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Low Frequency Observations of the ISM and Pulsar Timing Joris Verbiest Xiaopeng You (Southwest University, China) William Coles (UCSD) George Hobbs (ATNF)

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Presentation on theme: "Low Frequency Observations of the ISM and Pulsar Timing Joris Verbiest Xiaopeng You (Southwest University, China) William Coles (UCSD) George Hobbs (ATNF)"— Presentation transcript:

1 Low Frequency Observations of the ISM and Pulsar Timing Joris Verbiest Xiaopeng You (Southwest University, China) William Coles (UCSD) George Hobbs (ATNF) PPTA team Swinburne University & ATNF, Australia

2 Outline Brief intro to PPTA DM variations and the turbulent ISM PSR J0437-4715’s DM Structure Function TOA-intensity correlation Summary

3  Australia Telescope National Facility, CSIRO, Sydney Dick Manchester, George Hobbs, David Champion, John Sarkissian, John Reynolds, Mike Kesteven, Warwick Wilson, Grant Hampson, Andrew Brown, David Smith, Jonathan Khoo, (Russell Edwards)  Swinburne University of Technology, Melbourne Matthew Bailes, Willem van Straten, Joris Verbiest, Ramesh Bhat, Sarah Burke, Andrew Jameson  University of Texas, Brownsville Rick Jenet  University of California, San Diego Bill Coles  Franklin & Marshall College, Lancaster PA Andrea Lommen  University of Sydney, Sydney Daniel Yardley  National Observatories of China, Beijing Johnny Wen  Peking University, Beijing Kejia Lee  Southwest University, Chongqing Xiaopeng You  Curtin University, Perth Aidan Hotan PPTA Team Members

4 Pulsar Timing Arrays Main goal: Detect gravitational waves Secondary goals: Investigate time standards Investigate Solar System Investigate ISM …

5 DM Variations in Timing 50cm 20cm 10cm 20cm

6 PPTA DM Variations You et al., MNRAS, 2007

7 DM Structure Function Measure of turbulent power at different scales Expected to be exponential with spectral index α = 5/3 for Kolmogorov model

8 Typical SF You et al., MNRAS, 2007

9 Kolmogorov Slope (1000 days ≈ 7.8 AU) You et al., MNRAS, 2007

10 Large Inner Scale (10 days ≈ 0.4 AU) You et al., MNRAS, 2007

11 PSR J0437-4715 SF 1000 days ≈ 61 AU You et al., MNRAS, 2007

12 0437 DM Variations ~500 days ≈ 30 AU 2004 2008

13 Scintillation & TOAs PSR J0437-4715 685 MHz 2 hours, 8sec integrations TOA residual Signal-to-Noise -1

14 Scintillation/TOA - Simulations Coles et al., in preparation

15 Grad DM - Simulations Coles et al., in preparation

16 Correlation - Real Data Coles et al., in preparation

17 Conclusions PTAs need high timing precision.  ISM effects need to be corrected  Most easily measured at low frequencies  ISM: an interesting place that keeps surprising…

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