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JWST Solar System Science: Possibilities and GTO Plans
John Stansberry JWST Solar System Science Lead (STScI)
Stefanie Milam JWST Deputy Project Scientist for Solar System (GSFC)
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JWST Solar System Science
Applications: Sensitivity and Saturation
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Giant Planet Imaging with NIRCam
• Bright limits for 640x640 subarrays
• 160x160 limits are 15x higher
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JWST Capabilities: Giant Planets Imaging
• NIRCam Subarrays • short integration times • Significant FOV • Simultaneous 0.6-2.3 (shortwave)
and 2.4-5 (longwave) coverage • Matched FOVs
• Smaller subarrays available: 6402 (shown), 3202, 1602
• Dithers fill detector gaps in the
short-wave channel
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Giant Planet Imaging with MIRI
• Bright limits for 64x64 subarrays (6.4” FOV) • MIRI IFU spectroscopy limits are ~100x higher
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Giant Planet Spectroscopy: NIRSpec IFU
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Resolved Satellite Imaging: NIRCam
• Well-resolved satellites
• 1602 subarray bright limits
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Simulated Io Imaging with NIRISS AMI
Ke
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20
16
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Satellite Photometry with NIRCam
• 4002 subarray bright limits
• 1000 second exposure sensitivity
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Activity in Distant Comets and Centaurs
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3.6um: Dust 4.5um: Dust+Gas 4.5um: Gas Only
No background Subtraction
W/ background Subtraction
Courtesy of Mike Kelley, UMD
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Cometary Nuclei with NIRSpec & NIRCam
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• Comets can be studied throught the 1-5 um region
• High sensitivity (1000 sec sensitivities shown)
• At distances where H2O is unlikely to drive activity
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Simulated Comet Spectra
Milam et al. 2016
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NIRSpec Line Sensitivity
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KBO Photometry with NIRCam
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1.4: CH4
1.62: H2O
1.82: CH4
2.1: H2O
2.5: cont.
3.0: H2O
3.35: CH4
3.6: cont.
4.1: H2O CH4
4.3: N2 CO2
4.6: CO
4.8: cont.
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KBO Spectroscopy with NIRSpec
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KBO Thermal Radiometry with MIRI
• MIRI can measure temperature distributions for quite small KBOs
• Sensitivity well matched to that of ALMA
• Valuable for • Thermal inertia
• Composition • Regolith structure
• Emissivity • Albedo • Diameter
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Sub-mm (ALMA) vs. mid-IR (JWST)
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“beaming” parameter
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Sub-mm (ALMA) vs. mid-IR (JWST) Thermal ‘Beaming’
• Sub-mm accuracy • D ~5% • p_V ~10% • Temperature distribution of
warm regions sets systematic uncertainty
• What good are the warm regions? • Thermal inertia • Roughness • Rotation rate • Albedo variations
• Moons, rings, spots
• Volcanoes, plumes
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The Best Solution: BOTH!!
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JWST Solar System Science
Community White Papers
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PASP Special Issue (Jan 4, 2016)
Innovative Solar System Science with the James Webb Space Telescope
Stefanie Milam, Special Editor
http://iopscience.iop.org/1538-3873/128/959 11 topical papers
http://iopscience.iop.org/1538-3873/128/960 1 high-level paper (Norwood et al.)
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10 JWST Solar System Focus Groups
• Asteroids (Andy Rivkin, JHU/APL) • Comets (Chick Woodward, U. Minnesota) • Giant Planets (Jim Norwood, NMSU) • Mars (Geronimo Villanueva, GSFC) • NEOs (Cristina Thomas, GSFC) • Occultations (Pablo Santos-Sanz, IAA-CSIC, Spain) • Rings (Matt Tiscareno, Cornell) • Satellites (Laszlo Kestay, USGS) • Titan (Conor Nixon, GSFC) • TNOs (Alex Parker, SwRI) • JWST Solar System Capabilities (Milam, GSFC)
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(and 11 papers! http://iopscience.iop.org/1538-3873/128/959
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Flyers available here and on-line
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The James Webb Space Telescope’s plan for operations and instrument capabilities for
observations in the Solar System S.N. Milam et al.
The four science instruments on JWST cover the wavelength range from 0.6 – ~28μm and offer superb imaging and spectroscopic sensitivity. Subarray readouts will enable non-saturated observations of the giant planets and many bright primitive bodies in a variety of instrument modes.
JWST Solar System Science Possibilities and GTO Plans
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Science Capability Highlights • Important molecular (e.g. H2O, HDO, CO, CO2,
S2, CH4), ice, and mineral spectral features are at wavelengths accessible with JWST but not the ground.
• Near-IR spectra or colors (composition), and mid-IR photometry (albedos, sizes), for any Kuiper belt object known today.
• Semi-annual monitoring of planetary (and satellite) weather and seasonal changes.
• Near-simultaneous mapping and spectroscopy of cometary gas and dust from 0.6 – ~28 µm.
• Very sensitive spectral maps at R > 2000 over a 3”x3” field and with 0.1” spatial resolution.
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PASP Special Issue (Jan 4, 2016)
Innovative Solar System Science with the James Webb Space Telescope
Stefanie Milam, Special Editor
http://iopscience.iop.org/1538-3873/128/959 11 topical papers
http://iopscience.iop.org/1538-3873/128/960 1 high-level paper (Norwood et al.)
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JWST Solar System Science
Guaranteed Time Observer Preview
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Solar System GTO Time Allocations
• NIRCam – M. Reieke PI (J. Stansberry planning) • 20 – 30 hours, various KBO Characterization
• NIRSpec – P. Ferruit PI (Ferruit & Aurelie Guilbert planning) • 3 – 5 hours, spectra of smaller KBOs
• MIRI – G. Rieke (D. Hines), Gillian Wright (M. Mueller) • 10 Hours, KBO dwarf-planet thermal (Hines) • ~3 hours, EC contrib (M. Mueller)
• IDS – Hammel PI (S. Milam coordinating + planning) • 110 hours, Various programs based on PASP topics • Focused investigations of specific aspects of specific targets
• IDS – Lunine PI (planning starting) • 22 hours, Titan monitoring with MIRI (MRS) • 20 hours, KBOs (including Pluto)
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Probable Scope of GTO Investigations
• Kuiper Belt (NIRCam, Hammel, NIRSpec, MIRI) • Initial spectral characterization of dwarf planets, Triton • Detailed look at specific classes (e.g classicals, binaries, Haumea family) • Thermal characterization of a few objects
• Comets (Hammel) • Distant activity of periodic comets; TOO large Oort cloud comet
• Asteroids & NEOs (Hammel) • Characterization of a few specific targets
• Satellites (besides Titan and Triton) • Europa, Enceladus
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Possible Scope of GTO Investigations
• Giant Planets (Hammel) • Giant planet studies, temporal baseline; • Jovian & Saturnian aurorae
• Titan (Lunine, Hammel) • Preliminary spectral maps; 4.5 – 6 um hydrocarbons
• Rings (Hammel) • Investigate small satellites in Rings
• Mars (Hammel) • Cycle 2 program • D/H and water
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Where to Learn More…
Visit JWST at: - 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 - flickr: http://www.flickr.com/photos/nasawebbtelescope - JWST Public Facebook: http://www.facebook.com/webbtelescope - Twitter: @NASAWebbTelescp - Youtube: http://www.youtube.com/user/NASAWebbTelescope - JWST Webb-cam: http://www.jwst.nasa.gov/webcam.html - Newsletter at STScI: https://blogs.stsci.edu/newsletter/ - Newsletter at GSFC: http://www.jwst.nasa.gov/newsletters.html - Solar System Science with JWST: http://www.stsci.edu/jwst/science/solar-system Stefanie Milam, [email protected]
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Conclusions
• HST has made unique solar system science discoveries possible • JWST will be even better • Proposals do (and will) fare as well as those in other science
categories • They can have Discovery-class mission impact on Planetary
Science • IFF our community competes!
• Stay tuned! • More workshops and Webinars coming! • JWST Solar System Symposium, November 2017
• Ask questions! • Tell us what you need!
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JWST Science Instrument Overview
Instrument Modes, Sensitivity Comparison
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JWST Imaging Modes
Mode Instrument Wavelength (microns)
Pixel Scale (arcsec)
Full-Array* Field of View
Imaging
NIRCam* 0.6 – 2.3 0.032 2.2 x 2.2′
NIRCam* 2.4 – 5.0 0.065 2.2 x 2.2′
NIRISS 0.9 – 5.0 0.065 2.2 x 2.2′
MIRI* 5.0 – 28 0.11 1.23 x 1.88′
Aperture Mask Interferometry
NIRISS 3.8 – 4.8 0.065 ------
Coronography
NIRCam 0.6 – 2.3 0.032 20 x 20′′
NIRCam 2.4 – 5.0 0.065 20 x 20′′
MIRI 10.65 0.11 24 x 24′′
MIRI 11.4 0.11 24 x 24′′
MIRI 15.5 0.11 24 x 24′′
MIRI 23 0.11 30 x 30′′
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Simultaneous {
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Mode Instrument Wavelength (microns)
Resolving Power (λ/∆λ)
Field of View
Slitless Spectroscopy
NIRISS 1.0 – 2.5 150 2.2′ x 2.2′
NIRISS 0.6 – 2.5 700 single object
NIRCam 2.4 – 5.0 2000 2.2′ x 2.2′
Multi-Object Spectroscopy
NIRSpec 0.6 – 5.0 100, 1000, 2700 3.4′ x 3.4′ with 250k 0.2 x 0.5′′ microshutters
Single Slit Spectroscopy
NIRSpec 0.6 – 5.0 100, 1000, 2700
slit widths 0.4′′ x 3.8′′ 0.2′′ x 3.3′′ 1.6′′ x 1.6′′
MIRI 5.0 – ~14.0 ~100 at 7.5 microns 0.6′′ x 5.5′′ slit
Integral Field Spectroscopy
NIRSpec 0.6 – 5.0 100, 1000, 2700 3.0′′ x 3.0′′
MIRI 5.0 – 7.7 3500 3.0′′ x 3.9′′
MIRI 7.7 – 11.9 2800 3.5′′ x 4.4′′
MIRI 11.9 – 18.3 2700 5.2′′ x 6.2′′
MIRI 18.3 – 28.8 2200 6.7′′ x 7.7′′
JWST Spectroscopy Modes
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Photometric Sensitivity
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Medium Resolution Spectral Sensitivity
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Low Resolution Spectral Sensitivity
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