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The Gravitational Lensing Effect in the X-ray Observation

The Gravitational Lensing Effect in the X-ray Observation. Zhenya Zheng zhengzy@mail.ustc.edu.cn. Why Choose X-ray Band ?. Confusion Problem. 1. Optical obs. :

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The Gravitational Lensing Effect in the X-ray Observation

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  1. The Gravitational Lensing Effect in the X-ray Observation Zhenya Zheng zhengzy@mail.ustc.edu.cn

  2. Why Choose X-ray Band ? • Confusion Problem. • 1. Optical obs. : • Hard to separate stars from lensed quasars , even at high Galactic latitudes (Kochanek 1993. Castles, finding 96 lenses system until 1999) • 2. Radio obs. : ( Source structure) • Flat-spectrum radio lens surveys contain far more compact doubles than two-image lenses (e.g: JVAS, 66 of 2384 compact radio sources have multiple components within 0.3~6”, only 6 are lenses.) • Steep-spectrum surveys must cope with the enormous variety of extended radio-emission morphologies (Griffith et al. 1991)

  3. Why Choose X-ray Band ? • Confusion vanish for high-resolution X-ray imaging observation (e.g. Chandra) • 1. confusing Galactic sources are rare • 2. source structure is simple Chandra : angular resolution ~1”(on axis) covering area ~0.1 deg^2 • 3. mass estimate for clusters, from gas , stellars, and lens. Virial theory.

  4. Lenses in the X-rays, By Galaxies • Started from the Hard X-ray Luminosity Function (Ueda et al. 2003)

  5. Lensing optical depth & Magnification Bias • A Schechter Luminosity & Faber-Jackson relation • B

  6. The obs. Selection effect • Point Spread Function for Chandra • Fraction will increase with the multiple observation in one field • E.g. CDFs

  7. Searching lenses in Chandra Deep Feilds

  8. CDFS, XID 200 & XID 222 • XID200 z~ 0.75-1.38 XID 222 z~ 0.88-1.40 CL=95, photo-z (Zheng, et al 2004) Separation angle ~ 3-5” Optical image from

  9. Cluster Lensing • Very high cross section • Expected less number than galaxies. • Arclets. & effects on XRB Refregier & Loeb 1997

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