Upload
erno
View
40
Download
0
Embed Size (px)
DESCRIPTION
The Theory/Observation connection lecture 4 dark energy: linking with observations. Will Percival The University of Portsmouth. Lecture outline. Dark Energy review cosmological constant? quintessence? tangled defects? phantom dark energy? modified gravity? problems with the data? - PowerPoint PPT Presentation
Citation preview
The Theory/Observation connectionlecture 4
dark energy: linking with observations
Will Percival
The University of Portsmouth
Lecture outline
Dark Energy review– cosmological constant?
– quintessence?
– tangled defects?
– phantom dark energy?
– modified gravity?
– problems with the data?
Geometrical tests– SN1a
– BAO
Cosmological constant
Originally introduced by Einstein to make the Universe static Constant vacuum energy density, which is homogeneous and has constant density in time Equation of state
Particle physics provides a natural candidate: zero-point vacuum fluctuations for bosonic or fermionic fields
– typical scale of cosmological constant is (Mcutoff)4, where Mcutoff is UV cutoff of theory describing field
– Planck mass gives planck ~ (1019GeV)4
– Observations show
quintessence
adaption of scalar field theory developed for inflationary theories for late-time dark energy very weak potential required, with very small effective mass
– field can be frozen at early times
– or it can slowly roll down the potential, with energy density tracking dominant fluid until recently (“tracker” models)
equation-of-state generally evolves, although can be constant (with special choice of potential) In fact, any w(z)>-1 history can be obtained with right choice of potential
quintessence
Albrecht & Weller 2002, astro-ph/0106079
Parameterizations of w
If you don’t know the physics, you don’t have a well-defined set of models to test, it’s a free-for-all
Bassett et al. 2004, astro-ph/0407364
can parameterise using
w(a) = w0 + w1(1-a)
Tangled defects
Network of defects formed in phase transition grows with expansion of Universe
– For strings, lengths grow as a, and energy as a-2, so w=-1/3, and no acceleration (just)
– For walls, area grows as a2, and energy drops as a-1, so w=-2/3, which can produce acceleration
but observations show w ~ -1
Phantom dark energy
motivated by early supernovae data which favored strong acceleration w<-1 density increases as Universe expands can lead to divergence in finite time - big rip theoretically difficult to justify
– violate weak energy condition
– lead to ghosts - negative norm energy states
– can be classically and quantum mechanically unstable
If observations continue to show strong acceleration at low redshifts, may need a phase shift in theory
modified gravity
Can separate cosmological constant from stress-energy tensor
Can then imagine moving it to the other side of the equation
Should we consider alternatives if we’re going to be modifying gravity, rather than postulating a new component of energy?
modified gravity
Example from history: Mercury perihilion Newton + dark planet?
No! Modified gravity (GR)
Today, we need a modified Friedmann equation
modified gravity
Problem: we can always explain Adark by either stress-energy component or change to gravity.
Only way of telling apart is by structure formation (see next lecture)
Modified gravity: replace R with f(R) in action for gravity. Gives
DGP modifed gravity (5D braneworld)
Problems with the data …
data depends on astrophysics, so subject to systematics but, more than one test, so need a conspiracy that all the astrophysics points you to acceleration …
Still, worth reviewing all data
With this in mind, lets have a look at the evidence for acceleration …
All strong evidence is geometrical
All of the evidence depends on the expansion geometry, specifically through the Friedmann equation
equation of state of dark energy p = w(a)
SNLS Hubble diagram
First-Year SNLS Hubble Diagram
ΩM = 0.263 ± 0.042 (stat) ± 0.032 (sys)
<w>=-1.02 ± 0.09 (stat) ± 0.054 (sys) (with BAO + Flat Universe)
Astier et al (2006)A&A, 447, 31
Supernovae observations
Initially assumed all SN1a have same intrinsic peak brightness Now refined so that
Luminosity distance to supernova
Apparent magnitude of supernova
Absolute magnitude of supernova (assumed constant for all SN1a)
Stretch parameter s: corrects for lightcurve shape via
c=B-V colour: corrects for extinction/intrinsic effects via
Supernovae systematics
“Experimental Systematics”–Calibration, photometry, Malmquist-type effects
Contamination by other SNe or peculiar SNe Ia–Minimized by spectroscopic confirmation
Non-SNe systematics–Peculiar velocities; Hubble Bubble; Weak lensing
K-corrections and SN spectra–UV uncertain; “golden” redshifts; spectral evolution?
Extinction/Colour–Effective RV; Intrinsic colour versus dust
Redshift evolution in the mix of SNe–“Population drift” – environment?
Evolution in SN properties–Light-curves/Colors/Luminosities
From talk by Mark Sullivan
Hubble diagram by galaxy type
SNe in passive galaxies show a smaller scatter “Intrinsic dispersion” consistent with zero
(Does intrinsic dispersion in SNe arise from dust?)
Cleaner sample: But SNe in passive galaxies are at high-z (~20%: two component model) + very few locally
Passive hosts Star-forming hosts
Cosmological distribution of galaxy types
Future supernovae prospects
Short-term: Current constraints on <w>: <w>=-1 to ~6-7% (stat)
(inc. flat Universe, BAO+WMAP-3)
At SNLS survey end, statistical uncertainty will be 4-5%:– 500 SNLS + 200 SDSS + larger local samples– Improved external constraints (BAO, WL)
Longer term:
No evolutionary bias in cosmology detected (tests continue!)
SNe in passive galaxies: seem more powerful probes, but substantially rarer (esp. at high-z)
Colour corrections are the dominant uncertainty
– Urgent need for z<0.1 samples with wide wavelength coverage
– Not clear what the “next step” at high-z should be
Galaxy clustering
The power spectrum turn-over
varying the matter densitytimes the Hubble constant
In radiation dominated Universe, pressure support means that small perturbations cannot collapse. Jeans scale changes with time, leading to smooth turn-over of matter power spectrum.
However, it is hard to disentangle this shape change from galaxy bias and non-linear effects
Problem: galaxy bias
Galaxies do not form a Poisson sampling of the matter field
Peaks model: large scale offset in 2-pt clustering strength (next lecture)
Also non-linear effects in the matter
Also effects from the transition from mass to galaxies
Angulo et al., 2007, MNRAS, astro-ph/0702543
Baryon Acoustic Oscillations
“Wavelength” of baryonic acoustic oscillations is determined by the comoving sound horizon at recombination
At early times can ignore dark energy, so comoving sound horizon is given by
Sound speed cs
QuickTime™ and aTIFF (Uncompressed) decompressor
are needed to see this picture.
QuickTime™ and aTIFF (Uncompressed) decompressor
are needed to see this picture.
QuickTime™ and aTIFF (Uncompressed) decompressor
are needed to see this picture.
varying thebaryon fraction
Gives the comoving sound horizon ~110h-1Mpc, and BAO wavelength 0.06hMpc-1
Comparing CMB & BAO
SDSS GALAXIES
CMB
CREDIT: WMAP & SDSS websites
Comparing BAO at different redshifts
CREDIT: WMAP & SDSS websites
SDSS LRGs
SDSS main galaxies + 2dFGRS
Tell us more about the acceleration, rather than just that we need it!
z=0.35z=0.2
BAO as a standard ruler
Changes in cosmological model alter measured BAO scale (∆dcomov) by:
Radial direction
(evolution of Universe)
Angular direction
(line of sight)
Gives rise to the “rings of power”
Hu & Haiman 2003, astro-ph/0306053
BAO as a standard ruler
If we are considering radial and angular directions using randomly placed galaxy pairs, we constrain (to 1st order)
BAO position (in a redshift slice) therefore constrains some multiple of
Varying rs/DV
Changes in cosmological model alter measured BAO scale (∆dcomov) by:
Radial direction
(evolution of Universe)
Angular direction
(line of sight)
Why BAO are a good ruler
No change in position of oscillations, just a damping term.
Suppose that we measure an observed power that is related to the linear power by (halo model)
Linear baryon acoustic oscillations are ratio of linear matter power spectrum to a smooth fit
Then observed oscillations are related to linear BAO by
To change the observed positions of BAO, we need sharp features in the observed power
Eisenstein, Seo & White 2006, astro-ph/0604361Percival et al. 2007, astro-ph/0705.3323
Linear bias model also predicts this form
For linear bias model, peculiar velocities of galaxies gives Gaussian damping with width ~10Mpc
Going to 2nd order …
Perturbative treatment of (CDM+baryon) fluid system
L+++= )3()2()1( δδδδ
( e.g., Suto & Sasaki 1991)
Based on field-theoretical approach,
Crocce & Scoccimarro (2006ab,2007)
““Renormalized Perturbation TheoryRenormalized Perturbation Theory ( (RPTRPT)”)”
New approachNew approach
infinite class of perturbative corrections at all orders.Standard PT calculation can be improved by re-summing an
Related works: McDonald, Matarrese & Pietroni, Valageas, Matsubara (‘07)
Going to 2nd order …
At second order we get mode mixing, which causes shifts in the power spectrum BAO peaks
Shifts are <1%, and can be calculated
Crocce & Scoccimarro 2007; astro-ph/0704.2783
Not important for current data, but need to be included for future analyses
BAO from all the SDSS DR5 galaxies
Compared with WMAP 3-year best fit linear CDM cosmological model. N.B. not a fit to the data, but a prediction from WMAP.
Interesting features:
1. Overall P(k) shape
2. Observed baryon acoustic oscillations (BAO)
Percival et al., 2007, ApJ, 657, 645
BAO from the 2dFGRS + SDSS
BAO detected at low redshift 0<z<0.3 (effective redshift 0.2)
BAO detected at high redshift 0.15<z<0.5 (effective redshift 0.35)
BAO from combined sample (detected over the whole redshift range 0<z<0.5)
Percival et al., 2007, MNRAS, astro-ph/0705.3323
BAO distance scale constraints
Constraint fromDV(0.35)/DV(0.2)
Constraint fitting rs/DV(z)
Constraint including observed peak distance constrain from CMB rs/dA(cmb)=0.0104
SCDMSCDM
OCDMOCDMCDMCDM
Future BAO prospects
Short-term: SDSS-II improves low redshift measurements by factor ~2
– 1000000 galaxy redshifts to z~0.5 Wiggle-Z survey detects BAO at higher redshift
– 400 000 galaxy redshifts to z~1– weak constraints
Longer term:
Photometric surveys (e.g PanSTARRS, DES) find ~2--3% distance constraints out to z~1
Future spectroscopic surveys (e.g. HetDex, BOSS, WFMOS, Space) push to 1% distance constraints over a wide range of redshift (0.5<z<3)
With 1% constraints need to include 2nd order effects in analysis of BAO positions
Further reading
Supernovae– Astier et al. (2005), astro-ph/0510447
BAO– Blake & Glazebrook (2003), astro-ph/0301632– Seo & Eisenstein (2003), ApJ, 598, 720– Hu & Haiman (2003), astro-ph/0306053