Chemical conditions within the G333 Giant Molecular Cloud

1. Supervisors: Maria Cunningham (UNSW), James Urquhart (CSIRO)Michael Burton (UNSW) Collaborators: Nadia Lo (UNSW/CSIRO), BhaswatiMookerjea (Tata Institute) Great Barriers in High Mass Star Formation, 14th September 2010 Vicki Lowe University of New South WalesCSIRO Astronomy and Space Science Chemical conditions within the G333 Giant Molecular Cloud

2. Motivation  G333 GMC CLUMPFIND  Abundances  EGOs Motivation “Low mass stars are like weeds in the Galaxy” – Tom Megeath Characterising turbulence in molecular clouds (power spectrum analysis, D-variance analysis) Following molecular abundances through an entire cloud complex (e.g. principal component analysis, Lo et al., 2009; 13CO & masers, Breen et al., 2007)

3. Motivation  G333 GMC CLUMPFIND  Abundances  EGOs Motivation  G333 GMC CLUMPFIND  Abundances  EGOs The G333 Giant Molecular Cloud The G333 Giant Molecular Cloud Green Fuzzy HII region (RCW 106) b l 13COBains et al. (2006) C18OWong et al. (2008) Spitzer GLIMPSE: 3.6 µm (blue, starlight), 4.5 µm (green, shocked gas), 8.0 µm (red, ionised HII regions) Within the Galactic Molecular Ring, 3.6 kpc away 1.2 mm dust continuum Mookerjea et al. (2004)

4. Motivation  G333 GMC CLUMPFIND  Abundances  EGOs Dust continuum Mookerjea et al. (2004) • SIMBA on SEST 1.2 mm dust continuum • Cool, dense gas tracer • Molecules are complex • depletion, excitation • Use millimetre continuum to create a mask for molecules

5. Motivation  G333 GMC CLUMPFIND Abundances  EGOs Clump analysis CLUMPFIND • 1.2 mm continuum dust clumps was used as a mask to compare all molecular data • STARLINK(http://starlink.jach.hawaii.edu) • Clump identification algorithms • CLUMPFIND, GAUSSCLUMP, FELLWALKER, REINHOLD • 63 dust clumps were identified (3σcut-off)

6. Motivation  G333 GMC  CLUMPFIND  Abundances EGOs Chemical comparisons (i) Dense cold (< 20 K) gas tracern ~ 105 cm-3 Cold dense quiescent gas tracer High density tracer n ~ 104 cm-3 Optically thin Ubiquitous gas tracer Outflow & inflow tracer

7. Motivation  G333 GMC  CLUMPFIND  Abundances EGOs Chemical comparisons (ii) High density (n ~ 106 cm-3) tracer & Hot core molecule High density (n ~ 106 cm-3) tracer & Chemical clock Photodissociation regions Shocked gas

8. Motivation  G333 GMC  CLUMPFIND  Abundances EGOs EGOs / Green Fuzzies C2H – PDRs N2H+ – Cold, dense quiescent gas tracer

9. Motivation  G333 GMC  CLUMPFIND  Abundances  EGOs Summary Website: www.phys.unsw.edu.au/~mariac/dqs/dqs.html • The Mopra G333 Survey mapped approx. 20 different molecular transitions • Used 1.2 mm continuum dust clumps as a mask to compare all molecular data • CLUMPFIND with 3σ cut-off produced 63 millimetre continuum clumps • Variety of chemical conditions • e.g. green fuzzies Thank you  Poster #37 