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Shinya Komugi NAOJ Chile Observatory + Rie Miura, Sachiko Onodera, Tomoka Tosaki, Nario Kuno PowerPoint Presentation
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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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slide1

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

slide2

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

slide3

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

slide4

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

interaction of ism at 100pc in m33
Interaction of ISM at 100pc in M33

12CO(J=1-0) @ NRO 45m

Tosaki et al. (2011)

Catalog in progress

interaction of ism at 100pc in m331
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

interaction of is m at 100pc in m33
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 m332
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

slide9

・ 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

pc5 sfr m co32 m co10 plane
PC5 : SFR-MCO32-MCO10 plane

log MCO32

(M◉ pc-2)

log MCO10

(M◉ pc-2)

log SFR

(M◉ yr-1 pc-2)

slide11

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)
pc4 sfr m dust k s plane
PC4 : SFR-Mdust-KS plane

log Mdust

(M◉ pc-2)

ISRF

(K band mag.)

log SFR

(M◉ yr-1 pc-2)

slide13

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.

summary
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