1. CO Rotation Curves High-velocity Rotation, Deep Potential, & Dense Molecular Cores in Spiral Centers Sofue, Y., Koda, J., Nakanishi, H., Onodera, S., Egusa, F., Komugi, S., Kohno, K. 2006 June 26-30, Ishigaki ’ Mapping the Galaxy and Nearby Galaxies ’

2. Summary: Normal galaxies 1. Rotation curves & Mass structures are common (universal). 2. Dynamical mass much (~100x gas) dominates in <100 pc. 3. Nuclear gas is stable to produce/maintain dense gas core. Summary: Normal galaxies 1. Rotation curves & Mass structures are common (universal). 2. Dynamical mass much (~100x gas) dominates in <100 pc. 3. Nuclear gas is stable to produce/maintain dense gas core.

3. I. Introduction

4. Ha RC l Rubin.. 80’,90’ l Mathewson 80’; Persic.. 90’ HI RC l Roberts.. 70’ l Bosma; Rupen; Sancisi,.. 80’ CO RC Sofue, et al... 1995--- (cf: Sofue & Rubin 2001 ARAA) M/L Ratio Kent 80’; Persic 80’; Forbes 90’; Heraudeau 90’; Rubin et al. 90’; Takamiya, Sofue 90’ Rotation Curves and Dark Matter

5. l RC Mass Distri. l Halo Y es Yes l Disk Yes Yes l Bulge Yes Not clear l Core (1-100 pc) No No l BH (sub-pc) Yes Yes RC, Mass/DM distribution? RC, Mass/DM distribution?

6. Optical RCs: sometimes extinction and/or Balmar line absorption V↑ Position along major axis →

7. CO for Central Rotation Curve CO for Central Rotation Curve

8. CO Line Transparent (cf O ptical) Dense in the center (> HI) Low temperature/velocity dispersion High-spatial resolution High-velocity resolution High sensitivity

9. Interferometer CO-line Surveys OVRO BIMA PdB Nobeyama etc. Interferometer CO-line Surveys OVRO BIMA PdB Nobeyama etc.

10. Sakamoto et al. 1999 Sakamoto et al. 1999

11. BIMA SONG

12. II. Virgo CO Survey II. Virgo CO Survey

13. l Collaborators l Sofue, Y. l Koda, J. l Nakanishi, H. l Onodera, S. l Kohno, K l Okumura, S. l Tomita, A. l Egusa, F. l Komugi, S. l et. al. Nobeyama mm Array, 45-m l Future: l SUBARU l ALMA l (Virgo is visible)

14. l ｽﾗｲﾄﾞ 58 ｽﾗｲﾄﾞ 58 Why Virgo? Cepheid distance 16.1 Mpc Variety of spiral types Wealth of data sets Visible from ALMA

15. Observations 1. Nobeyama mm-wave Array AB+C+D Arrays (2-4” at 115 GHz) 2. 12 CO(J=10) line at 115 GHz 3. Normal CO-rich spirals (from Kenney & Young‘s 1988 CO catalog) 4. Observations 1. Nobeyama mm-wave Array AB+C+D Arrays (2-4” at 115 GHz) 2. 12 CO(J=10) line at 115 GHz 3. Normal CO-rich spirals (from Kenney & Young‘s 1988 CO catalog) 4. Long-Term project : 700 h 1999-2003 ( 1992 – 2006: individ. G. ; accumulated data from past)

16. 0.5 Mpc 1Mpc 2 Mpc Virgo survey galaxies CO images

17. FITS data available from http://www.ioa.s.u-tokyo.ac.jp/ Sofue et al. 2003a, b Onodera et al. 2004 Nakanishi et al., 2004 Koda et al. 2005

21. III. Rotation Curves III. Rotation Curves

22. HI CO l M51

23. l CO (1x1’) NGC 3079

24. l HI (Irwin & Seaquist 91) l CO (Young et al 93) l CO (NMA) Position-Velocity Diagram a case for N3079

25. l RC –> PV l diagram l simulation CO HI

26. Iteration Method to create RCs (Takamiya, et al. 2000)

28. Methods for RC Envelope tracing; Iteration; Peak tracing

29. Rotation Curves from single dish data

30. High accuracy RC for nearby galaxies

31. Rotation Curves from NMA atural weighting (3-5”)

35. Rotation Curves from NMA (Uniform weighting 1-2”)

36. NGC 4192

37. NGC 4501

38. NGC 4536

39. NGC 3079

40. High accuracy RC

42. Logarithmic RC

43. IV. Mass distributions IV. Mass distributions

44. Fitting by M iyamoto-Nagai Potential l Core l Bulge l Disk l Halo

45. > > Direct calculation of mass distribution from RC

47. Virgo @ higher resolution

48. SMD(mass) Surface mass density SMD(mass) Surface mass density l Core l Bulge l Disk l Halo

49. l Core l Bulge l Disk l Halo (@ higher resolution)

50. Fundamental structures of spiral galaxies Central BH Massive Core Bulge Disk Hallo

51. Massive Core 10 9 M sun in 100 pc SMD ~ a few x10 4 M sun /pc ー２ Center Cusp (DM/Stellar)

52. Fundamental mass structures of spiral galaxies Central BH Massive Core Bulge Disk Hallo

53. Mass structure is universal. Milky Way, M31, N253, …. Virgo galaxies, …. Even LMC, M82(hallo truncated)

54. l LMC = Dark Bulge + Disk + Dark Halo

55. IV. Molecular core in massive core IV. Molecular core in massive core

56. Center SMD(gas) vs SMD(dynamical)

57. SMD (gas) ~ 0.01 SMD(mass) 1000 M sun pc -2 100 M sun pc -2

58. Conversion factor < X co solar X co = 1 x 10 20 H 2 cm -2 /K km/s SMD(H 2 ) = 0.013 SMD (mass) Gas mass << Dynamical mass in 100 pc

59. Central gas distribution: Twin peaks vs Single peak

60. Twin peaks vs Single peak

61. Twin & Single

62. “Single Peaks” 6 Singles vs 1 Twin out of 15 galaxies 10“ (780 pc) NGC 4192 NGC 4212 NGC 4419 NGC 4501 NGC 4535 NGC 4536

63. Uniform weighting maps (1-2” resolution)

64. NGC 4192

65. NGC 4419

66. NGC 4536

67. NGC 3079

68. Single peaks are common. N H2 ~ 10 22-23 H 2 /cm 2 ~ 2x10 3 M sun /pc 2 (5 singles against 1 twin)

69. MW center Molecular core NGC3079 Molecular core NGC3079 l 100 pc l 10 pc

70. If thickness ~10 pc (like MW center) n H 2 ~ 3x10 3 H 2 cm ー 3 Then, Why stay in gas??? If thickness ~10 pc (like MW center) n H 2 ~ 3x10 3 H 2 cm ー 3 Then, Why stay in gas???

71. Toomre’s Q = Σ ｃ /Σ Σ ｃ =κ ｃ /πG Σ = SMD (gas ) κ~O(2Ω) ~ (0.5 My) -1 c ~ 30 km/s Σ ｃ ＝ 5 x 10 ３ (V 200 c 30 ／ R 100 ) M sun pc -2 (Koda et al. 2005)

72. 1000 M sun pc -2 100 M sun pc -2

73. Q > 1 or Q >> 1 (Jeans time >> 1/κ ） Gas is stable against gravitational contraction/SF.

74. Single-peak galaxy centers have: 1. Deep potential (High SMD, high rotation) 2. High-density molecular core (High gas SMD) 3. Gas stable (Q>>1, t J >1/κ) Single-peak galaxy centers have: 1. Deep potential (High SMD, high rotation) 2. High-density molecular core (High gas SMD) 3. Gas stable (Q>>1, t J >1/κ)

75. “Twin” ↓ “Single peak” = Stable dense molecular core Enough time for growth ↓ Burst, activity, ….exhaust gas,…. And cycle

76. Conclusion 1. Rotation curves & Mass structures are common (universal). 2. Dynamical mass much (~100x gas) dominates in <100 pc. 3. Nuclear gas is stable to produce/maintain dense gas core. Conclusion 1. Rotation curves & Mass structures are common (universal). 2. Dynamical mass much (~100x gas) dominates in <100 pc. 3. Nuclear gas is stable to produce/maintain dense gas core.

77. Future work: 1. Logarithmic Rotation Curves & mass/stability analyses as above, 100→10→1→0.1 pc 2. ALMA CO Virgo (Nearest cluster with acc. distance) Future work: 1. Logarithmic Rotation Curves & mass/stability analyses as above, 100→10→1→0.1 pc 2. ALMA CO Virgo (Nearest cluster with acc. distance)