Supermassive BHs do not correlate with DM haloes of galaxies

1. Supermassive BHs do not correlate with DM haloes of galaxies J. Kormendy & R. Bender 2011, Nature, 469, 377 2011 Feb 10 Sang Chul KIM (김상철)

2. Supermassive black holes (SMBHs) σ M● • Bigger BHs live in bigger bulges • “BH growth and bulge formation regulate each other” (“BHs and bulges coevolve.”)

3. M-sigma relation M● M● - σ relation χ2= 0.79 σ

4. M-L relation M● M● - L relation L

5. Bulge - disk Ferrarese (2002, ApJ, 578, 90)

6. Bulge - disk Baes et al. (2003, MN, 341, L44)

7. Bulge - disk • Ferrarese (2002, ApJ, 578, 90), Baes et al. (2003, MN, 341, L44) : correlation between BHs and the (non-baryonic) DM haloes • Vcirc – σ • circular rotation velocities of gas in the outer parts of galaxies, • where gravity is controlled by DM • DM also regulates BH growth. • unknown, exotic physics controls BH growth

8. Disk - DM Sancisi & van Albada (1987, IAU Symp 117, 67) Vcirc

9. BH – Disk ? Kormendy & Gebhardt (2001, 20th Texas Symp. Relativ. Astrophys, 363)

10. Correlations! Ferrarese 02 Disk Baes et al. 03 Vcirc bulge σ Kormendy & Gebhardt 01 M●-σrelation × Sancisi & van Albada 87 BH ? DM

12. Correlations! Disk bulge σ Vcirc M●-σrelation BH If ! DM • Vcirc should correlate tightly • with σeven in galaxies with no bulges

13. Vcirc – σrelation ? Fig 1 Bulgeless and pseudobulge galaxies (coloured points + N3198)  only a weak correlation between Vcirc and σ N2841 M31 N5457 (M101) N7331 N6946 N4258 9.2m Hobby-Eberly Telescope High Resolution Spectrograph - Instrumental vel. disp. = 8 km/s Vcirc-σrelation breaks down even at Vcirc = 210 km/s Black field circles – N3198, χ2= 0.25, r=0.95 Classical bulges pseudobulges + points : χ2=2.6, r=0.77

14. Metallicity Distribution Fu Ho (2007, ApJ, 668, 94)  weak correlation!

15. Is σ a surrogate for BH mass? Fig 1

16. M● - host galaxy properties

17. M● - host galaxy properties M● - σ relation M● - L relation E galaxies Classical bulges Pseudobulges NGC 2787 (a dominant pseudobulge + possibly a small classical bulge) Only a nuclear SC (neither a classical bulge, nor a large peudobulge) E galaxies S0 galaxies

18. M● - host galaxy properties Better! Good! M● - σ relation M● - L relation E galaxies Classical bulges Pseudobulges Classical bulges ~ E galaxies : both form by galaxy mergers Pseudobulges : high-density, central components in galaxies isolated galaxy disks evolve slowly as non-axisymmetries (such as bars) redistribute angular momentum  pseudobulges grow out of disk material  No correlation between M● - σ

19. M● - host galaxy properties χ2= 5.0, r=0.89 Better! χ2= 12.1, r=-0.82 Good! M● - σ relation M● - L relation E galaxies Classical bulges Pseudobulges NGC 2787 (a dominant pseudobulge + possibly a small classical bulge) Only a nuclear SC (neither a classical bulge, nor a large peudobulge) E galaxies S0 galaxies χ 2=10.4, r=-0.08 χ 2=63, r=0.27 χ 2=81, r=0.41 χ 2=11, r=0.29 Galaxy disks do not correlate with M● ! Classical bulge or E only!

20. BH – DM : none! χ 2=11, r=0.29 BHs do not correlate with DM!

21. Conclusion Ferrarese 02 Disk Baes et al. 03 Vcirc bulge σ Kormendy & Gebhardt 01 M●-σrelation × Sancisi & van Albada 87 BH × DM no correlation! No reason for the unknown, exotic physics of non-baryonic DM to control the BH growth

22. Thank you.

23. Kormendy, Bender, & Cornell 2011, Nature, 469, 374 M● - σ relation χ 2=5.0, r=0.89 M● - L relation χ 2=12, r=-0.82

24. Kormendy, Bender, & Cornell 2011, Nature, 469, 374 M● - L relation

25. Kormendy, Bender, & Cornell 2011, Nature, 469, 374 M● - σ relation