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Future LIGO Interferometers

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

By jacob
(280 views)

The Evolution and Outflows of Hyper-Accreting Disks

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

By caitlyn
(140 views)

Astrophysical tests of general relativity in the strong-field regime

Astrophysical tests of general relativity in the strong-field regime

Astrophysical tests of general relativity in the strong-field regime. Emanuele Berti , University of Mississippi/Caltech Texas Symposium, São Paulo, Dec 18 2012. What are “strong field ” tests? Alternatives to GR: massive scalars BH dynamics and superradiance

By melia
(127 views)

Background: simulation of merging black holes by Werner Berger

Background: simulation of merging black holes by Werner Berger

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

By iniko
(71 views)

Setting the Stage Dave Reitze LIGO Laboratory

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:

By bob
(155 views)

GW Memory from GRB Jets a possible DECIGO source

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.

By amanda
(114 views)

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

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

Advanced LIGO R&D Review Input Optics Peter King for the University of Florida (Dave Reitze, David Tanner, …) October 8, 2002. Current Status. Design Requirements Review (DRR) held May 2002 results obtained for high power Faraday isolator > 45 dB isolation achieved

By maris
(109 views)

Planning and Implementation Strategy for Advanced LIGO

Planning and Implementation Strategy for Advanced LIGO

Planning and Implementation Strategy for Advanced LIGO. Gary Sanders LSC Meeting Hanford, August 14, 2001. Ancient History. 1997 – 1998 Lab and LSC R&D Proposals Advanced R&D funding initiated by NSF November 1998 LSC White Paper

By wyanet
(90 views)

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

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.

By mandel
(118 views)

GEO600 Data Analysis Status

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).

By darva
(120 views)

Squeezed Light Techniques for Gravitational Wave Detection

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.

By jesse
(116 views)

What science can initial LIGO do with pulsars?

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

By kendall
(118 views)

Thermal Headaches in Advanced LIGO Input Optics

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

By marty
(129 views)

One Arm Cavity

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.

By hop
(165 views)

Thermal noise from optical coatings

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.

By hamlet
(130 views)

Advanced LIGO Update David Shoemaker LSC LHO August 2004

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

By aderyn
(149 views)

Status of LIGO

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.

By clara
(197 views)

ADVANCED LIGO SCIENCE

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

By rodney
(116 views)

Is there a future for LIGO underground?

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.

By pisces
(130 views)

Gravitational Wave Detection – current status & future prospects

Gravitational Wave Detection – current status & future prospects

Gravitational Wave Detection – current status & future prospects. Jonathan Gair. Extragalactic Group Seminar, IoA, 21 st November 2005. Gravitational Waves. Fluctuations in spacetime curvature, generated by rapidly accelerating masses.

By derex
(161 views)

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