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

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

・All but 1 SF region are 7Myr old log SFR=0.95 logΣ var (H 2 )-8.23 ・small 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

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

Interaction of ISM at 100pc in M33 12 NRO 45m Tosaki et al. (2011) Catalog in progress

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

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

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

・ 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 PC logSFR logK logM d = 0 ± 0.43 logSFR = (2.4 ± 0.3) logM dust – (0.23 ± 0.06) K mag ± 1.2 scatter = 0.4 dex ・ SFR, M CO10, M CO32 contains 99.6% of the information in PC logM CO logM CO logSFR = 0 ± 0.29 logM 32 = (0.86 ± 0.06) logM 10 + (0.12 ± 0.02) logSFR ± 0.02 scatter = 0.1 dex

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 )

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

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

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

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 ± 1.2scatter = 0.4 dex logM CO32 = (0.86 ± 0.06) logM CO10 + (0.12 ± 0.02) logSFR ± 0.02scatter = 0.1 dex