Transcript ANTARES/IceCube Multi-Messenger projects

ANTARES/IceCube
Multi-Messenger projects
Jürgen Brunner
CPPM
Image credit: Heidi Sagerud (IRAP,Toulouse)
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Multi-messenger programs
online and offline
GeV-TeVγ-rays
Fermi / HESS…
UHECR
Auger
HE neutrinos
Optic / X-ray
TAROT,MASTER,
ROTSE / Swift,
ZADKO
Markus Ahlers
Gravitational
Waves
Virgo / Ligo
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Multi-messenger programs
Time-dependent searches:
- GRB [Swift, Fermi, IPN]
- Micro-quasar and X-ray binaries [Fermi/LAT, Swift, RXTE]
- Flares of blazars [Fermi/LAT, IACT, TANAMI…]
- Flares of the Crab [Fermi/LAT]
- Supernovae Ib,c [Optical telescopes]
Multi-messenger correlation:
- Correlation with the UHE events [Auger]
- Correlation with the gravitational wave [Virgo/Ligo]
- 2pt-correlation with 2FGL catalogue, loc. galaxies, BH…
Real-time analysis:
- Follow-up of the neutrino alerts with optical telescopes
[TAROT, ZADKO, MASTER, PTF] and X-ray telescope [Swift/XRT]
and Gamma ray telescope [HESS, VERITAS, MAGIC]
- Online search of fast transient sources [GCN]
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Gravitational Waves & Neutrinos
Bruny Baret
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Sensitivities
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Auger & Telescope Array
• Event samples
– Auger : 231 events E > 52 EeV 2004-2014
– ANTARES (2007-2008) : 69 Auger event (2004-2009)
– TA :
87 events E > 57 EeV 2008-2014
• Magnetic deflection < 30
Mohamed Rameez
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Cosmic Ray Correlation
arXiv:1405.5303
x: Tracks
+: Cascades
arXiv:1507.04005
• 7 HESE Muons & 9 HE
upgoing muons above
100 TeV
• 39 Cascades
• Several correlation
studies
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Cosmic Ray Correlation
Compute the number of UHECR-neutrino pairs as a function of
the angular separation in the data and compare it with
expectations from an isotropic distribution of UHECRs
• Cascades
• Incompatible with
3.3σ post-trial with
isotropic distribution
of Cosmic rays
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Real Time Alert Sending
Follow-up of the neutrino alerts
with optical telescopes
[TAROT, ZADKO, MASTER, PTF]
X-ray telescope
[Swift/XRT]
Gamma-Ray telescope
[HESS, VERITAS, MAGIC]
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IceCube Followup scheme
FoV 2.3x3.50
Rmag < 21, 1.2m mirror
No prompt observations
Thomas Kintscher
Main trigger:
- doublet: 100sec & 3.50
- PTF (9/yr) & Swift (7/yr)
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Antares Followup scheme
ANTARES Shore Station:
Trigger decision
On-line reconstruction
Alert message (GCN
format)
4 types of triggers:
- doublet (0.04/yr)
- single HE (12/yr)
- single VHE (6/yr)
- single + loc galaxy
directions (12/yr)
ANTARES
Neutrino Telescope
ν
Aurore Mathieu
Optical 0telescopes
FoV 1.9x1.9
Rmag < 18, 0.2m mirror
prompt observations
Astroparticle Physics 35 (2012) 530-536, arXiv:1103.4477
Optical images
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Alerts for Optical Followup
Online processing:
- Triggering & online reconstruction: ~3-5 s
- Alert transmission: ~1-10 s depending on the telescope response
- Telescope slewing: ~1-5 s
Minimum delay between the 1st image and the neutrino: ~20 s
Angular performances:
PSF trigger HE
1.9°
1.9°
Trigger
Angular Fraction events
Muon
resolution
in fov
contamination
Mean
energy
HE
0.25-0.3°
96% (GRB)
68% (SN)
<0.1%
~7 TeV
Directional
0.3-0.4°
90% (GRB)
50% (SN)
~2%
~1 TeV
Average rate : 2 alerts per month
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Followup Optical Telescopes
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X-Ray Followup with Swift - ANTARES
 6 alerts per year
 sub-sample of High Energy event
Average Neutrino energy 50 TeV
 PSF : ~20 arcmin
Delay of observation ~6h
 Image: 2 x 2 tiles of 2ks exposure each
 Sensitivity: 2 10-13 erg/cm2/s
 4 tiles cover 48 arcmin fov
Further observation if variable object
above ROSAT catalogue limit is found
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X-Ray Followup with Swift - IceCube
7 tiles instead of four due to slightly worse angular
resolution of doublets
1.20
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Alert summary
Antares since 2009
165 to optical telescopes
10 to Swift
IceCube 2010 - 2014
31 to PTF
21 to Swift
High Energy Alerts
Directional alerts
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ANTARES: GRB search results
~1m
~1h
Several
hours
→ Comparison with optical
afterglow light curves
~10m
~20s
Grey:
158 optical afterglow
lightcurves detected
from 1997 to 2014
(Kann).
~70%
~95%
~35%
PRELIMINARY
~3%
Fast followup:
GRB excluded
Slow followup:
no constraint
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ANTARES: GRB search in X-Ray
→ 10 alerts sent to
Swift
Time to send the alert: ~20 s
Time to process the alert by XRT: few hours
XRT LC 2007-2015
→ No X-ray
counterpart
associated to our
neutrino alerts
→ Upper limits on
transient sources
magnitude
TAToO limits
PRELIMINARY
1h
15h
75%
40%
689 X-ray afterglow light curves detected by Swift/XRT from
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2007 to 2015
Gamma Ray Followup IceCube
• Started operation in March 2012
• Accept neutrinos close to predefined list of know
sources
• 21 sources in Northern sky selected (AGNs)
• Alert rate: MAGIC : 1 / year, VERITAS : 3 / years
• 13 alerts have been sent to MAGIC or VERITAS so
far no Gamma counterpart found
• Situation ANTARES : MoU with HESS signed
• Up to 3 alerts per year accepted
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Gamma Ray Followup IceCube
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•
•
•
Most significant alert: 2012/11/09
6 neutrinos in 4 days around source
-log10(pretrial p-value) = 4.6
VERITAS : no significant gamma ray emission
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Gamma Ray Followup IceCube
arXiv:1405.5303
x: Tracks
+: Cascades
arXiv:1507.04005
• 3 Northern sky HESE
Muons & 20 HE
upgoing muons
• Checked with VERITAS
• 40 hours observation
• No significant
detection of VHE
Gamma rays
• But : many months
after neutrino time
•  go to real time
Jon Dumm
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Concept : Combine several sub-threshold (multi-messenger)
observations into significant signal
Doug Cowen 24
AMON : Status of Participation
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IceCube SuperNova Detection
Chance probability 1.4% == 2.6σ
SN age : 169 days, Neutrino predictions ~10-3
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Recent Alert
• 01/09/2015 07:38
• High Energy event
• Energy estimate:
– 50-100 TeV
• Sent to Swift &
Master
• Observation after
9h Swift XRT, 10h
MASTER
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Follow-up Swift XRT
• Non catalogued X-Ray source found above ROSAT
limit  ATel #7987 , GCN #18231
• X-Ray source coincides with star
– USNO-B1 : 0626-0501169 (Rmag = 12.6)
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Follow-up Swift XRT
ATel & GCN
First observation
10h later
Neutrino Alert
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ANTARES
M4
Optical Followup MASTER (x+11h)
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Multi Wavelength Observations
• 11 ATels & 5 GCN circulars within few days
• Optical
– MASTER, Pan-STARRS
• Infrared/Optic (spectral analysis)
– NOT, SALT, WiFES, CAHA, Kepler 2, CAHA, LSGT, NishiHarina NIR, VLT/X-Shooter
• X-Ray
– GBM, MAXI, Integral
• Radio
– Jansky VLA
• Gamma Ray
– Contact with Fermi-LAT, HESS, HAWK
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Conclusion
 Multi-Messenger Analyses become more and
more important both or IceCube & ANTARES
 Various Results Combining Neutrino Results
with Optical, X-ray, Gamma-Rays, Gravitaitonal
Waves adnd UHE Cosmic Rays
Real Time Alert Systems operational with optical
telescopes, X-Ray satellies and Gamma rays
telescopes
Eagerly awaiting first significant coincidences
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Backup
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Multi-messenger correlation
- Correlation with the UHE events [Auger]
- Correlation with the gravitational wave [Virgo/Ligo]
- 2pt-correlation with 2FGL catalogue, loc. galaxies, BH…]
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Correlation with Auger UHE events
Analysis performed with
2007-08 data:
- Antares: 2190 events
- Auger: 69 events
 Optimum search in a cone of 4.9º around each Auger sources
 No correlation observed (deficit at 1.4 sigma)
 Upper-Limit: 5.010-8 GeV.cm-2.s-1
S. Adrián-Martínez et al. ApJ 774 (2013) 19
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2-pt correlation [2007-10]
N
2-pt correlation function:
n


N p     wi  w j  H ij  
i1 j 1
ANTARES: nHit weights

2FGL: gamma-ray flux (1-100GeV)
1873 sources
Post-trial p-value 68% for angles < 0.6°
ANTARES: nHit weights
GWGC: D-2 weighting
~53000 loc. gal.
Post-trial p-value 96% for angles < 0.3°
F. Schüssler, ICRC2013
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Correlation with Virgo/Ligo GW
1st search 2007 data:
S. Adrian-Martinez et al., JCAP 06 (2013) 008
2nd search 2009-10 data:
- Optimized event selections on
both side
- Improved likelihood analysis
T. Pradier, ICRC2013
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Time dependent searches
- GRB [Swift, Fermi, IPN]
- Micro-quasar and X-ray binaries [Fermi/LAT, Swift, RXTE]
- Flares of blazars [Fermi/LAT, IACT, TANAMI…]
- Flares of the Crab [Fermi/LAT]
- Supernovae Ib,c [Optical telescopes]
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Search for v from GRB
o Analysis of GRBs from late 2007 – 2011: 296 long GRBs,
Total prompt emission: 6.6 hours
Information from FERMI/SWIFT/GCN
PRELIMINARY
o GRB simulations of expected neutrino
fluence:NeuCosmA [Hümmer et al. (2010)]
and Guetta [Guetta et al. (2004)]
o Likelihood analysis & quality cut
optimized for NeuCosmA & highest
signal discovery probability
Grey: first ANTARES limit (40 GRBs, 2007)
 JCAP 03(2013) 006
o No events found within 10° window from GRB
Black: IceCube IC40+59 (215 GRBs)
Expected: 0.48 (Guetta), 0.061(NeuCosmA)
o Dedicated analysis for very peculiar: GRB080916C, GRB110918A, GRB130427
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Search
for
v
from
microquasars
Six micro-quasars with X-ray or γ-ray outbursts in the 2007-2010 satellite data:
Circinus X-1, GX339-4, H 1743-322, IGRJ17091-3624, Cygnus X-1, Cygnus X-3
Analysis of the 6 micro-quasars:

For 4 black hole binaries ν-search split in two:




During hard X-ray states : “slow” steady jet
During transition hard→soft : “fast” discrete ejection
Cyg X-3 : γ-ray outburst using Fermi/LAT data
Cir X-1 : X-rays + orbital phase/jet connection
GX339
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Search for v from microquasars
No neutrino found in time coincidence with microquasars
=> Upper-limit on the neutrino flux (F.C. 90%)
Model: Levinson, Waxman (2001),
Distefano (2002) assuming a flux
  E 2e
E 100TeV
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Search for v from AGN flares
3C279
Analysis of Fermi data:
- Counting map + lighcurve (2deg)
- Denoising LC (Maximum Likelihood Block method)
- Selection of significant flares
4C +21.35 (MAGIC)
First analysis: selection of 10 Fermi flaring blazars [2008]:
=> Astropart. Phys. 36 (2012) 204
Updated analyis: selection of Fermi flaring blazars [2008-2012] flaring TeV
blazars (HESS/MAGIC/VERITAS)
=> D. Dornic, A. Sanchez-Losa ICRC2013 - Paper in preparation
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Search for v from AGN flares
Unbinned searches performed [2008-2012]:
 For 42 Fermi sources: no significant cluster
 For the 8 TeV flares: no significant correlation
For 3C279: 2 events compatible with the
source direction and time distribution. Post
trial value 10%
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Background suppression
Atmospheric muons
Atmospheric neutrinos
Cosmic neutrinos
~10 per second
few per day
few per year (may be)
 Atm muons: quite easy to remove (zenith +quality cuts)
 Atm neutrinos: irreducible isotropic background, low energy
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Neutrino search method
Neutrino source: quite high energy and sharp
directional distribution, possible specific time
distribution
=> Search of clusters in space with a high
energy content (adding the information of energy
allows to gain ~25% discovery potential)
2 types of point-source analysis:
- All sky search: significant cluster
=> 8-10 ν per source @ 5σ discov
- Candidate list: 50 most promising sources
=> 5-6 ν per source @ 5σ discov
S. Adrian-Martinez et al., Astrophysical J. 760:53(2012)
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Point-source sensitivities
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Neutrino search method
2 types of point-source analysis:
- All sky search: significant cluster => 8-10 neutrinos per source
- Candidate list: 50 most promising sources => 5-6 neutrinos per source
Adding the time information:
=> 2-3 ν per source @ 5σ discov
=> Increase sensitivity by a factor 2-3
=> For a very short transient (GRB),
only 1 ν per source is sufficient !!!
Analysis for micro-quasars, flares of
AGN, supernovae, magnetar, GRB…
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