1. Hello!

2. 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

3. Hubble’s Tuning Fork Lenticular

4. 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.

5. Surface Brightness Distribution

6. NGC 661 V

7. Surface Brightness Profile

9. Bulge –Disk Decomposition UGC 1250  2 =  (o i -m i ) 2 /  i 2

10. Bulge-Disk Decomposition

11. Morphological Parameter Correlations

12. The Fundamental Plane

13. log r e = A log  + B log I e + c

14. Fundamental Plane for Morphological Mix of Galaxies

15. The Photometric Plane

16. 2-D Correlations Ellipticals and Early Type Bulges

17. Photometric Plane Ellipticals and Early Type Bulges Khoshroshahi etal ApJL 2000 Ellipticals Early type bulges

18. Photometric Plane Ellipticals Lenticulars Dwarf Ellipticals Bulges Residuals Ravikumar etal AA 2006

19. Bulge-Disk Correlations in Lenticular Galaxies Barway etal ApJL 2007 Barway etal MN 2009 Barway etal MN 2010 Barway etal 2011

20. 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.

21. Luminosity Distribution Bright field lenticulars observed in the K band: 35 Barway etal 2006 Less luminous field and cluster lenticulars with 2MASS data: 49 Bedregal etal 2006 Barway BAM06

22. Bulge-Disk Correlation field cluster =0.63 =0.19 =0.55 R=0.6 99.9% R=-0.57 99.9%

23. 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

24. 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.

25. Correlations With Sersic Index

26. Photometric Plane Bright lenticulars: Log n = 0.15 log r e – 0.06  b (0) + 1.05  bright = 0.019  faint = 0.038

27. Sersic index and B/T ratio Bright lenticulars with low n, low  b (0), low r e, low B/T. These are outliers in r e -r d plot. but well correlated here.

28. 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.

29. 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.

30. Color-color relations for S0 galaxies UV-optical-nir colors Ellipticals – Δ Bright S0s –  Faint S0s – 

31. Color-color relations for S0 galaxies UV-optical-nir colors Ellipticals – Δ Bright S0s –  Faint S0s – 

32. A Mass Fundamental Plane for SuperMassive Black Holes

33. Ferrarese & Ford 2004

35. 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 2000 Kormendy & Richstone 1995

36. Scatter 0.79 Ellipticals 0.40 Scatter 0.34 All Galaxies

37. SMBH Host Galaxies

38. The Fundamental Plane for SMBH Galaxies Scatter 0.068

39. The Mass Fundamental Plane for SMBH Scatter 0.061

40. Black Hole Mass from the Mass Fundamental Plane Scatter 0.19

41. Black Hole Mass from Fundamental Plane of Galaxies M~  

42. Black Hole Masses for Coma Ellipticals

43. SMBH to IMBH Ho, Green 04 Barth etal 05 SMBH

45. Younger etal arXiv:0804.2672.v2 Self-regulated growth of SMBH via major mrgers, minor mergers and disk instabilites through simulations.

46. Thank You

47. r e – r d Correlation

49. Kormendy & Kennicutt ARAA 2004 Rotation and Random Motions

50. Disk Central Surface Brightness and Scale Length Faint lenticulars Bright lenticulars Bulges of early type spirals

51. 2-Dimensional Relations

52. Bulge-Disk Correlation

54. Morphological Parameters and Entropy

55. 2-D Correlations

57. Deviations From Photometric Plane

58. Towards the Hyper-Plane

60. Photometric Plane of SMBH Galaxies

61. Kormendy Relation for SMBH Galaxies

62. Kormendy Relation – Luminosity Classes

64. Distribution of Sersic Index n Ellipticals and Early Type Bulges Khosroshahi et al ApJL 2000 ApJ 2001

65. 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

66. Kormendy Relation for Bulges

67. Morphological Mix of Galaxies Ravikumar et al 2006

68. The Entropic Plane Each galaxy type is in a quasi-equilibrium state. This corresponds to a local maximum in entropy. The entropy of self-gravitating system can be determined from thermodynamical considerations (Lima Neto etal 1999, Marquez etal 2001).

69. Entropy Secular evolution leads to slow change in entropy. Hierarchical merging or violent relaxation leads to rapid and greater entropic changes.

70. Entropy and the Face-on View

71. The Photometric Plane and Dispersion Velocity

72. The Hyper -Plane

73. Photometric Plane Ellipticals

74. Photometric Plane View from the top K 1 = 0.15*log n + 0.99*log r e K 2 = -0.06*log n + 0.01*log r e -  b (0)

75. Ajit Kembhavi IUCAA, Pune Galaxies Near and Far Lenticular Galaxies: Morphological Correlations and Formation Mechanisms Sudhanshu Barway Yogesh Wadadekar C.D. Ravi Kumar

76. 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?

77. SuperMassive Black Hole Systematics Ferrarese et al Residual 0.34Residual 0.42

78. Kormendy & Kennicutt ARAA 2004 Faber-Jackson Relation