Transcript ACTPol Observing the birth and evolution of the Universe through measurements of the fine angular scale temperature and polarization anisotropies in the CMB. AAS, Jan.

ACTPol
Observing the birth and evolution of the
Universe through measurements of the fine
angular scale temperature and polarization
anisotropies in the CMB.
AAS, Jan 7 2010
ACTPol
Measure the CMB between 200<l<10,000 in temperature
and polarization with a new generation of NIST detectors to
understand:
What are the initial conditions of the universe? What is the scalar spectral
index and does it “run” with k? Use TT and then EE spectra at l>2000, in
combination with PLANCK/WMAP.
What is the sum of the masses of neutrinos? Use EE spectrum, lensing, Bmodes, and cross correlations independently.
What is the growth rate of structure? Use gravitational lensing, SZ, KSZ crosscorrelations
Is there cosmic non-Gaussianity? Use high precision high resolution CMB maps.
The proposal builds on significant infrastructure and
investment at NIST, on a unique state-of-the art telescope in
Chile, on a forefront data analysis, and on a dynamic and
engaged team. It complements all other CMB probes.
AAS, Jan 7 2010
ACT
so far…
In the last 6 years our collaboration has:
•Built a 6 meter telescope in northern Chile.
•Built the largest array of mm-wave detectors to observe the sky.
•Developed all the infrastructure (including a hotel and power).
•Brought TDM into the instrumentation mainstream.
•Developed one of the first liquid-cryogen free 0.3K systems.
•Developed AR coated Si lenses.
•Developed a whole new generation of unbiased maximumlikelihood mapmaking and power spectrum estimation techniques.
•Published results and have many papers in progress. AAS, Jan 7 2010
Power Spectrum
Use to determine inflation parameters, cosmological parameters,
the diffuse SZ effect, and foreground effects.
148x148 GHz
The best measurement yet of the fine scale CMB anisotropy, and
the only measurement to connect the linear (l<2000) to the nonAAS, Jan 7 2010
linear regime (l>2000).
Power Spectrum
148x220 GHz
ACT complements Planck, which covers to l=2500, and will
be key for interpreting those data.
AAS, Jan 7 2010
Cluster Science
Use SZ clusters as an unbiased probe of the geometry of
space. The signal is largely independent of redshift. Need to
know the number in a mass range as a function of redshift.
Method:
Find clusters with ACT using SZ effect. We have developed
state-of-the-art filtering techniques.
Confirm and determine redshifts with optical telescopes.
We have observed with APO, SOAR, CTIO, NTT, with proposals in for
LABOCA, Keck, HST, CARMA, VLT, Gemini etc.
Determine mass with X-ray and detailed optical
measures. So far have used RASS, XMM, Chandra data, and are
awaiting SALT.
Coordinated observations with existing telescopes a
large advantage for ACT.
Advanced cluster
finding techniques
New Cluster
Point Source
1.2 deg
Bullet
A3040
AS0592
AS0295
New
New
A3128 NE SPT 0547-4345 New
New
Only
148 GHz
2008
Data
New
New
AS0520 RXC 0217-5244 New
A2941 SPT 0509-4342
24 SZ-Selected Clusters, 13 new
ones. All with optical confirmation.
Many more candidates to be
checked.
Marriage et al. 2010, in prep
Science status and ACTPol
The current camera on ACT (with Planck) will provide the best
measure of ns in TT limited by the ability to remove dusty
galaxies. We will find 100s of clusters, quantify the foreground
emission, and give a rich set of cross-correlations.
ACTPol will have ~5x the instantaneous sensitivity of ACT
With Polarization:
Get the high-l structure of the power spectrum, best path for ns and
related quantities.
Measure gravitation lensing for neutrino mass, high-z w, curvature.
Measure primordial Helium abundance
With Temperature:
Find many more clusters
Measure gravitation lensing
Search for non-Gaussianity, and foregrounds.
AAS, Jan 7 2010
Complementarity to Planck
Planck: sensitive to l=2000 in polarization
ACTPol looks through foregrounds in EE at l>2000 to
get at ns. CMB is more polarized than foreground
emission.
AAS, Jan 7 2010
Small-scale BB polarization.
• Gravitational lensing rotates E
modes into B modes.
Measurements of B modes can
be used to construct the
convergence field.
• Amplitude of convergence field
measures mass fluctuations at z
~ 1-2.
• Get sum of neutrino
masses to ~0.05 eV, the
limit set by neutrino
oscillation measurements.
New detectors from long standing
ACT collaborators at NIST.
NEW COLLABORATION: TRUCE
•Began with a small group in spring 08,
decided soon thereafter to use the
detectors for ABS, rapidly realized these
would be the ideal choice for ACTPol.
(ABS SERVES AS TESTBED FOR
ACTPoL.)
•(Later SPTPol also chose these
detectors, although only ~ 1/4 as many.)
•One of the founding members of the
group, Jeff McMahon, has decided to join
ACTPol as a new faculty member at
Michigan.
Who are we?
A dynamic, diverse, international group who has
gotten together to do great science!
LP, Matt Hilton, Felipe Menanteau, Jack Hughes, Jon Sievers, Polo Infante, Erik Leitch, Toby Marriage, Lucas
Parker, Paula Aguirre, Michele Limon, Tom Essinger-Hileman , Joe Fowler, Bruce Partridge, Brian Calvert, Amir
Hajian, Jeff Klein, Blake Edwards, Suzanne Staggs, Sudeep Das, Matthew Hasselfield, John Appel, Rene
Hlozek,Yen-Ting Lin, Mike Nolta, Vivi Acquaviva, Neelima Sehgal, Carlos Hernandez-Monteagudo,
Trac,
JB
AAS, Hy
Jan
7 2010
Ruin, Kavi Moodley, Carla Carvalho.
V. Acquaviva 1,2
P. Ade 3
P. Aguirre 4
M. Amiri 5
J. Appel 6
E. Battistelli 7,5
J. R. Bond 8
B. Brown 9
B. Burger 5
J. Chervenak 10
S. Das 6,1
M. Devlin 2
S. Dicker 2
W. B. Doriese 11
J. Dunkley 12,6,1
1 Princeton
R. Dunner 4
T. Essinger-Hileman 6
R.P. Fisher 6
J. W. Fowler 6
A. Hajian 6
M. Halpern 5
M. Hasselfield 5
C. Hernandez-Monteagudo 13,2
G. Hilton 11
M. Hilton 14, 15
A. D. Hincks 6
R. Hlozek 12
K. Huffenberger 16,6
D. Hughes 17
J. P. Hughes 18
University Astrophysics (USA)
2 University of Pennsylvania (USA)
3 Cardiff University (UK)
4 Pontifica Universidad Catolica de Chile (Chile)
5 University of British Columbia (Canada)
6 Princeton University Physics (USA)
7 University of Rome “La Sapienza” (Italy)
8 CITA, University of Toronto (Canada)
9 University of Pittsburgh (USA)
10 NASA Goddard Space Flight Center (USA)
11 NIST Boulder (USA)
12 Oxford University (UK)
13 Max Planck Institut fur Astrophysik (Germany)
14 University of KwaZulu-Natal (South Africa)
L. Infante 4
K.D. Irwin 11
N. Jarosik 6
R. Jimenez 19
J.B. Juin 4
M. Kaul 2
J. Klein 2
A. Kosowsky 9
J.M. Lau 20,6
M. Limon 21
Y.T. Lin 22,1,4
R. Lupton 1
T.A. Marriage 1,6
D. Marsden 2
15 South
K. Martocci 23,6
P. Mauskopf 3
F. Menanteau 18
K. Moodley 14
H. Moseley 10
B. Netterfield 24
M.D. Niemack 11,6
M.R. Nolta 8
L.A. Page (PI) 6
L. Parker 6
B. Partridge 25
H. Quintana 4
B. Reid 19,1
N. Sehgal 20,18
J. Sievers 8
D. Spergel 1
S.T. Staggs 6
O. Stryzak 6
D. Swetz 2
E. Switzer 23,6
R. Thornton 26,2
H. Trac 27,1
C. Tucker 3
L. Verde 19
R. Warne 14
G. Wilson 28
E. Wollack 10
Y. Zhao 6
African Astronomical Observatory
of Miami (USA)
17 INAOE (Mexico)
18 Rutgers (USA)
19 Institute de Ciencies de L’Espai (Spain)
20 KIPAC, Stanford (USA)
21 Columbia University (USA)
22 IPMU (Japan)
23 KICP, Chicago (USA)
24 University of Toronto (Canada)
25 Haverford College (USA)
26 West Chester University of Pennsylvania (USA)
27 Harvard-Smithsonian CfA (USA)
28 University of Massachusetts, Amherst (USA)
16 University