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From page 392... ... • 11.2.2.12 Segmented Telescope System -- This will be the most critical TRL element because it will include many of the completed activities in Table 11-5 in the LUVOIR final report. Even though this activity is a subscale of the telescope system, the panel suggests that it be designed to include any/all areas where the greatest uncertainties may exist. Read the entire page →
From page 393... ... models, end-to-end diffraction and wavefront control loops, and so on. These models have a level of fidelity that goes well beyond prior studies of coronagraphic or starshade instruments (except for the Roman Space Telescope) Read the entire page →
From page 394... ... Scott, and N Zimmerman, 2019, "Wavefront Sensing and Control Technologies for Exo-Earth Imaging," white paper submitted to Astro2020: Decadal Survey on Astronomy and Astrophysics. Read the entire page →
From page 395... ... The panel envisions developing a probe line as soon as is practical. Astrophysics will need to modify the program somewhat, but the EOS-1 panel suggests that a probe line would have the following characteristics. Read the entire page →
From page 396... ... For example, the Kepler mission, which originated as a Discovery mission, greatly expanded understanding of the number and diversity of planetary systems outside of our own solar system using the transit technique outside the confounding effects of Earth's atmosphere. The Spitzer Space Telescope, equivalent in today's dollars to a probe-class mission, was creatively repurposed beyond its original scientific objectives to probe the thermal structure, chemistry, and atmospheric dynamics of extrasolar planets. Read the entire page →
From page 397... ... Other science cases for SmallSats being developed now include a wide variety of astrophysical experiments, including exoplanets, stars, black holes and radio transients, galaxies, and multi-messenger astronomy. Achieving high-impact research with SmallSats is becoming increasingly feasible with advances in technologies such as precision pointing, compact sensitive detectors, and the miniaturization of propulsion systems.32 I.5.2 Foundational Programs The panel observes that several areas outside the usual mission development flow could have profound and far-reaching consequences if pursued. Read the entire page →
From page 398... ... Corrales, D Dragomir et al., 2019, "The Legacy of the Great Observatories: Panchromatic Coverage as a Strategic Goal for NASA Astrophysics," white paper submitted to Astro2020: Decadal Survey on Astronomy and Astrophysics, https://assets.pubpub.org/f2iwabky/11598545456167.pdf. Read the entire page →
From page 399... ... Because many galaxies are obscured by dust, it takes the synergy of two distinct kinds of observations to peer into their central regions: a high sensitivity and high-angular resolution X-ray imaging mission that can detect accretion onto the black holes themselves, and a far-IR spectroscopic mission that detects and pinpoints both the effects of the intense black hole radiation and the effects of star formation and evolution on galactic energetics. For the purposes of this report, these notional missions are called "Fire" and "Smoke." Fire and Smoke are based on the proposed flagship missions Lynx and Origins, respectively, but are scaled to fit into a single flagship program organized around the investigation of the cosmic dance science. Read the entire page →
From page 400... ... The panel reviewed a total of 55 white papers from the community, covering a range of diverse topics. Proposed space-based missions included experiments devoted to GeV and MeV gamma rays, hard X rays, high-resolution X-ray imaging, spectroscopy, timing, and polarimetry, far-IR, millimeter and MHz interferometry, the cosmic microwave background, cosmic rays, neutrinos, and gravitational waves. Read the entire page →
From page 401... ... APPENDIX J 401 TABLE J.1 EOS-2-Related Missions Operating or in Development Agency or Expected Mission Country Capabilities Spectral Coverage Launch Large Chandra NASA X-ray imaging and spectroscopy 0.2–10 keV γ-ray imaging and spectroscopy Transmission grating spectroscopy 0.08–10 keV Fermi NASA 30 MeV–300 GeV Spectroscopy 8 keV–30 MeV SOFIA NASA/DLR 2.7 m telescope 0.3–1600 µm IR imaging and spectroscopy XMM-Newton ESA X-ray imaging and spectroscopy 0.15–12 keV Reflection grating spectroscopy 0.33–2.5 keV X- and γ-ray imaging and spectroscopy UV/visible monitor 170–650 nm INTEGRAL ESA 3–35 keV; 15 keV–10 MeV Visible monitor 500–850 nm SRG DLR/Russia X-ray imaging and spectroscopy 0.2–10 keV; 5–30 keV γ-ray monitoring HXMT China X-ray imaging and spectroscopy 20–250 keV; 5–30 keV; 1–15 keV γ- and cosmic ray imaging and spectroscopy 5 GeV–10 TeV; 100 GeV–100 TeV 0.2–23 MeV DAMPE China Medium Swift NASA X- and γ-ray imaging and spectroscopy 0.2–10 keV; 15–150 keV UV/visible imaging 170–650 nm Astrosat India X-ray imaging and spectroscopy 0.3–100 keV UV/visible 200–300 nm; 130–180 nm Visible 320–550 nm X- and γ-ray all-sky monitor ISS-MAXI JAXA X-ray imaging and spectroscopy 2–30 keV; 0.5–12 keV GECAM China 6 keV–5 MeV Small NuSTAR NASA X-ray imaging and spectroscopy 3–79 keV Mission of Opportunity ISS-NICER NASA X-ray timing and spectroscopy 0.2–12 keV Approved JWST NASA IR imaging and spectroscopy 0.6–28.3 µm IXPE NASA X-ray polarimetry 2–8 keV GUSTO NASA IR high-resolution spectroscopy 63, 158, and 205 µm 2022 Einstein Probe China/DLR X-ray imaging and spectroscopy 0.5–5 keV; 0.3–10 keV 2022 X- and γ-ray imaging and spectroscopy XRISM Japan X-ray imaging and spectroscopy 0.4–13 keV; 0.3–12 keV 2023 SVOM China/France 0.3–10 keV; 4–150 keV 2023 Visible imaging 15 keV–5 MeV 400–950 nm γ-rays and electrons SPHEREx NASA IR spectroscopy 0.75–5 µm 2024 HERD China/ESA Tens of GeV–10 TeV 2027 member states Cosmic rays Up to PeV eXTP China/ESA X-ray imaging 2–50 keV 2027 member states Polarimetry 2–10 keV Spectroscopy 0.5–10 keV; 6–10 keV ARIEL/CASE ESA/NASA IR spectroscopy 1.25–7.8 µm 2029 Visible/IR photometry 0.5–0.55 µm; 0.8–1.0 µm; 1.0–1.2 µm Athena ESA X-ray imaging and spectroscopy 0.3–10 keV; 0.1–12 keV Early 2030s LISA ESA Gravitational waves 2 × 10–5–3 × 10–2 Hz 2034 NOTE: See Appendix P for definitions of acronyms. Read the entire page →
From page 402... ... The mission technical requirements are defined by the three scientific pillars described below, which map directly onto many of the key science questions and discovery areas from the Astro2020 science panels, especially the panels on Compact Objects and Energetic Phenomena, Cosmology, Galaxies, Interstellar Medium and Star and Planet Formation, and Stars, the Sun, and Stellar Populations. Pillar 1 -- The Dawn of Black Holes. Read the entire page →
From page 403... ... ; (2) Enhanced Main Array: FOV 1', pixel size 0.5", energy resolution ~2 eV (R ~3,000 at 6 keV) Read the entire page →
From page 404... ... These observations will open an electromagnetic J.2.2 Technology Driverswindow into the Dawn and Associated Risksof Black Holes. Lynx, using X-rays, and LISA, using gravitational waves, together will probe the growth of the first black holes by both Theaccretion primaryand Lynx technology mergers, driver unveiling is the development a complete picture of theirofearly the assembly. Read the entire page →
From page 405... ... Both processes are well 11 NASA Goddard Space Flight Center, 2019, Origins Space Telescope Mission Concept Study Report, Astrophysics Science Division, Greenbelt, MD. https://asd.gsfc.nasa.gov/firs/docs/OriginsVolume1MissionConceptStudyReport25Aug2020.pdf. Read the entire page →
From page 406... ... Theme 2 -- How do the conditions for habitability develop during the process of planet formation? Stars form within molecular clouds through accretion-disk–like structures onto protostellar cores. Read the entire page →
From page 407... ... . SOURCE: Top: NASA Goddard Space Flight Center, 2019, Origins Space Telescope Mission Concept Study Report, Astrophysics Science Division, Greenbelt, MD. Read the entire page →
From page 408... ... The primary differences between the TRACE analysis and that of the Origins team were in threat and reserve estimates, driving $56 million ($FY 2020) of the $88 million ($FY 2020) Read the entire page →
From page 409... ... J.4 THE COSMIC DANCE VISION: A JOINT X-RAY/FAR-IR FLAGSHIP PROGRAM As the panel reviewed the science of Lynx and Origins, it became clear that the missions complemented one another strongly. Neither mission by itself can address the full range of key science questions identified by the Astro2020 science panels, but together, they provide the required capabilities. Read the entire page →
From page 410... ... The two missions would be developed together as a single program, and launched contemporaneously, with a common science team to enable evaluation of trades both within and between them. While optimized for studying cosmic dance science, Fire and Smoke would also enable a broad range of high-priority science in other fields (as illustrated in Table J.3) Read the entire page →
From page 411... ... To ensure the feasibility of this approach for Fire and Smoke, the panel examined the data received through the TRACE analysis of Lynx and Origins, as well as the reports for AXIS and GEP. Recognizing that this panel cannot and should not design the cosmic dance program, the top-level cost scaling exercise described below was performed to ensure the feasibility of executing both Fire and Smoke concurrently, and within the available NASA budget. Read the entire page →
From page 412... ... Upper Bound: The panel was able to perform a more comprehensive cost estimation for Fire and Smoke by utilizing the TRACE estimates for the individual instruments required to accomplish the cosmic dance science. For Fire, this would be a wide-field imaging detector, while for Smoke, it would be a spectroscopic survey instrument. Read the entire page →
From page 413... ... TABLE J.2 EOS-2-Related Probe-Scale Mission Concepts Mission Concept Lead Author Closest Predecessor Science Capabilities Spectral Coverage FARSIDE Burns N/A z >10 neutral hydrogen and SETI search on lunar far 200 kHz–40 MHz side; exoplanets; heliophysics PICO Hanany Planck CMB polarization anisotropy 21–799 GHz CMB Spectral Kogut FIRAS CMB spectral distortions 10–6000 GHz Distortions GEP Glenn Spitzer, Herschel Star formation and SMBH growth over cosmic time 400–10 µm TSO Grindlay N/A UV–mid-IR time domain astronomy follow-up 5.0–0.3 µm AXIS Mushotzky Chandra, Athena Growth and fueling of SMBHs; transient universe; 0.3–10 keV galaxy formation and evolution STROBE-X Ray RXTE Compact objects; X-ray counterparts; time-domain 0.2–50 keV astronomy HEX-P Madsen NuSTAR Accreting compact objects; extreme environments 2–200 keV around black holes; neutron stars TAP Camp Swift Time-domain astrophysics 0.4 keV–1 MeV AMEGO McEnery Compton, Fermi Multi-messenger; γ-ray studies of neutron star 200 keV–10 GeV mergers; supernovae; flaring AGN POEMMA Olinto N/A Ultra-high-energy cosmic rays and cosmic neutrinos Cosmic rays >2 × from space 1019 eV Neutrinos >20 PeV MFB Michelson N/A Fills gaps in frequency coverage between LIGO and Gravitational waves LISA 10 mHz–1 Hz NOTE: See Appendix P for definitions of acronyms. Read the entire page →
From page 414... ... Therefore, new NASA-led time-domain missions with enhanced capabilities are urgently needed, both to ensure long-term continuity in this developing core field and to successfully capitalize on the science that will come from advanced gravitational wave detectors and the Rubin Observatory. Space-based platforms provide access to those bands that are undetectable from the ground: gamma rays, X rays, UV, and the mid- to far-IR. Read the entire page →

From page 392...

... • 11.2.2.12 Segmented Telescope System -- This will be the most critical TRL element because it will include many of the completed activities in Table 11-5 in the LUVOIR final report. Even though this activity is a subscale of the telescope system, the panel suggests that it be designed to include any/all areas where the greatest uncertainties may exist.