Probing Inflation and Dark Energy with the CMB

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Probing Inflation and Dark Energy with the CMB
Super Nova SNAP
?
CMB Galaxy Cluster Surveys APEX-SZ, SPT
CMB Polarization POLARBEAR

• Matt Dobbs
• for the Berkeley CMB group

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Berkeley CMB Team

• excellent National Lab/Campus synergy
• campus maneuverability merged with lab expertise
  in large detector systems
• 30 member group

Senior Scientists John Clarke (LBNL,UCB) William
Holzapfel (UCB) Adrian Lee (LBNL,UCB) Paul
Richards (UCB,SSL) George Smoot
(LBNL,UCB) Helmuth Spieler (LBNL) Martin White
(LBNL,UCB) Engineers John Joseph (LBNL) Chinh
Vu (LBNL)
Scientists Alex Amblard (UCB) Julian Borrill
(LBNL NERSC) Chris Cantalupo (LBNL NERSC) Sherry
Cho (UCB) Matt Dobbs (LBNL) Nils Halverson
(UCB,SSL) Radek Stompor (LBNL NERSC) Huan Tran
(UCB) 12 Graduate Students Few
Undergraduates
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pre-WMAP

• Concordance
• CMB SN1a together provide evidence for Dark
  Energy.

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post-WMAP

• Inflationary Big Bang Model is Alive and Healthy
• OTOT 1.02 0.02
• OMh2 0.1350.008
• Obh2 0.02240.0009
• H0 713 km/s/Mpc
• O? 0.730.04 (WMAP LSS)
• w lt -0.78 (WMAP LSS)
• E-mode Polarization (DASI,WMAP)
• TE ? t 0.170.04, first stars formed earlier
  than expected.

O?
Robust cosmological results arise from a web of
interconnected measurements.
OM
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• Next Generation CMB Experiments
• What is the nature of dark energy?
• measuring w, OM with the galaxy cluster surveys
• How well do we understand Inflation?
• probing inflation with the CMB Polarization

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Science Endorsed by Nat. Review Panels

• Quarks to the Cosmos report questions from the
  Turner panel
• What is the dark matter?
• What is the nature of the Dark Energy?
• How did the universe begin and how did
• its present Large Scale Structure form?
• Barish/Bagger Long Range HEP Planning Report
• origins of dark energy and dark matter are
  important
• components of a broader program of cosmological
• measurements including the CMB and LSS
• more than one approach will be necessary to
• understand the nature of dark energy

Measure Equation of State, w. SNAP APEX-SZ South
Pole Telescope
POLARBEAR CMBpol Satellite
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Galaxy cluster searches

• CMB photons are used to backlight structure in
  the universe.
• 1-2 of CMB photons
• traversing galaxy
• clusters are
• inverse Compton
• scattered to higher
• energy the Sunyaev
• Zeldovich Effect.
• Tool for mapping expansion history

FREQUENCY
FREQUENCY
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Galaxy cluster searches

• optical / X-ray sky?clusters fade away at high
  redshift.

Carlstrom et al.

• SZ observations do not fade away over large
  distances
• ? Clusters can be seen at any distance.

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Atacama Pathfinder Expt (APEX-SZ)

• 16,500 feet in Chilean Andes.
• 12m on-axis ALMA prototype
• Berkeley SZ Receiver
• 330 Bolometer array
• 25 telescope time
• Discover 4000 Clusters/2yrs
• Mass limit gt 4x1014 M0
• First Light Fall 2004.
• LBNL responsible for SQUID electronics readout

UC Berkeley/LBNL, MPI-Bonn/Munich, Cardiff
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South Pole Telescope

• 10m off axis telescope
• Dedicated to CMB observations
• 10x faster mapping than APEX
• deploy January 2007
• Berkeley
• 1000 Bolometer array
• cryogenics
• readout system (LBNL)

Chicago/CWRU/ SAO/UC Berkeley/LBNL
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Galaxy cluster searches
dN/dz for SPT 4000 sq degree Survey (one austral
winter)
Simulation of 1 deg2 of SZ sky
Springel, White, Hernquist astro-ph/0008133
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Gravity Waves from Inflation

• inflationary gravity wave background (IGB)
  provides fingerprint of inflation (1016 GeV)
• imprinted on CMB as curl component of
  polarization signal

TIME
IGB
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Gravity Waves from Inflation

• gravity wave signature encoded in CMB
  POLARIZATION
• factor 10-2 smaller than the temperature
  anisotropy.

Data from DASI 2002 (not sensitive enough for
this)
Example of what gravity waves would look like
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POLARBEAR
Berkeleys flagship CMB experiment.

• 3m off-axis telescope
• first light 2005
• 12000 UC Barcroft Site, White Mountain CA
• 300-1000s Bolometers
• new polarization sensitive antenna coupled
  sensors demonstrated.
• ultimate reach T/Slt 0.001
• probes physics at the highest energy scale.

• Also
• test-bed for CMBpol satellite technology.
• Berkeley co-I for west coast CMBpol
  collaboration

presentation to SAGENAP in April.
P. Ade, S. Cho, J. Clarke, M.A. Dobbs, G.
Engargiola, W. Holzapfel, Z. Kermish, T.
Lanting, A.T. Lee, M. Myers, R. OBrient, P.L.
Richards, H. Spieler
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CMB Polarization
100 µK RMS
Temperature
gradient-mode
4 µK RMS
W. Hu et al. astro-ph/0210096
curl-modes
300 nK RMS
1 degree
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CMB Polarization
gradient-mode
curl-modes
3 years observing (Assuming T/S0.35)

• POLARBEAR Ultimate Sensitivity
• T/S gt 0.0005 (roughly 5x1015 GeV)
• (current limit from SDSS WMAP, T/S lt 0.5 )

• Sufficient resolution to distinguish between
  gravity wave and lensing signals.

• 3 yrs x 25 duty
• 200 nK/pixel
• on 10 x 10 deg2

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Neutrino Mass

• Small angular scale gravitational lensing
• measures the matter content (all matter!, not
  just luminous matter!) along the light of sight.

• neutrinos smooth out the matter distribution on
  small scales causing matter power spectrum to be
  suppressed
• sensitive to sum of neutrino masses
• future CMBpol satellite sensitivity of m?0.03 eV.

Neutrino mass effects enter where linear
perturbation theory applies different from SNAP.
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Technology Drives New Experiments

• new technology advances (largely at Berkeley)
  make these experiments possible.
• LBNL responsible for SQUID readout, signal
  processing, and data acquisition.
• ? See Adrian Lees Talk Tomorrow.

1 mm
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Conclusions

• CMB Science is a cornerstone in a coherent
  program in dark energy and inflation.

• next generation CMB experiments
• probe inflation epoch (1016 GeV)
• this is physics at the highest energy scale (!!)
• measure expansion history using Galaxy Clusters
  surveys (w,O?,OM)
• LBNL key roles
• data analysis (Physics Div, NERSC)
• readout systems (Physics Div)

Super Nova SNAP
?
CMB Galaxy Cluster Surveys APEX-SZ, SPT
CMB Polarization POLARBEAR