ichep 2012 melbourne
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ICHEP 2012 Melbourne. Cosmological Neutrino mass constraint from the WiggleZ Dark Energy Survey. Signe Riemer-Sørensen, University of Queensland In collaboration with C. Blake (Swinburne), D. Parkinson (UQ), T. Davis (UQ) and the WiggleZ collaboration. - PowerPoint PPT PresentationTRANSCRIPT
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:Dm12
2 ≈ 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
Figu
re: T
amar
a D
avis
Large scales Small scales
Pro
porti
onal
to n
umbe
r of g
alax
ies
Previous results Cosmic Microwave Background (CMB)
Smu < 1.3eV (Komatsu 2010) CMB+Sloan Digital Sky Survey
Smu < 0.62eV (Reid 2010) CMB+SDSS+Lyα
Smu < 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 > 0.5Physical size ~ 1300 x 500 x 500 Mpc/hSouthern Hemisphere Surveys
GiggleZ simulations Gigaparsec WiggleZ Survey Simulations 21603 particles 1 Gpc3
Resolve 1.5x1011Msun/h
Power spectraz=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
ResultsSloan Digital Sky Survey (110000 galaxies)
Smu < 0.62eVWiggleZ (240000 galaxies)
Smu
< 0.60eVWiggleZ+H0+Baryonic Acoustic Oscillations
Smu < 0.29eV
Recent development Sloan Digital Sky Survey-III
1 mio photometric redshifts (low resolution)Smu < 0.30 eV (de Putter et al. Jan 2012)
Galaxy clusters, South Pole TelescopeX-ray luminosity-mass relationSmu < 0.28 eV (Benson et al. Dec 2011)
Hubble parameter measurementsMeasure expansion as function of redshiftSmu < 0.48 eV (Moresco et al. Feb 2012)
Future Euclid (ESA launch 2019)
1.5 mio galaxies spectraSmu < 0.1 eV S
choo
lwor
khel
per.n
et
ska.gov.au
Square Kilometer Array (2024)Use hydrogen to detect galaxiesSmu < 0.05 eV -> measurement
web.mit.edu KATRINBeta-decaymue < 0.2 eV
Summary Neutrino mass unknown Mass imprints on galaxy
distribution WiggleZ+WMAP+BAO
Smu < 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