Pathways to Discovery in Astronomy and Astrophysics for the 2020s (2023) / Chapter Skim
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Appendix J: Report of the Panel on Electromagnetic Observations from Space 2
Appendix J: Report of the Panel on Electromagnetic Observations from Space 2
Pages 398-421
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From page 398... ...
The panel discussed a wide array of white papers submitted by the community that are germane to this charge.1 In particular, the panel examined materials in support of two proposed flagship mission concepts, Lynx and the Origins Space Telescope, that provide new capabilities for X-ray and far-IR observations, respectively, as well as a suite of probe mission concepts covering a variety of fields. The panel requested and received Technical, Risk, and Cost Evaluations (TRACEs; see Appendix O)
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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.
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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.
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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.
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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.
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From page 403... ...
Athena's combination of moderate angular and (microcalorimeter-like) energy resolution is sufficient for point and significantly extended sources, but the Lynx combination of high throughput, 10× better angular resolution, and ultra-high spectral resolution, is crucial for detailed studies of galactic and circumgalactic environments.
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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.
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From page 405... ...
NASA Astrophysics budget for new missions that was presented to the panel, an additional 3+ years would be required. J.3 PROPOSED FAR-INFRARED FLAGSHIP MISSION CONCEPT: ORIGINS SPACE TELESCOPE The Origins Space Telescope is the second major flagship mission concept that falls within the purview of the EOS-2 panel.11 The mission concept is based on the Far-IR Surveyor notional mission envisioned in the NASA Astrophysics Roadmap Enduring Quests, Daring Visions.12 It would incorporate a 5.9 m cryogenic space telescope, operating from 2.8 to 588 μm, and deliver >1,000 times higher sensitivity than previous far-IR/submillimeter missions.
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With 8,000 pixels, it would be capable of wide field (>1,000 deg2) , diffraction-limited imaging that would address a variety of important astrophysical topics from the evolution of star formation over cosmic time to transient follow-up and monitoring.
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From page 407... ...
. SOURCE: Top: NASA Goddard Space Flight Center, 2019, Origins Space Telescope Mission Concept Study Report, Astrophysics Science Division, Greenbelt, MD.
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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)
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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.
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From page 410... ...
The [OIV] 25.9 μm line is detectable by Origins at the native resolving power of 300 and is an important diagnostic of black hole mass and accretion rates.
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From page 411... ...
Lower Bound: Although they are inadequate as proposed to fully explore the cosmic dance, the AXIS and GEP Probe concepts can be used to derive a reasonable lower bound for Fire and Smoke. The proposed costing for these missions, at ~$1 billion each as described in the concept reports and white papers, also assumed all requisite technology has achieved ~TRL 5 or 6 prior to mission start.
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From page 412... ...
The main difference between the TRACE analysis of Lynx and Origins and the cost estimates contained within the program reports was the addition of reserves and uncertainty based on prior program actuals, representing an increase in potential cost. In this costing exercise for a potential Fire and Smoke implementation, the same wrap rates for reserves and uncertainty recommended in the TRACE reports were maintained.
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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.
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From page 414... ...
Below, two high-priority science areas for strategic probe competitions are identified: Time-Domain and Multi-Messenger Astrophysics, and Early Universe Cosmology and Fundamental Physics. J.5.1 Time-Domain and Multi-Messenger Astrophysics In several of the science panels, time-domain astrophysics emerged as a key scientific priority for the next decade (see Table J.3, especially the entries for compact objects and energetic phenomena)
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From page 415... ...
At large angular scales, there is the prospect of detecting and characterizing relic gravitational waves from the Big Bang through their effect on CMB polarization. This has major implications for cosmology, since it provides insight into a critical phase when the infant universe expanded by a factor of ~1026 in 10–32 s.
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From page 416... ...
Flagship Missions: Major advances in scientific capability will continue to require multi-billion-dollar missions. While such flagship-class missions are scientifically compelling, maintaining a well-balanced portfolio requires that they be more accurately estimated and more tightly conceived and managed in a constrained environment.
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From page 417... ...
Explorers provide flexibility in the overall program not accessible to larger missions. While more narrowly focused in the scope of questions they can address, they allow for compressed time scales of development, permitting timely and rapid response to newly arising scientific questions, exploitation of the most recent innovations in instrumentation, and the opportunity for scientists and engineers to experience the end-to-end design and production of space missions.
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LISA will open up the millihertz-frequency band of gravitational waves, a band rich with sources ranging from white-dwarf binaries in the Milky Way to massive black holes throughout the entire universe.
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Q4. What seeds supermassive black holes, and D, Fire and Smoke: Detecting and characterizing the population of seed black how do they grow?
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Q3. How do supermassive black holes form and D, Fire: Measuring luminosity function of rapidly growing black holes in the first how is their growth coupled to the evolution of billion years.
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From page 421... ...
DA. "Industrial-scale" spectroscopy -- NOTE: CMB = cosmic microwave background; D = Science for which the mission is specifically designed; G = additional science to which the mission can make a Good contribution, but for which the mission is not specifically designed; GW = gravitational wave; NS = neutron star; S = additional science to which the mission can make a Strong contribution, but for which the mission is not specifically designed; TDA = time-domain astronomy.
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