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Are the relativistic Fe lines really relativistic?

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 25 th 2009.

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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 25th 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)‏ 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 : ~ 6.5 keV Objectives

  4. 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

  5. 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

  6. 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

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

  8. Comparing results with published data ResultfromCackett et al (2009) Resultfrommyproject Results

  9. Statistics on equivalent width Correlationbetween EW and n° of counts Correlationbetween EW and error • Broad line – result of bad statistics • Unlikely to be due to broadening mechanism of relativistic effect Results

  10. 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

  11. Distribution of energy and sigma Distribution of energy of centroid of Fe line Distribution of sigma of Fe line

  12. Background figure 35: Background spectrum for the pn camera during an observation with the filter wheel in the CLOSED position (top: single events, bottom: double events) in the energy range 0.2-18 keV. The prominent features around 1.5 keV are Al-K, at 5.5 keV Cr-K, at 8 keV Ni-K, Cu-K, Zn-K and at 17.5 keV (only in doubles) Mo-K fluorescence lines. The rise of the spectrum below 0.3 keV is due to the detector noise. The relative line strengths depend on the (variable) incident particle spectrum.

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