1 / 8

ALMA Science Workshop May 14-15, 2004 Star and Planet Formation Breakout Session

ALMA Science Workshop May 14-15, 2004 Star and Planet Formation Breakout Session. Facilitators: Doug Johnstone & Debra Shepherd. Science & the DSRP. Detailed summary of representative proposals: Claire Chandler , DRSP 2.1.6, OTF survey of large field

tilly
Download Presentation

ALMA Science Workshop May 14-15, 2004 Star and Planet Formation Breakout Session

An Image/Link below is provided (as is) to download presentation Download Policy: Content on the Website is provided to you AS IS for your information and personal use and may not be sold / licensed / shared on other websites without getting consent from its author. Content is provided to you AS IS for your information and personal use only. Download presentation by click this link. While downloading, if for some reason you are not able to download a presentation, the publisher may have deleted the file from their server. During download, if you can't get a presentation, the file might be deleted by the publisher.

E N D

Presentation Transcript

  1. ALMA Science WorkshopMay 14-15, 2004Star and Planet Formation Breakout Session Facilitators: Doug Johnstone & Debra Shepherd ALMA Science Workshop - May 2004

  2. Science & the DSRP • Detailed summary of representative proposals: • Claire Chandler, DRSP 2.1.6, OTF survey of large field • James Di Francesco, DRSP 2.1.9, Envelope/disk structure • David Wilner, protoplanetary disks - gas and dust continuum • Science talks: • Yancy Shirley - Dust continuum surveys – bringing in the DRSP • Derek Lis - Deuteration and other fractionations ALMA Science Workshop - May 2004

  3. Key issues from Science & DSRP • A significant number of star formation projects image large fields (> 1000 pointings) and require ACA with total power. OTF mosaics easily push the data rate beyond 6/60 MB/s specs. • Need for same uv coverage across mosaic  must get through mosaic fast, before configuration changes significantly. • Can’t always assume ACA integration time = 4 x ALMA. Some science requires same sensitivity/beam to get same mass sensitivity  ~90 times more integration time on ACA than on ALMA. Some sources only need same sensitivity of the uv data in overlap region between ACA & ALMA  4 x ALMA Needs more thought to determine impact on operations and determine how the ACA over-subscription will be handled. ALMA Science Workshop - May 2004

  4. Missing science in DSRP: • Transition objects to debris disks with little gas & dust. These will be closer, bigger & will have low surface brightness in large scale structure. Very challenging to get ACA, TP data with high enough sensitivity. This will impact planned capabilities because it will put pressure on ACA observing time that already appears to be more over-subscribed than the ALMA array. • Mosaic surveys with ACA only to get large scale structure in lesser known southern sources. Again, taxes an already severely over-subscribed ACA. • Continuum modeling of SEDs and uv amplitudes. Needs wide range of frequency to get good SED, 1-3% absolute calibration accuracy important across bands to constrain models. ALMA Science Workshop - May 2004

  5. More Issues: • Will ALMA plans support early science proposals? • Major problem: supporting mosaics, since lack of OTF mosaic capabilities at early science will delay science return for star forming regions, the ALMA project should think more about how and when this will be implemented. • If can't get through mosaic fast enough to get same uv coverage for all pointings, then relative calibration at different times must be extremely good. Issue: if mosaic not finished will it take a year to get back to a configuration to finish a mosaic? BAD. • If ALMA pipeline heuristics not well developed, need to guarantee one-on-one reduction/imaging support for non-expert users. ALMA Science Workshop - May 2004

  6. Synergy with other projects • ACA/TP over-subscription: Single dish surveys critical for large mosaics to pinpoint interesting regions for ALMA. Minimize ACA/TP time. JCMT/SCUBA-2 may be critical. • Need FIR - NIR - submm to get accurate SEDs. • JCMT/SCUBA2 & SMA at submm, • VLT at near-IR, • Need eVLA to characterized ionized gas at cm wavelengths: • Since high mass cores will be optically thick in dust emission with ALMA, eVLA at 43 GHz will be critical to see optically thin dust emission - As Neal Evans mentioned, this is the critical type of source to relate galactic star formation properties to more distant star bursts. ALMA Science Workshop - May 2004

  7. Questionnaire • Not clear from list what of science support activities what are core functions and what are non core functions. Needs to be made clearer. • Beyond core functions, highest priorities seem to be: 1) getting face-to-face support for reduction/imaging and training for students; and 2) Software development of analysis tools. • Band 10 is, of course, important. Very good that the Japanese will provide this. Some people think Bands 2 & 5 are the next most important. Band 8 also important. • Need to send back Questionnaire see how the statistics fall out. ALMA Science Workshop - May 2004

  8. Comments on the importance and/or science case for the ACA It is absolutely critical to star and planet formation projects Time required for ACA observations needs to be looked at more critically ALMA Science Workshop - May 2004

More Related