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Florencia Jiménez Luján

Measuring Ionisation parameters (ITP-WHT). Florencia Jiménez Luján. BAL QSO meeting 2009 Jun 24 – 26 Bologna (Italy). Introduction Data Results Fut ure plans Summary. Unification of AGN (Active Galactic Nuclei). (NLR).

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Florencia Jiménez Luján

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  1. Measuring Ionisation parameters (ITP-WHT) Florencia Jiménez Luján BAL QSO meeting 2009 Jun 24 – 26 Bologna (Italy)

  2. Introduction • Data • Results • Future plans • Summary

  3. Unification of AGN (Active Galactic Nuclei) (NLR) QSO (Quasi-Stellar Object, or quasar, QUASi-stellAR) in the center of each AGN: black hole surrounded by an accretion disk moving clouds: BLR (fast) & NLR (slow) classification: orientation scenario vs. evolutionary scenario (both???) know the properties & composition of the medium (BLR) Urry & Padovani, 1995

  4. Unification of AGN (Active Galactic Nuclei) No absorbers BAL QSO (Quasi-Stellar Object, or quasar, QUASi-stellAR) in the center of each AGN: black hole surrounded by an accretion disk moving clouds: BLR (fast) & NLR (slow) classification: orientation scenario vs. evolutionary scenario (both???) know the properties & composition of the medium NAL Elvis, 2000

  5. Unification of AGN (Active Galactic Nuclei) BALQSO have convex radio spectra (typical of CSS/GPS “young” radio sources) CSS: Compact Steep Spectrum; GPS: Gigahertz Peaked Spectrum QSO (Quasi-Stellar Object, or quasar, QUASi-stellAR) in the center of each AGN: black hole surrounded by an accretion disk moving clouds: BLR (fast) & NLR (slow) classification: orientation scenario vs. evolutionary scenario (both???) know the properties & composition of the medium Montenegro-Montes et al., 2008

  6. q11_020 1210+5256 z = 3.194 r = 18.50 Not in FIRST

  7. q11_039 1210+5256 z = 2.560 r = 17.77 FIRST: 1.9 mJy

  8. link

  9. q11_020 Central wavelength: 4790 Å (blue arm: b1,b2,b3) Flux Wavelength (Å)

  10. q11_020 Central wavelength: 5590 Å (red arm: r1) Flux Wavelength (Å)

  11. q11_020 Central wavelength: 6165 Å (red arm: r2,r3) Flux Wavelength (Å)

  12. q11_039 Central wavelength: 3970 Å (blue arm: b1) Flux Wavelength (Å)

  13. q11_039 Central wavelength: 5144 Å (red arm: r1) Flux Wavelength (Å)

  14. q11_020 Flux r1 resampling Flux r2_3 Wavelength (Å) CIV central source z = 3.194 absorbers z ~ 2.853 Wavelength (Å)

  15. q11_020 a b c CIV central source z = 3.194 absorbers z ~ 2.853

  16. q11_020 a: -25500 - -25470 km s-1 CIV central source z = 3.194 absorbers z ~ 2.853

  17. q11_020 b: -25410 - -25370 km s-1 CIV central source z = 3.194 absorbers z ~ 2.853

  18. q11_020 c: -25320 - -25290 km s-1 CIV central source z = 3.194 absorbers z ~ 2.853

  19. q11_020 r1 Flux Wavelength (Å) SiIV central source z = 3.194 absorbers z ~ 2.853

  20. q11_020 a b c SiIV central source z = 3.194 absorbers z ~ 2.853

  21. q11_020 a: -25500 - -25470 km s-1 SiIV central source z = 3.194 absorbers z ~ 2.853

  22. q11_020 b: -25410 - -25370 km s-1 SiIV central source z = 3.194 absorbers z ~ 2.853

  23. q11_020 c: -25320 - -25290 km s-1 SiIV central source z = 3.194 absorbers z ~ 2.853

  24. q11_020 central source z = 3.194 absorbers z ~ 2.853

  25. q11_039 b1 Flux OVI Wavelength (Å) central source z = 2.560 absorbers z ~ 2.527

  26. q11_039 a b c OVI central source z = 2.560 absorbers z ~ 2.527

  27. q11_039 a: -2360 - -2300 km s-1 OVI central source z = 2.560 absorbers z ~ 2.527

  28. q11_039 b: -2270 - -2220 km s-1 OVI central source z = 2.560 absorbers z ~ 2.527

  29. q11_039 c: -2190 - -2120 km s-1 OVI central source z = 2.560 absorbers z ~ 2.527

  30. q11_039 r1 Flux SiIV Wavelength (Å) central source z = 2.560 absorbers z ~ 2.527

  31. q11_039 a b c SiIV central source z = 2.560 absorbers z ~ 2.527

  32. q11_039 a: -2360 - -2300 km s-1 SiIV central source z = 2.560 absorbers z ~ 2.527

  33. q11_039 b: -2270 - -2220 km s-1 SiIV central source z = 2.560 absorbers z ~ 2.527

  34. q11_039 c: -2190 - -2120 km s-1 SiIV central source z = 2.560 absorbers z ~ 2.527

  35. q11_039 central source z = 2.560 absorbers z ~ 2.527

  36. Data analysis of all BAL QSOs (ITP-WHT) • Comparison with other method (power-law model, Arav’s group). Check compatibility for pure partial covering model with this method (q11_020, q11_039 compatible) • Variability (q11_030) • Line-locking • Estimation of the distances from the absorbers to the central sources (electron densities, VLT data)

  37. Data reduction of all BAL QSOs (ITP-WHT) • Errors in covering factors and optical depths from errors in Ib and Ir (errors in column densities and ionisation parameters from those ones) • Resampling for different exposures • Analysis of q11_020 and q11_039 (Ionisation parameters determination) • Compatibility with other method (Arav’s group) for pure partial covering model

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