1. General Assembly of IAU, Symposium #238 Black Holes: From Stars to Galaxies Aug 22, 2006, Prague, Czech Republic Presented by: George Chartas (Penn State) In collaboration with: Cristian Saez(Penn State), Xinyu Dai(OSU), Michael Eracleous(Penn State), Niel Brandt(Penn State), Bret Lehmer(Penn State), Franz Bauer(Columbia), Gordon Garmire (Penn State) X-ray Spectral Evolution of AGN

2. Evolution of AGN Commonly used methods of studying the evolution of AGN include : (a) Determining the evolution of the optical and X-ray luminosity functions and optical and X-ray space densities of AGN. (b) Determining the evolution of the host galaxies. (c) Determining the evolution of the spectra of the AGN (  vs z,  ox vs z).

3. Evolution of Space Density of type-I AGN The space density of type-I AGN changes significantly with redshift and luminosity. The redshift at which the space density peaks changes with luminosity from z ~ 0.5-0.7 for logL x = 42-43 ergs s -1 to z ~ 2 for logL x = 45-46 ergs s -1. The amount of change in the space density is also strongly dependent on luminosity.  ~ 10 for logL x = 42-43 ergs s -1  ~ 100 for logL x = 45-46 ergs s -1 The space density of low luminosity AGN is found to decline at high redshift. Hasinger et al (2005)

4. Evolution of Host Galaxy Barger et al. 2005 The absolute rest-frame 5000 A luminosities of the host galaxies vs. redshift for sources in the ACS GOODS-North region of the CDF-N. Triangles : L X > 10 44 ergs s -1 Diamonds: L X = 10 43 - 10 44 ergs s -1 Squares: L X = 10 42 - 10 43 ergs s -1

5. Evolution of Quasars One might expect to detect a change in the X-ray emission and accretion properties of quasars to accompany the dramatic change in the number density of quasars between z=1 and z=2 (Fan et al. 2001). Many X-ray surveys have attempted to find such a change by constraining  and the optical-to-X-ray spectral index,  ox The evolution of  with z is still debatable (eg., Bechtold et al. 2003, Vignali et al. 2003, Grupe et al. 2005) There is no indication that  correlates with luminosity for low z quasars (George et al. 2000, Reeves & Turner 2000) Evolution of quasar comoving number density as a function of z (Fan et al. 2001)

6.  ox dependence on the 2500 A monochromatic luminosity. The main sample is given by filled circles, the high-z sample by open squares, and the Sy 1 sample by open Triangles. Strateva et al. (2005) Correlation of  ox with z, only 1 sigma significant if the l UV dependence is taken into account. Strateva et al. (2005) Dependence of a ox of AGN with UV luminosity and z

7. X-ray Spectra of Radio-Quiet Quasars at z > 4 Shemmer et al. (2005) performed an investigation of moderate-to- high quality X-ray spectra of 10 quasars (z = 4 - 6.28). They do not find any significant difference between the spectra of these high z quasars compared to ones at lower z. If quasars have been evolving constantly over time observations of the most distant ones may provided the most ``leverage'' for constraining any changes in the X-ray spectra over cosmic time.  = 1.97 +/- 0.05, N H < 3 X 10 21 cm -2 (mean values) Fe Kα EW < 190 eV and R < 1.2 χ 2 contours from joint fit for entire and common energy ranges

8. X-ray Spectra of Radio-Quiet Quasars at z > 4 Shemmer et al. (2005) find significant scatter of  but no systematic trend of  with absolute B magnitude and redshift. |d  /dz| < 0.04

9. Employing the lensing magnification effect to observe high redshift quasars allows us to probe the luminosity range of 10 43-45 ergs s -1. (This luminosity range is practically inaccessible by most Chandra observations of unlensed quasars of similarly high redshift.) The lensing magnification (from a few to ~ 100) allows us to obtain moderate to high S/N spectra The main scientific goal of our survey of quasars was to study the evolution of spectroscopic properties of high redshift RQQs by searching for a possible correlation between photon index  and luminosity for high redshift quasars Gravitational lensing as a tool to study AGN evolution

10. Evolution of Radio Quiet AGN  - L X diagram from our recent analyses of high redshift (z > 1.5) radio quiet AGN. Significant correlations are found between  and the 0.2-2keV (2- 10keV) luminosities. The correlations are significant at the 99.9997% (98.6%) confidence levels, respectively. (Dai, Chartas, Eracleous & Garmire 2004)

11. Evolution of Radio Quiet Quasars Photon index vs. 2-10 keV luminosity for low redshift (z < 0.1 mostly) AGN. No significant correlation is found (George et al. 2000)

12. Evolution of Radio Quiet AGN To confirm the previously observed correlation between  and luminosity we have: Observed additional high z lensed AGN as part of the Chandra GTO program Have analyzed moderate-to-high redshift radio quiet AGN observed in the deep field observations performed with Chandra The larger sample allowed us to: Place tighter constraints on the correlation Test the correlation in narrower redshift bands and thus better constrain the epochs at which possible changes in the average emission properties of AGN occurred.

13. Evolution of Radio Quiet AGN Recent lensed high redshift AGN observed with Chandra and added to our sample Q 0142-100 BRI 0952-0115 Q 1017-207 SBS 1520+530 SDSS 0903+5028 Object z s ms Exposure (ks) 2.72 4.50 2.55 1.59 3.605 I=16.47 I=18.3 I=16.78 I=17.61 R=19.56 15 20 15 20

14. Evolution of Radio Quiet AGN

15. Using Chandra Deep Field Observations to Study AGN Evolution

16. N Counts 0500100015002000 1.0 10.0 100.0 1000.0 Number of Sources > N Counts CDF - S, z > 1.5 CDF - N, z > 1.5 CDF - S CDF - N

17. Using Chandra Deep Field Observations to Study AGN Evolution Source Selection l Selected the radio-quiet AGN from the CDF surveys with Nph (0.5-8 keV) > 200 cnts (~130 sources with z > 0.5) l Radio loud objects were filtered out using R = f 5GHz /f 4400A > 10 Afonso et al. (2006), Richards (2000) (~22/152 RLQs, ~14%). Spectral Analysis l 200 < Nph < 600 Cash statistic Nph > 600  2 statistic l Model : Absorbed power-law l Fitting range: (a) 0.5-7keV observed frame (b) 2-10keV rest frame

18. Using Chandra Deep Field Observations to Study AGN Evolution

20. Histograms of  and N H = 1.64 +/- 0.34 ~ 2.6 x 10 22 cm -2

21. Using Chandra Deep Field Observations to Study AGN Evolution Correlation Results:  - L(2-10 keV) & 1.6 < z < 3.3 Spearman: r c = 0.57 P(r > r c ) = 7.1 x 10 -4 Pearson: r = 0.55 P(r > r c ) = 1.1 x 10 -3  - L(2-5 keV) & 1.6 < z < 3.3 Spearman: r c = 0.59 P(r > r c ) = 4.3 x 10 -4 Pearson: r e = 0.61 P(r > r e ) = 2.3 x 10 -4 All spectral fits performed in the 0.5-7 keV observed frame

22. Using Chandra Deep Field Observations to Study AGN Evolution Correlation Results:  - L(2-10 keV) & 1.6 < z < 3.3 Spearman: r c = 0.43 P(r > r c ) = 2.4 x 10 -2 Pearson: r c = 0.49 P(r > r c ) = 7.6 x 10 -3  - L(2-5 keV) & 1.6 < z < 3.3 Spearman: r c = 0.54 P(r > r c ) = 2.9 x 10 -3 Pearson: r c = 0.61 P(r > r c ) = 5.8 x 10 -4 All spectral fits performed in the 2-10 keV rest-frame

23. Using Chandra Deep Field Observations to Study AGN Evolution

24. Correlation Results:  - L(2-10 keV) & 1.6 < z < 3.3 Spearman (1e43 - 5e45erg/s): r c = 0.6 P(r > r c ) = 5 x 10 -7 Pearson (1e43 - 2e45erg/s): r c = 0.51 P(r > r c ) = 1.4 x 10 -4

25. Using Chandra Deep Field Observations to Study AGN Evolution Possible Interpretations of the L X -  Correlation First Interpretation Narrow range of M at high z Large range of accretion rate Second Interpretation Narrow range of accretion rate at high z Large range in M

26. Using Chandra Deep Field Observations to Study Quasar Evolution Physical Interpretations of L X -  Hot corona model by Haardt et al. 1997 predicts that  increases with  of the corona  decreases with T of the corona If the corona is dominated by electron-positron pairs this model also predicts that  Log Lx

27. Conclusions We confirm the Lx -  correlation for radio quiet AGN at high z based on the spectral analysis of the CDF surveys. We find that the strength of Lx -  correlation is z dependent and peaks at z ~ 2.2 The Hot Corona model predicts the Lx -  correlation The redshift dependence of the correlation suggests that quasars near the peak of their comoving number density are accreting near Eddington and have different accretion properties than their low-z counterparts

28. Under the assumptions: (a)that high-z quasars emit near Eddington (b)that the optical depth  of the corona is dominated by electron-positron pairs. (c)The observed range in luminosity is due to a range in BH masses (~ 2-3 orders of magnitude) the hot corona model of Haardt & Maraschi 1993 predicts :  log[L(2-10keV)] The redshift dependence of the correlation implies that quasars near the peak of their comoving number density are accreting near Eddington and have different accretion properties than their low-z counterparts Evolution of Radio Quiet Quasars Possible Interpretation of  -L x is based on the hot corona model (Haardt & Maraschi 1993, Haardt, Maraschi, & Ghisellini 1997)

29. Conclusions (a)The spectral slope of the 1.4 < z < 4 radio-loud quasars appears not to vary significantly over 4 orders of magnitude in 2-10 keV luminosity. We do not find a significant correlation between the spectral slope  and X-ray luminosity as found in our 1.5 < z < 4 radio-quiet quasar sample. (b)The spectral slopes of the radio-loud quasars of the sample are significantly flatter than those of the radio-quiet sample possibly due to contamination from jet emission. (c)The limited number of quasars in the present sample combined with the medium S/N of several of the observations may have led to an unaccounted for systematic effect. Additional observations of z ~ 2 lensed radio-loud quasars with better S/N will allow us to obtain tighter constraints on a possible correlation between  and X-ray luminosity. (d) The X-ray variability of the high redshifts radio-loud quasars of our sample is consistent with the known correlation between excess variance and luminosity observed in NLS1s when extrapolated to the larger luminosities of the present sample.

30. CREDITS Director George Chartas Actors Xinyu Dai Michael Eracleous Digital Camera Personnel Gordon Garmire

31. Haardt, Maraschi, & Ghisellini (1997) predicted:  increases with , the optical depth of the Compton scattering.  decreases with T, the temperature of the corona. Model Predictions  Optical Depth of IC Scattering  Temperature of Corona

32. Haardt, Maraschi, & Ghisellini (1997) also predicted: In COMPACT CORONA, where the pair production dominates,  Log Lx This is similar to what we have observed. In a “Compact” Corona

33. Two Possible Interpretations of the Correlation Narrow range (of order a few) of M at high redshift. Large range of. First Interpretation

34. Opposite. The range is narrow, close to Eddington limits, and M range is large. The l c is the “compactness” of the corona. Haardt & Maraschi (1993) predicted that M  l c,  increases as l c increases. Second Interpretation  l c (Coronal Compactness) Consistent with semianlyti- cal model of Hauffmann & Haehnelt (2000) for the cosmological evolution of super massive black hole and their fueling rates.

35. Evolution of Radio Quiet Quasars We recently presented results from a survey of relatively high redshift (1.5<z<4) gravitationally lensed radio-quiet quasars (RQQs) observed with the Chandra and XMM-Newton (Dai et al. 2004).

36. Using gravitational lensing as a tool to study the evolution of distant quasars Gravitationally Lensed High-z Radio Quiet Quasars Near Eddington Luminosites at redshifts above z~1.5 High-z Radio Quiet Quasars from the Chandra Deep Field Surveys Conclusions Evolution of Quasars

37. Gravitational lensing as a tool to study AGN evolution Conceptual diagram of the gravitational deflection of light in a quad GL system.

38. Understanding the Evolution of Quasars Soft photons IC scattering Black Hole Accretion Disc Corona

39. Using Chandra Deep Field Observations to Study AGN Evolution Histograms of Lx and z