the complete survey of star-forming regions: nature vs. nurture alyssa a. goodman...

The COMPLETE Survey of Star-Forming Regions: Nature vs. Nurture

Alyssa A. GoodmanHarvard-Smithsonian Center for Astrophysics

cfa-www.harvard.edu/~agoodman

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)

Nature Nurture

Shu, Adams & Lizano 1987

CorporationsEnvironmentalist

s

Shu, Adams & Lizano 1987

TheoryObservatio

n

Shu, Adams & Lizano 1987

Molecular or Dark Clouds

"Cores" and Outflows

Star Formation 101: A “Natural” Framework

Jets and Disks

Extrasolar System

1 p

c

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 transientOutflows are episodicYoung stars can move rapidlyEnergetically significant spherical

outflows (e.g. SNe, winds) are common in star-forming regions

How do I know “that”?

Optical imagingNear-infrared imaging Thermal dust imaging

Molecular spectral-line mapping

MHD Simulations

Spectral Line MappingVelocitySpectral Line Observations

Mountain RangeNo loss ofinformatio

n

Loss of1 dimension

Star Forming Regions as Turbulent Flows: MHD Simulations

Stone, Gammie & Ostriker 1999•Driven Turbulence; M K; no gravity•Colors: log density•Computational volume: 2563

•Dark blue lines: B-field•Red : isosurface of passive contaminant after saturation

=0.01 =1

T / 10 K

nH 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 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

“Equipartition”Models

Summary Results from SCF Analysis

Fallo

ff o

f C

orr

ela

tion

wit

h S

cale

Magnitude of Spectral Correlation at 1 pc

Padoan, Goodman

& Juvela 2003

“Reality”

Scaled “Superalfvenic”Models

“Stochastic”Models

Do existing turbulence simulations “match” molecular clouds?

13CO maps Super-Alfvénic MHD Simulations

Fallo

ff o

f Sp

ect

ral C

orr

ela

tion

wit

h S

cale

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 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.

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

10-5

10-4

10-3

10-2

10-1

100

Mass

[M

sun]

0.12 3 4 5 6 7 8

12 3 4 5 6 7 8

102

Velocity [km s-1]

Power-law Slope of Sum = -2.7(arbitrarily >2)

Slope of Each Outburst = -2as in Matzner & McKee 2000

Episodicity changes Energy/Momentum Deposition (time)

(Some) Young stars may zoom through ISM

L1448

Bach

iller

et

al. 1

990

B5

Yu B

illaw

ala

& B

ally

199

9

Lada &

Fic

h 1

99

6

Bach

iller,

Tafa

lla &

Cern

icharo

19

94

Position-Velocity Diagrams

show YSO Outflows are Highly Episodic

Outflow Episodes:Position-Velocity Diagrams

Figure

fro

m A

rce &

Goodm

an 2

00

az1

a

HH300

NGC2264

10-5

10-4

10-3

10-2

10-1

100

Mass

[M

sun]

0.12 3 4 5 6 7 8

12 3 4 5 6 7 8

102

Velocity [km s-1]

Episodic Outflows: Steep Mass-Velocity Slopes Result from Summed

Bursts

Power-law Slope of Sum = -2.7(arbitrarily >2)

Slope of Each Outburst = -2as 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

PV Ceph

Episodic ejections from a

precessing or wobbling

moving moving source

Goodman & Arce 2003

PV Ceph is moving at ~10 km s-1

Goodman & Arce 2003

“Plasmon” Model of PV Ceph4x1018

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

“Plasmon” Model of PV Ceph4x1018

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 2002

For an HH object at 1 pc from source, dynamical time calculation overestimates age by factor of ten.

“Giant” Outflows, c. 2002

See references in H. Arce’s Thesis 2001

The action of multiple outflows in NGC 1333?

SCUBA 850 mm Image shows Ndust (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

regionsPreview Now, More Later!

COMPLETE Preview:Discovery of a Heated Dust Ring in

Ophiuchus

Goodman, Li & Schnee 2003

2 pc

COMPLETE Preview: Great

Bubble in Perseus

QuickTime™ and aTIFF (LZW) decompressorare needed to see this picture.

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

Nature Nurture

Shu, Adams & Lizano 1987

Star Formation 201 “Nurture”

Star Formation 201“Nurture”

CorporationsEnvironmentalist

s

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

distributionShocked 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 wavelengthsdust grain

sizes, dust temperature, plus disk characteristics

Molecular and atomic spectral-line mapping Gives gas density, temperature & velocity distribution

MHD Simulations

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

COMPLETEThe COordinated Molecular Probe Line Extinction Thermal Emission Survey}

The Value 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

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 AV>2”

2002-- 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

Is this Really Possible Now?

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 then

1 minute for a 13CO map now

Smoke Signals:

COMPLETE’s 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

Perseus in (Coldish) Molecular

Gas

QuickTime™ and aTIFF (Uncompressed) decompressorare 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

Perseus in (Warmish)

Dust 2 x 1051 erg SN

into 104 cm-3

5 pc in 1 MyrT=30K

vexp=1.5 km s-1

QuickTime™ and aTIFF (LZW) decompressorare needed to see this picture.

COMPLETE Perseus

IRAS + FCRAO

(73,000 13CO Spectra, see Scott

Schnee!)

Perseus

QuickTime™ and aTIFF (LZW) decompressorare needed to see this picture.QuickTime™ and aTIFF (LZW) decompressorare needed to see this picture.

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

QuickTime™ and aTIFF (LZW) decompressorare needed to see this picture.QuickTime™ and aTIFF (LZW) decompressorare needed to see this picture.+ =

Column Density Temperatur

e

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

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. 2005

Statistical Evaluation of Outflows’ RoleEvaluation 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/FCRAOCfA)Scott Schnee (CfA, PhD student)

Mario Tafalla (OAS, Spain)Tom Wilson (MPIfR)

Extra Slides

COMPLETE: JCMT/SCUBA>10 mag AV

2468

Perseus

Ophiuchus

10 pc

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?

-3

-8

-4

-8M

ass

/Velo

city

Velocity

How much gas will be pulled along for the ride?

Goodman & Arce 2002

Just how fast is PV

Ceph going?

1.5

1.0

0.5

0.0

-0.5

Inte

nsit

y

400350300250200150100

"Velocity"

Observed Spectrum

Telescope Spectrometer

All thanks to Doppler

Velocity from Spectroscopy

Radio Spectral-line Observations of Interstellar Clouds Spectral Line Observations

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 p

c

Molecular or Dark Clouds

"Cores" and Outflows

Star Formation 101

Jets and Disks

Extrasolar System

1 p

c

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 Grouphttp://astron.berkeley.edu/~cmckee/bafd/results.html Barranco & Goodman 1998

AMR Simulation

Simulated NH3 Map

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-1

]

3 4 5 6 7 8 91

2

TA [K]

TMC-1C, OH 1667 MHz

v=(0.67±0.02)TA-0.6±0.1

2

3

4

5

6

7

8

9

1

v

intr

insi

c[k

m s

-1]

6 7 8 90.1

2 3 4 5 6 7 8 91

TA [K]

TMC-1C, NH3 (1, 1)

vintrinsic=(0.25±0.02)T A-0.10±0.05

“Coherent Core”“Dark Cloud”

Size Scale

Velo

city

Dis

pers

ion

Cores = Order from Chaos

Order; N~R0.9

~0.1 pc(in Taurus)

Chaos; N~R0.1

Molecular or Dark Clouds

"Cores" and Outflows

Star Formation 101

Jets and Disks

Extrasolar System

1 p

c

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

2 pc