2. Demographics of Local Star-Forming Galaxies and Starbursts M82: Spitzer/CXO/HST

3. Spitzer Infrared Nearby Galaxies Survey (SINGS) –resolved UV  radio mapping of 75 galaxies –selection: maximize diversity in type, mass, IR/optical 11 Mpc H  /Ultraviolet Survey (11HUGS) –resolved H , UV imaging, integrated/resolved IR of 400 galaxies –selection: volume-complete within 11 Mpc (S-Irr) Survey for Ionization in Neutral-Gas Galaxies (SINGG) –resolved H , UV imaging, integrated/resolved IR of 500 galaxies –selection: HI-complete in 3 redshift slices Integrated Measurements –Ha flux catalogue (+IR, UV) for >3000 galaxies within 150 Mpc - integrated spectra (+IR, UV) for ~600 galaxies in same volume (Moustakas & Kennicutt 2006, 2007) Primary Datasets

4. Thanks to: S. Akiyama, J. Lee, C. Tremonti, J. Moustakas, C. Tremonti (Arizona), J. Funes (Vatican), S. Sakai (UCLA), L. van Zee (Indiana) + The SINGS Team: RCK, D. Calzetti, L. Armus, G. Bendo, C. Bot, J. Cannon, D. Dale, B. Draine, C. Engelbracht, K. Gordon, G. Helou, D. Hollenbach, T. Jarrett, S. Kendall, L. Kewley, C. Leitherer, A. Li, S. Malhotra, M. Meyer, E. Murphy, M. Regan, G. Rieke, M. Rieke, H. Roussel, K. Sheth, JD Smith, M. Thornley, F. Walter

5. Spitzer Local Volume Legacy UV/H  /IR census of local volume HST ANGST sample to 3.5 Mpc GALEX 11HUGS sampel to 11 Mpc

6. The Starburst Bestiary GEHRs SSCs HII galaxies ELGs CNELGs W-R galaxies BCGs BCDs LIGs, LIRGs ULIGs, ULIRGs LUVGs, UVLGs nuclear starbursts circumnuclear starbursts clumpy irregular galaxies Ly-  galaxies E+A galaxies K+A galaxies LBGs DRGs EROs SCUBA galaxies extreme starbursts

7. Demographics of Star-Forming Galaxies absolute SFR (M o /yr) –from H  corrected for [NII], dust SFR density, intensity (M o /yr/kpc 2 ) –defined as SFR/  R 2 SF –correlates strongly with gas density, SF timescale normalized SFR/mass; birthrate parameter b –ratio of present SFR to average past SFR –defined here globally – integrated over galaxy –primary evolutionary variable along Hubble sequence Baseline: 11 Mpc H  + Ultraviolet Survey (11HUGS) - all known galaxies w/gas within 11 Mpc + Ursa Major cluster - companion GALEX Legacy survey coming… Quantify SF properties in terms of 3 observables:

8. R = 100 pc 1 kpc 10 kpc 11HUGS/LVL Sample

9. 11HUGS Sample + H  GS + Goldmine Virgo Sample (James et al. 2003; Gavazzi et al. 2003)

10. Gronwall 1998 SFR * ~5 M o /yr

11. LIGs, ULIGs (Dopita et al., Soifer et al, Scoville et al) merger-driven inflows, starbursts

13. Martin 2005, ApJ, 619, L59

16. M gas /  Hubble  gas /  Hubble M gas /  dyn  crit 1 O5V/3_Myr 0.5” @ 4 Mpc Meurer limit

17. Lecture 4 Begins Here

19. IR-luminous: ~5-8% circumnuclear: ~3-4% BCGs, ELGs: ~5-8% Contributions to the global star formation budget Total fraction ~10-20%

20. 10 8 10 910 10 11 M o

21. 11MPC + BCGs (Gil de Paz et al. 2003)

22. Disk SF – Global Trends Kennicutt 1998, ARAA, 36, 189 Bendo et al. 2002, AJ, 124, 1380

23. Kennicutt, Tamblyn, Congdon 1994, ApJ, 435, 22

24. Sandage 1986, A&A, 161, 89

25. Kennicutt 1998, ARAA, 36, 189

26. Bell, de Jong 2000, MNRAS, 312, 497

28. SFR increase reflects an increase in frequency of SF events, and a shift in the mass spectrum of single events

29. Gas consumption –typical timescales for depletion ~few Gyr –stellar recycling of gas is significant factor !

30. Brinchmann et al. 2004, MNRAS, 351, 1151

31. blue sequence red sequence

32. Kauffmann et al. 2003, MNRAS, 341, 54

33. Lee & Kennicutt, in preparation

34. Disk SFRs: Main Results spectra best fitted with IMF ~ Salpeter for M* > 1 M o SF is ubiquitous when cold gas is present - <4% S-Irr non-detects in H , nearly all show trace SF in UV average SFR/mass increases by 5-10x per type bin (S0 - Sa - Sb, etc) –proportional changes in disk SF history with type - changes in frequency and characteristic mass of SF events large residual variation in SFR within a given type –most variation in disk SFR vs B/D ratio –more strongly correlated with mean gas density –temporal SFR variations (bursts) strong bimodality seen in SFR/mass vs galaxy mass –extension to dwarfs shows evidence for third mode radial gradients in disk age and metallicity Kennicutt 1998, ARAA, 36, 189 Brinchmann et al. 2004, MNRAS, 351, 1151

35. Janice Lee, PhD thesis

36. Disk Star Formation Rates and Histories evolutionary synthesis of integrated colors Tinsley 1968, ApJ, 151, 547 Searle et al. 1973, ApJ, 179, 427 Larson, Tinsley 1978, ApJ, 219, 46 results –disk colors consistent with sequence of constant age, IMF, Z, and variable SF history  (t) –best fit for ~Salpeter IMF –spectra fit with similar model sequence Kennicutt 1983, ApJ, 272, 54

37. Bruzual, Charlot 1993, ApJ, 405, 538

38. starburst duty cycle in dwarf galaxies (Lee 2006)

39. see poster by Lee et al.

40. Application to Starburst Duty Cycles bursts produce 20-40% of present-day SF in dwarfs fraction of bursting dwarfs in same sample is 5-10% the galaxies are bursting 5-10% of the time average burst amplitude is ~4-8x the background SFR typical burst durations are 10-100 Myr (e.g., Gallagher, Harris, Calzetti, Zaritsky, Hunter…) - a typical burst lasts for 0.1-1% of Hubble time a typical galaxy bursts ~10-20 times over a Hubble time, each time producing a few percent of its stars (every 500-1000 Myr)

42. NGC 1512 (HST)

43. NGC 1512 (GALEX FUV/NUV)

44. Kormendy & Kennicutt 2004, ARAA, 42, 603 Sakamoto et al. 1999, ApJ, 525, 691

45. M82 NGC 3034

46. Lo et al. 1987, ApJ, 312, 574

49. Kennicutt 1998, ARAA, 36, 189 ELS limit normal galaxies IR-luminous galaxies

50. Circumnuclear Star Formation - Trends with Type Ho et al. 1997, ApJ, 487, 595 ellipticals too?! Yi et al. 2005, ApJ, 619, L111

52. Borne et al. 2000, ApJ, 529, L77

54. IR-luminous: ~5-8% circumnuclear: ~3-4% BCGs, ELGs: ~5-8% Contributions to the global star formation budget Total fraction ~10-20%

55. L’Floch et al. 2005, ApJ, 632, 169 total IR-luminous starbursts

56. Kennicutt 1998, ApJ, 498, 541 Gao, Solomon 2004, ApJ, 606, 271 The Star Formation Law normal galaxies starbursts

57. Galaxies exhibit an immense diversity in star formation properties, varying by >10 7 in absolute SFR, SFR/mass and SFR/area. Over this range the SFR/area is correlated with gas surface density, following a truncated Schmidt power law with index N = 1.4 +-0.1 –the correlation of with dense gas (e.g., HCN) is roughly linear The Schmidt law shows a turnover below a threshold surface density that varies between galaxies. –in gas-rich, actively star-forming galaxies this transition is seen as a radial transition in the SFR/area –some gas-poor disks reside in the threshold regime at all radii Basic Observations

58. Kennicutt 1998, ApJ, 498, 541 Gao, Solomon 2004, ApJ, 606, 271 Scaling Laws normal galaxies starbursts

59. Crothswaite et al. 2003

60. Martin & Kennicutt 2001, ApJ, 555, 301

61. normal galaxies starburst galaxies HI+H 2 mass surface density SFR surface density

62. NGC 1291 Blue: Carnegie Atlas Sandage & Bedke 1994 H  + R: SINGG survey Meurer et al. 2006

63. Is the Schmidt law correlation really this good? –do all galaxies follow the same Schmidt law? –is the scatter driven by a second parameter? Is the global Schmidt law the result of a more fundamental underlying SF scaling law? –over what range of physical scales is the law valid? Is the SFR correlated more strongly with the total (atomic + molecular) surface density or with the molecular surface density alone? What is the physical origin of the relation? Questions: Schmidt Law

64. “Schmidt law”: SFR vs gas density power law “Silk law”: SFR vs gas density/dynamical time

65. Is the correlation really this good? –do all galaxies follow the same Schmidt law? –is the scatter driven by a second parameter? Is the Schmidt law the result of a more fundamental underlying SF scaling law? –over what range of physical scales is the law valid? Is the SFR correlated more strongly with the total (atomic + molecular) surface density or with the molecular surface density alone? What is the physical origin of the relation? Questions

66. Do the observed H  edges of galaxies trace proportional changes in the SFR/area? Does the SFR in the sub-threshold regime follow a (modified) Schmidt law? Or is it triggered entirely by local compression events? What is the physical nature of the threshold? Questions: Thresholds

68. The Global Schmidt Law Revisited analyze galaxies with spatially- mapped star formation (H , P , FIR), HI, and CO enlarged, diversified samples –normal galaxy sample 3x larger –larger ranges in gas and SFR densities –large subsamples of circumnuclear starbursts, low-metallicity galaxies incorporated densities averaged within active SF regions explicit corrections for [NII], extinction point-by-point analysis of SINGS + BIMA SONG galaxies Work in progress!

69. Kennicutt 1998, ApJ, 498, 541

70. metal-poor dwarf galaxies

71. The Spatially Resolved Star Formation Law in M51 Kennicutt et al. 2007, ApJ, submitted FUV, H , 24  m Calzetti et al. 2005, ApJ, 633, 871 - Use spatially-resolved measures of CO, HI, and SFR to characterize SFR vs gas surface density relation on a point-by-point basis - Use combinations of H  + P  and H  + 24  m emission to correct for extinction in SFR measurements - Probe scales from 300 - 1850 pc (IR/HII regions to unbiased sampling of the disk)

72. M51: BIMA SONG Survey Helfer et al. 2003

73. NGC 6946– THINGS VLA HI Survey F. Walter et al.

75. Scoville et al. 2000, AJ, 122, 3017

76. GALEX FUV + NUV (1500/2500 A) IRAC 8.0  m MIPS 24  m H  + R

77. Local Schmidt Law in M51 Kennicutt et al. 2006, in prep

83. Tentative Conclusions The disk-averaged Schmidt law in galaxies is rooted in a local relationship that persists to scales of <500 pc In M51 the SF density is tightly coupled to the local H 2 surface density, and not with HI density A kinematic star formation law does not seem to extend as well to local scales The disk-averaged SF law is confirmed with more/better observations. Some metal-poor galaxies lie systematically above the mean relation.

84. Extra Slides

85. Star Formation Rates and Histories synthesis models mainly sensitive to ratio of main sequence to red giant stars --> ratio of current star formation rate (SFR) to average past rate (b =  0 / ) Kennicutt 1989, ARAA, 36, 189 most sensitive measurements from spectral features that directly trace young population, combined with color constraints - UV continuum fluxes - nebular recombination lines (--> ionizing stellar continuum) - thermal dust emission (10-200  m)

86. Kron 1982, Vistas Astron, 26, 37 Michigan Spectral Catalog Vols 1-3

87. Kennicutt 1992, ApJS, 79, 255

88. 30 Doradus

90. Sbc, Sc, Scd, Sd

91. S0/a, Sa, Sab, Sb bar-driven inflows, circumnuclear starbursts

92. Sdm, Sm, Im, I0 + BCGs (Gil de Paz et al. 2003)

93. NGC 1365 (HST )

94. NGC 3885 Sa NGC 7690 Sab NGC 986 SBb NGC 3177 Sb NGC 5806 SbNGC 4030 Sbc Examples of pseudobulges: Kormendy & Kennicutt 2004, ARAA, 42, 603

95. Example: completeness of z=0 prism surveys (UCM) Early results suggest that prism surveys miss 40-55% of local SF