a (more) dynamic view of star formation alyssa a. goodman harvard-smithsonian center for...
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A (More) Dynamic View of A (More) Dynamic View of Star FormationStar Formation
Alyssa A. GoodmanAlyssa A. GoodmanHarvard-Smithsonian Center for AstrophysicsHarvard-Smithsonian Center for Astrophysics
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Physicist’s Glossaryfor Alyssa Goodman’s Talk at Rochester, 10/15/03
1 parsec = 1 pc = 3 x 1018 cm ≈ 3 light years = typical size scale for a “dark cloud”
1 solar mass = 2 x 1033 gage of the Sun (and ~the Earth) ~3 x 109 yrage of the Universe ~15 x 109 yr“extinction” = absorption+scattering (measure of how many photons
are “missing”)“molecular cloud” = condensation of molecular hydrogen (H2) in the
interstellar medium (typically colder & denser than surroundings)“H II region” blob of ionized hydrogen (free protons & electrons, a.k.a.
H II) surrounding hot young starCOMPLETE = COordinated Molecular Probe Line Extinction Thermal
Emission Survey (begun 2001)IRAS = Infrared Astronomy Satellite (1983)SIRTF = Space Infrared Telescope Facility (launched 8/03)
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“Speeding Young Stars”
• The quasi-static theory of star formation
• What stays still long enough for that? – not PV Ceph!
• Dynamic Star Formation • How can we measure it (COMPLETE)• What might it mean?
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Molecular or Dark Clouds
"Cores" and Outflows
Star Formation
Jets and Disks
Extrasolar System
3 lig
ht y
ears
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Molecular or Dark Clouds
"Cores" and Outflows
Quasi-Static
Jets and Disks
Extrasolar System
3 lig
ht y
ears
Core formation time >> 1 Myr
Outflow is steady, and lasts >>0.1 Myr
Accretion onto disk lasts~same time as flow (>>0.1 Myr)
Planet formation time ~1 Myr
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TheoryObservatio
n
Shu, Adams & Lizano 1987
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“Quiet” Taurus
E.E
. B
arna
rd,
5.5
hour
exp
osur
e at
Yer
kes
Obs
erva
tory
, 19
07
Jan
. 9
Next slide shows near-IR 1000x zoom on blobs like these
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Hubble Space Telescope Near-IR Images of Disks/Jets(c. 1998)
QuickTime™ and aTIFF (Uncompressed) decompressorare needed to see this picture.
DG Tau B
QuickTime™ and aTIFF (Uncompressed) decompressorare needed to see this picture.
IRAS 04302+2247
QuickTime™ and aTIFF (Uncompressed) decompressorare needed to see this picture.
Haro 6-5B
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Barnard’s TaurusColor shows far-IR Dust Emission from IRAS
E.E
. B
arn
ard
~5.5
. hou
r exp
osu
re a
t Yerk
es
Obse
rvato
ry,
c. 1
90
7
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Barnard’s TaurusColor shows far-IR Dust Emission from IRAS
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How do we see this move?
Red Plate, Digitized Palomar Observatory Sky Survey
The Oschin telescope, 48-inch aperture wide-field Schmidt camera
at Palomar
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Measuring Motions: Molecular Line Maps Spectral Line Observations
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Velocity from Spectroscopy
1.5
1.0
0.5
0.0
-0.5
Inte
nsit
y
400350300250200150100
"Velocity"
Observed Spectrum
All thanks to Doppler
Telescope Spectrometer
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Watching the Gas Move: Spectral Line Mapping
Data cubes are in position-position-velocity-intensity space– Very hard to visualize
Measurable with spectral line mapping– centroid velocity – line width (velocity dispersion)– rotation– infall– outflow– higher-order statistical properties of the flow (e.g. SCF)
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Simulated spectral-line map, based on work of Padoan, Nordlund, Juvela, et al.Excerpt from realization used in Padoan, Goodman &Juvela 2003
“Spectral-Line Map”
color in background shows “integrated”
intensity
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Alves, Lada & Lada 1999
Radio Spectral-Line Survey
Integrated Intensity Does not Show Velocity Information
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Watching the Gas Move: Spectral Line Mapping
Data cubes are in position-position-velocity-intensity space– Very hard to visualize
Measurable with spectral line mapping– centroid velocity – line width (velocity dispersion)– rotation– infall– outflow– higher-order statistical properties of the flow (e.g. SCF)
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The Taurus Dark Cloud Complex
Mizuno et al. 1995 13CO(1-0) integrated intensity map from Nagoya 4-mYoung star positions courtesy L. Hartmann
Size of wholemap shown in
next slide
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“Coherent Dense Cores”Islands of Calm in a Turbulent Sea
Goodman, Barranco, Wilner & Heyer 1998
Size of wholemap shown in
next slide
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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
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Goodman, Barranco, Wilner & Heyer 1998
Coherent 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
Notice typical velocity disperson on pc scales
is ~1 km s-1
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Order from Chaos
Order; N~R0.9
~0.1 pc(in Taurus)
Chaos; N~R0.1
Goodman et al. 1998
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Stars Form in Islands of Calm in a Turbulent Sea
"Rolling Waves" by KanO Tsunenobu © The Idemitsu Museum of Arts.
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Molecular or Dark Clouds
"Cores" and Outflows
Star Formation
Jets and Disks
Extrasolar System
3 lig
ht y
ears
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Young Stellar Outflows in General
and PV Ceph in particular
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Spectral Line Outflow Mapping
Usually…
In Extreme Cases… 1.0
0.8
0.6
0.4
0.2
0.0 120100806040200
1.0
0.8
0.6
0.4
0.2
0.0120100806040200 12010080604020 0
1.0
0.8
0.6
0.4
0.2
0.0120100806040200
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(All the) Maps of “Giant” Outflows, c. 2002
See references in H. Arce’s Thesis 2001
Greyscale shows ambient 1000 ptcl/cc gas
Red shows 100 ptcl/cc gas moving away from us
Blue shows 100 ptcl/cc gas moving toward us
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(All the) Maps of “Giant” Outflows, c. 2002
See references in H. Arce’s Thesis 2001
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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
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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The Usual Questions About Outflows
• How, exactly, do they carry away angular momentum from the forming star?
• Can they “drive” turbulence in star-forming regions?
• How are “optical” HH flows & molecular outflows related?
• How long do they last?• How many are there, really?
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Today’s Question
What can outflows tell us about the motion of a star relative to its environment?
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1 pc
“Giant” Herbig-
Haro Flow from
PV Ceph
Image from Reipurth, Bally & Devine 1997
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PV Ceph
Episodic ejections from a
precessing or wobbling
moving moving source
Goodman & Arce 2003
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PV Ceph is moving at ~20 km s-1
Goodman & Arce 2003
1 pc
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The “Plasmon” Model for Deceleration
Assumes each jet burst begins at 350 km s-1
Precession is neglected, so model executed in v*-vjet plane
Goodman & Arce 2003
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The Most Subtle
Evidence for PV Ceph’s Motion
Goodman & Arce 2003
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Deceleration Means
Outflows Lie About their
Age
Goodman & Arce 2003
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Backtracking
Goodman & Arce 2003
1 pc
?
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Ejected?!!
gap
DSS Image of NGC 7023
100 m IRAS Image of NGC 7023-PV Ceph Region
Goodman & Arce 2003
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How Much Gas Could Be Pulled Along for the Ride?
108
109
1010
1011
1012
GM*
/RBH
= σeff
2
[cm2 s-2]
0.0012 3 4 5 6 7 8 9
0.012 3 4 5 6 7 8 9
0.1RBH [ ]pc
5 6 7 8 91
2 3 4 5 6 7 8 910
2 3 4
RBH [ 500 ]arcsec at pc
10
50 MSun
5
σeff
2=(1 km s-1 )2
20
2 1 M Sun
- Effective Bondi Hoyle 7 Radius for MSun in
σeff=5 km s-1 Gas
σeff
2=(5 km s-1 )2
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How often does this happen?
Direct Proper Motion– RW Aur 16 km s-1, Jones & Herbig 1979
– BN object w.r.t. “I” 50 km s-1, Plambeck et al. 1995
– IRAS 16293-2422 30 km s-1, Loinard 2002
– T-Tau Sb 20 km s-1, Loinard et al. 2003
Deduced from Outflow Morphology– B5 IRS1~10 km s-1, Bally et al. 1996*
– PV Ceph 20 km s-1, Goodman & Arce 2003
*but the possibility of motion was dismissed!
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Dynamic Star
Formation
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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“Early” Times
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“Later” Times
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How to measure dynamic star formation?
Time is a key dimension but spatial statistics remain our best hope to
understand it.
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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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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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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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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)
Jonathan Foster (CfA, PhD student)Mark Heyer (UMASS/FCRAO)
Di Li (CfA)Doug Johnstone (HIA, Canada)
Naomi Ridge (CfA)Scott Schnee (CfA, PhD student)
Mario Tafalla (OAS, Spain)Tom Wilson (MPIfR)
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COMPLETE Perseus
IRAS + FCRAO
(73,000 13CO Spectra)
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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)
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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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A (More) Dynamic View of A (More) Dynamic View of Star FormationStar Formation
Alyssa A. GoodmanAlyssa A. GoodmanHarvard-Smithsonian Center for AstrophysicsHarvard-Smithsonian Center for Astrophysics