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Measuring cosmological parameters. par movies. Using WMAP3 + SDSS LRGs:. 75%. 21%. 4%. Cmbgg OmOl. 386. 430. 13.8. . C = h = G = k b = q e = 1. Cmbgg OmOl. Particle physics. Standard model parameters:. Required. Cosmology. Optional. How flat is space?. Cmbgg OmOl. closed. - PowerPoint PPT Presentation
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Max TegmarkDept. of Physics, MIT
[email protected] en la Playa
January 11-15, 2010
Measuringcosmologicalparameters
par movies
Cmbgg OmOl
Ordinary Matter5%
Dark Energy72%
Cold Dark Matter23%
Ordinary MatterDark EnergyCold Dark MatterHot Dark MatterPhotonsBudget Deficit
4% 21%
75%Using WMAP3 + SDSS LRGs:
430
386
13.8
Cmbgg OmOl
Stan
dard
mod
el p
aram
eter
s:C
osm
olog
yPa
rticl
e ph
ysic
s
Required
Optional
C = h = G
= kb = q
e = 1
Max TegmarkDept. of Physics, MIT
[email protected] en la Playa
January 11-15, 2010
Cmbgg OmOl How flat is space?
flatclosedopen
Why are we cosmologists so excited?
Max TegmarkDept. of Physics, MIT
[email protected] en la Playa
January 11-15, 2010
Cmbgg OmOl How flat is space?
Max TegmarkDept. of Physics, MIT
[email protected] en la Playa
January 11-15, 2010
Cmbgg OmOl How flat is space? Somewhat.
Max TegmarkDept. of Physics, MIT
[email protected] en la Playa
January 11-15, 2010
Cmbgg OmOl tot=1.003How flat is space?
Max TegmarkDept. of Physics, MIT
[email protected] en la Playa
January 11-15, 2010
Cmbgg OmOl
CMB+SN Ia
CMB+LRG
Beth Reid et al, arXiv 0907.1559
Max TegmarkDept. of Physics, MIT
[email protected] en la Playa
January 11-15, 2010
Cmbgg OmOl
CMB+LSS
Max TegmarkDept. of Physics, MIT
[email protected] en la Playa
January 11-15, 2010
Cmbgg OmOl
CMB+LSS
Max TegmarkDept. of Physics, MIT
[email protected] en la Playa
January 11-15, 2010
Cmbgg OmOl
CMB+LSS
Max TegmarkDept. of Physics, MIT
[email protected] en la Playa
January 11-15, 2010
Cmbgg OmOl
CMB+LSS
Max TegmarkDept. of Physics, MIT
[email protected] en la Playa
January 11-15, 2010
Cmbgg OmOl
CMB+LSS
Planck + SDSS: n=0.008, r=0.012
Max TegmarkDept. of Physics, MIT
[email protected] en la Playa
January 11-15, 2010
THE FUTUREIt's tough to make predictions, especially about the future. Yogi Berra
4%
75%
21%
Cosmological data
Cosmological Parameters
4%
75%
21%
Cosmological data
Cosmological Parameters
ARE WE DONE?
4%
75%
21%
Cosmological data
Fundamental theory ?
Cosmological Parameters
Nature of dark matter?
Nature of dark energy?
Nature of early Universe?
Why these particular values?
4%
75%
21%
Cosmological data
Fundamental theory ?
Cosmological Parameters
Nature of dark matter?
Nature of dark energy?
Nature of early Universe?
Why these particular values?
Map our universe!
Max TegmarkDept. of Physics, MIT
[email protected] en la Playa
January 11-15, 2010
Physics with 21 cm
tomography
Max TegmarkDept. of Physics, MIT
[email protected] en la Playa
January 11-15, 2010
Courtney Peterson Andy
Lutomirski
Tongyan Lin
Adrian Liu
Mike matejek
Chris Williams
T H E O M N I S C O P E R S
Max TegmarkDept. of Physics, MIT
[email protected] en la Playa
January 11-15, 2010
Courtney Peterson Andy
Lutomirski
Tongyan Lin
Adrian Liu
Mike matejek
Chris Williams
Ed Morgan
Joel Villasenor
Jackie Hewitt
T H E O M N I S C O P E R S
Scott Morrison
T H E O M N I S C O P E R S
Scott Morrison
Nevada Sanchez
Henrique Pondé
Oliveira PintoJoe
Lee
Angelica de Oliveira-Costa
Max TegmarkDept. of Physics, MIT
[email protected] en la Playa
January 11-15, 2010
Matias Zaldarriaga
T H E O M N I S C O P E R S
• Foreground modeling 0802.1525• Foreground removal astro-ph/0501081, 0807.3952 0903.4890 • Optimal mapmaking 0909.0001• Automatic calibration Liu et al, in prep• Faster correlation 0805.4414, 0909.0001• Corner turning 0910.1351• Survey design optimization 0802.1710
Max TegmarkDept. of Physics, MIT
[email protected] en la Playa
January 11-15, 2010
What are we so excited?
Max TegmarkDept. of Physics, MIT
[email protected] en la Playa
January 11-15, 2010
HistoryCMB
Fore
grou
nd-c
lean
ed W
MA
P m
ap fr
om T
egm
ark,
de
Oliv
eira
-Cos
ta &
Ham
ilton
, ast
ro-p
h/03
0249
6
Our observable universe
LSS
Our observable universe
LSS
The time frontier
Max TegmarkDept. of Physics, MIT
[email protected] en la Playa
January 11-15, 2010
The scale frontier
Physics of the 21 cm Line:
# of Antennas(Total) 30 dishes 10,000 8,192 16 (4)
# of Antennas(Installed) 30 dishes 2,000 (4 Tiles) 512 (32 Tiles) 8 (0)# of Tiles NA 20 (1 Tile=500 ant) 96(1 Tile=16 ant) 512 (1 Tile=16 ant) NA
Effective Area (m2) 5.104 7.0.104 1.0.105 ~ 104 1.0.104 1.0.106
Imaging Field of View 2o 3o - 7.5o ~ 5o 30o - 1o
Angular Resolution 3.8o - 0.4o 3’ 25” - 3.5” ~ 15’ < 0.1’
Frequency Range (MHz) 50 - 1420 50 - 200 10 - 240 80 - 300 110 - 200
Mapping Sensitivity 15mK/(day)1/2
Site India China Netherlands Australia USA/AUS AUS(?)
Year 2007 2007 2007 2008 2008 2015(?)
Experiment GMRT PAST/21CMA LOFAR MWA PAPER SKA
96 V crossed Dipoles
GMRT = Giant Metrewave Radio Telescope
Physics of the 21 cm Line:
# of Antennas(Total) 30 dishes 10,000 8,192 16 (4)
# of Antennas(Installed) 30 dishes 2,000 (4 Tiles) 512 (32 Tiles) 8 (0)# of Tiles NA 20 (1 Tile=500 ant) 96(1 Tile=16 ant) 512 (1 Tile=16 ant) NA
Effective Area (m2) 5.104 7.0.104 1.0.105 ~ 104 1.0.104 1.0.106
Imaging Field of View 2o 3o - 7.5o ~ 5o 30o - 1o
Angular Resolution 3.8o - 0.4o 3’ 25” - 3.5” ~ 15’ < 0.1’
Frequency Range (MHz) 50 - 1420 50 - 200 10 - 240 80 - 300 110 - 200
Mapping Sensitivity 15mK/(day)1/2
Site India China Netherlands Australia USA/AUS AUS(?)
Year 2007 2007 2007 2008 2008 2015(?)
Experiment GMRT PAST/21CMA LOFAR MWA PAPER SKA
96 V crossed Dipoles
21CMA/PaST = Primeval Structure Telescope
Physics of the 21 cm Line:
# of Antennas(Total) 30 dishes 10,000 8,192 16 (4)
# of Antennas(Installed) 30 dishes 2,000 (4 Tiles) 512 (32 Tiles) 8 (0)# of Tiles NA 20 (1 Tile=500 ant) 96(1 Tile=16 ant) 512 (1 Tile=16 ant) NA
Effective Area (m2) 5.104 7.0.104 1.0.105 ~ 104 1.0.104 1.0.106
Imaging Field of View 2o 3o - 7.5o ~ 5o 30o - 1o
Angular Resolution 3.8o - 0.4o 3’ 25” - 3.5” ~ 15’ < 0.1’
Frequency Range (MHz) 50 - 1420 50 - 200 10 - 240 80 - 300 110 - 200
Mapping Sensitivity 15mK/(day)1/2
Site India China Netherlands Australia USA/AUS AUS(?)
Year 2007 2007 2007 2008 2008 2015(?)
Experiment GMRT PAST/21CMA LOFAR MWA PAPER SKA
96 V crossed Dipoles
LOFAR = Low Frequency ARray
2 Km
100 Km
32 sta.
77 sta. vv
vv
vv
vv
Physics of the 21 cm Line:
# of Antennas(Total) 30 dishes 10,000 8,192 16 (4)
# of Antennas(Installed) 30 dishes 2,000 (4 Tiles) 512 (32 Tiles) 8 (0)# of Tiles NA 20 (1 Tile=500 ant) 96(1 Tile=16 ant) 512 (1 Tile=16 ant) NA
Effective Area (m2) 5.104 7.0.104 1.0.105 ~ 104 1.0.104 1.0.106
Imaging Field of View 2o 3o - 7.5o ~ 5o 30o - 1o
Angular Resolution 3.8o - 0.4o 3’ 25” - 3.5” ~ 15’ < 0.1’
Frequency Range (MHz) 50 - 1420 50 - 200 10 - 240 80 - 300 110 - 200
Mapping Sensitivity 15mK/(day)1/2
Site India China Netherlands Australia USA/AUS AUS(?)
Year 2007 2007 2007 2008 2008 2015(?)
Experiment GMRT PAST/21CMA LOFAR MWA PAPER SKA
96 V crossed Dipoles
MWA = Murchison Widefield Array
Physics of the 21 cm Line:
# of Antennas(Total) 30 dishes 10,000 8,192 16 (4)
# of Antennas(Installed) 30 dishes 2,000 (4 Tiles) 512 (32 Tiles) 8 (0)# of Tiles NA 20 (1 Tile=500 ant) 96(1 Tile=16 ant) 512 (1 Tile=16 ant) NA
Effective Area (m2) 5.104 7.0.104 1.0.105 ~ 104 1.0.104 1.0.106
Imaging Field of View 2o 3o - 7.5o ~ 5o 30o - 1o
Angular Resolution 3.8o - 0.4o 3’ 25” - 3.5” ~ 15’ < 0.1’
Frequency Range (MHz) 50 - 1420 50 - 200 10 - 240 80 - 300 110 - 200
Mapping Sensitivity 15mK/(day)1/2
Site India China Netherlands Australia USA/AUS AUS(?)
Year 2007 2007 2007 2008 2008 2015(?)
Experiment GMRT PAST/21CMA LOFAR MWA PAPER SKA
96 V crossed Dipoles
Cas A
3C 392
Cygnus A
PAPER = Precision Array to Probe Epoch of Reionization
Physics of the 21 cm Line:
# of Antennas(Total) 30 dishes 10,000 8,192 16 (4)
# of Antennas(Installed) 30 dishes 2,000 (4 Tiles) 512 (32 Tiles) 8 (0)# of Tiles NA 20 (1 Tile=500 ant) 96(1 Tile=16 ant) 512 (1 Tile=16 ant) NA
Effective Area (m2) 5.104 7.0.104 1.0.105 ~ 104 1.0.104 1.0.106
Imaging Field of View 2o 3o - 7.5o ~ 5o 30o - 1o
Angular Resolution 3.8o - 0.4o 3’ 25” - 3.5” ~ 15’ < 0.1’
Frequency Range (MHz) 50 - 1420 50 - 200 10 - 240 80 - 300 110 - 200
Mapping Sensitivity 15mK/(day)1/2
Site India China Netherlands Australia USA/AUS AUS(?)
Year 2007 2007 2007 2008 2008 2015(?)
Experiment GMRT PAST/21CMA LOFAR MWA PAPER SKA
96 V crossed Dipoles
SKA = Square Kilometer Array
Max TegmarkDept. of Physics, MIT
[email protected] en la Playa
January 11-15, 2010
Image: FORTE satellite
MWA
PAST/21CMALOFAR GMRTPAPER
SKA ?
21 cm tomography experiments:
Participants: MIT, Harvard, Washington, Berkeley, JPL, NRAO
PI: Jacqueline Hewitt, MIT
LARC: Lunar Array for Radio Cosmology
The Omniscope
MT & Matias Zaldarriaga, arXiv 0805.4414 [astro-ph]
Single-dish telescope:cost A1.35
Sensitivity T (A)-1/2
Interferometer:cost N2 A2
FFTT telescope idea:cost A, ~2
Telescopes as Fourier transformers
How get huge sensitivity at low cost?
Max TegmarkDept. of Physics, MIT
[email protected] en la Playa
January 11-15, 2010
QuickTime™ and a decompressor
are needed to see this picture.
Max TegmarkDept. of Physics, MIT
[email protected] en la Playa
January 11-15, 2010 Tegmark & Zaldarriaga 2008
The sensitivity frontier
Omniscope
LSS
Our observable universe
LSS
Our observable universe
Mao, MT, McQuinn, Zahn & Zaldarriaga 2008
Spatial curvature:WMAP+SDSS: tot= 0.01 Planck: tot= 0.00321cm: tot=0.0002
LSS
Our observable universe
Spectral index running:Planck: =0.00521cm =0.000172-potential: 0.00074-potential: 0.008
Mao, MT, McQuinn, Zahn & Zaldarriaga 2008
LSS
Our observable universe
Mao, MT, McQuinn, Zahn & Zaldarriaga 2008
Neutrino mass:WMAP+SDSS: m <0.3 eV+LyF: m <0.17 eV Oscillations m>0.04 eVFuture lensing: m~0.03 eV21cm: m=0.007 eV
