Improving Pulsar Timing

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Presentation transcript:

Improving Pulsar Timing Willem van Straten George Hobbs, Rick Jenet

Why? Gravitational Wave detection/sensitivity MSPs binary system dynamics Astrometry: Solar System Ephemeris Earth Wobble Terrestrial Time Timing Noise (incl. glitches)

EPTA (Effelsberg/ Westerbork/ Jodrell Bank) ~30 115 MHz – 8GHz ~1us Observatory Number of pulsars Observing span (yr) System Observing frequency Rms Jodrell Bank ~600 0-35 FB 600-1600MHz >10us Parkes msps 15 ~10 CD 1.4GHz, 3GHz >100ns Parkes young 114 1.4GHz PPTA 20 2 CD/DFB/CORR 600MHz, 1.4/3 GHz Arecibo 7 ~20 0.4/1.4/2.4GHz >200ns Greenbank EPTA (Effelsberg/ Westerbork/ Jodrell Bank) ~30 115 MHz – 8GHz ~1us Nancay ~1.4GHz ~500ns Urumqi 284 10 1.5GHz >100us Hartebeesthoek 30 1.6/2.3GHz GMRT 1 (1937+21) FB/CD 325/610 MHz G. Hobbs

How? Precision (Noise) Software/Modeling Accuracy (Systematics) Numerical Precision Arrival Time Estimation Time Standard Precision (Noise) Polarimetric Calibration Interstellar Scintillation Earth Wobble Accuracy (Systematics) RFI Mitigation Solar System Ephemeris Solar Wind Earth Atmosphere DM Variation Clock Correction Time/Freq Resolution Sensitivity Hardware/Instrumentation

Modelling Software (tempo2) Clock Corrections Physical Delays: Solar System Ephemeris (incl. Shapiro delay) Earth Wobble precession & nutation (40ns) polar motion (60ns) Atmospheric Delays troposphere (20ns) ionosphere (1ns)

RFI mitigation using an adaptive filter Kesteven et al. (2004)

Interstellar Scintillation Figure 1, Walker & Stinebring (2005)

Arrival Time Estimation Frequency domain (Taylor 1992) Multi-component Gaussian (Kramer et al. 1994) Invariant interval (Britton et al. 2000) Full polarization (van Straten 2004) Time vs. frequency domain (Hotan et al. 2005) Higher order moments (Jenet & Hobbs 2005)

Full Polarization TOA Useful for timing? (Kramer et al. 1999) Stokes Q, U, V often sharper than Stokes I Useful for timing? (Kramer et al. 1999)

PSR J0437-4715

PSR J1713+0747

PSR B1937+21

PSR J1022+1001

Formalism van Straten (2004)

Simulation Position Angle of Linear Polarization: Gaussian Total Intensity Profile with Width, w Constant Degree of Polarization, p Measurement noise, n

PSR J0437-4715 1.1

PSR J1713+0747 1.0

PSR B1937+21 1.4

PSR J1022+1001 1.6

PSR J0437-4715

PSR J1713+0747

PSR B1937+21

PSR J1022+1001

Results Pulsar Benefit Systematic J0437-4715 1.11(1) 300 ns 1713+0747 0.99(6) 35 ns B1937+21 1.4(3) 30 ns 1022+1001 1.56(8) 400 ns

Conclusion Effectiveness varies by pulsar To do: Full Polarization TOA holds promise Effectiveness varies by pulsar To do: Produce/acquire well-calibrated, high S/N polarimetric pulse profile (standards) Run simulations Improve arrival time estimates