Search for neutrinos from Fast Radio Bursts with the ANTARES - - PowerPoint PPT Presentation
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
ICRC 2017 @ Busan - 17/07/17
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Short transient : 1-10 ms and Very bright : 1-10 Jy ms (<S/N> = 22) → The brightest FRB 150807 reached Smax = 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 “Lorimer“ burst : FRB 010724 FRB150418 (@Parkes)
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Arecibo GBT Parkes UTMOST ASKAP UTMOST Parkes Arecibo Green bank
! High galactic latitude ! Expected rate :
~103 FRB/day/all sky
ASKAP
FRB 121102 FRB catalog : http://www.astronomy.swin.edu.au/pulsar/frbcat/
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Same story as GRB before the detection of the 1st optical afterglow ~20 yrs ago How to measure the distance?
=> z ≤ 1200 / DMIGM (Ioka 2003, Inoue 2004)
=> DMexcess~100-1200 cm-3 pc => zDM~0.2-1.4 => Evidence for cosmologic dist [DMmax (PSR J0131-7310) = 205 cm-3 pc]
=> Only case is FRB121102 (repeating): star forming dwarf galaxy at z=0.19
=> 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
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Milky Way 100-200 Mpc
FRB emission mechanism : Supergiant flares in the magnetosphere
rotating neutron stars embedded in a dense environment → Crab-like flares Repeating : Yes Distance : 100-200 Mpc DMexcess (100-1000 cm-3 pc) : Local environment around the NS + extragalactic IGM constant flare by flare ?
Young and rapidly rotating neutron stars
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Milky Way 1-20 Gpc z ~ 0.1 - 2 DMexcess = IGM
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. Magnetar: Giant flares in the magnetosphere of a magnetar (possibly associated to SGR). Repeating : No/No/Yes Distance : ~1-20 Gpc DMexcess (100-1000 cm-3 pc) : Local environment around the compact
constant flare by flare (magnetar)
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What are the radiative processes ? Where are they located ? Their distances ? Particle acceleration mechanisms ? Baryons ? Leptons ? γ-rays ? Need for a MW analysis → SED → photometric redshift Need for an unambiguous host identification Need for a spectroscopic obs. → redshift Need for MWL and MM
→ high-energy neutrinos = baryonic acceleration → radio + GeV obs. = distinguish between leptonic and hadronic scenarios
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Motivations: FRBs are probably explosive events associated to particle acceleration processes. If some baryons are accelerated → productions
➡ No hadronic/neutrino model dedicated to FRB in the market ➡ However, we can derive neutrino spectrum using the main models of
short GRBs, NSs…
FRB @ the coalescence time GHz γ + p → HEN Δt ~500s Baret et al. 11+ Short GRB Highly magnetised young NS Slow rotating magnetar (1) (2) || B = 1.5x1015 G, R = 10 km P1 = 100ms P2 = 5 s Dey et al.16,17 Zhang et al.03 FRB (giant flare) GHz UV/x-rays + TeV-PeV p → HEN
(10 TeV-100 PeV) ([1] 100 TeV-1 PeV, [2] 100 GeV-10 TeV)
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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/
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Check the ANTARES visibility at the FRB trigger time + stability of the data taking conditions ANTARES online data → online data at the FRB date → event track recostruction Event selection criteria → tcosθ >0 : upgoing track events → Λcut, β (reconstruction quality criterion) optimised to have 1 event for a 3σ discovery in the time window T2 Search for HEN in time and space correlation with a FRB → ROI = 2o around the FRB position (3σ ANTARES PSF, error pos. FRB negligible) → 2 different time windows : T1 = [TFRB-500s; TFRB+500s], short transient T2 = [TFRB-6h; TFRB+6h], moderate delay between the radio and the neutrino emission
Searching method adapted from an on-line search (cf poster #984)
Results → No neutrino in space/time correlation with the 9 FRBs → Expected background: μB ∼ 5 · 10−8 event/s, compatible with bkg fluctations → Set upper-limits on the neutrino fluence
FRB150215
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In absence of signal, set upper-limits at 90% C.L. on the neutrino fluence Fν,90% and in the isotropic total energy radiated in neutrinos in the rest frame Eiso.
Ωm = 0.308, ΩΛ = 0.692, H0 = 67.80 km s−1 Mpc−1
Preliminary
erg.cm−2 (GeV.cm−2 ) log10[GeV] erg.cm−2 (GeV.cm−2 ) log10[GeV]
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As the distance of each FRB is poorly constrained, we test different kind
(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, Eiso ︎ < 1052 erg
(E−2 source model).
➡ Poor constraint for the
cosmological origin.
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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 Fν ,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 Eiso ∼ 1045-52 erg. However, very poor constrains on the cosmological scenario (Eiso ~ 1054-55 erg for z∼ 0.1)
➡ + 2 papers with SUPERB accepted or in submission:
(2017) 469(4): 4465-4482
FRB discoveries and their follow-up, MNRAS (2017)
In the KM3NeT Fr site, few months ago…