2. Unraveling the Star Formation Scaling Laws in Galaxies (review + 2 new results) Robert Kennicutt Institute of Astronomy University of Cambridge M51: FUV, H , 24  m rants

3. 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: circa 1998

4. IR-luminous starbursts circumnuclear starbursts BCGs, ELGs

5. Kennicutt 1998, ApJ, 498, 541 Gao, Solomon 2004, ApJ, 606, 271 normal galaxies starbursts

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

9. Is the correlation really this good (or this bad)? –Why all the discrepant results yesterday (and today)? –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: Schmidt Law

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

12. Blitz & Rosolowsky 2006, ApJ, 650, 933 “pressure law”

13. Is the correlation really this good (or this bad)? –Why all the discrepant results? –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: Schmidt Law

14. 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

15. The “star formation law” and “star formation rate” mean different things on different linear scales –disk-averaged scale (1-20 kpc, >100 Myr): useful empirical recipes, but physical significance difficult to infer –radial averages (~1 kpc, 20-300 Myr): breaks some parametric degeneracies, but still smooths nonlinear phenomena over 10- 100’s of cloud scales –cloud scale or below (50-500 pc, 3-10 Myr): probes “star formation efficiency”, but with large observational scatter. “SFRs” really are measures of cluster luminosities. SF law on larger scales may have very different form. Key Caveats, Considerations (aka Rant #1)

16. Rant #2: Beware of the local coincidence between ISM phase vs gravitational instabilities Log P/k (pressure) Log N H    grav bound diffuse

17. It is important to match the SF and gas tracers to the application of interest –color-magnitude diagrams: nirvana: range of ages, stellar masses –H , P , 24  m knots: massive stars, last 3-10 Myr –FUV continuum: massive stars, last 0-200 Myr –diffuse dust continuum emission, 20-200  m + PAH emission: massive and intermediate mass stars, last 0-2 Gyr –CO, HI clumps: probably bound clouds, <10 Myr –diffuse CO, HI: anybody’s guess, probably ~0.1-1 Gyr Rant #3

19. Draine et al. 2007, astro-ph/0703213

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

21. M81 H  + R

22. Calzetti et al. 2007, ApJ, 666, 870

23. M 81 24µm70µm160µm

25. PHOENIGS: from the SINGS `ashes’ Project for Herschel On an Extragalactic Normal Infrared Galaxies Survey R. Kennicutt (IoA, Cambridge), L. Armus (SSC), A. Bollato (UMd), B. Brandl (Leiden), D. Calzetti (UMass), D. Dale (UWyo), B. Draine (Princeton), C. Engelbracht (UofA, USA), K. Gordon (UoA, USA), B. Groves (Leiden), L. Hunt (Oss Arcetri, Italy), J. Koda (Caltech), O. Krause, A. Leroy, H.W. Rix (MPIA), H. Roussel (IAP), M. Sauvage (CEA), E. Schinnerer (MPIA), J.D. Smith (Toledo), L. Vigroux (IAP), F. Walter (MPIA), M. Wolfire (UMd) + TBD Broad Science Objectives: Trace and characterize the flow of energy through the ISM in galaxies; Link heaters-emitters: use Herschel spatial resolution to enable definitive modeling of radiative transfer of dust and gas cooling in galaxies; Probe the nature/origin of extended cold dust envelopes; link warm-cold dust emission; Improve dust and spectral diagnostics of star formation and ISM properties. Approach: An objectively selected sample of nearby galaxies (SINGS-inspired), optimized to cover a broad and representative range of properties, and broad range of local physical environments; Exploit angular resolution for resolving infrared components and dust heating populations. Leverage existing and new ancillary data: from UV to radio Data and high-level data products would be delivered quickly to the broad community.

26. Spatially resolved measurements, vs disk-averaged or azimuthally-averaged data Extinction corrections (H , UV), and corrections for unextincted star formation (infrared, radio) Accurate molecular mass measurements (how reliable is CO?) IMF Observational Wishlist

27. NGC 628 (M74) C. Tremonti

28. SINGS Galaxies

30. 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!

31. Kennicutt (1998) sample expanded sample constant extinction

32. expanded sample constant extinction H  + 24  m extinction corrections

33. P  H  H  m H  total FIR HI + CO (const X )

34. HI + H 2 HI H 2

36. metal-poor dwarf galaxies

38. The Spatially Resolved Star Formation Law in M51 Kennicutt et al. 2007, ApJ, in press (astro-ph/0708.0922) 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 mm emission to correct for extinction in SFR measurements - Probe scales from 300 - 1850 pc (IR/HII regions to unbiased sampling of the disk)

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

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

41. Local Schmidt Law in M51 Kennicutt et al. 2007

46. 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.

47. Tentative Conclusions The combination of H  and 24  m imaging provides a reliable method for obtaining extinction-corrected ionizing fluxes of HII regions. The combination of Ha and FIR luminosities can provide reliable extinction- corrected SFRs of galaxies as a whole. As SFR estimators become more reliable, empirical characterization of the SF law will become increasingly limited by the accuracy and depth of cold gas tracers, especially for molecular gas.

53. Spitzer Infrared Nearby Galaxies Survey (SINGS) –resolved UV  radio mapping of 75 galaxies –selection: maximize diversity in type, mass, IR/optical 11 Mpc Ha/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

54. Beware the treacheries of correlation vs causation! –For a Q ~ 1 disk:   gas ~  c /  G    so   gas   –Likewise:   gas   tot, so P   2 –Also, for local Galactic ISM pressures,  crit for self-gravitating clouds is approximately the same as  crit for self-shielding of molecular clouds –And--- in SF regions much of HI may be a photodissociation product of UV radiation on H 2 Physical Origins of SF Law

55. 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

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

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

61. Kennicutt 1998, ApJ, 498, 541

62. Martin et al. 2005, ApJ, 619, L59 Wang & Heckman 1996, ApJ, 547, 965

63. H  + R