : t( ν ) ≈ DM x ν -2 → Dispersion measure (DM) : 266.5 → 1629.18 cm -3 pc → column of free electrons responsible of the radio scattering Pulse broadening : W ≈ ν - 4 ms FRB150418 (@Parkes) “Lorimer“ burst : FRB 010724 M. Sanguineti - ICRC 2017 @ Busan - 14/07/17 2
The FRB sky (27 FRBs) ! High galactic latitude The image cannot be displayed. Your computer may not have enough memory to open the image, or the image Arecibo may have been corrupted. Restart your computer, and then open the file again. If the red x still appears, you may ! Expected rate : have to delete the image and then insert it again. GBT ~10 3 FRB/day/all sky Parkes UTMOST ASKAP ASKAP FRB 121102 FRB catalog : http://www.astronomy.swin.edu.au/pulsar/frbcat/ Green bank Parkes Arecibo UTMOST M. Sanguineti - ICRC 2017 @ Busan - 14/07/17 3
At which distance ? Same story as GRB before the detection of the 1st optical afterglow ~20 yrs ago How to measure the distance? - From the dispersion measure : DM tot = DM gal + DM host + DM excess => z ≤ 1200 / DM IGM (Ioka 2003, Inoue 2004) => DM excess ~100-1200 cm -3 pc => z DM ~0.2-1.4 => Evidence for cosmologic dist [DM max (PSR J0131-7310) = 205 cm -3 pc] - Identification of the host galaxy (need FRB good localisation) => Only case is FRB121102 (repeating): star forming dwarf galaxy at z=0.19 - Spectroscopic/photo redshift (need optical/IR counterparts) => No EM counter-part detected except radio In 2016, Keane et al. reports a long radio counterpart (afterglow) of FRB 150418 + host association with a serendipitous association with an AGN DeLaunay et al. reports the discovery of a weak γ -ray counterpart from FRB 131104 with the Swift satellite but still debate in the community M. Sanguineti - ICRC 2017 @ Busan - 14/07/17 4
Progenitor: nearby extragalactic origin FRB emission mechanism : Supergiant flares in the magnetosphere Milky Way of young (<100 yrs) and rapidly (ms) rotating neutron stars embedded in a dense environment → Crab-like flares Repeating : Yes Distance : 100-200 Mpc 100-200 Mpc DM excess (100-1000 cm -3 pc) : Local environment around the NS + extragalactic IGM constant flare by flare ? Young and rapidly rotating neutron stars M. Sanguineti - ICRC 2017 @ Busan - 14/07/17 5
Progenitor: cosmological origin FRB emission mechanism : Supra massive neutron star's collapse: magnetic blast wave, shock front within the SN remnant. Merger: Magnetic reconnection between the two merging magnetospheres. Milky Way Magnetar: Giant flares in the magnetosphere of a magnetar (possibly associated to SGR). Repeating : DM excess = IGM No/No/Yes 1-20 Gpc z ~ 0.1 - 2 Distance : ~1-20 Gpc DM excess (100-1000 cm -3 pc) : Local environment around the compact object + extragalactic IGM constant flare by flare (magnetar) M. Sanguineti - ICRC 2017 @ Busan - 14/07/17 6
FRB origin: still many missing parts What are the radiative processes ? Where are they located ? Their distances ? Need for an unambiguous host identification Need for a MW analysis Need for a spectroscopic obs. → redshift → SED → photometric redshift Need for MWL and MM Particle acceleration observations mechanisms ? → high-energy neutrinos Baryons ? Leptons ? = baryonic acceleration γ -rays ? → radio + GeV obs. = distinguish between leptonic and hadronic scenarios M. Sanguineti - ICRC 2017 @ Busan - 14/07/17 7
HE neutrinos in FRB ? Motivations: FRBs are probably explosive events associated to particle acceleration processes. If some baryons are accelerated → productions of HE CR, γ -rays and HEN. ➡ No hadronic/neutrino model dedicated to FRB in the market ➡ However, we can derive neutrino spectrum using the main models of short GRBs, NSs… (2) (1) Short GRB Highly magnetised young NS || Slow rotating magnetar Dey et al.16,17 Zhang et al.03 P 1 = 100ms P 2 = 5 s B = 1.5x10 15 G, R = 10 km FRB @ the coalescence time Δ t ~500s GHz FRB (giant flare) GHz Baret et al. 11+ UV/x-rays + TeV-PeV p → HEN γ + p → HEN (10 TeV-100 PeV) ([1] 100 TeV-1 PeV, [2] 100 GeV-10 TeV) M. Sanguineti - ICRC 2017 @ Busan - 14/07/17 8
9 FRB analysed by ANTARES ANTARES neutrino telescope: 12 lignes (885 PMTs) takes continuously data since 2008 Between 2013-2017, 12 FRBs detected among them 9 visible as upgoing by ANTARES at the time of the burst ➡ Search for muon neutrino tracks in the online data FRB catalog : http://www.astronomy.swin.edu.au/pulsar/frbcat/ M. Sanguineti - ICRC 2017 @ Busan - 14/07/17 9
Searching method Searching method adapted from an on-line search (cf poster #984) Check the ANTARES visibility at the ANTARES online data → online data at the FRB date FRB trigger time + stability of the → event track recostruction data taking conditions Event selection criteria FRB150215 → tcos θ >0 : upgoing track events → Λ cut , β (reconstruction quality criterion) optimised to have 1 event for a 3 σ discovery in the time window T2 Search for HEN in time and space correlation with a FRB → ROI = 2 o around the FRB position (3 σ ANTARES PSF, error pos. FRB negligible) → 2 different time windows : T1 = [T FRB -500s; T FRB +500s], short transient T2 = [T FRB -6h; T FRB +6h], moderate delay between the radio and the neutrino emission Results → No neutrino in space/time correlation with the 9 FRBs → Expected background: μ B ∼ 5 · 10 − 8 event/s, compatible with bkg fluctations → Set upper-limits on the neutrino fluence M. Sanguineti - ICRC 2017 @ Busan - 14/07/17 10
Upper-limits In absence of signal, set upper-limits at 90% C.L. on the neutrino fluence F ν ,90% and in the isotropic total energy radiated in neutrinos in the rest frame E iso . { Ω m = 0.308, Ω Λ = 0.692, H 0 = 67.80 km s − 1 Mpc − 1 Preliminary erg.cm − 2 (GeV.cm − 2 ) log 10 [GeV] erg.cm − 2 (GeV.cm − 2 ) log 10 [GeV] M. Sanguineti - ICRC 2017 @ Busan - 14/07/17 11
Upper-limits As the distance of each FRB is poorly constrained, we test different kind of scenarios : a galactic origin (D ∈ [1 - 50] kpc), an extragalactic origin (D ∈ [0.05 - 100] Mpc) and a cosmological origin (z ∈ [0.02 - zDM]) If FRBs = neutrino emitters, ANTARES puts interesting constraints on the origin. ➡ D ︎ < 50 Mpc, E iso ︎ < 10 52 erg (E − 2 source model). ➡ Poor constraint for the cosmological origin. M. Sanguineti - ICRC 2017 @ Busan - 14/07/17 12
Conclusion ANTARES has reported the search for HE neutrino from a population of FRB detected these last four years (9 bursts) ➡ No neutrino in spatial/temporal correlation in a time window extended up to six hours before and after the radio bursts. ➡ Limits are of the order of F ν ,90% = ︎ 10 − 1 − 10 − 2 erg cm − 2 for a E − 1 and E − 2 source model. ➡ Galactic and very close extragalactic scenarios (D<1-10 Mpc) start to be interestingly restricted below E iso ∼ 10 45-52 erg. However, very poor constrains on the cosmological scenario (E iso ~ 10 54-55 erg for z ∼ 0.1) ➡ + 2 papers with SUPERB accepted or in submission: - A Polarized fast radio burst at low Galactic latitude, MNRAS (2017) 469(4): 4465-4482 - The Survey for Pulsars and Extragalactic Radio Bursts II: fourth FRB discoveries and their follow-up, MNRAS (2017) M. Sanguineti - ICRC 2017 @ Busan - 14/07/17 13
In the KM3NeT Fr site, few months ago…
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