![Page 1: Five long and independent baselines: Better SNR and much better directional resolution](https://reader035.vdocument.in/reader035/viewer/2022062500/56814f7e550346895dbd2e4f/html5/thumbnails/1.jpg)
Proposal to extend current AIGO High Optical Power research facility to a 5km advanced interferometer.
D G Blair on behalf of ACIGA
LIGO-G060284-00-Z
![Page 2: Five long and independent baselines: Better SNR and much better directional resolution](https://reader035.vdocument.in/reader035/viewer/2022062500/56814f7e550346895dbd2e4f/html5/thumbnails/2.jpg)
Five long and independent baselines:
Better SNR and much better directional resolution
![Page 3: Five long and independent baselines: Better SNR and much better directional resolution](https://reader035.vdocument.in/reader035/viewer/2022062500/56814f7e550346895dbd2e4f/html5/thumbnails/3.jpg)
Why is AIGO necessary
• Increased angular resolution :– average x 4– sometimes much more
• Coherent array analysis– increases the number of detectable sources x ~2
• Reduced Accidental coincidences– reduces as number of independent baselines to power N
Pacc ~t
c
R c N
![Page 4: Five long and independent baselines: Better SNR and much better directional resolution](https://reader035.vdocument.in/reader035/viewer/2022062500/56814f7e550346895dbd2e4f/html5/thumbnails/4.jpg)
Improved angular resolution with AIGO
• LIGO and VIRGO •LIGO, VIRGO and AIGO
![Page 5: Five long and independent baselines: Better SNR and much better directional resolution](https://reader035.vdocument.in/reader035/viewer/2022062500/56814f7e550346895dbd2e4f/html5/thumbnails/5.jpg)
QuickTime™ and aTIFF (Uncompressed) decompressor
are needed to see this picture.
![Page 6: Five long and independent baselines: Better SNR and much better directional resolution](https://reader035.vdocument.in/reader035/viewer/2022062500/56814f7e550346895dbd2e4f/html5/thumbnails/6.jpg)
QuickTime™ and aTIFF (Uncompressed) decompressor
are needed to see this picture.
![Page 7: Five long and independent baselines: Better SNR and much better directional resolution](https://reader035.vdocument.in/reader035/viewer/2022062500/56814f7e550346895dbd2e4f/html5/thumbnails/7.jpg)
The Process So Far• Gingin facility development 2000-2005• Western Australia funds Centre of Excellence for
gravitational astronomy 2005• AIGO Planning meeting Oct 2005: concept for
reduced pipe diameter.• WA Govt forms Steering Committee for AIGO
Nov 2005.• International Letter Writing Nov 2005…thanks!!• UWA and State Govt fund prospectus document
Dec 2005 and planning process May 2006.• ACIGA costing and planning:(LIGO support
through Adv LIGO review) May 2006.
![Page 8: Five long and independent baselines: Better SNR and much better directional resolution](https://reader035.vdocument.in/reader035/viewer/2022062500/56814f7e550346895dbd2e4f/html5/thumbnails/8.jpg)
![Page 9: Five long and independent baselines: Better SNR and much better directional resolution](https://reader035.vdocument.in/reader035/viewer/2022062500/56814f7e550346895dbd2e4f/html5/thumbnails/9.jpg)
![Page 10: Five long and independent baselines: Better SNR and much better directional resolution](https://reader035.vdocument.in/reader035/viewer/2022062500/56814f7e550346895dbd2e4f/html5/thumbnails/10.jpg)
Gingin facility Investment
• Clean rooms and assembly facilities
• Vacuum system and vacuum automation
• High optical power laser facilities
• Seismic surveying demonstrating excellent seismic attenuation.
• Roads and power infrastructure.
• Total investment so far ~ $20M
![Page 11: Five long and independent baselines: Better SNR and much better directional resolution](https://reader035.vdocument.in/reader035/viewer/2022062500/56814f7e550346895dbd2e4f/html5/thumbnails/11.jpg)
AIGO Concept
• AIGO: I for International• An Advanced detector built using maximum
knowhow, support and contribution from northern hemisphere detectors.
• A detector planned and advised internationally.• Utilising the best aspects of all detectors built to
date, combined with certain innovative features.• A detector that will feed data directly into the
international data analysis grid.
![Page 12: Five long and independent baselines: Better SNR and much better directional resolution](https://reader035.vdocument.in/reader035/viewer/2022062500/56814f7e550346895dbd2e4f/html5/thumbnails/12.jpg)
![Page 13: Five long and independent baselines: Better SNR and much better directional resolution](https://reader035.vdocument.in/reader035/viewer/2022062500/56814f7e550346895dbd2e4f/html5/thumbnails/13.jpg)
AIGO Realities
• Funds ~ $40m thought to be possible in Australia• Funds ~$10m available soon for pipe infrastructure.• Substantial data analysis effort funded separately.• Can we build an advanced detector for such a small
sum?• Not without international support
– Control systems
– Designs
– Monitoring
– Expertise in many areas
– Advisory committees
![Page 14: Five long and independent baselines: Better SNR and much better directional resolution](https://reader035.vdocument.in/reader035/viewer/2022062500/56814f7e550346895dbd2e4f/html5/thumbnails/14.jpg)
AIGO Preliminary Concept• 5km, 700mm diameter vacuum pipe (de Salvo)• keyhole welding, precision weld monitoring (CSIRO)• on site fabrication of pipe in long lengths (Duraduct)• spiral band saw baffle fabricated with pipe.(de
Salvo,Duraduct)• Low mass enclosure, solar bakeout. (VACUUM 44: 2,151-154 ( 1993)).
![Page 15: Five long and independent baselines: Better SNR and much better directional resolution](https://reader035.vdocument.in/reader035/viewer/2022062500/56814f7e550346895dbd2e4f/html5/thumbnails/15.jpg)
Light Scattering Noise (Takahashi)
• Modelling based on R Takahashi et al PRD 70,06,2003
• Number of effective baffles N:h=height of baffle,d=baffle spacing
N h
d
L
R
Spiral baffle represents significant overkill
![Page 16: Five long and independent baselines: Better SNR and much better directional resolution](https://reader035.vdocument.in/reader035/viewer/2022062500/56814f7e550346895dbd2e4f/html5/thumbnails/16.jpg)
Why 5km
• Arm length dilutes test mass thermal noise.
• Thermal noise penalty for parametric instability suppression by ring damping.
• Adv LIGO proposed performance can be regained with extra arm length.
![Page 17: Five long and independent baselines: Better SNR and much better directional resolution](https://reader035.vdocument.in/reader035/viewer/2022062500/56814f7e550346895dbd2e4f/html5/thumbnails/17.jpg)
Strong Thermal Lensing
Observation and compensation (PRL accepted 2006)
![Page 18: Five long and independent baselines: Better SNR and much better directional resolution](https://reader035.vdocument.in/reader035/viewer/2022062500/56814f7e550346895dbd2e4f/html5/thumbnails/18.jpg)
Parametric Instability (PRL2005)
Stabilisation requires ring damping: extra thermal noise. (see Ju Li’s talk)
![Page 19: Five long and independent baselines: Better SNR and much better directional resolution](https://reader035.vdocument.in/reader035/viewer/2022062500/56814f7e550346895dbd2e4f/html5/thumbnails/19.jpg)
![Page 20: Five long and independent baselines: Better SNR and much better directional resolution](https://reader035.vdocument.in/reader035/viewer/2022062500/56814f7e550346895dbd2e4f/html5/thumbnails/20.jpg)
Consortium
About 70 people
7 AustralianUniversities
2 CSIRO Institutes
2 Companies
![Page 21: Five long and independent baselines: Better SNR and much better directional resolution](https://reader035.vdocument.in/reader035/viewer/2022062500/56814f7e550346895dbd2e4f/html5/thumbnails/21.jpg)
Conclusion
• AIGO offers significant benefit to existing terrestrial detectors.
• Natural next step for world network.
• Can be achieved over next 8 years with community support.
• We would like to sign MOUs with organisations such as VESF
![Page 22: Five long and independent baselines: Better SNR and much better directional resolution](https://reader035.vdocument.in/reader035/viewer/2022062500/56814f7e550346895dbd2e4f/html5/thumbnails/22.jpg)
Thermal Gradient: Jerome Degallaix
Cavity Waist Position
Thermal compensation
Heat the compensation plateInput Test Mass
R1 =
![Page 23: Five long and independent baselines: Better SNR and much better directional resolution](https://reader035.vdocument.in/reader035/viewer/2022062500/56814f7e550346895dbd2e4f/html5/thumbnails/23.jpg)
Demonstrated Thermal Compensation
![Page 24: Five long and independent baselines: Better SNR and much better directional resolution](https://reader035.vdocument.in/reader035/viewer/2022062500/56814f7e550346895dbd2e4f/html5/thumbnails/24.jpg)
0.1
1
10
100
718 719 720 721 722
Radius of Curvature (m)
Max
imum
R o
f all
acou
stic
m
odes
Gingin prediction, Fused Silica
![Page 25: Five long and independent baselines: Better SNR and much better directional resolution](https://reader035.vdocument.in/reader035/viewer/2022062500/56814f7e550346895dbd2e4f/html5/thumbnails/25.jpg)
0.1
1
10
100
718 719 720 721 722
Radius of Curvature (m)
Max
imum
R o
f all
acou
stic
mod
esGingin prediction, Sapphire
![Page 26: Five long and independent baselines: Better SNR and much better directional resolution](https://reader035.vdocument.in/reader035/viewer/2022062500/56814f7e550346895dbd2e4f/html5/thumbnails/26.jpg)
![Page 27: Five long and independent baselines: Better SNR and much better directional resolution](https://reader035.vdocument.in/reader035/viewer/2022062500/56814f7e550346895dbd2e4f/html5/thumbnails/27.jpg)
QuickTime™ and aTIFF (LZW) decompressor
are needed to see this picture.
![Page 28: Five long and independent baselines: Better SNR and much better directional resolution](https://reader035.vdocument.in/reader035/viewer/2022062500/56814f7e550346895dbd2e4f/html5/thumbnails/28.jpg)
Astro-ph/061275Short GRB and binary black hole standard sirens as a probe of dark energy
Authors: Neal Dalal (CITA), Daniel E. Holz (LANL and U. Chicago), Scott A. Hughes (MIT), Bhuvnesh Jain (U. Penn.)
Comments: 8 pages, submitted to PRD
Short gamma-ray bursts, if produced by merging neutron star binaries, would be standard sirens with known redshifts detectable by ground-based GW networks such as LIGO-II, Virgo, and AIGO. Depending upon the collimation of these GRBs, a single year of observation of their gravitational waves can measure the Hubble constant to about 2%. When combined with measurement of the absolute distance to the last scattering surface of the cosmic microwave background, this determines the dark energy equation of state parameter w to 9%.
![Page 29: Five long and independent baselines: Better SNR and much better directional resolution](https://reader035.vdocument.in/reader035/viewer/2022062500/56814f7e550346895dbd2e4f/html5/thumbnails/29.jpg)
QuickTime™ and aTIFF (LZW) decompressor
are needed to see this picture.