1. On the Outliers of the Black Hole - Bulge Relation
Xue-Bing Wu
(Peking University)

2. Outline Black Hole - Bulge Relation High-z Quasars
Narrow CO PG Quasars
NLS1s
Discussions

3. I. Black Hole - Bulge Relation
Black hole mass / bulge mass ~ (0.002) (Maggorian et al. 1998, AJ, 115, 2285 )

4. Black Hole - Bulge Relation
Black hole mass - bulge stellar velocity relation (M -  relation) (Gebhardt et al. 2000; Merritt & Ferrarese 2000; Tremaine et al. 2002)
MBH 4
Tremaine et al. (2002)

5. Black Hole - Bulge Relation
Two of the first works using the M -  relation to estimate AGN BH mass (Wu & Han, 2001, A&A, 380, 31; Wu & Han, 2001, ApJ, 561, L59)
“Abstract: We estimated black hole masses for 9 Seyfert 1 and 13 Seyfert 2 galaxies in the Palomar and CfA bright Seyfert samples using the tight correlation between black hole mass and bulge velocity dispersion…”
(Woo & Urry 2002, ApJ)

6. Black Hole - Bulge Relation
Physics origin of the black hole -bulge relation
Close tie between BH and galaxy formation
Feedback scenario (Silk & Rees 1998; King 2003, 2005;…)
Xu, Wu & Zhao (2007 ApJ, in press) (a later talk by BingXiao Xu)

7. 2. High-z Quasars How about the M -  relation at Hi-z?
Black hole mass of hi-z quasars can be estimated using the R-L relation (3E9 solar mass for the BH of a quasar at z=6.4)(Willott et al. 2003; Barth et al. 2003)
How to estimate  at hi-z?
Direct measurement is difficult
Narrow line such as [OIII]? No

8. High-z Quasars
CO molecular emissions have been detected in a number of hi-z quasars, including SDSS J (z=6.42)
Walter et al. (2004, ApJL)

9. High-z Quasars
Hi-z quasars, outliers??
CO molecular line detected for a number of hi-z quasars (Solomon & Vanden Bout 2005 ARA&A)
CO line width as a surrogate for  (Shields et al ApJ, 641, 683)
=FWHM(CO)/2.35
(Shields et al. 2006)

10. High-z Quasars Wu (2007, ApJ) Can we use =FWHM(CO)/2.35 ??
A test with CO detected 33 Seyfert galaxies (Wu 2007, ApJ, 657, 177)
A better correlation using inclination-corrected line width
CO molecular disk coplanar with the galaxy disk (Heckman et al. 1989)
Wu (2007, ApJ)

11. High-z Quasars
Assuming inclination ~15o of hi-z quasars, we can re-estimate  values using the inclination-corrected CO line width and study the M -  relation at Hi-z
Wu (2007, ApJ)

12. High-z Quasars
Small inclinations (~15o) are also probably needed to explain the narrowness of CO line of hi-z quasars compared with the sub-millimeter galaxies (SMG) (Greve et al. 2005; Carilli & Wang 2006)
Carilli & Wang (2006,AJ)

13. 3. Narrow CO PG Quasars Are two narrow CO PG quasars the outliers?
PG (FWHM=60km/s) and PG (FWHM=90km/s)
(Shields et al. 2006)

14. Narrow CO PG Quasars PG 1415+451(FWHM(CO)=90km/s)
=11512 km/s (Kauffman et al. 2003, MNRAS)
Clearly, =FWHM(CO)/2.35 If
i=15o

15. Narrow CO PG Quasars PG 0838+770 (FWHM=60km/s) No  measurement
FWHM([OIII])=533 km/s (Shields et al. 2006)
If =FWHM([OIII])/2.35  =227 km/s If
i=5o

16. Narrow CO PG Quasars Narrow CO PG quasars are almost face-on (~5o-15o)
=FWHM(CO)/2.35 can not apply to them
They are not outliers of the M -  relation (If the proper  values can be obtained)

17. 3. NLS1s (narrow line Seyfert 1s)
True outliers?!
Supported by the study with a large sample of NLS1s from SDSS (Zhou et al. 2006)

18. 4. Discussions
Accurate measurements of BH mass and stellar velocity dispersion for a large sample of normal and active galaxies
Hi-z sources ( evolution of the BH – bulge relation?); mm astronomy with ALMA
NLS1s?
Theoretical works
Carilli et al. (2007)