Presentation is loading. Please wait.

Presentation is loading. Please wait.

Marcus Ziegler SCIPP/UCSCPulsar Meeting DC2 1 Fourier Transform with differences on Simulated and Real Pulsar Data UPDATE Gamma-ray Large Area Space Telescope.

Published by Modified over 9 years ago

Similar presentations

Presentation on theme: "Marcus Ziegler SCIPP/UCSCPulsar Meeting DC2 1 Fourier Transform with differences on Simulated and Real Pulsar Data UPDATE Gamma-ray Large Area Space Telescope."— Presentation transcript:

1 Marcus Ziegler SCIPP/UCSCPulsar Meeting DC2 1 Fourier Transform with differences on Simulated and Real Pulsar Data UPDATE Gamma-ray Large Area Space Telescope Marcus Ziegler Bill Atwood Brian Baughman Robert Johnson

2 Marcus Ziegler SCIPP/UCSCPulsar Meeting DC2 2 Basic Idea take only differences with  t < max_diff typical max_diff = 10 000s typical EGRET viewingperiod ~ 1 000 000s Calculate the Fourier-Transform of the time differences of the photon arrival times  t n.

3 Marcus Ziegler SCIPP/UCSCPulsar Meeting DC2 3 Dependence on max_diff The dependence of the signal width on max_diff Pulse width ~ 1/max_diff Simmulated Pulsar at 10Hz Power RMS off peak is called Noise Small max_diff + Small number of differences (fast) + Coarse stepping in Frequency space (fast) -Large noise (Small S/N ratio) Large max_diff + Good S/N ratio - Large number of differences (very slow)

4 Marcus Ziegler SCIPP/UCSCPulsar Meeting DC2 4 Blind Search for VELA VELA Viewing Period VP 7 max_diff 10 000s Scan region 1 Hz – 100 Hz Number of Photons 1 197 Number of differences 22 700 Number F trials 2 000 000 Calculations52 800 000 000 took 4h 30 min F0 catalog11.19888756 F0 from search 11.19882249 F1 catalog -0.1557 E-10 F1 from search 0.0850 E-10 F0 trials with S/N > 10 Refined search around good F0 candidates

5 Marcus Ziegler SCIPP/UCSCPulsar Meeting DC2 5 Blind Search for GEMINGA GEMINGA Viewing Period VP 10 max_diff 10 000s Scan region 1 Hz – 100 Hz Number of Photons 1 200 Number of differences 12 300 Number F trials 2 000 000 Calculations 2 400 000 000 took 3h 30 min F0 catalog4.2177501 F0 from search 4.2176815 F1 catalog -0.00195 E-10 F1 from search -0.00935 E-10 F0 trials with S/N > 10 Refined search around good F0 candidates

6 Marcus Ziegler SCIPP/UCSCPulsar Meeting DC2 6 The large F1 of CRAB Simmulate Pulsar F0 = 10Hz F1 = -3.0 E-10 F1 GEMINGA -0.00195 E-10 F1 VELA -0.15666 E-10 F1 CRAB -3.86228 E-10 Scan in F1 @ 10 Hz, max_diff 10 000s Scan in F1 CRAB max_diff 10 000s

7 Marcus Ziegler SCIPP/UCSCPulsar Meeting DC2 7 F0 and F1 Scan for CRAB Scan in F CRAB max_diff 10 000s F1 steps @ 10Hz 0.05 E-10 F1 steps @ 30Hz 0.15 E-10 F0 catalog30.2254 F0 from search 29.9493 F1 catalog -3.8623 E-10 F1 from search -3.7719 E-10 Epoch CRAB 40000 Epoch Search48393 Calculations took 4d 16h

Download ppt "Marcus Ziegler SCIPP/UCSCPulsar Meeting DC2 1 Fourier Transform with differences on Simulated and Real Pulsar Data UPDATE Gamma-ray Large Area Space Telescope."

Similar presentations

GLAST Science Support CenterAugust 9, 2004 Progress on Pulsar Tools Development Masaharu Hirayama (GLAST SSC—GSFC/UMBC)

GLAST Science Support CenterAugust 9, 2004 Progress on Pulsar Tools Development Masaharu Hirayama (GLAST SSC—GSFC/UMBC)
Analysis report of SN1006 D.Nishida( Kyoto-Univ.) JPS meeting Autumn 2005 Osaka.

Analysis report of SN1006 D.Nishida( Kyoto-Univ.) JPS meeting Autumn 2005 Osaka.
Pulsar High Energy Emission Models: What Works and What Doesn't “Standard” outer magnetosphere models - successes Shortcomings of the models Next steps?

Pulsar High Energy Emission Models: What Works and What Doesn't “Standard” outer magnetosphere models - successes Shortcomings of the models Next steps?
Bill Atwood, SCIPP/UCSC, Jan., 2006 GLAST 1 A Time Differencing Technique for doing Blind Pulsar Searches Bill Atwood, Brian Baughman, Marcus Ziegler,

Bill Atwood, SCIPP/UCSC, Jan., 2006 GLAST 1 A Time Differencing Technique for doing Blind Pulsar Searches Bill Atwood, Brian Baughman, Marcus Ziegler,
1 Hough transform Some Fourier basics: –Nyquist frequency: 1/2 , with  the difference between time samples. If signal is bandwidth limited below Nyquist.

1 Hough transform Some Fourier basics: –Nyquist frequency: 1/2 , with  the difference between time samples. If signal is bandwidth limited below Nyquist.
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.

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.
Blind search in EGRET data The bright pulsars Vele and Gminga can be found using a time difference window of only 3 hours. No scan in the frequency derivative.

Blind search in EGRET data The bright pulsars Vele and Gminga can be found using a time difference window of only 3 hours. No scan in the frequency derivative.
Pulsar modeling and simulations Gamma-ray Large Area Space Telescope Massimiliano Razzano Nicola Omodei LAT Collaboration Meeting (SLAC, August 29 th -

Pulsar modeling and simulations Gamma-ray Large Area Space Telescope Massimiliano Razzano Nicola Omodei LAT Collaboration Meeting (SLAC, August 29 th -
Marcus Ziegler SCIPP/UCSCPulsar VRVS Meeting 1 Light curves from pulsars found in a blind search in the DC2 data Gamma-ray Large Area Space Telescope Marcus.

Marcus Ziegler SCIPP/UCSCPulsar VRVS Meeting 1 Light curves from pulsars found in a blind search in the DC2 data Gamma-ray Large Area Space Telescope Marcus.
Fourier Transforms on Simulated Pulsar Data Gamma-ray Large Area Space Telescope.

Fourier Transforms on Simulated Pulsar Data Gamma-ray Large Area Space Telescope.
The Origins of X-Rays. The X-Ray Spectrum The X-Ray Spectrum (Changes in Voltage) The characteristic lines are a result of electrons ejecting orbital.

The Origins of X-Rays. The X-Ray Spectrum The X-Ray Spectrum (Changes in Voltage) The characteristic lines are a result of electrons ejecting orbital.
Fourier Transforms on Simulated Pulsar Data Gamma-ray Large Area Space Telescope.

Fourier Transforms on Simulated Pulsar Data Gamma-ray Large Area Space Telescope.
C&A 1 May 06 1 Point Source Detection and Localization Update Using the UW HealPixel database on DC2_2 data Toby Burnett University of Washington.

C&A 1 May 06 1 Point Source Detection and Localization Update Using the UW HealPixel database on DC2_2 data Toby Burnett University of Washington.
Marcus Ziegler SCIPP/UCSCPulsar VRVS Meeting 1 Pulsar Blind search on DC2 data Gamma-ray Large Area Space Telescope Marcus Ziegler Bill Atwood Brian Baughman.

Marcus Ziegler SCIPP/UCSCPulsar VRVS Meeting 1 Pulsar Blind search on DC2 data Gamma-ray Large Area Space Telescope Marcus Ziegler Bill Atwood Brian Baughman.
SLAC, 7 October 2004 1 Multifrequency Strategies for the Identification of Gamma-Ray Sources Marcus Ziegler Santa Cruz Institute for Particle Physics Gamma-ray.

SLAC, 7 October Multifrequency Strategies for the Identification of Gamma-Ray Sources Marcus Ziegler Santa Cruz Institute for Particle Physics Gamma-ray.
Fourier Transforms on Simulated Pulsar Data Gamma-ray Large Area Space Telescope.

Fourier Transforms on Simulated Pulsar Data Gamma-ray Large Area Space Telescope.
Marcus ZieglerAPS April Meeting 2006 1 Gamma-Ray Pulsars in the GLAST Era Gamma-ray Large Area Space Telescope Marcus Ziegler Santa Cruz Institute for.

Marcus ZieglerAPS April Meeting Gamma-Ray Pulsars in the GLAST Era Gamma-ray Large Area Space Telescope Marcus Ziegler Santa Cruz Institute for.
Marcus Ziegler SCIPP/UCSCPulsar Meeting 1/17/2006 1 Fourier Transform with differences on Simulated and Real Pulsar Data Gamma-ray Large Area Space Telescope.

Marcus Ziegler SCIPP/UCSCPulsar Meeting 1/17/ Fourier Transform with differences on Simulated and Real Pulsar Data Gamma-ray Large Area Space Telescope.
Gamma-Ray Pulsars in the GLAST Era Gamma-ray Large Area Space Telescope Marcus Ziegler University of California Santa Cruz Bill Atwood Brian Baugmann Rober.

Gamma-Ray Pulsars in the GLAST Era Gamma-ray Large Area Space Telescope Marcus Ziegler University of California Santa Cruz Bill Atwood Brian Baugmann Rober.
New observations of three AXPs at low radio frequencies Daria Teplykh & V.M. Malofeev, A.E. Rodin, S.V. Logvinenko. Pushchino Radio Astronomy Observatory.

New observations of three AXPs at low radio frequencies Daria Teplykh & V.M. Malofeev, A.E. Rodin, S.V. Logvinenko. Pushchino Radio Astronomy Observatory.

Similar presentations

Ads by Google