supermassive bhs do not correlate with dm haloes of galaxies
DESCRIPTION
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). σ. M ●. Bigger BHs live in bigger bulges - PowerPoint PPT PresentationTRANSCRIPT
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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