forecasting the axiverse david j. e. marsh, berkeley, 1/12/11 forecasting the axiverse, david j. e....
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Forecasting the Axiverse
David J. E. Marsh, David J. E. Marsh,
Berkeley, 1/12/11Berkeley, 1/12/11
Forecasting the Axiverse, David J. E. Marsh, Berkeley, 1/12/11 1/35
David J. E. Marsh, Edward Macaulay, Maxime Trebitsch and Pedro G. Ferreira, arXiv:astro-ph/1110.0502.
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Introduction: standard models
The “String Axiverse”
Axions and Cosmology
Forecasts (“Euclid-like”)
Conclusions and outlook
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Outline
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• Initial conditions:
• Dark sector:
• Radiation:
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The Concordance Model
• Ordinary matter:
Photons
Relativistic species, e.g. massless
neutrinosBaryons
Dark matter
Dark energy
… Inflation
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• Gauge forces: EM, strong and weak forces.
nucleosynthesis, recombination…
• Matter: quarks and leptons
baryons, massless neutrinosbaryons, massless neutrinos
• Neutrino masses?Neutrino masses?
• Strong CP problem and axions?Strong CP problem and axions?
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The Standard Model
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• Standard model has no candidates.
• Cosmology: CDM and a c.c. can fit all data.
• Extra relativistic species?
• DE equation of state or EDE?
• Particle Physics: CDM = WIMP (e.g. LSP).
• In addition, need massive neutrinos
(observationally) and possibly axions (theoretically).
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The Dark Sector
Komatsu et al (WMAP 7, 2011)
Dunkley et al (ACT, 2010)
Dark Matter is multi-component!
Giunti, arXiv:1106.4479 (2011) Peccei and Quinn, PRL 38,1440 (1977)
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The Axiverse: what? Arvanitaki et al PRD 81, 123530 (2010)
““String theory suggests the simultaneous presence of String theory suggests the simultaneous presence of
many ultra-light axions, possibly populating each decade many ultra-light axions, possibly populating each decade
of mass down to the Hubble scale, 10of mass down to the Hubble scale, 10-33 -33 eV”eV”
Figure: Arvanitaki et al
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• Potentials from non-perturbative physics (D-branes,
instantons etc.).
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The Axiverse: how? Svrcek and Witten, arXiv:hep-th/0605206
• String theory has extra
dimensions: compactify.
• Axions are KK zero-
modes of antisymmetric
tensor fields compactified
on closed cycles.
Many pseudo Goldstone bosons
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The Axiverse and QCD
• Require the QCD axion to solve strong CP:
http://www.hep.ph.ic.ac.uk/cms/physics/higgs.html
• SSB at scale fa, then
instantons tilt the hat.
• The QCD axion must
remain light to achieve
this. Many axions will remain light
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• Instanton action scales with the area of a cycle.• Masses distribute on a log scale:
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The Axiverse in this work (and why)
• Scales depend on the action of the instantons:• Canonically normalised axions are weakly
coupled
A source of ultra-light scalar dark matter
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Interlude Sikivie, Physics Today, Dec. ‘96
QuickTime™ and a decompressor
are needed to see this picture.
• You observe a flat table in a
room with a slanted floor.
How?
• You propose a mechanism
to straighten it accurately:
gravity.
• The required accuracy requires a long arm and heavy
weight.
• How can you test this? Look for relic oscillations from
production.Forecasting the Axiverse, David J. E. Marsh, Berkeley, 1/12/11
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• Well defined measure for abundance.
• Fine tuning?
• Isocurvature and gravity waves give constraints.
• Motivated as dark matter in many different contexts.
• Couplings give further constraints.
• Axions and inflation.
• Monodromy quintessence, BH superradiance, …
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Comments on Axions
Tegmark et al, PRD (2006)
Mack and Steinhardt, JCAP (2011)
Fox et al, hep-th/0409059
Sikivie, arXiv:1003.2426
Mortsell and Goobar, JCAP (2003)
Linde, PLB (1991)
Panda et al, arXiv:1011.5877
Arvanitaki and Dubovsky, PRD (2011)
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• Coupling to a modulus:
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Axiverse Extended DJEM, PRD (2011)
• Stabilisation in an attractor.
• Potential to solve initial conditions problem for axion?
• EDE and dark energy dynamics.
• Collapsing universe is asymptotic future.
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Cosmology of the Axiverse I
• Equations of motion:
• Stress energy tensor:
Ma and Bertschinger, APJ (1995)
Hu, APJ (1998)
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• Different background scaling implies different effects on Different background scaling implies different effects on
matter-radiation equality, and hence on the CMB.matter-radiation equality, and hence on the CMB.
• Relic density is non-thermal.Relic density is non-thermal.
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Background Evolution
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Cosmology of the Axiverse II
• WKB approx. gives a scale dependent sound speed:
• Process analogous to neutrino free-streaming:
Hu et al, PRL (2000)
Amendola and Barbieri, PLB (2006)
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• Many degeneracies as for massive neutrinos.
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Axion “Free-Streaming”
• This leads to steps in the matter power spectrum:
DJEM and Ferreira, PRD (2010)
Eisenstein and Hu, APJ (1997)
Hu, Eisenstein, Tegmark, PRL (1998)
DJEM and Ferreira, PRD (2010)
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Important Scales
DJEM et al, arXiv:1110.0502
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Implementation
• Module for CAMB solves field equations and
oscillations.
• Mass range restricted by this choice.
Amendola and Barbieri, PLB (2006)
QuickTime™ and a decompressor
are needed to see this picture.
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Observables: P(k) and BAO
• Model for smooth part changes: bias?
• Small change in sound horizon from background.
DJEM et al, arXiv:1110.0502
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Observables: Growth Rate
• Scale dependent growth, degenerate with more
CDM.
• Unique signal needs large scale measurement.
DJEM et al, arXiv:1110.0502
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Observables: Weak Lensing
• Convergence power spectrum measures dark matter
density directly from galaxy shear.
• Window function sets redshift bin: tomography.
DJEM et al, arXiv:1110.0502
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Observables: Weak Lensing
• Indistinguishable from
LCDM in single bin.
• Growth amplitude from
tomography gives very
strong constraints.Hu, PRD (2002)
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Observables: CMB
• Most effects can be removed due to total degeneracy with
horizon size and equality redshift.
• Breaks degeneracy with neutrino mass and number.
• Constraining power in ISW due to oscillations near
recombination: used in checks.
• Larger effects in lensing not used because of correlations.
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Forecasts: Implementation
• Fisher Matrix forecast for Planck + Euclid.
• CMB uses FIsherCodes by Sudeep Das.
• GRS and WLT are our own, by Edward and Maxime.
http://www.astro.princeton.edu/~sudeep/fisherCodesDoc
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“The Euclid survey can be thought of as the low-redshift, 3-
dimensional analogue and complement to the map of the high
redshift Universe provided by ESA’s Planck mission”.
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Forecasts: Euclid http://sci.esa.int/euclid
arXiv:1110.3193
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Forecasts: Survey Parameters
• Planck: TT, TE, EE in 100, 143 and 217 GHz.
• Euclid GRS: 15 redshift bins of varying volume.
43.68 million galaxies at a constant density of:43.68 million galaxies at a constant density of:
• Euclid WLT: 5 redshift bins, with constant # of sources.
Spectroscopic
Photometric
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Forecasts: Fiducial Models
• Fixed Hubble:
•Test 4 axion masses:
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Forecasts: Fiducial Models
• Fiducial cosmology:
• Marginalise over:
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Forecasts: Results
• Compare with massive neutrinos:
DJEM et al, arXiv:1110.0502
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Forecasts: Results
• Strong CMB degeneracies:
DJEM et al, arXiv:1110.0502
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Forecasts: Results
• Value of combining redshift information:
GRS alone can constrain 1% at 1
DJEM et al, arXiv:1110.0502
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Forecasts: Results
• Combined results:
Mass independent constraints
DJEM et al, arXiv:1110.0502
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Outlook
• Still much work to do for param. estimation.
• Fits comparing to specific neutrino models.
• Multiple, heavier species: Ly-alpha?
• Anharmonic potentials.
• Dynamics of extended model.
• Isocurvature?DJEM et al, in prep.
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Summary
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Thank You!
Questions?
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