2. Background Slides from Lecture 1

3. Multi-Wavelength SFR Diagnostics (  m) 1 10 100 1000 HH PP 8  m 24  m70  m160  m UV [OII] `calorimetric’ IR Dale et al. 2007, ApJ, 655, 863

5. 0.1 1 10 100 mag (A V )

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

8. Spitzer Infrared Nearby Galaxies Survey (SINGS) complete IRAC, MIPS imaging of 75 nearby galaxies (3.5 – 160  m) IRS, MIPS radial strip maps (10 – 100  m) IRS maps of centers, 75 extranuclear sources (5–37  m) ancillary imaging campaign covering UV to radio Kennicutt et al. 2003, PASP, 115, 928

9. UV Continuum Emission

10. Ultraviolet stellar continuum: key advantages -direct photospheric measure of young massive stars -primary groundbased SFR tracer for galaxies at z>2 - However: -heavily attenuated by dust. Dust `correction’ methods have limits (age-dust degeneracy). -dependent on the stellar population mix, usually measures timescales of ~100 Myr. Dale et al. 2007, ApJ, 655, 863

11. GALEX Mission - all-sky survey - 5 arcsec resolution - 1500 A, 2500 A to AB = 20-21 - 10,000 galaxies to z=0.02 - deep surveys to AB = 25.5, 26.5 - launched April 2003

12. Steidel et al. 1996, ApJ, 462, L17

13. Maeder, Meynet 1988, A&AS, 76, 411 Building an Evolutionary Synthesis Model Kurucz 1979, ApJS, 40, 1 + single star SED evolution model

14. Leitherer et al. 1999, ApJS, 123, 3 “Starburst99” “single burst models” “continuous star formation” models (single age star clusters)

15. apply evolutionary synthesis maodels to constrain IMF Kennicutt, Tamblyn, Congdon 1994, ApJ, 435, 22

16. UV, Dust, and Age Starbursts (Calzetti et al. 1994,1995,1996,1997,2000, Meurer et al. 1999, Goldader et al. 2002)  26 A dusty stellar population may have similar UV characteristics of an old population

17.  26 Blue= starbursts Red= normal SF

18. M51 Calzetti et al. 2005, ApJ, 633, 871 FUV, H , 24  m3.6, 4.5, 5.8, 8.0  m

20. Photoionization Methods: Emission Lines SINGG survey, G. Meurer et al. (NOAO) for ionization-bounded region observed recombination line flux scales with ionization rate ionization dominated by massive stars (M > 10 M o ), so nebular emission traces SFR in last 3-5 Myr ionizing UV reprocessed through few nebular lines, detectable to large distances only traces massive SFR, total rates sensitive to IMF extrapolation SFRs subject to systematic errors from extinction, escape of ionizing radiation from galaxy

21. Kennicutt 1992, ApJS, 79, 255

23. Local H  Surveys Survey N gal Selection PI GOLDMine 277 magnitude Coma/Virgo G. Gavazzi MOSAIC ~1000 H  Abell clusters R. Kennicutt H  GS 450 mag/volume field (<40 Mpc) P. James SINGG/SUNGG* 468 HIPASS field (<40 Mpc) G. Meurer STARFORM 150 volume field (<25 Mpc) S. Hameed 11HUGS *** 470 volume field (<11 Mpc) R. Kennicutt AMIGA ~270 magnitude isolated field L. Montenegro SINGS *** 75 multi-param <30 Mpc R. Kennicutt SMUDGES ~1000 mag field dwarfs L. van Zee UCM 376 obj prism field J. Gallego KISS ~2200 obj prism field J. Salzer ** paired GALEX survey

24. Photoionization Methods: Emission Lines SINGG survey, G. Meurer et al. (NOAO) for ionization-bounded region observed recombination line flux scales with ionization rate ionization dominated by massive stars (M > 10 M o ), so nebular emission traces SFR in last 3-5 Myr ionizing UV reprocessed through few nebular lines, detectable to large distances only traces massive SFR, total rates sensitive to IMF extrapolation SFRs subject to systematic errors from extinction, escape of ionizing radiation from galaxy

25. Leakage of Ionizing Flux at z ~ 3 Shapley et al. 2006, ApJ, 651, 688

26. composite spectrum

27. Calzetti et al., ApJ, submitted Kennicutt & Moustakas, in prep HII regions galaxies (integrated fluxes)

28. Other Emission Lines - H  (0.48  m) - Paschen-  (1.9  m) - Brackett-  (2.2  m) - [OII] (0.37  m) - Lyman-  (0.12  m) Scoville et al. 2000, AJ, 122, 3017

29. Wavelength

30. Moustakas, Kennicutt, Tremonti 2006, ApJ, 642, 775

31. Moustakas et al. 2006, ApJ, 642, 775

32. M83 = NGC 5236 (Sc) SINGG: Survey for Ionization in Neutral-Gas Galaxies 11 Mpc Ha/Ultraviolet Survey (11HUGS)

34. Lecture 2 Begins Here

35. Dust Emission Interstellar dust absorbs ~50% of starlight in galaxies, re-radiates in thermal infrared (3–1000  m) Provides near-bolometric measure of SFR in dusty starbursts, where absorbed fraction ~100% Largest systematic errors from non-absorbed star formation and dust heated by older stars Different components of IR trace distinct dust species and stellar sub-populations

37. FIR to SFR? Dale et al. 2007 (  m) 1 10 100 1000 8  m 24  m70  m160  m `calorimetric’ IR FIR - sensitive to heating from old stellar populations 8  m - mostly single photon heating (PAH emission) 24  m - both thermal and single photon heating 70  m and 160  m - mostly thermal, also from old stars

38. NGC 628 (M74) C. Tremonti

39. Moustakas et al. 2006, ApJ, 642, 775

40. Calzetti et al. 2007 Kennicutt & Moustakas 2007 HII regions galaxies (integrated fluxes)

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

42. M81 H  + R

43. M 81 24µm70µm160µm

44. Bell 2003, ApJ, 586, 794 Radio Continuum Emission exploits tight observed relation between 1.4 GHz radio continuum (synchrotron) and FIR luminosity correlation may reflect CR particle injection/acceleration by supernova remnants, and thus scale with SFR no ab initio SFR calibration, bootstrapped from FIR calibration valuable method when no other tracer is available

45. Cookbook Extinction-Free Limit (Salpeter IMF, Z=Z Sun ) SFR (M o yr -1 ) = 1.4 x 10 -28 L  (1500) ergs/s/Hz SFR (M o yr -1 ) = 7.9 x 10 -42 L (H  ) (ergs/s) Extinction-Dominated Limit; SF Dominated SFR (M o yr -1 ) = 4.5 x 10 -44 L (FIR) (ergs/s) SFR (M o yr -1 ) = 5.5 x 10 -29 L (1.4 GHz) (ergs/Hz) Composite: SF Dominated Limit SFR (M o yr -1 ) = 7.9 x 10 -42 [L H , obs + a L 24  m ] (erg s -1 ) [a = 0.15 – 0.31] SFR (M o yr -1 ) = 4.5 x 10 -44 [L(UV) + L (FIR)] (ergs/s)

46. General Points and Cautions Different emission components trace distinct stellar populations and ages –nebular emission lines and resolved 24  m dust sources trace ionizing stellar population, with ages <5-10 Myr –UV starlight mainly traces “intermediate” age population, ages 10-200 Myr –diffuse dust emission and PAH emission trace same “intermediate” age and older stars– 10 Myr to 10 Gyr(!) Consequence: it is important to match the SFR tracer to the application of interest –emission lines – Schmidt law, early SF phases –UV – time-averaged SFR and SFR in low surface brightness systems –dust emission – high optical depth regions Multiple tracers can constrain SF history, properties of starbursts, IMF, etc.

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

49. 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

50. 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

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

52. 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

53. 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:

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

55. 11HUGS Sample + H  GS + Goldmine Virgo Sample (James et al. 2003; Gavazzi et al. 2003)

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

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

59. Martin 2005, ApJ, 619, L59

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

63. Lecture 2 Ended Here Extra Slides Follow (from Lecture 4)

64. 10 8 10 910 10 11 M o

65. 11MPC + BCGs (Gil de Paz et al. 2003)

66. 11HUGS Sample + H  GS + Goldmine Virgo Sample (James et al. 2003; Gavazzi et al. 2003)

67. 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

68. 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

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

70. Kennicutt 1992, ApJS, 79, 255

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

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

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

74. Kennicutt 1998, ARAA, 36, 189

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

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

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

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

80. blue sequence red sequence

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

82. Lee & Kennicutt, in preparation

83. Janice Lee, PhD thesis

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

85. see poster by Lee et al.

86. 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)

87. 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

89. NGC 1512 (HST)

90. NGC 1512 (GALEX FUV/NUV)

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

92. M82 NGC 3034

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

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

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

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

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

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