'Advanced ligo' presentation slideshows

The Evolution and Outflows of Hyper-Accreting Disks

The Evolution and Outflows of Hyper-Accreting Disks. Brian Metzger, UC Berkeley. with Tony Piro, Eliot Quataert & Todd Thompson. Metzger, Thompson & Quataert (2007), ApJ, 659, 561 Metzger, Quataert & Thompson (2008), MNRAS, 385, 1455 Metzger, Thompson & Quataert (2008), ApJ, 676, 1130

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Squeezed Light Techniques for Gravitational Wave Detection

Squeezed Light Techniques for Gravitational Wave Detection. July 6, 2012 Daniel Sigg LIGO Hanford Observatory Seminar at TIFR, Mumbai, India. Abstract.

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Future LIGO Interferometers

Future LIGO Interferometers. Moriond 07 La Thuille, Italy. Rana Adhikari Caltech. Advanced LIGO. LIGO mission: detect gravitational waves and initiate GW astronomy Next detector Should have assured detectability of known sources

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One Arm Cavity

One Arm Cavity. QUAD. M0. TRIPLE. L1. M0. L1. L2. 16m. L2. TM. R = ?, T=1%. R = 20m, T=1%. Optimally coupled cavity (no mode matched light reflected back) Finesse ~ 625. Goals. QUAD TESTING: Electrostatic Drive (ESD) Hierarchical Control Lock Acquisition. ESDs.

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Is there a future for LIGO underground?

Is there a future for LIGO underground?. Fred Raab, LIGO Hanford Observatory. Basic Signature of Gravitational Waves for All Detectors. Different Frequency Bands of Laser-Based Detectors and Sources. space. terrestrial. Audio band.

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Status of LIGO

LIGO-G040540-00-E. Status of LIGO. Peter Shawhan (LIGO Laboratory / Caltech) Gravitational Wave Data Analysis Workshop December 15, 2004 Annecy, France Thanks to Rana Adhikari and David Shoemaker. The LIGO Observatories.

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372 views • 19 slides

Astrophysical tests of general relativity in the strong-field regime

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ADVANCED LIGO SCIENCE

ADVANCED LIGO SCIENCE. Kip S. Thorne CaRT, California Institute of Technology NSF Advanced R&D Panel - 29 January 2001. 300 in h ~10 7 in rate. h rms = h(f) ?f ?10 h(f). Open up wider band. 15 in h ~3000 in rate. From Initial Interferometers to Advanced. Most Optimistic Source

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What science can initial LIGO do with pulsars?

What science can initial LIGO do with pulsars?. Ben Owen. Detections or upper limits. Owen in Amaldi. New emission mechanisms Magnetic mountains Magnetic bottling Mountains all the way down Types of searches Known pulsars (radio) Low-mass x-ray binaries X-ray point sources

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Setting the Stage Dave Reitze LIGO Laboratory

GWADW: Gravitational Wave Detectors for 2015, 2020, and 2025. Setting the Stage Dave Reitze LIGO Laboratory. http://surfing-place.blogspot.com/2011/06/hawaii.html. Ground- based Detectors-- Past, Present, & Future. 2010 -- First Generation Interferometers:

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Thermal Headaches in Advanced LIGO Input Optics

Thermal Headaches in Advanced LIGO Input Optics Guido Mueller, Rupal Amin, David Guagliardo, David Tanner, and David Reitze Physics Department University of Florida Gainesville, FL. LIGO-G010130-00-Z. Input Optics Functions. RF Modulation Mode Cleaning Mode Matching Optical Isolation

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Thermal noise from optical coatings

Thermal noise from optical coatings. Gregory Harry Massachusetts Institute of Technology - on behalf of the LIGO Science Collaboration -. 25 July 2003 10 th Marcel Grossman Meeting Rio de Janeiro, Brazil. LIGO-G030337-00-R. Yuri Levin's Theorem.

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GW Memory from GRB Jets a possible DECIGO source

Ofek Birnholtz, Tsvi Piran Racah Institute of Physics, Hebrew University of Jerusalem arXiv:1302.5713v2 , submitted to PRD Yukawa International Seminar Yukawa Institute for Theoretical Physics Kyoto, Japan, 3.6.2013. GW Memory from GRB Jets a possible DECIGO source.

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Advanced LIGO Update David Shoemaker LSC LHO August 2004

Advanced LIGO Update David Shoemaker LSC LHO August 2004. Advanced LIGO. If you have been on Mars... ~Factor 10 in amplitude sensitivity ~Factor 4 lower frequency Tunable Recombined Fabry-Perot Michelson Signal recycling ~20x higher input power 40 kg masses Fused silica suspension

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A RTP crystal electro-optic modulator for next generation gravitational wave detector

A RTP crystal electro-optic modulator for next generation gravitational wave detector. Wan Wu, Volker Quetschke, Ira Thorpe, Guido Mueller, David Reitze, and David Tanner LIGO-G070243-00-Z. Physics Department University of Florida Gainesville, FL.

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Planning and Implementation Strategy for Advanced LIGO

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GEO600 Data Analysis Status

GEO600 Data Analysis Status. Bernard Schutz Albert Einstein Institute Potsdam/Golm. GEO Participation in Science Runs. GEO participated fully in S1, LSC analysis essentially finished. Two LSC working group co-chairs are GEO members: MA Papa (pulsar searches), J Romano (stochastic).

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Advanced LIGO R&D Review Input Optics Peter King for the University of Florida

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Background: simulation of merging black holes by Werner Berger

Gravitational Waves and LIGO Tiffany Summerscales, Dept. of Physics. What are gravitational waves?

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