1. David Smith CENBG Plans for Radio Pulsar Timing GLAST collaboration meeting, Stockholm, 30 August 2006 1 Radio Timing for GLAST Pulsars Radio Timing for GLAST Pulsars GLAST LAT collaboration meeting Stockholm, August 2006 David Smith for the PSR SNR PWNe group CENBG/In2p3/CNRS Bordeaux, France Parkes (Australia) Nançay (France) Jodrell (England)

2. David Smith CENBG Plans for Radio Pulsar Timing GLAST collaboration meeting, Stockholm, 30 August 2006 2 Pulsar, Supernova Remnant, Plerion Science Group Report D.J. Thompson & R.W. Romani, co-leadersAgenda Report on radio timing planning (David Smith) - 20 min.Report on radio timing planning (David Smith) - 20 min. Report on X-ray timing planning (Joe Dolan) - 10 minReport on X-ray timing planning (Joe Dolan) - 10 min Report on DC2 results (Alice Harding) - 20 min.Report on DC2 results (Alice Harding) - 20 min. Discussion of DC3 needs (Francesco Longo) - 10 min.Discussion of DC3 needs (Francesco Longo) - 10 min. Discussion of papers, especially LAT paper (Roger Romani) - 20 min.Discussion of papers, especially LAT paper (Roger Romani) - 20 min.

3. David Smith CENBG Plans for Radio Pulsar Timing GLAST collaboration meeting, Stockholm, 30 August 2006 3 Topics "Good ephemeredes will dramatically enhance pulsar (and PWN) science" -- Roger Romani, in "Radio Timing for GLAST: Requirements, Costs, and Triage'', 21 Feb 2006 1.Why we need a lot of radio pulsar timing 2.Which radio telescopes are expected to make which measurements 3.Distillation: protocol for radio ephemeredes to reach D4.fits file(s) on the LAT servers. Most hyperlinks in this talk can be found at "radio confluence", i.e.radio confluence https://confluence.slac.stanford.edu/display/SCIGRPS/Radio+timing+for+GLAST and in any case they’re active links in the powerpoint.

4. David Smith CENBG Plans for Radio Pulsar Timing GLAST collaboration meeting, Stockholm, 30 August 2006 4

5. David Smith CENBG Plans for Radio Pulsar Timing GLAST collaboration meeting, Stockholm, 30 August 2006 5 Galaxy of pulsars animation by Michael Kramer (Manchester/Jodrell)

6. David Smith CENBG Plans for Radio Pulsar Timing GLAST collaboration meeting, Stockholm, 30 August 2006 6 Why we need radio timing of pulsars 1.10x better pulsed sensitivity than without accurately known period DC2 seems to confirm N  _true = N  _observed/Ntrials, and Ntrials large for blind search. Timing noise makes blind search harder for multi-month data 2.Signatures of beam geometry and acceleration region & mechanism are in the variations of light curves with wavelength. 3.Most gamma ray pulsar candidates are young & noisy. That means, the rotation parameters (ephemeredes) "spoil" within weeks to months, so the radio measurements need to be repeated perdiodically throughout the mission. 4.GLAST won't point first year – will see all pulsars "all" the time. Slow accumulation of gammas over time requires long term accurate timing.

7. David Smith CENBG Plans for Radio Pulsar Timing GLAST collaboration meeting, Stockholm, 30 August 2006 7 Ephemeredes sooner, not later Realize later that PSR Jxxxx+yy might have been a good one? TOO LATE, you can’t go back, see e.g. 2229+6114 in astro-ph/0112518. (Thompson Digel Nolan Reimer) Fun fact : 600+ radio pulsars in Joe Fierro's "EGRET pulsars" thesis; 1400+ plus when I started with ATNF late last year ; 1500+ early this year ; 1600+ during the Spring ; Presently 1775….

8. David Smith CENBG Plans for Radio Pulsar Timing GLAST collaboration meeting, Stockholm, 30 August 2006 8 CGRO had the same issue "Worse" for GLAST LAT: 3x more known pulsars, 25x more sensitivity.

9. David Smith CENBG Plans for Radio Pulsar Timing GLAST collaboration meeting, Stockholm, 30 August 2006 9 Which are GLAST's candidates? Study of the huge* sample of known gamma pulsars leads to the conclusion that  Edot/d² is a good predictor of gamma ray emission, where Edot=dE/dt is the the rotation spin-down energy. Distance "d" often poorly known ( derived from DM=Dispersion Measure and model of electron density in interstellar space ), so hedge bets by also keeping large Edots. * That's a joke, son.

10. David Smith CENBG Plans for Radio Pulsar Timing GLAST collaboration meeting, Stockholm, 30 August 2006 10 Gamma ray pulsars From G. Kanbach, 363rd Heraeus seminar, May 2006 – other authors order these differently…

11. David Smith CENBG Plans for Radio Pulsar Timing GLAST collaboration meeting, Stockholm, 30 August 2006 11 Gamma ray pulsar candidates We made a list of 255 candidates, applying some convienient cuts to the ATNF database. All known "favorites" are ( hopefully !) included. CUT N' PASTE OF THE ATNF WWW EXPERT MENU: User-defined variables C1 (sqrt(Edot)/Dist1/Dist1)/5.362E18 ( normalize to ~Crab) Sort on field C1 Order Descending Condition (Edot>1E34 || (sqrt(Edot)/Dist1/Dist1)/5.362E18 > 0.01) (~1% of Crab)

12. David Smith CENBG Plans for Radio Pulsar Timing GLAST collaboration meeting, Stockholm, 30 August 2006 12 GLAST’s gamma candidates, compared to all known pulsars and the CGRO 7, prepared by J. Petit & C. Loumena

13. David Smith CENBG Plans for Radio Pulsar Timing GLAST collaboration meeting, Stockholm, 30 August 2006 13 TOA’s for "bread & butter" pulsars “Bread & butter” pulsars – a couple of hundred gamma candidates that are relatively easy to measure in radio. Roger defines Treq and VperY in his "TimingTriage.pdf": Treq: 100 meter class time (hours) required for needed Time-of-arrival (TOA) precision; VperY: Visits per Year to not loose count of neutron star rotations (depends mainly on Pdot) "Easy" means (Treq < 1 hour) for a 100 meter class telescope and (VperY < 3) For Treq<0.1 h, small telescopes can do. We will load into D4.fits any valid ephemeredes we can get our hands on, and search for gamma pulsations at those positions (even if no DC excess, apologies to Jean Ballet et al – remember PSR B1951+32 in EGRET!).

14. David Smith CENBG Plans for Radio Pulsar Timing GLAST collaboration meeting, Stockholm, 30 August 2006 14 The Big Three pulsar telescopes The Big Three pulsar telescopes for long term timing of hundreds of "bread & butter" gamma ray candidates Parkes (Australia) Nançay (France) Jodrell (England)

15. David Smith CENBG Plans for Radio Pulsar Timing GLAST collaboration meeting, Stockholm, 30 August 2006 15 TOA’s for "important but tough" pulsars “key but tough” pulsars – a dozen or two pulsars with the biggest spin-down energies (best gamma ray candidates) but faint radio signals (low S1400, high duty cycle, high b'grd makes high Treq) and large VperY. [ For radio flux density at 1400 MHz S1400 < 25 µJy, use X-ray satellites when possible, see Joe Dolan's presentation. ]

16. David Smith CENBG Plans for Radio Pulsar Timing GLAST collaboration meeting, Stockholm, 30 August 2006 16 Green Bank (West Virginia) Oversubscribed – not for bread & butter, only caviar & champagne. Save for e.g. deep searches of new geminga-likes. Arecibo (Puerto Rico) The Big Guns

17. David Smith CENBG Plans for Radio Pulsar Timing GLAST collaboration meeting, Stockholm, 30 August 2006 17 Building a strawman proposal Take list of 255 gamma pulsar candidates, see confluence radio timing page and next slide.confluence radio timing page  Calculate Roger’s Treq and VperY (my code is in strawman.tar at radio confluence)radio confluence  Jodrell (Nançay) works down to declination –35° (-39°), Parkes good as far north as  =+2°.  63 "Northern", 129 "Parkes", 62 "Either". Therefore, "eithers" better shared by Jodrell & Parkes, that is, 63+62=125 with  -30° for those two.

18. David Smith CENBG Plans for Radio Pulsar Timing GLAST collaboration meeting, Stockholm, 30 August 2006 18 Parkes strawman proposal Parkes strawman proposal (first 32 of 129, sorted by Treq) similar for the Northern telescopes… ( a lot of ) bread n' butter Ouch!

19. David Smith CENBG Plans for Radio Pulsar Timing GLAST collaboration meeting, Stockholm, 30 August 2006 19 Sharing the load Effelsberg (Germany) Nanshan (China) Some other instruments can time our radio-brighter ( small Treq ) but noisier ( large VperY ) pulsars. Relieve pressure on the Big Three Provide redundant measurements, fill in coverage gaps Special projects, e.g. tracking DM at frequencies besides 1400 MHz, searches for giant pulse correlations, etc. Remember – we need timing for years, but resources at each instrument ebb & flow. Many (most!) eager to work with GLAST. ATA (Hat Creek, California)

20. David Smith CENBG Plans for Radio Pulsar Timing GLAST collaboration meeting, Stockholm, 30 August 2006 20 GLAST Pulsar Radio Timing Discussions Report on GLAST Pulsar Radio Timing Discussions at the Prague IAU GA David Smith w. D. Dumora CENBG/In2p3/CNRS Bordeaux, France 16-17 August 2006

21. David Smith CENBG Plans for Radio Pulsar Timing GLAST collaboration meeting, Stockholm, 30 August 2006 21 GLAST radio timing "splinter session" at Prague Roger & Dave T on the JD02 organizing Committee, volunteered me to give “Future Gamma & TeV Observatories for Pulsars” (thank you!) (see talk at radio confluence.)radio confluence Many attendees are members of Glast Pulsar Advisory Group (see slide 18 of http://glast.gsfc.nasa.gov/ssc/resources/guc/050606/MultiwaveObs.pdf by Steve Thorsett) http://glast.gsfc.nasa.gov/ssc/resources/guc/050606/MultiwaveObs.pdf So organized a Splinter Session (see PragueDiscussion and PragueDiscussionBis at radio confluence.)radio confluence Well attended, about 20 people, a veritable Who’s Who of radio pulsarers. AGENDA: a) alert them to our ~250 favorite candidates, in hope of defining who- does-which ; b) alert them to D4.fits, to start process of translating their formats and conventions into ours. They’ve been waiting for our call. Eager and very well informed.

22. David Smith CENBG Plans for Radio Pulsar Timing GLAST collaboration meeting, Stockholm, 30 August 2006 22 So? What's the plan? Bread & butter:  Northern hemisphere, no real issue – most already being timed. Coordinate to make sure that all are, in a coherent way. The radio astronomers are in touch with each other.  Southern hemisphere – Parkes is the only big pulsar instrument. Not automated, requires shifters. Proposal has to be made & defended (Simon Johnston), and they request help for a person-year (e.g. student or technician). Important but tough  A few being timed anyway.  A few to be offloaded to X-ray instruments.  The others to be subjects of specific proposals Current key task – clarify exactly who does which how, then support PI's in writing and defending their proposals. Steve Thorsett and/or Roger Romani will be coordinating via personal contacts.

23. David Smith CENBG Plans for Radio Pulsar Timing GLAST collaboration meeting, Stockholm, 30 August 2006 23 Filling D4.fits* For gtpphase etc to work like in DC2, need  TOAs to become proper timing solutions ("ephemeredes")  Ephemeredes must get loaded into a D4.fits on the GSSC servers. D. Dumora wrote code² that takes TEMPO output from Nançay, Jodrell, etc and converts it to the.txt format prescribed for gtpulsardb. We appended 13 Nançay & Jodrell pulsars to the ~1100 CGRO ephemeredes in the D4.fits sample provided by Masa H & James P at GSSC 3. The whole chain works, tuning in progress. *Don't know what "D4.fits" means? Go to pulsar section of the SAS workbook and look for ephemeredes database, or look at e.g. Max Razzano's DC2 tutorials. ² http://www.cenbg.in2p3.fr/ftp/astropart/Smith/Pulsars/NançayTempoToLATascii.htmhttp://www.cenbg.in2p3.fr/ftp/astropart/Smith/Pulsars/NançayTempoToLATascii.htm 3 http://glast.gsfc.nasa.gov/ssc/dev/psr_tools/definitionD4.htmlhttp://glast.gsfc.nasa.gov/ssc/dev/psr_tools/definitionD4.html

24. David Smith CENBG Plans for Radio Pulsar Timing GLAST collaboration meeting, Stockholm, 30 August 2006 24 Filling D4.fits more on Filling D4.fits After this rustic beta-testing, will industrialize. Format conversion routines will become daemons at GSSC servers. Radio-astronomers will send their numbers to get loaded into D4.fits that will wind up on the GSSC servers*. Need tools to test validity of final numbers (quality control). * Tom Stephens already has these structures in place.

25. David Smith CENBG Plans for Radio Pulsar Timing GLAST collaboration meeting, Stockholm, 30 August 2006 25 Conclusion: Pulsar Timing Action Items 1.Refine lists of who does which, propose to the radiotelescopes, and iterate. 2.Identify PI’s for time requests at GBT, RXTE, etc. Support proposal preparation. 3.Continue to load D4.fits with real ephemeredes, and excercise Science Tools. Develop QA tools. 4.Help provide manpower or $$$ to radio observatories.