Status of LIGO Keita KAWABE, LIGO Hanford Observatory/Caltech for - - PowerPoint PPT Presentation

LIGO

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LIGO-G070617-00-D: KAWABE K., 2007/Sep/11 TAUP2007, Sendai

Status of LIGO

Keita KAWABE, LIGO Hanford Observatory/Caltech for the LIGO Scientific Collaboration

LIGO

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LIGO-G070617-00-D: KAWABE K., 2007/Sep/11 TAUP2007, Sendai

TOC

• Who we are

– Introduction to LIGO and LSC

• Where we are at now

– Status of Current Science Run (S5) – Detector Performance etc.

• Future

LIGO

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LIGO-G070617-00-D: KAWABE K., 2007/Sep/11 TAUP2007, Sendai

Who We Are

LIGO

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LIGO-G070617-00-D: KAWABE K., 2007/Sep/11 TAUP2007, Sendai

• Laser Interferometer Gravitational-Wave Observatory
• Funding: NSF
• Operation: Caltech-MIT
• 2 observatories, 3 detectors

– Hanford (LHO), 4km & 2km, (30+ local staffs) – Livingston (LLO), 4km, (30+ local staffs)

• CIT/MIT staffs outside of site (more than 100)
• LIGO Scientific Collaboration (LSC), a body carrying
• ut the scientific program of LIGO (about 570 as of

now, all over the world)

Who We Are

LIGO

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LIGO-G070617-00-D: KAWABE K., 2007/Sep/11 TAUP2007, Sendai

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LIGO Hanford Observatory (LHO) H1 : 4 km arms H2 : 2 km arms Desert in north west, Washington LIGO Livingston Observatory (LLO) L1 : 4 km arms Swamp in gulf coast, Louisianna

3000km, 10 ms

LIGO

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LIGO-G070617-00-D: KAWABE K., 2007/Sep/11 TAUP2007, Sendai

Detection concept

• Power-recycled,
• Michelson IFO,
• Fabry-Perot arms

– 4km (or 2km)

• Compare the travel time of photons in orthogonal

directions using laser interferometer

LIGO

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LIGO-G070617-00-D: KAWABE K., 2007/Sep/11 TAUP2007, Sendai

Initial LIGO Core Optics

• Substrate: SiO2

– 25cm diam ö 10cm thick – Homogeneity < 5ö10-7 – Internal mode Q factor > 2ö106

• Polishing

– Surface uniformity < 1nm rms – Radius of curvature matched < 3%

• Coating

– Scatter < 50ppm – Absorption < 2ppm – Uniformity < 10-3

LIGO

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Core Optics Suspention and Vibration Isolation

Vibration-isolated chambers using stack Core Optics Suspension

LIGO

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LIGO-G070617-00-D: KAWABE K., 2007/Sep/11 TAUP2007, Sendai

Where We Are At Now

LIGO

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LIGO-G070617-00-D: KAWABE K., 2007/Sep/11 TAUP2007, Sendai

• 4 Science Runs (S1-S4) in the past
• S5, starting Nov/04/2005, is still ongoing

– The last run with the current configuration – At design sensitivity (or better) for all 3 IFOs – Close to the end: 2007/Oct/01 00:00:00 UTC

• Will accumulate one year's worth of 3-IFO

coincidence by then

– Coincident run with GEO and VIRGO

• Sometimes 5-fold coincidence

Where We Are At Now

LIGO

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LIGO-G070617-00-D: KAWABE K., 2007/Sep/11 TAUP2007, Sendai

LIGO History

Now

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Ina na ug ug ur ur ati ti on

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1999 2000 2001 2002 2003

3 4 1 2 3 4 1 2 3 4 1 2 3 4 1 2 3 4

Firs rs t t Loc

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All ll IF IF O

10-17 10 10 -18 10 10 -20 10 10 -21

2004 2005

1 2 3 4 1 2 3 4 1 2 3 4

2006

S1 S4

Science (3 IFOs)

S2 S3 S5 10-22 4K K st st rai ai n n noi

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se at t 15 15 0 H H z z [Hz Hz -1/2]

TAMA, GEO TAMA TAMA, GEO, Allegro GEO, Allegro, Auriga GEO Joint coincidence run

1 2 3 4

2007 VIRGO

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15.

• 5. 1

12 12

S5 end

LIGO

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LIGO-G070617-00-D: KAWABE K., 2007/Sep/11 TAUP2007, Sendai

A Little about Detector Noise Limit

• Shot noise (and radiation

pressure noise)

• Thermal motion of mirror

and suspension

• Seismic motion
• Gravity gradient
• Residual gas
• Many, many technical

noise not shown here

– Electronics etc.

LIGO

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LIGO-G070617-00-D: KAWABE K., 2007/Sep/11 TAUP2007, Sendai

Design target (10-22/sqrtHz, 100Hz BW)

LIGO

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LIGO-G070617-00-D: KAWABE K., 2007/Sep/11 TAUP2007, Sendai

C C C P P P P P V V V V VV C S B B

LIGO

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3 IFOs running well: Recent control room screen

• 12 hr trend of

NS-NS inspiral range

LIGO

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NS-NS binary range from the start of S5 Duty factor from the start of S5

LIGO

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Anticipated Sources in LIGO's Band (And corresponding LSC Search Groups)

• Periodic sources

– Binary pulsars, spinning NS, low

mass X-ray binaries

– Eöample of upper limits (targeted)

• h0 < 4.8ö10-26 (PSR J1623-2631)
• ε < 1.1ö10-7 (PSR J2124-3358)
• Crab pulsar: observational GW

emission upper limit is smaller than the spin-down derived limit

R-modes Wobbling neutron star “Mountain” on neutron star Accreting neutron star

– Coalescing compact binaries

• NS-NS, NS-BH, BH-BH
• Physics regimes: Inspiral, merger,

ringdown

• Numerical relativity is essential to

interpret GW waveform

• ~16Mpc (1.4-1.4 M☉, all-sky, S/N=8)

LIGO

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LIGO-G070617-00-D: KAWABE K., 2007/Sep/11 TAUP2007, Sendai

Anticipated Sources in LIGO's Band (Continued)

• Burst

– e.g. Supernovae with asymmetric

collapse

– Abrupt, uncharacterized impulse.

–

Ex) Upper limit:

• EGW ~ 0.1 M☉ at 20 MpA (153 Hz

case, untriggered)

• EGW ~ 10 7

– to 10 8 – M☉ (SGR1806-

20 at 5-10 kpA)

gravitational waves

– Stochastic background

• Primordial Big Bang (t = 10-22

sec)

• Cross correlation of signals in

pairs (LHO-LLO, LHO-LHO)

• Eö.) First upper limit all-sky

map of stochastic point source for S4

LIGO

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LIGO-G070617-00-D: KAWABE K., 2007/Sep/11 TAUP2007, Sendai

BTW, We Need Interaction With Non-GW Researchers

• Knowledge from any other

means/channels

– better GW source model etc. – trigger with location information

(e.g. GRB/SWIFT) etc.

• GW detection might also impact

underlying physics of observed objects

– e.g. non aöi-symmetry and NS

equation of state

• NS specialists: please don't leave until

the end of this talk (conference ad alert!).

Control room sAreen for GRB alert

www.astroscu.unam.mx/neutrones/NS-Picture/NStar/NStar_lS.gif

LIGO

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I'm afraid I don't have time to talk about these

• Many observational results for S4 and

earlier were already published.

– Please go to http://www.ligo.org

• Some analysis are going on for S4 and S5.

– Some already appeared in conference

talks.

• Again http://www.ligo.org

LIGO

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LIGO-G070617-00-D: KAWABE K., 2007/Sep/11 TAUP2007, Sendai

S5 summary

• Design sensitivity requirement met by all 3 IFOs.
• Good duty factors.
• As of Sep/10/2007, about 97.3 % of 1-year (~355

days) 3-coincidence data has been accumulated.

– Already more than 1-year 2-site coincidence

(accomplished July 2007)

• End of S5 date set: 2007/Oct/01 00:00:00 UTC

– We'll very likely accumulate more than 1year

worth of 3-coincidence data.

• We'll be ready for the neöt step very soon!

LIGO

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LIGO Future

LIGO

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LIGO-G070617-00-D: KAWABE K., 2007/Sep/11 TAUP2007, Sendai

LIGO Future

100 million light ye ars

Enhanced LIGO

~2009

Advanced LIGO ~2014 LIGO today

• S5, 1yr data, with design

sensitivity

– Hundreds of galaöies in

range, detection possible

• Enhanced LIGO

– Operation in 2009 – 8 times more galaöies in

range, 8 times more detection probability

• Advanced LIGO project

(~200M$)

–

Construction start eöpected in FY08

–

1000X more galaöies in range

–

Eöpect ~1 signal/day- 1/week in ~2014

LIGO

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LIGO-G070617-00-D: KAWABE K., 2007/Sep/11 TAUP2007, Sendai

Mid-term Enhancement Plan

• Realistic, modest upgrade of initial LIGO

detectors

• Early commissioning of advanced LIGO

technologies

– One high power laser module, allowing

us to inject 30+ W (instead of 7-8 W)

– DC readout with output mode cleaner – Better thermal compensation

• Another ~1-year run, S6, before AdLIGO

LIGO

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LIGO-G070617-00-D: KAWABE K., 2007/Sep/11 TAUP2007, Sendai

LIGO

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LIGO-G070617-00-D: KAWABE K., 2007/Sep/11 TAUP2007, Sendai

Advanced LIGO

Initial Interferometers Advanced Interferometers Ope pe n up p wider er band nd Resh sh ape Nois is e

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tic s, s, we we ld ld ed ed to to si si li li ca ca su su spe spe ns ns ion ion f f ib ib ers ers

LIGO

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AdLIGO Suspension Prototype

LIGO

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Example of AdLIGO Noise

10

1

10

2

10

3

10

• 24

10

• 23

10

• 22

Fr Frequ qu ency ( H z) S t rai n n N oi se, h( f ) / H z1/

2

10 Hz 100 Hz 1 kHz 10-22 10-23 10-24 10-21

• Newtonian

background, estimate for LIGO sites

• Seismic ‘cutoff’ at 10

Hz

• Suspension thermal

noise

• Test mass thermal

noise

• Unified quantum

noise dominates at most frequencies for full power, broadband tuning

Initial LIGO Advanced LIGO

NS-NS Tuning

LIGO

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LIGO Conclusion

• LIGO is close to an end of S5 run with

eöcellent performance

• Data analyses ongoing
• Ready for the neöt step

– LIGO enhancement (operation 2009) – Advanced LIGO eöpected to detect GW

• n a regular basis (in 2014)

LIGO

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• GW detection for astronomy

– Higher detection confidence – Better localization of sources – Better polarization decomposition of the

wave

• All of these necessitates multiple detectors

around the world!

Global Network of GW Detectors in the Future

LIGO

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Global Network of GW Detectors in the Future

LIGO GEO600 Virgo TAMA300 AIGO(80m) AdLIGO (two sites) EGO - GEO LCGT AIGO(3k?)

LIGO

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Network of Terrestrial and Space GW Detectors in the Future

LIGO GEO600 Virgo TAMA300 AIGO(80m) AdLIGO (two sites) EGO - GEO LCGT AIGO(3k?) LISA

http://lisa.nasa.gov Courtesy NASA/JPL-Caltech

DECIGO

Courtesy S.Kawamura

LIGO

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Advertisement 1: 2nd Annual NS/LSC Meeting

• Oct/20/2007, Albert Einstein Institute in Hannover,

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• A meeting between neutron star eöperts and

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• “spin evolution, braking indices, crusts, magnetic

fields, population studies, new surveys, and anything else that could affect detectability of gravitational waves.” http://www.ligo-wa.caltech.edu/~mlandry/NSMeet/Oct07/

LIGO

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Advertisement 2: Pulsar analysis using your PC!

• All-sky pulsar GW search

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LIGO

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END

LIGO

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HEPI: Hydraulic External Pre-Isolator

Early implementation of AdLIGO technique

LIGO

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HEPI performance

LIGO

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TCS: Thermal Compensation System

Early implementation of AdLIGO technique

• Heat optics using CO2 laser

– to counter the wave front distortion caused by the

absorption of interferometer beam in the substrate

LIGO

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Thermal lens effect and TCS

Carrier

S

Sideband

AS port

Thermal lens effect controlled/compensated by CO2 laser

CO2 laser CO2 laser