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The COMPLETE Survey of Star-Forming Regions at Age 2 Alyssa A. Goodman Harvard-Smithsonian Center for Astrophysics cfa-www.harvard.edu/~agoodman The COordinated Molecular Probe Line Extinction Thermal Emission Survey COMPLETE 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/FCRAOCfA) Scott Schnee (CfA, PhD student) Mario Tafalla (OAS, Spain) Tom Wilson (MPIfR) COMPLETE’s Birthplace: The 2001 Santa Cruz Star Formation Workshop The Lesson of Coordination: B68 Optical Image Dust Emission C18O 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 C18O 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 NICER Extinction Map Radial Density Profile, with Critical Bonnor-Ebert Sphere Fit Nagahama et al. 1998 13CO (1-0) Survey Un(coordinated) MolecularProbe Line, Extinction and Thermal Emission Observations Molecular Line Map 2MASS/NICER Extinction Map of Orion 1:50 50 1 pc 55 2:00 2:00 05 10 10 20 15 1 pc 20 30 25 SCUBA 30 40 5:41:00 20 40 R.A. (2000) 40 42:00 SCUBA 42:00 Johnstone et al. 2001 Lombardi & Alves 2001 30 41:00 R.A. (2000) 30 Johnstone et al. 2001 5:40:00 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 Time is a key dimension but spatial statistics remain our best hope to understand it. Could we really…? 10 10 Time (hours) 10 10 3 1 day for a map when the 3 wise men were 40 A V~5 mag, Resolution~1' 13CO 2 A V~30 mag, Resolution~10" 13 CO Spectra for 32 Positions in a Dark Cloud (S/N~3) Sub-mm Map of a Dense Core at 450 and 850 m 1 Day 1 0 1 Hour NICER/8-m 10 1 Week -1 1 Minute SEQUOIA+ 10 10 -2 1 minute for the same 13CO map today -3 SCUBA-2 1 Second 10 NICER/2MASS -4 1980 1985 1990 1995 NICER/SIRTF 2000 Year 2005 2010 2015 The COMPLETE COordinate d Molecular Probe Line Extinction Thermal Emission Survey COMPLETE, Part 1 Observations: 5 degrees (~tens of pc) SIRTF Legacy Coverage of Perseus 2003-4-- Mid- and Far-IR SIRTF Legacy Observations: point-source census, >10-degree scale Near-IR Extinction, Molecular Line and Dust Emission Science: Surveys of Perseus, Ophiuchus & Serpens, <1 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 AV>2” 2002-4-- FCRAO/SEQUOIA 13CO and 13CO Observations: gas temperature, density and velocity information ~40" resolution on all AV>1 –Combined Thermal Emission data: dust spectral-energy distributions, giving emissivity, Tdust and Ndust –Extinction/Thermal Emission inter-comparison: unprecedented constraints on dust properties and cloud distances, in addition to high-dynamic range Ndust map –Spectral-line/Ndust Comparisons Systematic censes of inflow, outflow & (Lee, Myers & Tafalla 2001). COMPLE TE, Part 2 (2003-5) FCRAO N2H+ map with CS spectra superimposed. Observations, using target list generated from Part 1: <arcminute-scale core maps to get density & Science: velocity structure all the way from >10 pc to 0.01 pc NICER/8-m/IR camera Observations: best density profiles for dust associated with "cores". ~10" resolution FCRAO + IRAM N2H+ Observations: gas temperature, density and velocity information for "cores” ~15" resolution Multiplicity/fragmentation studies Detailed modeling of pressure structure on <0.3 pc scales Searches for the "loss" of turbulent energy (coherence) 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) 1. Structures are Highly Transient •MHD turbulence gives “t=0” conditions; Jeans mass=1 Msun •50 Msun, 0.38 pc, navg=3 x 105 ptcls/cc •forms ~50 objects •T=10 K •SPH, no B or L, G •movie=1.4 free-fall times Bate, Bonnell & Bromm 2002 QuickTime™ and a Cinepak decompressor are needed to see this picture. B5 Yu, Billawala & Bally 1999 Bachiller et al. 1990 L1448 Lada & Fich 1996 Bachiller, Tafalla & Cernicharo 1994 2. YSO Outflows are Highly Episodic Outflow Episodes:Position-Velocity Diagrams NGC2264 Figure from Arce & Goodman 2001 HH300 3. Powering source of (some) outflows may zoom through ISM PV Ceph is moving at ~10 km s-1 1 pc Goodman & Arce 2003 4x 10 Moving Source & Slowing Knots 18 500x10 70 15 60 Star Distance along x-direction (cm) y k not positions (cm) 400 2 Star-Knot Difference (%) 50 300 Star-Knot Difference 40 30 200 1 Star-Knot Difference/Star Offset (Percent) 3 20 Knot 100 Initial jet 250 km s1; star motion 10 km s-1 0 -4x 10 17 -2 10 0 0 5 10 15x10 3 0 0 x k not posns. w.r.t. star "now" (c m) Elapsed Time since Burst (Years) Goodman & Arce 2003 4x 10 Dynamical Time Estimates off by x10 18 10 9 8 3 "Dynamical Time"/Elapsed Time y k not positions (cm) 7 2 6 5 For an HH object at 1 pc from source, dynamical time calculation overestimates age by factor of ~ten. 4 3 2 1 1 0.0 0.5 1.0 1.5 2.0 2.5 3.0x10 18 Distance of Knot from Source (cm) 0 -4x 10 17 -2 0 x k not posns. w.r.t. star "now" (c m) Goodman & Arce 2003 (All the) Maps of “Giant” Outflows, c. 2002 See references in H. Arce’s Thesis 2001 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 COMPLETE Discovery of a Heated Dust Ring in Ophiuchus 2 pc Goodman, Li & Schnee 200 Re-calibrated IRAS Dust Column Density Re-Calibrated IRAS Dust Temperature Heated Dust Ring Smoke Signals from Ophiuchus 0.5 x 1051 erg SN into 105 cm-3 2 pc in 200,000 yr T=38K vexp=1.7 km s-1 ROSAT PSPC The star r-Oph and RXJ1625.52326 Region known as “r-Oph Cluster” Goodman, Gaensler, Wolk & Schnee 2003 ROSAT Pointed Observation Real r-Oph Cluster inside newly discovered heated ring 1RXS J162554.5-233037 In each panel where it is sho n, the white ring shows a 2 pc circle, corresponding to the size and shape of the heated ring apparent in the IRAS Ionized Gas in the Ophiuchus Smoke Shell Quick Time™ and a TIFF (LZW) decompressor are needed to see this picture. QuickTime™ and a TIFF (LZW) decompressor are needed to see this picture. SII QuickTime™ and a TIFF (L ZW) decompre ssor are n eed ed to se e th is p icture. SHASSA Data courtesy of John Gaustad Ha COMPLETE Warm Dust Emission shows Great Bubble in Perseus 2 x 1051 erg SN into 104 cm-3 5 pc in 1 Myr T=30K vexp=1.5 km s-1 Perseus in (Coldish) Molecular Gas QuickTime™ and a TIFF (Uncompressed) decompressor are needed to see this picture. Map of 1200 13CO 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 COMPLET E Perseus IRAS + FCRAO (73,000 13CO Spectra) Perseus Total Dust Column (0 to 15 mag AV) (Based on 60/100 microns) Dust Temperature (25 to 45 K) (Based on 60/100 microns) QuickTime™ and a TIFF (LZW) decompressor are needed to see this picture. QuickTime™ and a TIFF (LZW) decompressor are needed to see this picture. Hot Source in a Warm Shell Column Density Temperature + QuickTime™ and TIFF (LZW) decompressor are needed to see this picture. QuickTime™ and a TIFF (LZW) decompressor are needed toasee this picture. = The action of multiple bipolar outflows in NGC 1333? SCUBA 850 mm Image shows Ndust (Sandell & Knee 2001) Dotted lines show CO outflow orientations (Knee & Sandell 2000) >10 mag AV 8 6 4 2 JCMT/SCUBA COMPLETE ~100 hours at SCUBA 10 pc 10 pc NGC1333 Map Ophiuchus = in SCUBA archive = observed Spring ‘03 Perseus All at >5 mag, by 2004 My Near-Term “COMPLETE” Agenda Statistical Evaluation of Outflows’ Role Evaluation of Constructive/Destructive Role of Explosions/Winds Tracking down progeny “Early” Times “Later” Times The COordinated Molecular Probe Line Extinction Thermal Emission Survey COMPLETE 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/FCRAOCfA) Scott Schnee (CfA, PhD student) Mario Tafalla (OAS, Spain) Tom Wilson (MPIfR) 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? • What is the time-history of star production in a “cloud”? Are all the stars formed still “there”? (Big cloud--“Starless” Core--Outflow--Planet Formation--Clearing) Extra Slides Nature Shu, Adams & Lizano 1987 Nurture Corporations Shu, Adams & Lizano 1987 Environmentalists Theory Shu, Adams & Lizano 1987 Observation • Slope steepens when t corrections made – Previously unaccounted-for mass at low velocities • Slope often (much) steeper than “canonical” -2 • Seems burstier sources have steeper slopes? Mass/Velocity “Steep” Mass-Velocity Relations -3 -8 Velocity -4 -8 HH300 (Arce & Goodman 2001a) How much gas will be pulled along for the ride? Goodman & Arce 2002 Perseus in (Coldish) Molecular Gas Cores = Order from Chaos ~0.1 pc (in Taurus) Order; N~R0.9 Chaos; N~R0.1