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James Webb Space Telescope (JWST)
The First Light Machine
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Origins Themes TwoFundamental Questions
H w Di W H r ?
Are We Alone?
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How Did We Get Here?
Trace Our Cosmic Roots
Formation of galaxies
Formation of stars
Formation of heavy elements
Formation of planetary systems
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Are We Alone?
Search for life outside the solar system
Search for other planetary systems
Search for habitable planets
Identify remotely detectable bio-signatures
Search for smoking guns indicatingbiological activities
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Missions Supporting the Origins Goals
How Did We Get Here? Are We Alone?
Keck Interferometer
Science &
Technology
JWST
SIM
SOFIA
FUSE
TPF
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A Vision for Large Telescopes & Collectors
100-1000m diameterToward Accomplishing
... the Impossible!
20-40m diameter
~10m diameter
Life FinderStellar ImagerPlanet Ima e
diameter
HST
Operational Developmental Conceptual Unimaginable
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JWST Science Themes
Big BangBig BangFirstStarsFirstStars
GalaxiesGalaxies PlanetsPlanetsLifeLife
Galaxies EvolveGalaxies Evolve
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JWST Summary ss on ec ve
Study origin & evolution of galaxies, stars & planetary systems
Optimized for near infrared wavelength (0.6 28 m)
OrganizationMission Lead: Goddard Space Flight Center
Prime Contractor: Northrop Grumman Space Technology
Instruments:
Near Infrared Camera (NIRCam) Univ. of Arizona
Near Infrared Spectrometer (NIRSpec) ESA
Mid-Infrared Instrument (MIRI) JPL/ESA
Fine Guidance Sensor (FGS) CSA
Operations: Space Telescope Science Institute
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JWST Requirements
Optical Telescope Element
25 sq meter Collecting Area
< 50K (~35K) Operating Temp
r mary rror
6.6 meter diameter (tip to tip)
< 25 kg/m2 Areal Density< 4 m rea ost
18 Hex Segments in 2 Rings
Drop Leaf Wing DeploymentLow (0-5 cycles/aper) 4 nm rms
CSF 5-35 c cles/a er 18 nm rms
Segments
1.315 meter Flat to Flat Diameter
Mid (35-65K
cycles/aper) 7 nm rms
< 20 nm rms Surface Figure Error-
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OTE Architecture Concept
OTE Clear Aperture: 25 m2
Secondary Mirror
Support Structure (SMSS)
ISIM Enclosure
p cs u sys em
Secondary Mirror Assembly (SMA)
Light-weighted, rigid Be mirror Hexapod actuator Stray light baffle
Primary Mirror Segment
Assemblies (PMSA)
BackPlaneDeployment Tower Subsystem
ISIM Electronics Compartment (IEC)
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Investments Have Reduced Risk
Mirror SystemMirror Actuators
AMSD SBMDMirrors
Wavefront Sensing and Control, Mirror Phasing
1 Hz OTE Isolators
Cryogenic Deployable OpticalTelescope Assembly (DOTA)
PrimaryMirrorStructureHinges and
WheelIsolators
Half-Scale SunshieldModel
Secondary Mirror
Structure Hinges
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JWST Technology Demonstrations for TNARMirror Phasing Algorithms Beryllium Primary
Mirror Segment
Backplane
Sunshield Membrane
Shutters
Near-Infrared Detector Mid-Infrared DetectorCryogenic ASICs
Cryocooler
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JWST
Technology Development of Large Optical Systems
Mirror Segment TechnologyDevelopment Lead for JWST
AMSD II Be, technology
selected for JWST
6.5
The 18 Primary Mirror segments
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AMSD Ball & Kodak
Specifications
Diameter 1.4 meter point-to-point
Ra ius 10 meter
Areal Density < 20 kg/m2Areal Cost < $4M/m2
Beryllium Optical Performance
Ambient Fig 47 nm rms (initial)
Ambient Fig 20 nm rms (final)
290K 30K 77 nm rms
55K 30K 7 nm rms
pt ca er ormanceAmbient Fig 38 nm rms (initial)
290K 30K 188 nm rms
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Advantages of Beryllium
Very High Specific Stiffness Modulus/Mass RatioSaves Mass Saves Money
High Conductivity & Below 100K, CTE is virtually zero.
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Figure Change: 30-55K Operational Range
ULEGlass
Beryllium
X
Y
VertexX
Y
Y
Surface
Figure WithAlignment
15.0mm
15.0mm
Gravity
15.0 mm15.0 mm
Gravity
on
er ex
XY
Vertex
X with 36ZernikesRemoved
15.0m
m
15.0m
m
Gravity
15.0 mm15.0 mm
Gravity
Vertex
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Mirror Manufacturing Process
Completed Mirror Blank
HIP Vessel being loading i nto chamber Machining of Web Structure Machining of Optical Surface
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Brush Wellman
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Substrate Fabrication
PM Segments SN 19-20
powder in loading container
egmen s -
HIP can prepared for powder loading
-
loaded HIP can in degas furnace
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Fabrication Process
Movie
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Quality Control X-Ray Inspection
PM Segment SN 17 after finish machining PM Segment SN 17 after x-ray
PM Segment SN 18 during finish machining PM Segment SN 18 during x-ray
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Status = Flight Mirror Blank Fabrication Complete
Be fabrication Brush-Wellman
Pathfinder
SecondaryMirrorSecondaryMirror
2 Flight
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Axsys Technologies
8 CNC Machining Centers
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Axsys Technologies
PMSA Engineering Development Unit
PMSA EDU rear side machined ockets PMSA EDU front side machined o tical surface
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Axsys Technologies
PMSA #1 (EDU-A / A1) PMSA #2 (3 / B1) PMSA #3 (4 / C1)
a c egmen s
PMSA #4 (5 / A2) PMSA #5 (6 / B2) PMSA #6 (7 / C2)
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Status = Flight Mirror Lightweighting Complete
Lightweighting Axsys
Pathfinder
SecondaryMirror
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Tinsley Laboratories
1st CCOS machine assembled in
JWST production area
Production Preparation CCOS Machines1st 4th CCOS machine bases assembled and operational
5th 8th CCOS machines received and in storage installation to start 4/4/05
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Status = Flight Mirror Polishing Started
Mirror Polishing Tinsley
Pathfinder
Coarse grind
fine grind
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PMSA Assembly
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PMSA Assy
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PMSA Assembly
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PMSA Assembly on its way to Optical Test
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PMSA Assembly on its way to Optical Test
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MSFC JWST Support Effort Facility Upgrades
Gate Valve
,
Add Forward He Extension
New XL Shrouds sections
Support System
5DOFTable - Upgrade
East End Dome
MSFC JWST Support Effort BSTA Test
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MSFC JWST Support Effort BSTA TestConfiguration
100 New He Shroud
15150.27
130.14 90New chamber
Lighting
61.69
38.47ac y p ca
Axis
New Facilit FloorExisting Table and
Stand-Offs
XRCF CCS Cross section1-10-05
Based on XL 90% Design ReviewData
Existing Table positioning
Actuators, 3 places
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XRCF Facility Upgrades in FY 05-06
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XRCF CCS Assembly
Shroud Reassembly 1 of 3 Shrouds rough cleaning
1 of 3 floors move into clean room Shrouds move into clean room
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XRCF CCS Fit- Check
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XRCF Facility With Be AMSD II Mirror
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JWST I&T
Chamber size 55' diam, 117' high
Existing Shrouds LN2 shroud, GHe panels
Chamber Door 40' diam
High bay space ~102'Lx71'W
JSC C U T C fi i
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Center of Curvature Null
JSC Cup Up Test Configuration
u o- o ma ng a s(used for double pass
optical testing).
Commercial DMIs used
and Interferometer
Accessible from top
for drift sensing, hexapod
for control.
Telescope Cup Up
Gravit offloaded and
Focal Plane Interferometer
and sources accessibleOn Ambient Isolators
Connected to Concrete)
rom e ow
Isolators used to controlhigh frequency vibration.
JSC Size, Accessibility, and Large Side Door Access
Make it Well Suited for This Configuration
JSC Ch b A Th l V F ilit
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JSC Chamber A Thermal Vacuum Facility
Chamber A was used for
Apollo landers and
already includes Nitrogen
and Helium systems. Plan
is to upgrade it with a new
Helium Inner Shroud and
Helium refrigerators.
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JWST Launch and Deployment
LongFairing
JWST is folded intostowed position to fit into
the a load fairin of the17m
Ariane V launch vehicle
Upper stage
deploy during transit to its
L2 orbit
H155Core stage
P230 SolidPropellant
Stowed Configuration
JWST vs HST orbit
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JWST vs. HST - orbit
SunSun
HST in Low Earth Orbit, ~500 km up.HST in Low Earth Orbit, ~500 km up.
EarthEarth
MoonMoon
Imaging affected by proximity to EarthImaging affected by proximity to Earth
Second Lagrange Point,1,000,000 miles away
45
JWST will operate at the 2nd Lagrange Point (L2) which is 1.5Million km away from the earth
JWST will operate at the 2nd Lagrange Point (L2) which is 1.5Million km away from the earth
L2L2
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S O
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JWST Optical Path
Off Axis Annular FOV
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Off-Axis Annular FOV
nv gne e s own n ac
OTE WFE < 131 nm rms within area bounded by black dashed line
The science instrument placement allocations are shown in blue
5.7
3.0
3.9
.
FGS-TFFGS-TF
0.2
1.1
2.1
arcm
in
NIRCam
-2.5
-1.6
-0.7
MIRI
-9.1
-8.2
-7.3
-6.4
-5.5
-4.6
-3.6
-2.7
-1.8
-0.9 0
.00
.9 1.8
2.7
3.6
4.6
5.5
6.4
7.3
8.2
9.1
arcmin
-3.4
JWST Mirror Phasing
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JWST Mirror Phasing
Telescope Deployment
FirstLightFirstLight
Secondary
Mirror
Focus
Sweep
Secondary
Mirror
Focus
Sweep
Segment Search
Segment - Image Array
Global Alignment
Image Stacking
Fine Phasing
Wavefront maintenance
W f t S i & C t l (WFS&C)
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Wavefront Sensing & Control (WFS&C)
Segment WFE
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Keck Demonstration of WFS&C
ACS Commands Measured
Preliminary results compared with PCS:
Peak-to-valley edge detection error = 0.45 microns
Rms detection error = 0.12 microns
Use or disclosure of data contained on this page is subject to the restriction(s) on the t itle page of this document.
JWST Phasing Algorithms Demonstrated
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JWST Phasing Algorithms Demonstrated
Coarse Phasing(Segment to segment piston)
Fine Phasing
Before Coarse Phasing
me
ters
)
After Coarse Phasing SWFE(nano
R
Fine Phasing Control Iteration
How to win at Astronomy
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How to win at Astronomy
=
Big Telescopes with Sensitive Detectors In Space
Photographic & electronic detection1010
WST
108
6 ograp
hy C
CDs
HS
Improvementover the Eye
104
Pho
0
leo
102
gens
piece
fra
tios
ort
s21.5
sche
lls48
es72
ntWilson
100
ntPa
lomar
20
iet6-m
Adapted from Cosmic
Discovery, M. Harwit 1600 1700 1800 1900 2000
Ga
li
Huy
ey
Slo S
Her
Ros
Mou
Mou
Sov
JWST Expands on HST Capabilities
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JWST Expands on HST Capabilities
: . m ame er r mary rror : . m ame er r mary rror
Room Temperature < 50 K (~ -223 C or -370 F)
as x e g ga er ng capa y o e
Hubble Space Telescope
JWST operates in extreme cold to enable sensitive infrared
light collection
How big is JWST?
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How big is JWST?
Full Scale JWST Mockup
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Full Scale JWST Mockup
21st
National Space Symposium, Colorado Springs, The Space Foundation
Full Scale JWST Mockup
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Full Scale JWST Mockup
21st
National Space Symposium, Colorado Springs, The Space Foundation
Why go to Space Wavelength Coverage
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Why go to Space Wavelength Coverage
1
NGSTr)
32m class
Space100s
urvey(h
nimagin
104
tomake
1 year
Tim
8m classGrnd-based
10 year
SIRTF
106
1 10
Wavelength (m)
Infrared Light
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Infrared Light
COLDCOLD
Why Infrared ?
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Why Infrared ?
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What are the first luminous objects?What are the first galaxies?
What sources caused reionization?
to identify the first luminous sources toform and to determine the ionization history of
Hubble Ultra Deep Field
the early universe.
A Brief History of Time
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y
First Galaxies
Form
Galaxies
Evolve
Intelligence
Particle
Atoms &
Radiation
3
TodayBig
Bang
300,000
years
minutes
100 million
yearsCOBE
JWST
1 billion
years 13.7 Billion years
MAPHST roun
Based
Observatories
History of Time?
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When and how did reionization occur?
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Reionization happened atz>6 or 1 billion years
WMAP says maybe twice?
Probably galaxies, maybe
quasar contr ut on
Spectra of the most distantquasars
S ectra of faint alaxies
First Light: Observing Reionization Edge
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Redshift
zzi
.
Patchy AbsorptionLyman Forest Absorption Black Gunn-Peterson trough
End of the dark ages: first light and reionization
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First galaxies are small & faint
Light is redshifted into infrared.
Low-metallicity, massive stars.
SNe! GRBs!
JWST Observations
Ultra-Deep NIR survey (1.4 nJy),
spec roscop c -
confirmation.
First Light
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What did the first stars galaxies to form look like?We dont know, but models suggest first stars were very massive!
Infrared Light
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Light from the first galaxies is redshifted from the visibleinto the infrared.
The Hubble Deep Field
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5.8
1.1
3.3
2.2
.
2.2
STScI Science Project: Robert Williams. et al. (1997)
.
Age
(Gyr)
How do we see first light objects?
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ereenue
+ + =
Deep Imaging: Look for near-IR drop-outsDeep Imaging: Look for near-IR drop-outs
5.8 Gyr 2.2 Gyr
3.3 Gyr 1.8 G r
. .
Hubble Ultra Deep Field- Advanced Camera for Surveys
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Advanced Camera for Surveys
,
Sept-Oct (40 days), Dec-Jan (40 days)
B V I z
F435W F606W F775W F850LP
m m m m
m m m m
JWST is designed to routinely operatein the dee surve ima in mode
Ultra Deep Field
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~
AGN z = 5.5
Malhotra et al. 2004
Galaxy z = 5.8 Galaxy z = 6.7
QSO z = 2.5Galaxy z = 0.48
New Results from UDF
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Z=0.48 Z = 5.5 Z = 5.8 Z = 6.7
How do we see first light objects?
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The first stars may be detected when they becamebright supernovae. But, they will be very rare objects!The first stars may be detected when they becamebright supernovae. But, they will be very rare objects!
How do we see first light objects?
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The Renaissance after the Dark AgesHubble Ultra Deep Field
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DarkAgesHubble
Deep
Ba
ng
ation
S1Here
Now
pr mor agalaxy
Bi
)com
bi
normal
H II(r
H Igalaxy
TIGM ~ 4
zK
t
TIGM ~ 10
4
K
JWST
Sensitivity Matters
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GOODS CDFS 13 orbits HUDF 400 orbits
JWST Science Theme #2:
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The assembly of galaxies
Where and when did the Hubble Sequence form?
How did the heavy elements form?
to determine how galaxies and the dark matter, gas,stars, metals, morphological structures, and active nuclei
M81 by Spitzer
within them evolved from the epoch of reionization to thepresent day.
The Hubble Sequence
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Hubble classified nearby (present-day) galaxiesinto Spirals and Ellipticals.
The Hubble Space Telescope hasextended this to the distant ast.
Where and when did the Hubble Sequence form?
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hierarchical merging
Components of galaxies have variety ofages & compositions
JWST Observations:
NIRCam imaging
Spectra of 1000s of galaxies
Distant Galaxies are Train Wrecks
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Unusual objects
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Clusters of Galaxies
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Unexpected Big Babies
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Spitzer and Hubble haveidentified a dozen very old(almost 13 Billion lightyears away) very massive
(up to 10X larger than ourMilky Way) galaxies.
At an epoch when the
~of its present size, and~7% of its current age.
This is a surprising resultunex ected in currentgalaxy formation models.
Michael Werner, Spitzer Space Telescope, William H. Pickering Lecture, AIAA Space 2007.
.
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News reports thatS itzer and Hubbleposed a CosmicConundrum byfinding these verymassive galaxies inthe earlyUniverse.Thisc a enges eor esof structure
Michael Werner, Spitzer Space Telescope, William H. Pickering Lecture, AIAA Space 2007.
JWST Science Theme #3:
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Birth of stars and protoplanetary systems
How do clouds collapse?
How does environment affect star-formation?
to unravel the birth and early evolution of
stars, from infall on to dust-enshrouded
David Hardy
protostars, to the genesis of planetary systems.
How do proto-stellar clouds collapse?
f i ll i ll i
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Stars form in small regions collapsinggravitationally within larger molecular
.
Infrared sees throu h thick dust clouds
Proto-stars begin to shine within the
clouds, revealing temperature and
density structure.
JWST Observations:Deep NIR and MIR imaging of dark clouds
Barnard 68 in visible lightBarnard 68 in infrared
and proto-stars
How does environment affect star-formation?
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Massive stars produce wind & radiation
Either disrupt star formation, or causes it.
dwarf stars & planets is unknown
Different processes? Or continuum?
JWST Observations:
urvey ar c ou s, e ep an run s an
star-forming regions
as seen by HST
as seen in the infrared
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Spitzer has
FoundMountains
Creation
Michael Werner, SpitzerSpace Telescope, William
L. Allen, CfA [GTO]
. ,Space 2007.
The Mountains Tell Their TaleInterstellar erosion & star formation
propagate thro gh the clo d
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propagate through the cloud
Young (Solar Mass) Stars are
Shown in This Panel
Really Young Stars are Shown in
This Panel
Michael Werner, Spitzer Space Telescope, William H. Pickering Lecture, AIAA Space 2007.
Birth of Stars and Proto-planetary Systems
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How are Planets Assembled?
Protoplanetary Disk
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Protoplanetary Disk
Michael Werner, Spitzer Space Telescope, William H. Pickering Lecture, AIAA Space 2007.
Dust disks are durable andomnipresent
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The central star of the Helix Nebula, a hot, luminous White Dwarf, showsan infrared excess attributable to a disk in a lanetar s stem which
survived the stars chaotic evolution
Michael Werner, Spitzer Space Telescope, William H. Pickering Lecture, AIAA Space 2007.
How are circumstellar disks like our Solar System?
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Here is an
illustration of
what MIRI might
very young core
in Ophiuchus,
VLA 1623
artists concept of
protostellar disk
from T. Greene,
.
approximate field for JWST NIRSpec & MIRI
integral field spectroscopy
JWST Science Theme #4:
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Planetary systems and the origins of life
How do planets form?
How are circumstellar disks like our Solar S stem?How are habitable zones established?
to determine the physical and chemicalproperties of planetary systems including our
Robert Hurt
own, an o nves ga e e po en a or eorigins of life in those systems.
How do planets form?
-
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Solar System primordial disk is now in small planets, moons, asteroidsan comets
JWST Observations:Coronagraphy of exosolar planets
Compare spectra of comets & circumstellar disks
Fomalhaut (ACS): Kalas, Graham & Clampin 2005
Planetary systems and the Origins of Life
Fomalhaut system at 24 m
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(Spitzer Space Telescope)
72
Malfait et al 1998Simulated JWST imageFomalhaut at 24 microns
Planetary Systems and the Origins of Life
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Planetary Systems and the Origins of Life
Model of Vega system at 24 m (Wilner et al. 2000)
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ode o ega syste at ( e et a 000)
orma au sys em a m(Spitzer Space Telescope)
(HST/ACS)
972
History of Known (current) NEO Population
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1800180019001950199019992006 Known
The Inner Solar System in 2006
Earth
minor planets
~4500 NEOs
~850
Outside
Earths
Hazardous
Objects (PHOs)
Orbit
Scott
Armagh
Observatory
Manley
Landis, Piloted Flight to a Near-Earth Object, AIAA Conference 19 Sep 07
Brown Dwarfs Form Like Stars:
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A Brown Dwarf With a Planet-Forming DiskMichael Werner, Spitzer Space Telescope, William H. Pickering Lecture, AIAA Space 2007.
How are habitable zones established?
Source of Earths H20 and organics is not knownTitan
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gComets? Asteroids?
History of clearing the disk of gas and small bodiesTitan
JWST Observations:
Comets, Kuiper Belt Objects
Icy moons in outer solar system
Search for Habitable Planets
amosp ere
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amosp ere
a a
L. Cook
Sara Seager (2006)
Atmospheres of Extrasolar Planets
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Extrasolar Planet Transits
Detecting terrestrial planet atmospheres
Burrows, Sudarsky and Lunine (2003)
Transiting Planet Science
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-
10-4
Courtesy Lori Allen
10-2
HD 189733b: First [one-dimensional]temperature map of an exoplanet
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970K on night side; 1210K
on day side
8um over morethan half an
orbit
of high-noon point.
High easterly winds, 6000mph, carry heat around
p anePrecise Spitzer
observations indicateelliptical orbit => unseen
Model: Assumestidal locking of
planet, could be as small
as Earth?
and extrapolates
in latitude.
Michael Werner, Spitzer Space Telescope, William H. Pickering Lecture, AIAA Space 2007.
Search for Life
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at s e
Life Metabolizes
Sara Seager (2006)
All Earth life useschemical energy
enerated from redox
reactions
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Life takes advantage ofthese spontaneousreactions that are
kinetically inhibited
Diversity ofmetabolisms rivalsdiversit of exo lanets
Lane, Nature May 2006 Sara Seager (2006)
Bio Markers
Spectroscopic Indicators of Life
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Absorption Lines
CO2
Water
Red Edge
Is there water in an Exoplanet?
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Michael Werner, Spitzer Space Telescope, William H. Pickering Lecture, AIAA Space 2007.
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Kasting Sci. Am. 2004See Kaltenegger et al. 2006Earth from the Moon
Seager
Countdown to Launch
Planned for 2013 Launch
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Ariane 5Ariane 5
Any Questions?
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UDF
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