Shinya KomugiNAOJ Chile Observatory + Rie Miura, Sachiko Onodera, Tomoka Tosaki, Nario Kuno
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Transcript of Shinya KomugiNAOJ Chile Observatory + Rie Miura, Sachiko Onodera, Tomoka Tosaki, Nario Kuno
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
MAGiC IV : 星間物質の基本平面
Star formation relation within M33
Increased scatter at 100pc scaleEffect 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・ gas=CO@OVRO, sfr=Paα@TAO
log SFR=0.95 logΣvar(H2)-8.23
・ small dispersion @ 700pcσ = 0.1 for
varying Xcoc.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
InterstellarRadiation
Field
Molecular gas
(CO)
Dust
Opt.-Near IR
“Dense” gas
Xco
metallicitytemperature
emissivity
heating
K-S law
Gas/dust ratio
IMF
UV input
extinction
The ISM at GMC scales
Hα, 24um
1.1 mm
12CO(J=1-0)
12CO(J=3-2)
2.1 um
+ time evolution
Interaction of ISM at 100pc in M33
12CO(J=1-0) @ NRO 45mTosaki et al. (2011)Catalog in progress
Interaction of ISM at 100pc in M33
12CO(J=3-2) map @ASTEMiura et al. (2012)
71 GMCs cataloguedLco, rmaj, rmin, σv, Tmb
Radius range 20 ~ 40
Interaction of ISM at 100pc in M33
1.1mm and dust temperature map ASTE and Spitzer 160umKomugi et al. (2011)
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
・ PC4 and PC5 have smallest variance, i.e. we can writePC4 = 0PC5 = 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 PC50.75 logMCO32 - 0.64 logMCO10 - 0.14 logSFR = 0 ± 0.29
logM32 = (0.86 ± 0.06) logM10 + (0.12 ± 0.02) logSFR + 1.0 ± 0.02scatter = 0.1 dex
PC5 : SFR-MCO32-MCO10 plane
log MCO32
(M◉ pc-2)
log MCO10
(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-MCO32-MCO10 plane
PC4 : SFR-Mdust-KS plane
log Mdust
(M◉ pc-2)
log SFR(M◉ yr-1 pc-2)
ISRF(K band mag.)
• 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.
PC4 : SFR-Mdust- KS 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) logMd – (0.23 ± 0.06) Kmag. + 0.15 ± 1.2scatter = 0.4 dex
logMCO32 = (0.86 ± 0.06) logMCO10 + (0.12 ± 0.02) logSFR + 1.0 ± 0.02 scatter = 0.1 dex