The Milky Way, Schroedinger’s Cat, and You. Galaxies, the Building Blocks of the Universe. Raja Guha Thakurta (in collaboration with Sandra Faber) UCO/Lick Observatory University of California at Santa Cruz.

ByImagining the Future. What can we do about the Quantum Noise Limit in Gravitational-wave Detectors?. Nergis Mavalvala Penn State October 2004. Quantum Noise in Optical Measurements. Measurement process Interaction of light with test mass Counting signal photons with a photodetector

By9 May 2014 AKPA meeting , University of Chicago Yannis K. Semertzidis. C enter for A xion and P recision P hysics. CAPP : a completely new IBS center at the KAIST campus. Strong CP-problem Axion dark-matter experiment ; solar axions Proton Electric Dipole Moment experiment

ByLaser Interferometer Gravitational-wave Detectors: Advancing toward a Global Network. Stan Whitcomb LIGO/Caltech ICGC, Goa, 18 December 2011. LIGO-G1101272-v1. Outline. The Challenge of GW Detection What has been accomplished? What comes next? A peek at Results from First G eneration

ByQuantum Noise. Michael A. Nielsen University of Queensland. Goals: To introduce a tool – the density matrix – that is used to describe noise in quantum systems, and to give some examples. Density matrices. Generalization of the quantum state used to describe noisy quantum systems.

ByWideband, Next Gen, Gravitational-Wave Antennae. APS - Atlanta - April - 2012 Rana Adhikari Caltech. OUTLINE. Gravitational Waves and the Past The LIGO Detectors The Global Network and the Indian Possibility The Future of GW Detectors & Observations. GW Sources in LIGO Band 50-1000 Hz.

ByThe noise spectra of mesoscopic structures. Eitan Rothstein With Amnon Aharony and Ora Entin. 22.09.10. University of Latvia, Riga, Latvia. The desert in Israel. Outline. Introduction to mesoscopic physics Introduction to noise The scattering matrix formalism

ByBME5002 Image Processing Lecture 1 John G. Harris 1/26/01. Image Processing Goals. Improve image quality Image enhancement Feature extraction Computer-aided diagnosis Required for image formation for some modalities (CT, MRI, etc.). Aspects of Image Quality. Contrast vs. dynamic range

ByQuantum Noise. Michael A. Nielsen University of Queensland. Goals: To introduce a tool – the density matrix – that is used to describe noise in quantum systems, and to give some examples. Density matrices. Generalization of the quantum state used to describe noisy quantum systems.

ByQuantum Noise. Michael A. Nielsen University of Queensland. Goals: To introduce a tool – the density matrix – that is used to describe noise in quantum systems, and to give some examples. Density matrices. Generalization of the quantum state used to describe noisy quantum systems.

ByQuantum Noise Spectrum of QND RSE Using Mod-Demod Scheme. LSC Meeting 2001 Aug. K.Somiya. Abstract. Detuned RSE can beat SQL because of optical spring as is shown by A. Buonanno and Y. Chen (2001). It can beat SQL even without homodyne detection ,

ByFundamental Sensitivity Limits for Coherent and Direct Detection. Jonas Zmuidzinas Caltech. Coherent vs. Direct Detection. MKID Day et al., 2003. Coherent amplification using ideal maser/laser Gain and noise are optimized when energy level populations are perfectly inverted

ByAdvanced LIGO Sensing and Control Readout schemes for Advanced LIGO. K.A. Strain University of Glasgow G030076 & G030077. Contents. R&D progress Sensing for control Sensing for GW readout Control issues Options and timescale. R&D Progress. Three step program

ByDeci-hertz Interferometer Gravitational Wave Observatory (DECIGO). 7th Gravitational Wave Data Analysis Workshop December 17, 2002 @ International Institute for Advanced Studies, Japan Seiji Kawamura National Astronomical Observatory of Japan. Contents. Introduction What is DECIGO ?

ByRochester Institute of Technology -Proposal to join the LSC-. Shally Saraf Rochester Institute of Technology Quantum Electronics Group (RITQEG). LIGO-G060437-00-Z. August 15, 2006. Who is RITQEG?. Shally Saraf - Part of LSC since 1999

ByGround-based GW interferometers in the LISA epoch. David Shoemaker MIT LIGO 20 July 02. Points of departure. LISA will join the network of ground-based detectors ~2011, with a 10-year lifetime What will the interferometric detector ground network look like at this time?

ByDECIGO – Japanese Space Gravitational Wave Detector. International Workshop on GPS Meteorology January 17, 2003 @ Tsukuba Center for Institutes Seiji Kawamura* and DECIGO-WG (*) National Astronomical Observatory of Japan. What is Gravitational Wave?.

ByQuantum Noise in (High-Gain) FELs. Kwang -Je Kim Argonne National Laboratory March 8, 2012 Future Light Sources WS Jefferson Laboratory Newport News, VA. EM Field Operator. Complex field amplitude operator ( Hermitian conjugate) Intensity = ,

ByBeyond The Standard Quantum Limit. B. W. Barr Institute for Gravitational Research University of Glasgow. Standard Quantum Limit?. Heisenberg Uncertainty principal for position-momentum. (min).

ByStrongly Correlated Systems of Cold Atoms Detection of many-body quantum phases by measuring correlation functions. Anatoli Polkovnikov Boston University Ehud Altman Weizmann Vladimir Gritsev Harvard

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