Alexis Coleiro APC - Université Paris Diderot Second ASTROGAM

SYNERGIES BETWEEN
NEUTRINO DETECTORS AND ASTROGAM
Alexis Coleiro
APC - Université Paris Diderot
!
Second ASTROGAM workshop - Paris, March 27 2015
WHY NEUTRINOS ?
p
ɣ
𝝼
•
•
•
Photons are absorbed by the ISM
Protons are deviated by magnetic fields
Neutrinos are neutral, stable and weakly interacting particles
Signature of hadronic acceleration : sites of cosmic rays production
BASIC INGREDIENTS
BASIC INGREDIENTS
Leptonic processes ?
!
Inverse Compton
Synchrotron
Hadronic processes ?
p + ɣ ➝ π0 + p
ɣɣ
p + ɣ ➝ π+ + n
μ νμ
νμ νe e
CANDIDATE SOURCES OF HIGH
ENERGY NEUTRINOS
- Sites of particle acceleration
SNR
PWN
X-ray,
γ-ray and
colliding wind binaries
CANDIDATE SOURCES OF HIGH
ENERGY NEUTRINOS
- Sites of particle acceleration
Galactic center
AGN
Star-forming galaxies
GRB
CANDIDATE SOURCES OF HIGH
ENERGY NEUTRINOS
- Sites of particle acceleration
Galactic center
AGN
Star-forming galaxies
Sources that will be studied by ASTROGAM
GRB
CURRENT DETECTORS
Baikal
ANTARES
IceCube
CURRENT DETECTORS
ANTARES
IceCube
Baikal
RECENT RESULTS
IceCube collaboration
Science, 342 (2013)
IceCube collaboration
PRL, 113 (2014)
-
28 neutrino events between May 2010 and May 2012 over 30 TeV (37 now)
More than expected from atmospheric backgrounds
Reject a purely atmospheric origin at the 4σ level (5.7σ now)
RECENT RESULTS
Constraint on a Galactic center neutrino emission with ANTARES
ANTARES collaboration, ApJ, 786 (2014)
-
6 years of ANTARES data
90% CL upper limit on the muon neutrino flux normalization
between 3.5 and 5.1 x 10-8 GeV cm-2 s-1
A point source is
excluded by ANTARES
RECENT RESULTS
Constraint on a neutrino emission from the Fermi bubbles with ANTARES
(more data to come: ~65% increase in sensitivity expected with 2012-2016 data)
no cutoff
500 TeV cutoff
100 TeV cutoff
50 TeV cutoff
ANTARES collaboration
EPJC, C74 (2014)
MULTI-MESSENGER STUDIES
Time integrated analysis
clustering
E2 φν90CL [GeV cm-2 s -1]
IceCube collaboration
ApJ 796 (2014)
The Astrophysical Journal Letters, 786:L5 (5pp), 2014 May 1
correlation with Fermi
ANTARES collaboration, ApJ, 786 (2014)
10-6
ANTARES sensitivity (1338 days)
ANTARES (1338 days)
ANTARES full-sky limit - 1° bands (1338 days)
ANTARES Eν <100 TeV sensitivity
IceCube 3 years
IceCube 3 years sensitivity
IceCube 3 years Eν < 100 TeV sensitivity
10-7
10-8
10-9
-1
ANTARES collaboration
JCAP 05 (2014)
-0.8
-0.6
-0.4
-0.2
0
0.2
0.4
0.6
0.8
1
sin(δ)
MULTI-MESSENGER STUDIES
Time-dependent analysis (for transient sources)
for instance: microquasar analysis
ANTARES collaboration
JHEAp 3 (2014)
MULTI-MESSENGER STUDIES
Time-dependent analysis
+
GRB, AGN, etc. (IceCube and ANTARES) with the
same approach:
•
information on the emission time obtained from observation of
electromagnetic radiation
•
selecting a time window around the neutrino emission period
(reduce the background)
!
MULTI-MESSENGER STUDIES
Follow-up of neutrino events
two examples
TAToO: optical follow-up
HESS: gamma-ray follow-up
F. Schüssler et al..
ICRC (2013)
ANTARES collaboration
Astroparticle Physics 35 (2012)
+ IceCube and ANTARES alerts
FUNDAMENTAL PHYSICS
-
Common origin of gravitationnal wave and HE neutrinos ?
!
!
!
-
Dark matter indirect search
NEXT GENERATION OF DETECTORS
KM3NeT/ARCA (Astroparticle Research Using Cosmics in the Abyss): - phase 1 funded: 24 lines + 8 towers being deployed at Capo Passero
- phase 2: 2 building blocks (after 2016)
- phase 3: beyond 2020: 6 building blocks
NEXT GENERATION OF DETECTORS
KM3NeT/ARCA (Astroparticle Research Using Cosmics in the Abyss): - phase 1 funded: 24 lines + 8 towers being deployed at Capo Passero
- phase 2: 2 building blocks (after 2016)
- phase 3: beyond 2020: 6 building blocks (~600 lines)
NEXT GENERATION OF DETECTORS
Point source:
considering a fully hadronic process:
KM3NeT phase 3 - preliminary
for a E-2 spectrum
5"
significance (Nσ)
KM3NeT phase 2 preliminary
Galactic center
Diffuse flux:
4"
3"
2"
1"
0"
1"
2"
3"
years"
4"
5"
- The IceCube diffuse signal should be observed in the first year of operation
- Fermi Bubbles: one order of improvement in sensitivity w.r.t. ANTARES
all results/designs shown are preliminary
Geometries
Strawman
Designs
N
EXT
G
ENERATION
OF
DETECTORS
All upgrades also include PINGU low-energy strings (not shown) —
IceCube
generation:
onetechnology
order of magnitude
detection
these use 2nd
the current
IceCube
(1x large higher
PMT modules)
rate expected
IceCube collaboration, Aachen 2014
IceCube
“Sunflower” 240m
“Sunflower” 300m
top area (+60m border): 0.9km2
volume: 1.2 km3
strings: IC86
spacing: ~125m
top area (+60m border): km2
volume: 9.7 km3
strings: IC86+120
spacing: ~240m
top area (+60m border): km2
volume: 14.2 km3
strings: IC86+120
spacing: ~300m
CONCLUSION
- We are at the very beginning of the neutrino astronomy (IceCube
diffuse flux)
- ASTROGAM can help detecting neutrino sources (multi-messenger
studies + multi-wavelength follow-up)
- Next generation of neutrino telescopes: not so far from a point
source detection !
- 2025-2030: we can expect joint observations with ASTROGAM of
sources…