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Shinya Komugi NAOJ Chile Observatory + Rie Miura, Sachiko Onodera, Tomoka Tosaki, Nario Kuno

MAGiC IV : 星間物質の基本平面. Shinya Komugi NAOJ Chile Observatory + Rie Miura, Sachiko Onodera, Tomoka Tosaki, Nario Kuno + many (NRO Legacy MAGiC team, ASTE team, AzTEC team). NRO UM Jul. 25 2013. Star formation relation within M33. Increased scatter at 100pc scale Effect of GMC evolution ?

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Shinya Komugi NAOJ Chile Observatory + Rie Miura, Sachiko Onodera, Tomoka Tosaki, Nario Kuno

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

  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. Star formation relation within Taffy I (Komugi+ 2012) J=blue、H=green、Ks=red ・All but 1 SF region are 7Myr old ・gas=CO@OVRO, sfr=Paα@TAO log SFR=0.95 logΣvar(H2)-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

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

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

  6. Interaction of ISM at 100pc in M33 12CO(J=3-2) map @ASTE Miura et al. (2012) 71 GMCs catalogued Lco, rmaj, rmin, σv, Tmb 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 12CO(J=1-0)  M10 : total molecular gas 12CO(J=3-2)  M32 : dense molecular gas 1.1mm  Mdust : dust mass (using Tcold 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, Md contains 99.3% of the information in PC4 0.72 logSFR + 0.29 logK - 0.62 logMd = 0 ± 0.43 logSFR = (2.4 ± 0.3) logMdust – (0.23 ± 0.06) Kmag. + 0.15 ± 1.2 scatter = 0.4 dex ・ SFR, M CO10, MCO32 contains 99.6% of the information in PC5 0.75 logMCO32 - 0.64 logMCO10 - 0.14 logSFR = 0 ± 0.29 logM32 = (0.86 ± 0.06) logM10 + (0.12 ± 0.02) logSFR + 1.0 ± 0.02 scatter = 0.1 dex

  10. PC5 : SFR-MCO32-MCO10 plane log MCO32 (M◉ pc-2) log MCO10 (M◉ pc-2) log SFR (M◉ yr-1 pc-2)

  11. PC5 : SFR-MCO32-MCO10 plane • 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)

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

  13. PC4 : SFR-Mdust- KS plane • SFR-Mdust tighter than SFR-MCO32 or SFR-MCO10 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.

  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) logMd – (0.23 ± 0.06) Kmag. + 0.15 ± 1.2 scatter = 0.4 dex logMCO32 = (0.86 ± 0.06) logMCO10 + (0.12 ± 0.02) logSFR + 1.0 ± 0.02 scatter = 0.1 dex

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