1. The COMPLETE Survey of Star-Forming Regions at Age 2 Alyssa A. Goodman Harvard-Smithsonian Center for Astrophysics cfa-www.harvard.edu/~agoodman

2. 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) Di Li (CfA) Doug Johnstone (HIA, Canada) Naomi Ridge (UMASS/FCRAO  CfA) Scott Schnee (CfA, PhD student) Mario Tafalla (OAS, Spain) Tom Wilson (MPIfR) COMPLETE The COordinated Molecular Probe Line Extinction Thermal Emission Survey

3. COMPLETE’s Birthplace: The 2001 Santa Cruz Star Formation Workshop

4. The Lesson of Coordination: B68 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

5. Un(coordinated) Molecular- Probe Line, Extinction and Thermal Emission Observations Molecular Line Map Nagahama et al. 1998 13 CO (1-0) Survey Lombardi & Alves 2001Johnstone et al. 2001

6. Bipolar outflows from young stars + Stellar winds & photons from older stars + Large Explosions (SNe, GRBs) create, maintain, & destroy molecular clouds & ultimately determine stellar output vs. time a.k.a. what we’d all like to know

7. Time is a key dimension but spatial statistics remain our best hope to understand it.

8. Could we really…? 1 day for a 13 CO map when the 3 wise men were 40 1 minute for the same 13 CO map today

9. COMPLETE The COordinate d Molecular Probe Line Extinction Thermal Emission Survey

10. COMPLETE, Part 1 Observations: 2003-4-- Mid- and Far-IR SIRTF Legacy Observations: point-source census, dust temperature and column density maps ~5 degrees mapped with ~15" resolution (at 70  m) 2002-3-- NICER/2MASS Extinction Mapping: dust column density maps ~5 degrees mapped with ~5' resolution 2003-4-- SCUBA Observations: dust column density maps, finds all "cold" source ~20" resolution on all A V >2” 2002-4-- FCRAO/SEQUOIA 13 CO and 13 CO Observations: gas temperature, density and velocity information ~40" resolution on all A V >1 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 >10-degree scale Near-IR Extinction, Molecular Line and Dust Emission Surveys of Perseus, Ophiuchus & Serpens, <1 arcmin resolution

11. COMPLE TE, Part 2 (2003-5) Observations, using target list generated from Part 1:  NICER/8-m/IR camera 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 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). 10 pc to 0.01 pc

12. Time Dependences we did not worry about when David, Chris & Frank were 50 1.Structures in a turbulent, self-gravitating, flow are highly transient 2.Outflows are episodic 3.Young stars can move rapidly 4.Energetically significant spherical outflows (e.g. SNe, winds) are common in star-forming regions 5.(Aging)

13. 1. Structures are Highly Transient Bate, Bonnell & Bromm 2002 MHD turbulence gives “t=0” conditions; Jeans mass=1 M sun 50 M sun, 0.38 pc, n avg =3 x 10 5 ptcls/cc forms ~50 objects T=10 K SPH, no B or  movie=1.4 free-fall times

14. L1448 Bachiller et al. 1990 B5 Yu, Billawala & Bally 1999 Lada & Fich 1996 Bachiller, Tafalla & Cernicharo 1994 2. YSO Outflows are Highly Episodic

15. Outflow Episodes:Position-Velocity Diagrams Figure from Arce & Goodman 2001 HH300 NGC2264

16. Episodic Outflows: Steep Mass-Velocity Slopes Result from Summed Bursts Observed Power-law Slope >2 (2=momentum-conserving shell) Arce & Goodman 2001

17. 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 1999 Arce & Goodman 2001

18. 3. Powering source of (some) outflows may zoom through ISM

19. 1 pc “Giant” Herbig- Haro Flow from PV Ceph Image from Reipurth, Bally & Devine 1997

20. moving PV Ceph Episodic ejections from a precessing or wobbling moving source Goodman & Arce 2003

21. PV Ceph is moving at ~10 km s -1 Goodman & Arce 2003 1 pc

22. Moving Source & Slowing Knots 500x10 15 400 300 200 100 0 Distance along x-direction (cm) 15x10 3 1050 Elapsed Time since Burst (Years) 70 60 50 40 30 20 10 0 Star-Knot Difference/Star Offset (Percent) KnotStarStar-Knot Difference Star-Knot Difference (%) Initial jet 250 km s - 1 ; star motion 10 km s -1 Goodman & Arce 2003

23. Dynamical Time Estimates off by x10 Goodman & Arce 2003 For an HH object at 1 pc from source, dynamical time calculation overestimates age by factor of ~ten.

24. (All the) Maps of “Giant” Outflows, c. 2002 See references in H. Arce’s Thesis 2001

25. Time Dependences we did not worry about when David, Chris & Frank were 40 1.Structures in a turbulent, self-gravitating, flow are highly transient 2.Outflows are episodic 3.Young stars can move rapidly 4.Energetically significant spherical outflows (e.g. SNe, winds) are common in star-forming regions

26. COMPLETE Discovery of a Heated Dust Ring in Ophiuchus Goodman, Li & Schnee 2003 2 pc

27. Smoke Signals from Ophiuchus 0.5 x 10 51 erg SN into 10 5 cm -3 2 pc in 200,000 yr T=38K v exp =1.7 km s -1 Heated Dust Ring Region known as “  -Oph Cluster” Re-calibratedIRAS Dust Column Density Re-CalibratedIRAS DustTemperature ROSAT PSPC In each panel where itis shon, thewhite ring shows a 2 pccircle, correspondingto the size and shape ofthe heatedring apparent in the IRAS Temperature Map. ROSAT PointedObservation Real  -Oph Cluster inside newly discovered heated ring 1RXS J162554.5-233037 The star  -Oph and RXJ1625.5- 2326 Goodman, Gaensler, Wolk & Schnee 2003

28. Ionized Gas in the Ophiuchus Smoke Shell HH SII SHASSA Data courtesy of John Gaustad

29. Putting this in Perspective

30. COMPLETE Warm Dust Emission shows Great Bubble in Perseus 2 x 10 51 erg SN into 10 4 cm -3 5 pc in 1 Myr T=30K v exp =1.5 km s -1

31. Perseus in (Coldish) Molecular Gas Map of 1200 13 CO Spectra from Bachiller & Cernicharo 1986 (made with Bordeaux 2.5-m, Beam Area = 31 x FCRAO) COMPLETE/FCRAO noise is twice as low, and velocity resolution is 6 x higher

32. COMPLET E Perseus IRAS + FCRAO (73,000 13 CO Spectra)

33. Perseus Total Dust Column (0 to 15 mag A V ) (Based on 60/100 microns) Dust Temperature (25 to 45 K) (Based on 60/100 microns)

34. Hot Source in a Warm Shell + = Column Density Temperature

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

36. JCMT/SCUBA COMPLETE >10 mag A V 2 4 6 8 Perseus Ophiuchus 10 pc ~100 hours at SCUBA = in SCUBA archive = observed Spring ‘03 NGC1333 Map All at >5 mag, by 2004

37. My Near-Term “COMPLETE” Agenda Statistical Evaluation of Outflows’ Role Evaluation of Constructive/Destructive Role of Explosions/Winds Tracking down progeny

38. “Early” Times

39. “Later” Times

40. 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) Di Li (CfA) Doug Johnstone (HIA, Canada) Naomi Ridge (UMASS/FCRAO  CfA) Scott Schnee (CfA, PhD student) Mario Tafalla (OAS, Spain) Tom Wilson (MPIfR)

41. Questions up for Grabs How do processes in each stage impact upon each other? (Sequential star formation, outflows reshaping clouds…) How long do “stages” last and how are they mixed? (Big cloud--“Starless” Core--Outflow--Planet Formation--Clearing) What is the time-history of star production in a “cloud”? Are all the stars formed still “there”?

42. Extra Slides

43. Polarization

44. NatureNurture Shu, Adams & Lizano 1987

45. CorporationsEnvironmentalists Shu, Adams & Lizano 1987

46. TheoryObservation Shu, Adams & Lizano 1987 Some

47. “Steep” Mass-Velocity Relations HH300 (Arce & Goodman 2001a) Slope steepens when  corrections made –Previously unaccounted-for mass at low velocities Slope often (much) steeper than “canonical” -2 Seems burstier sources have steeper slopes? -3 -8 -4 -8 Mass/Velocity Velocity

48. How much gas will be pulled along for the ride? Goodman & Arce 2002

49. Perseus in (Coldish) Molecular Gas

50. Cores = Order from Chaos Order; N~R 0.9 ~0.1 pc (in Taurus) Chaos; N~R 0.1