COMPLETE The COordinated Molecular Probe Line Extinction Thermal Emission Survey Alyssa A. Goodman, Principal Investigator (CfA) João Alves (ESA, Germany) Héctor Arce (Caltech) Paola Caselli (Arcetri, Italy) James DiFrancesco (HIA, Canada) Mark Heyer (UMASS/FCRAO) Doug Johnstone (HIA, Canada) Scott Schnee (CfA, PhD student) Mario Tafalla (OAN, Spain) Tom Wilson (MPIfR/SMTO)

Current, Un-coordinated, State of Affairs Molecular Line Map Nagahama et al CO (1-0) Survey Lombardi & Alves 2001Johnstone et al. 2001

The Rewards of Coordination C 18 O Dust Emission Optical Image NICER Extinction Map Radial Density Profile, with Critical Bonnor-Ebert Sphere Fit Coordinated Molecular-Probe Line, Extinction & Thermal Emission Observations of Barnard 68 This figure highlights the work of Senior Collaborator João Alves and his collaborators. The top left panel shows a deep VLT image (Alves, Lada & Lada 2001). The middle top panel shows the 850  m continuum emission (Visser, Richer & Chandler 2001) from the dust causing the extinction seen optically. The top right panel highlights the extreme depletion seen at high extinctions in C 18 O emission (Lada et al. 2001). The inset on the bottom right panel shows the extinction map derived from applying the NICER method applied to NTT near-infrared observations of the most extinguished portion of B68. The graph in the bottom right panel shows the incredible radial-density profile derived from the NICER extinction map (Alves, Lada & Lada 2001). Notice that the fit to this profile shows the inner portion of B68 to be essentially a perfect critical Bonner-Ebert sphere

COMPLETE, Part 1 Observations: NICER/2MASS Extinction Mapping: dust column density maps ~5 degrees mapped with ~5' resolution FCRAO/SEQUOIA 12 CO and 13 CO Observations: gas temperature, density and velocity information ~40" resolution on all A V >1(COMPLETE Awarded Key Project Status, 10/02) SCUBA Observations: dust column density maps, finds all "cold" source ~20" resolution on all A V >6 mag (COMPLETE Awarded Time, 12/10/02) c2d Mid- and Far-IR SIRTF c2d Legacy Observations: dust temperature and column density maps ~5 degrees mapped with ~15" resolution (70  m + NICER on point source distribution) Science: –Combined Thermal Emission data: dust spectral-energy distributions, giving emissivity, T dust and N dust –Extinction/Thermal Emission inter-comparison: unprecedented constraints on dust properties and cloud distances, in addition to high-dynamic range N dust map –Spectral-line/N dust Comparisons Systematic censes of inflow, outflow & turbulent motions enabled –CO maps in conjunction with SIRTF point sources will comprise YSO outflow census 5 degrees (~tens of pc) SIRTF Legacy Coverage of Perseus

COMPLE TE, Part 2 (2003-5) Observations, using target list generated from Part 1:  NICER/8-m/IR camera OIR Observations: best density profiles for dust associated with "cores". ~10" resolution  FCRAO + IRAM N 2 H + Observations: gas temperature, density and velocity information for "cores” ~15" resolution, ongoing beginning 2002 Science:  Multiplicity/fragmentation studies  Detailed modeling of pressure structure on <0.3 pc scales  Searches for the "loss" of turbulent energy (coherence) FCRAO N 2 H + map with CS spectra superimposed. (Lee, Myers & Tafalla 2001).

Is this Really Possible Now? 1 day for a 13 CO map then 1 minute for a 13 CO map now

Pilot COMPLE TE Observations in Perseus, Spring 2002

The action of multiple outflows in NGC 1333? SCUBA 850 mm Image shows N dust (Sandell & Knee 2001) Dotted lines show CO outflow orientations (Knee & Sandell 2000)

Perseus according to IRAS (warm dust!)

COMPLETE: SCUBA >10 mag A V Perseus Ophiuchus 10 pc Johnstone, Goodman & the COMPLETE team, SCUBA 2003(?!) ~100 hours at SCUBA

COMPLETE SCUBA-Prep led to Discovery of a Heated Dust Ring in Ophiuchus Goodman, Li & Schnee pc

…and the famous “1RXS J ” is right in the Middle !? 2 pc

The “COMPLETE” + c2d Truth about Star Formation, c Statistical Evaluation of Outflows’ Role Evaluation of Constructive/Destructive Role of Explosions/Winds Tracking down progeny (includes USNO-B work) All data to NVO

Truth?: Part 1

Part II

Complications Observing Biases Temporal Behavior Regional Variations

Temporal Evolution Mass [M sun ] Velocity [km s -1 ] Power-law Slope of Sum = -2.7 (arbitrarily >2) Slope of Each Outburst = -2 as in Matzner & McKee 2000 Example 1: Episodicity changes Energy/Momentum Deposition (time) Example 2: (Some) Young stars may zoom through ISM

1. Episodic Outflows: Steep Mass-Velocity Slopes Result from Summed Bursts Power-law Slope of Sum = -2.7 (arbitrarily >2) Slope of Each Outburst = -2 as in Matzner & McKee 2000 Arce & Goodman 2001b