Документ взят из кэша поисковой машины. Адрес оригинального документа : http://www.stsci.edu/jwst/news/2011/DPS2011_JWSTFlyer.pdf Дата изменения: Unknown Дата индексирования: Tue Feb 5 03:24:17 2013 Кодировка: Поисковые слова: spitzer space telescope

"There are three main areas in which collabora2on with other parts of NASA could benefit the solar system explora2on program....the Hubble Space Telescope has a long history of successful planetary observa2ons, and this collabora2on can be a model for future telescopes such as the James Webb Space Telescope."


Vision and Voyages for Planetary Science in the Decade 2013 2022

Going Beyond Hubble and Spitzer: Planetary Science with the

James Webb Space Telescope

NASA's Great Observatories have provided both astronomers and planetary scienLsts unique imaging and spectroscopic capabiliLes for many years. The Hubble Space Telescope and Spitzer Space Telescope have advanced research on virtually every topic in space science, and planetary scienists have led proposals on these telescopes that have helped to reshape our view of the solar system. Among the many discoveries that these telescopes have provided are: Discovery of new moons around Pluto. Discovery of the largest ring around Saturn. CharacterizaLon of Ceres, Vesta, and other dwarf planets and asteroids. Discovery of new Kuiper Belt Objects (KBOs). Detailed studies of cloud structure in outer gas giants. Long term monitoring of the MarLan atmosphere. And much more...


As Hubble and Spitzer near the end of their lives, NASA, ESA, and the CSA are building their successor, the James Webb Space Telescope (JWST). JWST is a flagship mission that will revoluLonize our understanding of the Universe. It is much larger, more sensiLve, and has higher resoluLon than other Great Observatories. A significant amount of Lme on JWST is expected to be devoted to planetary science, where it will be more than 100 Lmes as powerful as Hubble and Spitzer at infrared wavelengths. JWST Quick Facts 6.5 meter primary aperture 0.6 ­ 28.5 micron wavelength range DiffracLon limited 65 mas resoluLon at 2 microns Unprecedented IR sensiLvity: S/N = 10 at K = 27.5 AB mag in 10 min

Planetary Science with JWST
PoinLng control system enables observaLons of solar system objects with rates of moLon up to 0.03 arcsec per second. This includes all planets and asteroids beyond Earth's orbit.

1.) Kuiper Belt Objects (KBOs) JWST will:
Image all known KBOs in the mid infrared. Perform near infrared spectroscopy with R = 100 of all known KBOs (V < 25); S/N = 20 in 3 hours. Provide higher resoluLon spectra of bright KBOs.


Spectral coverage and resoluLon will directly constrain surface composiLon (H2O, CH4, CH3OH) and volaLle inventories of all known KBOs, and provide the first spectra of these objects at 2.5­5 microns. The ice/water hydraLon band at 3.1 microns is easily within the reach of NIRSpec in the vast majority of all KBOs. Such results will directly address the dynamical (and chemical) history of the solar system and test formaLon theories. The observaLons will also elucidate the role that giant planet migraLon has played in the evoluLon of the solar system. Radiometry of KBOs will enable beker characterizaLon of their albedos and hence the size distribuLon within the Kuiper Belt.


2.) Dwarf Planets JWST will:
Perform Lme resolved imaging of Pluto, Eris, Sedna and other dwarf planets. Provide infrared spectroscopy of large bodies in the outer solar system.


JWST observaLons will reveal seasonal behavior of the largest outer solar system bodies and provide a new level of understanding on their surface composiLons. The spectra will be well suited to track variaLons in N2 and CH4, and will also likely result in the discovery of new organic molecules or previously undetected ices. The combinaLon of high resoluLon temporal imaging and spectroscopy will explore correlaLons between atmospheric chemistry changes and albedo. Ar2st's impression of a binary KBO

3.) Comets JWST will:
Provide Near infrared spectroscopy with R = 1000 of cometary comae. Provide Mid infrared spectroscopy of cometary dust grains. Perform the first spectroscopic studies of the new class of icy comets in the main asteroid belt.


JWST will enable studies of the chemical composiLon of cometary ice and dust with unprecedented sensiLvity. Spectroscopy will measure abundances of H2O, CO2, CO, and CH3OH in the comae of faint comets and also constrain the raLo of ortho and para H2O to reveal formaLon temperatures. This set of observaLons is a criLcal ingredient in understanding planetary system formaLon and evoluLon, when combined with synergisLc JWST observaLons of circumstellar disks. AddiLonally, the study of icy comets in the asteroid belt may reveal the source objects that were responsible for the delivery of water to the Earth. JWST Observing Modes Four science instruments with mulLple imaging, co NIRCam 0.6 ­ 5 micron sensiLvity 26 wide, medium, and narrow band filters DiffracLon limited Coronographs RI MI 5.0 ­ 28.5 micron sensiLvity R = 100 slit spectrograph Integral Field Spectroscopy (R = 3000) 3 phase masks and Lyot Coronograph

ronographic, and spectroscopic capabiliLes. NIRSpec 1 ­ 5 micron sensiLvity MulL object (>100) dispersive spectrograph R = 100, 1000, 2700 spectral resoluLon Integral Field Spectroscopy FGS and NIRISS 1 ­ 5 micron sensiLvity Near IR imaging R = 150 and R = 700 grism spectroscopy Non Redundant Mask for high res. imaging


4.) Planets and Moons
JWST's capabiliLes will provide unmatched imaging and spectroscopic studies of Mars and all outer solar systems planets and moons. These data enable new science invesLgaLons.


Mars JWST will: Use Lme resolved near infrared spectroscopy to study the variability of atmospheric species including CO2, CO, and H2O and constrain radiaLve and absorpLve properLes of airborn dust, enabling photochemical and dynamical modeling of the MarLan climate. Use direct near infrared detecLon to assess magnitude and scale of diurnal, seasonal, and interannual volaLle transport, and discriminate surface and atmospheric ices and clouds. Characterize potenLal large methane outbursts.


Jupiter and Saturn JWST will: Use mid infrared medium resoluLon spectroscopy and IFU data to study the rich planet and atmosphere composiLon. Fully explore infrared diagnosLcs such as phosphine and methane flourescence, which link to verLcal dynamics and thermal structure of the upper atmosphere. Provide a global context on large scale weather pakerns for high resoluLon studies from complementary planetary missions (e.g., Juno and Cassini).


Uranus and Neptune JWST will: Image spectral features coming from high laLtudes in each planet with high sensiLvity and map clouds in both planets. Perform spectral characterizaLon of H3+, CO in flourescence, detailed mapping of 5 micron window, search for minor species, and measure isotopic raLos of major elements. Use mid infrared observaLons to measure temporal variaLons in temperature, resolve sources of underlying driving dynamics, and disentangle causes of rotaLon modulaLon.


Icy Moons JWST will: Complement and extend planetary missions such as Cassini. Perform long Lme baseline observaLons of both atmospheric and surface changes. For Titan, use near IR spectrometry with a resoluLon >6 Lmes Cassini's to determine types of organic species present on the surface. The higher spectral resoluLon over midlaLtute regions will reveal whether surface changes or secular atmospheric changes are in evidence over a decadal Lmescale. For More InformaJon:


1.) Lunine, J. et al. (2010), JWST White Paper, "JWST Planetary Observa2ons within the Solar System" 2.) Sonneborn, G. et al. (2009), "JWST Study of Planetary Systems and Solar System Observa2ons" JWST website: hkp://www.stsci.edu/jwst What can JWST do for you? Visit the JWST Exposure Time Calculator at hkp://jwstetc.stsci.edu/etc/