1 / 12

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.

prue
Download Presentation

Are the relativistic Fe lines really relativistic?

An Image/Link below is provided (as is) to download presentation Download Policy: Content on the Website is provided to you AS IS for your information and personal use and may not be sold / licensed / shared on other websites without getting consent from its author. Content is provided to you AS IS for your information and personal use only. Download presentation by click this link. While downloading, if for some reason you are not able to download a presentation, the publisher may have deleted the file from their server. During download, if you can't get a presentation, the file might be deleted by the publisher.

E N D

Presentation Transcript

  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.

More Related