1. Current Results and Future Capabilities of Pulsar Timing Andrea N. Lommen International Liaison for NANOGrav Associate Professor of Physics and Astronomy Head of Astronomy Program Director of Grundy Observatory Franklin and Marshall College Lancaster, PA “Pulsar Timing: No longer a blunt instrument for gravitational Wave detection” Lommen, Journal of Physics, 2012

2. IPTA = NANOGrav + EPTA + PPTA NANOGrav = North American Nanohertz Observatory of Gravitational Waves EPTA = European Pulsar Timing Array PPTA = Parkes Pulsar Timing Array (Australia)

3. The International Pulsar Timing Array www.ipta4gw.org

4. Pulsar2 Pulsar1 Earth Photo Courtesy of Virgo Adapted from NASA figure

5. Detectability of a Waveform

6. A sense of what’s detectable

7. NANOGrav Residuals Adapted from Demorest et al (2013) by David Nice

8. NANOGrav 5-year timing results summary Demorest et al (2013)

10. Constraining the Properties of Supermassive Black Hole Systems Using Pulsar Timing: Application to 3C 66b, Jenet, Lommen, Larson and Wen (2004) ApJ 606:799-803. (NANOGrav) Data from Kaspi, Taylor, Ryba 1994 10 Orbital Motion in the Radio Galaxy 3C 66B: Evidence for a Supermassive Black Hole Binary Sudou, Iguchi, Murata, Taniguchi (2003) Science 300: 1263-1265. Residual(  s) -10 10 0 Residual(  s) -10 10 0 Simulated residuals due to 3c66b

11. Hellings and Downs Curve (Overlap Reduction Function) Courtesy of Rick Jenet (NANOGrav) and George Hobbs (PPTA). Original figure from Hellings and Downs (1983).

12. Yardley et al 2011 (PPTA)

13. Measure the polarisation properties of gravitational wave Test theories of gravity…! (NANOGrav -> EPTA) Lee et al. (2008)

14. Sydney Chamberlin (UW Milwaukee, NANOGrav) Non-Einsteinian gravitational waves using PTAs Chamberlin et al, PhRvD (2012)

15. Yardley et al 2011 (PPTA)

16. Van Haasteren et al 2011 (EPTA)

17. Figure by Paul Demorest, NANOGrav (see arXiv:0902.2968 and arXiv:1201.6641) MBH-MBH (indiv) Gal NS/BH BH-BH (indiv) PSRs

18. Sesana, Vecchio and Volunteri 2009 (NANOGrav, EPTA)

19. Method used from: Ellis, Siemens, and Creighton ApJ 2012. Plot courtesy of Xavi Siemens. (NANOGrav) Similar to work of Yardley et al (2011, PPTA) but about a factor of 7 more sensitive

20. Ability to constrain position is function of h Kejia Lee (EPTA) et al, 2011, MNRAS

21. From Sesana & Vecchio (2010), EPTA 100 pulsars, SNR=10 Sky position frequency Inclination angle Source amp phase Polarization angle

22. A 5 x 10 9 solar-mass black hole binary coalescing 100 Mpc away. 30 IPTA pulsars, improved by 10, sampled once a day. Thank you to Manuela Campanelli, Carlos O. Lousto, Hiroyuki Nakano, and Yosef Zlochower for waveforms. Phys.Rev.D79:084010 (2009). http://ccrg.rit.edu/downloads/waveforms From Finn & Lommen 2010 (NANOGrav)

23. Kejia Lee et al (2010), EPTA Measuring the graviton mass

24. Cosmic String Tension Upper Limits Sotirios Sanidas, Richard Battye, and Ben Stappers (U of Manchester and Jodrell Bank Center for Astrophysics, EPTA) 2011

25. Measuring spin-orbit precession of BHBs using pulsar timing by Mingarelli et al, PhRvL (2012) Trevor Sidery, Kat Grover, Rory Smith, Chiara Mingarelli.

26. Deng & Finn (NANOGrav, 2011) curvature of the waveform Pitkin & Woan (2012) a clever use of the “pulsar term” to increase the possibility of detecting a burst signal. (LIGO!)

27. The GW sky is not isotropic in the PTA band!(Joe Simon, Franklin and Marshall College, NANOGrav, in prep) Should we expect nHz gravitational- wave hotspots?

28. New Telescopes

29. A Large European Array for Pulsars = LEAP! Coherently add pulsar observations from 5 of the largest telescopes in Europe (and the world!) to obtain most precise TOA’s for GW detection. Combine telescopes to form a phased array, a telescope with equivalent size of a 200 m dish - ~5% SKA! A LEAP in collecting area. Funded by European Research Council Advanced Grant (PI Kramer).

30. 30  Unique Karst depression as the site  Active main reflector  Cable - parallel robot feed support 100 米 300 米 500 米 Five-hundred-meter Aperture Spherical radio Telescope (FAST)

31. GW-sensitivity IPTA IPTA ＋ FAST

32. We need & want people to join us Lots of data, low on people-power $6.5M grant from NSF -> NANOGrav to foster international collaboration. Student and faculty exchanges.

33. The Pulsar Data Challenge Opened a week ago (March 23) Will close in Sept Go to www.ipta4gw.org

34. Summary Pulsars make a galactic scale gravitational wave observatory which is poised to detect gravitational waves in 5-10 years. Stochastic, single sources, alternate polarizations, waveform and location recovery, mass of the graviton, spin-orbit coupling, cosmic strings… Coopetition works even though it’s not a real word Please get involved, through data challenges is one way, student and faculty exchanges another We expect to be surprised.