Are the relativistic Fe lines really relativistic Traineeship

Outline 1. Objectives Fe K emission line Inner region of the accretion disk 2.

Neutron Star Low-mass X-ray binaries (NS LMXB) Roche-lobe overflow Low-mass star Weakly magnetized NS

Neutron Star Low-mass X-ray binaries (NS LMXB) Cackett et al (2008) Ap. J 674:

Neutron Star Low-mass X-ray binaries (NS LMXB) • Systematic analysis • All publicly available

Treatment of Pile-up No. of counts normalized to 1 Single & Double-px event pattern

Evolution of spectrum fit abs ( gaussian +diskbbody+bbodyrad + Fe K line ) +gaussian

Gaussian & Laor comparison on 4 U 1543 -62 Gaussian Laor 7 Data analysis

Gaussian & Laor comparison on 4 U 1543 -62 Gaussian Laor Energy : Sigma

Comparing results with published data 8 Results

Statistics on equivalent width 9 Results

Conclusion • Relativistic origin for the broadening of Fe cannot be claimed • Further

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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 Cherry Ng September 24 th 2009 1 Supervisors: • Maria Diaz-Trigo • Marion Cadolle • Simone Migliari

Outline 1. Objectives Fe K emission line Inner region of the accretion disk 2. Data analysis Importance of pile-up treatment 3. Results Relativistic Fe K line ? 4. Conclusion 2 Outline

Neutron Star Low-mass X-ray binaries (NS LMXB) Roche-lobe overflow Low-mass star Weakly magnetized NS Accretion disk • Fe K emission line • Typical energy : ~ 6. 5 ke. V 3 Objectives

Neutron Star Low-mass X-ray binaries (NS LMXB) Cackett et al (2008) Ap. J 674: 415 -420 Roche-lobe overflow Low-mass star Weakly magnetized NS Accretion disk • Fe K emission line • Typical energy : ~ 6. 5 ke. V 3 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 4 Objectives

Treatment of Pile-up No. of counts normalized to 1 Single & Double-px event pattern plot of Ser X 1 • Common problem of bright sources • 2 photons of lower energy read as 1 photon of higher energy • Distortion of spectra 5 Data analysis

Treatment of Pile-up No. of counts normalized to 1 Single & Double-px event pattern plot of Ser X 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 5 Data analysis

Treatment of Pile-up No. of counts normalized to 1 Single & Double-px event pattern plot of Ser X 1 Comparison of Ser X 1 spectra before and after pile-up removal 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 5 Data analysis

Treatment of Pile-up No. of counts normalized to 1 Single & Double-px event pattern plot of Ser X 1 Comparison of Ser X 1 spectra before and after pile-up removal Single-px event Excess emission 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 5 Data analysis

Evolution of spectrum fit abs ( gaussian +diskbbody+bbodyrad + Fe K line ) +gaussian calib 1. 84 ke. V calib 2. 28 ke. V Emission 1 ke. V 6 Data analysis

Gaussian & Laor comparison on 4 U 1543 -62 Gaussian Laor 7 Data analysis

Gaussian & Laor comparison on 4 U 1543 -62 Gaussian Laor Energy : Sigma : 0. 33± 0. 13 Laor index : 0. 97 Inclination : EW : Reduced X² : Rin: EW : Reduced X² : 7 32 ± 9 e. V 0. 96 Data analysis

Gaussian & Laor comparison on 4 U 1543 -62 Gaussian Laor Energy : Sigma : 0. 33± 0. 13 Laor index : 0. 97 Inclination : EW : Reduced X² : Rin: EW : Reduced X² : 32 ± 9 e. V 0. 96 • Narrow line width • Small inner radius • Similar X² • Insignificant evidence of asymmetric profile 7 Data analysis

Comparing results with published data 8 Results

Statistics on equivalent width 9 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 Thank you ! 10 Conclusion