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Astronomie des ondes
gravitationnelles :
Détections avec le réseau LIGO-Virgo et
70 observatoires (de la radio au TeV)
Image Credit: LSC/Sonoma State University/Aurore Simonnet
What are Gravitational waves ?
2
3
Multimessenger astronomyHE (>1 TeV) ν
LE ( MeV ) ν
Gamma-rays
X-rays
Optical
Radio
GRB
SGR/AXP
Giant Flare
Pulsar/ pulsar glitches
Supernovaetype II
4
Advanced generation detectors
Michelson interferometerGoal : (Lx-Ly)/Lx = 10-23
High power laser
High qualityoptics – 40 kgSurface RMS ~nm
Fabry-Perotcavities
SuspendedOptics
Attenuation1014 @ 10 Hz
Full system undervacuum ~10-12 atm
5
Feedback loops fromfew Hz to few kHz
200 W
The GW detectors networks
Virgo 3-km
GEO 600mLIGO –Hanford 4-km
LIGO –Livingston 4-km
3-km in 2017-18
4-km in 2020-22
6
Full ITF in 2020
O2 run
7
Ch
rist
mas
bre
ak
Co
mm
issi
on
ing
bre
ak
Earthquake close to Hanford
Detections after January 2017
8@ Leo Singer
August 2017
an interesting summer
9
GW170814 : Virgo first detection
10
7.3 13.7 4.4
GW170814: A Three-Detector Observation of Gravitational Waves from a Binary Black Hole Coalescence, Abbott et al. , PRL 119, 141101
A new binary black hole
11
GW170814: A Three-Detector Observation of Gravitational Wavesfrom a Binary Black Hole Coalescence, Abbott et al. , PRL 119, 141101
Better sky localisation (compare to LIGO only)
12
Source parameters improvements
13
Error in sky area : factor 20 !Reduced incertitude in distance by 1.5
8h 6h 4h 2h 0h 22h
30°
0°
-30° -30°
DL=0 250 500 750 1000Mpc 10°
1160 deg2
1oo deg2
6o deg2RA = 03h 11mDec = -44° 57m
Rapid localization
HL
HLV
Final localization
570 Mpc+300-230
540 Mpc-210+130
GW170814: A Three-Detector Observation of Gravitational Waves from a Binary Black Hole Coalescence, Abbott et al. , PRL 119, 141101
Polarization in GR
14
Tensor modes
Only ones expected with GR
Vector modes
Scalar modes
Allowed by other gravitation theories
Favor pure tensor vs pure vector or scalar
Cannot conclude on mixed version
GW170814: A Three-Detector Observation of Gravitational Waves from a Binary Black Hole Coalescence, Abbott et al. , PRL 119, 141101
Antenna pattern
17th of August
15
Masses
16
MChirp
=(m
1m
2)3/5
(m1+m
2)1/5
=1.188-0.002+0.004M
Known BNS
Allow by EOSs
Largest knownmass for NS
Source parameters
17
Pro
perties
of th
e bin
aryn
eutro
n sta
r merg
erG
W170817, A
bb
ott et al, su
bm
ittedto
PR
X, 2018
GW
1708
17 :
Ob
serv
ati
on
of
gra
vit
ati
on
alw
aves
fro
ma
bin
ary
neu
tro
n s
tar
insp
iral
, PR
L 2
017
Equation of state (EOS)
18
Lµk2
R
m
æ
èç
ö
ø÷
5
Remanent object
19
Properties of the binary neutron star merger GW170817, Abbott et al, submitted to PRX, 2018
QNM ≥ 6kHz
Signal from ms to 10s ks
delay betweenms to 10s of ks
Signal ~ ms
Key role from Virgo in the
localisation
20
« Multi-messenger observations of a binary neutron star merger », Abbott et al., ApJ, 2017
17/08/201712:41:04
GW170817
+5h GW : send updatedskymap with the 3
detectors
+10h GW : send updatedskymap with refined
algorithm
GW170817 localization
2 interferometers (HL) AddingVirgo (HLV)
190 deg2, distance 40 Mpc 28 deg2, distance 40 MpcVolume : 380 Mpc3
Less than 100 galaxies couldbe the host of the event !!
What an alert !
21
« Gravitational waves and Gamma-rays from binary neutron star merger: GW170817 and GRB170817A », Abbott et al., ApJ, 2017
Signal from BNS :GW170817
Detection fromFermi/GBM of a short gamma-ray burst(GRB170817A)
First reports fromtemporal coincidences
with GW170817
17/08/201712:41:04
+2 s
GRB alert sent+16 s
Sent alert on GW sideBEGINNING OF THE
MULTI-MESSENGER
CAMPAIGN
+40 min
+1h20min
Report from Integral/SPI-ACSDetected GRB170817A
P(GW-GRB only by chance) < 5 10-
8
Discovery of kilonovaAT2017gfo by SwopeFind host galaxy : NGC4993START CAMPAIGN ON AT2017GFO
22
17/08/201712:41:04
Localisation with GWDistance 40 Mpc
+2 s GRB170817A
+5h
GW170817
+11h
+1.2j First spectra of the kilonova
+9j Discovery of an X-ray counterpart
First radio signal found
with VLA
+16j
«M
ult
i-m
esse
ng
ero
bse
rva
tio
ns
of
a b
inar
yn
eutr
on
sta
r m
erg
er»,
Ab
bo
tt e
t al
., A
pJ,
201
7
Observation inX increasing
+150j
GRB detection
23
Goldstein, A., et al., “An Ordinary Short Gamma-Ray Burst with Extraordinary Implications: Fermi-GBM Detection of GRB 170817A.” 2017, ApJL, Vol. 848, issue 2,
Model for short gamma-ray bursts
24
secondsdays
Common GW-GRB analysisTest for fundamental physics
using time delay and source distance
25
-3 10-15 £vGW - vEM
vEM
£ + 710-16
dtS = -1+g
c3U(r(l ))dl
re
ro
ò
-2.610-7 £gGW -gEM £1.210-6gravitational
potentialDeviation to Einsten-Maxwell
Improve between a factor 2 and 1010
previous constraints
"Gravitational Waves and Gamma Rays from a Binary Neutron Star Merger: GW170817 and GRB 170817A", ApJL (2017)
Common GW-GRB analysisAstrophysical impact
26"Gravitational Waves and Gamma Rays from a Binary Neutron Star Merger: GW170817 and GRB 170817A", ApJL in press (2017)
Is this a standard short GRB ?
27
"Gravitational Waves and Gamma Rays from a Binary Neutron Star Merger: GW170817 and GRB 170817A", ApJL in press (2017)
Possible scenarios
28
"Gravitational Waves and Gamma Rays from a Binary Neutron Star Merger: GW170817 and GRB 170817A", ApJL in press (2017)Swift and NuSTAR observations of GW170817: detection of a blue kilonova, Evans et al, Science
Could we detect similar events ?
29
Redshift (z)
Cu
mula
tive
Observ
ed
Rate
(yr
)
Known sGRBpopulation 40/year
GR
B17
0817
A
GRB detections (/year):• O3 : 0.1-1.4 • Design : 0.3 – 1.7
BNS detections (/year):• O3 : 1-50• Design : 6-120
"Gravitational Waves and Gamma Rays from a Binary Neutron Star Merger: GW170817 and GRB 170817A", ApJL in press (2017)
GW rate=1540-1220
+3200 Gpc-3y-1
Kilonova
30
Fer
nan
dez
an
d M
etzg
er,
A..
Rev
. Nu
c. P
art.
Sci
. 201
6, 6
6
Kilonova – spectral observations
31
Date
Blue Red Near infrared
Grawita Spectrum ESO/VLT & Gemini
ePESSTO - Spectrum ESO/VLT & Gemini
Signal
continuous (BB)
absorption Cs,Te
Blue Red Near infrared
TGW+2.5 d
Hubble constant measurement
32
H0 = 70-8
+12kms
-1Mpc
-1
"A standard siren measurement of the Hubble constant with GW170817", Nature in press (2017)
h(t)µMchirp
5/6
Df (cosi)
Main results with GW170817
33
LIGO and Virgo in the next years
34
Observing scenario
35
LIGO
Virgo
2015 2016 2017 2018 2019 2020 2021 2022 2023
KAGRA
60-80
Mpc
Early Mid Late Design
60-100
Mpc
O2 O3O1
O3
200
Mpc
130
Mpc
140
Mpc
O2
Futur is bright !
36
Imag
e C
red
it: N
AS
A G
od
dar
d S
pac
e F
igh
t C
ente
r /
CI
Lab
backup
37
The full campaign
(up to now)
38
-100 -50 0 50
GW
g-ray
X-ray
UV
Optical
IR
Radio
10-2
t-tc (s) t-tc (days)10-1 100 101
LIGO, Virgo
Fermi, INTEGRAL, Astrosat, IPN, Insight-HXMT, Swift, AGILE, CALET, H.E.S.S., HAWC, Konus-Wind
Swift, MAXI/GSC, NuSTAR, Chandra, INTEGRAL
Swift, HST
Swope, DECam, DLT40, REM-ROS2, HST, Las Cumbres, SkyMapper, VISTA, MASTER, Magellan, Subaru, Pan-STARRS1, HCT, TZAC, LSGT, T17, Gemini-South, NTT, GROND, SOAR, ESO-VLT, KMTNet, ESO-VST, VIRT, SALT, CHILESCOPE, TOROS, BOOTES-5, Zadko, iTelescope.Net, AAT, Pi of the Sky, AST3-2, ATLAS, Danish Tel, DFN, T80S, EABA
REM-ROS2, VISTA, Gemini-South, 2MASS,Spitzer, NTT, GROND, SOAR, NOT, ESO-VLT, Kanata Telescope, HST
ATCA, VLA, ASKAP, VLBA, GMRT, MWA, LOFAR, LWA, ALMA, OVRO, EVN, e-MERLIN, MeerKAT, Parkes, SRT, Effelsberg
SALT
ESO-NTTSOAR
ESO-VLT
7000o
4000o
t-tc(days)
1.2
1.4
2.4
wavelength (nm)
no
rma
lize
d F
l
400 600 1000 2000
INTEGRAL/SPI-ACS
Fermi/GBM
t-tc (s) -12 -10 -8 -6 -4 -2 0 2 4 6
counts
/s (arb
. sca
le)
fre
qu
en
cy (
Hz)
500400300
200
100
50
LIGO - Virgo
Chandra
9d
J VLA
16.4d Radio
Las Cumbres
11.57h w
DECam
11.40h iz
MASTER
11.31h W
VISTA
11.24h YJKs X-ray
DLT40
11.08h h
1M2H Swope
10.86h i
«M
ult
i-m
esse
ng
ero
bse
rva
tio
ns
of
a b
inar
yn
eutr
on
sta
r m
erg
er»,
Ab
bo
tt e
t al
., A
pJ,
201
7
39
Wikipedia
40
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