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Precision Cosmology LCDMD
AR
K M
AT
TER
DA
RK
EN
ER
GY
INFLA
TIO
N
BA
RYO
GEN
ES
IS
Beyond the Standard Model Physics
Precision Cosmology
A precision cosmological model that agreed with observations for 1300 years!Earth
MarsEpicycle
Deferent
Eccentric
Equant
We have to discover how dark matter, dark energy, inflation, baryon asymmetry is grounded in physical law.
(At Least) 75 Years of Dark MatterOpik 1915Kapteyn 1922Jeans 1922Oort 1932
Zwicky 1937 75 Years Ago Dark Matter Coma (M/L) ~ 500
Babcock 1939 73 Years Ago Dark Matter in M31 (M/L) ~ 60
Rubin & Ford 1969 43 Years Ago Dark Matter in M31 (M/L) ~ 60
Cowsik & McClelland 1972 40 Years Ago 1st WIMP Candidate (light n )
Lee & Weinberg 1977 35 Years AgoPrototype WIMP (heavy n )
Stecker 1977 35 Years Ago Indirect Detection (WIMP annih.)
Goldberg 1983 29 Years AgoPhotino (SUSY WIMP)Ellis, Hagelin, et al. 1983 29 Years AgoNeutralino (SUSY WIMP)
Goodman & Witten 1985 27 Years Ago Direct Detection Possible
Ahlen et al. 1987 25 Years Ago First Direct Detection Limits
Stellar motions to galactic plane dark matter in the local solar neighborhood: (M/L) ~ 2 to 3
Interaction Strength
only gravitational: wimpzillas
strongly interacting: B balls
thermal relics or decay of oroscillation from thermal relics
nonthermalrelics
Particle Dark Matter Taxonomy• neutrinos (hot)
• sterile neutrinos, gravitinos (warm)
• Lightest supersymmetric particle (cold)
• Lightest Kaluza-Klein particle (cold)
• Bose-Einstein condensates
• axions, axion clusters
• solitons (Q-balls, B-balls, …)
• supermassive wimpzillas from inflation
Mass
10-22 eV (10-56 g) Bose-Einstein
10-8 Mʘ (10+25 g) axion clusters
coherentstate of ascalar field
Rel
ativ
e ab
un
dan
ce
M / T
equilibrium e-M / Tequilibrium e-M / Tequilibrium e-M / Tequilibrium e-M / T
101 102 103110-20
10-15
10-10
10-5
1
increasing sA
decreasing W
Cold Thermal Relics*
* An object of particular veneration.
W
W
W
… often used to give an impression of great and unusual value in a trivial context …
The WIMP “Miracle”
Cold thermal relic: weak scale cross section (and mass?)(1 GeV − 1 TeV ) WIMP (Weakly Interacting Massive Particle)
WIMPs are BSM, but not far BSM
mir·a·cle \ˈmir-i-kəl \ noun
1 : an extraordinary event manifesting divine intervention in human affairs
Low-mass region:either unexplained backgrounds in DAMA, CoGeNT, and CRESST-II, … or… other experiments do not understand low recoil energy calibration, … or… can’t compare different experiments(velocity, fn ≠ fn, …)
High-mass region:Reaching shades of grey of the CMSSM iceberg, just as heat from LHC melts it!
Direct Detection
Finkbeiner & Su 1207.7060
129 GeVc + c g + g
111 GeVc + c g + Z
About 3s
Six stacked galaxy clusters: signal at 3.2sHektor, Raidal, Tempel 1207.4466
Fermi/GLAST Line(s)No results yet from dwarf stacking Geringger-Saneth, & Koushiappas 1206.0796
Maverick WIMP
• WIMP is a loner
• Use effective field theory,e.g.: 4-Fermi interaction
• WIMP only new species
• Clearer relationship between
sA , sS , and sP
Social WIMP
• WIMP part of a social network
• Motivated model framework,e.g., low-energy SUSY, UED, ...
• Many new particles/parameters
• Unclear relationships between sA , sS , and sP
LHC: Is WIMP Social or Maverick Species
gluinos, squarks, charginos will be discovered before neutralinos
SUSY WIMPs at the LHC
LHC chewing away at allowed region
• Analysis s-model dependent
• Can s-wiggle out
• But it is getting harder
• Don’t throw in towel-ino
• “SUSY is alive and well” ……but not as well as it once was…
twiki.cern.ch/twiki/bin/view/CMSPublic/PhysicsResultsEXO11059Winter2012
Also CDF:1203.0742
Maverick Limits from LHC
http://indico.cern.ch/getFile.py/access?contribId=176&sessionId=79&resId=0&materialId=slides&confId=181298
• Direct detectors, indirect detectors, & colliders race for discovery
• Suppose by 2020 have credible signals from all three (three miracles)?
• Three miracles WIMP sainthood ?
• How will we know they are all seeing the same phenomenon?
• When can we say we have made darkness visible?
The Decade of the WIMP• WIMP coincidence or causation (it ain’t a miracle)?
• Situation now is muddled
• Ten years from now the WIMP hypothesis will have either:convincing evidence or near-death experience
Taking Sides!Can’t hide from the data – LCDM too good to ignore
– SNe– Subtraction: 1.0 - 0.3 = 0.7– Baryon acoustic oscillations– Galaxy clusters– Weak lensing– …
H(z) not given by
Einstein–de Sitter
G00 (FLRW) 8 G T00(matter)
Modify left-hand side of Einstein equations (DG00)
3. Beyond Einstein (modified gravity)
4. (Just) Einstein (back reaction of inhomogeneities)
Modify right-hand side of Einstein equations (DT00)
1. Constant (“just” a cosmoillogical constant)
2. Not constant (dynamics described by a scalar field)
The Nature of the Higgs• No single decay mode can tell us everything: use multiple decay modes
Different decay modes have different strengths and weaknessesDifferent systematic uncertainties in different decay modesDifferent decay modes sensitive to new physics in different ways
The Nature of Dark Energy• No single technique can tell us everything: use multiple techniques
Different techniques have different strengths and weaknessesDifferent systematic uncertainties in different techniquesDifferent techniques sensitive to new physics in different ways
w0 or wa
LCDM
Supernova
Weak Lensing
Baryon Acoustic Oscillations
Redshift Space Distortions
Clusters
Introduction:
“ … production of matter, merely by expansion,… Alarmed by these prospects, I have examined the matter in more detail.”
Conclusion:
“ … There will be a mutual adulteration of [particles] in the course of time, giving rise to … the ‘alarming phenomenon’.”
Disturbing the Quantum Vacuum
Erwin Schrödinger, Physica 6, 899 (1939)The Proper Vibrations of the Expanding Universe
Creation of a single pair of particles somewhere
in our Hubble volume VH = (c H0)-3 = 1013
ly3
in the next Hubble time tH = H0-1 = 1010 years
with a Hubble energy EH = H0 = 10-33 eVAlarming?
Disturbing the Quantum Vacuum
Erwin Schrödinger, Physica 6, 899 (1939)The Proper Vibrations of the Expanding Universe
Disturbing the Quantum Vacuum
expansion
of space
Schrödinger’s alarming phenomenon (1939)
Expanding Universe Temperature & density fluctuations
Expanding Universe Creation of Gravitons
Disturbing the Quantum Vacuum
expansion
of space
GG
G G
Schrödinger’s alarming phenomenon (1939)
Most Fundamental Question
1. Is inflation eternal? Is there a multiverse?
Does inflation do what it was invented to do?
• What will Planck tell us about spectral index (n)?
• Search for gravitational waves from B-mode polarization
(r).
• Search for non-gaussianity ( fNL ).
• Theory developments: effective field theory approach.
• Who is the inflaton … superstrings inflaton ?
Next Most Fundamental Question
2. What if exact Harrison-Zel’dovich perturbation spectrum?
scalar spectral index exactly unityno gravitational wavesexactly gaussian perturbations only curvature perturbations
Harrison Zel’dovich
Inflation & Superstrings Are a Match
Make perturbations?
Lonely 33-year-old scalar field (inflaton) seeks a fundamental theory in which to be embedded.
Strings attached?
Mature 38-year-old idea (superstrings) seeks a partner to develop some physical observables.
Very high degree of compatibility
“Until cosmology and particle physics can be brought together in the same context, there is not much hope for real progress in cosmology.”
— N. Bohr, 1939
Philip Morrison, Private Communication, ca. 1984
The COSMO Spirit