The COMPLETE Survey of Star-Forming Regions: Nature vs. Nurture Alyssa A. Goodman Harvard-Smithsonian Center for Astrophysics cfa-

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)

NatureNurture Shu, Adams & Lizano 1987

CorporationsEnvironmentalists Shu, Adams & Lizano 1987

TheoryObservation Shu, Adams & Lizano 1987

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

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

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

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

Star Forming Regions as Turbulent Flows: MHD Simulations Stone, Gammie & Ostriker 1999 Driven Turbulence; M  K; no gravity Colors: log density Computational volume: 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

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

“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

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

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

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

Episodic Outflows, from Moving Sources 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 Episodicity changes Energy/Momentum Deposition (time) (Some) Young stars may zoom through ISM

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

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

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

Powering source of (some) outflows may zoom through ISM

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

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

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

“Plasmon” Model of PV Ceph 500x Distance along x-direction (cm) 15x Elapsed Time since Burst (Years) 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

“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.

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

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)

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!

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

COMPLETE Preview: Great Bubble in Perseus

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

NatureNurture Shu, Adams & Lizano 1987

Star Formation 201 “Nurture”

CorporationsEnvironmentalists Shu, Adams & Lizano 1987

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”?

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

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

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

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

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

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

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

Smoke Signals: COMPLET E’s Ophiuchus 0.5 x 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 J The star  -Oph and RXJ Goodman, Gaensler, Wolk & Schnee 2003

Perseus in (Coldish) Molecular Gas

Map of 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

Perseus in (Warmish) Dust 2 x erg SN into 10 4 cm -3 5 pc in 1 Myr T=30K v exp =1.5 km s -1

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

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)

Hot Source in a Warm Shell + = Column Density Temperature

Polarization

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

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

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

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)

Extra Slides

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

“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? Mass/Velocity Velocity

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

Just how fast is PV Ceph going?

Intensity "Velocity" Observed Spectrum Telescope  Spectrometer All thanks to Doppler Velocity from Spectroscopy

Radio Spectral-line Observations of Interstellar Clouds

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

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

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

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

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

Islands (a.k.a. Dense Cores) Berkeley Astrophysical Fluid Dynamics Group Barranco & Goodman 1998 AMR Simulation Simulated NH 3 Map

Goodman, Barranco, Wilner & Heyer 1998 Observed ‘Starting’ Cores: 0.1 pc Islands of (Relative) Calm  v [km s ] T A [K] TMC-1C, OH 1667 MHz  v=(0.67±0.02)T A -0.6±  v intrinsic [km s ] 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

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

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

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