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James Webb Space Telescope
Organization Mission Lead: Goddard Space Flight Center Senior Project Scientist: Dr John Mather International collaboration: ESA & CSA Prime Contractor: Northrop Grumman Aerospace Systems Instruments: · Near Infrared Camera (NIRCam) ­ Univ. of Arizona · Near Infrared Spectrograph (NIRSpec) ­ ESA · Mid-Infrared Instrument (MIRI) ­ JPL/ESA · Fine Guidance Sensor (FGS) & Tunable Filter Imager ­ CSA Operations: Space Telescope Science Institute Description · Deployable infrared telescope with 6.5 meter diameter segmented adjustable primary mirror · Cryogenic temperature telescope and instruments for infrared performance · Launch on an ESA-supplied Ariane 5 rocket to Sun-Earth L2 · 5-year science mission requirement (10-year propellant lifetime)

JWST


Your Science Working Group

Hammel

Lunine

Lilly

McCaughrean

Stiavelli Windhorst

M. Rieke

Franx

G. Rieke

Wright

Doyon

Mountain

Clampin Flanagan Gardner Greenhouse Hutchings Jakobsen Mather Sonneborn


Decadal 2000 & 2010 Science with JWST
M81

HST-UDF

First Light and Re-Ionization
HH-30

Assembly of Galaxies
GL146

M-16

Birth of stars and proto-planetary systems
JWST

Planetary systems and the origin of life


The James Webb Space Telescope
JWST

6.5 meters

Hubble

2.4 meters

Spitzer
0.85 meters

Light Gathering Power
JWST = 25 m2 ; Hubble = 4.5 m2 ; Spitzer = 0.6 m2


JWST In

The James Webb Space Telesc struments ope

The Near Infrared Camera (NIRCam)

- Visible and near infrared camera (0.6 ­ 5 micron) - 2.2 x 4.4 arcmin field of view, diffraction limited - Coronographs

The Near Infrared Spectrograph (NIRSpec)
Multi-object dispersive spectrograph (1 ­ 5 micron) 3.4 x 3.4 arcmin field of view with 0.1 arcsec pixels R = 1000 and 2700 gratings and R = 100 prism IFU over 3 x 3 arcsecond region

The Mid Infrared Instrument (MIRI)
Mid-infrared camera and slit spectrograph (5 ­ 28 microns) 1.9 x 1.4 arcmin imaging field of view with 0.11 arcsec pixels R = 100 slit spectrograph (5 ­ 10 micron) and IFU (R = 3000) Coronographs

NIRCam

The Tunable Filter Imager (TFI)
- Infrared imager and slit spectrograph - 2.2 x 2.2 arcmin field of view

The Fine Guidance Sensor (FGS)

- 2.4 x 2.4 arcmin imager for target acquisition - Rapid readout of subarray for ACS control - Ensures 95% probability of finding a guide star anywhere in sky

NIRSpec


JWST Sci

The James Webb Space ence Themes e The Quest for Origin Telescop ­

s

1.) The End of the Dark Ages

- Discover the first stars, protogalaxies, supernovae, and black holes - Follow the Universe's ionization history across cosmic time

2.) The Assembly and Evolution of Galaxies

- Track the merger of protogalaxies - Study the effects of black holes on their surroundings - Map the evolution of dark matter, stars, and metals through galaxy growth

3.) The Birth of Stars and Planetary Systems
Unveil newborn stars and planets in dusty clouds Reveal the dependency of star formation to environment Measure how chemical elements are produced and recirculated Complete the stellar and substellar inventory Measure the IMF to below the H-burning limit, in different environments

4.) The Origins of Life

- Study the formation of planets - Measure the composition of atmospheres, probe for liquid water - Complete the census of the outer solar system JWST Science summarized in 15 JWST Science White Papers http://www.stsci.edu/jwst/science/whitepapers


JWST Sci
1 2 3 4 .) .) .) .) What When What What

The James Webb Space ence Themes e The End of the Dark Telescop ­

Ages

JWST Questions
are the first galaxies? did reionization occur? is the Universe's reionization history? sources caused reionization?


JWST Sci

The James Webb Space ence Themes e The End of the Dark Telescop ­
The Hubble UDF (F105W, F125W, F160W)

Ages

Simulated JWST

JWST will have higher angular resolution than Hubble for deep fields


JWST Sci

The James Webb Space Telescop ­ ence Themese The Assembly and E

volution of Galaxies

JWST Questions
1.) Where and when did the hubble sequence form? 2.) Do hierarchical formation models and global scaling relations explain diverse galaxy morphologies and their cosmic evolution? 3.) How did the heavy elements form? 4.) What role do ULIRGs and AGN play in galaxy evolution?


JWST Sc

The James Webb Space Tele hemes ­ ience Tscope The Birth of Stars an

d Planetary Systems

The power of high-res ir imaging (Hints from WFC3)

The Carina Nebula


JWST Sc

The James Webb Space Tele hem p ­ ience Tscoese The Birth of Stars an

d Planetary Systems

- Lifting the Curtain on Star Formation (optical)


JWST Sc

The James Webb Space Tele hem p ­ ience Tscoese The Birth of Stars an

d Planetary Systems

- Lifting the Curtain on Star Formation

JWST Questions
1.) How 2.) How 3.) How new 4.) How 5.) Wha 6.) How do clouds collapse and form stars and planets? does environment affect star formation? does feedback from star formation affect environment, and trigger star formation? are chemical elements produced and recirculated? t is the stellar and substellar IMF, to and beyond the H-burning limit? does the IMF depend on environment (age, metallicity, binarity)?


JWST Sci

The James Webb Space Telescop ­ ence Themes e The Origins of Life

Atmospheric transmission spectrum (4 hours) for HD209458like Kepler source using NIRSpec (R=3000). Simulation from J. Valenti

JWST Questions
1 2 3 4 .) .) .) .) How do planets Form? What are the properties of circumstellar disks like our solar system? What criteria should be used to establish habitable zones? Is there evidence for liquid water on exoplanets? JWST will detect water in habitable zone super Earths


The James Webb Space Telescope The Outer Solar Sys

te m

1.) NIRSpec will measure IR spectra for all known Kuiper Belt Objects (KBOs). 2.) Spectral features from water ice will be mapped at redder wavelengths than currently possible, revealing surface mineralogy. 3.) The Chemical compositions of these provide clues to the nature of the so This in turn provides insights on the formation and evolution of the solar
Artist's impression of a binary KBO

objects will lar nebula. early system.

NIRC spectra of water ice features in Haumea collision family objects


The James Webb Space Telescope Protoplanetary Disks
1.) Resolve structure in the nearest disks at >30 AU scales with TFI and MIRI Coronography 2.) Measure dust settling characteristics as a part of planetesimal build up 3.) Trace gaps and asymmetries produced by embedded protoplanets

4.) Delineate gas content and parent populations 5.) Measure radial dependency of gas chemistry 6.) Probe mass inflow and outflow 7.) Measure statistics of disk properties vs stellar mass and environment

HH 30 edge-on disk with NIRSpec/MIRI IFU FOV


The James Webb Space Telescope Massive Stars: Forma

tion

1.) How do hot, massive stars emerge from their dust-obscured natal cocoons? 2.) How does their presence affect the formation of other stars?

Massive Stars: Feedback
3.) How does the evolution of massive stars shape their galactic environments? 4.) How does metallicity effect massive star evolution?

Massive Stars: Circumstellar Structure
5.) What causes circumstellar nebulae to form around LBV and WR stars? 6.) How is mass lost from these stars? 7.) How are their outflows structured?
Bow shock around the Galactic O-type runaway star Ophiuchi


Resolved

The James Webb Space Tellarscopte ­ Local Group le Popula ions Ste

1.) NIRCam and TFI Imaging plus NIRSpec MOS spectroscopy of star forming regions and Milky Way components will provide age and abundances distributions, testing formation and assembly models.

2.) Use near-IR imaging to complete a stellar inventory of nearby populations, by measuring stars from the brightest giant phases to low mass dwarfs. 3.) MIRI imaging and spectroscopy will penetrate extincted regions to discover and characterize Teff, log(g), and mass for stars down the hydrCaren buruling lAmi,t, SA, d .intoth (UCsterlkeley), and the Hubble Heritage Team og ina Neb n a - N i SA E an N Smi sub- B e lar (STScI regimes. /AURA)


The James Webb Space Telescope Resolved Stellar Popu

lations ­ Local Volume

1.) Photometry will reach faint main sequence stars like our Sun in galaxies outside the local group. Extended star formation periods will be efficiently measured with filters well-separated in wavelength. 2.) Relative to HST Imaging, JWST/NIRCAM will have superb sensitivity over a broad wavelength range, be diffraction limited, and have a larger field of view. This will yield deep near-IR CMDs with excellent age discrimination.

3.) A view of the nearby universe, with galaxies at their true distances. Concentric circles correspond to hypothetical observing programs of 10, 100, and 1000 hours. 4.) At a given distance, JWST will see nearly six times faster than HST for this type of work. 5.) For a given exposure time, JWST can explore galaxies about 50% further away than those available to HST.


Transien

The James Webb Space Telescope t Objects

1.) Explore the nature of exotic transients through increased sensitivity and resolution (GRBs, Sne, tidal disruption events, unknown objects, ...). 2.) Measure the nature of Dark Energy through IR light curves of SNe. 3.) Measure the SNe rate at high-z and probe its connection with the star formation rate and galaxy morphology.


Dark En
1 2 3 4 5 . . . . . ) ) ) ) )

The James Webb Space Telescope ergy and Dark Matter: The acceleration para

meter of the Universe

Leverage multiple techniques to minimize systematic errors. wide field surveys will find targets. Measure very distant supernovae (standard candles?) SNe rest frame IR light curves ­ may be better standard candles? directly measure effects of dark matter from distorted geometry of distant objects, masses of galaxies and clusters to high-z, rotation curves, etc... 6.) Map cosmic archeology at high-z (prior to acceleration, formation of clusters). 7.) Measure Cepheid variables in galaxies with known maser distances.

JWST will constrain Dark Energy through exquisite measurements of H

O


Specific

The James Webb Space JWST Sciencpe ficiencies Telesco e Ef

Solar System ­ JWST/MIRI spectroscopy of gas giants will resolve temperature sensors and shed l igh t on underlying driving dynamics. Debris Disks ­ JWST/MIRI will provide sensitivity and resolution to map the 10 and 20 micron silicate emission features generated by circumstellar dust graints (<2 hours). Exoplanets ­ JWST/NIRSpec will measure phase curves of exoplanets around nearby M dwarfs (< 1 hour) and characterize water features in the atmospheres of "ocean planets". Stars and Star Clusters ­ JWST/NIRCam will measure the stellar mass function down to the hydrogen burning limit in stellar populations out to 25 kpc (<3 hours). Galaxy Evolution ­ JWST spectroscopy of star forming galaxies allows calculation of escape fraction and contributions to ionization budget. First Objects ­ JWST will resolve ambiguities from Hubble and Spitzer in fitting SEDs by spectroscopically characterizing early systems at z = 9, and characterizing stellar contributions to z > 10. First explosions will be seen through a time rise of radiation as the fireball expands and cools. Dark Energy ­ JWST/NIRCam sensitivity will enable high precision measurements of the Hubble


Visit

The James Webb Space Te JWST at:lescope

- The Space Telescope Science Institute (STScI): http://www.stsci.edu/jwst/ - NASA Goddard Space Flight Center (GSFC): http://www.jwst.nasa.gov/ - European Space Agency (ESA): http://sci.esa.int/science-e/www/area/index.cfm?fareaid=29 - Canadian Space Agency (CSA): http://www.asc-csa.gc.ca/eng/satellites/jwst/default.asp - Northrop Grumman: http://www.as.northropgrumman.com/products/jwst/index.html - JWST Observer Facebook: http://www.facebook.com/pages/JWSTObserver/103134319723237 - flickr: http://www.flickr.com/photos/nasawebbtelescope/ - Twitter: @auraJWST JWST Public Website: http://webbtelescope.org/webb_telescope/ JWST Public Facebook: http://www.facebook.com/webbtelescope Twitter: @NASAWebbTelescp Youtube: http://www.youtube.com/user/NASAWebbTelescope

- Newsletter at STScI: https://blogs.stsci.edu/newsletter/ - Newsletter at GSFC: http://www.jwst.nasa.gov/newsletters.html