POEMMA POEMMA: Probe of Extreme : Probe of Extreme Multi-Messenger Astrophysics Multi-Messenger Astrophysics Angela V. Olinto � ICRC 2017:18 July �
NASA Probe Studies for 2020 Decadal Survey - NASA funding 10 Probe Class (below 1B$) Mission (18 mos) Studies in PreparaAon for the 2020 Decadal Survey - PI responsible for the final report (due NLT Dec 2018) - NASA will submit these studies to the Decadal Survey - Decadal Survey CommiLee will have the opAon to prioriAze any of these mission concepts, or recommend a competed line of Probes (similar to Explorers) - SelecAon based on Science Merit (cost, schedule) POEMMA POEMMA
POEMMA Study Collaboration � POEMMA Study Collaboration University of Chicago: Angela V. Olinto (PI) NASA/MSFC: Mark J. Christl (deputy PI), Roy M. Young, Peter Bertone NASA/GSFC: John W. Mitchell, John Krizmanic, Jeremy S Perkins, Julie McEnery, Elizabeth Hays, Floyd Stecker, Stan Hunter, Jonathan Ormes, Robert StreitmaLer University of Utah: Doug Bergman, John MaLhews University of Alabama, Huntsville: James Adams, Patrick Reardon, Evgeny Kuznetsov, Malek Mastafa Colorado School of Mines: Lawrence Wiencke, Frederic Sarazin City University of New York, Lehman College: Luis Anchordoqu, Thomas C. Paul Georgia InsAtute of Technology: A. Nepomuk OLe Space Sciences Laboratory, University of California, Berkeley: Eleanor Judd University of Iowa: Mary Hall Reno Jet Propulsion Laboratory: Insoo Jun, L. M. MarAnez-Sierra Vanderbilt University: Steven E Csorna APC Univerite de Paris 7: EAenne Parizot, Guillaume Prevot Universita di Torino: Mario Edoardo Bertaina, Francesco Fenu, Kenji Shinozaki University of Geneva: Andrii Neronov Gran Sasso Science InsAtute: Roberto Aloisio Scientists from16+ institutions from Scientists from16+ institutions from � OWL, JEM-EUSO, Auger, TA, OWL, JEM-EUSO, Auger, TA, Veritas Veritas, CTA, Fermi, Theory , CTA, Fermi, Theory �
POEMMA Study Collaboration � POEMMA Study Collaboration University of Chicago: Angela V. Olinto (PI) NASA/MSFC: Mark J. Christl (deputy PI), Roy M. Young, Peter Bertone NASA/GSFC: John W. Mitchell, John Krizmanic, Jeremy S Perkins, Julie McEnery, Elizabeth Hays, Floyd Stecker, Stan Hunter, Jonathan Ormes, Robert StreitmaLer University of Utah: Doug Bergman, John MaLhews University of Alabama, Huntsville: James Adams, Patrick Reardon, Evgeny Kuznetsov, Malek Mastafa Colorado School of Mines: Lawrence Wiencke, Frederic Sarazin City University of New York, Lehman College: Luis Anchordoqu, Thomas C. Paul Georgia InsAtute of Technology: A. Nepomuk OLe Space Sciences Laboratory, University of California, Berkeley: Eleanor Judd University of Iowa: Mary Hall Reno Jet Propulsion Laboratory: Insoo Jun, L. M. MarAnez-Sierra Vanderbilt University: Steven E Csorna APC Univerite de Paris 7: EAenne Parizot, Guillaume Prevot Universita di Torino: Mario Edoardo Bertaina, Francesco Fenu, Kenji Shinozaki University of Geneva: Andrii Neronov Gran Sasso Science InsAtute: Roberto Aloisio Space Missions can address the Flux Challenges Space Missions can address the Flux Challenges �
Ultra-High Energy Cosmic Ray Flux � knee 1 km -2 yr - 1 0.1 km -2 1 m -2 yr -1 century - 1 ankle Space Missions Space Missions � can address the can address the � Flux Challenges Flux Challenges �
Ultra-High Energy Cosmic Ray Flux � Particle Astronomy Starts Here � Particle Astronomy Starts Here knee 1 km -2 yr - 1 0.1 km -2 1 m -2 yr -1 century - 1 ankle Space Missions � Space Missions can address the � can address the Flux Challenges Flux Challenges �
Cosmogenic Neutrinos � IceCube HESE IceCube ν μ Space Missions Space Missions � can address the can address the � Flux Challenges Flux Challenges � Kotera, AVO arXiv: 1101.4256 arXiv:1009.1382
Extensive Air- shower Fluorescence � from SPACE � JEM-EUSO on the � Japanese Experiment Module � OWL � 2002 EUSO: � design � Extreme Universe Space Observatory � 8 8
Cosmogenic Neutrinos � CHANT CHANT
To Address open ques9ons: What objects can accelerate par9cles to ~ 10 20 eV? How are they distributed in the sky? How does the composi9on of UHECRs evolve at the highest energies? How strong are magne9c fields in the intergalac9c medium? What is the flux of cosmogenic neutri nos? POEMMA: POEMMA: � Probe of Extreme Multi-Messenger Astrophysics Probe of Extreme Multi-Messenger Astrophysics
To Address open ques9ons: What objects can accelerate par9cles to ~ 10 20 eV? How are they distributed in the sky? How does the composi9on of UHECRs evolve at the highest energies? How strong are magne9c fields in the intergalac9c medium? What is the flux of cosmogenic neutrinos ? Need to discover anisotropies in the UHECR sky distribuCon; measure spectrum and composiCon of UHECR accurately above 50 EeV, and detect cosmogenic neutrinos POEMMA: POEMMA: � Probe of Extreme Multi-Messenger Astrophysics Probe of Extreme Multi-Messenger Astrophysics
To Address open ques9ons: What objects can accelerate par9cles to ~ 10 20 eV? How are they distributed in the sky? How does the composi9on of UHECRs evolve at the highest energies? How strong are magne9c fields in the intergalac9c medium? What is the flux of cosmogenic neutrinos ? Need to discover anisotropies in the UHECR sky distribuCon; measure spectrum and composiCon of UHECR accurately above 50 EeV, and detect cosmogenic neutrinos => Need for substanAal increase in staAsAcs [10 x ground] UHECRs (E ≥ 10 EeV) substanAal [100 x ground] increase in UHECR X max shower maximum (X max ) resoluAon (below ~ 20 g/cm 2 ) full sky coverage with 1 observatory small angular resoluAon (~ 1 o ) Cherenkov monitoring Earth’s horizon to observe tau neutrinos POEMMA: POEMMA: � Probe of Extreme Multi-Messenger Astrophysics Probe of Extreme Multi-Messenger Astrophysics
POEMMA: POEMMA: � Probe of Extreme Multi-Messenger Astrophysics Probe of Extreme Multi-Messenger Astrophysics 2 formaAon-flying spacecraq (OWL concept) f/1 Schmidt camera, 45° FoV, Detailed design being defined – OWL scaling: 10 m diam. primary mirror deployable (OWL: 7m) 4.3 m diam. corrector lens 8 m 2 focal plane with ~500,000 pixels (~ 0.06 O pixel ~1 km 2 projected on the ground at 1,000km alAtude) 14 m 2 effecAve aperture (OWL: 7.07 m 2 ) weight TBD ~2400 kg; power consumpAon TBD ~600 W * *100 Ames fluorescence Aperture
OWL Mechanical Design Rodger Farley et al., NASA GSFC
POEMMA Mechanical Design �
Large Reflectors POEMMA � JWST � Realizing Large Structures in Space - Jeremy A. Banik, 9/2015
POEMMA Mission Design � Science priorities � Orbits from 525 to 1000 km alAtude, inclin 28.5 o UHECR cross-calibraAon with ground UHECR sky map, composiAon above 10 EeV UHECR flux at 100 EeV Below limb: Tau decay search Above limb: horizontal showers
JEM-EUSO Program
EUSO-SPB1: EUSO-SPB1: � Extreme Universe Space Observatory Extreme Universe Space Observatory � on a Super Pressure Balloon on a Super Pressure Balloon �
Cherenkov detector* *(possibly with SiPM)
POEMMA: Probe of Extreme POEMMA: Probe of Extreme Multi-Messenger Astrophysics Multi-Messenger Astrophysics 45 o � POEMMA POEMMA FoV FoV 45 Altitude: 525 Altitude: 525–1000km 1000km � radius ground Circle Nadir: 200-400 km radius ground Circle Nadir: 200-400 km � Tilt to Limb distance: 2640-3700 km Tilt to Limb distance: 2640-3700 km �
� � POEMMA Nadir: Nadir: � Limb: Limb: � Radius Radius 200-400 km 200-400 km � Radius Radius 2.6-3.7 10 2.6-3.7 10 3 km km �
POEMMA � Yearly UHE proton exposure for 10% duty cycle �
UHECR Exposure History � today
Cosmogenic Neutrinos POEMMA POEMMA
POEMMA: POEMMA: � TO Explain the TO Explain the � Extreme Multi-Messenger Extreme Multi-Messenger � Universe from Space Universe from Space
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