1. The Cosmic Background at High l
Experimental Overview
Steven T. Myers
National Radio Astronomy Observatory
Socorro, NM

2. Courtesy Wayne Hu – http://background.uchicago.edu
The march of progress
Courtesy Wayne Hu –

3. Courtesy Wayne Hu – http://background.uchicago.edu
After WMAP…
Power spectrum
measured to l < 1000
Primary CMB
First 3 peaks
Courtesy Wayne Hu –

4. Courtesy Wayne Hu – http://background.uchicago.edu
…and Planck
Power spectrum
measured to l < 1000
Primary CMB
First 6 peaks
Courtesy Wayne Hu –

5. A Theoretical Digression

6. Secondary Anisotropies
Courtesy Wayne Hu –

7. Gravitational Secondaries
Due to CMB photons passing through potential fluctuations (spatial and temporal)
Includes:
Early ISW (decay, matter-radiation transition at last scattering)
Late ISW (decay, in open or lambda model)
Rees-Sciama (growth, non-linear structures)
Tensors (gravity waves, ‘nuff said)
Lensing (spatial distortions)
Courtesy Wayne Hu –

8. Courtesy Wayne Hu – http://background.uchicago.edu
CMB Lensing
Distorts the background temperature and polarization
Converts E to B polarization
Can reconstruct from T,E,B on arcminute scales
Can probe clusters
Courtesy Wayne Hu –

9. Scattering Secondaries
Due to variations in:
Density
Linear = Vishniac effect
Clusters = thermal Sunyaev-Zeldovich effect
Velocity (Doppler)
Clusters = kinetic SZE
Ionization fraction
Coherent reionization suppression
“Patchy” reionization

10. Courtesy Wayne Hu – http://background.uchicago.edu
Vishniac Effect
Reionization + Structure
Linear regime
Second order (not cancelled)
aka Ostriker-Vishniac effect
Courtesy Wayne Hu –

11. Patchy Reionization Structure in ionization Effects similar
Can distinguish between ionization histories
Confusion, e.g. kSZ effect
e.g. Santos et al. ( )
Effects similar
kSZ, OV, PReI
Different z’s, use lensing?

12. 2ndary SZE Anisotropies
Spectral distortion of CMB
Dominated by massive halos (galaxy clusters)
Low-z clusters: ~ 20’-30’
z=1: ~1’  expected dominant signal in CMB on small angular scales
Amplitude highly sensitive to s8
pengjie map is 1.19 deg x 1.19 deg; color scale is dT/T=-2y
A. Cooray (astro-ph/ )
P. Zhang, U. Pen, & B. Wang (astro-ph/ )

13. The Experiments

14. Experimental State of the Art
Sunyaev Zeldovich Array (SZA)
South Pole Telescope (SPT)
ACBAR
BIMA
BLAST
Green Bank Telescope / Penn Array
ALMA
CBI

15. The SZ Array
&
South Pole Telescope
J. Carlstrom et al.

16. Courtesy J. Mohr - http://cosmology.astro.uiuc.edu/~jmohr/
The SZA (Carlstrom)
8 antennas, 3.5m diameter, 30 GHz
CARMA site in CA
6 x 10.4m OVRO
11 x 6m BIMA
Combined array
Courtesy J. Mohr -

17. Courtesy J. Mohr - http://cosmology.astro.uiuc.edu/~jmohr/
SZE Surveys (e.g. SZA)
Exploit redshift-independence of SZE
Massive clusters – high bias, tail of distribution
Probe dark energy
Competing effects:
Volume vs. redshift
Growth of structure vs. redshift
Problems
Uncertain Mass/SZE relation
Redshifts
Confusion (w/CMB, lower mass objects)
Courtesy J. Mohr -

18. South Pole Telescope (Carlstrom)
8 meter telescope, off-axis
1027 element bolometer arrays
@ 90, 150, 217, 270 GHz
Survey 4000 sq. deg with 1.3’ pixels at 150 GHz
Spiderweb TES bolometers (Adrian Lee)
Courtesy J. Mohr -

19. ACBAR

20. The Arcminute Cosmology Bolometer Array Receiver
U.C. Berkeley:
W.L. Holzapfel (co-PI)
M.D. Daub
C.L. Kuo
M. Lueker
M. Newcomb
D. Woolsey
C. Cantalupo
Case-Western:
J. Ruhl (co-PI)
J. Leong
Caltech:
A.E. Lange
C. Reichardt
M.C. Runyan
UCSB:
J. Goldstein
E. Torbet
CMU:
P. Gomez
J.B. Peterson
A.K. Romer
Cardiff:
P.A.R. Ade
C.V. Haynes
C. Tucker
JPL:
J.J. Bock
A.D. Turner
ESA:
R.S. Bhatia
G.I. Sirbi
ACBAR is funded by the NSF Office of Polar Programs

21. Overview of ACBAR:
ACBAR Instrument
16-pixel, multi-frequency, 240 mK, millimeter-wave bolometer array.
Observes from 2m Viper telescope at the South Pole with 4-5 beams.
2002 Winter Crew
Bands, filters, detectors, and angular resolution similar to Planck HFI.
Assembled: Fall 2000
Installed: January 2001
Upgraded: December 2001
Observed through Nov 2002

22. Frequency Bands: Configurable to observe simultaneously at:
Thermal SZ (y=10-4)
Frequency Bands:
Configurable to observe simultaneously at:
Bands located at peak intensity of CMB anisotropies and across the SZ thermal null.
 
150 GHz GHz (20%)
220 GHz GHz (14%)
280 GHz GHz (18%)
350 GHz GHz (7%)
100 K
CMB
Avoids foregrounds:
Dust
Radio sources
Atmosphere
Model of SP atmospheric transmission

23. Panel lowers for low-EL observations
Viper Telescope: 2m off-axis Gregorian
Chopping flat at image of primary formed by secondary
Skirt reflects primary spill-over to sky.
Ground shield blocks emission from EL< 25º.
Panel lowers for low-EL observations
Large AZ chop (~3°)
+ small beams (~4-5)
= broad -space coverage
(~75 to 3000)

24. Beams and Calibration: 2002: Venus 2001: Mars
band FWHM
150 GHz 
220 GHz 
280 GHz 
350 GHz 
2001: Mars
band FWHM
150 GHz 
220 GHz 
280 GHz 

25. 2001 & 2002 Observations: Centered fields on mm-bright point sources.
(Finkbeiner, Davis, & Schlegel, 1999)
150 GHz Dust Model
Centered fields on mm-bright point sources.
Each field is ~18 deg2.
Point source provides monitor of pointing and beams. Coadded point source image includes beam size and pointing jitter.
FIELD (PMN object) RA (J2000) DEC Time (d) 150/beam
CMB2 (J ) ~9K
CMB5 (J ) ~5K
CMB6 (J ) —
CMB7 (J ) —

26. CMB2 Field (~10 deg2) Mostly from 2001 150 GHz
Temperature Map
150 GHz
Lead/Main/Trail
Subtracted to
Remove Scan
Synchronous
Offsets
Noise Map
S/N~40 on
degree scale
structure

27. CMB5 Field
Winter 2002
Highest S/N
Map of the
CMB
to date
S/N~100
On degree
scale
structure

28. LBNL-NERSC Supercomputer tackles number crunching
ACBAR Power spectrum before/after foreground subtraction
IRAS Dust Template
102(CMB2)+68(CMB5) PMN Radio Sources

29. Kuo et al. astro-ph/ 0212289 ACBAR VS. the World Pre-WMAP Sample
Variance
dominated
Noise
Dominated
ACBAR
VS.
the World
Pre-WMAP

30. First ACBAR
Cluster
Image: A3266
z=.0545
Tx=6.2 keV
Lx=9.5x1044
Requires
Multi-frequency
Data to Subtract
CMB

31. ACBAR So Far: Completed 2nd year of observations.
Instrument performing well and meeting specifications.
Power spectrum and cosmological parameters based on two fields just released (astro-ph/ , ).
Analysis of power spectrum from two times more sky underway.
Deep pointed observations of the nine brightest REFLEX clusters accessible from the Pole.
Analysis of pointed SZ cluster observations and SZ cluster search is in progress.

32. Future Plans for ACBAR:
2003:
2004:
1/2 year with instrument unchanged from 2002 configuration. More sky coverage and more clusters.
Reconfigure focal plane to match mapping sensitivities at 150 and 220 GHz.
Separate primary CMB and SZ!
Measure SZ power spectrum
Improve ability to find unknown SZ clusters in blank fields.

33. W. Holzapfel, J. Carlstrom
BIMA
W. Holzapfel, J. Carlstrom

34. BIMA Survey
of Arcminute Scale
CMB Anisotropy

35. BIMA Observations 9 Telescopes in Compact Array
28.5 GHz Observing Frequency
6.6’ FWHM
~150 μJy/beam RMS (u-v < 1.1 kλ)
15 μK for 2’ Synthesized Beam

36. CL , z = 0.55
X-Ray
SZE:  = 15 K, contours =2

37. Sample from 60 OVRO/BIMA imaged clusters,
0.07 < z < 1.03

38. BIMA Blank Field Survey
BDF3
Time ~60 hours
u-v = kl,
Beam=18”X25”
RMS ~ 150mJy/beam
u-v = kl,
Beam=99”X116”
RMS ~ 150mJy/beam ~ 15mK
Now have 18 fields
Of comparable depth
Selected for low dust
contrast.

39. Window Functions for the two BIMA band powers

40. VLA Observations
Identify Radio Point Source Contaminants with Deep Observations at 4.8 GHz
1.5 hrs per Field, All 10 fields have been imaged
~25 μJy/beam RMS, 9’ FWHM beam
6s source positions used to project out in covariance matrix

41. Comparison with Models for SZ power Spectrum
Includes sample variance
Statistical error only
Dawson et al. ApJ 581, 86D 2002

42. Cosmological Constraints
Komatsu, 2002.

43. Summary
1. Observations with the BIMA array have resulted in a significant detection of excess power on the scales at which the SZ effect is expected to dominate
2. The measured anisotropy is consistent with a σ8 = cosmology.
3. Analysis of the BIMA image statistics and follow-up optical observations are in progress to determine the source of the excess power.

44. BLAST

45. Balloon-borne Large Aperture Submillimeter Telescope
BLAST
Balloon-borne Large Aperture
Submillimeter Telescope
University of Pennsylvania
Brown University
University of Miami
JPL
University of Toronto
University of British Columbia
INAOE – Mexico
Cardiff University

46. The Sub-millimeter Background is Largely Unexplored Territory

47. BLAST Telescope and Detector Parameters
State-of-the-art
detectors
SPIRE assembly
Compact arrays
LDB flight
High-altitude
telescope
JPL
Spiderweb
bolometers

48. Simulated Sky at 250 microns Smoothed to BLAST Beams
BLAST Telescope and Detectors Combine to Give Impressive Mapping Capabilities
BLAST Array Coverage
6.5 X 13 arcmin
Simulated Sky at 250 microns
Smoothed to BLAST Beams

49. The Star Formation History of the Universe
BLAST will make maps of the sub-millimeter sky covering
1-10 sq. deg.
Steidel 2000

50. Star Formation History
Steidel
Madau
Lilly (SCUBA)
Compilation from Blain 2002

51. Evidence for High Star Formation Rates at High - z
Peak in AGN activity at z=2-3 implies that massive structures exist at high-z. (At low-z, powerful AGN reside in the most massive galaxies; > 5 L* , M > 5 x 1011 M)
At z=3, the Universe is 2 Gyrs old. This requires SFR > 250 M/yr to build massive galaxies.
Lyman drop-out galaxies at z~3 show SFRs ~ ~5 -50 M/yr (accounting for dust obscuration)
Old elliptical galaxies exist at z = 1.5 with ages of 3-4 Gyrs
The current sensitivities of sub-mm surveys only allows the detection of luminous (> 1012 L) starburst galaxies with SFRs > 100 M/yr

52. Can You Find the Galaxy?
I/K band observations with SCUBA 850 m and candidate counterparts
Results are inhibited by uncertainties in identification and redshift determination
25” panels (from Smail 2002)

53. Photometric Redshifts in Sub-mm
Z = 4
BLAST
Z = 0.1
SCUBA

54. Strong Negative k-correction Saves the Day
Negative k-correction produces a “constant” sub-mm flux for a galaxy of fixed luminosity with increasing redshift.

55. LOTS and LOTS of Galaxies Later……
The expected error is dominated by the range in SED models

56. Science Goals of BLAST + Extragalactic Surveys 250-500 m
Wide (shallow) and narrow (confusion–limited)
extragalactic surveys –
BLAST will identify the galaxy populations responsible for producing the far-IR and sub-mm backgrounds. BLAST will also determine the amplitude of clustering of sub-mm galaxies on scales of 0.1 – 10 degrees.

57. Science Goals of BLAST + + + Extragalactic Surveys 250-500 m
Sub-mm Source
Counts + +
Measure SEDs
Measure sub-mm source counts -
BLAST will place the strongest constraints to date on evolutionary models and global star formation history of starburst galaxies at high redshift.

58. 50 hour 250 m LDB Survey Strategies
Galaxy Counts
Survey Area
(sq. deg)
1 depth
mJy
# of pixels
# of Gal.
> 5
> 10
# of 5 Gal.
Z > 1
Z > 3
1.0 5
18334
835
265
765
147
2.0 7
36668
1012
291
927
151
4.0 10
73336
1100
294
988 36 30
660024
990
246
895
105
The depth of the surveys can be adjusted to address different science goals.
The number of galaxies detected at 5  will be more than 20 times the total number of 5  sources detected by SCUBA in the last 4 years.

59. Fast Return on Science 500 m array Test pointing and star tracker
First North American flight in 2003
500 m array
Test pointing and star tracker
First LDB flight in 2003
BLAST Gondola

60. A 3 Millimeter Array Receiver For the GBT
PENN Array :
A 3 Millimeter Array Receiver For the GBT
PI: Mark Devlin (Upenn)
GBT: Brian Mason

61. The GBT is BIG…..Really BIG
100 by 110 m off-axis Gregorian system
unblocked aperture
interchangeable receivers
2000 panels
Active Surface good to 100 GHz

62. After we include the efficiency of the receiver this is:
3 mm Receiver on the GBT
In phase III the GBT will have an effective surface area of ~2500m2
For an 18 GHz band:
This is for each PSF!
After we include the efficiency of the receiver this is:

63. PSF “System Temperature”
Including receiver efficiency

64. GBT Surface Accuracy Phase 1 Active Surface off Holographic Alignment
1.0 mm surface RMS
Phase 2
Active Surface controlled by model
0.36 mm surface RMS
Phase 3
Laser ranging system turned on
accurate to 100 mm over 200m
0.24 mm surface RMS
Surface good to frequencies of 100 GHz

65. Penn Array Receiver 81 to 99 GHz bandpass
8 by 8 array of TES bolometric detectors
beam: 8’’ fwhm
A fully sampled (0.5fλ) focal plane
Background limited detectors

66. Point source (switching)
In one hour……..
Observing mode
Sky coverage
Sensitivity (1σ)
Point source (switching)
32″ × 32″
3.0 μJy
Photometric redshifts for known sources
Observations of the galactic center
Measuring the albedo of known Trans-Neptunian objects
20 μJy
5′ × 5′
Slow scanning
High resolution maps of the Sunyaev-Zel’dovich effect
Understanding the physics of star and planet formation
Studies of centimeter-sized dust grains in the Solar system
107 μJy
1° × 0.2°
Fast scanning
Large area surveys : Trans Neptunian objects, galactic plane etc

67. The Sunyaev-Zel’dovich effect
With Nobeyama 45m
RX J
80″
0.5 mJy/beam
34 hour integration 8″
0.05 mJy/beam
15 minute integration
Z~0.08  8’’=8 kpc !
With the GBT
Pointecoateau etal. 2002

68. PAR Time line: On the GBT by Fall 2004 Already done: To Do:
basic optics design
cryogenic design / test dewar
detector parameters
Build detectors & Mux
Receiver Control Electronics
Cryogenics testing
Data Analysis pipeline
On the GBT by Fall 2004

69. GBT: Properties of Faint Sources at High Frequencies
Sensitive Targeted Surveys
GOAL Better understanding of faint point source population, high-L follow up.
GBT 1cm Rx
26 – 40 GHz
MAP-style balanced radiometers (dual-pol’n)  excellent 1/f rejection
0.25 mJy/sec^0.5
Radiometry & (spectro)polarimetry of faint sources
ON THE TELESCOPE BY FALL 2003

70. ALMA

71. ALMA Cosmology Atacama Large Millimeter Array
North America (NRAO), Europe (ESO)
Japan may join as a partner
64 antennas, 12 m diameter, Chajnantor site
Compact configuration, largest out to 17 km
Lowest bands: 90 GHz, GHz (if Japan joins)
Sub-mm galaxies identification and followup
SZE in compact config
Possible Compact Array with 7m antennas
First telescopes ’06, First science ’07, Operations ’10