The Coming Global Gravitational-wave
Detector Network with an
Emphasis on Advanced LIGO"

LIGO-G1201199

David Reitze!
LIGO Laboratory!
California Institute of Technology!1!
ICRR Seminar, U. Tokyo, November 16, 2012

Topics"
 Initial LIGO!
 Selected Science Results from LIGOʼs S5

and S6 Science Runs!
 Advanced LIGO – Status and Progress!
 LIGO-India: Status and Prospects!

2!
ICRR Seminar, U. Tokyo, November 16, 2012

LIGO Laboratory"
LIGO Hanford

LIGO Observatories are operated
by Caltech and MIT

MIT

CaltechLIGO Livingston

3!

ICRR Seminar, U. Tokyo, November 16, 2012

Initial LIGO Concept"











Power-recycled Michelsoninterferometer!
4 km long Fabry-Perot arm
cavites !
Passive seismic isolation !
10 kg mirrors figured to λ/1000!
10 W à 30 W pre-stabilized
laser operating at 1064 nm!
Passing GWs modulate thetime-of-flight of light between
the end test mass and thebeam splitter!
The interferometer acts as atransducer, turning GWs into
photocurrent !
»

2!L
h=
L
10 kW

10 kW

250 W
5W

A coherent detector!

4!
ICRR Seminar, U. Tokyo, November 16, 2012

LIGO History"








1989: LIGO Project proposed to NSF!
1992: LIGO Project funded by NSF!
1995 – 1999: LIGO facilities construction at Hanford and Livingston!
1998 – 2002: Installation/integration of initial LIGO interferometers!
2002 - 2005: Interferometer commissioning interleaved with scienceruns (S1-S4)!
Nov 4, 2005 – Sept 31, 2007: S5 science run!
» Design sensitivity reached; 15 Mpc range; > 1 year of triple coincidence data !

2007 – 2009: Enhanced LIGO instrument upgrade!
» Low cost upgrade, tests key Advanced LIGO technologies!



April 2008: Advanced LIGO Construction begins!
July 7, 2009 – Oct 20, 2010: S6 science run!
» 18 Mpc range to merging binary neutron stars!

!
5!
ICRR Seminar, U. Tokyo, November 16, 2012

Best Strain Sensitivity: S6 Science Run-19

10

Seismic Noise

-20

10

Strain (1/√Hz)(1/ Hz)StrainHanford 4 km S6
Livingston 4 km S6
Initial LIGO Science Requirement

-21

10

-22

10

Shot Noise
Suspension Thermal
Noise

-23

10

2

3

4

5

6 7 8 9

2

10

2

3

4

5

6 7 8 93

10Frequency(Hz) 16, 2012
ICRR Seminar,
U. Tokyo, November

2

3

4

5

6 7 8 9

6!

4

10

!
Recent LIGO/Virgo/GEO
science results"

All LSC/Virgo Observational Papers:
https://www.lsc-group.phys.uwm.edu/ppcomm/Papers.html
7!
ICRR Seminar, U. Tokyo, November 16, 2012

Astrophysical Sources of Gravitational
Waves"
Asymmetric Core
Collapse
Supernovae

Coalescing
Compact Binary
Systems: NeutronStar-NS, Black
Hole-NS, BH-BH- Weak emitters,
not well-modeled(‘bursts’), transient- Strong emitters,
well-modeled,- (effectively)transientCredit: Chandra X-ray Observatory

Credit: AEI, CCT, LSU- Cosmic strings, soft
gamma repeaters,
pulsar glitches also in‘burst’ class

Cosmic Gravitationalwave BackgroundSpinning neutronstars- Residue of the Big
Bang, long duration- (effectively)
monotonic waveform- Long duration,
stochastic background- Long duration
NASA/WMAP Science Team

Casey Reed, Penn State

8!
ICRR Seminar, U. Tokyo, November 16, 2012

Astrophysical Sources of Gravitational
Waves"
Asymmetric Core
Collapse
Supernovae

Coalescing
Compact Binary
Systems: NeutronStar-NS, Black
Hole-NS, BH-BH- Weak emitters,
not well-modeled(‘bursts’), transient- Strong emitters,
well-modeled,

In addition
to these known- (effectively)transientsources,
there may be surprisingsources of gravitational waves.
Cosmic GravitationalCredit: Chandra X-ray Observatory

Credit: AEI, CCT, LSU

Spinning neutronstars- Cosmic strings, soft
gamma repeaters,
pulsar glitches also in‘burst’ classwave Background- Residue of the Big
Bang, long duration- (effectively)
monotonic waveform- Long duration,
stochastic background- Long duration
NASA/WMAP Science Team

Casey Reed, Penn State

9!
ICRR Seminar, U. Tokyo, November 16, 2012

Compact binary
inspiral, merger, ringdown"

Thereʼs a lot ofphysics andastrophysics inthe waveforms!!
 Waveformreconstruction(often buried in
detector noise).!


InspiralMerger Ringdown

10!
ICRR Seminar, U. Tokyo, November 16, 2012

Searches for Binary Mergers"
This source:!
Binary BH-BH system

Buried in this noise stream:

Produces this waveform:
We use different
methods (in this case
optimal Wiener filtering
using matched
templates) to pull thesesignals from the noise:h“Chirp” waveform

11!
The problem is that non-astrophysical sources also produces signals (false positives)
ICRR Seminar, U. Tokyo, November 16, 2012

The Current GW Detector Network"
LIGO
HanfordLIGO
Livingston

GEO600

Virgo

12!
ICRR Seminar, U. Tokyo, November 16, 2012

Expected detection rates for compact
binary mergers"
Binary coalescences rates !

LIGO Scientific and Virgo Collaborations,“Predictions for the Rates ofCompact Binary Coalescences Observable by Ground-based Gravitationalwave Detectors” Class. Quantum Grav. 27 (2010) 173001» neutron star (NS) = 1.4 M¤, Black Hole (BH) = 10 M¤"

Initial !
LIGO!
Advanced!
LIGO!
The error bar is large and important!!
13!
ICRR Seminar, U. Tokyo, November 16, 2012

Searching for Low Mass Compact
Binary Coalescences"
LIGO Scientific and Virgo Collaborations, “Search for Gravitational Waves from Low Mass Compact Binary Coalescence in LIGO's
Sixth Science Run and Virgo's Science Runs 2 and 3”, Phys. Rev D85 (2012) 082002

Latest LIGO-Virgo
upper limits

Predicted rates

14!
ICRR Seminar, U. Tokyo, November 16, 2012ʻEventʼ GW100916 – A Blind Injection"
http://www.ligo.org/science/GW100916/
Hanford

Livingston

ICRR Seminar, U. Tokyo, November 16, 2012

Virgo

15!

Searching for High Mass Compact
Binary Coalescences"

IMBH formation proposed to complete BH mass hierarchy…!
»

…but their existence is uncertain!
»

Via stellar collision in globular clusters, stalled supernovae of early pop III stars, progressive accumulation into higher
mass !
Stellar winds suppression of runaway accumulation, merger recoil ejection of BH from GC!

Candidates exist: ultraluminous x-ray sources M82 X-1, NGC 1313 X-2 !
S5/VSR1 search using constrained unmodelled waveform (Coherent WaveBurst algorithm) !
Effective Range (Mpc) for H1H2L1V1Rate Density Upper Limit (Mpc-3 Myr-1)

LIGO Scientific and Virgo Collaborations, “Search for gravitational waves from intermediate mass
binary black holes”, Phys. Rev. D85, 102004 (2012)

ICRR Seminar, U. Tokyo, November 16, 201216!

Triggered searches for gamma-ray
bursts"

GRBs are good candidates for GW
emission!
GRB progenitor models!
»»Long GRB à Core collapse SN of a massively
spinning star!
Short GRB à coalescence of a neutron star
and a compact object!
– ≤ 15% from neutron star quakes!

Compact, relativistic, asymmetric!!
»

But measured red shifts à 10 Gpc!

Credit: Ute Kraus

17!
ICRR Seminar, U. Tokyo, November 16, 2012

Searches for GWs from nearby
GRB sources"


GRB050311, GRB070201: short GRBs withsky localizations that overlap nearby galaxies!
»
»





GRB050311 overlap with M81 (3.6 Mpc)!
GRB070201 overlap with M31 (770 kpc)!

Binary coalescence in M31 excluded at >99%
confidence level!
BNS coalescence in M81 excluded at 98%
confidence level!

M31, GRB 070201

GRB051103
M81
GRB 051103
LIGO Scientific Collaboration, K. Hurley,“Implications for the Origin of GRB 070201
from LIGO Observations”, Astrophys. J. 681(2008) 1419

LIGO Scientific Collaboration, “Implications for theOrigin of GRB 051103 from LIGO Observations”,
arXiv:1201.4413

ICRR Seminar, U. Tokyo, November 16, 201218!

Searches for GWs from known
pulsars"Continuous gravitational-wave emission
due to asymmetry rotation axis !
»
»
»




Spin-down limit:!
Crab pulsar (using LIGO data):!
»h0 < hsd/7, EGW < 0.02Etotal!

Vela pulsar (using Virgo data):!
»

elastic deformations of the solid crust or core !
Distortion an extremely strong misaligned
magnetic field!
Weak emitters !

h0 < 0.66hsd, EGW < 0.45Etotal!

S5 search of 116 pulsars!
ll

Lowest upper-limit h0: 2.3 x 10-26(PSR J1603-7202)!
Lowest upper-limit ellipticity: 7 x 10-8 (PSR
J2124-3358)!

LIGO Scientific and Virgo Collaborations, “Beating the spindown limit on gravitational wave emission from the Crabpulsar”, Astrophys. J. Lett. 683 (2008) 45

LIGO Scientific and Virgo Collaborations, “Beating the spindown limit on gravitational wave emission from the Velapulsar,” Astrophys. J. 737 (2011) 93

LIGO Scientific and Virgo Collaborations, “First search forgravitational waves from the youngest known neutron star”,
Astrophys. J. 722 (2010) 1504

LIGO Scientific and Virgo Collaborations, “Searches For
Gravitational Waves From Known Pulsars With Science
Run 5 LIGO Data”, Astrophys. J. 713 (2010) 671
19!

ICRR Seminar, U. Tokyo, November 16, 2012

Upper limit on the Stochastic GW
Background"

LIGO S5 result: 	

Ω0 < 6.9 x 10-6!

Abbott, et al. “An upper limit on thestochastic gravitational-wave backgroundof cosmological origin”, Nature., V460:
990 (2009).

20!
ICRR Seminar, U. Tokyo, November 16, 2012!

!

Advanced LIGO"

21!
ICRR Seminar, U. Tokyo, November 16, 2012

Advanced LIGO"Initial LIGOAdvanced LIGO – a complete
upgrade of the LIGO
interferometers!
Advanced LIGO is designed toincrease the distance probed(ʻreachʼ) by ~ 10X !
» Leads to 1000X increase in volume à
1000X increase in event rate !

Expect 10s of detections per year
at design sensitivity"» 1 aLIGO observational day = a few
years of iLIGO !
Image courtesy of Beverly Berger
Cluster map by Richard Powell22!
ICRR Seminar, U. Tokyo, November 16, 2012

Rochus Vogt, Ron Drever,
Kip Thorne, Rai Weiss
1987
ICRR Seminar, U. Tokyo, November 16, 201223!

Advanced LIGO MREFC
construction project"Advanced LIGO funded April 2008 !
» 7 year construction project !

$205.1M in funding from NSF!
Plus capital contributions from international partners!
» $14M from the Science and Technology Facilities Council (UK) – quadruple test
mass suspensions!
» $14M from the Max Planck Institute (Germany) – 200 W front-end stabilized laser!
» $1.7M from the Australian Research Council – interferometer sensing and control
components!

Complete upgrade to 2 Hanford and 1 Livingston 4 km
interferometers!
» Advanced LIGO baseline plan (more later)!

Construction by LIGO Laboratory with participation by member
groups of the LIGO Scientific Collaboration!
On schedule (and on budget) to complete in March 2015 !
24!
ICRR Seminar, U. Tokyo, November 16, 2012

-19

10

Hanford4 km S6
Livingston
4 km S6-20

Strain (1/√Hz)

Strain (1/ Hz)

10

-21

10

AdvLIGO,
No Signal
Recycling(earlyoperation)

-22

10

AdvLIGO,
Zero Detuning(Low Power)

-23

10

AdvLIGO, Zero
Detuning (High Power)
AdvLIGO, NS-NS
optiimized

AdvLIGO, High Frequency Detuning

-24

10

1

10

2

3

4

5

6 7 8 9

2

2

3

4

5

6 7 8 9

10

3

2

3

4

5

6 7 8 910

Frequency (Hz)ICRR Seminar, U. Tokyo, November 16, 2012

4

10
25!

-19

10

Hanford4 km S6
Livingston
4 km S6-20

10

NS-NS!

BH-BH!
(30 M¤)!

No
SRM!

150 Mpc!

1.60 Gpc!

0-det
low P!

145 Mpc!

1.65 Gpc!

0-det
high P!

190 Mpc!

1.85 Gpc!

NS-NS
tuned!

200 Mpc!

1.65 Gpc!

Strain (1/√Hz)

Strain (1/ Hz)

case!
-21

10

AdvLIGO,
No Signal
Recycling(earlyoperation)

-22

10

AdvLIGO,
Zero Detuning(Low Power)

-23

10

AdvLIGO, Zero
Detuning (High Power)
AdvLIGO, NS-NS
optiimized

AdvLIGO, High Frequency Detuning

-24

10

1

10

2

3

4

5

6 7 8 9

2

2

3

4

5

6 7 8 9

10

3

2

3

4

5

6 7 8 910

Frequency (Hz)ICRR Seminar, U. Tokyo, November 16, 2012

4

10
26!

Fundamental Noise Budget"

27!
ICRR Seminar, U. Tokyo, November 16, 2012

Best Strain Sensitivities for the LIGO Interferometers
Comparisons among S1 - S5 Runs

LIGO-G060009-03-Z

1e-16
LLO 4km - S1 (2002.09.07)
LLO 4km - S2 (2003.03.01)
LHO 4km - S3 (2004.01.04)
LHO 4km - S4 (2005.02.26)
LHO 4km - S5 (2007.03.18)
LIGO I SRD Goal, 4km

1e-17h[f], 1/Sqrt[Hz]

1e-18
1e-19
1e-20
1e-21
1e-22
1e-23
1e-24
10

100

1000
Frequency [Hz]ICRR Seminar, U. Tokyo, November 16, 2012

10000
28!

Advanced LIGO overview"
What is Advanced?!
Parameter!

Initial LIGO!

Advanced
LIGO!

Input Laser
Power!

10 W!
(10 kW arm)!

180 W!
(>700 kW arm)!

Mirror Mass !

10 kg!

40 kg!

Interferometer
Topology!

Powerrecycled
Fabry-Perot
arm cavityEOM
Laser
Michelson!

Dual-recycled
Fabry-Perot
arm cavity
Michelson!
(stablerecycling
cavities)!

GW Readout
Method!

RF heterodyne!

DC homodyne!

Optimal Strain
Sensitivity !

3 x 10-23 / rHz!

Tunable, better
than 5 x 10-24 /rHz inbroadband!

Seismic
Isolation
Performance!

flow ~ 50 Hz!

flow ~ 13 Hz!

MirrorSuspensions!

SinglePendulum!

Quadruple
pendulum!

29!
ICRR Seminar, U. Tokyo, November 16, 2012

Advanced LIGO Schedule Summary - Sept. ʻ12(Including selected control milestones showing project contingency)
Last Planned
Acceptance Date

MREFC Funding Start April 2008

FY08

FY09

FY10

FY11

FY12

FY13

FY14

Last Acceptance
NSF Reporting Date

FY15

L1 Fab. / Procure / Assemble
L1 Hand-off

L1 Hand-off NSF Reporting Date

L1 De-install / install
Install Complete 1st Site

Install Complete 1st Site NSF Reporting Date

L1 Integration / Testing
L1 Acceptance
L1 Acceptance NSF Reporting Date

H1 & H2 Fab. / Procure / Assemble
H2 Hand-off (Stage 1)

H1 and H2 Hand-off NSF Reporting Date

H2 Stage 1 De-install / Install
H2 Single Arm Locking Test
H2 Storage & Acceptance
H1 Hand-off

H2 Storage &Acceptance NSF
Reporting Date

H2 Storage & Accept

H1 De-install / Install
Install Complete 2nd Site
NSF Reporting Date
HIFO-Y

Install Complete 2nd Site
HIFO-X

H1 Integration/ Testing
PSL/IO/IMC

DRMI

H1 Acceptance

30!
G1000195-v11 September 2012 Current

Full Lock

H1 Acceptance NSF
Reporting Date

End Project Construction
ICRR Seminar, U. Tokyo, November 16, 2012

Advanced LIGO Subsystem Summary – Sept ʻ12(Showing Development and Project Production Early Milestones)
Last
PlannedAcceptance Date

MREFC Funding Start

FY07

FY08

FY09

FY10

FY11

FY12

FY13

FY14

Last NSF
Acceptance
Date

FY15

Project Management

Seismic Isolation

Suspensions (US)

Suspensions (UK)
Facility Mods & Prep.
Core Opticsu Development Endu L1 Production Endu H1 Production Endu I1 Stored for Indiau Installation End
Production

Pre-Stabilized Laser
Pre-Stabilized Laser (AEI)IFO Sensing & Control
Auxiliary Optic Systems

Installation & Testing

Data Acquist. & Controls

Input Optics
Installation & Testing L1
Installation & Testing H1
Data Computing Systems
G1000195-v11 September 2012 Current

L1/H2Seminar,
Hand-Off U. Tokyo, November
H1 Hand-Off
ICRR
16, 2012

End Project Construction31!

Pre-stabilized Laser"
Diagnostic
Breadboard!

To
IFO!

32!
ICRR Seminar, U. Tokyo, November 16, 2012

Advanced LIGO Pre-stabilized
Laser"!
ICRR Seminar, U. Tokyo, November 16, 2012

Pre-mode cleaner:
spatial & temporal filtering"§ bow tie configuration, round-trip length of 2m!
§ Finesse of 124, circulating power 9kW (200W
§
§
§

input)!
Linewidth: 575 kHz (HWHM)!
Length control with automatic lock acquisition!
PZT actuator / thermal actuator to off-load PZT!

!

50 cm

10

-1

1x
2x
1y
2y
laser requirements

Power noise at RF!

34!

relative pointing noise (Hz -1/2 )

10 -2

10 -3

10 -4

10 -5

10

-6

10

-7

10 -8

Beam pointing !
fluctuations before PMC!

1

10

ICRR Seminar, U. Tokyo, November 16, 2012100
Fourier frequency (Hz)

1k

10k

Advanced LIGO Seismic!
Isolation!
10

Displacement ( m/Hz0.5 )

10
10
10

Optical Table X displacements at successive steps of control

-5

-6

-7

-8

! HAM Chambers Equipment
10
10
10
10

-9

! HEPI: !
Hydraulic External!
Pre Isolator!

! ISI:
Single Stage
Internal Seismic Isolator

-10

-11

-12

No Control
S1 and S2 under HFB Control
S1 under HFB, S2 under LFB
Sensor Correction ON! ISI:
10-1! BSC Chambers Equipment

0

Two-Stage
10
10Frequency
Internal
Seismic(Hz)Isolator
ICRR Seminar, U. Tokyo, November 16, 20121

! HEPI: !
Hydraulic External!
Pre Isolator!
35

Suspensions"

ICRR Seminar, U. Tokyo, November 16, 201236!

Quadruple Suspensions"37
ICRR Seminar, U. Tokyo, November 16, 2012

Welding Suspension Fibers to a Test Mass

38!
ICRR Seminar, U. Tokyo, November 16, 2012

Fibers Are Fragile…."

39!
ICRR Seminar, U. Tokyo, November 16, 2012

1 DOF of Top2Top TFs for All 2 Fiber/
Glass QUADs"

40
ICRR Seminar, U. Tokyo, November 16, 2012

Advanced LIGO Core Optics"


40 kg masses, 38 cm in diameter, and figured to 0.15 nm rms!
All substrates and polishing successfully executed!
Successful coatings demonstrated for all kinds of optics except for ETMs!
–

challenge is 10-3 uniformity over the larger beam diameter!

The greatest single technical risk, still !

41!
ICRR Seminar, U. Tokyo, November 16, 2012

Putting it all together…"


Photos of equipment in place!

ETM/TransMon !
Telescope!

Mode Cleaner Suspensions !

42!

Beamsplitter Seismic/!
Suspension Installation!
ICRR Seminar, U. Tokyo, November 16, 2012

One-Arm Test (OAT)"

A single, complete 4km arm at LHO, to perform integrated testing!
Arm-length stabilization system using phase-locked 532 nm light!
» Addresses biggest initial challenge – locking – seen in iLIGO!
Two complete chambers: Optics, suspensions, seismic isolation!
» One optics suspended with fused-silica fibers, one with wire suspension!

BSC ISI!
Quad SUS!

HEPI!

ACB!

ACB!

ITM!

ETM!

TrMon SUS!
1064 / 532 nm
NPRO!

TM!

Arm
Cavitylength &alignmentsensing!

HEPI!

Quad SUS!

BSC ISI!

HEPI!

Y-End! ICRR Seminar, U. Tokyo,4Novemberkm !
16, 2012

LVEA !

HEPI!

OAT Set-up"

44!
ICRR Seminar, U. Tokyo, November 16, 2012

One-Arm Test"

Locking camevery quickly(subsystem test
paying off!),
enabling realcharacterizationof system!
Extremely usefulfor tuning seismic
isolation systembefore fullinterferometer
configuration
realized!

45
ICRR Seminar, U. Tokyo, November 16, 2012

Squeezed Interferometry: A Possible
Upgrade to Advanced LIGO"Shot noise and radiation pressure come from statistical fluctuations ultimately
arising from the Heisenberg uncertainty principle !
»A noise reduction in one quadrature can be achieved at the expense of theother quadrature à ʻsqueezed lightʼ!
»»!

These fluctuations exist in the vacuum state. They enter the interferometer at the output port.!

3 dB injected squeezed vacuum reduces noise by √ 2!
Possible to achieve 10 dB !
Coherent Statex2

Coherent Vacuum
State x2

Δx1
Δx2
x1

x1

Δx1Δx2≥1
Phase Squeezingx2

Amplitude Squeezing

x2

x1

x1

Squeezed Vacuum
State x2

Δx1
Δx2
46!

ICRR Seminar, U. Tokyo, November 16, 2012x1

First Demonstration of Squeezed Interferometry in a
Gravitational-wave Detector"

GEO600

GEO6003.5 dB
reduction in noise

LIGO Scientific Collaboration, “A gravitational wave
observatory operating beyond the quantum shot-noise
limit”, Nature Physics 7, 962–965 (2011)

ICRR Seminar, U. Tokyo, November 16, 201247!

Using Squeezed Light to Improve
LIGO Sensitivity"
LSC, "Enhancing the astrophysical reach of the LIGO gravitational
wave detector by using squeezed states of light”, in preparation

Improved sensitivity above 150 Hz
2.1 dB above 500 Hz

48!
ICRR Seminar, U. Tokyo, November 16, 2012

!

!

LIGO-India"

49!
ICRR Seminar, U. Tokyo, November 16, 2012

LIGO-India"
The idea in a nutshell– !
 A direct partnership
between LIGO
Laboratory and India tobuild a LIGO
interferometer on Indiansoil!
!
 Follows from earlier
attempt to locate a
LIGO detector inAustralia!
50!
ICRR Seminar, U. Tokyo, November 16, 2012

Enabling multi-messenger astronomy
with gravitational waves"






»

wide field telescopes!

LIGO
Hanford

t1

t2
LIGO
Livingston+ Image tiling!
+ Galaxy weighting!

à

X-ray, γ-ray !
follow-up !

Crude estimate of angularresolution!

! GW ~ "GW / d ~ few degrees
à

Swift
Swift

Many GWs sources arelikely to radiate in theelectromagnetic spectrum !
We want to see them via
different observational
methods simultaneously!
GW ʻAperture synthesisʼ!

Coherent
Detector
NetworkVirgo

t3

Neutrino observatories!
Optical !
follow-up!

Image:
http://earthobservatory.nasa.gov/

51!
ICRR Seminar, U. Tokyo, November 16, 2012

Example: GW100916 Skymap"
LIGO-Virgo source localization ~ O(100NGC2380deg2) !
(Credit: Las Cumbras»Skymap for 100916 ‘event’!10

Observatory www.lcogt.net)

Disconnected regions!

Top probability pixels imaged by Swiftand other ground-based opticaltelescopes !
Swift pixels maximized probability on
NGC2380 and ESO492-010!

!15

nearby	  	
  galaxies	
  Zadko	  dec (deg)



Swi$	
  

!20

SkyMapper	
  
!25

!30

TAROT,	
  ROTSE	
  Zadko	
  
!35
105

110
115
ra (deg)

120

LIGO Scientific and Virgo Collaborations, “Swift
Follow-Up Observations Of Candidate GravitationalWave Transient Events” arXiv:1205.1124

!120

!60

0
ra (deg)

60

120

180
52!

ICRR Seminar, U. Tokyo, November 16, 2012

LIGO-India"

LIGO Lab (with its UK, German and Australian partners) provides components for
one Advanced LIGO interferometer (H2) from the Advanced LIGO project!
India provides the infrastructure (site, roads, building, vacuum system), “shipping& handling,” staff for installation & commissioning, operating costs!
Indian Institutional Participants: !
»
»
»
»



Indian funding – LIGO-India is a Mega-science Project»»Inter-University Centre for Astronomy and Astrophysics (Astrophysics, Site Selection, Computing) !
Raja Ramanna Centre for Advanced Technology (Detector Development)!
Institute for Plasma Research (Facility and Vacuum construction, control systems)!
+ IndIGO Consortium (broader scientific community in India)!
!

Total request of ~ $230M to fund construction and operations!
Funding status: approved by DAE/DST, referred to Cabinet of the Prime Minister of India for
approval!

US funding – funding for aLIGO components through MREFC (no new costs) !
»Total contribution $140M (includes aLIGO components, designs, documentation)!

53!
ICRR Seminar, U. Tokyo, November 16, 2012

Binary Neutron Star Merger
Localization: Hanford-Livingston-Virgo"
3 site network!
x denotes blind spots!

S. Fairhurst, “Improved source localization with
LIGO India”, arXiv:1205.6611v1
54!
ICRR Seminar, U. Tokyo, November 16, 2012

Binary Neutron Star Merger Localization:
Hanford-Livingston-Virgo-India"
4 site network!

S. Fairhurst, “Improved source localization with
LIGO India”, arXiv:1205.6611v1
55!
ICRR Seminar, U. Tokyo, November 16, 2012

Binary Neutron Star Merger Localization:
Hanford-Livingston-Virgo-KAGRA"
4 site network!

S. Fairhurst, “Improved source localization with
LIGO India”, arXiv:1205.6611v1
56!
ICRR Seminar, U. Tokyo, November 16, 2012

Binary Neutron Star Merger Localization:
Hanford-Livingston-Virgo-India-KAGRA"
5 site network!

S. Fairhurst, “Improved source localization with
LIGO India”, arXiv:1205.6611v1
57!
ICRR Seminar, U. Tokyo, November 16, 2012

LIGO-India Status"
Status in the US: -- the National Science Board has given
permission to NSF, at its discretion, “to approve theproposed aLIGO Project in scope, enabling plans for the
relocation of an advanced detector to India” !
 Status in India – awaiting Cabinet approval and beginningof seed funding for facility design work!
 Major activities in India are now focused on site
evaluation/selection as well as development of a Tier 2
computing center @ IUCAA !


Expect LIGO-India to begin operations in 2020 or 2021!
58!
ICRR Seminar, U. Tokyo, November 16, 2012

Summary"
Observational papers from initial LIGO in partnershipwith Virgo producing interesting limits on astrophysicalsources of gravitational waves!
 Advanced LIGO progressing well; on target to begin
operations by 2015!
 LIGO-India is an exciting opportunity to expand theglobal gravitational wave network !
We are excited by the prospects for KAGRA"
 These are exciting times for gravitational wave
physicists and astronomers! "

どうもありがとう！"
ICRR Seminar, U. Tokyo, November 16, 201259!