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Are the relativistic Fe lines really relativistic? PowerPoint Presentation
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Are the relativistic Fe lines really relativistic?

Are the relativistic Fe lines really relativistic?

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Are the relativistic Fe lines really relativistic?

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  1. Are the relativistic Fe lines really relativistic? Traineeship 2009 : A systematic analysis of the Fe K line from inner region of accretion disk of Neutron star LMXB with XMM-Newton • Supervisors: • Maria Diaz-Trigo • Marion Cadolle • Simone Migliari Cherry Ng September 24th 2009

  2. Outline Fe K emission line Inner region of the accretion disk Objectives Data analysis Results Conclusion Importance of pile-up treatment Relativistic Fe K line ? Outline

  3. Neutron Star Low-mass X-ray binaries (NS LMXB)‏ Low-mass star Roche-lobe overflow Accretion disk Weakly magnetized NS • Fe K emission line • Typical energy : ~ 6.5keV Objectives

  4. Neutron Star Low-mass X-ray binaries (NS LMXB)‏ Cackett et al (2008) ApJ 674:415-420 Low-mass star Roche-lobe overflow Accretion disk Weakly magnetized NS • Fe K emission line • Typical energy : ~ 6.5keV Objectives

  5. Neutron Star Low-mass X-ray binaries (NS LMXB)‏ • Systematic analysis • All publicly available bright Neutron Star LMXB • XMM-Newton •  26 observations •  17 sources Objectives

  6. Treatment of Pile-up Single & Double-px event pattern plot of Ser X1 No. of counts normalized to 1 • Common problem of bright sources • 2 photons of lower energy read as 1 photon of higher energy • Distortion of spectra Data analysis

  7. Treatment of Pile-up Single & Double-px event pattern plot of Ser X1 No. of counts normalized to 1 Single-px event Double-px event • Common problem of bright sources • 2 photons of lower energy read as 1 photon of higher energy • Distortion of spectra Data analysis

  8. Treatment of Pile-up Single & Double-px event pattern plot of Ser X1 Comparison of Ser X1 spectra before and after pile-up removal No. of counts normalized to 1 Single-px event Double-px event • Common problem of bright sources • 2 photons of lower energy read as 1 photon of higher energy • Distortion of spectra Data analysis

  9. Treatment of Pile-up Single & Double-px event pattern plot of Ser X1 Comparison of Ser X1 spectra before and after pile-up removal No. of counts normalized to 1 Single-px event Excessemission Double-px event Before pile-up removal After pile-up removal • Common problem of bright sources • 2 photons of lower energy read as 1 photon of higher energy • Distortion of spectra Data analysis

  10. Evolution of spectrum fit ( + + ) + abs gaussian diskbbody+bbodyrad Fe K line gaussian+gaussian calib 1.84keV calib 2.28keV Emission 1keV Data analysis

  11. Evolution of spectrum fit ( + + ) + abs abs gaussian diskbbody+bbodyrad diskbbody+bbodyrad Fe K line gaussian+gaussian calib 1.84keV calib 2.28keV Emission 1keV Data analysis

  12. Evolution of spectrum fit ( + + ) + abs gaussian diskbbody+bbodyrad Fe K line gaussian+gaussian gaussian+gaussian calib 1.84keV calib 2.28keV Emission 1keV Data analysis

  13. Evolution of spectrum fit ( + + ) + abs gaussian gaussian diskbbody+bbodyrad Fe K line gaussian+gaussian calib 1.84keV calib 2.28keV Emission 1keV Data analysis

  14. Evolution of spectrum fit ( + + ) + abs gaussian gaussian diskbbody+bbodyrad Fe K line gaussian+gaussian calib 1.84keV calib 2.28keV Emission 1keV Data analysis

  15. Evolution of spectrum fit ( + + ) + abs gaussian diskbbody+bbodyrad Fe K line Fe K line gaussian+gaussian calib 1.84keV calib 2.28keV Emission 1keV Data analysis

  16. Evolution of spectrum fit ( + + ) + abs gaussian diskbbody+bbodyrad Fe K line Fe K line gaussian+gaussian calib 1.84keV calib 2.28keV Emission 1keV Data analysis

  17. Evolution of spectrum fit ( + + ) + abs gaussian diskbbody+bbodyrad Fe K line gaussian+gaussian calib 1.84keV calib 2.28keV Emission 1keV Data analysis

  18. Evolution of spectrum fit ( + + ) + abs abs gaussian gaussian diskbbody+bbodyrad diskbbody+bbodyrad Fe K line Fe K line gaussian+gaussian gaussian+gaussian calib 1.84keV calib 2.28keV Emission 1keV Data analysis

  19. Gaussian & Laor comparison on 4U 1543-62 Gaussian Laor Data analysis

  20. Gaussian & Laor comparison on 4U 1543-62 Gaussian Laor Data analysis

  21. Gaussian & Laor comparison on 4U 1543-62 Gaussian Laor Data analysis

  22. Gaussian & Laor comparison on 4U 1543-62 Gaussian Laor • Narrow line width • Small inner radius • Similar X² • Insignificant evidence of asymmetric profile Data analysis

  23. Comparing results with published data Results

  24. Statistics on equivalent width Results

  25. Conclusion • Relativistic origin for the broadening of Fe cannot be claimed • Further higher resolution spectroscopic data needed --> to place better constraints on possible contribution to the line emission from various parts of disk Thankyou !  Conclusion