'Pulsar timing' diaporamas de présentation

Observing Vela With XDM The First Year

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PTA and GW detection --- Lecture

PTA and GW detection --- Lecture. K. J. Lee ( ??? ) Max-Planck Institute for Radio astronomy kjlee007@gmail.com Aug. 2013. Outline. Pulsar timing array Basic physics about GW Pulsar timing response to GW Detect GW background Detect single source Practical aspects of pulsar timing array

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PTA and GW detection --- Lecture

PTA and GW detection --- Lecture. K. J. Lee ( ??? ) Max-Planck Institute for Radio astronomy kjlee007@gmail.com Aug. 2013. Outline. Pulsar timing array Basic physics about GW Pulsar timing response to GW Detect GW background Detect single source Practical aspects of pulsar timing array

722 views • 49 slides

The timing behaviour of radio pulsars

The timing behaviour of radio pulsars. George Hobbs Australia Telescope National Facility george.hobbs@csiro.au. Contents. Radio pulsars Pulsar timing A few things that you can do with pulsar timing Young pulsars - a new (predictive?) model for timing noise

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Pulsar, Gravitational wave, Gravitational wave polarization

Pulsar, Gravitational wave, Gravitational wave polarization. K.J.Lee Jul. 2009 NAOC. Outline. Gravity theory, Spacetime geometry Gravitational Wave and its polarization Pulsar, Pulsar timing signal Detect G-wave using pulsar Present uplimit Can we say GR is correct?.

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The timing behaviour of radio pulsars

The timing behaviour of radio pulsars. George Hobbs Australia Telescope National Facility george.hobbs@csiro.au. Contents. Radio pulsars Pulsar timing A few things that you can do with pulsar timing Young pulsars - a new (predictive?) model for timing noise

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Exoplanets Searching for New Worlds Larry Morgan

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Pulsar timing with tempo2

Pulsar timing with tempo2. George Hobbs Australia Telescope National Facility george.hobbs@csiro.au. Contents. Basis of pulsar timing Getting tempo2 Using tempo2 Developing tempo2. Must average many thousands of pulses together to obtain stable profile.

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Present and future of pulsar research: the Italian contribute

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Gravitational Wave Detection Using Pulsar Timing Current Status and Future Progress

Gravitational Wave Detection Using Pulsar Timing Current Status and Future Progress. Fredrick A. Jenet Center for Gravitational Wave Astronomy University of Texas at Brownsville. Dick Manchester ATNF/CSIRO Australia. George Hobbs ATNF/CSIRO Australia. KJ Lee Peking U. China.

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Detecting Gravitational Waves with Pulsars

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The Parkes Pulsar Timing Array Project

The Parkes Pulsar Timing Array Project. R. N. Manchester. Australia Telescope National Facility, CSIRO Sydney Australia. Summary. Brief introduction to pulsars and pulsar timing Gravitational waves and pulsars The Parkes Pulsar Timing Array project. Pulsar Origins.

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30 YEARS OF COSMIC STRINGS

30 YEARS OF COSMIC STRINGS. Alex Vilenkin. Tufts Institute of Cosmology. 30 YEARS OF COSMIC STRINGS. String evolution. FOCUS ON:. Detection (bounds). 30 YEARS OF COSMIC STRINGS. LEAVE OUT:. Superconducting strings Vortons Semilocal strings String formation Strings in GUTs

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Pulsar Timing Phenomenology

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SKADS Science Overview

SKADS Science Overview. SKADS Science Overview. SKA Science Case SKADS Science Interactions. Strong Field Tests of Gravity. Binary orbit permits determination of masses. Relativistic effects permit (re) determination of masses. ALL MUST AGREE. http://www.jb.man.ac.uk/~pulsar/.

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Gravitational Wave and Pulsar Timing

Gravitational Wave and Pulsar Timing. Xiaopeng You , Jinlin Han, Dick Manchester National Astronomical Observatories, Chinese Academy of Sciences. Outline. Gravitational Wave Physics of gravitational waves Gravitational wave detection Gravitational wave sources

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Low Frequency Observations of the ISM and Pulsar Timing

Low Frequency Observations of the ISM and Pulsar Timing. Joris Verbiest. Swinburne University & ATNF, Australia. Xiaopeng You (Southwest University, China) William Coles (UCSD) George Hobbs (ATNF) PPTA team. Outline. Brief intro to PPTA DM variations and the turbulent ISM

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Determining orbits from radial velocities

Determining orbits from radial velocities. Observe system over n times (observations) n observations n (V r , t) V = F(K,e, w,g ,T,P) since T,P enter expression for V via q , from time of observation t, estimates or known values of P,e,T, hence E (ecc. anomoly) Thus:

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GLAST Large Area Telescope High-Energy Multiwavelength Activities: An Invitation

GLAST Large Area Telescope High-Energy Multiwavelength Activities: An Invitation. GLAST LAT. opacity t for source at z. g -ray energy (GeV). opaque. Salamon and Stecker, 1998. No significant attenuation below 10 GeV. K. S. Wood (NRL), D. J. Thompson (GSFC), R. A. Cameron (SLAC),

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Data analysis and Results

Pulsars Timing with the Nanshan Radio Telescope J. P. Yuan, N. Wang, Z. Y. Liu Xinjiang Astronomical Observatory, CAS na.wang@xao.ac.cn.

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