1. Reverberation Mapping - Extending the Luminosity Range Shai Kaspi Tel-Aviv University & Technion – Haifa Israel “AGNs: From Atoms to Black Holes” Tel-Aviv University, 22 February 2006 A black hole obsessed/addict …it’s Hagai’s fault….

2. Outline - Introduction to reverberation mapping by B. Peterson - Current BLR Size – Luminosity Relation - Broadening the luminosity range - Mapping low luminosity AGNs - Mapping of high-luminosity quasars – preliminary results Maoz D., Netzer H., Peterson B.M., Vestergaard M., Jannuzi B. (Kaspi et al. 2005, ApJ, 629, 61) Maoz D., Netzer H., Brandt W.N., Schneider D.P., Shemmer O. (Kaspi et al. in preparation) Laor A., Maoz, D., Peterson B., Filippenko A.

3. Peterson et al. (2004) compiled all studies to date. 35 objects with Balmer (mainly H  ) lines time lag. Characteristic BLR size = Time Lag * speed of light. The BLR size – luminosity relation Both are measured quantities. Luminosities in the Optical, UV, and X-rays. BLR size from averaging all Balmer lines time lag. Reverberation Mapping

4. Linear Regression Uncertainties in both quantities And Intrinsic scatter in the relation Two regression methods: 1. FITEXY from Press et al. (1992) implemented by Tremaine et al. (2002). 2. BCES (Bivariate Correlated Errors and intrinsic Scatter) by Akritas & Bershady (1996). …and also outlier points…

5. H  R BLR – Optical luminosity (5100 A) R BLR    [ L (5100 Å)] (0.69±0.05)

6. H  R BLR – Optical luminosity (5100 A) R BLR    [ L (5100 Å)] (0.518±0.039) ( Bentz et al. Aph/0602412 )

7. H  R BLR – UV luminosity (1450 A) R BLR   [ L (1450 Å)] (0.56±0.05) 58 points 32 points

8. R BLR – X-ray luminosity (2-10 keV) 54 points 30 points R BLR  [ L (2-10 keV)] (0.70±0.14)

9. R BLR – luminosity Relation, conclusions Though small differences exist between the different regression methods the results are generally consistent. Average slope is 0.67±0.05 for the optical continuum and broad Hβ luminosity, about 0.56±0.05 for the UV luminosity, and about 0.70±0.14 for the X-ray luminosity. We find in these relations an intrinsic scatter of about 40%. In most energy bands the slope is roughly like the naive theoretical prediction of 0.5. This prediction is naively based on the assumption that all AGNs have the same ionization parameter, BLR density, column density, and ionizing SED. 0.52±0.04

10. Broadening the Luminosity range - H  Current studies span 4 orders of magnitude. We need to expand the luminosity range with reverberation mapping studies. There are 4 more orders of magnitude to be explored. Extrapolation does not necessarily give the real situation.

11. Broadening the Luminosity range – C IV Up to 2004 only four AGNs with C IV BLR size measurements

12. Broadening the Luminosity range – C IV Peterson et al. (2005) added NGC4395 four orders of magnitude in luminosity lower

13. Broadening the Luminosity range – C IV Still there are the high luminosity quasars at three orders of magnitude higher

14. Higher luminosities monitoring Photometrically monitoring 11 quasars for the past decade. 7 of which are spectroscopically monitored for the past 5 years. 2.1 < z < 3.2 10 45.6 < L (5100 Å) < 10 47 erg/s Photometric observation at the 1m Wise Observatory. Spectroscopic observation at 9m Hobby-Eberly Telescope (HET) and at the Wise Observatory. Lines monitored are C IV and Ly  using the method of a comparison star simultaneously with the quasar in the slit. … Some preliminary results… (Kaspi et al. in preparation)

15. Continuum light curves Z log L  R  B 2.628 46.14 0.34 0.44 3.177 46.88 0.16 0.22 2.172 46.05 0.34 0.44 2.824 46.62 0.25 0.27 3.200 46.96 0.14 0.19 2.722 47.04 0.16 0.20

16. SBS 1116+603 L (5100 Å) = 1.4×10 46 erg/s z = 2.628  R=0.34  B=0.44

17. SBS 1116+603 : C IV – Continuum CCF No measurable time lag is found

18. S4 0636+68 L (5100 Å) = 7.6×10 46 erg/s z = 3.117  R=0.16  B=0.22

19. HS 1700+6416 L (5100 Å) = 10 47 erg/s z = 2.722  R=0.16  B=0.20

20. S5 0836+71 L (5100 Å) = 1.1×10 46 erg/s z = 2.172  R=0.34  B=0.44

21. S5 0836+71: C IV – Continuum CCF Rest frame time lag: 188 +27 days -37

22. Broadening the Luminosity range – C IV A preliminary result suggest a correlation between the C IV size and the luminosity

23. Mass – Luminosity Relation S5 0836+71: M  Peterson et al. (2005).

24. Scaling C IV size to H  size NGC4395: CIV lag: min ⇒ H  lag about: min In two weeks, optical monitoring of NGC4395 spectroscopically from KPNO and photometrically from four observatories around the world cover 22 hours a day for four days. S5 0836+71: CIV lag: days ⇒ H  lag about: days

25. Summary In the 10 42 to 10 46 erg/s luminosity range a firm relation exist between the BLR size and luminosity. Slope ranging from 0.5 to 0.7. Expanding the luminosity range is important and first steps are being taken: Low luminosity Seyferts and LINERS to cover the luminosity range of 10 40 to 10 42 erg/sec. High luminosity quasars – preliminary results are encouraging. When this long term project is concluded reverberation mapping studies will cover the luminosity range up to 10 47 ergs/s, an additional one order of magnitude to the current luminosity range and 7 orders of magnitude in total. Dust Reverberation mapping (torus size?)