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The COMPLETE Survey of Star-Forming Regions at Age 2
Alyssa A. GoodmanHarvard-Smithsonian Center for Astrophysicscfa-www.harvard.edu/~agoodman
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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
The COordinated Molecular Probe Line Extinction Thermal Emission Survey
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COMPLETE’s Birthplace:The 2001 Santa Cruz
Star Formation Workshop
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The Lesson of Coordination: B68
C18ODust EmissionOptical 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 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
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2MASS/NICER Extinction Map of Orion
Un(coordinated) Molecular-Probe Line,
Extinction and Thermal Emission Observations
5:41:0040 20 40 42:00
2:00
55
50
05
10
15
20
25
30
R.A. (2000)
1 pc
SCUBA
5:40:003041:003042:00
2:00
1:50
10
20
30
40
R.A. (2000)
1 pc
SCUBA
Molecular Line Map
Nagahama et al. 1998 13CO (1-0) Survey
Lombardi & Alves 2001Johnstone et al. 2001 Johnstone et al. 2001
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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
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Time is a key dimensionbut
spatial statistics remain our best hope to understand it.
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Could we really…?
10-4
10-3
10-2
10-1
100
101
102
103
Time (hours)
20152010200520001995199019851980
Year
1 Hour
1 Minute
1 Day
1 Second
1 Week
SCUBA-2
SEQUOIA+
NICER/8-m
NICER/SIRTFNICER/2MASS
AV~5 mag, Resolution~1'
AV~30 mag, Resolution~10"
13CO 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 for a 13CO map when
the 3 wise men were 40
1 minute for the same
13CO map today
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COMPLETEThe COordinated Molecular Probe Line Extinction Thermal Emission Survey
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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 AV>2”
2002-4-- FCRAO/SEQUOIA 13CO and 13CO Observations: gas temperature, density and velocity information ~40" resolution on all AV>1
Science:– 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 & 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
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COMPLETE, 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 N2H+ Observations: gas temperature, density and velocity information for "cores” ~15" resolution
Science:Multiplicity/fragmentation studies
Detailed modeling of pressure structure on <0.3 pc scalesSearches for the "loss" of turbulent energy (coherence)
FCRAO N2H+ map with CS spectra superimposed.
(Le
e,
Mye
rs &
Ta
falla
20
01
).
<arcminute-scale core maps to get density & velocity structure all the way from >10 pc
to 0.01 pc
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Time Dependences we did not worry about when David, Chris & Frank were
501. Structures in a turbulent, self-
gravitating, flow are highly transient2. Outflows are episodic3. Young stars can move rapidly4. Energetically significant spherical
outflows (e.g. SNe, winds) are common in star-forming regions
5. (Aging)
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1. Structures are Highly Transient
Bate, Bonnell & Bromm 2002
•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 •movie=1.4 free-fall times
QuickTime™ and aCinepak decompressorare needed to see this picture.
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L1448
Bach
iller
et
al. 1
990
B5
Yu, B
illaw
ala
& B
ally
1999
Lada &
Fic
h 1
99
6
Bach
iller,
Tafa
lla &
Cern
icharo
19
94
2. YSO Outflows are Highly Episodic
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Outflow Episodes:Position-Velocity Diagrams
Figure
fro
m A
rce &
Goodm
an 2
00
1
HH300
NGC2264
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3. Powering source of (some) outflows may zoom through ISM
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PV Ceph is moving at ~10 km s-1
Goodman & Arce 2003
1 pc
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Moving Source & Slowing Knots4x1018
3
2
1
0
y knot positions (cm)
-4x1017
-2 0
x knot posns. w.r.t. star "now" (cm)
500x1015
400
300
200
100
0
Dis
tance
alo
ng x
-dir
ect
ion (
cm)
15x103
1050
Elapsed Time since Burst (Years)
70
60
50
40
30
20
10
0
Sta
r-Knot D
iffere
nce
/Sta
r Off
set (P
erce
nt)Knot
Star
Star-KnotDifference
Star-KnotDifference
(%)
Initial jet 250 km s-1; star motion
10 km s-1
Goodman & Arce 2003
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Dynamical Time Estimates off by x104x10
18
3
2
1
0
y knot positions (cm)
-4x1017
-2 0
x knot posns. w.r.t. star "now" (cm)
1
2
3
4
5
6
7
8
9
10
"Dynamical Time"/Elapsed Time
3.0x1018
2.52.01.51.00.50.0
Distance of Knot from Source (cm)
Goodman & Arce 2003
For an HH object at 1 pc from source,
dynamical time calculation overestimates age by factor of
~ten.
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(All the) Maps of “Giant” Outflows, c. 2002
See references in H. Arce’s Thesis 2001
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Time Dependences we did not worry about when David, Chris & Frank were
401. Structures in a turbulent, self-
gravitating, flow are highly transient2. Outflows are episodic3. Young stars can move rapidly4. Energetically significant spherical
outflows (e.g. SNe, winds) are common in star-forming regions
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COMPLETE Discovery of a Heated Dust Ring in
Ophiuchus
Goodman, Li & Schnee 2003
2 pc
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Smoke Signals from Ophiuchus
0.5 x 1051 erg SNinto 105 cm-3
2 pc in 200,000 yr T=38K
vexp=1.7 km s-1
HeatedDustRing
Regionknownas
“-OphCluster”
Re-calibrated IRAS Dust Column Density Re-Calibrated IRAS Dust Temperature
ROSAT PSPC
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
Temperature Map.
ROSAT Pointed Observation
Real -OphCluster
inside newlydiscoveredheated ring
1RXS J162554.5-233037
The star-Ophand
RXJ1625.5-2326
Goodman, Gaensler, Wolk & Schnee 2003
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Ionized Gas in the Ophiuchus Smoke Shell
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H
SII
SH
ASSA
Data
court
esy
of
John G
aust
ad
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COMPLETE Warm Dust Emission
shows
Great Bubble in Perseus
2 x 1051 erg SNinto 104 cm-3
5 pc in 1 MyrT=30K
vexp=1.5 km s-1
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Perseus in (Coldish)
Molecular Gas
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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
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COMPLETE Perseus
IRAS + FCRAO
(73,000 13CO Spectra)
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Perseus
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Total Dust Column (0 to 15 mag AV) (Based on 60/100 microns)
Dust Temperature (25 to 45 K)(Based on 60/100 microns)
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Hot Source in a Warm Shell
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Column Density Temperatur
e
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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)
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JCMT/SCUBA COMPLETE>10 mag AV
2468
Perseus
Ophiuchus
10 pc
10 pc~100 hours at SCUBA
= in SCUBA archive= observed Spring ‘03
NGC1333 Map
All at >5 mag, by 2004
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My Near-Term “COMPLETE” Agenda
Statistical Evaluation of Outflows’ RoleEvaluation of Constructive/Destructive Role of
Explosions/Winds
Tracking down progeny
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“Early” Times
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“Later” Times
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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/FCRAOCfA)Scott Schnee (CfA, PhD student)
Mario Tafalla (OAS, Spain)Tom Wilson (MPIfR)
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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”?
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Extra Slides
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Nature Nurture
Shu, Adams & Lizano 1987
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CorporationsEnvironmentalist
s
Shu, Adams & Lizano 1987
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TheoryObservatio
n
Shu, Adams & Lizano 1987
Some
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“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
-8M
ass
/Velo
city
Velocity
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How much gas will be pulled along for the ride?
Goodman & Arce 2002
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Perseus in (Coldish) Molecular
Gas
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Cores = Order from Chaos
Order; N~R0.9
~0.1 pc(in Taurus)
Chaos; N~R0.1