2. The COMPLETE Survey of Star-Forming Regions: Nature vs. Nurture Alyssa A. Goodman Harvard-Smithsonian Center for Astrophysics cfa-www.harvard.edu/~agoodman

3. 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)

4. NatureNurture Shu, Adams & Lizano 1987

5. CorporationsEnvironmentalists Shu, Adams & Lizano 1987

6. TheoryObservation Shu, Adams & Lizano 1987

7. Molecular or Dark Clouds "Cores" and Outflows Star Formation 101: A “Natural” Framework Jets and Disks Extrasolar System 1 pc

8. On the way to Star Formation 201 Ten Years Ago, this picture was OK…but now I know that: Structures in a turbulent, self-gravitating, flow are highly transient Outflows are episodic Young stars can move rapidly Energetically significant spherical outflows (e.g. SNe, winds) are common in star- forming regions

9. How do I know “that”? Optical imaging Near-infrared imaging Thermal dust imaging Molecular spectral-line mapping MHD Simulations

10. Spectral Line Mapping  Velocity No loss of information Loss of 1 dimension

11. Star Forming Regions as Turbulent Flows: MHD Simulations Stone, Gammie & Ostriker 1999 Driven Turbulence; M  K; no gravity Colors: log density Computational volume: 256 3 Dark blue lines: B-field Red : isosurface of passive contaminant after saturation  =0.01  =1  T /10 K  n H 2 /100 cm -3  B /1.4  G  2

12. Simulated map, based on work of Padoan, Nordlund, Juvela, et al. Excerpt from realization used in Padoan, Goodman &Juvela 20023 Characterizing Spectral Line Maps of Observed & Simulated “Turbulent “Flows The Spectral Correlation Function (SCF) See also PCA analysis (Heyer et al.) & many other methods

13. “Equipartition” Models Summary Results from SCF Analysis Falloff of Correlation with Scale Magnitude of Spectral Correlation at 1 pc Padoan, Goodman & Juvela 2003 “Reality” Scaled “Superalfvenic” Models “Stochastic” Models

14. Do existing turbulence simulations “match” molecular clouds? 13 CO maps Super-Alfvénic MHD Simulations Falloff of Spectral Correlation with Scale Magnitude of Spectral Correlation at 1 pc Padoan, Goodman & Juvela 2003

15. 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

16. On the way to Star Formation 201 Structures in a turbulent, self-gravitating, flows are highly transient Outflows are episodic Young stars can move rapidly Energetically significant spherical outflows (e.g. SNe, winds) are common in star-forming regions

17. Episodic Outflows, from Moving Sources 10 -5 10 -4 10 -3 10 -2 10 10 0 Mass [M sun ] 0.1 234567 8 1 2 3 4 5678 10 2 Velocity [km s -1 ] Power-law Slope of Sum = -2.7 (arbitrarily >2) Slope of Each Outburst = -2 as in Matzner & McKee 2000 Episodicity changes Energy/Momentum Deposition (time) (Some) Young stars may zoom through ISM

18. L1448 Bachiller et al. 1990 B5 Yu Billawala & Bally 1999 Lada & Fich 1996 Bachiller, Tafalla & Cernicharo 1994 Position-Velocity Diagrams show YSO Outflows are Highly Episodic

19. Outflow Episodes:Position-Velocity Diagrams Figure from Arce & Goodman 200az1a HH300 NGC2264

20. 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

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

22. 1 pc “Giant” Herbig- Haro Flow from PV Ceph Image from Reipurth, Bally & Devine 1997

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

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

25. “Plasmon” Model of PV Ceph 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

26. “Plasmon” Model of PV Ceph Goodman & Arce 2002 For an HH object at 1 pc from source, dynamical time calculation overestimates age by factor of ten.

27. “Giant” Outflows, c. 2002 See references in H. Arce’s Thesis 2001

28. 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)

29. On the way to Star Formation 201 Structures in a turbulent, self-gravitating, flows are highly transient Outflows are episodic Young stars can move rapidly Energetically significant spherical outflows (e.g. SNe, winds) are common in star-forming regions Preview Now, More Later!

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

31. COMPLETE Preview: Great Bubble in Perseus

32. Does fecundity = demise? Bipolar outflows from young stars + Stellar Winds (& photons) from older stars + Large Explosions (SNe, GRBs) All have the power both to create & destroy

33. NatureNurture Shu, Adams & Lizano 1987

34. Star Formation 201 “Nurture”

36. CorporationsEnvironmentalists Shu, Adams & Lizano 1987

37. Environmental Impact Statement 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”?

38. What’s the right “environmentalist” approach? Gather a sample where you can statistically understand: Observing Biases Temporal Behavior Regional Variations

39. The Environmentalist’s Toolkit Optical imaging Extinction, reddening  dust grain sizes, dust column density distribution Shocked gas (e.g. HH jets) Near-infrared imaging Same as optical, plus reveals deeply “embedded” young sources (+ disks) X-ray Imaging and Spectroscopy Reveals “embedded” sources & identifies sources of bipolar & spherical outflows Thermal dust imaging Cold dust “glows” at far-IR and sub-mm wavelengths  dust grain sizes, dust temperature, plus disk characteristics Molecular and atomic spectral-line mapping Gives gas density, temperature & velocity distribution MHD Simulations

40. 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

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

42. The Value 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

43. COMPLETE, Part 1 Observations: 2003-- Mid- and Far-IR SIRTF Legacy Observations: dust temperature and column density maps ~5 degrees mapped with ~15" resolution (at 70  m) 2002-- NICER/2MASS Extinction Mapping: dust column density maps ~5 degrees mapped with ~5' resolution 2003-- SCUBA Observations: dust column density maps, finds all "cold" source ~20" resolution on all A V >2” 2002-- 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

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

45. Smoke Signals: COMPLET E’s 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

46. Perseus in (Coldish) Molecular Gas

47. 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

48. Perseus in (Warmish) Dust 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

49. COMPLET E Perseus IRAS + FCRAO (73,000 13 CO Spectra, see Scott Schnee!)

50. 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)

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

52. Polarization

53. 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

54. On the way to Star Formation 201 Structures in a turbulent, self-gravitating, flows are highly transient Outflows are episodic Young stars can move rapidly Energetically significant spherical outflows (e.g. SNe, winds) are common in star-forming regions

55. “COMPLETE” Star Formation c. 2005 Statistical Evaluation of Outflows’ Role Evaluation of Constructive/Destructive Role of Explosions/Winds Tracking down progeny (includes USNO-B work)

56. 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)

57. Extra Slides

58. COMPLETE: JCMT/SCUBA >10 mag A V 2 4 6 8 Perseus Ophiuchus 10 pc Johnstone, Goodman & the COMPLETE team, SCUBA 2003(?!) ~100 hours at SCUBA

59. “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

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

61. Just how fast is PV Ceph going?

62. 1.5 1.0 0.5 0.0 -0.5 Intensity 400350300250200150100 "Velocity" Observed Spectrum Telescope  Spectrometer All thanks to Doppler Velocity from Spectroscopy

63. Radio Spectral-line Observations of Interstellar Clouds

64. Alves, Lada & Lada 1999 Radio Spectral-Line Survey Radio Spectral-line Observations of Interstellar Clouds

65. Molecular or Dark Clouds "Cores" and Outflows Star Formation 101 Jets and Disks Extrasolar System 1 pc

66. Molecular or Dark Clouds "Cores" and Outflows Star Formation 101 Jets and Disks Extrasolar System 1 pc

67. Cores: Islands of Calm in a Turbulent Sea? "Rolling Waves" by KanO Tsunenobu © The Idemitsu Museum of Arts.

68. Islands of Calm in a Turbulent Sea Goodman, Barranco, Wilner & Heyer 1998

69. Islands (a.k.a. Dense Cores) Berkeley Astrophysical Fluid Dynamics Group http://astron.berkeley.edu/~cmckee/bafd/results.html Barranco & Goodman 1998 AMR Simulation Simulated NH 3 Map

70. Goodman, Barranco, Wilner & Heyer 1998 Observed ‘Starting’ Cores: 0.1 pc Islands of (Relative) Calm 2 3 4 5 6 7 8 9 1  v [km s ] 3456789 1 2 T A [K] TMC-1C, OH 1667 MHz  v=(0.67±0.02)T A -0.6±0.1 2 3 4 5 6 7 8 9 1  v intrinsic [km s ] 6789 0.1 23456789 1 T A [K] TMC-1C, NH 3 (1, 1)  v intrinsic =(0.25±0.02)T A -0.10±0.05 “Coherent Core”“Dark Cloud” Size Scale Velocity Dispersion

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

72. Molecular or Dark Clouds "Cores" and Outflows Star Formation 101 Jets and Disks Extrasolar System 1 pc

73. …and the famous “1RXS J162554.5-233037” is right in the Middle !? 2 pc