Title Deep integration on the massive jet source HH80-81: the disk-outflow connection Pi D. Shepherd Time 95 hrs DRSP 2.0, re-submittal of DRSP 1.1 project 2.2.9 1. Name: Deep integration on the massive jet source HH80-81: the disk-outflow connection. 2. Science goal(s): HH 80-81 is a well-collimated jet powered by an intermediate-mass young stellar object with a spectral type later than B1. It is the most massive star known which powers a well-collimated, parsec-scale jet similar to those produced by low-mass young stellar objects. The dynamics of the jet suggest that it is a scaled-up version of a T Tauri star, thus, it should have an accretion disk with a *VERY* powerful wind. Assuming the outflow and central source has been mapped with ALMA and the source powering the outflow jet has been identified, this proposal seeks to map several outflow/disk tracers to get a handle on the disk properties and the outflowing wind as close to the surface of the disk as possible. Obtaining clear evidence for ionized or molecular gas outflow from the disk and providing constraints on where the outflow gas originates will help to determine whether a disk wind or X-wind powers this massive flow. This proposal requires very sensitive observations (to detect faint emission originating from the disk surface) at high resolution to resolve out confusing, extended emission. The disk radius that is relevant should be about 1-100 AU (= 0.5-50 mas at distance of 1.7 kpc). At 270-700 GHz (bands 7 & 9), the array will have a resolution of roughly 8-13 mas - this seems like a reasonable compromise between getting adequate resolution to see the fine-scale structure and not resolving out too much of the disk material. Lines of interest include hydrogen recombination lines (H25a, H21a) to trace ionized outflow, molecular disk tracers (e.g. CH3CN), and molecular outflow tracers (e.g. 12CO, C34S, 13CO, SiO, H13CO+) and even a H2O maser transition. 3. Number of sources: 1, single field. 4. Coordinates: 4.1. Rough RA and DEC Central coordinates: 18 19 12.11 -20 47 30.4 (J2000), (Galactic coordinates: LII= 10.8415 BII= -2.5916) 4.2. Moving target: no 4.3. Time critical: no 4.4. Scheduling constraints: (optional) None 5. Spatial scales: 5.1. Angular resolution (arcsec): 0.008"-0.013" (depending on line) 5.2. Range of spatial scales/FOV (arcsec): 10-1000 AU = 0.005" - 0.5" single field 5.3. Required pointing accuracy: 1 arcsec 6. Observational setup 6.1. Single dish total power data: no Observing modes for single dish total power: N/A 6.2. Stand-alone ACA: no 6.3. Cross-correlation of 7m ACA & 12m baseline-ALMA antennas: no 6.4. Subarrays of 12m baseline-ALMA antennas: yes/no 7. Frequencies: 7.1. Receiver band: Bands 7 and 9 7.2. Lines and Frequencies (GHz): 7.2.1 Receiver band 7: 6-10 lines around 280, 300, 340 GHz 7.2.2 Receiver band 9: 12-15 lines around 613-694 GHz. 7.3. Spectral resolution (km/s):0.1 to 0.3 km/s (differs with line depending on whether it is an outflow or disk/dense gas tracer). 7.4. Bandwidth or spectral coverage (km/s or GHz): 20-200 km/s per line 8. Continuum flux density: 8.1. Typical value (Jy): 0.5-10 mJy 8.2. Required continuum rms (Jy or K): 0.03 mJy (to detect primary driving source of the flow as well as any lower-mass YSOs in the cluster) 8.3. Dynamic range within image: > 20 Mixture of weak and bright emission in some lines. 8.4. Calibration requirements: absolute ( 1-3% / 5% / 10% / n/a ) 5% repeatability ( 1-3% / 5% / 10% / n/a ) 5% relative ( 1-3% / 5% / 10% / n/a ) 5% 9. Line intensity: 9.1. Typical value (K or Jy): Unknown at this resolution, this will be a deep survey to see if any are detected. At lower resolution, all lines are strong in star forming regions. We want microJy RMS levels. 9.2. Required rms per channel (K or Jy): It would be good to get 1 microJy/beam but this is unreasonable. Band 7: Choose 1 mJy/beam with 0.3 km/s resolution Band 9: Choose 2 mJy/beam 9.3. Spectral dynamic range: > 100 9.4. Calibration requirements: absolute ( 1-3% / 5% / 10% / n/a ) 5% repeatability ( 1-3% / 5% / 10% / n/a ) 1-3% relative ( 1-3% / 5% / 10% / n/a ) 1-3% 10. Polarization: No 10.1. Required Stokes parameters: 10.2. Total polarized flux density (Jy): 10.3. Required polarization rms and/or dynamic range: 10.4. Polarization fidelity: 10.5. Required calibration accuracy: 11. Integration time for each observing mode/receiver setting (hr): 12. Total integration time for program (hr): 10.1 Integration time: For a line with 0.3 km/s resolution: 1 mJy/beam RMS => 15 hrs integration (band 7, 275-370 GHz) 2 mJy/beam RMS => 80 hrs integration (band 9, 602-720 GHz) 13. Comments on observing strategy : (optional) (e.g. line surveys, Target of Opportunity, Sun, ...): -------------------------------------------------- Review v2.0: 2.2.9 Shepherd Deep integration on the massive jet source HH80-81 This project is fine as written although I agree with Munetake that it is not clear such high velocity resolution is needed in the first instance. That said, undoubtedly ALMA will try and do this type of observation!