Bounding the strength of gravitational radiation from Sco-X1 C Messenger on behalf of the LSC pulsar group GWDAW 2004 Annecy, 15 th – 18 th December 2004 G Z

Scope of S2 analysis Sco-X1 is an LMXB -> GW emission mechanism supported via accretion [R.V.Wagoner, ApJ. 278,345 (1984)] Using F-statistic as detection statistic [Jaranowski,Krolak,Schutz, PRD,58,063001,(1998)] GWs at 2 f rot (mass quadrupole [L.Bildsten, ApJ.Lett,501,L89 (1998)], not yet r- modes [Andersson et al,,ApJ 516,307 (99)] ) 2 frequency windows: 464 – 484 Hz (strong spectral features) and 604 – 624 Hz (reasonably clean) [Van der Klis, Annu. Rev. Astron. Astrophys, :717-60] Also search orbital parameter space of Sco-X1 T obs = 6 hrs (set by computational resources) Analyse L1 and H1 in coincidence H1 L1 (whole S2) L1 H2 GWDAW, Annecy 15 th – 18 th December, 2004 G Z AIM : Set frequentist upper-limit on GWs on a wide parameter space using coherent frequency domain approach SCO-X1 6 hours, 1 filter

Analysis pipeline S2 L1 dataS2 H1 data S2 L1 data subset S2 H1 data subset Compute F statistic over bank of filters and frequency range Store results above “threshold” Compute F statistic over bank of filters and frequency range Store results above “threshold” Selection of 6 Hour dataset Generate Orbital template Bank For L1 L1 6 hour Template bank H1 6 hour Template bank Generate Orbital template Bank For H1 L1 F-Statistic above threshold H1 F-Statistic above threshold Find Coincidence events Coincident Results Find loudest event per band Generate PDF’s Via MC injection Calculate Upper Limits per band Follow up candidates GWDAW, Annecy 15 th – 18 th December, 2004 G Z

Selecting the optimal 6hr We construct the following measure of detector sensitivity to a particular sky position GWDAW, Annecy 15 th – 18 th December, 2004 G Z

Sco-X1 parameter space The orbital ephemeris is taken from the latest (and first) direct observations of the lower mass object within Sco X-1 [Steeghs and Cesares, ApJ,568: ,2002] The orbit has eccentricity<10 -3  Search for circular orbit (e=0) The period (P) is known very well and is NOT be a search parameter GWDAW, Annecy 15 th – 18 th December, 2004 G Z The Search parameters are : –The projected orbital semi-major axis is (4.33+/-0.52) X 10 8 m –The time of periapse passage (SSB frame) is /-299 sec –The GW frequency is not well known and the current model predicts two possible bands, (464<f0<484) and (604<f0<624) Hz. [Van der Klis, Annu. Rev. Astron. Astrophys, :717-60]

Computational Costs This scaling limits this coherent search to an observation time of ~6 hours Additional parameter space dimensions become important for T>10 6 (inc spin up/down, period error, eccentricity) 6 hours 2 weeks Using Tsunami (200 node Beowulf cluster) For 1  errors In parameters GWDAW, Annecy 15 th – 18 th December, 2004 G Z T<PP<T<10 6 # Orbital Templates T3T3 constant # Frequency Templates TT CPU time per template TT Computational time T5T5 T2T2 The scaling of computational time with observation time :

Orbital templates Templates are laid in an approximately “flat” 2D space by choosing a sensible parameterisation. The template bank covers the uncertainty in the value of the projected semi-major axis and the time of periapse passage. The template placement is governed by the parameter space metric [Brady et al, PRD 57,2101 (1998), Dhurandhar and Vecchio, PRD, 63, (1998)] GWDAW, Annecy 15 th – 18 th December, 2004 G Z

The frequency resolution Using the projected metric to lay orbital templates takes advantage of frequency – orbital parameter correlations. A mismatch in orbital parameters can be compensated for by a mismatch in frequency. GWDAW, Annecy 15 th – 18 th December, 2004 G Z We find that a frequency resolution of 1/(5T obs ) approximates a continuous frequency spectrum. A consequence of this approach is that the detection template and signal can differ in frequency by up to +/15 bins

Coincidence events The orbital template bank guarantees a >90% match with the closest filter. If a signal triggers a template we can identify a region around that template within which the true signal lies. Now find the possible closest templates in the second detector. The coincidence detection is based on geometric arguments only. Typically ~8 possible orbital and ~30 possible frequency coincidence locations ~200 possible coincident locations per event. GWDAW, Annecy 15 th – 18 th December, 2004 G Z >90% in Detector 1 >90% in Detector 2

The search sensitivity The “11.4” factor is based on a false alarm rate of 1% and a false dismissal rate of 10% for a single filter search We use ~10 8 per 1 Hz band This significantly increases the chances of “seeing” something large just from the noise. Therefore we require stronger signals to obtain the same false dismissal and false alarm rates. S1 paper ~ 20 GWDAW, Annecy 15 th – 18 th December, 2004 G Z

Currently –We have analysed 1/5 th of the parameter space –Completing LSC code review (Organising and checking the growing number of codes + documentation) –Ready to run the pipeline on the full parameter space and set frequentist upper limits via Monte-Carlo injections. Targets –Implement suitable veto strategies (Fstat shape test, Fstat time domain test, …) –Follow up loudest candidate(s) with an aim to veto them out (observe for longer ?, observe another data stretch ?, …) –Start applying our understanding to the incoherent stacking approach (see poster by Virginia Re) –Apply the coherent approach to other LMXB parameter space searches. GWDAW, Annecy 15 th – 18 th December, 2004 G Z Status and future work