1. Chris Wilson McMaster University - C. Wilson, F. Israel, S. Serjeant (coordinators) - B. Warren, E. Sinukoff, D. Attewell; C. Baker, J. Newton, T. Parkin, H. Meng (major data processing)

2. C. Wilson, F. Israel, S. Serjeant (coordinators) B. Warren, E. Sinukoff, D. Attewell; C. Baker, J. Newton, T. Parkin (major data processing) G. Bendo, H. Butner, E. Brinks, S. Courteau, D. Clement, J. Irwin, J. Gallego, W. Heesen, J. Knapen, J. Leech, H. Matthews, A. Mok, S. Muhle, A. Mortimer, G. Petitpas, K. Spekkens, B. Tan, R. Tilanus, A. Usero, P. van der Werf, C. Vlahkis, T. Wiegert, M. Zhu plus ~35 additional collaborators from the UK, Canada, and Netherlands

3. Relative mass and physical properties of different dust components (Galliano et al. 2003) How reliable are integrated measurements of physical conditions in galaxies? Molecular gas and the gas-to-dust ratio (Neininger et al. 1996) Effect of galaxy morphology on the ISM Effect of dense cluster environments (Kenney & Young 1989) Effect of metallicity on the ISM (Madden et al. 2006) The local submillimetre luminosity function (Dunne et al. 2000)

4. Relative mass and physical properties of different dust components (Galliano et al. 2003) How reliable are integrated measurements of physical conditions in galaxies? Molecular gas and the gas-to-dust ratio (Neininger et al. 1996) Effect of galaxy morphology on the ISM Effect of dense cluster environments (Kenney & Young 1989) Effect of metallicity on the ISM (Madden et al. 2006) The local submillimetre luminosity function (Dunne et al. 2000)

5. 155 galaxies between 2 and 25 Mpc HI flux > 6 Jy km/s 47 SINGS galaxies (Kennicutt et al. 2003) 18 HI brightest Irr and E galaxies (HI flux > 3 Jy km/s) + 18 randomly selected spirals in Virgo Cluster random selection of 72 field galaxies –D 25 < 5’ –Randomly select 18 galaxies in each of 4 morphology bins (E, early S, late S, Irr)

6. CO J=3-2 data cubes (256 hours) –Area covered is D 25 /2 –Sensitivity 19 mK at 20 km/s resolution rms –Equivalent to Av = 1 mag or 2x10 21 H/cm 2 rms –Detect ~45% of spirals, 20% of ellipticals, almost no irregulars SCUBA-2 850 and 450 micron imaging (100 hours) –Area covered is roughly D 25 /2 –Sensitivity goal 1.8 mJy/beam at 850  m in center of map –48 spiral galaxies observed (25 from SINGS sample) –Only ~40% of SINGS galaxies observed in sufficiently good weather that 450  m data usable 9 papers published so far + 1 in preparation

7. SCUBA-2 850 and 450 micron imaging (100 hours) –Area covered is roughly D 25 /2 –Sensitivity goal 1.8 mJy/beam at 850  m in center of map 48 spiral galaxies observed (25 from SINGS sample) Only ~40% of SINGS galaxies observed in sufficiently good weather that 450  m data usable

8. Data reduction is still in progress … “One regime in which SMURF does not presently perform well is in maps of faint extended structures” (Chapin et al. 2013, MNRAS) - exactly the regime of the NGLS! Don’t have a good idea of our rms noise level yet but is likely higher than target of 1.8 mJy/beam Filtering in map making removes large-scale structure –Clearly seen in a comparison of SCUBA-2 and Herschel data for NGC 3627 (J. Newton, M.Sc. Thesis, McMaster)

9. NGC 4254 (M99) NGC 4579 (M58) NGC 4569 (M90) NGC 4321 (M100) Wilson et al. 2009, ApJ

10. All images are on same colour scale SFR recipe from Calzetti et al. 2007

11. NGC4254 0.7 Gyr NGC4321 1.1 Gyr NGC4569 Quite uniform gas depletion times when CO J=3-2 used to trace mass of molecular gas 1.1 Gyr t gas = M mol /SFR (SFR = H  + 24  m)

12. Warren et al., 2010, ApJ

13. Gas velocity dispersion is an important input to the Toomre criterion for disk stability Q =  g  G  g HI velocity dispersion 10+/-2 km/s at r 25 (higher in interior,Tamburro et al. 2009) Measurements of  g in molecular component are rare

14. An important input to the Toomre criterion for disk stability Q =  g  G  g Measurements of  g for molecular gas are rare C. Wilson et al., 2011, MNRAS

15. NGC3521 Warren et al., 2010, ApJ

16. C. Wilson et al., 2011, MNRAS

18. Slope (0.92+/-0.03) is similar to HCN (Gao & Solomon 2004) and significantly steeper than CO(1-0) (Yao et al. 2003) (Iono et al. 2009, ApJ)

19. L FIR /L CO(3-2) is 5 times larger for the U/LIRGs and high redshift galaxies from Iono et al. (2009) than for the SINGS galaxies from the NGLS (Wilson et al. 2012, MNRAS)

20. Similar M(H 2 ) but different t gas = M(H 2 )/SFR in Virgo, group, and isolated galaxies Mok et al., 2015, in prep.

21. 450 micron 500 micron JCMT+SCUBA2 Herschel+SPIRE NGLS KINGFISH (Kennicutt et al. 2011, PASP)

22. 450 micron 500 micron JCMT+SCUBA2 Herschel+SPIRE NGLS(Wilson et al.) KINGFISH (Kennicutt et al. 2011, PASP)

23.  free T M dust J. Newton, M.Sc. thesis

24. (850) NGC 3627 (450) M51 (850) Wilson, Parkin, Newton, Meng et al., in prep

25. Sample selected to overlap with H-ATLAS, MaNGA, SKA Pathfinder surveys Compare integrated ISM with resolved stellar properties Molecular gas and dust properties, kinematics, metallicity, SFR, SFE log SFR (M o / yr)

26. NGLS CO survey has produced exciting new results (overview in Wilson et al. 2012) Reduction and analysis of SCUBA-2 data still at a very early stage New larger survey proposed (JINGLE) that will exploit multi-wavelength, multi-survey synergies Public link to reduced CO J=3-2 data cubes and maps for complete NGLS: http://www.physics.mcmaster.ca/~wilson/www_xfer/NGLS/

27. 450 micron (cropped) 500 micron JCMT+SCUBA2 Herschel+SPIRE NGLS KINGFISH (Kennicutt et al. 2011, PASP)

28. NGLS CO survey has produced exciting new results (overview in Wilson et al. 2012) Reduction and analysis of SCUBA-2 data still at a very early stage New larger survey proposed (JINGLE) that will exploit multi-wavelength, multi-survey synergies Public link to reduced CO J=3-2 data cubes and maps for complete NGLS: http://www.physics.mcmaster.ca/~wilson/www_xfer/NGLS/

29. I.Star-forming molecular gas in Virgo Cluster spiral galaxies, Wilson et al., 2009, ApJ, 693, 1736 II.Warm molecular gas and star formation in three field spiral galaxies, Warren et al., 2010, ApJ, 714, 571 III.The relations among PAHs, cold dust, molecular, and atomic gas in NGC 2403, G. Bendo et al., 2010, MNRAS, 402, 1409 IV.Very low velocity dispersions in the molecular interstellar medium of spiral galaxies, C. Wilson et al., 2011, MNRAS, 410, 1409

30. V.The CO(J= 3-2) distribution and molecular outflow in NGC 4631, Irwin et al., 2011, MNRAS, 410, 1423 VI.The distribution of gas and star formation in M 81, Sanchez-Gallego et al., 2011, A&A, 527, 16 VII.Halpha imaging and massive star formation properties, Sanchez-Gallego et al., 2012, A&A, 422, 3208 VIII.CO data and the LCO(3-2)-LFIR correlation in the SINGS sample, Wilson et al., 2012, MNRAS, 424, 3050 - overview of survey IX.12CO J = 3-->2 observations of NGC 2976 and NGC 3351, Tan et al., 2013, MNRAS, 436, 921

31. Public link to reduced CO J=3-2 data cubes and maps for complete NGLS: http://www.physics.mcmaster.ca/~wilson/ www_xfer/NGLS/