渦状銀河における gmc の進化と星形 成 evolution of gmcs and star formation in spiral...
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渦状銀河における GMC の進化と星形成Evolution of GMCs and star formation in spiral
galaxies
Nario KunoNobeyama Radio Observatory
1. NRO M33 All-Disk Survey of Giant Molecular Clouds (NRO MAGiC)
2. Preliminary results of ALMA cycle 0 observations of M833. CO Galactic Plane Survey by NRO 45-m telescope
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CollaboratorsT. Tosaki1, S.Onodera2, R. Miura3, K. Muraoka5, S. Komugi3, T. Sawada3, K. Nakanishi3, K. Kohno4, H. Kaneko6, A. Hirota7, N. Arimoto7, H. Nakanisi8, R. Kawabe3, F. Egusa9, K. Wada8
1 Joetsu University of Education2 Meisei university3 Chile observatory, NAOJ4 University of Tokyo5 Osaka Prefecture University6 Tsukuba university, 7 NAOJ 8 Kagoshima University9 ISAS
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Introduction• Cycle of matter in galaxies
– Evolution of molecular clouds (from atomic gas to dense gas) are one of the main themes of radio astronomy
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Observations of GMCs in nearby galaxies
– LMC: Kawamura et al. 2009, Hughes et al. 2010…– M33: Rosolowsky et al. 2007, Gratier et al. 2012…– M51: Koda et al. 2011, Egusa et al. 2011…– IC10: Leroy et al. 2006– M31: Rosolowsky et al. 2007
Scientific objectives: • Basic properties of GMCs ( mass, size, … ) • Evolution of ISM star formation process⇔
– GMC formation → dense gas → stars → destruction of GMCs
GMCs in M33 and M83
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1. NRO M33 All-Disk Survey of Giant Molecular Clouds (NRO MAGiC)
Close to our Galaxy (D = 840 kpc)
each GMC can be resolved
(NRO 45m resolution :
20"~ 80 pc)
The best target for studying GMCs and star formation within a whole galaxy
Moderately face-on
GMCs are distributed throughout the disk and are in relation to other components(e.g. star-forming regions, arms,…)
(Arimoto et al.)
Many star-forming regions over the whole disk
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• Data– Molecular gas : 12CO(1-0) (45m)– Warm and dense molecular gas : 12CO ( 3-2 )
( ASTE ) : 13CO(1-0)
(45m)– Cold dust : 1.1mm ( ASTE :
AzTEC )– Star-forming region : Ha ( SUBARU )– Stars : B,V,R,I ( SUBARU )– Atomic gas, IR … : ( Archived data )Properties and evolution of GMCs
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High resolution & wide field mapping w/ NRO 45m/ASTE 10m + OTF
• HPBW=16” @ CO(1-0)• 25 beams! + OTF
Array receivers“25BEARS”
• HPBW=22” @ CO(3-2)• Tsys~150K! + OTF
NRO 45m Atacama Submillimeter Telescope Experiment
“CATS345”
Highly uniform quality
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12CO(1-0) map with NRO 45m
12CO(1-0) with 45m Velocity field
1 kpcMany GMCs are identified Globally galactic rotation
Tosaki et al. 2011
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Color : 12CO(3-2) with ASTEGrey & contour : 12CO(1-0) with NRO 45m
ΔTmb ~ 13 -20 mk
5×5
7.3×3.3
4.2×4.2
5.2×5.6
2.5×3 3.3×3.3
4.4×4
2.5×2.5
Total ~ 140 arcmin2
Wide range of CO(3-2)/CO(1-0)
Miura et al. 2012
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1.1 mm mapKomugi et al. 2011
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1.1 Formation of molecular clouds1.2 Relation between molecular gas and star formation1.3 Evolution of Giant Molecular Clouds1.4 Radial gradient of dust temperature
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1.1 Formation of molecular clouds– Molecular gas is formed more efficiently in inner region
than outer region ( Tosaki et al. 2011 )
CO+HI CO+SFR
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Correlation between gas surface density and fmol
Two distinct sequences on the Σgas – fmol
Σgas
fmol
2
2mol HHI
H
f
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Molecular gas fraction; fmol
Function of 1. metallicity Z2. radiation field U3. gas pressure (or gas volume density n)(Elmegreen 1993)
high Z/high n efficient H2 formation⇒high U efficient H2 destruction⇒
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Vilchez et al. 1988
• Sharp increase of metallicity in the central region from ~2kpc
• Model calculations are consistent with the observed results quantitatively
2 kpc
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1.2 Relation between molecular gas and star formation
Kennicutt-Schmidt law• global correlation between
surface density of gas and star formation rate
To what scale is the Kennicutt-Schmidt law valid?
(Kennicutt et al. 2007)
M51
0.5-2kpc scale
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Check by changing spatial resolution from 1kpc to 80pc
Becomes looser with higher spatial resolution
⇒The Kennicutt-Schmidt law becomes invalid in GMC scale (~80pc)
Difference of evolutionary stage of GMCs
Σ(S
FR
) Hα
,corr [
Moyr
-1p
c-2]
(Onodera et al. 2010)Σ(H2)[Mo pc-2]
Resolution~80pc ~250pc
~500pc ~1kpc
2σ
• Breakdown of the Kennicutt-Schmidt law at high resolution (~ 80 pc)
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(Onodera et al. 2012 PASJ in press)
SFR vs. CO(3-2) intensitySFR vs. CO(1-0) intensity
Correlation between CO(3-2) and SFR => CO(3-2) traces denser and warmer gas
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1.3 Evolution of Giant Molecular Clouds– Variation of star-forming activity in molecular clouds ( Miura et al. 2012 )
Type C:With HII regions With young stellar groups (< 10 Myr)
71 GMCs• Ha, 24um => HII regions • Stellar groupsOptical data => age of stars
CO(3-2)/CO(1-0)
CO(3-2) + young stars CO(1-0) + young stars
Ha + young stars
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Classification of GMCs: 4 types of GMCs
Type A:No HII regions No young stellar groups
1 %
Type B:With HII regions No young stellar groups
20 %
Type C:With HII regions With young stellar groups (< 10 Myr)
45 %
Type D:With HII regions With old stellar groups (10-30 Myr)
34 %
Þ Life time of a GMC with a mass > 105 M => 20-40 Myr
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CO(3-2)/CO(1-0) => fraction of warm and dense gas
• GMCs with high SFR have higher CO(3-2)/CO(1-0) ratio
=> higher dense and warm gas fraction (Consistent with the correltion between CO(3-2) and SFR)
• Higher mass GMCs have higher CO(3-2)/CO(1-0) ratio (for GMCs with low SFR)
=> higher dense gas fraction
Red > 5x10-9Mo yr-1 pc-2
Blue < 5x10-9Mo yr-1 pc-2
1.3 Evolution of Giant Molecular Clouds– Relation between properties of molecular clouds (evolutionary
stage, mass) and dense gas fraction ( Onodera et al. 2012 )
Muraoka+ 2007
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M33 AzTEC / ASTE
・ D= 0.84 Mpc, opt. size = 70’ x 40’
・ obsered 2007-08, 30 hours on source avg. τ220GHz = 0.06
・ 30’ x 30’ x 2 field, 28” = 120pc res. most of SF disk
・ 1σ = 4-5 mJy/b = ~ 600 Modust
・ 1100 um concentrated along spiral arms, SF regions. Good spatial correlation w/ HI overdensity regions
・ can be used for : Dust physics (w/ AKARI, Spitzer, Herschel) GMC evolution, SF studies (w/ CO, HI) star cluster / galaxy evolution (w/ Subaru)
1kpc
Komugi et al. 2011
Cold dust temperature mapfrom 1.1mm and Spitzer data
Smooth gradient from G.C> to outer R
1.4 Radial gradient of dust temperature
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2. Preliminary results of ALMA cycle 0 observations of M83 (PI: A. Hirota)• Mapping of M83 in
12CO(1-0)• HPBW=2.3”~50pc• GMC can be
resolved
• Best target for the comparison of GMC properties in spiral arms, bar, and central region
=> Influence on the GMC properties and their star forming activityHubble
45m+NMA200pcX100pc
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ALMA Cycle 1 observations (PI: A. Hirota)
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3 . CO Galactic Plane Survey with the NRO 45-m telescope
• OTF mapping of the Galactic plane and the outer disk in 12CO(1-0), 13(1-0), C18O(1-0) (simultaneously) with FOREST
• Mapping area– l : 10° ~ 50° b : ±1° ( 80 deg2)
• Spiral arms ( Perseus, Sagittarius. Scutum-Centarus arms ) , bar sturcture, molecular gas ring
– l : 198° ~ 236° b : ±1°• Comparison between inner and outer regions (GemOB1,
MonOB1, Maddalena cloud, CMa OB1 etc)• Closer than the inner region => Noise level ~ 3 times higher
than the inner region=> Observing time : ~1/9
FOREST2X2 beam X 2 Pols X 2SB
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NASA/R. Hurt
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• Advantages of NRO survey– High angular resolution
Þ Can resolve clumps in the main Galactic structures (arm, bar, inner disk, outer disk)
– Multi-line observation (simultaneously)Þ Structure of molecular clouds : Diffuse molecular gas – dense gas
– Collaboration with VERAÞ measurements of the distance with VERA
GRS
NRO survey
Nakanishi et al. 2006
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Members• Kagoshima univ.
Handa, T., Nakanishi, H., Omodaka, T., Tanaka, A.( M2 ) , Matsuo, T.( M2 ) , Kamezaki(D1), Yoshida(M1),
• Osaka prefecture univ.Onishi, T., Nishimura (D2), Tokuda (M2)
• Joetsu education univ.Tosaki, T., Odaka(M1)
• Meisei univ.Onodera, S., Sofue, Y., Tsuda, Y.( M2 ) , Ozawa, T. ( M2 )
• ISASTsuboi, M.
• NROKuno, N., Umemoto, T., Hirota, A. ( PD ) , Matsui K. (PD)
• Chili observatoryHiguchi, A. ( PD )
• Mizusawa VLBI observatoryHonma, M. et al.
• JCMT: CO(3-2)• Mini-TAO: Paα
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Summary• M33
– Molecular gas is formed more efficiently in the inner region than outer region
– The Kennicutt-Schmidt law becomes invalid in GMC scale (~80pc) for CO(1-0), but it is still valid for CO(3-2)
– Life time of GMCs is estimated to be 20-40 Myr– Correlations between
• star forming activity and CO(3-2)/CO(1-0) ratio of GMCs• GMC mass and CO(3-2)/CO(1-0) ratio
– The cold dust temperature gradually decreases with radius• M83
– Excellent data of the ALMA cycle 0– Larger area will be mapped by ALMA cycle 1 observations
• CO Galactic Plane Survey with the NRO 45-m– GMC evolution and dense clump formation
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