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Erik Muller ATNF/CSIRO

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?.

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Erik Muller ATNF/CSIRO

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  1. 12CO(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.

  2. Why CO in the Mag. Clouds? • 12CO(1-0) is a tracer for lower-density molecular gas - signpost for SF. • MCs are nearby (50-60 kpc) & have very low metallicities • (LMC=0.5 Zsol, SMC = 0.1 Zsol) , • Emulate conditions as they were in the early universe?

  3. Technical… • Observation strategy: • Observe ~5x5 amin region in OTF mode (RA - direction) • CO(1-0) (115.271 GHz) • ~1.75 hrs per area • BW~64 MHz • ΔV = ~0.16 Km/s • RMS~0.4 K (before smoothing) • Tsys @115 GHz ~>400 K

  4. SMC: SW SF region. Spitzer data: Bolatto et al. 2005 (Priv. Comm)

  5. SMC: CO according to NANTEN N66 Nanten 12CO(1-0) overlaid on SERC-J. Mizuno et al, 2001 N27 N12 N84

  6. CO CO + NANTEN Rubio et al, 1993a, 1993b,1996 SMC: 12CO(1-0) Latest result, smoothed to 90 asec, rebinned in velocity to ~0.5km/s, 3sig clip.

  7. N12/LIRS 36 N27/LIRS 49 SMC B1#1 N25/26 N21/23 ?? SMC: 12CO(1-0) CO Latest result, smoothed to 90 asec, rebinned in velocity to ~0.5km/s, 3sig clip. Data is ‘first pass’ only. Very noisy! Only three peaks appear where ICO>5sig! Need deeper observations…

  8. SMC: 12CO(1-0) New Mopra Results are generally consistent with the literature. “Clumpfind” does not perform well with noisy data. Using alternatives…

  9. CO N12/LIRS 36 N27/LIRS 49 SMC B1#1 N25/26 N21/23 ?? SMC: 12CO(1-0), HI HI (1/25) CO

  10. SMC: ASTE/APEX • APEX, high order transitions of CO (4-3) • Comparable resolutions to Mopra • ASTE observations are underway (U Nagoya) Contours: APEX CO(4-3) transition. Background image: 2MASS J band – (UMASS/IPAC)

  11. LMC, SMC: 12CO(1-0) • 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..)

  12. Hα N12/LIRS 36 N27/LIRS 49 N25/26 N21/23 SMC: CO, Hα CO

  13. 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)

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