12 12 CO(1-0) emission in CO(1-0) emission in the Magellanic the Magellanic Clouds, according to Clouds, according to Mopra Mopra (Also starring the Magellanic Bridge…) (Also starring the Magellanic Bridge…) Erik Muller Erik Muller ATNF/CSIRO ATNF/CSIRO Collaborators so far: Collaborators so far: Juergen Ott (PI, ATNF), Annie Juergen Ott (PI, ATNF), Annie Hughes (Swinburne), Tony Wong Hughes (Swinburne), Tony Wong (ATNF/UNSW), Jorge Pineda (Bonn) (ATNF/UNSW), Jorge Pineda (Bonn) and more. and more.
12 CO(1-0) emission in the Magellanic Clouds, according to Mopra (Also starring the Magellanic Bridge…). Erik Muller ATNF/CSIRO. Collaborators so far: Juergen Ott (PI, ATNF), Annie Hughes (Swinburne), Tony Wong (ATNF/UNSW), Jorge Pineda (Bonn) and more. Why CO in the Mag. Clouds?. - PowerPoint PPT Presentation
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1212CO(1-0) emission in CO(1-0) emission in the Magellanic Clouds, the Magellanic Clouds,
according to Mopraaccording to Mopra(Also starring the Magellanic Bridge…)(Also starring the Magellanic Bridge…)
Erik MullerErik Muller
ATNF/CSIROATNF/CSIROCollaborators so far: Collaborators so far:
Juergen Ott (PI, ATNF), Annie Hughes Juergen Ott (PI, ATNF), Annie Hughes (Swinburne), Tony Wong (ATNF/UNSW), (Swinburne), Tony Wong (ATNF/UNSW),
Jorge Pineda (Bonn) and more. Jorge Pineda (Bonn) and more.
Why CO in the Mag. Clouds?Why CO in the Mag. Clouds?
►1212CO(1-0) is a tracer for lower-density CO(1-0) is a tracer for lower-density molecular gas - signpost for SF.molecular gas - signpost for SF.
►MCs are nearby (50-60 kpc) & have MCs are nearby (50-60 kpc) & have very low metallicities very low metallicities (LMC=0.5 Z(LMC=0.5 Zsolsol, SMC = 0.1 Z, SMC = 0.1 Zsolsol) , ) , Emulate conditions as they were in the Emulate conditions as they were in the
Tmb=2.23 Tmb=2.23 ±0.4±0.4 I ICOCO=6.7 =6.7 ± 4, R± 4, Rcc~ ~ 15 pc15 pc
MMVIRVIR~3.3x10~3.3x104 4 (M(Msolsol) ) (!)(!)
New Mopra Results are generally consistent with the literature.
“Clumpfind” does not perform well with noisy data.
Using alternatives…
SMC: SMC: 1212CO(1-0), HCO(1-0), HIICO
N27/LIRS 49N12/LIRS 36
N25/26
N21/23
??
SMC B1#1
HI (1/25)CO
• APEX, high order transitions of CO (4-3) •Comparable resolutions to Mopra
• ASTE observations are underway (U Nagoya)
SMC: ASTE/APEX SMC: ASTE/APEX
Contours: APEX CO(4-3) transition.Background image: 2MASS J band – (UMASS/IPAC)
• ICO, Tmb are much lower for SMC than for LMC (can be x ~10!)
• Cloud radii are much smaller in SMC than for LMC• More exact quantifiction of ‘much smaller’ pending less noisy results •~Rlmc/Rsmc ~2-3 for brightest clouds).•ΔVlmc/ ΔVsmc ~2
•Mvirlmc/Mvirsmc ~ 8-12 (or more..)
LMC, SMC: LMC, SMC: 1212CO(1-0)CO(1-0)
Hα
SMC: CO, HSMC: CO, HααCO
N27/LIRS 49 N12/LIRS 36
N25/26
N21/23
SMC. Where to with Mopra?SMC. Where to with Mopra?
• Continue to fully sample SW area with Mopra? • Multi wavelength obs for N88/N66 ?• ASTE @ CO(3-2) has comparable resolution to Mopra @ CO(1-0)
• Other regions in SMC?• Existing CO(1-0) (and (2-1)) data for N66 are small field and mostly under sampled
•Dense core tracers (or ATCA? E.g. Muller+Ott in prep. HCO+, HCN)