The document discusses a physics colloquium presentation about dark matter. It begins with an outline comparing the talk to fictional stories of Superman. The talk then reviews evidence that dark matter exists from astronomical observations. Next, it discusses the status of the weakly interacting massive particle (WIMP) as a leading dark matter candidate. The talk provides historical context for the WIMP hypothesis from the 1990s and outlines several open questions in particle physics that a WIMP could potentially address, such as the hierarchy problem. It describes how supersymmetry is a favored theoretical framework that could explain a WIMP through the introduction of superpartner particles.
The overwhelming observational evidence for the existence of dark matter is only matched by the awkward scarcity of information about what it might actually be. Laboratory searches for dark matter now appear to exclude many of the "weakly interacting massive particle" models that were favored by particle physicists for decades. Where does that leave the hunt for dark matter? If we've left the WIMP behind, what are we looking for? We give a brief, biased, and largely fictional history of the WIMP in order to establish what has and has not been excluded, and why it matters.
This general-interest presentation grew out of discussions with astronomers who wanted to understand why some of their particle physics colleagues are "searching for WIMPs" while the others
have decided to live in a "post-WIMP world."
The overwhelming observational evidence for the existence of dark matter is only matched by the awkward scarcity of information about what it might actually be. Laboratory searches for dark matter now appear to exclude many of the "weakly interacting massive particle" models that were favored by particle physicists for decades. Where does that leave the hunt for dark matter? If we've left the WIMP behind, what are we looking for? We give a brief, biased, and largely fictional history of the WIMP in order to establish what has and has not been excluded, and why it matters.
This general-interest presentation grew out of discussions with astronomers who wanted to understand why some of their particle physics colleagues are "searching for WIMPs" while the others
have decided to live in a "post-WIMP world."
A preponderance of scientific evidence over the last hundred years tells us that our galaxy is filled with an unknown substance called dark matter. In fact, there is five times as much dark matter in the universe than there is ordinary matter: we are swimming in an ocean of dark matter and we have no firm idea what it is. We suspect that dark matter is composed of undiscovered elementary particles whose properties may, in turn, unlock some of the most pressing open questions in fundamental physics. So why haven't we figured out how to study dark matter in the lab, and why should we be optimistic that we may make progress in the coming decades?
Talk for the 26th Fr. Ciriaco Pedrosa, O.P. Memorial Lecture Series and 8th International Symposium on Mathematics and Physics at the University of Santo Tomas (Manila, Philippines). Presented remotely on Nov 26, 2021
USC Physics & Astronomy Colloquium, 22 Oct 2018. Laboratory searches for dark matter now exclude many of the “weakly interacting massive particle” models that were favored by particle physicists for decades. We discuss what this means for the theoretical and experimental frontier of particle physics and address what we really mean when we say “WIMP”.
Based on recent work on quantum gravity and the holographic principle I argue that, instead of thinking of the universe as a 'bubble out of nothing', we should think of space, time, and gravity as emerging 'out of information'.
Proceedings of a talk given at the American Translators Association's 53rd conference.
Abstract:
Recently, the news outlets were buzzing with excitement about the possible discovery of a new particle at the Large Hadron Collider (LHC). The LHC at CERN is not only the world's largest machine and fridge, but also home of the world’s largest international scientific collaborations, with several thousand scientists from over 100 different nations. As such, the underlying science may be of interest to linguists. This paper presents a basic overview over our current knowledge of the universe and aims at explaining the big fuss about the search for the Higgs (also known as the “God particle”) and its possible connection to dark matter. No knowledge of advanced mathematics or physics is required to read this paper. For readers who want to know more, some references and recommendations for further reading are included at the end.
Short introduction to the Standard Model of particle physics given at Maplesoft R&D group. Historical introduction of particle physics, introduction to the Higgs boson and the current state of the art techniques in particle physics.
Slides elaborated to illustrate the intervention of Mariano Artigas in the Summer School, June 10-15 2004: "The Impact of the Humanities on the Development of European Science", Venice (Italy). Organized by the Istituto Veneto di Scienze, Lettere ed Arti and the Galileo Chair of History of Science of the University of Padua.
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A preponderance of scientific evidence over the last hundred years tells us that our galaxy is filled with an unknown substance called dark matter. In fact, there is five times as much dark matter in the universe than there is ordinary matter: we are swimming in an ocean of dark matter and we have no firm idea what it is. We suspect that dark matter is composed of undiscovered elementary particles whose properties may, in turn, unlock some of the most pressing open questions in fundamental physics. So why haven't we figured out how to study dark matter in the lab, and why should we be optimistic that we may make progress in the coming decades?
Talk for the 26th Fr. Ciriaco Pedrosa, O.P. Memorial Lecture Series and 8th International Symposium on Mathematics and Physics at the University of Santo Tomas (Manila, Philippines). Presented remotely on Nov 26, 2021
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Whatever Happened to the WIMP of Tomorrow?
1. @ f l i p . t a n e d o CORNELL PHYSICS COLLOQUIUM
Whatever happened to the
WIMP of tomorrow?
Flip Tanedo
October 12, 2020
The Silver Age of Dark Matter
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Outline
… with my apologies to DC comics
Images: Cham & Whiteson We Have No Idea + The Guardian (Adam West Obituary), Johns Action Comics #858,
Moore Whatever Happened to the Man of Tomorrow, Jurgens et al, Superman: Reign of the Supermen
2
3. @ f l i p . t a n e d o CORNELL PHYSICS COLLOQUIUM 64
Outline
… with my apologies to DC comics
Images: Cham & Whiteson We Have No Idea + The Guardian (Adam West Obituary), Johns Action Comics #858,
Moore Whatever Happened to the Man of Tomorrow, Jurgens et al, Superman: Reign of the Supermen
3
4. @ f l i p . t a n e d o CORNELL PHYSICS COLLOQUIUM 64
Assumption for this talk: dark matter exists
Cham & Whiteson , We Have No Idea
4
And we know roughly how much there is
5. @ f l i p . t a n e d o CORNELL PHYSICS COLLOQUIUM 64
Astronomy and Cosmology tell us Dark Matter Exists
Images: Jeff Filippini (Berkeley Cosmology 2005), NASA APOD 2006, NASA WMAP
5
5%
27%
68%
Standard Model is not complete
ROTATION CURVES GRAVITATIONAL LENSING COSMIC MICROWAVE BACKGROUND
This talk: new particle(s)
Conservative assumption
could be other options
And we know roughly how much there is
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6
Evidence… looks like an astro talk
1. Rotation Curves
Rubin, Ford & Thonnard 1978
What we learn:
mass fraction
distribution
2. Cluster Dynamics
What we learn:
mass fraction
distribution
Zwicky 1937
3. Cluster Gas
What we learn:
mass fraction
distribution
~90% of the luminous
matter in a cluster is
hot gas
4. Strong Gravitational Lensing
What we learn:
mass fraction
distribution
5.Weak Gravitational Lensing
What we learn:
distribution
shape
structure
Dietrich et al. 2016
6. Cosmological Microlensing
What we learn:
mass fraction
smoothness
Lewis & Irwin 1996
Joachim Wambsganss
7. CMB Acoustic Peaks
What we learn:
ratio of DM/
collisional
matter
thermal history
Hinshaw et al. 2013
WMAP 9
SPT
ACT
odd-numbered peaks
boosted relative to even as
baryon fraction increases
8. Matter Power Spectrum
What we learn:
ratio of DM/
collisional
matter
thermal history
Chabanier et al. 2019
9. Large Scale Structure
What we learn:
ratio of DM/
collisional
matter
thermal history
Paul Angel, Tiamat Simulation
Excellent agreement
between simulations
and galaxy distribution
on the largest scales
10. Galaxy/Cluster Collisions
What we learn:
distribution
separation from
collisional
matter
self-interaction
NASA/Clowe et al. 2006
Difficult to explain
without
collisionless matter
11. Big Bang Nucleosynthesis
What we learn:
amount of
baryonic matter
PDG 2018
Remaining mystery:
lithium abundance
(but still need low
baryon fraction)
12. Local Stellar Motions
What we learn:
local dark
matter density
Buser 2000
Estimates:
ρDM ~ 0.3 GeV/cm3
~ 0.008 MSun/pc3
via Katie Mack (ACP Colloquium 2019)
6
Astronomy and Cosmology tell us Dark Matter Exists
7. @ f l i p . t a n e d o CORNELL PHYSICS COLLOQUIUM 64
Outline
… with my apologies to DC comics
Images: Cham & Whiteson We Have No Idea + The Guardian (Adam West Obituary), Johns Action Comics #858,
Moore Whatever Happened to the Man of Tomorrow, Jurgens et al, Superman: Reign of the Supermen
7
8. @ f l i p . t a n e d o CORNELL PHYSICS COLLOQUIUM 64
Present Status
8
Adapted from “Dewey Defeats Truman,” via history.com
originally from the St. Louis Globe-Democrat
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Hooper, CfA Colloquium: youtube.com/watch?v=j3Wmvijk70E 9
10. @ f l i p . t a n e d o CORNELL PHYSICS COLLOQUIUM 64
Weakly Interacting Massive Particle
10
how weak?
“weak” or eak?
W±
<latexit sha1_base64="smXTBkHfQl+094B8aAuLaVLnUvk=">AAAB7HicbVDLSgNBEOyNrxhfUY9eBoPgKeyKoMegF48R3CSQrGF2MpsMmccyMyuEJd/gxYMiXv0gb/6Nk2QPmljQUFR1090Vp5wZ6/vfXmltfWNzq7xd2dnd2z+oHh61jMo0oSFRXOlOjA3lTNLQMstpJ9UUi5jTdjy+nfntJ6oNU/LBTlIaCTyULGEEWyeF7cdeKvrVml/350CrJChIDQo0+9Wv3kCRTFBpCcfGdAM/tVGOtWWE02mllxmaYjLGQ9p1VGJBTZTPj52iM6cMUKK0K2nRXP09kWNhzETErlNgOzLL3kz8z+tmNrmOcibTzFJJFouSjCOr0OxzNGCaEssnjmCimbsVkRHWmFiXT8WFECy/vEpaF/XArwf3l7XGTRFHGU7gFM4hgCtowB00IQQCDJ7hFd486b14797HorXkFTPH8Afe5w+0eI6a</latexit>
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<latexit sha1_base64="smXTBkHfQl+094B8aAuLaVLnUvk=">AAAB7HicbVDLSgNBEOyNrxhfUY9eBoPgKeyKoMegF48R3CSQrGF2MpsMmccyMyuEJd/gxYMiXv0gb/6Nk2QPmljQUFR1090Vp5wZ6/vfXmltfWNzq7xd2dnd2z+oHh61jMo0oSFRXOlOjA3lTNLQMstpJ9UUi5jTdjy+nfntJ6oNU/LBTlIaCTyULGEEWyeF7cdeKvrVml/350CrJChIDQo0+9Wv3kCRTFBpCcfGdAM/tVGOtWWE02mllxmaYjLGQ9p1VGJBTZTPj52iM6cMUKK0K2nRXP09kWNhzETErlNgOzLL3kz8z+tmNrmOcibTzFJJFouSjCOr0OxzNGCaEssnjmCimbsVkRHWmFiXT8WFECy/vEpaF/XArwf3l7XGTRFHGU7gFM4hgCtowB00IQQCDJ7hFd486b14797HorXkFTPH8Afe5w+0eI6a</latexit>
<latexit sha1_base64="smXTBkHfQl+094B8aAuLaVLnUvk=">AAAB7HicbVDLSgNBEOyNrxhfUY9eBoPgKeyKoMegF48R3CSQrGF2MpsMmccyMyuEJd/gxYMiXv0gb/6Nk2QPmljQUFR1090Vp5wZ6/vfXmltfWNzq7xd2dnd2z+oHh61jMo0oSFRXOlOjA3lTNLQMstpJ9UUi5jTdjy+nfntJ6oNU/LBTlIaCTyULGEEWyeF7cdeKvrVml/350CrJChIDQo0+9Wv3kCRTFBpCcfGdAM/tVGOtWWE02mllxmaYjLGQ9p1VGJBTZTPj52iM6cMUKK0K2nRXP09kWNhzETErlNgOzLL3kz8z+tmNrmOcibTzFJJFouSjCOr0OxzNGCaEssnjmCimbsVkRHWmFiXT8WFECy/vEpaF/XArwf3l7XGTRFHGU7gFM4hgCtowB00IQQCDJ7hFd486b14797HorXkFTPH8Afe5w+0eI6a</latexit>
interacting
with what?
how
massive?
in what regime
is it particle-y?
11. @ f l i p . t a n e d o CORNELL PHYSICS COLLOQUIUM 64
Weakly Interacting Massive Particle
Cham & Whiteson We Have No Idea
11
electroweak
interactions
electroweak
Particles
electroweak
Mass
particle; certainly in
electroweak regime
definition
for this talk
why this
definition?
12. @ f l i p . t a n e d o CORNELL PHYSICS COLLOQUIUM 64
Defining the WIMP
Bertone & Hooper, “History of Dark Matter,” 1605.04909, RMP
12
original WIMP: neutrinos
… it turns out that they don’t work.
why this definition?
13. @ f l i p . t a n e d o CORNELL PHYSICS COLLOQUIUM 64
Outline
… with my apologies to DC comics
Images: Cham & Whiteson We Have No Idea + The Guardian (Adam West Obituary), Johns Action Comics #858,
Moore Whatever Happened to the Man of Tomorrow, Jurgens et al, Superman: Reign of the Supermen
13
14. @ f l i p . t a n e d o CORNELL PHYSICS COLLOQUIUM 64
A historical fiction about the WIMP
Whatever happened to the man of tomorrow?
14
… an imaginary story which told the
final tale of the Silver Age Superman and
his long mythology … Wikipedia 6/2019
actual history
grad students should cite this
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Particle Physics, circa 1990s
15
/ /
¯ / − /
¯ / /
/ −/
¯ / −
/
/
( ) ( )
fundamental forces
matter
particles
or something to explain
unitarity of WW scattering
?
Image: Stanford ATLAS website
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Particle Physicists
Cham and Whiteson, We Have No Idea
16
CMS
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17
Maximilien Brice, CERN via National Geographic (May 2012)
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D. Overbye, New York Times, 4 July 2012
18
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Known Unknowns in Particle Physics
1990s - 2020; incomplete list
Images: Cham and Whiteson, We Have No Idea
19
Why is the Higgs boson light?
Hierarchy Problem
Why is there more matter than antimatter?
Why is ϴYM small? Strong CP Problem
What is the origin of neutrino mass?
What is dark matter?
Missing Mass Problem
Other puzzles (possibly related to dark matter?)
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The Hierarchy Problem
FT, Quantum Diaries, “The Hierarchy Problem” (2012)
20
The Higgs has a
snowball’s chance in hell
of being 125 GeV.
(and yet here we are)
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One favorite answer: supersymmetry
See also extra dimensions, compositeness…
21
matter particle force particle
force particle matter particle
N E W PA R T I C L E S
V I S I B L E S T U F F
SUSY
22. @ f l i p . t a n e d o CORNELL PHYSICS COLLOQUIUM 64
How it works
Idealized version
22
a little bit of model-building required.
In practice:
It has been well known since lep that in order to pu
stop masses, me
t ⇠ 1 1.4 tev. Pushing the stop
The stops contribute not only to the Higgs quartic—
also to the soft mass m2
Hu
from loops of the form
+
24
tops contribute not only to the Higgs quartic—which we need to push the Hi
o the soft mass m2
Hu
from loops of the form
+
24
23. @ f l i p . t a n e d o CORNELL PHYSICS COLLOQUIUM 64
A little bit of patching up: R-Parity
Preventing proton decay
23
¯
d
ū
ē
d,ē
s,ē
b
4 1
Q
L
ū ū
by squarks. Arrows indicate helicity and should not be confused
Dirac spinors [14]. Tildes indicate superpartners while bars are
ticles into left-chiral fields in the conjugate representation.
ariation of this is to impose the above constraint using
PR = ( )3(B L)+2s
,
e spin of the field. Conservation of matter parity implies
e ( )2s
factor always cancels in any interaction term sin
h term has an even number of fermions. Observe tha
superpartner fields have R-parity 1. (This is simila
e diagrams assocaited with electroweak precision obser
e R-parity requires pair-production of superpartners,
rections cannot occur at tree-level and must come from
PR[ ordinary matter ] = +
PR[ superpartner ] = −
Added bonus:
lightest superpartner is stable.
?
24. @ f l i p . t a n e d o CORNELL PHYSICS COLLOQUIUM 64
The story so far: supersymmetry
Images: Cham and Whiteson, We Have No Idea
24
mh ?
!
Missing Mass
25. @ f l i p . t a n e d o CORNELL PHYSICS COLLOQUIUM 64
The story so far: supersymmetry
25
mh ?
SUSY New Particles
p+ stability
R-parity
?
Dark Matter ?
Missing Mass
26. @ f l i p . t a n e d o CORNELL PHYSICS COLLOQUIUM 64
The story so far: supersymmetry
26
mh ?
Dark Matter ?
Missing Mass
Weak scale mass ~100 GeV
Weak scale interaction strength GF
No additional parameters (roughly)
27. @ f l i p . t a n e d o CORNELL PHYSICS COLLOQUIUM 64
Ingredients for a model of dark matter?
Anticipating how the WIMP became larger than life
1. At least one new particle.
2. Mechanism to produce 𝜌DM.
3. Experimental viability.
4. Strategy to test the model.
27
?
Moore Whatever Happened to the Man of Tomorrow
28. @ f l i p . t a n e d o CORNELL PHYSICS COLLOQUIUM
28
Approx. 1 WIMP
per mug of coffee
~ GeV / cm3
29. @ f l i p . t a n e d o CORNELL PHYSICS COLLOQUIUM 64
Weakly-Interacting Massive Particle
29
mh ?
Dark Matter ?
Missing Mass
Weak scale mass ~100 GeV
Weak scale interaction strength GF
No additional parameters (roughly)
How much
dark matter?
30. @ f l i p . t a n e d o CORNELL PHYSICS COLLOQUIUM 64
How much dark matter is there?
30
1 10
equilibrium
time ~ mass / temp
[comoving]
number
density
SM
SM
SM
SM
=
… so there is
no dark matter
E Q U I L I B R I U M
A N N I H I L AT I O N
SM
SM
31. @ f l i p . t a n e d o CORNELL PHYSICS COLLOQUIUM 64
How much dark matter is there?
31
1 10
equilibrium
time ~ mass / temp
[comoving]
number
density
A N N I H I L AT I O N
SM
SM
H U B B L E
freeze out
32. @ f l i p . t a n e d o CORNELL PHYSICS COLLOQUIUM 64
The WIMP Miracle
Automatically obtain [almost] the correct abundance
32
c
a
p
t
u
r
e
annihilation
SM
SM
Z
“WEAK SCALE” MASS
WEAK
FORCE
annihilation
⌦ h2
⇠
0.1 pb
h annvi
“WEAK SCALE”
ANNIHILATION RATE
PRESENT
ABUNDANCE
expansion of universe
33. @ f l i p . t a n e d o CORNELL PHYSICS COLLOQUIUM 64
PHYSICS REPORTS
ELSEWIER Physics Reports 267 (1996) 195-373
Supersymmetric dark matter
Gerard Jungmana, Marc Kamionkowskib,“, Kim Griestd
aDepartment of Physics, syyacuse University, Syracuse, NY 13244, USA. jungman@npac.syr.edu,
bDepartment of Physics, Columbia University, New York, NY 10027, USA. kamion@phys.columbia.edu,
‘School of Natural Sciences, Institute for Advanced Study, Princeton, NJ 08540. USA,
aDepartment of Physics, University of California, San Diego, La Jolla, CA 92093, USA. kgriest@ucsd.edu
Received June 1995; editor: D.N. Schramm
Contents
1. Introduction 198 6.4. Fermion final states 252
Supersymmetric WIMP Bible
33
34. @ f l i p . t a n e d o CORNELL PHYSICS COLLOQUIUM 64
The story so far: supersymmetry
34
mh ?
SUSY New Particles
p+ stability
R-parity
?
Dark Matter
with correct
abundance !
35. @ f l i p . t a n e d o CORNELL PHYSICS COLLOQUIUM 64
The story so far: extra dimensions
35
mh ?
Extra
Dimensions
New Particles
precision
observables
KK-parity
?
Dark Matter
with correct
abundance !
free in
flat XD
warped
extra dim.
36. @ f l i p . t a n e d o CORNELL PHYSICS COLLOQUIUM 64
The story so far: composite Higgs
36
mh ?
composite New Particles
precision
observables
T-parity
?
Dark Matter
with correct
abundance !
37. @ f l i p . t a n e d o CORNELL PHYSICS COLLOQUIUM 64
The general story
37
mh ?
new symmetry New Particles
precision
observables
new parity
?
Dark Matter
with correct
abundance !
38. @ f l i p . t a n e d o CORNELL PHYSICS COLLOQUIUM 64
A great love story
Andrew Grant, Science News, June 2013
38
39. @ f l i p . t a n e d o CORNELL PHYSICS COLLOQUIUM 64
What is a model of dark matter?
Ingredients
1. At least one new particle.
2. Mechanism to produce 𝜌DM.
3. Experimental viability.
4. Strategy to test the model.
39
?
40. @ f l i p . t a n e d o CORNELL PHYSICS COLLOQUIUM 64
The general story
40
mh ?
new symmetry New Particles
precision
observables
new parity
?
Dark Matter
with correct
abundance !
predictions
no
more
free
parameters
41. @ f l i p . t a n e d o CORNELL PHYSICS COLLOQUIUM 64
WIMP Complementarity
41
χ
χ
χ χ χ
χ
A
N
N
I
H
I
L
ATION
D
I
RECT DETECTIO
N
COLLIDER
Ωχh2
INDIRECT DIRECT COLLIDER
telescopes underground high energy
& abundance
Dark matter searches related by crossing symmetry
42. @ f l i p . t a n e d o CORNELL PHYSICS COLLOQUIUM
Direct Detection
Underground,
high-volume,
high-sensitivity.
Recoil of dark matter off nuclei
via LUX-LZ (kipac.stanford.edu/research/topics/direct-dark-matter-detection)
43. @ f l i p . t a n e d o CORNELL PHYSICS COLLOQUIUM 64
PDG Dark Matter Review 2018
43
Figure 27.1: WIMP cross sections (normalized to a single nucleon) for spin-
direct detection
44. @ f l i p . t a n e d o CORNELL PHYSICS COLLOQUIUM 64
PDG Dark Matter Review 2018
44
Figure 27.1: WIMP cross sections (normalized to a single nucleon) for spin-
weak scale coupling
weak scale mass
45. @ f l i p . t a n e d o CORNELL PHYSICS COLLOQUIUM 64
A great love story . . . and a break up
45
46. @ f l i p . t a n e d o CORNELL PHYSICS COLLOQUIUM 64
WIMP Complementarity
46
χ
χ
χ χ χ
χ
A
N
N
I
H
I
L
ATION
D
I
RECT DETECTIO
N
COLLIDER
2
INDIRECT
Standard Model
Dark Matter
WEAK FORCE
W I M P M I R AC L E YO U ’ R E K I L L I N G M E N OT G R E AT, E I T H E R
DIRECT COLLIDE
47. @ f l i p . t a n e d o CORNELL PHYSICS COLLOQUIUM 64
A great love story . . . and a break up
47
48. @ f l i p . t a n e d o CORNELL PHYSICS COLLOQUIUM 64
Are WIMPs dead?
48
49. @ f l i p . t a n e d o CORNELL PHYSICS COLLOQUIUM 64
Are WIMPs dead?
49
(Like asking “is SUSY dead?”)
Technically? No.
Linguistically? No.
Experimentally? No.
Emotionally? Yes.
The WIMP is dead to me.
“weak” vs “electroweak”
Experimental program is robust!
ways to ‘hide’ a
neutralino-esque WIMP
This is the wrong question!
50. @ f l i p . t a n e d o CORNELL PHYSICS COLLOQUIUM 64
The general story
50
mh ?
new symmetry New Particles
precision
observables
new parity
?
Dark Matter
with correct
abundance !
predictions
no
more
free
parameters
51. @ f l i p . t a n e d o CORNELL PHYSICS COLLOQUIUM 64
The general story
51
mh ?
new symmetry New Particles
precision
observables
new parity
?
Dark Matter
with correct
abundance !
predictions
no
more
free
parameters
52. @ f l i p . t a n e d o CORNELL PHYSICS COLLOQUIUM 64
Known Unknowns in Particle Physics
1990s - 2020; incomplete list
Images: Cham and Whiteson, We Have No Idea
52
Why is the Higgs boson light?
Hierarchy Problem
Why is there more matter than antimatter?
Why is ϴYM small? Strong CP Problem
What is the origin of neutrino mass?
What is dark matter?
Missing Mass Problem
Other puzzles (possibly related to dark matter?)
53. @ f l i p . t a n e d o CORNELL PHYSICS COLLOQUIUM 64
Outline
… with my apologies to DC comics
Images: Cham & Whiteson We Have No Idea + The Guardian (Adam West Obituary), Johns Action Comics #858,
Moore Whatever Happened to the Man of Tomorrow, Jurgens et al, Superman: Reign of the Supermen
53
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54
Chris Burden, Urban Light, 2008, Los Angeles County Museum of Art; photo courtesy of @neohumanity via Instagram
Have we been looking under the wrong lamp-post?
1. At least one new particle.
2. Mechanism to produce 𝜌DM.
3. Experimental viability.
4. Strategy to test the model.
55. @ f l i p . t a n e d o CORNELL PHYSICS COLLOQUIUM 64
The Elephant in the Room
The abundance of dark matter
55
How did it get here?
Why is it still here?
56. @ f l i p . t a n e d o CORNELL PHYSICS COLLOQUIUM 64
Recap: WIMP Miracle
56
mh ?
new symmetry New Particles
new parity
?
dangerous
processes
Dark Matter !
How did it get here?
Why is it still here?
57. @ f l i p . t a n e d o CORNELL PHYSICS COLLOQUIUM 64
A phenomenological approach
How do we cast the widest net?
57
Dark Matter
with correct
abundance
predictions
UV theory?
pheno.
theory
start here
What is the theory of dark matter?
Explore broad possibilities without top-
down theory prejudice.
How do we discover dark matter?
On a budget! Using the experiments and
telescopes that we have.
58. @ f l i p . t a n e d o CORNELL PHYSICS COLLOQUIUM 64
A phenomenological approach
How do we cast the widest net?
58
Dark Matter
with correct
abundance
predictions
Fix couplings
How’d it
get here?
Why is it
still here?
new particles
UV theory?
pheno.
theory
start here
What is the theory of dark matter?
Explore broad possibilities without top-
down theory prejudice.
How do we discover dark matter?
On a budget! Using the experiments and
telescopes that we have.
59. @ f l i p . t a n e d o CORNELL PHYSICS COLLOQUIUM 64
Example: Dark Sector with Light Mediator
Non-WIMP lamp-post
59
e
e
e
e
e
e
e
e
e e
capture
a
n
n
i
h
i
l
a
t
i
o
n
x x
A0
A0
INDIRECT DIRECT COLLIDER
Standard Model
Mediator
N N
q
q
A
N
N
I
H
I
L
ATION
COLLIDER
D I R E C T
Dark Matter
Halo Morpholo
• SIDM particles follow the
0 2 4 6 8
0
2
4
6
8
R HkpcL
z
HkpcL
constant density contours
Kaplinghat, Linden, Keeley, HBY (2013) (PR
Co
dis
SELF
60. @ f l i p . t a n e d o CORNELL PHYSICS COLLOQUIUM 64
e.g. Earth capture of dark matter
Not possible with neutralinos
J. Feng, J. Smolinsky, FT 1509.07525, 1602.01465, 1701.03168 ; A. Green, FT 1808.03700
60
1
2
3 4
61. @ f l i p . t a n e d o CORNELL PHYSICS COLLOQUIUM 64
e.g. Holographic Dark Sectors
Non-minimal mediators
Brax, Fichet, Tanedo 10906.02199; Costantino, Fichet, Tanedo 19010.02972
61
62. @ f l i p . t a n e d o CORNELL PHYSICS COLLOQUIUM
62
Chris Burden, Urban Light, 2008, Los Angeles County Museum of Art; photo courtesy of @neohumanity via Instagram
Have we been looking under the wrong lamp-post?
non-thermal production
complicated dark sectors
decaying dark matter
macroscopic dark matter lumps
primordial black holes
axions, ultralight dark matter
gravity is very weird
many other possibilities…
1. At least one new particle.
2. Mechanism to produce 𝜌DM.
3. Experimental viability.
4. Strategy to test the model.
63. @ f l i p . t a n e d o CORNELL PHYSICS COLLOQUIUM 64
Big Picture: why this matters
More interdisciplinary than ever
Hunt for dark matter is multi-frontier. Each
sub-community has its own jargon.
WIMP is jargon whose meaning has drifted to
mean something slightly different to different
people.
This gets in the way of seeing why certain
ideas were well-motivated, and why/how we
are moving beyond them.
US particle physics community’s decadal strategic planning process: snowmass21.org
63
64. @ f l i p . t a n e d o CORNELL PHYSICS COLLOQUIUM 64
Thanks
Csáki group, September 2012; Photo Courtesy of Cornell
64