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This article explores the evidence from astrophysics on heavy and light species of dark matter candidates, including SUSY WIMPs, sterile neutrinos, axions, fuzzy/ultralight dark matter, and primordial black holes.
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Astrophysical Evidence on Heavy and Light Species Annika Peter Center for Cosmology and AstroParticle Physics (CCAPP) The Ohio State University @HowWeScience on Instagram and Twitter
Whoooo are you…ooh ooh…ooh ooh From Alex’s talk US Cosmic Vision 2017
Whoooo are you…ooh ooh…ooh ooh 1067 eV 10-21 eV From Alex’s talk US Cosmic Vision 2017
By type of equations of motion:Do you behave like a SUSY WIMP Sterile neutrino Axions Fuzzy/ultralight DM Primordial black holes (MaCHOs)
By how it interacts with us and/or itself: Cold Dark Matter is: Not relativistic (stays put, unlike my child) Doesn’t interact with anyone or anything (unlike my child) Totally stable (sense a theme?)
By how it interacts with us and/or itself: “halo” Cold Dark Matter is: Not relativistic (stays put, unlike my child) Doesn’t interact with anyone or anything (unlike my child) Totally stable (sense a theme?) Halos all the way down… Image credit: V. Springel, MPA
By how it interacts with us and/or itself: Halo mass scale where CDM is a BAD fit Buckley & AP, 1712.06615 Low Interaction w/Standard Model High
By how it interacts with us and/or itself: Halo mass scale where CDM is a BAD fit Buckley & AP, 1712.06615 Low Interaction w/Standard Model High Lab + astrophysics
By how it interacts with us and/or itself Early-time effects (warmness, large de Broglie wavelength)—Halo abundance Late-time effects (decays, self-interactions)— Halo shape Halo mass scale where CDM is a BAD fit Buckley & AP, 1712.06615 Low Interaction w/Standard Model High Lab + astrophysics
By type of equations of motion:Do you behave like a Detection of individual objects
Whoooo are you…ooh ooh…ooh ooh 1067 eV 10-21 eV US Cosmic Vision 2017
Primordial black holes (PBH)/MaCHOs Paczynzki, Griest, Zel’dovich, Hawking Direct collapse to BH Bringmann, Scott, Akrami 1110.2484
Primordial black holes (PBH)/MaCHOs MACHO, EROS, OGLE Alcock+ 1993, Augbourg+ 1993 https://www.nature.com/articles/d41586-018-07006-8#ref-CR5
Primordial black holes (PBH)/MaCHOs MACHO, EROS, OGLE Alcock+ 1993, Augbourg+ 1993 https://www.nature.com/articles/d41586-018-07006-8#ref-CR5
Primordial black holes (PBH)/MaCHOs LIGO collaboration 2017
Primordial black holes (PBH)/MaCHOs Season 10/11 (after a LONG hiatus) LIGO collaboration 2017
Primordial black holes (PBH)/MaCHOs Carr(+), 1901.07803 (1607.06077) A good summary of issues in Anne Green’s Invisibles 2019 talk. The truth is out there. But see Montero-Camacho+ 1906.05950 (go Bucks!) for windows at asteroid mass
Thank U, Next From elephant to mouse
By type of equations of motion:Do you behave like a Collective action
By how it interacts with us and/or itself Astrophysics Halo mass scale where CDM is a BAD fit Buckley & AP, 1712.06615 Low Interaction w/Standard Model High Lab + astrophysics
Fuzzy dark matter Ultra-light dark matter (axions; e.g., Hu+ 2000, Hui+ 2016) m ~ 10-22 eV The larger the de Broglie wavelength, the bigger the core, and the fewer the small halos. Schive+ 2014 See talks by Kfir Blum, Scott Tremaine @2019 PCTS workshop
Fuzzy dark matter Requirements to make cores Wasserman+ 1905.10373: m= 3x10-22 eV Van Dokkum+ 2016 Dragonfly 44 Robles+ 1807.06018
Fuzzy dark matter Requirements to make enough satellites Segue I and ~50 of its Milky Way friends (image credit: M. Geha) Drlica-Wagner+ 2015 DES; see Pan-Starrs, ATLAS, HSC-SSP survey papers
Fuzzy dark matter Requirements to make enough satellites Segue I and ~50 of its Milky Way friends (image credit: M. Geha) Completeness Correction For the Milky Way Kim, AP & Hargis 1711.06267
Fuzzy dark matter Requirements to make enough satellites Segue I and ~50 of its Milky Way friends (image credit: M. Geha) Completeness Correction For the Milky Way Nadler+ 1904.10000: m> 3x10-21 eV 10x higher than what’s needed for cores. Kim, AP & Hargis 1711.06267
By how it interacts with us and/or itself Astrophysics Halo mass scale where CDM is a BAD fit Buckley & AP, 1712.06615 Low Interaction w/Standard Model High Lab + astrophysics
Axions and the Sun Sikivie 1983 http://www.int.washington.edu/talks/WorkShops/int_12_50W/People/Ruz_J/Ruz.pdf Good constraints because we know the physics of stars so well. From Drlica-Wagner+ LSST DM paper 1902.01055
Plain old WIMPs: main-sequence stars It’s a trap!: capture by elastic scattering. Energy injection (annihilation). Extra source of heat conduction (can be non-local).
Plain old WIMPs: main-sequence stars Everything old is new again. Galactic Center Asymmetric DM+ Sun First stars Lopes, Silk, Taoso Scott+ 0809.1871 Freese, Bromm, Gondolo… NASA/SDO Stacy+ 2013
Plain old WIMPs: compact objects Dark matter Neutron star
Plain old WIMPs: compact objects Dark matter Neutron star Bonk
Plain old WIMPs: compact objects Kinetic energy from dark matter means there’s a lower limit for temperature of thermal radiation from nearby neutron stars…a subject for JWST. Baryakhtar, Bramante, Li, Linden, Raj 1704.01577 Go Bucks!
Plain old WIMPs: be careful about interpretation See talk by Chris Cappiello (OSU) on Thursday Digman+ incl. AP, 1907.10618
Pathways to detection (Kerstin’s talk)
Takeaways for astrophysical measurement of dark matter physics
Astrophysicists’ particle classification Small de Broglie wavelength Big Early Universe behavior affects abundance of halos overdensity r Cold (non-relativistic) Warm Hot (relativistic) Early Universe---typical velocity at creation epoch (or de Broglie wavelength)
Astrophysicists’ particle classification Late-time effects on halo morphology Self –Interacting Dark Matter (Core collapse) Elbert+ incl. AP 1412.1477