Signe Riemer-Sørensen, University of Queensland In collaboration with C. Blake (Swinburne), D. Parkinson (UQ), T. Davis (UQ) and the WiggleZ collaboration.

Signe Riemer-Sørensen, University of QueenslandIn collaboration with C. Blake (Swinburne), D. Parkinson

(UQ), T. Davis (UQ) and the WiggleZ collaboration

COSMOLOGICAL NEUTRINO MASS CONSTRAINT FROM THE WIGGLEZ DARK ENERGY SURVEY

Hubble Space Telescope and particlezoo.net

ICHEP 2012 Melbourne

Neutrinos Exactly mass-less in Standard Model Oscillations imply mass:

Atmospheric and accelerator neutrinos: Dm32

2 ≈ 3×10-3 eV2

Solar and reactor neutrinos:

Dm122 ≈ 8×10-5 eV2

One species > 0.05 eV

mne < 2.05 eV (beta decay)

Cannot (yet) measure absolute mass!

particlezoo.net

13.7 billion years of history

http://map.gsfc.nasa.gov/

13.7 billion years of history

http://map.gsfc.nasa.gov/

13.7 billion years of history

http://map.gsfc.nasa.gov/

Neutrinos and structures Relativistic when decoupling Velocities decay with

expansion Spreading out gravitational

potential Heavy neutrinos = strong

suppression over short range Light neutrinos = weak

suppression over long range

Measure of structure

nedwww.ipac.caltech.edu

3D galaxy map

Hubblesite.org

Power spectrum

heavier neutrinoslighter neutrinos

Fig

ure:

Tam

ara

Dav

is

Large scales Small scales

Pro

port

iona

l to

num

ber

of g

alax

ies

Previous results Cosmic Microwave Background (CMB)

Sm u < 1.3eV (Komatsu 2010)

CMB+Sloan Digital Sky SurveySm u < 0.62eV (Reid 2010)

CMB+SDSS+Lyα Sm u < 0.28eV (Seljak 2006)

Require strong assumptions

Remember: Lower limit is Smu > 0.05eV

WiggleZ Dark Energy Survey 3D galaxy map from Anglo Australian

Telescope (AAT) 238,000 star-forming blue emission line

galaxies 4 redshift bins, z = 0.1-0.9

http://wigglez.swin.edu.au/Michael Drinkwater and David WoodsChris Blake

WiggleZ Dark Energy Survey 3D galaxy map from Anglo Australian

Telescope (AAT) 238,000 blue emission line galaxies Redshift 0.1-0.9, 4 bins

http://wigglez.swin.edu.au/Michael Drinkwater and David WoodsChris Blake

7 equatorial fields, each 100-200 deg2

>9° on side, ~3 x BAO scale at z > 0.5

Physical size ~ 1300 x 500 x 500 Mpc/h

Southern Hemisphere Surveys

GiggleZ simulations

Gigaparsec WiggleZ Survey Simulations 21603 particles 1 Gpc3

Resolve 1.5x1011Msun/h

Power spectra

z=0.4-0.8

Matter and movement Bias

Galaxies does not trace dark matter directly

WiggleZ bias linear, marginalise over scaling

Matter and movement Bias

Galaxies does not trace dark matter directly

WiggleZ bias linear, marginalise over scaling

Figure: John Peacock

Redshift Space DistortionsPeculiar velocities due to

structures affect redshift to distance conversion

Simulated halos

Massive highly biased galaxies

at z = 0.2

WiggleZ galaxies at

z = 0.2

WiggleZ galaxies at z = 0.6

Importance of modeling

LinearHalofit

Jennings et al. fitting formulaJennings et al. with zero velocity

Empirical dampingN-body calibrated

Model selection Fitting

simulated power spectrum

Ability recover input parameters

Quality of fit for input parameters

Simulation calibrated model Similar to Reid et al. but calibrated to GiggleZ

bias

Halofit non-wiggly

Acoustic peaks and their broadening

Non-linear effects from GiggleZ scaled to cosmology

Results

Sloan Digital Sky Survey (110000 galaxies)

Sm u < 0.62eVWiggleZ (240000 galaxies)

Sm u

< 0.60eVWiggleZ+H0+Baryonic Acoustic Oscillations

Sm u < 0.29eV

Recent development

Sloan Digital Sky Survey-III1 mio photometric redshifts (low resolution)Sm u < 0.30 eV (de Putter et al. Jan 2012)

Galaxy clusters, South Pole TelescopeX-ray luminosity-mass relationSm u < 0.28 eV (Benson et al. Dec 2011)

Hubble parameter measurementsMeasure expansion as function of redshiftSm u < 0.48 eV (Moresco et al. Feb 2012)

Future

Euclid (ESA launch 2019)1.5 mio galaxies spectraSm u < 0.1 eV S

choo

lwor

khe

lper

.ne

t

ska.gov.au

Square Kilometer Array (2024)Use hydrogen to detect galaxiesSm u < 0.05 eV -> measurement

web.mit.edu KATRINBeta-decaymue < 0.2 eV

Summary Neutrino mass unknown Mass imprints on galaxy

distribution WiggleZ+WMAP+BAO

Sm u < 0.29eVRiemer-Sørensen et al, arXiv:1112.4940

Stay tuned for data release and CosmoMC module I’LL BE WORKING ON THE LARGEST AND

SMALLEST OBJECTS IN THE UNIVERSE – SUPER CLUSTERS AND NEUTRINOS. I’D LIKE YOU TO HANDLE EVERYTHING IN BETWEEN”

WiggleZ highlights WiggleZ survey info

Drinkwater et al. 2010 MNRAS 401(3), 1429 http://wigglez.swin.edu.au/

WiggleZ selection function and power spectrum Blake et al. 2010, MNRAS 406(2), 803

Growth of structure, using Redshift space distortions Blake et al. 2010, MNRAS (in press: 1104.2948)

H(z), using Alcock-Paczynski effect (sphericity of spheres) Blake, Glazebrook, Davis et al. (submitted)

DA(z), using Baryon Acoustic Oscillations (standard rulers) Blake, Davis et al. 2011, MNRAS (in press: 1105.2862) Blake, Kazin, Beutler, Davis et al. (submitted)

Neutrino mass, structure damping on small scales Riemer-Sørensen, Blake, Parkinson, Davis et al. (submitted)

DA(z) and H(z), using 2D BAO’s Davis, Blake et al. (in prep)

Homogeneity of the universe, using number density Scrimgeour, Davis et al. (submitted)

Growth of structure from redshift space distortions

Baryonic Acoustic Oscillations

Acceleration from Alcock-Paczynski effect

particlezoo.net

Example spectrum z=0.72

Hβ, OIIIOII

This light was emitted

6.5 billion years ago

Sidestep: Neutrino dark matter

Weakly interacting Not emitting light Too few and too light