Stefanie Milam NASA Goddard Space Flight Center January 12, 2017 · 2017-01-12 · NASA Mission...
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Stefanie Milam NASA Goddard Space Flight Center January 12, 2017 SBAG – Tucson, AZ
Transcript of Stefanie Milam NASA Goddard Space Flight Center January 12, 2017 · 2017-01-12 · NASA Mission...
Stefanie Milam NASA Goddard Space Flight Center January 12, 2017
SBAG – Tucson, AZ
NASA Mission concept for 2020 Decadal review; launch 2030ish 10 μm – 1000 μm (ish), Large aperture 8-15 m Study Chairs: Margaret Meixner & Asantha Cooray
SBAG – Tucson, AZ
NASA Mission concept for 2020 Decadal review; launch 2030ish 10 μm – 1000 μm (ish), Large aperture 8-15 m Study Chairs: Margaret Meixner & Asantha Cooray Comes from the NASA Astrophysics Roadmap, Enduring Quests, Daring Visions: Improvements from Herschel • large gain in sensitivity • angular resolution sufficient to overcome spatial confusion in deep
cosmic surveys • new spectroscopic capability
Community Chairs: Margaret Meixner, STSCI, Asantha Cooray, UC Irvine
NASA Study Center: Goddard Space Flight Center (GSFC): Ruth Carter, David Leisawitz, Mike Dipirro, Anel Flores
NASA Head Quarters (HQ) Program Scientists (non-voting): Kartik Sheth and Dominic Benford
Ex officio non-voting representatives: Susan Neff & Deborah Padgett, NASA Cosmic Origins Program Office; Susanne Alato, SNSB; Douglas Scott, CAS; Maryvonne Gerin, CNES; Itsuki Sakon, JAXA; Frank Helmich, SRON; Roland Vavrek, ESA; Karl Menten, DLR; Sean Carey, IPAC
Members appointed by NASA (> 90 applications): Lee Armus, NASA IPAC; Cara Battersby, Harvard-Smithsonian CfA; Edwin Bergin, University of Michigan; Matt Bradford, NASA JPL; Kim Ennico-Smith, NASA Ames; Gary Melnick, Harvard-Smithsonian CfA; Stefanie Milam, NASA GSFC; Desika Narayanan, University of Florida; Klaus Pontopiddan, STSCI; Alexandra Pope, University of Massachusetts; Thomas Roellig, NASA Ames; Karin Sandstrom, UC, San Diego; Kate Y. L. Su, University of Arizona; Joaquin Vieira, University of Illinois, Urbana Champaign; Edward Wright, UC Los Angeles; Jonas Zmuidzinas, Caltech
Community Chairs: Margaret Meixner, STSCI, Asantha Cooray, UC Irvine
NASA Study Center: Goddard Space Flight Center (GSFC): Ruth Carter, David Leisawitz, Mike Dipirro, Anel Flores
NASA Head Quarters (HQ) Program Scientists (non-voting): Kartik Sheth and Dominic Benford
Ex officio non-voting representatives: Susan Neff & Deborah Padgett, NASA Cosmic Origins Program Office; Susanne Alato, SNSB; Douglas Scott, CAS; Maryvonne Gerin, CNES; Itsuki Sakon, JAXA; Frank Helmich, SRON; Roland Vavrek, ESA; Karl Menten, DLR; Sean Carey, IPAC
Members appointed by NASA (> 90 applications): Lee Armus, NASA IPAC; Cara Battersby, Harvard-Smithsonian CfA; Edwin Bergin, University of Michigan; Matt Bradford, NASA JPL; Kim Ennico-Smith, NASA Ames; Gary Melnick, Harvard-Smithsonian CfA; Stefanie Milam, NASA GSFC; Desika Narayanan, University of Florida; Klaus Pontopiddan, STSCI; Alexandra Pope, University of Massachusetts; Thomas Roellig, NASA Ames; Karin Sandstrom, UC, San Diego; Kate Y. L. Su, University of Arizona; Joaquin Vieira, University of Illinois, Urbana Champaign; Edward Wright, UC Los Angeles; Jonas Zmuidzinas, Caltech
Technical Definition
Aperture Diameter
FOV Diffraction Limited at
Temperature
8-15 m 0.5-1 square degree
40 μm ~4 K
Telescope Parameters
Technical Definition
Technical Definition
Instrument Specifications
Instrument
Wavelength Coverage μm
Spectral Resolution (λ/Δλ)
Field of view #spatial pixels
Typical Required Sensitivity: Other
Low-Res Spectrometer 35 to 500
low-res~500 high-res~104
100 per channel
10-21 W/m2 (spectral line) multi-channel
High-Res Spectrometer 50 to 500
low-res ~ 8x104 high-res~5x105 100
10-21 W/m2 5 σ (spectral line)
photo-counting
Heterodyne Spectrometer 150 to 500 ~107 10 - 100
2 mK in 0.2 km/s @ 1 THz
polarized, background limited
Far-infrared imager 35 to 500 R~15 100,000
1 μJy - 10 mJy (confusion limit)
5 to 10 channels, polarimetry, spectral line filters
Mid-Infrared Instrument 6 to 40
imager: R~15, spectrometer: R>500 106
photometric: 1 μJy @10 μm
coronagraph~10^-6 @ 0.5" @ 10 μm
Technical Definition: Telescope Design
Technical Definition: Telescope Design
Off-Axis 9.3m Diameter Projected Area: ~56m2
37 Segments Segment Flat to Flat: 1320mm Mass Rough Estimate: 3462 kg
Backplane Depth: ~495mm
JWST Segment 56m2 Area
5m x 19.8m Fairing Inst: 48m3
Bus: 38m3
Technical Definition: JWST Segment 56 m2 Area
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Presenter
Presentation Notes
JWST Segment 56m2 Area
Melnick
Technical Definition: Telescope Temperature
1/12/2017 13
Presenter
Presentation Notes
Why are cold telescopes important?? This plot shows the zodical light plus the telescope emission flux… The telescope temperatures range from 10 K down to 3 K… We can see that around 3 to 4+ K we become limited by the astronomical background as opposed to telescope background.
29 International Members Advise on Science Goals,
Capability Requirements, Complementary Science
Solar System Sub-Group
Anderson Carrie GSFC Arenberg Jon NGC Bauer Gerbs JPL Bergin Ted U. Mich Bjoraker Gordon GSFC Cordiner Martin CUA de Pater Imke Berkeley Ennico Kim Ames Fletcher Leigh Leicester Gerakines Perry GSFC Gurwell Mark CfA Hesman Brigette Umd Leisawitz David GSFC Lillie Charles Lillie Consulting Lis Darek Caltech Livengood Timothy UMd Milam Stefanie GSFC Moullet Arielle NRAO Nixon Conor GSFC Orton Glenn JPL Padget Deborah GSFC Palomba Ernesto IAPS-INAF Pontoppidan Klaus STScI Reach Bill USRA Santos Sanz Pablo IAA Stansberry John STScI Su Kate UAz Sylvestre Melody Bristol Unwin Stephen JPL
SBAG – Tucson, AZ
The Origins Space Telescope: Stefanie Milam
• How does presolar deuterium chemistry inform our understanding of D/H in the solar system and the development of Earth’s oceans?
• Measure HDO in 100s of comets for an un-biased survey.
• Measure accurate isotopic ratios (H, C, N, O) and abundances of trace gases, to constrain models and inform understanding of solar system origin and evolution.
Thermo-Chemical History of Comets and Water
Delivery to Earth Studies of Isotopes Across the Solar System (SS)
D/H measurements in comets, from Altwegg, K. et al. 2015. A larger statistical sample of targets are needed to determine the origin of Earth’s ocean and measure the dispersion of this ratio in both dynamic families.
With a 20m aperture (2e-21 W/m2) we can observe nearly ALL short and long period comets at multiple epochs. NOTE: Figure of Merit (FOM) = [30.68 + 1.23 log10 (Delta) - 0.25mV Q(H2O)/∆(AU)*1028]/Delta.
Presenter
Presentation Notes
Can we determine the origin of water (Earth’s Oceans) in the solar system from isotopic evidence in small bodies? Can statistical studies of volatile isotopes reveal the origin of volatiles to terrestrial bodies? There has been a limited number of measurements of D/H in comets (~dozen). Two have suggested a D/H ratio comparable to Earth’s oceans. A statistical survey of comets (both Oort Cloud and Jupiter family), 100s, will provide insight into whether these bodies contributed. OST will be able to measure this ratio in comets much fainter and less active than current facilities. Additionally, OST Observations of water in planets, satellites, and small bodies can help determine the distribution of water in the presolar disk, the origin of small bodies, as well as provide a tracer for planetary activity, potential sites for extraterrestrial biology, and offer insight into the nature of water in other planetary systems.
The Origins Space Telescope: Stefanie Milam
• Measure the thermal emission (via Far-IR imaging) of small bodies in outer SS –Sseveral 1000’s of targets out to >100 AU and sizes down to <10 km.
• Volatile isotope measurements (HCNO) across the SS
• Constrain the Thermal History/Evolution of the Solar System – He/H2 measurements.
• Not limited by confusion.
Survey of Small Bodies in the Outer Solar System
Heliocentric Distance (AU)
History and Evolution of the Solar System (SS)
Dia
met
er (k
m)
Bauer & Lovell 2016
50 µJy limit 30 µJy limit
KBOs and SDCs Main Belt
NEOs
10000
1000
100
10
10 100
Presenter
Presentation Notes
Coming to our own solar system, the Far-IR Surveyor can allow us to probe the history and evolution of the solar system… The left diagram shows the diameter vs. heliocentric distance of all the small bodies in the solar system and the lines show the continuum flux limits needed to measure these bodies at 125 microns for a 10m (cyan line) and 15m (green line) telescope. Note that most of the objects falling below these two lines were first measured al smaller heliocentric distances. In addition to the dust continuum the spectral line measurements of the volatiles as well as He and H_2
What’s happening now: •Five science working groups: membership is open to the community (US and foreign)
•Deciding on science questions in the post-JWST, 15 years of ALMA operations in an era of Extremely Large Telescope (ELT) and instrument requirements
Solar system: Stefanie Milam Planet formation and exoplanets: Klaus Pontoppidan and Kate Su Milky-Way, ISM and local volume of galaxies: Cara Battersby and Karin Sandstorm Galaxy and blackhole evolution over cosmic time: Lee Armus and Alexandra Pope First Billion years: Joaquin Vieira, Matt Bradford
Email: [email protected]
