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Cosmology
Dark MatterAESHEP 2012 10 25
Kavli IPMU, University of Tokyo
UC Berkeley, Lawrence Berkeley LaboratoryHitoshi Murayama
I OD IAS
TODAI INSTIT UTES FO R ADVANCED STUD Y
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How did the Universe begin?
What is its fate?What is it made of?What are its fundamental laws?
Why do we exist?
interdisciplinary institute ofastronomy , physics and mathematics
10-year program by Japanesegovernment since 2007
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Oct 2007
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Oct 2008
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Oct 2009
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Oct 2010
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Oct 2011
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Oct 2012
picture will be taken on Oct 19
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Oct 1 2007 Apr 1 2008 Oct 1 2008 Apr 1 2009 Oct 1 2009 Apr 1 2010 Oct 1 2010 Apr 1 2011 Oct 1 2011 Apr 1 2012 Oct 1 2012
Japanese Asian American European AustralianOthers*
Full-time Scientists paid by IPMU
*Argentina, Chile, Canada
10/01/2012
+30 students, 35 staffs ! 140 on site
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brand-new building 2010
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obelisk “L’Universo é scritto in
lingua matematica ”
“European town square ”
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ofciallyKavli IPMU on April 1, 2012First research institute in Japan namedafter a donor, breaking new grounds
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May 9, meeting with Prime Minister Noda
http://www.kantei.go.jp/jp/noda/actions/201205/09kavli.html
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• Basic research is very important, because it is a
common resource shared by the wholehumanity.
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Cosmology
Dark MatterAESHEP 2012 10 25
Kavli IPMU, University of TokyoUC Berkeley, Lawrence Berkeley Laboratory
Hitoshi Murayama
I OD IAS
TODAI INSTIT UTES FO R ADVANCED STUD Y
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star
Big Bangdark ages
13.7Gyr
particle soup
Earth
The wholeUniverse wassmaller than
an atom
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Solar System
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375 km2010 4 7
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Sep 30, 2008Kaguya
380,000km=1.3 light seconds
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380,000km=1.3 light seconds
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1.5" 108km=8.3 light minutes
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Made of atoms
• everything around us is made of atoms• stars are made of atoms, too
• spectroscopy
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metals
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1.5" 108km=8.3 light minutes
E=mc 2
5 Mt lighter every secondturning mass to energy
burning hydrogen
proton
4He
+ 2 e + + 2 !e + 25MeV
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proof nuclear fusion also produces neutrinostens of trillions of neutrinos going through our bodyevery second
1 km underground
SuperKamiokande
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luck
Feb 231987
1 6 0, 0 0 0 y e a r s
distant stars aremade of atoms, too
N
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Earth resolves around the Sun with 30km/sec
Solar SystemNeptune
4 light hours
I t ok
a w a
2 0 l i g h
t mi n
u t e s
16
v ∝1
√ r
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High School physicsF =
M m
r 2
ma = m
v2
r
GM m
r 2 = m
v 2
r
v =GM
r ∝1
√ r
16
v ∝1
√ r
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Proxima Centauri
4.2 light years
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Milky Way and Galaxies
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28,000light years
~10 11 stars
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1 5 0 0 l y r
2 8, 0 0 0 l y r
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28,000light years
few stars
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Andromeda M33 = 2.5M lyr
will collide with usin 4.5 billion years
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How do we measure
the rotation curve?• Special relativity
• hyperne splitting inneutral hydrogen
• 21cm line can be excitedby the cosmic
microwave background• kT 0=0.23 meV• h c/ 21cm = 0.94 " eV
f 0 = r c ∓ vc ± v
f ≈ 1 ∓cv
f
F =1
F =0
21cm
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VeraRubin
1960s
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100k lyrs
??
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connects galaxies– 12 –
Fig. 2.— The mean surface mass density prole as a function of the distance from the centre of galaxies. The thick solid curve is the mean of all haloes above the mass threshold. The dash-dottedcurve represents the contribution from particles bound to haloes, i.e., particles that reside withinthe virial radius of all haloes. The data with error bars are the observational estimate by MSFR
as in the previous gure.Ménard et al 2009
– 14 –
Fig. 4.— Fraction of mass contained in the sphere centred on individual haloes with radius α R vir ,where R vir is the pseudovirial radius and α is the multiplier represented in the abscissa. The solidcurve is 0 . 23ln+0 .23 given in the text.
Masaki Fukugita Yoshida 2011
stacking 85k quasars near 20M galaxies
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Center of Milky Way
http://www.eso.org/public/outreach/press-rel/pr-2008/phot-46-08.html
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http://www.eso.org/public/outreach/press-rel/pr-2008/phot-46-08.html
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Supermassive Black Hole
• supermassive blackhole of mass~4M Msun at the center of MilkyWay
• swallows gas around it• “death cry” for about 30 min
• but can’t be dark matter, far lessthan 100billion stars
http://www.eso.org/public/outreach/press-rel/pr-2008/phot-46-08.html
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Cluster of Galaxies
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Coma cluster
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motion of galaxies
• galaxies are moving inthe mutual gravitational
potential• assume virialized motion
<v 2>= G N M/r
• but they are too fast, too
• rst proposal of “darkmatter”
Fred Zwicky
i i l l i
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gravitational lensing
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gravitational lensing
r 0r
starlens
x
y
( x,y)
d 1 d 2 -1 -0.5 0.5 1
-1
-0.5
0.5
1
deection angleθ = 2
r S
r = 4
G N M
c 2 r
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Clusters of galaxies
distortion in images of BG galaxies 2D map of dark matter
0
– 8 a r e a
d e n s i t y ( g / c m
2 )
1
2
3
4
1 0 0 K l y – 8
8 0
8
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“see” invisible dark matter
Subaru telescope
more than 80% of matter is not atoms!
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as expected by theory
Subaru measurements.Okabe, Takada+ 11
45 clusters stacked consistent with NFW prole
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collion of clusters at 4500 km/s
lucky we are not here
4 billion l r awa
Dark Matter
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Dark Matter
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y-through based on SDSS-III data
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galaxy 13.2 billion lyr away
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dark ages
13.6 billion lyr away
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You can still see the Big Bang13.7 G lyr away= 13.7 Gyr ago
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CMB temperature
CMB dipole
we are moving at~1% of c relative to CMB
CMB anisotropyat ~10 –5
1mm ripple on 100m sea
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protons
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soup of particles
p
electrons quasars
galaxies
Cosmic Microwave Background Radiation
Big Bang 380,000 yrs 10 Gyrs 13.7 Gyrs
r e c o m b i n a t i o n
time
3 8 0 k1 3 . 7 G
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k y r G y r
CMB
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Friedmann Universe
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three possible fates• depending on the
“energy”, there arethree possible fates of
the Universe• adiabatic expansion
T ! R –1
• past universe wassmaller and hotter
• “energy” corresponds tothe curvature of space
• actually, it is at
time s i z e o
f t h e
U n
i v e r s e
E<0
E=0E>0
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Current Universe• knowing the l.h.s. tells us
the current energydensity
•l.h.s. = H02 from Hubblelaw v =H0 d
• r.h.s. denes the criticaldensity %c
• dene &i =%i /%c
• ' i &i =1
R
R !2
=8 π
3G N ρ − const
H 0 =R
R = 71km/s/Mpc
ρ c =8 π
G + N − 1 H 20 = 5 . 3 × 10 − 6 GeVcm − 3
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Early Universe• adiabatic expansion
T ! R –1
• T =T 0(1+ z )
• z : redshift = R0/R• $=$0(1+ z )• matter: %! R –3
• radiation (masslessparticles): %! R –4
• matter-radiationequality: z ! 3300
• recombination: z! 1300
R
R !2
=8 π
3G N ρ − const
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Large-Scale Structure
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CMB temperature
CMB dipole
we are moving at~1% of c relative to CMB
CMB anisotropyat ~10 –5
1mm ripple on 100m sea
2 b i l li
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nearly homogeneoussmall winkles
2 0 b i l l i onl y r
l i o n l y r
2 b i l l i o n l y r
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Dark Matter is
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Dark Matter isour birth mother
no dark matter with dark matter
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reenacting Big Ban with Cal Band
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Known Factsabout Dark Matter
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• By the time of matter-radiation equality anduntil now, dark matter must be non-relativistic and clump together bygravitational attraction
• must be electrically neutral
Cold and Neutral
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Search for MACHOs(Massive Compact Halo Objects)
Large Magellanic Cloud
Not enough of them!
Dim Stars?
MACHO95% cl
0.2
−6 −2−8 −4 0 20.0
0.4
0.6
f =
−
7
EROS−2 + EROS−1upper limit (95% cl)
logM= 2log( /70d)tE
EROSastro-ph/0607207
Mass Limits
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• Clumps to form structure
•imagine
• “Bohr radius”:
• too small m won’t “t” in a galaxy!
• m >10 ! 22 eV “uncertainty principle” bound(modied from Hu, Barkana, Gruzinov, astro-ph/0003365)
V = G N
m
rr B =
G N M m 2
Mass Limits
“Uncertaint Princi le”
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• 10-31 GeV to 10 50 GeV
• we narrowed it down towithin 81 orders ofmagnitude
• a big progress in 70 years
since Zwicky
Mass Limits
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• if self-coupling too big, will “smoothout” cuspy prole at the galacticcenter
• some people want it
(Spergel and Steinhardt, astro-ph/9909386)
• need core < 35 kpc/h from data( < 1.7 x 10 -25 cm2 (m/GeV)
(Yoshida, Springel, White, astro-ph/0006134)
• bullet cluster:( < 1.7x10 -24 cm2 (m/GeV)(Markevitch et al, astro-ph/0309303)
Self-Coupling
f
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•At least of the order of age of the universe14Gyr
• Beyond that, it depends on decay modes,branching fractions, all model-dependent
Lifetime
l l l
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Cosmological scales
101
matter
all atoms = 5 .70 +0 .39
− 0 .61
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(n&)0 = (n&f = 1001(m,m~~g~‘2 JA+)N 10-S/[(m,/GeV)((~A~)/10-27 cm3 s-‘)I,
where the subscript f denotes the value at freezeout and the subscript 0 denotes theThe current entropy density is so N 4000 cmm3,and the critical density
h l l
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• thermal equilibrium whenT>m !
• Once T<m ! , no more ! created
• if stable, only way to losethem is annihilation• but universe expands and
! get dilute
• at some point they can’tnd each other
• their number in comovingvolume “frozen”
pC II 10-5h2 GeVcmp3, where is the Hubble constant in units of 100 km s-l M ppresent mass d ensity in units of the critical density is given by
0,h2 = mxn,/p, N (3 x 1O-27 cm3 C1/(oAv)) .
The result is independent of the mass of the WIMP (except for logarithmic correcinversely proportional to its annihilation cross section.
Fig. 4 shows numerical solutions to the Boltzmann equation. The equilibrium (sactual (dashed lines) abundan ces per comoving volume a re plotted as a function
0 0 1
0 0 0 1
0 0 0 0 1
10 b
,h10-s
-; 10-7
caJ 10-aa
2
10-Q
p lo-‘9
lo-”
z 10-m
F o-‘3
10 100
x=m/T (time +)
Fig. 4. Comoving number density of a WIMP in the early Universe. The dashed curves are the actual the solid curve is the equilibrium abundance. From [31].
thermal relic
F
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• WIMP freezes out whenthe annihilation ratedrops below the
expansion rate
• Yield Y=n/s constantunder expansion
• stronger annihilation less abundance
H ≈ g1 / 2∗
T 2
M P lΓ ann ≈ σ ann v n
H (T f ) = Γ ann
n ≈ g1
/2
∗
T 2f
M P l σ ann v
s ≈ g∗ T 3
Y = n
s ≈ g
− 1 / 2∗
1
M P l T f σ ann vΩ
χ =
m χ Y s0
ρ c
≈ g− 1 / 2∗
x f
M 3
P l σ ann v
s 0
H 2
0
Freeze-out
O d f i d
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• “Known” &! =0.23determines the WIMPannihilation crosssection
• simple estimate of theannihilation crosssection
• weak-scale mass!!!
Ωχ ≈ g
− 1 / 2∗
x f
M 3P l σ ann v
s 0
H 20
σ ann v ≈ 1 .12 × 10− 10
GeV− 2
x f g
1 / 2∗
Ωχ h 2
∼ 10 − 9 GeV − 2
σ ann v ≈ πα
2
m 2χ
m χ ≈ 300 GeV
Order of magnitude
0 0 1
0 0 0 1
0 0 0 0 1
10 b
10 sh l li
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• Solve the Boltzmann equation
• assume Maxwell distribution, 1=2= ! , E1=E2=m !
• Note momentum dependence may beimportant close to thresholds, resonances
• re roduce the estimate with
dn
dt + 3 Hn = − σ ann v (n 2 − n 2
eq )
xf ≈ 24 + ln
m χ
100GeV + ln
σ ann v
10 − 9 GeV − 2 −
1
2 ln
g ∗
100
dn 1
dt + 3 Hn 1 = −
4
i =1
d3 pi
(2π )3 2E i|M (12 → 34)| 2 (2π )4 δ 4 ( p1 + p2 − p3 − p4 )
[f 1 f 2 (1 ± f 3 )(1 ± f 4 ) − f 3 f 4 (1 ± f 1 )(1 ± f 2 )]
,h10-s
-; 10-7
caJ 10-aa
2
10-Q
p lo-‘9
lo-”
z 10-m
F o-‘3
10 100
x=m/T (time +)
Fig. 4. Comoving number density of a WIMP in the early Universe. The dashed curves are the actualthe solid curve is the equilibrium abundance. From [31].
thermal relic
WIMP
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• A stable particle at the weak scale with “EM-strength” coupling naturally gives the correctabundance
• This is where we expect new particlesbecause of the hierarchy problem!
• Many candidates of this type: SUSY, little Higgswith T-parity, Universal Extra Dimensinos, etc
• If so, we may even create dark matter ataccelerators
WIMP
Mi i l M d l
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Minimal Model• Dark Matter clearly a new degree of
freedom
•The smallest degree of freedom you canadd to the QFT is a real Klein-Gordon eldS:dof=1
• assign odd Z 2 parity to S, everything else
even• Most general renormalizable coupling LS =
1
2! µS ! µS −
1
2m2
S S 2 − k 2
| H | 2 S 2 − h4!
S 4 .
C i h k
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Consistency check • correct Dark Matter abundance• evades direct detection limits• satises triviality/instability limits from RGE
•consistent with precision electroweak data
180
190
170
160
150
140
130
m h
( G e V
) m S
=1
8 0 0 G e V
1 0 0 0
3 0 0
2 0 5 0
7 5
7 5
h (m Z )=01.01.2 i nst a b i l i t y
t r iv ialit y of λ
t r i v i a l i t y o f k
5. 5
σ p
( c m 2 )
10 − 40
10 − 42
10 − 44
10 − 46
DAMA (3 σ )
C D M S - I I ( 9 0 % C L )
mh = 150GeV Ω
S h 2=0.11
C R E S S T I I
Z E P L I N 4 / MA X
C D M S - I I
E d e l w e i s s 2