1. Shinya KomugiNAOJ Chile Observatory + Rie Miura, Sachiko Onodera, Tomoka Tosaki, Nario Kuno + many (NRO Legacy MAGiC team, ASTE team, AzTEC team) NRO UM Jul. 25 2013 MAGiC IV : 星間物質の基本平面

2. Star formation relation within M33 Increased scatter at 100pc scale Effect of GMC evolution ? (e.g., Kawamura et al. 2009, Onodera et al. 2010) Onodera et al. 2010

3. ・All but 1 SF region are 7Myr old ・gas=CO@OVRO, sfr=Paα@TAO log SFR=0.95 logΣ var (H 2 )-8.23 ・small dispersion @ 700pc σ ＝0.1 for varying Xco c.f.σ =0.5 in M51 (Liu+11) GMCs (SF regions) at a similar Evolution stage give tight SK laws Star formation relation within Taffy I (Komugi+ 2012) J=blue 、 H=green 、 Ks=red

4. Star formation Interstellar Radiation Field Interstellar Radiation Field Molecular gas (CO) Molecular gas (CO) Dust Opt.-Near IR “Dense” gas Xco metallicity temperature emissivity heating K-S law Gas/dust ratio IMF UV input extinction The ISM at GMC scales Hα, 24um 1.1 mm 12 CO(J=1-0) 12 CO(J=3-2) 2.1 um + time evolution

5. Interaction of ISM at 100pc in M33 12 CO(J=1-0) @ NRO 45m Tosaki et al. (2011) Catalog in progress

6. Interaction of ISM at 100pc in M33 12 CO(J=3-2) map @ASTE Miura et al. (2012) 71 GMCs catalogued L co, r maj, r min, σ v, T mb Radius range 20 ~ 40

7. Interaction of ISM at 100pc in M33 1.1mm and dust temperature map ASTE and Spitzer 160um Komugi et al. (2011)

8. Interaction of ISM at 100pc in M33 57 GMCs at ~100pc resolution with 12 CO(J=1-0)  M 10 : total molecular gas 12 CO(J=3-2)  M 32 : dense molecular gas 1.1mm  M dust : dust mass (using T cold map and β=2) Ks band  K : measure of ISRF from old stellar pop. Hα, 24um  SFR : star formation rate (UV photon) Type  B, C, D : evolutionary stage

9. ・ PC4 and PC5 have smallest variance, i.e. we can write PC4 = 0 PC5 = 0 ・ SFR, K, M d contains 99.3% of the information in PC4 0.72 logSFR + 0.29 logK - 0.62 logM d = 0 ± 0.43 logSFR = (2.4 ± 0.3) logM dust – (0.23 ± 0.06) K mag. + 0.15 ± 1.2 scatter = 0.4 dex ・ SFR, M CO10, M CO32 contains 99.6% of the information in PC5 0.75 logM CO32 - 0.64 logM CO10 - 0.14 logSFR = 0 ± 0.29 logM 32 = (0.86 ± 0.06) logM 10 + (0.12 ± 0.02) logSFR + 1.0 ± 0.02 scatter = 0.1 dex

10. PC5 : SFR-M CO32 -M CO10 plane log M CO32 (M ◉ pc -2 ) log M CO10 (M ◉ pc -2 ) log SFR (M ◉ yr -1 pc -2 )

11. 3D version of SK law, but strongest correlation is between CO32 and CO10.  SK law at 100 pc is better expressed as “CO32/CO10 ratio is modulated by SFR”  Consistent with “dense gas fraction is larger for clouds with more active SF” (Onodera+ 2012) PC5 : SFR-M CO32 -M CO10 plane

12. PC4 : SFR-M dust -K S plane log M dust (M ◉ pc -2 ) log SFR (M ◉ yr -1 pc -2 ) ISRF (K band mag.)

13. SFR-M dust tighter than SFR-M CO32 or SFR-M CO10  Dust traces molecular gas better ?? GMC evolution = movement in the plane; young GMC  2um dark, less dust, small SFR < 10Myr GMC  2um bright, range of dust and SFR > 10Myr GMC  intermediate in SFR, dust, 2um. PC4 : SFR-M dust - K S plane

14. summary Multi-parameter analysis of GMC in M33 2 most fundamental relations ; “Classical” KS law can be explained by combining these PCA can be a powerful tool to interpret the entangled relations in the ISM Needs verification in other galaxies  12CO + Paα survey of NGC300 ongoing logSFR = (2.4 ± 0.3) logM d – (0.23 ± 0.06) K mag. + 0.15 ± 1.2scatter = 0.4 dex logM CO32 = (0.86 ± 0.06) logM CO10 + (0.12 ± 0.02) logSFR + 1.0 ± 0.02scatter = 0.1 dex