CW signals: plans for S2CW signals: plans for S2

June 16-17 the group held a f2f meeting to discuss plans for analyses of S2 data (and beyond).

Slides from the various presentations can be found at www.lsc-group.phys.uwm.edu/pulgroup/

The content of this presentation is mostly cut-and-paste from these.

Next f2f scheduled 1 day before LSC meeting.

Coherent search methods

•Time domain Bayesian analyses:

• extend to all known isolated pulsars emitting above ~ 50 Hz (Glasgow).

• special search for Crab (Glasgow)

• Metropolis-Hastings Markov Chain Monte Carlo method for parameter estimation and small parameter space searches (Carleton)

• Frequency domain analyses:

• extend to inspect a larger parameter space (non-targeted search) (AEI+UWM)

• extend to search for signals from a pulsar in a binary system, will be applied to Sco X-1 (Birmingham)

Non-coherent search methodsNon-coherent search methods

• Unbiased searches (Michigan)

• Hough search (UIB, AEI)

• Stack-slide (Hanford)

TDS: Known pulsarsTDS: Known pulsars

(R. Dupuis, G. Woan, M. Pitkin GLASGOW)

Perform similar statistical analysis as S1 for all known isolated radio pulsars with f

GW > 50 Hz.

Total of 34 pulsars Computational cost minimal: processing time on Medusa should

be around 15 min per pulsar. Another 15 minutes on a workstation to calculate posterior probability. Automatic characterization of noise in small freq. band

Crab pulsar

young pulsar with large spindown and timing noise: dedicated effort.

Would like to perform a coherent analysis using all IFOs for every pulsar.

• Preliminary results should be available by August LSC.

Isolated pulsars with fGW

> 50 Hz# PULSAR FREQUENCY (HZ)

1 B0021-72C 173.7082189660532 B0021-72D 186.6516698568383 B0021-72F 381.158663656554 B0021-72G 247.501525096525 B0021-72L 230.087746291506 B0021-72M 271.987228788937 B0021-72N 327.444318617558 J0024-7204V 207.909 J0030+0451 205.5306992749310 B0531+21 30.2254370 11 J0537-6910 62.05509612 J0711-6830 182.11723766639013 J1024-0719 193.7156866910314 B1516+02A 180.0636246972715 J1629-6902 166.6499060407416 B1639+36A 96.36223456417 J1709+23 215.9418 J1721-2457 285.989348011919 J1730-2304 123.11028917979720 J1744-1134 245.426123707305921 J1748-2446C 118.538253056322 B1820-30A 183.8234354177723 B1821-24 327.4056651498924 J1910-5959B 119.648732845725 J1910-5959C 189.4898710701926 J1910-5959D 110.677191984027 J1910-5959E 218.733857589328 B1937+21 641.928261106808229 J2124-3358 202.79389723498830 B2127+11D 208.21168801031 B2127+11E 214.98740790632 B2127+11F 248.32118076033 B2127+11H 148.29327256534 J2322+2057 207.968166802197

Black dots show expected upper limit using H2 S2 data.Red dots show limits on ellipticity based on spindown.

MCMC's (N. Christensen) Definitely useful to nail down signal parameter values around candidates Might be useful for small parameter space searches, e.g. the Middleditch optical pulsar in SNR1987A. On-going work to efficiently search over additional parameters (frequency, fdot, wobble angle) in low signal-to-noise conditions.

Automation of TDS (G. Santostasi) Plan to automate the data processing done in the time domain

search making it an on-line analysis (perhaps LDAS?)

Just starting to look at this.

Time Domain SearchesTime Domain Searches

FDS: parameter space searchesFDS: parameter space searches

(M.A. Papa, X. Siemens – AEI , UWM)

Moving towards a hierarchical search. We now expand the coherent search to inspect a larger parameter space. (At the same time the incoherent stage is being developed and tested)

The limiting factor is computational time need to decide how to spend the computing cycles that we have

We have decided to pursue two types of searches:

short observation time (~1/2 day), no spin-down params, wide band (~300 Hz) centered at ~ 300 Hz, all sky search

perhaps longer observation time, 1 spin-down param, small area search (galactic plane/SNRs), small bands. There is a delicate trade-off between sensitivity, observation time (spanned and effective), resolution in parameter space and class of sources that one chooses to target. Calibration info needed to finalize choice.

Note: different choices could be made in order to produce the best ULs.

FDS: Sco X1FDS: Sco X1

(C. Messenger, A. Vecchio – Birmingham)

Sco X-1:• Frequency: not known a priori – search on a wide band (~ 100 Hz)• Doppler effects:

• Source position: known (no search over sky position)• Orbit: circular (e < 3x10-4), therefore 3 search parameters (projected semi-

major axis, orbital period, initial phase on the orbit)• For T < 1 month period is not a search parameters• Search over only 2 parameters (flat parameter space)

• Spin-down/up: number of spin-down parameters depend on the integration time, but for T < 10 days signal monochromatic

• Physical scenarios:• Accretion induced temperature asymmetry (Bildsten, 1998;

Ushomirsky, Cutler, Bildsten, 2000)• R-modes (Andersson et al, 1999; Wagoner, 2002)

Sco X-1 and LIGO/GEO sensitivity

PSR J1939+2134

Sco X-1 (Rejean’s plot)

Upper-limit on Sco X-1Upper-limit on Sco X-1

PULG F2F Meeting, UWM, 16PULG F2F Meeting, UWM, 16thth - 17 - 17thth March, 2003 March, 2003

June 16, 2003 face-to-face pulsar meeting - UWM

Unbiased, All-sky CW Search -- Michigan Group

10

Unbiased All-Sky Search (Michigan)[ D. Chin, V. Dergachev, K. Riles ]

Analysis Strategy:• Measure power in selected bins of averaged periodograms• Bins defined by source parameters (f, RA, ) • Estimate noise level & statistics from neighboring bins• Set “raw” upper limit on quasi-sinusoidal signal on top of

empirically determined noise• Scale upper limit by antenna pattern correction, Doppler

modulation correction, orientation correction• Refine corrected upper limits further with results from

explicit signal simulation

What will be ready by August LSC meeting?

• Expect bare-bones baseline limits over samples of clean frequency ranges with semi-analytical efficiency corrections

Primary goal in next two months

What is unlikely to be ready by August:

• Graceful handling of problematic frequency ranges

• Efficiency corrections based on full MC simulations

Hough TransformHough Transform

(B. Krishnan, A.M. Sintes, M.A. Papa – AEI-UIB)

• start with SFTs with baseline of ~ 30 minutes (or more if stationarity of data allows it).

• for every SFT () select frequency bins i such |SFT|i2/<|SFT|2> exceeds some threshold time-frequency plane of zeros and ones.

• Hough transform: track patterns of “ones” consistent with what one would expect from a signal.

• use of SFT input data (non-demodulated data)

• peak selection on a time-frequency plane

• Hough transform for the different template parameters: sky location, f0, fk, i.e. build histograms for all points in the template parameter space.

We make use of an efficient implementation of a HT:

- stereographic projection is used to tile the sky (to avoid unnecessary distortions and facilitate calculations)

- use of LUT

- many computational savings if spin-down search parameters are considered.

Future plans include performing an incoherent search using F statistic as input data (but not for S2). The (LAL) Hough routines are general and can already handle this case.

11stst Driver code – in final validation phase Driver code – in final validation phase

• This driver code will analyze a large sky area (on a coarse grid) in a given frequency band (to be determined), with possible spin-down parameters.

• Perform an incoherent Hough search using S2 data, with the main purpose of determine a detailed implementation using real IFO data and then setting an strategy for signal detection or setting an upper limit

• Issues to be addressed mainly concern automatic handling on noise features and robust psd estimation.

Plans for S2 Plans for S2

Stack slideStack slide

(M . Landry, G. Mendell – Hanford)

• new proposal presented in May at a meeting devoted to new data analysis proposals

• based on P.R. Brady, T. Creighton Phys.Rev. D61 (2000) 082001

• it is a hierarchical search with a several passes of coherent and incoherent searches. The incoherent search consists in summing (stacking) appropriately (by choosing the appropriate search frequency values – this is the sliding) the outcome of the previous stage.

• new effort, a lot of work. Probably can take advantage of some of the lessons learned while developing the Hough code.

• The group has discussed whether to eventually consider the S2 and S3 data sets together. The discussion was inconclusive, depending on too many unknowns like the character of the S3 data and the outcome of the S2 analyses. For now we’ll concentrate 100% on S2 data.

• Papers:

• there will likely be more than 1 paper

• a possible scenario is to group searches according to the method that was used – common statistical analysis:

ULs on 34 known pulsars FD methods: search for Sco X1 and for parameter space searches (all-sky,wide band, no spin-down & small area search, narrow band, 1 spin-down param) incoherent methods: unbiased, hough, stack

S2 and S3, papersS2 and S3, papers