Observation of Gravitational Waves from a Binary Black Hope Merger

Hiro Yamamoto LIGO Lab / Caltech
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Hiro Yamamoto ICRR seminar on February 22, 2016

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LIGO-G1600270-v4

Hiro Yamamoto ICRR seminar on February 22, 20162

Observation of Gravitational Waves
from a Binary Black Hope Merger
Hiro Yamamoto LIGO lab/Caltech● New Astronomy bygravitational wave signal at
the 100th memorial year ofgeneral relativity» Just the beginning …

Cosmic Background Explorer● How the GW signals look like● Basics of interferometer or

how to hear the GW signal?
● GW signal in advanced LIGO
● Scope for the future
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Hiro Yamamoto ICRR seminar on February 22, 2016

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G1600220-v8
1.3GlyRedshift = 0.09
5.1σ
1/200,000 year
M1=36 M⊙,
M2=29 M⊙
Mfinal=62 M⊙
3 M⊙ radiatedto GW wave

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h=10-21h x arm= 10-18 m= proton / 1000h x earth = 10-14= 10 proton
2~400 1/Gpc3yr

Hiro Yamamoto ICRR seminar on February 22, 2016

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Two Black Holes Merge into One

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Black Hole Waves Simulation

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Hiro Yamamoto ICRR seminar on February 22, 2016

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Gravitational waves●

Gravitational waves arepropagating dynamic fluctuations inthe curvature of space-time(‘ripples’ in space-time)●Emissions from rapidly accelerating
non-spherical mass distributions» Quadrupolar radiation

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Hiro Yamamoto ICRR seminar on February 22, 20167

Interferometer for
Gravitational Wave detection
2 mirrors in thearm effectively
lengthen the armby ~1000
L2

E2

E1

L1

Dark port
L1 − L2h=
L1 + L2
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E1- E2 ∝ L1-L2
h~10-21
L1-L2~10-18m

Hiro Yamamoto ICRR seminar on February 22, 2016

Hanford
Observatory(H2K and H4K)

LIGO sites

4 km+ 2 kmHanford, WA (LHO)• located on DOE reservation

4 km• treeless, semi-arid high desert

Livingston
Observatory(L4K)• 25 km from Richland, WA• iLIGO : H2K and H4K ⇒aLIGO : 4k LHO + 4k LIGO-India

Livingston, LA (LLO)• located in forested, rural area
• commercial logging, wet climate• 50km from Baton Rouge, LA• One L4K IFO
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Hiro Yamamoto ICRR seminar on February 22, 20169

Event GW100916: blind injection FAKE
http://www.ligo.org/science/GW100916/ on Sep.16,2010
Hanford

Livingston

Virgo

LHO SNR=15
LLO SNR=10

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Hiro Yamamoto ICRR seminar on February 22, 201610

The Chirp of Two Black Holes
Colliding : GW150914 REAL

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Signal vs GRpredictions

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Hiro Yamamoto ICRR seminar on February 22, 201612

How could we see the signal1) better sensitivity●September 12, 2015 ~ October 20, 2015 (January 12, 2016)» H1:70%, L1:55%, H1+L1:48% => 16 days of data analyzed for data

Around 100 Hz, h = 8 10−24 /√Hz.
● 30 M⊙ black holes - 1.3Gpc = 4.1 x iLIGO, rate x70● 1.4 M⊙ neutron star - 70–80Mpc = 3.5 x iLIGO, rate x40●

1000

10-21300

S6 runO1 runAdv. LIGO designFuture upgrades

10-22
SNRStrain Noise (1/Hz )30M⊙ Black Hole Binaries

100Line : optimal orientation

30

10-23

GW150914

10S6 Threshold (SNR=8)

GW150914 (S6)

10-24
10100
Frequency (Hz)LIGO-G1600270-v4

1000

0.03

0.1

0.3
Redshift

Hiro Yamamoto ICRR seminar on February 22, 2016

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Fundamental Sensitivity Limits in
Advanced LIGO
Radiation pressure
noise : #photons
recoiling against thetest mass mirror=>heavy mass

−2110−22

Strain [1/√Hz]

10Suspension:
Thermal noise =>fused silica fiber,
heavy mass

Seismic noise :−23
ground 10motion
tomass =>better
isolation system−2410−2510Quantum fluctuations
Seismic vibrations
Newtonian Gravity
Suspension Thermal noise
Mirror Coating Brownian
Mirror Coating Thermo−Optic
Mirror Substrate Brownian
Residual Gas
Total noise

Shot noise : quantum
nature of laser =>increase power

Coating Brownian noise :thermal fluctuation of coating
later and loss => better coatingand larger beam
1

10
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2

3

10 on February 22, 2016
Hiro 10
Yamamoto ICRR seminar

Frequency [Hz]

Sensitivities during O1

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Hiro Yamamoto ICRR seminar on February 22, 201615

The real instrument isfar more complex…
ETMY

L. Barsotti - March 9, 2012
Adapted from G1200071-v1

ITMY

Input
ModeCleaner

MC3

MC2

MC1

ITMX

ETMX TRANSMON
ALS

PRM

HAM1

BS

PR3

FI

PSL

HAM2

Power
Recycling
Cavity

PR2

HAM3
SR2

HAM4

SignalRecycling
Cavity

SRM

SR3

HAM5

FI

Differential
Arm Length
Readout

DCPD

OutputModeCleaner

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HAM6

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Advanced LIGO
in Pictures
Pre-stabilized Laser

Quadruple
suspension

Active Seismic Isolation
40kg test mass
34cm ϕ x 20cmInput Optics

Output Mode Cleaner

Auxiliary Laser
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Lock acquisition
1μm to 1pm ala iLIGO
Optics Letters Vol. 27, Issue 8, pp. 598-600 (2002)
This image cannot currently be displayed.

1~10µmλ/1000~1 nm
1 pm

L x h = 10-18 = 1 pm/106
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Hiro Yamamoto ICRR seminar on February 22, 201618

Advanced LIGO optics
OplusE 1207 特集６
重力波観測用レーザー干渉計における光学設計
This image cannot currently be displayed.

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Hiro Yamamoto ICRR seminar on February 22, 2016

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How could we see the signal2) better understanding of IFO
This image cannot currently be displayed.

This image cannot currently be displayed.

initial LIGO

advanced LIGO
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G1400628-v3 by P. Fritschel

Speedier commissioning
This image cannot currently be displayed.

qLock acquisition strategy
designed in from the start,
including a new Arm Length
Stabilization systemØ Enables a controlled
acquisition process●4 km arm

Better teams on hand» More people and with more experience» Observatory staff, including operators, involved from the beginning●Better support structure in place»»●Software tools in place
Online web tools in place

Having been there before helps a lot!

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Hiro Yamamoto ICRR seminar on February 22, 2016

Project Integrated Testing Plan
Integrated testing phases interleaved with installation● Complementary division between LHO and LLO●» Designed to address biggest areas of risk as soon as possible» H1 focused on long arm cavities; L1 worked outward from the vertexJuly2012

H1Oct2012

Jan2013

One Arm Test
1st arm cavity
Green only

Build & test from the arms backward

L1

Input Mode Cleaner
with high power testApr2013

July2013

Oct2013

Jan2014

Input Mode Cleaner

Apr2014

July
2014

HIFO-XY
Both arms +corner
No AS port

HIFO-YY-arm +corner
Green +PSL IR

Dual recycled Michelson
IIIIII

Build & test from the laser outward
Hiro Yamamoto ICRR seminar on February 22, 2016
LIGO-G1600270-v4

FullInterferometer

LIGO Chronology

Journey for the new astronomy

Real size R&D for the real detection

Dreveridea to realization ~ 15 years

Weiss

1970s
Feasibility studies and early work on laser interferometer gravitational-wave detectors
1979
National Science Foundation (NSF) funds Caltech and MIT for laser interferometer R&D
1984
Development of multiple pendulum Advanced LIGO Concept
1989 December Construction proposal for LIGO submitted to the NSF ($365M as of 2002)
1990 May
National Science Board approves LIGO construction proposal
1994 July
Groundbreaking at Hanford site
1999
LIGO Scientific Collaboration White Paper on a Advanced LIGO interferometer concept
2000 October
Achieved “first lock” on Hanford 2-km interferometer in power-recycled configuration
2002 AugustFirst scientific operation of all three interferometers in S1 run
2003
Proposal for Advanced LIGO to the NSF ($205 NSF + $30 UK+Germany)
2004 OctoberApproval by NSB of Advanced LIGO
2005 November Start of initial LIGO Science run, S5, with design sensitivity
2008 April
Advanced LIGO Project start
2009 July
Science run (“S6”) starts with enhanced initial detectors
2014 May
Advanced LIGO Livingston first two-hour lockVogt
2015 March
Advanced LIGO all interferometers accepted2015 September Advanced LIGO observation run 1 scheduled
Executive
Initial LIGO eventsAdvanced LIGO events
R&D of aLIGO using iLIGO facility

LIGO-G1600270-v4

Thorn

Hiro Yamamoto ICRR seminar on February 22, 2016

producer &consultant ofmovie“Intersteller”

23Advanced LIGO Data analysis●Burst (generic transient search)»»●Compact Binary Coalescence Search»●●P1500229: Observing gravitational-wave transient GW150914 with minimal assumptions
All-sky search for generic GW transients, in low latency for EM follow up and deep, offline for 4σdetection confidence»P1500269 : GW150914: First results from the search for binary black hole coalescence with Advanced
LIGO
Low latency, all-sky search for BNS and NS-BH systems»Search for binary neutron-star and black-hole systems (BNS, BHNS, BBH)

Continuous Wave
»All-sky deep/broad search for isolated stars»

Targeted search for high value, known pulsars

Stochastic Gravitational Wave background»»

P1500222: GW150914: Implications for the stochastic gravitational-wave background from binary
black holesDirectional and isotropic search for stochastic gravitational wave backgroundConstraints of a detected background of astrophysical origin with long transients

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Significance

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Improving sensitivity●Near term upgrade» So far so good – based on past experience– More challenges waiting» Thermal compensation» Parametric instability – mirror vibration couples to field modeexcitation» Gas dumping» Charge fluctuation in mass
» Low frequency unknown noise● Long term upgrade» Third IFO to be joined» Voyager – use LIGO facility, cryogenic, Silicon, 2μ laser» Cosmic Explorer – new facility, very long arm

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Advanced LIGO
~ BNS rates#events by advanced LIGO ~1000 x #events by initial LIGO
Assumes NS-NS rate between 10 -8 Mpc-3yr-1
and 10-5 Mpc-3yr-1

Observation run
1
2
327

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Hiro Yamamoto ICRR seminar on February 22, 2016

Planning for Advanced LIGO Science
DetectedFullsensitivity(200 Mpc):end-2018
2106 months
3 months
2 months1

Number of events

10N e v e n t s="34π !√1××2 Rang e I F O × T ime
M pc 3 M y r
32nd run: 6 months @80120 Mpc more detection

3rd: 2017-2018

2016(July)-2017
010

Threshold for likely detection

2015(Sep)-2016(Jan)−110

1st run: 4 months @70-80
Mpc DETECTED
2 detectors, 1 year @ 15 Mpc

Astronomy
LIGO-G1600270-v4−21020

40

60

80

100120Range [Mpc]

Hiro Yamamoto ICRR seminar on February 22, 2016

14016028180200

Aiming for the future
beyond advanced LIGO

Range z > 1 ( 10 x aLIGO)
New facility ⇒ Major cost
40km arm, bigger mass, bettercoating, reduction of losses

Range ~ 2x aLIGO (340Mpc)
Cost O( $10M )Squeezing, bigger mass, bettercoating, reduced thermal noise

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Range ~ 2x A+ (700 MPc)
Cost O( $50M~$100M )Cryogenic (120K), 1550nm
laser, Silicon, better coating

Hiro Yamamoto ICRR seminar on February 22, 201629

LIGO = LIGO Lab (CIT,MIT,UFL) +LSC (LIGO Science Collaboration)●1006 members, 83 institutions, 15 countries

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Welcome! The LIGO Open Science Center (LOSC,
https://losc.ligo.org) provides access to a variety of LIGO data
products, as well as documentation, tutorials, and online tools forfinding and viewing data.

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International network

Dave: I am positively delighted to
inform you that yesterday, LIGOIndia was formally approved as an
official Mega-Science project by
the government of India!

§ detection confidence§ locate the sources§all detectors should have comparable sensitivity (~factor 2)§decompose the polarization of gravitational waves§ open up a new field of astrophysics!
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Hiro Yamamoto ICRR seminar on February 22, 2016

Localization
poor because of only 2 IFOs

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Improvement of Binary Neutron Star
Merger Localization by Adding LIGO-India
Hanford+Livingston+one more

Hanford+Livingston+two more

x denotes blind spots
S. Fairhurst, “Improved source localization with
LIGO India”, J. Phys.: Conf. Ser. 484 012007
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Hiro Yamamoto ICRR seminar on February 22, 201634

LIGO needs partner GW detectors
with similar sensitivity●LIGO is seriously seeking for third/fourth good IFOs
» AdVirgo is trying to join O2, but still have some problems to solve» LIGO-India has been approved, many years to come●To improve sky coverage, sensitivity > 0.5 of LIGO
» < 20 Mpc is useless●To KAGRA» Eagerly waiting to join the international GW network» Good sensitivity is a must as a good partner» Sooner the better– Simpler configuration need to be considered

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Hiro Yamamoto ICRR seminar on February 22, 201635

Multi-messenger astronomy
collaborations with Groups
Detecting other signals
Discussions going toward the new astrophysical era● Complementary alert system●●

Complementary and supplemental information about the source●

Many MOUs exchanged with EM partners, covering the whole EMspectrum.

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Hiro Yamamoto ICRR seminar on February 22, 201636

New era may be opening …
●Fermi GBM Observations of LIGO Gravitational Wave event
GW150914 (arXiv:1602.03920v2)»With an instantaneous view of 70% of the sky, the Fermi Gamma-ray Burst Monitor (GBM) isan excellent partner in the search for electromagnetic counterparts to gravitational wave (GW)
events. GBM observations at the time of the Laser Interferometer Gravitational-wave
Observatory (LIGO) event GW150914 reveal the presence of a weak transient source above
50 keV, 0.4 s after the GW event was detected, with a false alarm probability of 0.0022.

»Message from Tsune Kamae : FermiのGlastBurstMonitor（NaaIとBGOのシンチレータからなる、簡単にモニター）だけで、受かっています。信号は小さいのですが、タイミングが、ほぼドンピシャリなので、本当に何かあったのだと思います。
NS-NSではもっと大量のガンマ線が出ると予想されています。ビーミングでずれていたのかもしれません。BH-BHなら、強いガンマ線が予言されていないのです
が、どこまで精密に計算されているのかは判りません。
●ELECTROMAGNETIC COUNTERPARTS TO BLACK HOLE
MERGERS DETECTED BY LIGO (non-LSC publication) ( A. Loeb,arXiv:1602.04735v1)» Message from Patrick Brady : Welcome to astronomy! This is great.
Hiro Yamamoto ICRR seminar on February 22, 2016
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End of slides

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Hiro Yamamoto ICRR seminar on February 22, 2016

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Test Masses withthermal compensation system●

Requires the state of the art in substrates,
polishing and coating» Fabri-Perot cavity is used to measurearm length or space distortion
40 kg

Test Masses:●

Half-nm flatness over 300mm diameter●

0.2 ppm absorption at 1064nm●

Coating specs for 1064 and 532 nm●

Mechanical requirements: bulk and coating
thermal noise, high resonant frequency

34cm ϕ x 20cm

Round-trip opticalloss: 75 ppm max

Ringheater

Compensation plates:
34cm ϕ x 10cm

BS:
37cm ϕ x 6cmLIGO-G1600270-v4

ITM
T = 1.4%

Hiro Yamamoto ICRR seminar on February 22, 201639

Three major issues(2) Parametric Instabilities

LIGO-G1600270-v4

Hiro Yamamoto ICRR seminaronal.,February
22, 2016
Evans etPhys. Rev.
Lett. 114, 161102 (2015)

LIGO

LIGO-T0900582

Three major issues(3) Squeeze film damping●Small gap (5 mm) between ETM and its reaction
mass increased damping from residual gas» Current poor vacuum level at LLO end station means this is asignificant thermal noise term below ~60 Hz» At expected vacuum
level, squeeze film damping noise will
The conclusion is that the area of the ESD supporting annulus results in a noise level whichapproximately
matchesnoisethat of thewith a 2cm gap, and that this level dominates the totalcompete with radiationpressure
atITM-CP
full power
for annular designs 3cm thick or more.

●Beyond lower vacuum,
the Failuressolution is a new,
6.1 Complicated
are the (holeresults for ain
couplecomplicatedannular reaction Heremass
theof moremiddle)»»»

designs that seemed promising, but turned out not to giveProvides same amountof electro-static
drive
actuation
good results.
The “vented” ERM hasthe ESD
supportedby a 1cm thick annulus which is held 1cm away from theReduces damping 11cm
forcebyERM
a factorof 2.5x
thickby some kindof stand off, leaving theERM at 25mm from the TM. Another is the “engraved”
Working towards possible
2016
annular ERMretrofit
in which inthe earlygaps in theESD pattern are
cut out to a depth of 2cm, thus minimizing the surface
area which is close to the TM.

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Hiro Yamamoto ICRR seminar on February 22, 2016

Squeezed Light in LIGO
suppressing quantum noise without increasing power§

Heisenberg Uncertainty Principle§

Squeezed state§ Reduce noise in one quadrature at theexpense of the other§ Shot noise - phase,radiation pressure - amplitude
X1 and X2
associatedwithamplitude
and phase

X2

GEO600−2110−2210

LIGO H1−2310X1
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Strain Sensitivity [1 / √ Hz]

Typical noise without squeezing
Squeezing−enahnced sensitivity

210310Frequency (Hz)Aasi, et al., (LIGO ScientificCollaboration), Nature Physics, 7, 962(2011); Nature Photonics 7 613 (2013).

Hiro Yamamoto ICRR seminar on February 22, 201642

Cryogenic in Voyger

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Hiro Yamamoto ICRR seminar on February 22, 201643

Cosmic Explorer :Long is good
● Coating noise» Gain: L1.5
» Cryogenic/Crystal: no need
● Displacement noise» Gain: L» Newtonian N. irrelevant● Radiation pressure» Becomes irrelevant● Shot noise» Gain: ~sqrt(L)» Freq. indep. Squeezing● Vertical susp. Thermal» Gain: constant
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Hiro Yamamoto ICRR seminar on February 22, 2016

Carson Sink, Nevada (Alkali flat)
40km
40km

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Hiro Yamamoto ICRR seminar on February 22, 2016

From G1101133 by D.H.ShoemakerIn the beginning●Rai Weiss of MIT was teaching a course on GR
in the late ʻ60s●

Wanted a good homework problem for the students
Why not ask them to work out how to use
laser interferometry to detect gravitational waves?

●●…led to the instruction book we have been following
ever since46

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Hiro Yamamoto ICRR seminar on February 22, 2016

The Gravitational Wave Spectrum
Cosmic Strings
Relic radiation

Supernovae
BH and NS
Extreme Mass RatioBinaries
Inspirals

Supermassive BH Binaries
Binaries coalescencesSpinning NS
10-16 Hz
Inflation Probe

10-9 HzPulsar timing

10-4 Hz
100 Hz103 HzSpace detectors
Ground interferometers

Laser Interferometer
Gravitational Wave
Observatory

LIGO-G1600270-v4Slide
Credit: Matt Evans (MIT)Hiro Yamamoto ICRR seminar on February 22, 2016