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## Are the relativistic Fe lines really relativistic?

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**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**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**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**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**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**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**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**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**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**Evolution of spectrum fit**( + + ) + abs gaussian diskbbody+bbodyrad Fe K line gaussian+gaussian calib 1.84keV calib 2.28keV Emission 1keV Data analysis**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**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**Evolution of spectrum fit**( + + ) + abs gaussian gaussian diskbbody+bbodyrad Fe K line gaussian+gaussian calib 1.84keV calib 2.28keV Emission 1keV Data analysis**Evolution of spectrum fit**( + + ) + abs gaussian gaussian diskbbody+bbodyrad Fe K line gaussian+gaussian calib 1.84keV calib 2.28keV Emission 1keV Data analysis**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**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**Evolution of spectrum fit**( + + ) + abs gaussian diskbbody+bbodyrad Fe K line gaussian+gaussian calib 1.84keV calib 2.28keV Emission 1keV Data analysis**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**Gaussian & Laor comparison on 4U 1543-62**Gaussian Laor Data analysis**Gaussian & Laor comparison on 4U 1543-62**Gaussian Laor Data analysis**Gaussian & Laor comparison on 4U 1543-62**Gaussian Laor Data analysis**Gaussian & Laor comparison on 4U 1543-62**Gaussian Laor • Narrow line width • Small inner radius • Similar X² • Insignificant evidence of asymmetric profile Data analysis**Statistics on equivalent width**Results**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