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Constraints on cosmological parameters from the 6dF Galaxy Survey. Matthew Colless 6dFGS Workshop 11 July 2003. What can the 6dFGS tell us?.

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constraints on cosmological parameters from the 6df galaxy survey

Constraints on cosmological parameters from the 6dF Galaxy Survey

Matthew Colless

6dFGS Workshop

11 July 2003

what can the 6dfgs tell us
What can the 6dFGS tell us?
  • Strong constraints on cosmological parameters result from combining the wide range of existing datasets: 2dFGRS/SDSS, WMAP, distant SNe, Lyman  forest, weak lensing…
  • Given this plethora of data, what can the 6dFGS add?
  • Specifically, what advantage does the combination of redshift and peculiar velocity information give?
  • The answers presented here are based on…

“Prospects for galaxy-mass relations from the 6dF Galaxy Redshift & Peculiar Velocity survey” Dan Burkey & Andy Taylor

z surveys and v surveys
z-surveys and v-surveys
  • Galaxy redshift surveys: simple, quick and easy (ha!) so can be very large, but…
    • unknown ‘bias’ linking galaxies to the matter distribution;
    • z-space distortion mixes Hubble expansion and peculiar velocities (both positive and negative consequences).
  • Peculiar velocity surveys are the best way to map the matter distribution, but…
    • measuring v’s is difficult and time-consuming;
    • only works nearby, so surveys must cover large areas;
    • hence v-surveys are generally small (~1000 objects), or eclectic compilations of different samples and methods.
the 6df galaxy survey
The 6dF Galaxy Survey
  • The 6dFGS is designed to be the first of a new generation of combined z+v-surveys, combining…
    • A NIR-selected redshift survey of the local universe.
    • A peculiar velocity survey using Dn- distances.
  • Survey strategy…
    • survey whole southern sky with |b|>10°
    • primary z-survey sample: 2MASS galaxies to Ktot<12.75
    • (secondary samples: H<13, J<13.75, r<15.7, b<17)
    • (additional samples: sources from radio, X-ray, IRAS…)
    • v-survey sample: ~15,000 brightest early-type galaxies
the fisher information matrix
The Fisher information matrix
  • The information in a survey of a random field (r) parameterised by ; if the field is Gaussian, then
  • where the power spectrum P is defined by
  • and the effective volume of the survey is
  • The covariance of the discretely sampled field is
  • For P(k) the uncertainty is:

(Fisher matrix)

properties of the fisher matrix
Properties of the Fisher matrix
  • The Fisher matrix, F, …
    • has the conditional error for a parameter on its diagonal;
    • gives the marginalized error for the ith parameter as
    • gives the correlation between measured parameters as
    • the variance in maximum likelihood (minimum variance) parameter estimates is the marginalized error from F.
    • for multiple fields, the covariance matrices of each can be combined to give a joint Fisher matrix.
application to surveys
Application to surveys
  • Burkey & Taylor use the Fisher matrix methods to estimate the uncertainties in estimating cosmological parameters from z- and v-surveys and z+v-surveys.
  • The fields are the z-space density perturbations and the radial gradient of the radial peculiar velocities.
  • The auto- and cross-power spectra of these fields are specified by: the matter power spectrum Pmm(k), the bias parameter bPgg/Pmm=bL2+2/Pmm, the linear redshift-space distortion parameter Ω0.6/b, the Hubble constant H0.
parameters of model
Parameters of model
  • The cosmological parameters used to specify the cosmological model are:
    • the amplitude of the galaxy power spectrum, Ag = b Am
    • the power spectrum shape parameter,  = mh
    • the redshift-space distortion parameter,   Ω0.6/b
    • the mass density in baryons, b (or b = bh2)
    • the correlation between luminous and dark matter, rg
  • Parameters not considered are:
    • the index of the primordial mass spectrum, n (= -1)
    • the small-scale pairwise velocity dispersion, v
parameters of survey
Parameters of survey
  • The parameters of the survey itself enter through the noise terms:
    • the level of shot noise is determined by the number density of galaxies, ng(r), in the z- and v-surveys;
    • the fractional error in the Dn-s relation determines the precision of the peculiar velocities.
  • For the z-survey the operational parameters are sky coverage, fsky; sampling fraction, a; median depth rm
  • For the v-survey the operational parameters are the equivalent set plus s0
optimal z survey design

fsky=0.25

=1

fsky=0.5

fsky=0.75

fsky=1.0

Optimal z-survey design
  • B&T first employ this machinery to determine the depth of a redshift survey that minimizes the error in Ag in fixed time.
  • Other things being equal, want largest possible fsky
  • If Klim 5logrm - 0.255 optimum hemisphere survey has Klim=11.8, a=0.7, rm= 255 Mpc/h
  • Compare with 6dFGS, which has Klim=12.75, a<0.9, rm=150 Mpc/h
recovered power spectrum
Recovered power spectrum

Effective volume

Linear PS for optimal survey, lnk=0.5 bands

shot noise/mode

parameter degeneracies
Parameter degeneracies
  • Degeneracies can be seen by comparing derivatives of the PS w.r.t. the various parameters.
  • Similar curves mean almost degenerate parameters.
  • Ag, , and rg are all ~constant and so ~degenerate.
  •  and b are also similar (both relate to damping of the PS); the effective shape is eff = exp(-2bh)
density field parameters 1
Density field parameters - 1
  • Models with Ag, , 
  • At kmax~0.2 h/Mpc (limit set by non-linear clustering) the uncertainties are 2-3% on all three parameters.
  • Correlations are:
    • very strong between  and  (a change in amplitude can be mimicked by a change in scale);
    • moderate between Ag and , with Ag~Amm0.6.

Fractional marginalized uncertainties

Correlations

Maximum wavenumber (k/h Mpc-1)

density field parameters 2
Density field parameters - 2
  • Models with Ag, , , rg
  • Ag,  are unaffected (errors of 2-3%), but uncertainties on, rg are much larger (~35%)
  • This is due to the strong correlation between  and rg, which results because both parameters affect the normalization of the galaxy PS

Fractional marginalized uncertainties

Correlations

peculiar velocity power spectrum
Peculiar velocity power spectrum
  • Expected 6dFGS 3D velocity PS, lnk=0.5 bands (+effective volume)
  • Larger errors reflect smaller size of survey and 1D peculiar velocities
  • Effective volume for each mode is also shown
optimal v survey design

6dFGS

Optimal v-survey design
  • ‘Optimal’ survey minimizes the error in Av in given time
  • For various fixed fsky, the figure shows the error in Av in terms of the single free parameter, the degenerate variable 0/1/2.

fsky

0.25

0.50

0.75

1.00

20% distances from Dn-

  • Distance errors dominate, and need to be minimized.
  • Sampling should be as complete as possible.
  • Large sky fractions help, but don’t gain linearly.
  • The 6dFGS v-survey should give Av to about 25%.
velocity field parameters
Velocity field parameters
  • Models with Av, .
  • At kmax~0.2 h/Mpc (limit set by non-linear clustering) the uncertainties are ~25% on both parameters.
  • Av and  are strongly anti-correlated (change in normalization can be mimicked by a shift in scale).

Fractional marginalized uncertainties

Correlation

joint z v survey constraints 1
Joint z+v-survey constraints - 1
  • Combine z- and v-survey data and estimate joint constraints from overall Fisher matrix.
  • For models with Ag, ,  the errors are still 2-3% in all three.
  • This is very similar to z-survey, as v-survey does not break the main Ag- degeneracy.

z-onlyz+v

1 contours on pairs of parameters

slide21

Joint z+v-survey constraints - 2

  • For models with Ag, , , rg the errors are still 2-3% in the first three, but <2% in rg.
  • Ag,  are unchanged by v-survey and  has degraded slightly (due to residual correlation with rg).
  • The v-survey greatly improves the joint constraint on  and rg, which are now only relatively weakly correlated.

z-onlyz+v

1 contours on pairs of parameters

scale constraints on r g and b
Scale constraints on rg and b
  • Do the bias or the galaxy/mass correlation vary with scale?
  • Figure shows errors on band estimates of rg and b (each assuming the other is fixed).

Errors in bands(bands shown by dots)

  • If b is fixed, variations in rg can be measured at 5-10% level.
  • If rg is fixed, variations in b can be measured at the few % level over a wide range of scales.
conclusions
Conclusions
  • In terms of constraining cosmological parameters, the major advantage of the 6dFGS is combining the redshift and peculiar velocity surveys to…
    • Break the degeneracy between the redshift-space distortion parameter =0.6/b and the galaxy-mass correlation parameter rg.
    • Measure the four parameters Ag, ,  and rg with precisions of between 1% and 3%.
    • Measure the variation of rg and b with scale to within a few % over a wide range of scales.