Marcus Ziegler SCIPP/UCSCDC2 Closeout Meeting 1 Pulsar Blind search in the DC2 data Gamma-ray Large Area Space Telescope Marcus Ziegler Bill Atwood Brian.

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Presentation transcript:

Marcus Ziegler SCIPP/UCSCDC2 Closeout Meeting 1 Pulsar Blind search in the DC2 data Gamma-ray Large Area Space Telescope Marcus Ziegler Bill Atwood Brian Baughman Robert Johnson

Marcus Ziegler SCIPP/UCSCDC2 Closeout Meeting 2 Data Selection As input all sources listed in the LATSourceCatalog_v1 were used (=> 380 sources) James Chiang and Johann Cohen helped to write a Python script to: - Pick a source from the catalog - Select all photons within a 2° radius around the source (energy dependent cut based on GLAST PSF did not improve the signal) - Correct the photon arrival time - Output the data into a text file -> Calculate differences and Perform the FFT

Marcus Ziegler SCIPP/UCSCDC2 Closeout Meeting 3 Finding a Pulsar Candidate Source MRF0035 Look for frequency with the highest power Found F0 = /s DC2 Catalog = /s

Marcus Ziegler SCIPP/UCSCDC2 Closeout Meeting 4 Test statistic (signal/noise) -> Calculate the RMS of the power spectrum Test Statistik (signal to noise) = max_power_in_FFT / RMS Work with Joe Dolan in progress to get a measure of the significance of the found peaks. (See how likely it is that a random fluctuaton created a peak of the same height) Take a cloer look at sources with s/n > 45

Marcus Ziegler SCIPP/UCSCDC2 Closeout Meeting 5 Sources with large s/n Unknown large s/n source in the galactic plane. No natching pulsar in the database. Vela Geminga (2 nd harmonic)

Marcus Ziegler SCIPP/UCSCDC2 Closeout Meeting 6 Covered phase space All 100 pulsars from pulsar data base Scan for pulsars (0.5 Hz to 64 Hz) F dot /F up to 3x10 -9 (300 1x ) Scan for ms pulsars (0.5 Hz to 512 Hz) F dot /F up to 3x (6 0.5x ) Scan found 16 Radio Loud pulsars 3 Radio Quiet pulsars A maximum time difference of s was used -> Calculation took about 2 weeks on a PC

Marcus Ziegler SCIPP/UCSCDC2 Closeout Meeting 7 Blind Search Catalog with reprocessed DC2 Data Source_NameLBTest Stat.F0F1 MRF E-13Unknown Pulsar MRF PSR_J0904m5008 MRF E-11PSR_B0833m45 Vela MRF PSR_J1735m5757 MRF PSR_J0633p1746 2xGeminga MRF E-11PSR_J2229p6114 MRF PSR_J0717m1235 MRF E-11PSR_J1420m6048 MRF E-13Unknown Pulsar MRF PSR_J1739m2903 MRF E-12PSR_J1015m5719 MRF PSR_J1852m2610 MRF PSR_J1638m5226 MRF E-13Unknown Pulsar MRF E-12PSR_J1637m4642 MRF E-10PSR_B0531p21 3xCrab MRF PSR_J1741m3927 MRF E-12PSR_J1825m1446 MRF E-12PSR_J1856p0113 MRF E-11?

Marcus Ziegler SCIPP/UCSCDC2 Closeout Meeting 8 Flux Sensitivity Pulsar with lowest flux: Off plane (b=11.9): PSR_J1852m2610 flux 3x10 -7 Ph/cm 2 s In plane (b= -0.9) PSR_J1856p0113 flux 7x10 -7 Ph/cm 2 s

Marcus Ziegler SCIPP/UCSCDC2 Closeout Meeting 9 Recover light curve for source MRF0168 (Vela) Vela Radio Position Ra = Dec = MRF0168 Position Ra = Dec = Light curve: Barycenter time correction for MRF0168 position. Pulsar spin parameter from radio position. Radio :Ep= F0= F1= e-011 F2= 6.26E-22 Optimized :Ep= F0= F1= e-011 F2= -2.30E-20 Barycenter time correction for MRF0168 position. Optimized pulsar spin parameter for MRF0168 pos.

Marcus Ziegler SCIPP/UCSCDC2 Closeout Meeting 10 Light curves of pulsars without radio data Epoch_MET = F0 = F1 = e-013 F2 = 6.0 e-022 Epoch_MET = F0 = F1 = e-013 F2 = -3.3 e-021 Epoch_MET = F0= F1= e-012 F2= 1.0 e-021

Marcus Ziegler SCIPP/UCSCDC2 Closeout Meeting 11 Summary + Future plans Thank you for this excellent data set to perform a realistic blind search! Bill’s differencing method is an easy and fast way of finding pulsations from pulsars pulsars were found and the spin parameters/light curve an be derived Things to improve - Add up harmonics to increase the sensitivity - Get PC with more memory to perform larger FFTs (we are also looking into a hardware FFT implementation) - Implement the alorythm into the the science tools

Marcus Ziegler SCIPP/UCSCDC2 Closeout Meeting 12 Basic Idea take only differences with  t < max_diff max_diff used for DC2 data = s Calculate the Fourier-Transform of the time differences of the photon arrival times  t n.