1. 21st-Century Astronomy Sensitivity Higher Sensitivity Enables: –Large surveys –Deep exposures Resolution Higher Resolution Enables: –Detailed view of nearby regions –Close-up views of distant regions Computing Enhanced Computing Enables: –More complete analysis, and long-term storage, of data –Much more realistic numerical simulations

2. Higher Sensitivity: Surveys Goal: Complete censuses of star-forming material (gas, dust) and YSOs in nearby SFRs. Science: Understand star-formation efficiency in detail nearby, and apply results to unresolved regions at larger distance. Instruments Needed: Dedicated, remotely controlled wide-field, high-sensitivity telescopes at near-IR through cm wavelengths

3. Surveying Dust in SFRs Dust: e.g. IRAM 30-m 50 OTF maps, 16 days of observing (Motte, André & Neri 1998) 30 arcmin To do much more (from the ground): –larger format mm/sub-mm arrays (in prep by IRAM, JCMT: CfA could contribute here) –Dedicated telescopes (e.g. HHT/12-m: CfA collaboration could be expanded) –Better sites (consider Atacama 15- m collaboration) –Large-interferometer (e.g. ALMA; use SMA experience, mostly just wait) –Fully exploit near-IR extinction techniques (use 2MASS data plus wide-field deep exposures from good IR camera on MMT/Magellan) State-of-the-Art 2000

4. Surveying Gas in SFRs Gas: Consider multi-line surveys (e.g. Bergin et al. 1997, above) or multi-region single- line surveys, or multi-line, multi-region surveys) To do much more: –Large-format mm/sub-mm detector arrays for spectroscopy on single-dishes (e.g. FCRAO's current SEQUOIA + future array for LMT; HHT/12-m/JCMT/CSO could all use one--CfA could build one?) –Interferometer surveys (merged BIMA/OVRO plus SMA could do nearest regions; ALMA & SKA will be best 10-30 year time horizon) –Dedicated telescopes (e.g. 12-m or post-LMT FCRAO could be dedicated to this, like CfA mini is now) –Better sites (consider Atacama 15-m collaboration--with spectral-line capablity, this would be better than FCRAO or 12-m, but time might be too limited for survey ) –In general: Explore multi-institution collaboration to achieve large amount of time required for surveys (e.g. SMA- BIMA/OVRO collaborative projects)

5. Young Stars in SFRs NICMOS Image Near 30 Doradus Two branches for research: Censuses, requiring wide-field images & much time; and detailed studies, requiring deep, high-resolution images (e.g. of disks/jets, planet-forming regions) Primary tool: Large-format near and mid-IR arrays (CfA should outfit MMT/Magellan appropriately; and Atacama telescope would be good for deep exposures) New twist: Proper motion surveys will give much information on dynamics of newly-born stars, plus jet kinematics

6. Higher Resolution: "Watching" Nearby Star Formation VLBI: masers tracing outflows from & disks around young stars Connected-element interferometers: Circumstellar disks and outflows, including kinematics, but now with sub-arcsec resolution (SMA/SKA/ALMA) Above the atmosphere: SIRTF resolution too low; SOFIA interesting at shortest 's Ground-based optical-style single-element observatories: –Direct imaging of YSOs –  Near-IR Spectroscopy of YSOs--age determinations are vital (should drive some MMT/Magellan planning) –highest-resolution (with A.O.) might be able to see extinction variations on tiny scales near YSOs Ground-based optical-style interferometers: Fluxes from young stars are very low & would require a huge amount of collecting area

7. Higher Resolution: Extragalactic Close-ups Need to connect our understanding of nearby SFRs with "empirical" extragalactic SF results –1 pc at 1 Mpc is 0.2" –1 km baseline at 450 microns gives 0.1" resolution –ALMA gives HST resolution CO (contours) on H I (color) in NGC 3627 (BIMA)

8. Computing "Proposal" for an Advanced Scientific Computing Division at the CfA Is there a need for a CfA-wide data archiving system? Would the CfA benefit from an on-site supercomputer, or better access to one? (for simulations & large data-reduction problems) Would on-site software specialists, who could develop expert systems to search new & existing databases, be beneficial? See http://cfa-www.harvard.edu/~agoodman/ascd/draft_7_00.html for more details.