NASA James Webb Space Telescope

8/14/2019 NASA James Webb Space Telescope

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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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21st

National Space Symposium, Colorado Springs, The Space Foundation



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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



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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!



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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




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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


Birth of Stars and Proto-planetary Systems


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How are Planets Assembled?

Protoplanetary Disk


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Protoplanetary Disk


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


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



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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.


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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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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NASA James Webb Space Telescope

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Transcript of NASA James Webb Space Telescope