m. boër, vulcano workshop 2016...m. boër vulcano workshop 2016 13 . m. boër vulcano workshop 2016...
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M. Boër Vulcano workshop 2016 1
M. Boër, Vulcano workshop 2016
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Since H. Neanderthalensis and H. Sapiens the photon has been the main « messenger » for the observation and understanding of the sky
Astronomy, as a science, started with physics, hence it evolves also with particle physics
In the XX th century start of multi-wavelength astronomy
Vulcano workshop 2016 2
LIGHT, THE HISTORICAL MESSENGER
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Information drawn from one
messenger is par tial
Deriving a consistent picture of a
phenomenon / source from a
variety of information sources
Exemple: multiwavelength
astronomy
Galactic magnetism
AGN, and AGN in their galaxy
GRBs
Multimessenger astronomy
means the coordinated use of
several par ticles/wavelengths as
they provide complementary
information about an
astronomical
source/phenomenon
WHAT MEANS MULTIMESSENGER
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M. Boër Vulcano workshop 2016 4
OVERVIEW OF A COSMIC ACCELERATOR
HAWK call, ICRC 2015
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Jacobsen et a l . ,
2015
M. Boër Vulcano workshop 2016 5
MULTI-
MESSENGER
EMISSION
IN AGNS
GW
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Progenitor can
be e i ther a
massive star
co l lapsing in a
black hole
( long GRB) or
the merger of a
compact
neut ron star
b inar y system
(shor t GRB)
M. Boër Vulcano workshop 2016 6
GAMMA-
RAY
BURSTS
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M. Boër Vulcano workshop 2016 7
INTERNAL SHOCK SCENARIO
�, CR
�, CR
�, GW
GW (mHz)
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Object EM Counterpart VHE/UHE Cosmic rays Neutrinos Gravitational
waves
The Sun Observed (since
long)
HE gamma-rays Observed Observed N/A
Supernovae / SNR Observed (since
long)
Observed SNR Observed (SN) If in Galaxy
Hypernovae,
(lGRB)
Observed Up to 20 GeV Predicted, but no
association
Predicted, but no
association
too faint
BHBH Merger Probably very faint No association No association No association GW 150914
NSBH merger faint, observed? No association No association No association Expected (>= 02)
NSNS Observed (sGRB) Observed (LAT) No association No association Expected ALV and
LISA (before
merger)
SMBH/AGNs Observed Observed Expected but no
association (CenA)
No association LISA (SMBH)?
Stochastic
(discrete)
N/A Observed ? Expected (>O2)
Stochastic
(cosmological)
CMB N/A Too faint probably,
can be indirect
Dark matter Indirect evidence N/A Too light N/A Vulcano workshop 2016 8
ASTROPHYSICAL OBJECTS SEND MORE
THAN ONE MESSENGER
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Cosmic rays Observed since beginning of XX th
century Several experiments, Auger, Tel.
Array AMS, CREAM, PAMELA, ISS-CREAM…
Antimatter, CR composition, UHECR, missing baryons/dark matter.
Trace supernovae explosions and magnetic fields SNRs Is knee connected to SNR turn
off?
Origin of ankle?
In galaxy(ies)
HE/UHECR extragalactic? Source?
AGNs (radiogalaxies)?
GRBs?
Why isotropy?
Other (topological defect, etc.)
COSMIC RAYS
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Swift sources (no correlation)
Cen. A hot spot (but needs more data)
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AUGER EVENTS
Auger coll., ICRC 2015
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Neutrino astrophysics has already started since the 80s The Sun
SN 1987A Probably the first
« multimessenger » observation
Important results drawn Neutrino oscillations
Supernovae models
Upper bonds on neutrino mass, charge, etc.
Wait for next galactic SN
NEUTRINOS
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Icecube Map of 37 IceCube
detections
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HIGH ENERGY NEUTRINOS
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Detected s ince 2012 by IceCube and now Antares
30 – 1200TeV Photopion production from particle
accelerated at UH energies (Fermi acceleration)
Origin: AGN?
GRB (no simultaneous detection)?
SN remnants?
Accumulation near Galactic Centre? Extended source?
I ceCube and ANTARES have been l inked to automated te lescope exper iments (no pos i t ive resul ts so far despi te many obser vat ions with TAROT, Zadko and other te lescopes) TAToO program (TAROT/ROTSE/ANTARES)
I ceCube events now on GCN/TAN (Trans ient Ast ronomy Network) for prompt EM fo l low -up (ht tp ://gcn .gs fc .nasa.gov )
Now corre lated searches Neutr inos/UHECR/GW
Perspect ives : IceCube-Grn2
Km3Net
HIGH ENERGY NEUTRINOS
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ANTARES FOLLOW-UP
Slide fm A. Coleiro, ANTARES)
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ANTARES 3 TeV – 1 PeV
IceCube 200 TeV – 100 PeV
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ANTARES/ICECUBE SEARCHES FOR
NEUTRINOS FROM GW 150914
Adrian-Martinez et al., 2016
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CR and � spectra
(Asano & Mészaros, ApJ, 2014)
� spectra
(Asano & Murase, Ad A, 2015)
M. Boër Vulcano workshop 2016 16
DIFFUSE COSMIC-RAY AND NEUTRINO
FLUXES FROM GRBS
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Merger of black holes
GW signal – EM??? GW 150914
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FIRST GW EVENT
MERGER OF BLACK HOLES
M. Boër
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Last « new messenger » Detection of GW 150914
while ALIGO was (almost) in its first run open expectations for a large number of sources CBC (BHBH/NSBH/NSNS)
Impact on stellar evolution and SFR (we have the numbers)
Expect stochastic signal
See large number of papers by LIGO/Virgo collab.
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GRAVITATIONAL WAVES
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63 groups receive the GW alerts 30 of them have actually
followed-up the alerts
Problem of error box size 1000 sq. deg >> 100 sq deg
Time to get the position 2 days for GW 150914,
expected several hours
Hope it will improve
Is the source EM bright? Few hopes for BHBH
Better for NSBH
sGRB for NSNS
M. Branchesi talk Friday
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EM FOLLOW-UP OF GW SOURCES
LIGO/Virgo Coll. et al. 2016, ApJL
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NS – NS Merger
GW + EM signal
NS – BH Mergers
GW + EM? signal
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NS – NS AND NS - BH
NASA GSFC Piran, Nakar and Rosswog, 2013
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Vulcano workshop 2016 21
DID SWIFT DETECT NSBH MERGERS?
Siellez et al. 2016
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Vulcano workshop 2016 22
THE SEQUENCE OF EVENTS
SNAPSHOT AND SENSITIVITY
Burst Afterglow
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THE ERROR BOX SIZE
M. Boër
Abadi et al. 2012
Singer et al. 2016
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M. Boër Vulcano workshop 2016 24
CORRELATION WITH GALAXIES
Courtois et al. 2013
100Mpc 3D map
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In space, instruments with large fov Swift, Fermi, SVOM
Difficulty to use XMM-Newton
On ground large facilities include SKA and LOFAR But correlation in time not
granted
For optical/IR, large facilities Needs galaxy catalog and
information on distance (Singer et al. 2016)
Vulcano workshop 2016 25
FACILITIES FOR FOLLOW-UP
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TAROT-ZADKO NETWORK
WIDE FIELD OF VIEW WORLDWIDE NETWORK
TCH Chile
(25cm)
TCA France (25cm)
ZADKO
(1m)
CADOR
(server
) C2PU Calern (1m) Obs. Nat. Aurès, DZ
(15 x 0.4m + 1 x 1m)
TRE Réunion (F)
(20cm 08/16)
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RAMSES PROJECT AT AURES OBS. R O B O T I C A D VA N C E D M U LT I M E S S E N G E R A N D S PAC E E N V I R O N M E N T S U R V E YO R
Problem Pave the field of 100 sq. deg.
With enough sensitivity
And reactivity: Low latency trigger -10s, i.e. 5s
And flexibility Look at the whole field at the
start, then concentrate on candidates
The RAMSES project “Métatélescope”, 16 x 45cm x
2.5° (Boër, 2015 + patent)
Generic instrument, chosen for the Aurès National Observatory (Algeria, Seghouani et al. 2015)
Reduced costs, modular maintenance
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EMRIs SMBH eat ing a smal le r BH
(NASA)
Ultra-compact binary sytems
PSR J0348+0432 (ESO)
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LISA (2034--)
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M. Boër Vulcano workshop 2016 29
GRAVITATIONAL WAVE LANDSCAPE
http://rhcole.com/apps/GWplotter/
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XX th was the century of panchromatic and t ime domain astronomy
The XXI st century sees the begining of mult imessenger astronomy UHECR: Auger, TA
� : ANTARES/IceCube/KM3Net
GW: LIGO/Virgo/LISA/ET
VHE/UHE: Magic, HESS, CTA, Fermi
In few years CR, neutr inos and grav itational waves have been observed
But the EM fol low -up needs dedicated strategies and faci l i t ies Already existing or in construction
LOFAR/TAROT-Zadko, HESS, SKA, HAWK
Swift , Fermi, XMM
Or planned RAMSES@ONA, BlackGem
SKA, CTA, JWST
SVOM, Athena, JEM EUSO
LSST
Mult imessenger is st i l l in i ts infancy, but great resul ts obtained (GW, CR, neutr inos)
They open a window on many processes from fundamental physics to cosmology to ste l lar astrophysics General relativity and beyond
Supermassive BH and galaxy core dynamics, jets…
Acceleration of CR and neutrino production
Compact binaries in a wide range of masses and type (BH/NS, and possibly WD with LISA)
Stochastic background from discrete sources
Cosmological stochastic background (may be)
Vulcano workshop 2016 30
CONCLUSIONS
M. Boër