Project: The outflows in G5.89-0.39 PI: Klaassen Time: 8 hrs 2. One short paragraph with science goal(s) When the massive star forming region G5.89-0.39 is observed with a single dish (i.e. the JCMT), a large scale (diameter ~1pc, ~2') outflow predominantly in the E-W direction is observed (Klaassen et al. 2006). When it is observed with an interferometer (i.e. the SMA), other, much smaller outflows are observed predominantly in the NE-SW direction (Sollins et al. 2005, Hunter et al. 2008). A high resolution ALMA mosaic (with total power flux included) will show if/how these outflows are related to eachother. 3. Number of sources G5.89-0.39; which has already been observed in CO J=3-2 at the JCMT (15'' resolution) and SMA (3'' resolution) 4. Coordinates: 4.1. Rough RA and DEC RA 18 hr, DEC -24 deg 4.2. Moving target: no 4.3. Time critical: no 4.4. Scheduling constraints: None 5. Spatial scales: 5.1. Angular resolution (arcsec): 0.2'' 5.2. Range of spatial scales/FOV (arcsec): 0.2'' - 2.5' these observations will require mosaicing, as well as total power observations (and ACA observations for middle scale structures) 5.3. Required pointing accuracy: 0.1'' 6. Observational setup 6.1. Single dish total power data: required Observing modes for single dish total power: OTF mapping 6.2. Stand-alone ACA: required 6.3. Cross-correlation of 7m ACA and 12m baseline-ALMA antennas: no 6.4. Subarrays of 12m baseline-ALMA antennas: no 7. Frequencies: 7.1. Receiver band: Band 7 7.2. Lines and Frequencies (GHz): CO & 13CO J=3-2, SiO J=8-7 (since they've already been observed with the JCMT and SMA) 7.3. Spectral resolution (km/s): 0.25 km/s 7.4. Bandwidth or spectral coverage (km/s or GHz): CO linewidths in this source can get up to 200 km/s 8. Continuum flux density: 8.1. Typical value (Jy): 2 8.2. Required continuum rms (Jy or K): 0.02 Jy 8.3. Dynamic range within image: 100 8.4. Calibration requirements: absolute ( 1-3% / 5% / 10% / n/a ) repeatability ( 1-3% / 5% / 10% / n/a ) relative ( 1-3% / 5% / 10% / n/a ) 9. Line intensity: 9.1. Typical value (K or Jy): CO = 45 K (full power) 9.2. Required rms per channel (K or Jy): 0.5 K 9.3. Spectral dynamic range: 9.4. Calibration requirements: absolute ( 1-3% / 5% / 10% / n/a ) repeatability ( 1-3% / 5% / 10% / n/a ) relative ( 1-3% / 5% / 10% / n/a ) 10. Polarization: no 11. Integration time for each observing mode/receiver setting (hr): each pointing will take 2.5 minutes. Since the ALMA beam at 345 GHz is 18'', the mosaic pointings will need to be spaced by 9''. To fully map the large scale outflow, this will require 170 pointings. At 2.5 min. per pointing, this project requires 7 hours of integration with 50 antennas (and much smaller integration times with the ACA and TP antennae). 12. Total integration time for program (hr): about 8 hours 13. Comments on observing strategy : (optional)