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High Resolution Measurements of CMB Anisotropies with ACBAR
U.C. Berkeley:W.L. Holzapfel (co-PI)M.D. DaubM. LuekerCase-Western:J. Ruhl (co-PI)J. GoldsteinJPL/Caltech:J.J. BockC.L. KuoA.E. LangeC. Reichardt
CMU:J.B. PetersonSussex:A.K. RomerL. ValkonenCardiff:P.A. AdeAround the WorldM.C. Runyan
ACBAR is funded by the NSF Office of Polar Programs
ACBAR Collaborators
ACBAR was built to:
(Gomez et al. 2003)
Measure the CMB temperature anisotropies
Search for new SZ clusters
Make targeted multi- SZ
observations of clusters.
(White, Hernquist, & Springel 2002)
ACBAR’scoverage
WMAP
CMB Power Spectrum• CMB physics is well-understood
and calculable (linear regime: cdm~10-3)
• Experiments measure exactly what theory predicts!
• What is the universe made of?• What drives its dynamics? • How did structure form?
(C. Lineweaver, 2003)
Plasma falling into a dark matter overdensity
The Damping TailPhoton diffuse out of over-dense regions & carry baryons with them. The acoustic oscillator has a Q~5.The damping scale measures theangular scale of Silk length at recombination: Silk length ~ 3.5 Mpc (m/ b)1/2 (mh2)-3/4
An independent measure of cosmological parameters
•Break degeneracies•Test for new physics
(W. Hu, 2002)
ACBAR:
Instrument and Observations
Winterover
Special Thanks to our Crazy Winter-overs
Helium fill:Winter 2002
Matt Newcomb, 2001 & 2002
Justus Brevik 2004
Jessica Dempsey2005
Cooled to 230mKHe3/He3/He4Fridge
24-hour hold time
Arcminute Cosmology Bolometer Array Receiver
4K
350mK
230mK
FET
120K
JPL MDL Bolometers
16-element arrayCorrugated feed horns
Picture and bolometer provided by JPL Microdevices Lab ACBAR Bolometers
•Fast (~3 ms)
•Broadband
•Very sensitive
Map 1 deg2 to 10 K per beam at 150 GHz in ~3h.
# Band
(GHz)
TRJ
(K)
NETCMB
(Ks)
8x(added 2005)
150 34 330
8x 150 39 345
The Viper TelescopeSchematic diagram of the optics (2m off-axis Gregorian)
Triangular wave 0.3 Hz, 3ºpeak to peak
Large Chop (~3˚)+ small beams = wide -range
Ground shield blocks emission from EL < 25˚
Optimizing the Analysis
CMB5 FieldWinter 2002
CMB5 field, M-(L+T)/2
CMB5, un-differenced
Cosmic Variance:3x area
Noise:S/N improves by 8/3
No-LMTScan with nearly constant elevation
CalibrationQuickTime™ and a
TIFF (LZW) decompressorare needed to see this picture.
CMB DipoleWMAP
Boomerang
ACBAR
Galactic sources mapped multiple times per day.
Used to construct
pointing model and calibration
Raster map of RCW38
B03 observed RCW38 at 150
GHz too!
6% calibrationin temperature
Foregrounds
Avoids foregrounds:• Dust• Radio sources
Plenty of low-dust sky available year-round
Radio sources: cmb5
Sources in the PMN radio source catalogue are removed in the PS analysis.
Monitor beam size and pointing with mm-bright point sources in each field.
Black: ACBAR new analysisRed: ACBAR 2002 releaseRed: ACBAR 2002 releaseGreen: CBIGreen: CBI
No-LMT Power Spectrum – preview•New analysis method (no-LMT)•Improved calibration •2x more sky
More to come from ACBAR!
2004: 5 months of observationInstrument unchanged from 2002
2005: Full winter of observationReconfigured the focal plane to double the number of detectors at 150 GHz
6.5x More Sky&
3.7x More Time!ACBAR B03
Improved Calibration
Portion of B03 Deep Field
Full ACBAR Dataset
• Measure the higher acoustic peaks and damping tail of the power spectrum with high signal-to-noise
• Improve calibration by factor of 2-3 – Even better with
WMAP 4th year!
Improve estimates of m, b, ns, dns/dlnk …
QuickTime™ and aTIFF (LZW) decompressor
are needed to see this picture.
Hu, 2001, ApJL
Lensing probes the large scale matter distributionusing smaller objects with known (average) shape
The growth of large scale structure depends critically on dark energy
Challenge: CMB is a gaussian random field w/o fixed shape
Unlensed Lensed
ACBAR’s deep fieldsshould have 2-3 sigma detection.
Really Massive Source
Lensing
CBI’s High- Excess
•Point Sources–Radio sources–dusty galaxies
•Non-standard Inflation
•SZE
355 103 K2 at 30 GHz
Cooray & Melchiorri, 2002astro-ph/0204250
Predictions: Non-standard inflation: power equal at 150 GHzSZ excess: power reduced by ~4 at 150 GHz
QuickTime™ and aTIFF (LZW) decompressor
are needed to see this picture.
High- Excess?
SZ results in a ratio 4 for the observed powers.
• Looking good: SZE from clusters, SZE from pop. III stars..
• NOT looking good: primordial magnetic fields, primordial voids…
SZ
Primordial…CBI
BIMA
ACBAR
Goldstein et al. astro-ph/0212517
Dawson et al.
LMT Analysis: consistent with either
Reanalysis (no-lmt) of 2002 Data
Summary
• ACBAR has measured CMB temperature anisotropies with high S/N to > 2000– Paper coming out soon
• Analysis is underway to:– Calibrate with CMB anisotropies to WMAP and B03– Improved power spectrum measurement by including nearly
4x more data and 7x more sky from last winter.
– Detect Gravitational Lensing
– SZ clusters• Pointed Observations• Blind search for unknown clusters
The End