Heavy and Light Species Annika Peter Center for Cosmology and AstroParticle Physics CCAPP The Ohio State University HowWeScience on Instagram and Twitter Whoooo are youooh oohooh ooh ID: 791889
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Slide1
Astrophysical Evidence on
Heavy and Light Species
Annika PeterCenter for Cosmology and AstroParticle Physics (CCAPP)The Ohio State University@HowWeScience on Instagram and Twitter
Slide2Whoooo are you…ooh ooh…ooh ooh
US Cosmic Vision 2017
From Alex’s talk
Slide3Whoooo are you…ooh ooh…ooh ooh
US Cosmic Vision 2017
10-21 eV1067 eV
From Alex’s talk
Slide4How do we classify dark matter candidates?
Slide5By type of equations of motion:
Do you behave like a
Slide6By type of equations of motion:
Do you behave like a
Primordial black holes
(
MaCHOs
)
Axions
Fuzzy/ultralight DM
SUSY WIMP
Sterile neutrino
Slide7By how it interacts with us and/or itself:Cold Dark M
atter is:Not relativistic (stays put, unlike my child)Doesn’t interact with anyone or anything (unlike my child)Totally stable (sense a theme?)
Slide8By how it interacts with us and/or itself:Cold Dark M
atter is:Not relativistic (stays put, unlike my child)Doesn’t interact with anyone or anything (unlike my child)Totally stable (sense a theme?)
“halo”
Image credit: V. Springel, MPAHalos all the way down…
Slide9By how it interacts with us and/or itself:
Halo mass scale where CDM is a BAD fitBuckley & AP,1712.06615
Low Interaction w/Standard Model High
Slide10By how it interacts with us and/or itself:
Halo mass scale where CDM is a BAD fitBuckley & AP,1712.06615
Low Interaction w/Standard Model High
Lab + astrophysics
Slide11By how it interacts with us and/or itself
Halo mass scale where CDM is a BAD fitBuckley & AP,1712.06615
Low Interaction w/Standard Model High
Lab + astrophysicsEarly-time effects(warmness, large de Broglie wavelength)—Halo abundanceLate-time effects(decays, self-interactions)—Halo shape
Slide12By type of equations of motion: Do you behave like a
Detection of individual objects
Slide13Whoooo are you…ooh ooh…ooh ooh
US Cosmic Vision 2017
10-21 eV1067 eV
Slide14Primordial black holes (PBH)/MaCHOs
Bringmann, Scott, Akrami 1110.2484Direct collapse to BH
Paczynzki, Griest, Zel’dovich, Hawking
Slide15Primordial black holes (PBH)/MaCHOs
Alcock+ 1993, Augbourg+ 1993https://www.nature.com/articles/d41586-018-07006-8#ref-CR5
MACHO, EROS, OGLE
Slide16Primordial black holes (PBH)/MaCHOs
Alcock+ 1993, Augbourg+ 1993https://www.nature.com/articles/d41586-018-07006-8#ref-CR5
MACHO, EROS, OGLE
Slide17Primordial black holes (PBH)/MaCHOs
LIGO collaboration 2017
Slide18Primordial black holes (PBH)/MaCHOs
LIGO collaboration 2017
Season 10/11 (after a LONG hiatus)
Slide19Primordial black holes (PBH)/MaCHOs
Carr(+), 1901.07803 (1607.06077)
But see Montero-Camacho+ 1906.05950 (go Bucks!) for windows at asteroid massThe truth is out there.A good summary of issues in Anne Green’s Invisibles 2019 talk.
Slide20Thank U, NextFrom elephant to mouse
Slide21By type of equations of motion: Do you behave like a
Collective action
Slide22By how it interacts with us and/or itself
Halo mass scale where CDM is a BAD fitBuckley & AP,1712.06615
Low Interaction w/Standard Model High
Lab + astrophysicsAstrophysics
Slide23Pathways to detection
Slide24Fuzzy dark matter
Schive
+ 2014Ultra-light dark matter (axions; e.g., Hu+ 2000, Hui+ 2016) m ~ 10-22 eV
See talks by Kfir Blum, Scott Tremaine @2019 PCTS workshop The larger the de Broglie wavelength, the bigger the core, and the fewer the small halos.
Slide25Fuzzy dark matterRequirements to make cores
Robles+ 1807.06018
Van Dokkum+ 2016 Dragonfly 44
Wasserman+ 1905.10373:m= 3x10-22 eV
Slide26Fuzzy dark matterRequirements 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
Slide27Fuzzy dark matterRequirements to make enough satellites
Kim, AP & Hargis 1711.06267
Segue I and ~50 of its Milky Way friends(image credit: M. Geha)Completeness
CorrectionFor theMilky Way
Slide28Fuzzy dark matterRequirements to make enough satellites
Kim, AP & Hargis 1711.06267
Segue I and ~50 of its Milky Way friends(image credit: M. Geha)Completeness
CorrectionFor theMilky WayNadler+ 1904.10000:m> 3x10-21 eV10x higher than what’s needed for cores.
Slide29Unpopular opinion: Thank U, Next
Slide30By how it interacts with us and/or itself
Halo mass scale where CDM is a BAD fitBuckley & AP,1712.06615
Low Interaction w/Standard Model High
Lab + astrophysicsAstrophysics
Slide31Pathways to detection
Slide32Axions and the Sun
From Drlica-Wagner+ LSST DM paper 1902.01055Sikivie 1983
http://www.int.washington.edu/talks/WorkShops/int_12_50W/People/Ruz_J/Ruz.pdfGood constraints because we know the physics of stars so well.
Slide33Plain old WIMPs: main-sequence stars
Slide34Plain 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).
Slide35Plain old WIMPs: main-sequence starsEverything old is new again.
Galactic Center Asymmetric DM+ Sun First stars
Scott+ 0809.1871NASA/SDOLopes, Silk,
TaosoFreese, Bromm, Gondolo…Stacy+ 2013
Slide36Plain old WIMPs: compact objectsNeutron star
Dark matter
Slide37Plain old WIMPs: compact objectsNeutron star
Dark matter
Bonk
Slide38Plain 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.
Type equation here.
Baryakhtar, Bramante, Li, Linden, Raj 1704.01577Go Bucks!
Slide39Plain old WIMPs: be careful about interpretation
Digman+ incl. AP, 1907.10618See talk by Chris Cappiello (OSU) on Thursday
Slide40Pathways to detection
(Kerstin’s talk)
Slide41Takeaways for astrophysical measurement of dark matter physics
Slide42Astrophysicists’ particle classificationEarly Universe---typical velocity at creation epoch (or de Broglie wavelength)
Cold (non-relativistic) Warm Hot (relativistic)
r
overdensity
Early Universe behavior affects
abundance
of halos
Small de Broglie wavelength Big
Slide43Astrophysicists’ particle classificationLate-time effects on halo morphology
Self –Interacting Dark Matter
Elbert+ incl. AP 1412.1477(Core collapse)