Astrophysical Evidence on Heavy and Light Species

1. 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

2. Whoooo are you…ooh ooh…ooh ooh From Alex’s talk US Cosmic Vision 2017

3. Whoooo are you…ooh ooh…ooh ooh 1067 eV 10-21 eV From Alex’s talk US Cosmic Vision 2017

4. How do we classify dark matter candidates?

5. By type of equations of motion:Do you behave like a

6. By type of equations of motion:Do you behave like a SUSY WIMP Sterile neutrino Axions Fuzzy/ultralight DM Primordial black holes (MaCHOs)

7. 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?)

8. 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

9. 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

10. 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

11. 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

12. By type of equations of motion:Do you behave like a Detection of individual objects

13. Whoooo are you…ooh ooh…ooh ooh 1067 eV 10-21 eV US Cosmic Vision 2017

14. Primordial black holes (PBH)/MaCHOs Paczynzki, Griest, Zel’dovich, Hawking Direct collapse to BH Bringmann, Scott, Akrami 1110.2484

15. Primordial black holes (PBH)/MaCHOs MACHO, EROS, OGLE Alcock+ 1993, Augbourg+ 1993 https://www.nature.com/articles/d41586-018-07006-8#ref-CR5

16. Primordial black holes (PBH)/MaCHOs MACHO, EROS, OGLE Alcock+ 1993, Augbourg+ 1993 https://www.nature.com/articles/d41586-018-07006-8#ref-CR5

17. Primordial black holes (PBH)/MaCHOs LIGO collaboration 2017

18. Primordial black holes (PBH)/MaCHOs Season 10/11 (after a LONG hiatus) LIGO collaboration 2017

19. 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

20. Thank U, Next From elephant to mouse

21. By type of equations of motion:Do you behave like a Collective action

22. 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

23. Pathways to detection

24. 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

25. Fuzzy dark matter Requirements to make cores Wasserman+ 1905.10373: m= 3x10-22 eV Van Dokkum+ 2016 Dragonfly 44 Robles+ 1807.06018

26. 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

27. 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

28. 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

29. Unpopular opinion: Thank U, Next

30. 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

31. Pathways to detection

32. 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

33. Plain old WIMPs: main-sequence stars

34. 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).

35. 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

36. Plain old WIMPs: compact objects Dark matter Neutron star

37. Plain old WIMPs: compact objects Dark matter Neutron star Bonk

38. 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!

39. Plain old WIMPs: be careful about interpretation See talk by Chris Cappiello (OSU) on Thursday Digman+ incl. AP, 1907.10618

40. Pathways to detection (Kerstin’s talk)

41. Takeaways for astrophysical measurement of dark matter physics

42. 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)

43. Astrophysicists’ particle classification Late-time effects on halo morphology Self –Interacting Dark Matter (Core collapse) Elbert+ incl. AP 1412.1477