1. High-Resolution X-ray Spectroscopy of AGN Warm Absorbers Rebecca Smith MSSL, UCL with G. Branduardi-Raymont and M. Page

4. Aims Studying a variety of AGN warm absorbers Comparison offers clues to dynamics, chemical composition, physical structure and origin High-resolution soft X-ray spectra vital diagnostic tool Three objects presented today, focussing on data from XMM-Newton RGS

5. Objects Markarian 509  Seyfert 1  z=0.034  Very high luminosity Seyfert 1  L 2-10keV = 1.3-2.6x10 44 erg s -1  Galactic N H =4.4x10 20 cm -2  Bright X-ray NLS1  L 2-10keV = 2.4x10 43 erg s -1  Galactic N H =6.4x10 20 cm -2  Spectral variation between observations  L 2-10keV = 8x10 42 -3x10 43 erg s -1  Galactic N H =5.8x10 20 cm -2 Arakelian 564  NLS1  z=0.025 1H 0707-495  NLS1  z=0.041

6. Flux (photons m -2 s -1 Å -1 ) Markarian 509 Phase 1:  log  = 0.89 ± 0.07  outflow vel = 510 ± 200km s -1  N H = 0.79x10 21 cm -2 Phase 2:  log  =2.14 ± 0.08  outflow vel = 260 ± 120km s -1  N H = 0.75x10 21 cm -2 Phase 3:  log  = 3.26 ± 0.03  outflow vel = 60 ± 100km s -1  N H = 5.50x10 21 cm -2 Wavelength ( Å ) XMM-Newton RGS Smith et al. 2007

7.     T Thermal Stability Graph Pressure form ionization parameter: Phases with the same value of  can be in pressure equilibrium and so exist within the same cloud Smith et al. 2007

8. Flux (photons m -2 s -1 Å -1 ) Arakelian 564 Phase 1:  log  = 0.29 ± 0.20  outflow vel = 10 ± 90km s -1  Col Dens = 0.31x10 21 cm -2 Phase 2:  log  = 2.56 ± 0.09  outflow vel = 20 ± 100km s -1  Col Dens = 0.71x10 21 cm -2 Narrow emission lines from OVIII and NVII with outflow velocity ~ 500km s -1 Wavelength ( Å ) Smith et al. in prep XMM-Newton RGS

9. 1H 0707-495 Energy (keV)‏ Normalized counts /s / keV Spectral changes between 2000 observation (black) and 2002 observation (red)‏ Shift in energy of large feature at ~7keV‏ Gallo et al. 2004 XMM-Newton EPIC PN 2000 2002

10. 2000 20022 Wavelength (Å)‏ Counts m -2 s -1 Å -1 XMM-Newton RGS1H 0707-495

11. Gallo et al. 2004 Two features, with ~8% energy shift Change in ionization or velocity? XMM-Newton RGS 1H 0707-495 XMM-Newton EPIC PN Wavelength ( Å ) Energy (keV)‏ Counts m -2 s -1 Å -1 normalized counts s -1 keV -1 2002 2000 Smith et al. in prep 2002 2000

12. 10 15 20 25 30 35 Counts m -2 s -1 Å -1 XMM-Newton RGS 1H 0707-495 2000 2002 Wavelength (Å)‏

13. XMM-Newton RGS Arakelian 564 Markarian 509 Counts m -2 s -1 Å -1 1H 0707-495 2000 1H 0707-495 2002 10 15 20 25 30 35 Wavelength ( Å )

14. Conclusions Have analysed three Seyfert 1s with high-resolution soft X- ray spectra Interesting diversity of characteristics in outflows and emission features Connected UV and X-ray absorbers in Mrk 509 and Ark 564 Mrk 509 shows strong broad emission lines consistent with the optical broad line region Ark 564 has a highly ionized absorber with a surprisingly low outflow velocity 1H 0707-495 shows dramatic soft X-ray spectral variability in strength of warm absorber and energy of 'shoulder'