Dark Matter

The Dark Matter

Ali ÖVGÜN

Sections

 1. Dark Matter and WIMPs
(now)

 2. f(R) Gravity and its relation to the
interaction between DE and DM
(next time)

Title
Dark Energy 73%
(Cosmological Constant)

Neutrinos
Ordinary Matter 4% 0.1-2%
(of this only about Dark Matter
10% luminous) 23%

Mass and Gravity
 All mass has gravity.
 Gravity attracts all things with mass.
 Kepler’s Third Law tells us how mass
moves due to gravity.
 Use Kepler’s Third Law to find out how
much mass is where.

Mass and Luminosity

 Most mass gives off light.
 Amount of light tells how much mass is
present.
 Where there’s more light, there is more
mass.
 More light from galaxy centers vs. edges.
 Conclude more mass in center vs. edges.

Dark Matter
 Look at:
 Our galaxy.
 Other galaxies.
 Pairs of galaxies.
 Clusters of galaxies.
 Mass due to gravity.
 Mass indicated by luminosity.
 Same?
 No!  Dark Matter.

Evidence for Dark Matter
Use the fact that massive objects, even if they emit no light,
exert gravitational forces on other massive objects.

m1
r12
m2

Study the motions (dynamics) of visible objects like stars
in galaxies, and look for effects that are not explicable by
the mass of the other light emmitting or absorbing objects
around them.

Sun’s Rotation Speed Around
Milky Way
 In the milky way, all stars rotates around the
center of the galaxy
 According to Newton’s gravitational theory，the
rotation speed of the sun depends on the mass
distribution and the distance to the center

According to this formula, the
Rotation speed of the sun
Shall be around 170km/s, however r
The actual speed is about 220 v(r)
-250km/s.

What do we see?
 From variable stars we know distances.
 From Doppler shift we know rotation
velocity.

 Edges of Milky Way go too fast.
 Must be extra mass near edges of galaxy.

Rotation Curves
 If HI gas is rotating or moving, the
21cm radiation will be Doppler Shifted.

More Galaxy Masses
 Apply Kepler’s Laws to galaxy pairs.
 Get mass due to gravity.
 Look at total light from both galaxies.
 Estimate mass from luminous objects.

Evidences — galaxy scale
GM ( r )
v circ 
 From the Kepler’s law, r for r much
larger than the luminous terms, you should have v∝r-1/2
However, it is flat or rises slightly.

The most direct
evidence of the
existence of dark
matter.

Corbelli & Salucci (2000);
Bergstrom (2000)

Here’s one simple way to
mass a galaxy

Mass of galaxy = number of stars x average mass of star

It turns out that galaxies do not have enough
visible mass to stay grouped in clusters. The
extra mass they need must come from dark
matter.

Galaxy Rotation
 Objects in the disk,
orbit in the disk.
 Kepler’s Third Law
gives the total mass
in orbits.
3
Separation ( AU )
Period ( yrs ) 
2

Total Mass

 Basically, it states that the square of the
time of one orbital period (T2) is equal to
the cube of its average orbital radius
(R3). (1 AU = 150,000,000 km)

Distributed Mass
 In Kepler’s Law, the total mass is the
mass “inside” the orbit.

What should we expect?
 Solar System:
Planet Separation Velocity
(AU) (km/s)
Mercury 0.5 48
+
Earth 1 30

Saturn 10 10 V

Pluto 40 5 D

Even More Galaxy Masses
 Look for gravitational lenses near galaxy clusters.
 More lensing means more mass.

 Compare mass from lensing to luminosity.

Dark Matter content in a
galaxy
 This implies the existence of a dark halo, with mass
density
ρ(r) ∝ 1/r2, i.e., M(r) ∝ r;
 At some point ρ will have to fall off faster (in order
to keep the total mass of the galaxy finite), but we
do not know at what radius this will happen.
 This leads to a lower bound on the DM mass density,
ΩDM>∼0.1,
where ΩX ≡ ρ /ρcrit, ρcrit being the critical mass
X

density to be described later (i.e., Ωtot = 1)

Local Dark Matter Density
 The DM density in the ―neighborhood‖ of our solar
system was first estimated as early as 1922 by J.H.
Jeans, who analyzed the motion of nearby stars
transverse to the galactic plane. He concluded that in
our galactic neighborhood, the average density of DM
must be roughly equal to that of luminous matter
(stars, gas, dust).
 Remarkably enough, the most recent estimates, based
on a detailed model of our galaxy, find quite similar
results
ρlocal DM = 0.3 GeV/cm3;
This value is known to within a factor of two or so.

DM content from clusters of galaxies

 The observation of clusters of galaxies tends to give
somewhat larger values, ΩDM 0.2 to 0.3.
 These observations include measurements of
 the peculiar velocities of galaxies in the cluster, which are a
measure of their potential energy if the cluster is virialized;
 measurements of the X-ray temperature of hot gas in the
cluster, which again correlates with the gravitational
potential felt by the gas; and—most directly—
 studies of (weak) gravitational lensing of background galaxies
on the cluster.

Rotation of Stars around Galactic
Centres
We can measure how fast stars rotate around galactic
centres by looking at the frequency shift of known spectral
lines originating in the stars due to the Doppler effect.

Star’s motion towards you, relative to the
galactic centre alters wavelength of light

21 cm Radiation as Tracer
of Gas Clouds

21 cm map of our Galaxy

The Correct Way to Think
about Our Galaxy

RECESSIONAL VELOCITIES

Hubble (1929)
 The original evidence
that the universe is
expanding

 Now carried out to far
larger distances with
supernovae

 Constrains the
acceleration of
expansion:
WL - WM
“Attractive matter vs.
repulsive dark energy”

COSMIC MICROWAVE BACKGROUND

• dT/T << 1: The
universe is isotropic
and homogeneous on
large scales

• Constrains the
geometry of the
universe:
WL + WM
“total energy density”

BIG BANG NUCLEOSYNTHESIS
• At T ~ 1 MeV, the universe
cooled enough for light
elements to start forming

• The abundance of each light
species is fixed by h, the
baryon-to-photon ratio

• These determinations are
consistent* and constrain
(with the CMB) the density in
baryons: WB
Fields, Sarkar, PDG (2002)

SYNTHESIS
• Remarkable agreement

Dark Matter: 23% ± 4%
Dark Energy: 73% ± 4%
Baryons: 4% ± 0.4%
[ns: 0.2% for Sm = 0.1 eV]

• Remarkable precision
(~10%)

• Remarkable results

Question:
Is the mass in the universe all observable through
emmission or absorbsion of electromagnetic radiation ?

Dark Matter
...is matter that does not shine or absorb light, and has
therefore escaped direct detection by electromagnetic
transducers like telescopes, radio antennas, x-ray satellites...

It turns out that there is strong
experimental evidence that there is more
than 4 times as much dark matter as
luminous matter in the observable universe

Possible Dark-Matter Candidates

What is it?
 Dark Matter: Ordinary or Extraordinary?
 What kind of ordinary matter is dark?
 Black holes
 Black dwarfs (cool white dwarfs)
 Brown Dwarfs (failed stars)
 Planets
 Bowling Balls

Nature of the dark matter—Hot
or cold

 Hot dark matter is relativistic at the collapse epoch and
free-streaming out the galaxy-sized over density. Larger
structure forms early and fragments to smaller ones.
 Cold DM is non-relativistic
at de-coupling, forms
structure in a hierarchical,
bottom-up scenario.
 HDM is tightly bound from
observation and LSS forma-
tion theory

What we learned

In the universe there exists non-
baryonic, non-hot, dark matter

What Could Constitute the Dark Matter (1)?
IDEA 1 : Rocks

-from pebbles to giant planets like Jupiter.
If there are enough of them, they could make
up the dark matter.

Jupiter-size and above planets are a serious contender,
and are called MACHOs by the community - MAssive
Compact Halo Objects.

IDEA 2: Neutrinos

Light, neutral particles of which at least some have a small
mass. Produced in enormous numbers in stars and possibly
at the big bang. If there are enough of them, they could
(maybe) be the dark matter.

What Could Constitute the Dark Matter (2) ?

IDEA 3: Black Holes

Don’t emit significant amounts of light, can be
very massive. Would need lots of them.

IDEA 4: Cosmic Strings

Dense filamentary structures that some theorists think
could thread the universe, giving rise to its present-
day lumpiness. Currently disfavoured by cosmological data,
but may come back into vogue sometime.

What Could Constitute the Dark Matter (3) ?
IDEA 5: Axions

Very light particles, mass around 1/1,000,000,000,000
of an electron. Needed for building most realistic models
of the neutron from standard model particle physics. Not
detected. To be the dark matter, there should be around
10,000,000,000,000 per cubic centimetre here on Earth.

IDEA 6: WIMPS (for the rest of this talk)

Particles having mass roughly that of an atomic nucleus,
could be as light as carbon or as heavy as 7 nuclei of xenon.
Need a few per litre to constitute dark matter. Unlike nucleus,
only interact WEAKLY with other matter, through the same
mechanism that is responsible for nuclear beta-decay.

DARK MATTER
Known DM properties

• Gravitationally
interacting
• Not short-lived
• Not hot
• Not baryonic

Unambiguous evidence for new particles

DARK MATTER CANDIDATES
 There are many

 Masses and interaction
strengths span many,
many orders of
magnitude, but the
gauge hierarchy
problem especially
motivates Terascale
masses

HEPAP/AAAC DMSAG Subpanel (2007)

MOND
 In 1983, Milgrom proposed a modified Newtonian
dynamics in which F=ma is modified to F=maµ, which µ
is 1 for large acceleration, becomes a/a0 when a is
small.

 To explain the rotational curve, one can choose

Problems with MOND
 Cannot fit into a framework consistent
with GR.
 Hard to describe the expansion history,
therefore the CMB fluctuation and
galaxy distribution.
 Hard to explain the bullet cluster.
 No MOND can explain all gravitational
anomalies without introducing DM.

From particle physics

WIMP(Weakly interacting massive
particles)

is a natural dark matter candidate giving
correct relic density

Dark Matter Content
 The currently most accurate determination of ΩDM
comes from global fits of cosmological parameters to
a variety of observations: the anisotropy of CMB and
of the spatial distribution of galaxies, one finds a
density of cold, non–baryonic matter
Ωnbmh2 = 0.106 ± 0.008
where h is the Hubble constant in units of 100
km/(s·Mpc).
 Some part of the baryonic matter density,
Ωbh2 = 0.022 ± 0.001
may well contribute to (baryonic) DM, e.g., MACHOs
or cold molecular gas clouds

Matter Formation in the Big
Bang
 Start with hot dense “soup” of elementary particles and
radiation
 Expand, cool, “freeze out”

 Predictions for light element abundance
 Cosmic microwave background

 Strict upper bound on baryon content
 Evidence for non-baryonic dark matter

Agreement on the Numbers:
 Gravitational Lensing provides additional
graphic evidence for dark matter

 All techniques converge:
 3% luminous conventional matter
 14% dark conventional matter
 83% non-baryonic dark matter

WIMP hypothesis
 Weakly Interacting Massive Particle

 WIMPs freeze out early as the universe expands
and cools

 WIMP density at freeze-out is determined by the
strength sx of the WIMP interaction with normal
matter

 Leads to sx ~ sweak interaction

What we DO NOT know…
 The WIMP mass Mx
 prejudice 10<Mx<10000 Gev/c2

 The WIMP Interaction Cross-Section
 Prejudice s~sweak
 (give or take several orders or magnitude…)

 The nature of the interaction
 Spin coupling?
 Atomic Number coupling?

earth, air, baryons, ns,
fire, water dark matter,
dark energy

 We live in interesting times: we know how much there is,
but we have no idea what it is

 Precise, unambiguous evidence for new particle physics

Dark Matter Production

 2.1. Thermal Production
 WIMPs and many other dark matter
candidates are in thermal equilibrium in
the early universe and decouple once
their interactions become too weak to
keep them in equilibrium.
Those particles are called thermal relics

 As their density today is determined by
the thermal equilibrium of the early
universe. When the annihilation
processes of WIMPs into SM parti-
cles and vice versa happend at equal
rates, there is a equilibrium abundance.

 When the Universe cooled down and
the rate of expansion of the universe H
exceeds the annihilation rate,
the WIMPs effectively decouple from
the remaining SM particles.So the
equilibrium abundance drops
exponentially until the freeze-out
point.The abundance of cosmological
relics remained almost constant until
today.

Calculations
 Now we will see how the calculation of
the relic density of WIMPs proceeds
within the
standard cosmological scenario.

 If the candidate is stable or has a long
lifetime, the number of particles is
conserved after
it decouples, so the number density falls
like Specifically, we use the Lee-
Weinberg Equation. It describes
annihilation and creation of χ particles.

DECOUPLING
 Decoupling of particle species is an essential concept for particle
cosmology. It is described by the Boltzmann equation

Dilution from XX → f ‾
f f f‾ XX
→
expansion

 Particles decouple (or freeze out) when

 An example: neutrino decoupling. By dimensional analysis,

 : the equilibrium number density of the relic particles
 3Hnχ: the effect of the expansion of the universe
 < σv > :the thermal average of the annihilation cross
section σ multiplied with the relative velocity v of the two annihilating χ
particles
 other term on RHS is the decrease (increase) of the number density
due to annihilation into (production from) lighter particles

 The Lee-Weinberg equation assumes that χ is in kinetic
equilibrium with the standard model particles
 Now we use the effect of the expansion of the Universe by
considering the evolution of
the number of particles in a portion of comoving volume given
by

 We can then introduce the convenient quantity

 such that

 In addition, since the interaction term usually depend
explicitly upon temperature rather
than time, we introduce the x = m/T , the scaled
inverse temperature.
 During the radiation dominated period of the
universe, thermal production of WIMPs
takes also place . In this period, the expansion rate is
given by

 And then

 Where and where denotes the number of
intrinsic degrees of freedom for particle.

 Hence , last format of our equation is

 where

 After all little tricks , our Lee-Weinberg
equation can be recast as

 where

 To integrate the Lee-Weinberg equation, we need to
have an expression for the equilibrium number
density in comoving volume.
 Once the particle is non-relativistic, the difference
in statics is not important.

 The general equation of equilibrium number density
in comoving volume is

 For the nonrelativistic case at low
temperatures T << mχ one obtains,

At high temperatures, χ are abundant
and rapidly annihilate with its own
antiparticle χ into the standard model
particles.

 Shortly after that T has dropped below
mχ(T << mχ) ,the number density of χ
drops exponentially, until the
annihilation rate
 Γχ =N(x) < σv > becomes less than the
expansion rate H

 The temperature at which the particle
decouples (The time when the number of
particles reaches this constant value) from
the thermal bath is called freeze-out
temperature TF .
 Therefore χ particles are no longer able to
annihilate efficiently and the number density
per comoving volume becomes almost
constant.

 An approximate solution for the relic
abundance is given by

 and is freeze-out temperature
and approximately, for the typical case
 One has that is a solution of

 We can then finally calculate the contribution of χ to
the energy density parameter finding a well know
result

 It is intriguing that so called "WIMPS"(e.g. the
lightest supersymmetric particle) dark
matter particles seem to reproduce naturally the right
abundance since they have a weak cross section

 ,and masses mx mew 100GeV .
 This observations is called the "WIMP
miracle" and typically considered as an
encouraging point supporting WIMPS
as Dark Matter candidates.

1) Initially, neutralinos c are in
thermal equilibrium:
cc ↔ f f
2) Universe cools:
N = NEQ ~ e -m/T
3) cs “freeze out”:
N ~ constant

Freeze out determined by
annihilation cross section: for
neutralinos, WDM ~ 0.1; natural
– no new scales!

 Lee-Weinberg equation, the termal production, is the
most traditional mechanism but that
many other mechanisms have been considered in the
literature such as non thermal produc-
tion of very massive particles(so called
WIMPZILLAS) at preheating or even right-handed
neutrino oscillations.

Detection Promising
c

c

c
f
Crossing

symmetry
c f

f
f
Annihilation Scattering
Correct relic density  efficient annihilation then
 efficient annihilation now, efficient scattering
now
No-Lose Theorem

• Assume gravitino is LSP. Early
universe behaves as usual,
WIMP freezes out with
desired thermal relic density
WIMP
M*2/MW3 ~ year

≈
G

• A year passes…then all
WIMPs decay to gravitinos

Gravitinos are dark matter now. They are superWIMPs –
superweakly-interacting massive particles

Title

Inner space and
outer space
are closely related

FREEZE OUT: QUALITATIVE
(1) Assume a new heavy (1)
particle X is initially in
Increasing
thermal equilibrium: (2) annihilation
strength
XX ↔ qq ↓
(2) Universe cools:
←
XX  qq (3)
/
→

(3) Universe expands:
→
/
XX /← qq Feng, ARAA (2010)

Zeldovich et al. (1960s)

WIMP EXAMPLES

• Weakly-interacting massive particles: many examples,
broadly similar, but different in detail

• The prototypical WIMP: neutralinos in supersymmetry
Goldberg (1983)

• KK B1 (“KK photons”) in universal extra dimensions
Servant, Tait (2002); Cheng, Feng, Matchev (2002)
• Cosmology and particle physics both point to the Terascale
for new particles, with viable WIMP candidates from SUSY,
UED, etc.

WIMP DETECTION
Correct relic density  Efficient annihilation then

Efficient production now
(Indirect detection)
Efficient annihilation now

c c

(Particle colliders)
q q

Efficient scattering now
(Direct detection)

DIRECT DETECTION
 Look for normal matter
recoiling from DM collisions
 WIMP properties
 m ~ 100 GeV
 velocity ~ 10-3 c
 Recoil energy ~ 1-100 keV

 Typically focus on ultra-
sensitive detectors placed
deep underground DM

 But first, what range of
interaction strengths are to
be probed?

INDIRECT DETECTION

Dark Matter Madlibs!

Dark matter annihilates in ________________ to
a place
__________ , which are detected by _____________ .
particles an experiment

INDIRECT DETECTION
Dark Matter annihilates in the halo to
a place
positrons , which are detected by PAMELA/ATIC/Fermi…
.
some particles an experiment

PAMELA ATIC Fermi

Dark Matter annihilates in the center of the Sun to
a place
neutrinos , which are detected by IceCube .

Dark Matter annihilates in the galactic center to
a place
photons , which are detected by Fermi, VERITAS, … .

• Lines from XX  gg, gZ
• Continuum from XX  ff  g
Particle Astro-
Physics Physics

Halo profiles are
poorly understood
near the galactic
center

PARTICLE COLLIDERS

20-22 June 11 Feng 85

DIRECT PRODUCTION AT COLLIDERS

• Thermal relic WIMPs annihilate to SM particles, and so
should be produced directly at colliders

• Pair production is invisible, so consider photon radiation

• Also mono-jets, mono-photons at Tevatron and LHC
Birkedal, Matchev, Perelstein (2004); Feng, Su, Takayama (2005)
Konar, Kong, Matchev, Perelstein (2009)

PRECISION DM AT COLLIDERS
If there is a signal, what do we learn?

 Cosmology can’t discover • Particle colliders can’t
SUSY discover DM

Lifetime > 10 -7 s  1017 s ?

DARK MATTER AT THE LHC
• What LHC actually sees:
– E.g., qq pair production
– Each q  neutralino c
– 2 c’s escape detector
– missing momentum

• This is not the discovery
of dark matter
– Lifetime > 10-7 s  1017 s?

DARK MATTER ANALOGUE
 Particle physics  dark
matter abundance
prediction

 Compare to dark
matter abundance
observation

 How well can we do?

SUMMARY
 Thermal relic WIMPs can be detected directly,
indirectly, and at colliders, and the thermal relic
density implies significant rates

 There are currently tantalizing anomalies

 Definitive dark matter detection and understanding
will require signals in several types of experiments

Next time
 f(R) Gravity and its relation to the
interaction between DE and DM

Dark Matter

More Related Content

What's hot (20)

Similar to Dark Matter (20)

More from Eastern Mediterranean University (10)

Recently uploaded (20)

Dark Matter