1. The Large Scale Structure of Seyferts and LINERs and Implications for their Central Engines Anca Constantin Drexel University AGN are not unbiased tracers of the whole galaxy population, with respect to mass: - Seyferts are less clustered than galaxies  less massive but actively accreting BHs - LINERs cluster like galaxies.  more massive but weakly active BHs --with thanks to Michael Vogeley

2. The SDSS main galaxy sample -DR2 2627 sq. deg. footprint area ~250,000 galaxies with spectra 0 < z <~ 0.3 r dered < 17.77 Broad-line objects ( spectroscopically flagged as QSOs ) excluded

3. The SDSS main galaxy sample -DR2 2627 sq. deg. footprint area ~250,000 galaxies with spectra 0 < z <~ 0.3 r dered < 17.77 Broad-line objects ( spectroscopically flagged as QSOs ) excluded “ Best ” absolute magnitude limited sample

4. Finding AGN among SDSS galaxies Seyferts H II nuclei LINERs Transition objects emission-line 20% of all galaxies are strong line-emitters among which: 52% H II 20% (pure) LINERs 7% Transition Objects 5% Seyferts

5. The Clustering Amplitude r 0 : H IIs: r 0 = 5.7  0.2  less clustered than galaxies Seyferts: r 0 = 6.0  0.6  less clustered than galaxies LINERs: r 0 = 7.3  0.6  clustered like galaxies r 0 is measured in h -1 Mpc = scale where the probability of finding a galaxy pair is 2  random all galaxies: r 0 = 7.8  0.5 Absolute Magnitude limited samples, -21.6 <M < -20.2

6. The Clustering Amplitude r 0 : H IIs: r 0 = 5.7  0.2  less clustered than galaxies Seyferts: r 0 = 6.0  0.6  less clustered than galaxies LINERs: r 0 = 7.3  0.6  clustered like galaxies r 0 is measured in h -1 Mpc = scale where the probability of finding a galaxy pair is 2  random all galaxies: r 0 = 7.8  0.5 higher peaks in the density field are more clustered Seyferts & H II’s : - less massive Dark Matter halos LINERs : - more massive Dark Matter halos Absolute Magnitude limited samples, -21.6 <M < -20.2

7. The Clustering Amplitude r 0 : H IIs: r 0 = 5.7  0.2  less clustered than galaxies Seyferts: r 0 = 6.0  0.6  less clustered than galaxies LINERs: r 0 = 7.3  0.6  clustered like galaxies r 0 is measured in h -1 Mpc = scale where the probability of finding a galaxy pair is 2  random all galaxies: r 0 = 7.8  0.5 higher peaks in the density field are more clustered Seyferts & H II’s : - less massive Dark Matter halos LINERs : - more massive Dark Matter halos Absolute Magnitude limited samples, -21.6 <M < -20.2 M BH Seyferts < M BH LINERs M DM halo ~ M BH (Ferraresse 2002, Baes et al. 2003)

8. Driven by the host morphology? H IIsSeyferts LINERs blue red-ish red-ish, KS color = 0.617 late type earlier types like Seyferts! KS conc = 0.104 bluered early late

9. Driven by the host morphology? NO! H IIsSeyferts LINERs blue red-ish red-ish, KS color = 0.617 late type earlier types like Seyferts! KS conc = 0.104 bluered early late

10. Low L[O I]: r 0 = 13.15  1.09 LINER dominated High L[O I]: r 0 = 6.1  0.3 H II dominated Low L[O III]: r 0 = 8.8  0.7 LINER dominated High L[O III]: r 0 = 6.2  0.6 almost no LINERs! mostly H II high L[O I] high L[O III] low L[O I] low L[O III] lowest L [O I],[O III] objects = strongly clustered highest L [O I],[O III] objects = weakly clustered

11. Different availability of fuel? LINERs show particularly low levels of obscuration & gas densities Seyferts exhibit generally high gas densities & moderately high N HI

12. Summary & Possible interpretation H IIs SeyfertsLINERs hosts : blue red-ish red-ish, late type earlier types like the Seyferts r 0 : weakly weakly clustered like clusteredclustered average galaxies fueling average relatively high (very) low rate:- efficient?-inefficient? gas low high lower than density: in Seyferts obscuration: high wide range (very) low BH mass: small small large life-time: ? short long Constantin & Vogeley 2006, in ApJ today

13. Stellar massBH mass Accretion rate, [O I]Accretion rate, [O III] Stellar ages Obscuration Dist to 3rd nearest Dist to 1st nearest