Signe Riemer-Sørensen, University of Queensland In collaboration with C. Blake (Swinburne), D....
-
Upload
tyrone-shannon-dorsey -
Category
Documents
-
view
223 -
download
3
Transcript of Signe Riemer-Sørensen, University of Queensland In collaboration with C. Blake (Swinburne), D....
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
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
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
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