1 / 42

Sarah Gallagher (UCLA) January 2007

Stratified Quasar Winds Revealed. Sarah Gallagher (UCLA) January 2007. (Urry & Padovani 1995). The Quasar Epoch: z=2-3. (Richards et al. 2006a; Nagamine et al. 2006). Normal Quasar. Ly  CIV  MgII H  H . Quasars with Outflows: BAL Quasars.

habib
Download Presentation

Sarah Gallagher (UCLA) January 2007

An Image/Link below is provided (as is) to download presentation Download Policy: Content on the Website is provided to you AS IS for your information and personal use and may not be sold / licensed / shared on other websites without getting consent from its author. Content is provided to you AS IS for your information and personal use only. Download presentation by click this link. While downloading, if for some reason you are not able to download a presentation, the publisher may have deleted the file from their server. During download, if you can't get a presentation, the file might be deleted by the publisher.

E N D

Presentation Transcript

  1. Stratified Quasar Winds Revealed Sarah Gallagher (UCLA) January 2007 (Urry & Padovani 1995)

  2. The Quasar Epoch: z=2-3 (Richards et al. 2006a; Nagamine et al. 2006)

  3. Normal Quasar LyCIV MgII H H

  4. Quasars with Outflows: BAL Quasars voutflow ~ (0.03-0.2)c Ly/NV SiIV CIV Broad Absorption Lines (P Cygni profiles)

  5. Infrared Optical-UV X-ray `big blue bump’ lt days `torus’ 1-10 pc `corona’ ~AUs NASA/CXC

  6. A Model for AllRadio-Quiet Quasars UV emission lines ~light yr (1017 cm) X-ray continuum source ~light hrs (1014-15 cm) UV/optical continuum source ~light hrs-days (1016 cm) (Gallagher et al. 2002a: Adapted from Königl & Kartje 1994; Murray et al. 1995)

  7. Two Views Through the Wind X-ray UV shielding gas Broad Absorption Line (BAL) Quasars BAL Wind Does it exist?

  8. X-ray Properties of Quasars 2 keV 2500 Å aox = 0.384 log (f2 keV / f2500 Å) (Laor et al. 1997)

  9. UV Luminosity vs.aox brighter in X-rays Define: Daox=aox -aox (Luv) fainter in X-rays log(Luv) (ergs s-1 Hz-1) 228 SDSS Quasars with ROSAT(Strateva et al. 2005)

  10. Bright Quasar Survey z<0.5 Sample BAL Quasars Daox X-ray weak (400x) X-ray normal 55 BQS Quasars with z<0.5(Data from Brandt, Laor, & Wills 2000)

  11. X-ray Absorption by Neutral Gas G = 2 NH = almost optically thick to Compton scattering (assuming solar metallicity)

  12. PG 2112+059 (z=0.466): First BAL Quasar X-ray Spectra G = 1.97±0.25; NH ~ 1022 cm-2 (Gallagher et al. 2001)

  13. X-ray Spectroscopy of ~12 RQ BAL Quasars • normal underlying X-ray continua • significant intrinsic absorption • NH = (0.1-5.0) x 1023 cm-2 • from >5 keV continuum: • normal aox (UV/X-ray flux ratio) • not just simple absorption • partial coverage and/or ionized gas (e.g., Gallagher et al. 2002b; Chartas et al. 2002, 2003; Aldcroft & Green 2003; Grupe et al. 2003; Page et al. 2005; Shemmer et al. 2005)

  14. PG 2112+059 Revisited: Dramatic Spectral Variability PG 2112+059:ASCA Oct 1999;ChandraSep 2002 (Gallagher et al., 2004)

  15. PG 2112+059 Revisited: Comparison of Models FeKa (Gallagher et al. 2004)

  16. Major Change  Increased NH + + Chandra ASCA Partial-covering absorber model

  17. fl (erg cm2 s1 Å) O VI Observed Wavelength (Å) Little Variability in UV BALs

  18. Chandra BAL Quasar Survey Large, well-defined sample • 35 luminous BAL quasars • z = 1.4—2.9 • MB ~ -26.1 to -28.4 • UV spectra for all (from literature) • 4—7 ks exploratory observations • 35 observed; 27 detected (77%) (Gallagher et al. 2006) Collaborators: Niel Brandt, George Chartas, Gordon Garmire (Penn State), Robert Priddey (Hertfordshire), & Rita Sambruna (Goddard)

  19. Exploratory Surveys: X-ray Data • Rough continuum shape: GHR • from hardness ratio: (hard-soft)/(hard+soft) (analogous to B-V spectral index) • Relative UV-to-X-ray power: Daox

  20. All RQ BAL quasars show evidence for X-ray absorption (complex with NH ~ (1—80)x1022 cm-2) Spectral Shape vs. X-ray Weakness: X-ray Faint  X-ray Hard normal RQ quasars: G = 2.0 ± 0.25 Daox = 0.0 ± 0.15 Softer (less absorbed) Harder (more absorbed) % covered Daox Fainter Brighter

  21. Bright Quasar Survey z<0.5 Sample BAL Quasars Daox X-ray weak (400x) X-ray normal 55 BQS Quasars with z<0.5(Data from Brandt, Laor, & Wills 2000)

  22. BQS + Chandra BAL Quasars Chandra BALQs Daox No correlation for BAL quasars.

  23. UV Spectra:X-ray Bright vs. X-ray Weak CIV CIV SiIV SiIV X-ray BRIGHT X-ray FAINT

  24. vmaxvs. Daox te~1 Daox High velocity appears to require large NH.

  25. Conclusions I:X-ray Observations • compact & thick ‘X-ray—only’ absorbers • X-ray & UV absorption not consistent • NH and variability properties • some may be Compton-thick! • (te ~ 1; NH~1.5x1024 cm2) (Gallagher et al. 2006)

  26. X-ray and UV Continua Emitting Regions Are Not Cospatial • Implied by Compton-thick X-ray absorption. • Consistent with results from gravitational micro-lensing. (Kochanek et al. 2006)

  27. Conclusions I:X-ray Observations • compact & thick ‘X-ray—only’ absorbers • X-ray & UV absorption not consistent • some may be Compton-thick! • (te ~ 1; NH~1.5x1024 cm2) • likely correlation of vmax & Daox • first UV/X-ray correlation found  supports radiative driving of UV outflows (Gallagher et al. 2006)

  28. Link Between Shielding Gas and vmax thinner shield  less X-ray weak thicker shield  more X-ray weak larger Rlaunch  lower vterm smaller Rlaunch  higher vterm • (Gallagher et al. 2006; Gallagher & Everett 2007) vterm ~ (GMBH/Rlaunch)1/2 • (cf. Chelouche & Netzer 2000; Everett 2005)

  29. IR Opt-UV X-ray `big blue bump’ <1 pc `torus’ 1-10 pc `corona’ ~AUs disk wind from here NASA/CXC

  30. The Dusty Outflow • The inner radius of the dusty outflow is set by the temperature at which dust sublimates: • r=1.3(Luv/1046)½(T/1500)-2.8 pc (Adapted from Königl & Kartje 1994)

  31. Sample SEDs of Non-BAL Quasars mid-infrared optical 8 m 5000 Å spectral indices (L~ ): ,ir,opt

  32. IR-Luminous Quasars Typically Have Steeper Spectral Slopes (Gallagher et al., submitted)

  33. IR-Luminous Quasars Show Spectral Curvature

  34. F (erg s-1 cm-2 Hz-1) 1200 K black body  (Å) Sample ‘Hot Bump’ (Rodríguez-Ardila& Mazzalay 2006)

  35. Changing Shape of Dusty Outflow? Less Luminous More Luminous

  36. BAL Quasar IRS Spectra silicates (Gallagher et al. in prep; see also Shi et al. 2006)

  37. Clouds and a Torus (Urry & Padovani 1995)

  38. Multiwavelength Synthesis: The Stratified Wind Picture

  39. Physical Parameters of the Stratified Wind

  40. Stratified Wind Driving Mechanisms • UV BAL wind • Radiation pressure on UV resonance lines • Dusty Outflow • Radiation pressure on dust • Shielding Gas • Continuum radiation pressure • Magneto-hydrodynamic driving?

  41. Future Work 1. Accepted Spitzer Cycle 3 theory project. Illuminating the Dusty Wind: 3D Modeling of Quasar Silicate Emission Collaborators: John Everett (Wisconsin) & Dean Hines (SSC) 2. Chandra follow-up of vmax vs. ox correlation. 3. Suzaku (10-30 keV) follow-up of nearby Compton-thick BAL quasars. 4. Long term: Constellation-X spectroscopy of X-ray outflows in absorption.

  42. Resolving the Shielding Gas with Constellation-X Model: Two component outflow with different ionization states, velocities, and velocity dispersions. (Flux matches BAL quasar PG1115+080.)

More Related