32
ICRR talk on Dec.9,2003 1 LIGO-G030672-00-E LIGO I status and advanced LIGO proposal Hiro Yamamoto LIGO Lab / Caltech LIGO I » basic design » current status advanced LIGO » outline of the proposal » technical issues GW signals and data analysis

LIGO I status and advanced LIGO proposalhiro/talks/G030672.pdfLIGO-G030672-00-E ICRR talk on Dec.9,2003 1 LIGO I status and advanced LIGO proposal Hiro Yamamoto LIGO Lab / Caltech

  • Upload
    others

  • View
    12

  • Download
    0

Embed Size (px)

Citation preview

Page 1: LIGO I status and advanced LIGO proposalhiro/talks/G030672.pdfLIGO-G030672-00-E ICRR talk on Dec.9,2003 1 LIGO I status and advanced LIGO proposal Hiro Yamamoto LIGO Lab / Caltech

ICRR talk on Dec.9,2003 1LIGO-G030672-00-E

LIGO I status andadvanced LIGO proposal

Hiro Yamamoto LIGO Lab / Caltech

LIGO I» basic design» current status

advanced LIGO» outline of the proposal» technical issues

GW signals and data analysis

Page 2: LIGO I status and advanced LIGO proposalhiro/talks/G030672.pdfLIGO-G030672-00-E ICRR talk on Dec.9,2003 1 LIGO I status and advanced LIGO proposal Hiro Yamamoto LIGO Lab / Caltech

ICRR talk on Dec.9,2003 2LIGO-G030672-00-E

Sources of today’s talk

NSF review : G.Sanders, D.H.Shoemaker, M.Zucker, K.Thorne» June 2003 : advanced LIGO review» November 2003 : 2003 annual review of LIGO

LSC meeting : B.Barish» November 2003

Program advisory committee : B.Barish» December 2000 : PAC9» November 2001 : PAC11

Presentations» December 2003 : CaJAGWR seminar (Caltech) : S. Marka» December 2003 : 13th GRG (Osaka) : A.Lazzarini

advanced LIGO proposal and cost book» http://www.ligo.caltech.edu/advLIGO/

Page 3: LIGO I status and advanced LIGO proposalhiro/talks/G030672.pdfLIGO-G030672-00-E ICRR talk on Dec.9,2003 1 LIGO I status and advanced LIGO proposal Hiro Yamamoto LIGO Lab / Caltech

ICRR talk on Dec.9,2003 3LIGO-G030672-00-E

An International Network ofInterferometers

LIGO

•detection confidence•locate the sources•decompose thepolarization ofgravitational waves• complemental - timeand direction

GEO VirgoTAMA

AIGO

Page 4: LIGO I status and advanced LIGO proposalhiro/talks/G030672.pdfLIGO-G030672-00-E ICRR talk on Dec.9,2003 1 LIGO I status and advanced LIGO proposal Hiro Yamamoto LIGO Lab / Caltech

ICRR talk on Dec.9,2003 4LIGO-G030672-00-E

The LIGO Laboratory SitesInterferometers are aligned along the great circle connecting the sites

Hanford, WA (4 km (H1) + 2 km (H2))

Caltech

MIT

3002 km(L/c = 10 ms)

Livingston, LA (4 km (L1))

Page 5: LIGO I status and advanced LIGO proposalhiro/talks/G030672.pdfLIGO-G030672-00-E ICRR talk on Dec.9,2003 1 LIGO I status and advanced LIGO proposal Hiro Yamamoto LIGO Lab / Caltech

ICRR talk on Dec.9,2003 5LIGO-G030672-00-E

LIGO ObservatoriesLIGO Observatories

Hanford ObservatoryWashingtonTwo interferometers(4 km and 2 km arms)

Livingston ObservatoryLouisianaOne interferometer (4km)

GEODETIC DATA (WGS84)h: 142.555 m X arm: N35.9993°Wφ: N46°27’18.527841” Y arm: S54.0007°Wλ: W119°24’27.565681”

GEODETIC DATA (WGS84)h: -6.574 m X arm: S72.2836°Wφ: N30°33’46.419531” Y arm: S17.7164°Eλ: W90°46’27.265294”

Hanford, WA ->

<- Livingston, LA

Page 6: LIGO I status and advanced LIGO proposalhiro/talks/G030672.pdfLIGO-G030672-00-E ICRR talk on Dec.9,2003 1 LIGO I status and advanced LIGO proposal Hiro Yamamoto LIGO Lab / Caltech

ICRR talk on Dec.9,2003 6LIGO-G030672-00-E

Interferometer Concept

Laser used to measurerelative lengths of twoorthogonal arms

L1- L2 ~ 10-19 m or

h=(L1- L2)/L~ 10-23

6W

150W

20kW

4km

0.5W

(1) seismic (low freq)

(2) thermal (medium freq)

(3) shot (high freq)

signal ~ L1- L2

Page 7: LIGO I status and advanced LIGO proposalhiro/talks/G030672.pdfLIGO-G030672-00-E ICRR talk on Dec.9,2003 1 LIGO I status and advanced LIGO proposal Hiro Yamamoto LIGO Lab / Caltech

ICRR talk on Dec.9,2003 7LIGO-G030672-00-E

LIGO Beam Tube

LIGO beam tube underconstruction in January 1998

65 ft spiral welded sections

girth welded in portable cleanroom in the field

1.2 m diameter - 3mm stainless50 km of weld

NO LEAKS !!

Page 8: LIGO I status and advanced LIGO proposalhiro/talks/G030672.pdfLIGO-G030672-00-E ICRR talk on Dec.9,2003 1 LIGO I status and advanced LIGO proposal Hiro Yamamoto LIGO Lab / Caltech

ICRR talk on Dec.9,2003 8LIGO-G030672-00-E

LIGO Vacuum Equipment

Page 9: LIGO I status and advanced LIGO proposalhiro/talks/G030672.pdfLIGO-G030672-00-E ICRR talk on Dec.9,2003 1 LIGO I status and advanced LIGO proposal Hiro Yamamoto LIGO Lab / Caltech

ICRR talk on Dec.9,2003 9LIGO-G030672-00-E

Seismic Isolation System

Tubular coil springs with internaldamping, layered between steelreaction masses

Isolation Performance

Page 10: LIGO I status and advanced LIGO proposalhiro/talks/G030672.pdfLIGO-G030672-00-E ICRR talk on Dec.9,2003 1 LIGO I status and advanced LIGO proposal Hiro Yamamoto LIGO Lab / Caltech

ICRR talk on Dec.9,2003 10LIGO-G030672-00-E

A LIGO Mirror

Substrates: SiO225 cm Diameter, 10 cm thick

Homogeneity < 5 x 10-7

Internal mode Q’s > 2 x 106

PolishingSurface uniformity < 1 nm rms

Radii of curvature matched < 3%

CoatingScatter < 50 ppm

Absorption < 0.5 ppmUniformity <10-3

Best mirrors are λ/6000 over the central 8 cm diameter

Page 11: LIGO I status and advanced LIGO proposalhiro/talks/G030672.pdfLIGO-G030672-00-E ICRR talk on Dec.9,2003 1 LIGO I status and advanced LIGO proposal Hiro Yamamoto LIGO Lab / Caltech

ICRR talk on Dec.9,2003 11LIGO-G030672-00-E

Core Opticsinstallation and alignment

Page 12: LIGO I status and advanced LIGO proposalhiro/talks/G030672.pdfLIGO-G030672-00-E ICRR talk on Dec.9,2003 1 LIGO I status and advanced LIGO proposal Hiro Yamamoto LIGO Lab / Caltech

ICRR talk on Dec.9,2003 12LIGO-G030672-00-E

LIGO Organization & Support

LIGO Laboratory

MIT + Caltech~170 people

LIGO Scientific Collaboration

44 member institutions> 400 scientists

U.S. National Science Foundation

UKGermany

JapanRussiaIndiaSpain

Australia

$

SCIENCEdata analysismonitor tool Detector

R&DDESIGN

CONSTRUCTIONOPERATION

Page 13: LIGO I status and advanced LIGO proposalhiro/talks/G030672.pdfLIGO-G030672-00-E ICRR talk on Dec.9,2003 1 LIGO I status and advanced LIGO proposal Hiro Yamamoto LIGO Lab / Caltech

ICRR talk on Dec.9,2003 13LIGO-G030672-00-E

Construction and related R&D costsPAC9 Dec.2000 by B.Barish

0

50

100

150

200

250

30095

-2

95-4

96-2

96-4

97-2

97-4

98-2

98-4

99-2

99-4

00-2

00-4

01-2

01-4

LIGO Quarter

$ M

illio

ns

Original Plan - $250M

Current Plan - $285M

Cooperative Agreement - $292M

Performance - $281M

Actuals Costs - $278M

Page 14: LIGO I status and advanced LIGO proposalhiro/talks/G030672.pdfLIGO-G030672-00-E ICRR talk on Dec.9,2003 1 LIGO I status and advanced LIGO proposal Hiro Yamamoto LIGO Lab / Caltech

ICRR talk on Dec.9,2003 14LIGO-G030672-00-E

0

5

10

15

20

25

30

35

40

FY 2001 FY 2002 FY 2003 FY 2004 FY 2005 FY 2006

$ M

illio

ns

Hardware to Support of LSC R&D

Increase for Ops R&D Support

Basic Operations

Increase for Full Operations

Basic Ops R&D Support

Advanced R&D

LIGO Budgets

FY 2001 funding normalized to 12 months shown for comparison

CurrentFunding

PAC11 Nov.2001 by B.Barish

Page 15: LIGO I status and advanced LIGO proposalhiro/talks/G030672.pdfLIGO-G030672-00-E ICRR talk on Dec.9,2003 1 LIGO I status and advanced LIGO proposal Hiro Yamamoto LIGO Lab / Caltech

ICRR talk on Dec.9,2003 15LIGO-G030672-00-E

LIGO Commissioning andScience Timeline

AnalyzedAnalysis in

Processincludes TAMA DT8

Data taking inProcess

includes TAMA DT9

Page 16: LIGO I status and advanced LIGO proposalhiro/talks/G030672.pdfLIGO-G030672-00-E ICRR talk on Dec.9,2003 1 LIGO I status and advanced LIGO proposal Hiro Yamamoto LIGO Lab / Caltech

ICRR talk on Dec.9,2003 16LIGO-G030672-00-E

Lock Acquisition- developed using simulation -

•Fast sensors monitorcirculating powers, RFsidebands in cavities•Sequencing codedigitally switchesfeedback state atproper transition times•Loop gains areactively scaled (everysample) to matchinstantaneous carrier& sideband buildups•Designed by MattEvans (PhD thesis)

Page 17: LIGO I status and advanced LIGO proposalhiro/talks/G030672.pdfLIGO-G030672-00-E ICRR talk on Dec.9,2003 1 LIGO I status and advanced LIGO proposal Hiro Yamamoto LIGO Lab / Caltech

ICRR talk on Dec.9,2003 17LIGO-G030672-00-E

What Limits Sensitivityof Interferometers?

• Seismic noise & vibrationlimit at low frequencies

• Atomic vibrations (ThermalNoise) inside componentslimit at mid frequencies

• Quantum nature of light(Shot Noise) limits at highfrequencies

• Myriad details of the lasers,electronics, etc., can makeproblems above these levels

Running at 10-7

Page 18: LIGO I status and advanced LIGO proposalhiro/talks/G030672.pdfLIGO-G030672-00-E ICRR talk on Dec.9,2003 1 LIGO I status and advanced LIGO proposal Hiro Yamamoto LIGO Lab / Caltech

ICRR talk on Dec.9,2003 18LIGO-G030672-00-E

S3: All 3 LIGO Interferometers atExtragalactic Sensitivity

Displacement spectral density

Page 19: LIGO I status and advanced LIGO proposalhiro/talks/G030672.pdfLIGO-G030672-00-E ICRR talk on Dec.9,2003 1 LIGO I status and advanced LIGO proposal Hiro Yamamoto LIGO Lab / Caltech

ICRR talk on Dec.9,2003 19LIGO-G030672-00-E

S2 -- L1 reaches Andromeda

M31 in Andromeda

Page 20: LIGO I status and advanced LIGO proposalhiro/talks/G030672.pdfLIGO-G030672-00-E ICRR talk on Dec.9,2003 1 LIGO I status and advanced LIGO proposal Hiro Yamamoto LIGO Lab / Caltech

ICRR talk on Dec.9,2003 20LIGO-G030672-00-E

3. Periodic sources3. Periodic sources

-- GEO-- L 2km-- H 4km-- L 4km

h

0

S1 sensitivities

Crab pulsar

h0: Amplitude detectable with 99%confidence during observation time T

Limit of detectability for rotating NSwith equatorial ellipticity, ε = δI/Izz:

10-3 , 10-4 , 10-5 @ 10 kpc

PSR J1939+2134P = 0.00155781 sfGW = 1283.86 Hz

P = 1.0519 10-19 s/sD = 3.6 kpc

.

Known EM pulsarsValues of h0 derived from

measured spin-down IF spin-down were entirely

attributable to GW emissions Rigorous astrophysical upper

limit from energy conservationarguments

Page 21: LIGO I status and advanced LIGO proposalhiro/talks/G030672.pdfLIGO-G030672-00-E ICRR talk on Dec.9,2003 1 LIGO I status and advanced LIGO proposal Hiro Yamamoto LIGO Lab / Caltech

ICRR talk on Dec.9,2003 21LIGO-G030672-00-E

Data analysis organizationLIGO Scientific Collaboration (LSC)

Data analysis is organized in four working groups organized by source type

• Unmodeled Signals -- SNe, GRBs, …» 1. Burst Group:

– Non-parametric techniques» Excess power in frequency-time domain» Excess amplitude change, rise-time in time domain

Deterministic Signals:» 2. Binary Inspiral Group» 3. Pulsars/CW Group

– Amplitude and frequency evolution parameterized– Set of templates covering parameter space matched to data

Statistical Signals» 4. Stochastic BG Group

– Cross-correlation of detector pairs, look for correlations above statistical variations

LIGO S1 author list includes more than 300 scientists and representing more than 30 institutions from the USA,Europe, and Asia.

Page 22: LIGO I status and advanced LIGO proposalhiro/talks/G030672.pdfLIGO-G030672-00-E ICRR talk on Dec.9,2003 1 LIGO I status and advanced LIGO proposal Hiro Yamamoto LIGO Lab / Caltech

ICRR talk on Dec.9,2003 22LIGO-G030672-00-E

Summary Science Run Metrics

75%

90%

90%

90%

DUTYFACTOR

7,000

14,000

14,000

BNSRANGE

(kpc)

GOAL ("SRD")

11%*22%24%3-way

DUTYFACTOR

BNSRANGE

(kpc)

DUTYFACTOR

BNSRANGE

(kpc)

DUTYFACTOR

BNSRANGE

(kpc)

IFO⇓

65%*

69%*

19%*

1,000

2,200

1,200

S3*

58%20073%~40H2

74%35059%~30H1

37%90043%~150L1

S2S1RUN⇒

*PRELIMINARY--RUN IN PROGRESS

Page 23: LIGO I status and advanced LIGO proposalhiro/talks/G030672.pdfLIGO-G030672-00-E ICRR talk on Dec.9,2003 1 LIGO I status and advanced LIGO proposal Hiro Yamamoto LIGO Lab / Caltech

ICRR talk on Dec.9,2003 23LIGO-G030672-00-E

What Next? From S3 to S4 + Stability & uptime

» Seismic retrofit at LLO ⇒ L1» Adapt WFS controls for radiation pressure torques» WFS bandwidth upgrade (wean off optical levers)» Possible wind noise mitigation for LHO

Sensitivity» Thermal compensation system (TCS) ⇒ H1 test» Higher effective laser power (power & sideband overlap)

– Laser & input optics efficiency improvement– Output mode cleaner (OMC) [possibly]

» Finish acoustic mitigation– Enclosures for other output ports– Relocate electronics racks remotely ⇒ L1 test

» Electronics cleanup: EMC upgrade ⇒ L1 test» Custom low-noise DAC's, other electronics upgrades

Page 24: LIGO I status and advanced LIGO proposalhiro/talks/G030672.pdfLIGO-G030672-00-E ICRR talk on Dec.9,2003 1 LIGO I status and advanced LIGO proposal Hiro Yamamoto LIGO Lab / Caltech

ICRR talk on Dec.9,2003 24LIGO-G030672-00-E

Advanced LIGOproposed in early 2003

Active Seismic

Multiple Suspensions

Sapphire Optics

Higher Power Laser

Silica Suspension

Dual recycling

Page 25: LIGO I status and advanced LIGO proposalhiro/talks/G030672.pdfLIGO-G030672-00-E ICRR talk on Dec.9,2003 1 LIGO I status and advanced LIGO proposal Hiro Yamamoto LIGO Lab / Caltech

ICRR talk on Dec.9,2003 25LIGO-G030672-00-E

Dual Recycling Interferometer

180 W LASER,MODULATION SYSTEM

40 KG SAPPHIRETEST MASSES

QUAD SILICASUSPENSION

PRM Power Recycling MirrorBS Beam SplitterITM Input Test MassETM End Test MassSRM Signal Recycling MirrorPD Photodiode

Page 26: LIGO I status and advanced LIGO proposalhiro/talks/G030672.pdfLIGO-G030672-00-E ICRR talk on Dec.9,2003 1 LIGO I status and advanced LIGO proposal Hiro Yamamoto LIGO Lab / Caltech

ICRR talk on Dec.9,2003 26LIGO-G030672-00-E

101 102 10310-24

10-23

10-22

Frequency (Hz)

Strain Noise,

h(f)

/Hz1/2

10 Hz 100 Hz 1 kHz

10-22

10-23

10-24

10-21

Anatomy of the projectedAdvanced LIGO detector performance

Newtonian background,estimate for LIGO sites

Seismic ‘cutoff’ at 10 Hz

Suspension thermal noise

Test mass thermal noise

Unified quantum noisedominates atmost frequencies for fullpower, broadband tuning

Advanced LIGO's Fabry-Perot Michelson Interferometer is flexible – can tailor towhat we learn before and after we bring it on line, to the limits of this topology

Initial LIGO

Advanced LIGO

Page 27: LIGO I status and advanced LIGO proposalhiro/talks/G030672.pdfLIGO-G030672-00-E ICRR talk on Dec.9,2003 1 LIGO I status and advanced LIGO proposal Hiro Yamamoto LIGO Lab / Caltech

ICRR talk on Dec.9,2003 27LIGO-G030672-00-E

Initial and Advanced LIGO

Factor 10 better amplitudesensitivity

» (Reach)3 = rate Factor 4 lower frequency

bound NS Binaries: for three

interferometers,» Initial LIGO: ~20 Mpc» Adv LIGO: ~350 Mpc

BH Binaries:» Initial LIGO: 10 Mo, 100 Mpc» Adv LIGO : 50 Mo, z=2

Stochastic background:» Initial LIGO: ~3e-6» Adv LIGO ~3e-9

Page 28: LIGO I status and advanced LIGO proposalhiro/talks/G030672.pdfLIGO-G030672-00-E ICRR talk on Dec.9,2003 1 LIGO I status and advanced LIGO proposal Hiro Yamamoto LIGO Lab / Caltech

ICRR talk on Dec.9,2003 28LIGO-G030672-00-E

Baseline planLIGO(122M$)&LSC[UK(11.5),Germany(11.5),Australia(2.5)]

Initial LIGO Observation at design sensitivity 2004 – 2006» Significant observation within LIGO Observatory» Significant networked observation with GEO, VIRGO, TAMA

Structured R&D program to develop technologies» Conceptual design developed by LSC in 1998» Cooperative Agreement carries R&D to Final Design

2003: Proposal for fabrication, installation» NSF considering proposal and timeline

Proposal calls for project start in 2005» Sapphire Test Mass material, seismic isolation fabrication long leads» Prepare a ‘stock’ of equipment for minimum downtime, rapid installation

Start installation in 2007» Baseline is a staggered installation, Livingston and then Hanford

Coincident observations by 2010» At an advanced level of commissioning

Page 29: LIGO I status and advanced LIGO proposalhiro/talks/G030672.pdfLIGO-G030672-00-E ICRR talk on Dec.9,2003 1 LIGO I status and advanced LIGO proposal Hiro Yamamoto LIGO Lab / Caltech

ICRR talk on Dec.9,2003 29LIGO-G030672-00-E

Sensing for Advanced LIGO Build on initial LIGO layout –

» retain Fabry-Perot cavities, power recycling Increase the laser power to a practical limit to lower shot noise

» Laser power – require TEM00, stability in frequency and intensity» Absorption in optics – state-of-the-art substrates and coatings, compensation system

to correct for focussing» ~180 W input power is the practical optimum for Advanced LIGO» Leads to ~0.8 MW in cavities (6cm radius beams, though)» Significant motion due to photon pressure – quantum limited!

Modify optical layout: Add signal recycling mirror» Gives resonance for signal frequencies –

can be used to optimize response» Couples photon shot noise and

backreaction – some squeezing of light Laser

Page 30: LIGO I status and advanced LIGO proposalhiro/talks/G030672.pdfLIGO-G030672-00-E ICRR talk on Dec.9,2003 1 LIGO I status and advanced LIGO proposal Hiro Yamamoto LIGO Lab / Caltech

ICRR talk on Dec.9,2003 30LIGO-G030672-00-E

Managing Stray forcesin Advanced LIGO

Seismic Isolation: use servo-control techniques and low-noise seismometersto ‘slave’ optics platform to inertial space

» Decreases motion in the gravitational-wave band to a negligible level» Decreases motion in ‘controls’ band, moving forces away from test mass

Suspension thermal noise: all-silica fiber construction» Intrinsically low-loss material» Welded and ‘contacted’ construction also very low loss

Substrate thermal noise: use monolithic Sapphire» High Young’s modulus» Low mechanical loss» (fallback: very low-loss silica)

Optical coating thermal noise: develop low-loss materials and techniques» Area of active development

Page 31: LIGO I status and advanced LIGO proposalhiro/talks/G030672.pdfLIGO-G030672-00-E ICRR talk on Dec.9,2003 1 LIGO I status and advanced LIGO proposal Hiro Yamamoto LIGO Lab / Caltech

ICRR talk on Dec.9,2003 31LIGO-G030672-00-E

Advanced LIGO R&D LIGO with LSC(LIGO Scientific Collaboration) making good progress

Laser: in 2003,» selected baseline power head design,» supported prototyping of design, observe >1/2 final power goal in _ of system.» Demonstrated intensity stabilization to requirements at 40 Hz and higher, within factor of 5 at most

stringent frequency (10 Hz) Substrates: in 2003,

» Received full-size 40 kg, 32 cm diameter sapphire substrates» Found mechanical losses in these substrates to meet requirements» Characterized absorption in these substrates, supported successful annealing techniques on

smaller pieces to reduce absorption – scaling up now» New high Q measurements of small (200e6) and LIGO-sized (120e6) of fused silica; supported

annealing on small pieces to reduce mechanical losses – scaling up now Coatings, in 2003,

» Refined models for coating thermal noise» Observed coating thermal noise in two experiments, consistent with theory» Measured and supported measurements of mechanical losses on trial coatings» Developed strategy for coating development, put plan into motion

Page 32: LIGO I status and advanced LIGO proposalhiro/talks/G030672.pdfLIGO-G030672-00-E ICRR talk on Dec.9,2003 1 LIGO I status and advanced LIGO proposal Hiro Yamamoto LIGO Lab / Caltech

ICRR talk on Dec.9,2003 32LIGO-G030672-00-E

Summary report of theNSF review on advanced LIGO

Advanced LIGO will provide the capability to observe a variety ofastrophysical phenomena including inspiral events, continuous-wave sources, bursts, and stochastic backgrounds.  Achievementof the design strain sensitivity (more than a factor of ten beyondInitial LIGO) is feasible and detection of events is plausible. Detection of any source would be a dramatic direct confirmation ofthe existence of gravitational waves and would have exciting andwide-ranging implications for gravitational physics, astrophysics,and our understanding of the universe.

The committee agrees that the current state of the proposedproject is at a sufficiently mature level that the process leading toconstruction should proceed.  Although technical challengesremain, the plan for solving the technical problems appears soundand no major obstacles have been identified that would justifydelaying the construction of Advanced LIGO.