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

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

I. Black Hole - Bulge Relation Black hole mass / bulge mass ~ 0.006 (0.002) (Maggorian et al. 1998, AJ, 115, 2285 )

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)

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)

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)

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

High-z Quasars CO molecular emissions have been detected in a number of hi-z quasars, including SDSS J114816.64 + 525150.3 (z=6.42) Walter et al. (2004, ApJL)

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. 2006 ApJ, 641, 683) =FWHM(CO)/2.35 (Shields et al. 2006)

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)

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)

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)

3. Narrow CO PG Quasars Are two narrow CO PG quasars the outliers? PG 0838+770 (FWHM=60km/s) and PG 1415+451(FWHM=90km/s) (Shields et al. 2006)

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

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

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)

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

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)