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 )

Supermassive black holes (SMBHs)

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Bigger BHs live in bigger bulges

“BH growth and bulge formation regulate each other” (“BHs and bulges coevolve.”)

M● σ

M-sigma relation

M●

σ

χ2= 0.79

M● - σ relation

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M-L relation

M●

L

M● - L relation

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Bulge - disk

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Ferrarese (2002, ApJ, 578, 90)

Bulge - disk

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Baes et al. (2003, MN, 341, L44)

Bulge - disk

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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

Disk - DM

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Sancisi & van Albada (1987, IAU Symp 117, 67)

Vcirc

BH – Disk ?

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Kormendy & Gebhardt (2001, 20th Texas Symp. Relativ. Astrophys, 363)

DiskVcirc

Baes et al. 03

Ferrarese 02

Correlations!

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bulgeσ

BH

M●-σ relation

Sancisi & van Albada 87

DM

×Kormendy &

Gebhardt 01

?

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DiskVcirc

Correlations!

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bulgeσ

BH

M●-σ relation

DM

If !

Vcirc should correlate tightly

with σ even in galaxies with no bulges

Vcirc – σ relation ?Fig 1

Bulgeless and pseudobulge galaxies (coloured points + N3198)

only a weak correlation between Vcirc and σ

9.2m Hobby-Eberly Telescope

High Resolution Spectrograph

- Instrumental vel. disp. = 8 km/s

N5457 (M101)

N6946

Vcirc-σ relation breaks down even at Vcirc = 210 km/s

N4258

N2841

M31N7331

Classical bulges

pseudobulges

Black field circles – N3198,

χ2= 0.25, r=0.95

+ points :

χ2=2.6, r=0.7713

Metallicity Distribution FuHo (2007, ApJ, 668, 94)

weak correlation!

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Is σ a surrogate for BH mass?

Fig 1

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M● - host galaxy properties

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M● - host galaxy properties

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

M● - L re

lation

M● - σ relation

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M● - host galaxy properties

E galaxies

Classical bulges

Pseudobulges

M● - L re

lation

M● - σ relationGood!

Better!

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

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M● - host galaxy properties

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

M● - L re

lation

M● - σ relation

χ2 = 12.1, r=-0.82

Good!

χ 2= 5.0, r=0.89 Better!

Galaxy disks do not correlate with M● !

Classical bulge or E only!

χ 2=63, r=0.27

χ 2=10.4, r=-0.08

χ 2=81, r=0.41 χ 2=11,

r=0.29

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BH – DM : none!

BHs do not correlate with DM!

χ 2=11, r=0.29

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DiskVcirc

Baes et al. 03

Ferrarese 02

Conclusion

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bulgeσ

BH

M●-σ relation

Sancisi & van Albada 87

DM

×Kormendy &

Gebhardt 01

no correlation!

×

No reason for the unknown, exotic physics of non-baryonic DM to control the BH growth

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Thank you.

Kormendy, Bender, & Cornell 2011, Nature, 469, 374

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M● - L relation

M● - σ relation

χ 2=12, r=-0.82

χ 2=5.0, r=0.89

Kormendy, Bender, & Cornell 2011, Nature, 469, 374

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M● - L relation

Kormendy, Bender, & Cornell 2011, Nature, 469, 374

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M● - σ relation