The COMPLETE Survey of Star-Forming Regions at Age 2

Alyssa A. GoodmanHarvard-Smithsonian Center for Astrophysicscfa-www.harvard.edu/~agoodman

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

COMPLETE’s Birthplace:The 2001 Santa Cruz

Star Formation Workshop

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

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

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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

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 dimensionbut

spatial statistics remain our best hope to understand it.

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

COMPLETEThe COordinated Molecular Probe Line Extinction Thermal Emission Survey

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

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

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)

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.

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

Outflow Episodes:Position-Velocity Diagrams

Figure

fro

m A

rce &

Goodm

an 2

00

1

HH300

NGC2264

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

PV Ceph is moving at ~10 km s-1

Goodman & Arce 2003

1 pc

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

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)

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3

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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.

(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

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

COMPLETE Discovery of a Heated Dust Ring in

Ophiuchus

Goodman, Li & Schnee 2003

2 pc

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

Ionized Gas in the Ophiuchus Smoke Shell

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H

SII

SH

ASSA

Data

court

esy

of

John G

aust

ad

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

COMPLETE Perseus

IRAS + FCRAO

(73,000 13CO Spectra)

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)

Hot Source in a Warm Shell

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Column Density Temperatur

e

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)

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

My Near-Term “COMPLETE” Agenda

Statistical Evaluation of Outflows’ RoleEvaluation of Constructive/Destructive Role of

Explosions/Winds

Tracking down progeny

“Early” Times

“Later” Times

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)

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”?

Extra Slides

Nature Nurture

Shu, Adams & Lizano 1987

CorporationsEnvironmentalist

s

Shu, Adams & Lizano 1987

TheoryObservatio

n

Shu, Adams & Lizano 1987

Some

“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

How much gas will be pulled along for the ride?

Goodman & Arce 2002

Perseus in (Coldish) Molecular

Gas

Cores = Order from Chaos

Order; N~R0.9

~0.1 pc(in Taurus)

Chaos; N~R0.1