Pulsar timing with tempo2 George Hobbs Australia Telescope National Facility

Slides:



Advertisements
Similar presentations
A walk through some statistic details of LSC results.
Advertisements

Use of Kalman filters in time and frequency analysis John Davis 1st May 2011.
Effect of Surface Loading on Regional Reference Frame Realization Hans-Peter Plag Nevada Bureau of Mines and Geology and Seismological Laboratory University.
Measuring Dispersion in Signals from the Crab Pulsar Jared Crossley National Radio Astronomy Observatory Tim Hankins & Jean Eilek New Mexico Tech Jared.
Using Tempo to calculate solar barycentric time Dejan Paradiž University of Ljubljana.
Excess phase computation S. Casotto, A. Nardo, P. Zoccarato, M. Bardella CISAS, University of Padova.
Gravitational Wave Detection Using Pulsar Timing Current Status and Future Progress Fredrick A. Jenet Center for Gravitational Wave Astronomy University.
Coordinate-systems and time. Seeber 2.1. NON INERTIAL SYSTEM CTS: Conventional Terrestrial System Mean-rotationaxis Greenwich X Y- Rotates.
General Relativity Physics Honours 2006 A/Prof. Geraint F. Lewis Rm 557, A29 Lecture Notes 5.
Navigation using pulsars ASTRONOMY AND SPACE SCIENCE George Hobbs Nov 2014.
Principles of the Global Positioning System Lecture 14 Prof. Thomas Herring Room A;
1 Time Scales Virtual Clocks and Algorithms Ricardo José de Carvalho National Observatory Time Service Division February 06, 2008.
Search for the Gravitational Wave Memory effect with the Parkes Pulsar Timing Array Jingbo Wang 1,2,3, Hobbs George 3, Dick Manchester 3, Na Wang 1,4 1.
Radio Pulsars R. N. Manchester Australia Telescope National Facility, CSIRO Sydney, Australia Summary Introduction to pulsar basics Multibeam searches.
25 Facts about Parkes, Pulsars and
A short tutorial on LAT pulsar analysis tools Gamma-ray Large Area Space Telescope Massimiliano Razzano (Istituto Nazionale di Fisica Nucleare, sec. Pisa)
ElectroScience Lab IGARSS 2011 Vancouver Jul 26th, 2011 Chun-Sik Chae and Joel T. Johnson ElectroScience Laboratory Department of Electrical and Computer.
Satellite Engineering Research Corporation Practical Relativistic Timing Effects in GPS and Galileo Robert A. Nelson Satellite Engineering Research Corporation.
The Effect of Solar Wind on Pulsar Observations Xiaopeng YOU Southwest University, Chongqing, China.
Timing Relativistic Binary Pulsars to test Gravitation and measure NS masses Paulo C. C. Freire Arecibo Observatory / Cornell University.
Neutron Star (Mostly Pulsar) Masses Ingrid Stairs UBC Vancouver CAWONAPS TRIUMF Dec. 9, 2010.
Semi-Empirical MHD Modeling of the Solar Wind Igor V. Sokolov, Ofer Cohen, Tamas I. Gombosi CSEM, University of Michigan Ilia I Roussev, Institute for.
Chapter 8: The future geodetic reference frames Thomas Herring, Hans-Peter Plag, Jim Ray, Zuheir Altamimi.
Space Geodesy (1/3) Geodesy provides a foundation for all Earth observations Space geodesy is the use of precise measurements between space objects (e.g.,
Gravitational wave detection using radio pulsar timing Fredrick A Jenet CGWA/UTB.
Pulsar Timing Phenomenology … an overview…. George Hobbs Australia Telescope National Facility.
The timing behaviour of radio pulsars George Hobbs Australia Telescope National Facility
Page 1 PACS NHSC Data Processing Workshop – Pasadena 26 th - 30 th Aug 2013 Overview of SPIRE Photometer Pipeline Kevin Xu NHSC/IPAC on behalf of the SPIRE.
Timing studies and PSR J analysis Till Eifert, HU Berlin April, 2005.
Fundamental Principles of General Relativity  general principle: laws of physics must be the same for all observers (accelerated or not)  general covariance:
Relativistic Spin Precession in the Double Pulsar Victoria Kaspi McGill University R. Breton, V. Kaspi, M. Kramer, M. McLaughlin, M. Lyutikov, S. Ransom,
National Time Service Center. CAS Time Standard and Ensemble Pulsar Time Scale Ding Chen, George & Bill, Dick, PPTA team 2011 年 5 月 9 日, Beijing.
Pulsar search and timing Pulsar search and timing 22/10/2011 INDIGO Bhal Chandra Joshi Bhal Chandra Joshi.
Why Solar Electron Beams Stop Producing Type III Radio Emission Hamish Reid, Eduard Kontar SUPA School of Physics and Astronomy University of Glasgow,
GWDAW - Annecy December 17 th 2004 LIGO-G Z1 Searching for gravitational waves from known pulsars Matthew Pitkin for the LIGO Scientific Collaboration.
Real-time Acquisition and Processing of Data from the GMRT Pulsar Back- ends Ramchandra M. Dabade (VNIT, Nagpur) Guided By, Yashwant Gupta.
18/04/2004New Windows on the Universe Jan Kuijpers Part 1: Gravitation & relativityPart 1: Gravitation & relativity J.A. Peacock, Cosmological Physics,
童明雷 中国科学院国家授时中心 Pulsar timing residuals induced by non-evolving single GW sources.
Gravitational Wave and Pulsar Timing Xiaopeng You, Jinlin Han, Dick Manchester National Astronomical Observatories, Chinese Academy of Sciences.
Aristeidis Noutsos University of Manchester. Pulsar Polarization Pulsar radiation is elliptically polarised with a high degree of linear polarization.
RELATIVISTIC POSITIONING AND NAVIGATION
Franz Hofmann, Jürgen Müller, Institut für Erdmessung, Leibniz Universität Hannover Institut für Erdmessung Hannover LLR analysis software „LUNAR“
Name EPOCH (Hz) (10 –12 s –2 ) Data Range (MJD) J (4)– (1)55666 – (7)– (5)55912.
Scuola nazionale de Astrofisica Radio Pulsars 2: Timing and ISM
Sarah Burke Spolaor Jet Propulsion Laboratory, California Institute of Technology Gravitational Wave Detection with Pulsar Timing Arrays: Status and Prospects.
Satellite Engineering Research Corporation Precise Time Synchronization Throughout the Solar System Robert A. Nelson Satellite Engineering Research Corporation.
LLR Analysis – Relativistic Model and Tests of Gravitational Physics James G. Williams Dale H. Boggs Slava G. Turyshev Jet Propulsion Laboratory California.
Observing Vela With XDM The First Year Sarah Buchner KAT Bursary conference – Dec 2009.
PTA and GW detection --- Lecture K. J. Lee ( 李柯伽 ) Max-Planck Institute for Radio astronomy Aug
Status of pulsar simulation for DC 2 Gamma-ray Large Area Space Telescope Massimiliano Razzano Nicola Omodei GLAST DC2 Software Workshop (Goddard Space.
Satellite geodesy (ge-2112) Introduction E. Schrama.
What Goes into a Pulsar Timing Model? David Nice Physics Department, Princeton University Pulsar Timing Array: A Nanohertz Gravitational Wave Telescope.
Low Frequency Observations of the ISM and Pulsar Timing Joris Verbiest Xiaopeng You (Southwest University, China) William Coles (UCSD) George Hobbs (ATNF)
Tempo2 software installation ASTRONOMY AND SPACE SCIENCE George Hobbs August 2015.
Soichiro Isoyama Collaborators : Norichika Sago, Ryuichi Fujita, and Takahiro Tanaka The gravitational wave from an EMRI binary Influence of the beyond.
Pulsar timing ASTRONOMY AND SPACE SCIENCE George Hobbs October 2015, Urumqi.
Pulsar timing ASTRONOMY AND SPACE SCIENCE George Hobbs August 2015, Kunming, China-NZ-SA Joint SKA summer school.
A Fan Beam Model for Radio Pulsars Hongguang Wang (王洪光) Center for Astrophysics, Guangzhou University 广州大学天体物理中心 Fast Pulsar Symposium 4.
GLAST and pulsars: models and simulations
MAGIC pulsar workshop, Padova, Feb 2010
Long-Term Timing of Globular Cluster Pulsars
S3 time domain known pulsar search
S3 time domain known pulsar search
NANOGrav Long-term timing of two faint millisecond pulsars at Arecibo
Improving Pulsar Timing
Speaker:Yi Xie Lunch Talk
Extrasolar planet detection: a view from the trenches
Center for Gravitational Wave Physics Penn State University
Principles of the Global Positioning System Lecture 14
J. Ellis, F. Jenet, & M. McLaughlin
Presentation transcript:

Pulsar timing with tempo2 George Hobbs Australia Telescope National Facility

CSIRO. Gravitational wave detection Contents Basis of pulsar timing Getting tempo2 Using tempo2 Developing tempo2

CSIRO. Gravitational wave detection Must average many thousands of pulses together to obtain stable profile Must convert to reference frame suitable for the timing model – e.g. solar system barycentre Must convert to arrival times at infinite frequency Must convert to conform with terrestrial time standards Must add extra propagation delays e.g. through the solar system Pulsar timing: The basics (see Hobbs, Edwards & Manchester 2006, MNRAS) Obtain pulse arrival times at observatory Model for pulsar spin down Form timing residuals – how good is the timing model at predicting the arrival times Improve timing model

CSIRO. Gravitational wave detection Tempo2 Paper 1: Hobbs, Edwards & Manchester (2006), MNRAS, 369, 655 Paper 2: Edwards, Hobbs & Manchester (2006), MNRAS, 372, 1549 Paper 3: Hobbs, Jenet, Lee et al. (2009), MNRAS, 394, 1945

CSIRO. Gravitational wave detection Getting tempo2 Wiki: Main repository: Get data: > cvs -z3 co tempo2 distribution list: Ingrid’s help page for using tempo2:

CSIRO. Gravitational wave detection Paper I: overview Tempo2 accurate for known physics to 1ns (factor of ~100 better than tempo1 and ~1000 better than psrtime) Tempo2 is compliant with the general relativistic framework of the IAU 1991 and 2000 resolutions - uses the international celestial reference system, barycentric coordinate time and up- to-date precession, nutation and polar motion models

CSIRO. Gravitational wave detection Paper I: overview Two parts to tempo2: 1) Forming the pulse emission time and 2) updating the pulsar timing model 1) Forming the pulse emission time Clock corrections Atmospheric delays Solar system Einstein delay SS Roemer delay SS Shapiro delay Dispersive component Secular motion Orbital motion

CSIRO. Gravitational wave detection Forming the pulse emission time: clock corrections TOAs are recorded against local observatory clocks Probably don’t have good long term stability Can transform to the best terrestrial time-scale by applying corrections derived from monitoring the offsets between pairs of clocks E.g. Parkes clock -> GPS -> UTC(AUS) -> UTC -> TAI UTC = time-scale formed through the weighting of data from an ensemble of atomic clocks TAI = UTC + leap seconds to maintain synchrony with Earth’s rotation

CSIRO. Gravitational wave detection Clock corrections Clock corrections are in > $TEMPO2/clock Part of pks2gps.clk

CSIRO. Gravitational wave detection Atmospheric propagation delays Can get effects by the ionised fraction of the atmosphere (ionosphere) and the neutron fraction (mainly the troposphere). It is possible to provide TEMPO2 with lists of surface atmospheric pressure for the most accurate determinations. Not normally needed!

CSIRO. Gravitational wave detection Einstein delay Damour & Deruelle 1986 Quantifies the change in TOAs due to variations in clocks at the observatory and the SSB due to changes in the gravitational potential of the Earth and the Earth’s motion Use barycentric corrdinate time (TBC) instead of barycentric dynamical time which was used in tempo1 => tempo1 parameter files can not immediately be used in tempo2 Note: tempo2 parameters are in SI units …. Tempo1 parameters are not!

CSIRO. Gravitational wave detection Converting tempo1 files to tempo2 > tempo2 -gr transform 1939_t1.par 1939_t2.par or > tempo2 …. -tempo1

CSIRO. Gravitational wave detection Roemer delay The vacuum light travel time between the pulse arriving at the observatory and the equivalent arrival time at the SSB Calculated by determining the time-delay between a pulse arriving at the observatory and at the Earth’s centre and from the Earth’s centre to the SSB Pulsar positions determined in the ICRS (International celestial reference system). Telescope positions are in the ITRF (International terrestrial reference system). Require precession, nutation, polar motion and Earth rotation information to convert between the two. TEMPO1 does not include polar motion Use DEXXX or INPOPXX Solar System models for conversion. Recommend DE405.

CSIRO. Gravitational wave detection More tempo2 files $TEMPO2/ephemeris contains the planetary ephemerides $TEMPO2/observatory contains observatory coordinates Observatory.dat

CSIRO. Gravitational wave detection Solar system Shapiro delay Accounts for the time-delay caused by the passage of the pulse through curved space-time Mainly due to the Sun, but significant Shapiro delay caused by Jupiter.

CSIRO. Gravitational wave detection Dispersive effects Caused by the ISM - assume delays propto f^-2. Also dispersive delay caused by the Solar wind. Approximated in tempo2 with the electron density decreasing as an inverse square law from the centre of the sun. You Xiaopeng developed this model - see You, Hobbs, Coles et al. (2007MNRAS ) and You, Hobbs, Coles et al. (2007ApJ )

CSIRO. Gravitational wave detection Shklovskii effect and radial motion Pulsar-timing measurements are affected by the motion of the pulsar relative to the SSB. This includes radial velocity, the Shklovskii effect and radial acceleration. Can be absorbed by other parameters or included individually

CSIRO. Gravitational wave detection Fitting routines Tempo2 can carry out normal single pulsar fits and also global fits to multiple pulsars

CSIRO. Gravitational wave detection The timing model Use: The frequency derivative terms are fitable parameters Can also include glitch events in the model

CSIRO. Gravitational wave detection Binary models Have various models implemented from tempo1 (BT, ELL1, DD, MSS …) Recommend use of T2 binary model Can assume GR (DDGR model) or small eccentricities (ELL1)

CSIRO. Gravitational wave detection Standard usage of tempo2: Input arrival times Require a file containing arrival times. Required File identifier Observing frequency (MHz) Arrival time (MJD) TOA uncertainty (us) Telescope code User defined flags

CSIRO. Gravitational wave detection Standard usage of tempo2: Input pulsar model Require a parameter file (traditionally *.par) Require: PSRJ RAJ DECJ F0 PEPOCH DM Each parameter Label value MODE 1 = fit with weights MODE 0 = fit without weights SINI KIN => Link the parameters SINI and KIN JUMP -f flag 0 1 FJUMP -f

CSIRO. Gravitational wave detection Standard usage of tempo2 No plugins: tempo2 -f mypar.par mytim.tim

CSIRO. Gravitational wave detection Standard usage of tempo2 Using plk: tempo2 -gr plk -f mypar.par mytim.tim

CSIRO. Gravitational wave detection More plugins Tempo2 -gr spectrum -f mypar.par mytim.tim

CSIRO. Gravitational wave detection The splk plugin

CSIRO. Gravitational wave detection Output plugins: general

CSIRO. Gravitational wave detection Output plugins: general2 Tempo2 -output general2 -s “Hello: {sat} {post}\n” -f mypar.par mytim.tim

CSIRO. Gravitational wave detection Many plugins exist …. Plotting Spectral analysis Simulating data Adding noise to data Adding gravitational wave signals to data ….

CSIRO. Gravitational wave detection Developing tempo2 Anyone can create more plugins. Talk to me if you want to modify the main tempo2 code. Easiest to use C/C++ and pgplot, but can use other languages/libraries

CSIRO. Gravitational wave detection A very simple ‘output’ plugin #include #include “tempo2.h” extern "C" int tempoOutput(int argc,char *argv[],pulsar *psr,int npsr) { int i; printf(“Number of observations = %d\n”,psr[0].nobs); printf(“Name of pulsar = %s\n”,psr[0].name); printf(“A list of site-arrival-times, observing frequencies and residuals\n”); for (i=0;i<psr[0].nobs;i++){ printf(“sat = %g, freq = %g, res = %g\n”,(double)psr[0].obsn[i].sat, (double)psr[0].obsn[i].freq,(double)psr[0].obsn[i].residual); } } See documentation on the tempo2 wiki

CSIRO. Gravitational wave detection Ideas for new plugins Want to analyse the residuals in a new way (wavelet analysis?) Want to model the effect of precession in pulsar timing Want to look for correlated signals in multiple pulsar timing residuals Want to simulate thousands of realisations of realistic timing residuals …

CSIRO. Gravitational wave detection Tempo2 demonstration No plugins General2 Plk - plot options, filter, pass, zoom, delete, measure, highlight, turning jumps on and off Splk Spectrum