multi-messenger analyses with the antares high energy...

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Multi-messenger analyses with the ANTARES high energy neutrino telescope

Aurore Mathieuon behalf of the ANTARES collaboration

Frontiers of Fundamental PhysicsMarseille, July 15-18, 2014

Aurore Mathieu FFP – Marseille, July 15-18, 2014 1

The ANTARES telescope12 lines25 storeys/line3 PMs/storey

~ 70 m

14.5 m

40 km of cable

Depth: 2500 m

Shore station


The ANTARES telescopePerformances : ➔ 12-lines data taking since 2008➔ ~ 7000 neutrinos➔ Angular resolution: 0.3 – 0.4°➔ Effective area: ~ 1m² (30 TeV)➔ Visibility: ¾ of the sky, majority of

the galactic plane➔ Real-time data processing


Motivation● Link between CR / γ / ν:

- CRs and UHECRs origin?- Hadronic , leptonic or lepto-hadronic models?- Jet composition? ...

Cosmic neutrinos:➔ Neutrinos possibly produced in the interaction of high energy

nucleons with matter or radiation➔ If hadronic mechanisms:

High energy nucleons + hadrons mesons + hadrons neutrinos and photons➔ Simultaneous emitters of neutrinos and photons➔ Detection from a cosmic source would be a direct evidence of

hadronic scenario


Transient analysesANTARES can perform a wide range of analyses:

● Point Source analyses: discovering of astrophysical neutrino sources (all sky search or candidates list)

● Multi-messenger study: coincident (space+time) neutrino and photon signal ⇾ improved performance with respect to not using time info at all

Coincidence of γ and neutrino emission: different transient sources can be analyzed

1) μ-quasars: galactic variable sources (hours ↔ months)

2) Blazars: extra-galactic variable sources (hours ↔ months)

3) GRBs: most energetic known events(sec ↔ days)


Microquasar analysisSix μ-quasars with X-ray or γ-ray outbursts in the 2007–2010 satellite data:Circinus X-1 IGRJ17091-3624 GX339-4 Cygnus X-1 H 1743-322 Cygnus X-3

● ANTARES data period 2007–2010 (813 live time days)● Multi-messenger info provided by SWIFT, ROSSI and FERMI

X-ray light curves sample of GX 339-4 between 2007 and 2010, from top to bottom: SWIFT and Rossi X-ray LCs and hardness ratio


Microquasar results

No neutrino found in time coincidence with microquasar emissions

=> Upper limits on the neutrino flux (F.C. @90% C.L.)

Upper limits (F.C.@90%) on a neutrino flux φ ∝ E−2 e −√(E/100TeV) (circles) compared with the expectations of Distefano et al. (2002) in the ηp = ηe case (triangles). For IGRJ17091-3624 no measurement has been found to estimate the neutrino flux.


Blazar analysis➔ Previous ANTARES AGN analysis with 2008 data:

Astropart. Phys., Vol. 36, 204 [arXiv:1111.3473]➔ Updated analysis: 2008-2012 data, FERMI + HESS/VERITAS/MAGIC + X-ray➔ Flares in two energy ranges: γ-rays (FERMI) and HE-VHE γ-rays (IACT)

FERMI: ● Catalogue base:

2FGL(+Fermiblog+TANAMI) → 1873(+43+13) sources

● Reduced to 97(+43+13) pre-selected sources (cuts on catalogue parameters)

● Significant flares found on 41 flaring sources: 3C 454.3, 3C 279, 4C +21.35, PKS 1510-08, ...


Blazar analysis➔ Previous ANTARES AGN analysis with 2008 data:

Astropart. Phys., Vol. 36, 204 [arXiv:1111.3473]➔ Updated analysis: 2008-2012 data, FERMI + HESS/VERITAS/MAGIC + X-ray➔ Flares in two energy ranges: γ-rays (FERMI) and HE-VHE γ-rays (IACT)

IACT: ● 7 flaring sources selected from

publications on HESS, MAGIC and VERITAS: 4C +21.35, PG 1553+113, PKS 1424+240, 1ES 1218+30.4, 1ES 0229+200, HESS J1943+213 and PKS 0447-439


Blazar results➔ Only 3 sources show a neutrino event in time and space coincidence with the flare:

3C 279, PKS 1124-186 and PKS 0235-618➔ Most significant source: 3C 279 for E¯² with p-value 1.9% (54% post-trial)➔ Background fluctuation compatible➔ Paper in preparation

LEFT: Neutrino events around 3C 279. The circles are the estimated angular error from the reconstruction.RIGHT: γ-Ray light curve for 3C 279 with the selected neutrino events within 3° around the source. [events during and out of the flare]

Optical counterpart search

Follow-up of high energy ν


TAToO● Optical/X-ray follow-up of individual ν direction in real-time● No hypothesis on the nature of the source

Triggers● Directional:

1 neutrino in the direction (< 0.4°) of a local galaxy (< 20 Mpc)12 per year

● High energy: 1 neutrino with E > 5-10 TeV12 per year

● Doublet: Two neutrinos in a 3° angle and in a time window of 15 minutes0.04 per year


TAToO


Trigger Angular resolution

Fraction events in fov

Mean energy

HE 0.25-0.3° 96% (GRB)68% (SN) ~ 7 TeV

Directional 0.3-0.4° 90% (GRB)50% (SN) ~ 1 TeV

● Online processing: - Online reconstruction + trigger: ~ 3-5 s- Alert sending: ~ 1-10 s depending on the telescope response- Telescope slewing: ~ 1-5 s

Minimum delay between the neutrino and the first image: ~ 20 s

● Angular performances:

Optical follow-up strategy


Telescopes


TAROT

ROTSE

ZADKO

Telescopes


TAROT

ROTSE

ZADKO

TAROT Calern

● Two 25 cm telescopes

● Fov 1.86°x1.86°

● Slewing time ~ 10s

Telescopes


TAROT

ROTSE

ZADKO

ROTSE 3a● Four 45 cm telescopes

● Fov 1.85°x1.85°

● Slewing time ~ 10s

Telescopes


TAROT

ROTSE

ZADKO

Zadko

● One-metre telescope

● Fov 23 x 23 arcmin

● Max. Slew speed 3°/s

Telescopes


TAROT

ROTSE

ZADKO

SWIFT● X-ray follow-up

● Fov 23.6 x 23.6 arcmin

● 0.3-10 keV energy range

Alerts


Since 2009: ● 108 alerts sent:

- 11 not followed (telescope maintenance, too close to the Sun...)- 97 followed by at least 1 telescope and at least 1 night- 90 followed by at least 1 telescope and at least 3 nights



● Analysis based on the image subtraction:

● Development of a new pipeline for image analysis



Hypothesis: neutrino emission simultaneously with photons→ No transient optical counterpart associated with a neutrino detection→ Upper limits on transient sources magnitude

Alert Delay since trigger

U.L. MagS/N=5

ANT100123A 15h20m15s 12

ANT100302A 24h20m8s 15.7

ANT100725A 0h01m15s 14.5

ANT100922A 1h08m06s 14.0

ANT101211A 12h03m30s 15.1

ANT110409A 0h04m17s 18.1

ANT110529A 0h07m33s 15.6

ANT110613A 0h01m08s 17.0

ANT120730A 0h00m21s 17.6

ANT120907A 0h00m25s 16.9

ANT121010A 0h00m24s 18.6

ANT121206A 0h00m27s 16.9Based on only detected light curves [kann2010]


X-ray follow-up with SWIFT

Follow-up with SWIFT


X-ray follow-up: complementary informations to optical signals→ The X-ray sky is rich in variable and transient sources→ Fast response: increase sensitivity to fast transient sources (GRBs)

Strategy:MoU 6 with alerts/yrOnly HE triggers with higher energy selection2x2 tiles with 2ks exposure each

⇒ Sensitivity: 2.10-13 erg.cm-2.s-1

⇒ 4 tiles cover 48 arcmin fov~60-70 % of the PSF

Observation strategy: 1) Automatic response to ToO (priority 1) → online analysis 2) Follow-up only if an interesting candidate is found (priority 2)

Image processing: Phil Evans (Leicester University)



⇒ 5 alerts sent to the XRT since June 2013After a delay of: 23s / 25s / 18s / 18s / 24sProcessing after: 1h08 / 6h24 / 5h06 / 6h43 / 5h36

⇒ No X-ray counterpart associated to a neutrino detection

In case of GRB: compare with the afterglow

lightcurves detected by Swift/XRT

TAToO limitsTAToO limits

XRT LC 2008-2013 (503 GRBs)

PRELIMINARY

Conclusions


➔ Transient and multi-messenger analyses are performed, on-line and off-line

➔ First results on μ-quasar analysis with ANTARES (2007-2010)

➔ The μ-quasar analysis is being updated with new data and new sources

➔ Second AGN analysis updates up to 2008-2012 dataPrevious analysis (2008) (Astropart. Phys. 36 (2012) 204)

➔ Images from TAToO follow-up are currently analyzed to search for long transient (core collapse SN)

➔ More multi-messenger analysis:Gravitational waves (VIRGO/LIGO): GWHEN


Backup

Detection principle

Aurore Mathieu FFP – Marseille, July 15-18, 2014 B1

Looking for up-going events

Atmospheric muons ~10 per secondAtmospheric neutrinos few per dayCosmic neutrinos few per year ?

Background suppression: Atm. Muons: quite easy to remove (zenith + quality cuts)Atm. Neutrinos: irreducible isotropic background, low energy

Microquasar analysis


Selection of sources:The selection of the candidate microquasars is based on both the presence of X-ray outbursts and the possibility to relate them to the radio counterpart.➔ ~ 20 known microquasars in our Galaxy➔ 17 microquasars visible by ANTARES and monitored by ASM and BAT

➔ Baseline of each LC is calculated by means of a gaussian fit of the rate distributions➔ The outburst selection then proceeds by looking for a first rate measure for which rate-3σrate >

baseline+3σbaseline, and successive measures for which rate-σrate > baseline+3σbaseline

➔ To avoid a single high flux measure to trigger an outburst, at least two consecutive measures (i.e. at least two days) are required to select the time window

➔ All sources that do not show any bursting activity are discarded➔ 2 sources are discarded because the ASM and BAT LCs are not sufficient to relate the X-ray

activity to the jet acceleration➔ Sources selected with X-rays: Cir X-1 (NSB), GX 339-4, H1743-322, IGR J17091-3624, Cyg X-1➔ Source selected with γ-rays: Cyg X-3

Microquasar analysis


Analysis of the 6 μ-quasars : - For 4 black hole binaries, ν search split in two cases:

- Hard X-ray states (HS): “slow” steady jet- Transition hard ↔ soft (TS): “fast” discrete ejection

Relativistic jets → ν emission- Cyg X-3: γ-ray outburst using Fermi/LAT data- Cir X-1: X-rays + orbital phase/jet connection

Blazar analysis


FERMI dataCuts on catalogue parameters:

Blazars | DS > 25 σ | VI > 41.64 | δ > 35° |

Fermi analysis: LCs extracted from FERMI photon counting data: Maximum Likelihood Block denoising treatment with a fluence threshold

Φmin1−100 GeV

>10−9 photons.cm−2 . s−1

LEFT: 3C 273 CMAP from FERMI data. RIGHT: Corresponding LC with a MLB characterization. The selected flaring periods are done by a fluence threshold.

Variability_Index: a value greater than 41.64 indicates there is a less than 1% chance of being a steady source.

Blazar analysis


IACT dataLCs extracted from publications: flat emission assumed during the reported flaring periods.

● Analysis with 2008–2012 data: from September 6th to December 31st, 2012 (1044 days of live time)● Unbinned time-dependant search method with a likelihood ratio● Implementation of a possible lag (±5 days) in ν/γ signal in the likelihood for avoid

missing short flares● Inclusion of a new energy estimator with a more physical justification, declination

dependence considered● Various energy spectra taken in consideration:

E−2 , E−2 with cutoffs at 1 TeV and 10 TeV, E−1

● Re-optimization of preliminary general cuts:cos(θ) > −0.15 && β < 1° [Discovery Flux at 3σ]

● Individual Λ quality cut optimization[Model Discovery Potential at 3σ]

Image analysis


Co-addition: SWarp : resampling and co-adding images

Subtraction:Reference selectionPixel by pixel

Astrometry / photometry: SExtractor : catalogue of extracted sourcesSCAMP : astrometric calibrationLe PHARE : photometric calibration

Image correction: Bias, dark subtractionFlat-fieldingFringe correction

Residuals inspection:Visual scanComparison with cataloguesLight curve scan

Telescope site{{{{{

Telescopes response


HE trigger SWIFT




Alert 2014/01/24:

If an uncatalogued source is found, 2 questions are asked to identify the afterglow:1) Is the source “bright”?2) Is the source fading?

No counterpart

GWHEN


Search for coincident gravitational waves and high energy neutrinos using ANTARES, LIGO and Virgo

Scientific motivations:- Sources invisible in photons:

“failed” GRBs = hidden sources (optically thick media: no or weak γ-ray emission)- Coincident detection (time+space): validation of GW and HEN detections- Unique information on internal processes: accretion, ejection...

GW emission: collapse of binary mergers HEN emission: acceleration of protons, followed by pp and pγ interactions → neutrinos

GWHEN: method


GWHEN


Analysis of 2007 data: completed→ no GW in coincidence with a neutrino signal

Analysis of 2009-2010 data: on-going

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