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Hello!. Galaxy Morphology, SuperMassive Black Holes and all that. Galaxies Near and Far. Ajit Kembhavi IUCAA, Pune. Sudhanshu Barway Yogesh Wadadekar Vinu Vikram Abhishek Rawat C.D. Ravi Kumar Habib Khushroshahi. Hubble’s Tuning Fork. Lenticular. - PowerPoint PPT PresentationTRANSCRIPT
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Hello!
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Ajit Kembhavi IUCAA, Pune
Galaxies Near and Far
Galaxy Morphology, SuperMassive Black Holes
and all that
Sudhanshu Barway Yogesh Wadadekar
Vinu Vikram Abhishek Rawat
C.D. Ravi Kumar Habib Khushroshahi
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Hubble’s Tuning Fork
Lenticular
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Lenticular galaxies are a morphological transition class between ellipticals and early type spirals.
B/T ratios, colors and spectral properties, neutral and molecular gas fraction, star formation rate, average luminosity, M/L ratio are intermediate to ellipticals and spirals.
Bulges of lenticulars are very similar to ellipticals. Their disk are similar to those of early type spirals, but they have no spiral arms.
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Surface Brightness Distribution
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NGC 661 V
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Surface Brightness Profile
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Bulge –Disk Decomposition
UGC 1250
2 = (oi-mi)2/i2
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Bulge-Disk Decomposition
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Morphological Parameter
Correlations
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The Fundamental Plane
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log re = A log + B log Ie + c
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Fundamental Plane for Morphological Mix of Galaxies
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The Photometric Plane
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2-D Correlations
Ellipticals and Early Type
Bulges
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Photometric Plane
Ellipticals and Early Type
Bulges
Khoshroshahi etal ApJL 2000
EllipticalsEarly type bulges
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Photometric Plane
Ellipticals Lenticulars
Dwarf Ellipticals Bulges
Residuals
Ravikumar etal AA 2006
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Bulge-Disk Correlations in Lenticular Galaxies
Barway etal ApJL 2007 Barway etal MN 2009 Barway etal MN 2010
Barway etal 2011
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•N-body simulations indicate that the bulge component of massive (luminous) lenticulars formed from major mergers.
•But bulges in the less luminous elliptical probably formed from minor mergers or accretion events. Stripping of gas from the halo and disk lead to a change in morphology.
•Correlation between photometric parameters can be a signature of the formation mechanism.
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Luminosity
Distribution Bright field lenticulars observed in the K band: 35Barway etal 2006
Less luminous field and cluster lenticulars with 2MASS data: 49Bedregal etal 2006
Barway
BAM06
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Bulge-Disk Correlation fieldcluster
<B/T>=0.63
<B/T>=0.19<B/T>=0.55
R=0.6 99.9%
R=-0.57 99.9%
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Positive correlation in low-luminosity lenticulars implies that they formed by the stripping of gas from spirals, whose bulges formed through secular evolution.
Bulges of more luminous lenticulars have likely formed through major mergers and rapid collapse.
Luminosity as Differentiator
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Kormendy Relation
Faint lenticulars
Bright lenticulars
Ellipticals
x Bright lenticulars with bars
- Faint lenticulars with bars
Bulges of bright lenticulars and ellipticals show similar tight correlation. These bulges are therefore more virialized than those of faint lenticulars.
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Correlations With Sersic Index
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Photometric Plane
Bright lenticulars: Log n = 0.15 log re – 0.06b(0) + 1.05
bright = 0.019 faint =
0.038
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Sersic index and B/T ratio
Bright lenticulars with low n, low b(0), low re, low B/T. These are outliers in re-rd plot. but well correlated here.
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Bar Fraction and Luminosity
Barred
Unbarred
M(K)=-24.5
M(r)=-24.5
UGC + SDSS + 2MASS + Hyperleda, 385 galaxies
83% barred lenticulars belong to the faint group. Bars are found in 21% of the faint group, but in only 6% of the bright group.
Faint barred galaxies occur more frequently in groups and clusters than their bright counterparts.
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Environmental Dependence
Kormendy Relation
Faint field lenticulars
Faint cluster lenticulars
Cluster lenticulars appear to have faded relative to field lenticulars. They could be early type spirals which have lost gas due to ram pressure stripping or galaxy harassment.
Field lenticulars show clear anti-correlation. Cluster lenticulars are restricted to a limited region and show downward scatter. This is consistent with removal of gas from the disk (and bulge) in cluster lenticulars.
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Color-color relations for S0 galaxies
UV-optical-nir colorsEllipticals – ΔBright S0s – Faint S0s –
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Color-color relations for S0 galaxies
UV-optical-nir colorsEllipticals – ΔBright S0s – Faint S0s –
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A Mass Fundamental Plane for SuperMassive Black Holes
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Ferrarese & Ford 2004
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SMBH Systematics
All nearby galaxies with a significant bulge contain super-massive black holes
The black hole mass is proportional to the bulge mass, and to the fourth power of the central velocity dispersion
The relation has been extended to lower masses, as in Seyferts
Ferrarese & Merritt 2000; Gebhardt etal 2000Kormendy & Richstone 1995
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Scatter 0.79Ellipticals 0.40
Scatter 0.34All Galaxies
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SMBH Host Galaxies
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The Fundamental Plane for SMBH
GalaxiesScatter 0.068
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The Mass Fundamental
Plane for SMBH
Scatter 0.061
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Black Hole Mass from the Mass
Fundamental PlaneScatter
0.19
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Black Hole Mass from
Fundamental Plane of Galaxies
M~
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Black Hole Masses for
Coma Ellipticals
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SMBH to IMBH
Ho, Green 04Barth etal 05
SMBH
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Younger etal arXiv:0804.2672.v2
Self-regulated growth of SMBH via major mrgers, minor mergers and disk instabilites through simulations.
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Thank You
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re – rd Correlation
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Kormendy & Kennicutt ARAA 2004
Rotation and Random Motions
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Disk Central Surface Brightness and Scale
Length
Faint lenticulars
Bright lenticulars
Bulges of early type spirals
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2-Dimensional Relations
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Bulge-DiskCorrelation
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Bulge-DiskCorrelation
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Morphological Parameters and Entropy
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2-D Correlations
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Deviations From Photometric Plane
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Towards the Hyper-Plane
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Photometric Plane of
SMBH Galaxies
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Kormendy Relation for
SMBH Galaxies
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Kormendy Relation –Luminosity
Classes
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Distribution of Sersic Index n
Ellipticals and Early Type Bulges
Khosroshahi et al ApJL 2000
ApJ 2001
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Abell clusters ellipticals 34
Coma ellipticals 42
UGC field lenticulars 37
Bulges of early type spirals 26
Bulges of late type spirals 40
Early type dwarf galaxies 128
Morphological Mix
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Morphological Mix of Galaxies
Ravikumar et al 2006
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The Photometric Plane and Dispersion Velocity
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The Hyper -Plane
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Photometric PlaneEllipticals
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Photometric Plane
View from the top
K1 = 0.15*log n + 0.99*log re
K2 = -0.06*log n + 0.01*log re -b(0)
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Ajit Kembhavi IUCAA, Pune
Galaxies Near and Far
Lenticular Galaxies: Morphological Correlations and Formation Mechanisms
Sudhanshu Barway Yogesh Wadadekar
C.D. Ravi Kumar
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Black Hole Search
• Stellar Dynamics: Stellar motion indicative of a central massive dark object.
M87, M37, Galactic Centre _________________________________________________________________
• Gas Dynamics: Rotating gas disk. on various scales M87, NGC4258
________________________________________________• Relativistic effects close to the dark mass. MCG 6-30-15 _________________________________________________• Reverberation mapping and related techniques Seyfert galaxies Massive Dark Object or Black Hole?
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Kormendy & Kennicutt ARAA 2004
Faber-Jackson Relation