The UNSW–CSIRO Millimetre Collaboration: An overview of the Star Formation Program Michael Burton.

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Presentation transcript:

The UNSW–CSIRO Millimetre Collaboration: An overview of the Star Formation Program Michael Burton

UNSW / CSIRO Collaboration MNRF-funded upgrade to ATCA (1997) UNSW SIP grant (1999-2001): Extend dish to 22-m for mm-capable performance Operate over mm “season” Research Tool Teaching Tool (how to get money from a university) MM astronomy Using a telescope (“Black Box” national facilities!) Extended for 2002 through UNSW RIBG

UNSW / CSIRO Collaboration 3 hands-on workshops help at Mopra / SSO ~ 20 students / postdocs / academics trained in mm’s ARC LIEF awarded for 2003/04: 8 GHz Digital Filterbank (+ Engineering Friend) UNSW / CSIRO / U Sydney / Monash New science opportunities: Extra-galactic molecular lines High-z (ie uncertain wavelength) Multiple lines MM-continuum

The Mopra 22-m Millimetre-Wave Observatory The biggest in the South Soon to be the only significantly sized 3-mm capable system too!

Mopra Operations Wait for Lucyna's talk! MOU between UNSW & CSIRO 3-4 month mm “season” VLBI, then split between UNSW and Open Time “Friend” supporting operations (Ramesh Balasubramanyam, Lucyna Kedziora-Chudczer) Documentation, communication, software www.phys.unsw.edu.au/astro/mopra Maintenance and Upgrades Pointing, Surface, Coma, Tuning, Correlator, MMIC An ongoing story…... Wait for Lucyna's talk!

The Multi-wavelength Milky Way Optical Near-Infrared (1–3.5µm, COBE) Far–Infrared (12–100µm, IRAS) Methanol Masers (6.6 GHz) Pestalozzi, 2002 Sites of massive star formation

HII Regions and Molecular Cores What's happening here?

Time-dependent Chemical Signatures? N-rich or C-rich? Is there a signature of the progress of star formation? Need to constrain the chemistry with observations! CH3CN CH3OH HC3N CH3OCH3 100 K 300 K Abundance Time Rodgers & Charnley, 2001 Ammonia injected from ice

Hot Core Chemistry in 18060-2005A See Cormac's Talk 850µm HCO+ CH3OH CH3CN HCN

See Tracey's talk A sequence of mm cores? CC JCMT SEST HMC HMC CC HMC 850µm Images HMC CC JCMT SEST HMC See Tracey's talk HMC CC UCHII HMC UCHII Minier et al, 2003

The structure of star-forming cores? Time-dependent chemical segregation (Lines) See Vincent's talk Source multiplicity (Continuum) Isolated Methanol Masers Coincident

Other Star Formation Programs Distances to MSX-selected sites of massive star formation (Hoare, Lumsden: U. Leeds) Methanol maser emission at mm-wavelengths (Cragg, Godfrey: Monash, Ellingsen: Tasmania) Massive star formation by coalescence or accretion (Walsh, Myers: CfA) Spectral line survey of HMCs (Kim) Protostellar disks (Maddison: Swinburne)

See Peter and Paul's talks! Yet more programs…... “Medium-mass” star formation Barnes The Search for Biogenic Molecules Hunt, Jones See Peter and Paul's talks!

Finally, a plea Three elements or five? Over full 85-110 GHz range Real-time phase correction (300m  3”; 3km  0.3”) Australia’s radio future depends on our achieving it soon! Mopra + ATCA provides a unique facility for mm-wave astronomy

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