Star formation in GMCs
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- Daniel Mitchell
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1 ALMA Image: N159W
2 Star formation in GMCs Most stars form in GMCs K-S law: Gas surface density SF activities Gas SF is a key to understand the galaxy s evolution Initial conditions for high mass SF Need high Jeans mass (effective a~10km/s) Collision/Interaction process Magellanic Clouds + some local galaxies Recent high resolution observations + Uniform sample + Uniform sample of high mass formation from GMC scale
3 Magellanic Clouds D~ 50 kpc (one of the nearest) Different environment from the MW. High gas-dust ratio Low metallicity Active star formation Massive star formation Young populous clusters The Large Magellanic Cloud The Small Magellanic Cloud
4 Examples of Large scale observations Spitzer survey of the LMC SAGE: Surveying the Agency of the galaxy s evolution (Meixner et al ) GMCs, dust, YSOs, HII regions, SNRs, AGBs,, + Herschel Hα, HI, 3.6μm 8.0μm 24μm 1-8 NANTEN CO: from 1.2 Kkm/s 1.2Kkm/s intervals 2.7 =40pc resolution (Fukui et al. 2008)
5 N159 N159 One of the largest Mass:10 7 Mo Size:220 pc Has strongest CO emission Active star formation Five young clusters age<10myr (Bica et al. 1996) N arcmin = 40pc 5
6 N159: Most active on-going star formation in the Local Group: Resolving filaments and cloud cores in the LMC Fukui [PI] Yamamoto Ohama Onishi Kawamura Minamidani Inbedetouw Madden Galametz Lebouteiller N.Mizuno R.Chen Seale Sewio Meixner Hα EAST Contour: ASTE 12CO(3-2), 22 = 5pc 24μm WEST CO(4-3)/CO(1-0) 6 Y. Mizuno et al. 2010
7 N159E N159 Papillion Saigo et al beam(~0.3 pc) N159W NANTEN (40 pc), Fukui et al North East Fukui et al South beam(~0.3 pc) West Strongest CO(3-2) in LMC ASTE (5 pc), Minamidani et al. 2008
8 N159W 12CO(2-1) Massive Protostar 1.6x10 5 Lo 33Mo Massive Protostar 1.9x10 5 Lo, 38Mo
9 N159W 13CO(2-1) Massive Protostar Massive Protostar
10 N159W Massive Protostar 13CO(2-1) Massive Protostar
11
12 Massive star formation by cloud-cloud collisions 3-D MHD simulation with self-gravity of colliding clouds Inoue & Fukui 2013 Large effective Jeans mass owing to the enhancement of the magnetic field strength by shock compression and turbulence in the compressed layer
13 13CO(2-1) Outflow from massive YSO Image: Continuum Red, Blue: Outflow Blue Component Red Component
14 Star formation in N159W [ALMA cycle1] Colliding (Merging?) filaments Width: 1pc Velocity difference: 2-5 km/s Total velocity width: ~ 8km/s Time scale: 6 x 10 4 yrs Massive YSOs at the intersection Outflow: Mass is infalling (~10 4 yrs) Mass accretion rate: 37Mo/6 x 10 4 yrs=6x10-4 Mo/yr Radio Massive recombination stars are formed lines: rapidly Noafter the collision Fukui et 15al. (2015)
![N159: Most active on-going star formation in the Local Group: Resolving filaments and cloud cores in the LMC Fukui [PI] Yamamoto Ohama Onishi Kawamura Minamidani](/docs-images/56/39396520/images/15-0.jpg "Inbedetouw Madden Galametz Lebouteiller N.Mizuno R.Chen Seale Sewio Meixner Hα EAST Contour: ASTE 12CO(3-2), 22 = 5pc 24μm WEST CO(4-3)/CO(1-0) 16 Y. Mizuno et al.")
15 N159: Most active on-going star formation in the Local Group: Resolving filaments and cloud cores in the LMC Fukui [PI] Yamamoto Ohama Onishi Kawamura Minamidani Inbedetouw Madden Galametz Lebouteiller N.Mizuno R.Chen Seale Sewio Meixner Hα EAST Contour: ASTE 12CO(3-2), 22 = 5pc 24μm WEST CO(4-3)/CO(1-0) 16 Y. Mizuno et al. 2010
16 N159E 12CO(2-1) Papillon nebula (Compact HII region: 50Mo star?)
17 N159 East Papillon 2pc (8arcsec) 2pc (8arcsec) Black Contour: 12CO(2-1) White Contour: 98GHz Continuum (free-free) Magenta Contour: H30α White Contour: 12CO(2-1) Yellow dashed Contour: 231GHz Continuum (therma
18 Three velocity components? Blue: 228km/s 232km/s Green: 232km/s 334km/s Red: 235km/s 240km/s Filaments are merging at Papillon CO gas is rapidly dissociated by the high-mass star Similar, but more complex velocity structure compared with the N159W filaments
19 Star formation in N159{WE} [ALMA] Colliding (Merging?) 2, 3 filaments Width: 1pc, 2pc Velocity difference: 2-5 km/s, ~6km/s Time scale: 6 x 10 4 yrs, a few x 10 5 yrs Massive YSOs (30-50Mo) at the intersection Outflow: Mass is infalling (~10 4 yrs), No outflow(~10 5 yrs) Mass accretion rate: 37Mo/6 x 10 4 yrs=6x10-4 Mo/yr No mass accretion Radio recombination lines: No, Yes CO hole (Compact HII region; ~10 5 yrs) Fukui et al. (2015), Saigo et al. (2015)
20 ALMA observations N159W/E in the LMC Full of Filaments and Arcs Complex velocity structures Molecular outflows Dust continuum/radio Recombination Lines Some filaments are colliding/merging Leading to rapid highmass star formation Outflow 37Mo YSO
21 GMCs in the Galaxy and LMC Massive star forming regions: >30Mo, 10 5 Lo Similar shapes Filaments + Multiple velocity components Filament-filament interaction? Different column density GMCs in the LMC have higher N(H2) More active star formation in the LMC??
22 GMCs in the LMC Clouds in super star cluster: 30Dor PI. R. Indebetouw GMCs with different evolutionary stages PI: A. Kawamura Developed HII regions: N55 PI: T. Onishi, N. Naslim Cold GMC at the edge of the LMC PI: T. Wong High mass star formation in an isolated environment PI: R. Harada
23 30 Doradus: Dense Gas in the Nearest Super- Star Cluster 160μm HERITAGE Meixner Hα MCELS Smith++ [CII] BICE Mochizuki Rubin M stars ~10 6 M HI ~10 5 M CO Why study molecular gas in 30 Doradus?Extreme Sources: how do they form, what do they do? 8μm SAGE Meixner Hα MCELS Smith++ Chandra Townsley HI Kim
24 Indebetouw et al CO(2-1) ALMA + APEX
25 Contours: 0.6, 1.6, 2.6, 4.6, Indebetouw and 8.6 Jy/beam/[kms] et al. 2013
26 Indebetouw et al. 2013
27 GMCs & high mass star formation activities in the LMC 44 clouds (26%) Time scale 7Myr 88 clouds (51%) 14Myr 39 clouds (23%) Associated with 82 clusters 6Myr Kawamura et al. (2009) 55 clusters 4Myr
28 Tracing an evolution of giant molecular clouds in the Large Magellanic Cloud Kawamura et al.
29
30 GMCs in the LMC Starless GMCs A number of clumps, some filamentary clouds GMCs with high-mass star formation Compact clumps + highly filamentary clouds Scaling relations, Mass spectra in progress...
31 press releases as well as on the web. Our team has a strong track record of condu programs (SAGE, HERITAGE, MAGMA) and for releasing our results and reduced astronomical community. Isolated High-mass star formation Figures - YSO:Gruendl At least 200pc away from NANTEN clouds The isolated YSOs are located in gas with an HI column density <10 21 cm -2, the region where the models of Krumolz et al. (2009) predict there should be virtually no star formation because of a low predicted molecular fraction. densities. See poster by R. Harada Positions of the isolated high-mass YSOs for the present ALMA observations.
32 Isolated High-mass star formation At least 200pc away from NANTEN clouds HI column density <10 21 cm -2 Mass of YSO: 10-20Mo Associated with many low-mass stars YSOs at the cloud center Mass of molecular clouds: Mo Larger linewidth around YSOs See poster by R. Harada
33 N83 in the SMC NANTEN CO Red contour : ASTE 12CO(J=3-2)
34 SMC: ALMA observations Clumps are starting to be spatially resolved R ~ 1pc, M ~ 1000Mo X Factor from Virial analysis 10 x Galactic value Consistent with the metallicity Density of 12CO clump a few x 10 4 cm -3 a few x 10 3 cm -3 : MW and LMC T kin 40K CO heavily dissociated? [CI] observations expected
35 Summary LMC Filaments + Multiple velocity components Filament-filament interaction Formation of high-mass stars (>30Mo) Higher column density than MW clouds? More active star formation in the LMC Populous cluster forming clump? SMC Clumps are starting to be spatially resolved X Factor ~ 10 x Galactic value 12CO clump: high-density, high-temperature No significant filaments?
36 ALMA Image: N159W Massive YSOs (~30Mo)
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