# Presentation: 577533

## Cosmic Microwave BackgroundProgram at Berkeley

- 	_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)
- + ~10 _Graduate Students_
-      Few Undergraduates

**Notes:**
Equal parts faculty/senior   &   postdocs  & students   ≡ giving us a total group size around 30 people.
Half of senior are instrumentation experts—
Probably anyone in the community would agree this is one of the strongest and well rounded CMB groups in the country.

You’ll see in these slides a good synergy of campus PI and lab technical capabilities which have come together to do good science.

In terms of career people, half of the effort  is LBL based.  (LBL = 3 + 3 + 2,  UCB =3.5 + 4)

## New Instrumentation↔New Experiments

*Readout *
*Multiplexing*

_**South Pole Telescope**_ 2006
- Discover 104s of Galaxy Clusters—Measure ***w, Ω******M***

_**CMBPol**_ 2014?
- Polarization Satellite

*Large Format Bolometer Arrays*
*Manufactured Photolithographically*

_**APEX-SZ **_2004
- Discover 103s of Galaxy Clusters—Measure ***w, Ω******M***

- time

_**Polarbear I**_ 2005
- Polarization from ground
- Early IGW sensitivity, proof of concept

*Polarization*
*Sensitive Planar Antennae*

_**Polarbear II**_ 2006/7
- Polarization from ground
- Excellent IGW sensitivity

## History of the universe

**History of the universe**

***You are here***

**LHC  probes physics **
**relevant to the universe**
**at age 10****-14**** sec.**

- NOW  	  (15 Billion years)

- Stars form 	   (1 Billion years)

- Nuclei Form  (180 seconds)

- Atoms Form  (300 000 years)

- Protons and Neutrons Form (10-10 sec)

- Quarks Differentiate (10-34 sec ?)

**CMB**

**& B mode polarization**

**Inflation? <10****16**** GeV**

- CMB is a near perfect black body, 2.7o K
- 	(*l*=0 monopole)
- Dipole Anisotropy 10-3
- 	(*l*=1 dipole)
- 	(our motion in the CMB `rest frame’)
- Temperature Anisotropy 10-5

**Cobe 1992**

**Cobe 1992**

**Cobe 1992**

**WMAP 2003**

## Where We Stand post-WMAP

- CMB Blackbody Temperature
- Observed
- Well Characterized
- CMB Temperature Anisotropy
- Observed
- Well Characterized
- CMB E-mode Polarization
- Observed (?)
- Well Characterized
- CMB B-mode Polarization
- Observed
- Well Characterized
- CMB SZ cluster surveys
- Observed
- Counted and Mapped

## 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 LSS 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”

- Independent confirmation of the ***w*** measurement
**APEX-SZ **
** ****South Pole Telescope**

- Precise measurement of ***w, w’***
- with **SNAP**

- Inflationary Gravity Waves
- in the CMB Polarization
-  **POLARBEAR**
** ****CMBPol Satellite**

## New Instrumentation↔New Experiments

*Readout *
*Multiplexing*

_**South Pole Telescope**_ 2006
- Discover 104s of Galaxy Clusters—Measure ***w, Ω******M***

_**CMBPol**_ 2014?
- Polarization Satellite

*Large Format Bolometer Arrays*
*Manufactured Photolithographically*

_**APEX-SZ **_2004
- Discover 103s of Galaxy Clusters—Measure ***w, Ω******M***

- time

_**Polarbear I**_ 2005
- Polarization from ground
- Early IGW sensitivity, proof of concept

*Polarization*
*Sensitive Planar Antennae*

_**Polarbear II**_ 2006/7
- Polarization from ground
- Excellent IGW sensitivity

## Sunyaev Zel’dovich Effect

**Sunyaev Zel’dovich Effect**

- Carlstrom et al, ARAA, 2002

_**Thermal SZ**_: Inverse Compton Scattering in the hot inter galactic
-                       medium “kicks”  CMB photons up to higher energy.
_**Kinetic SZ**_: doppler shift due to cluster motion.

- SuZIE (W. Holzapfel et al.)

**Measured deviation from Black body spectrum.**

- Simulations from M. White.

**Dotted line:**
**    ****Kinetic SZ**

## Sunyaev Zel’dovich Effect is Independent of Distance

- In the X-ray sky, clusters fade away at high redshift.

- SZ observations are independent of redshift
-  ***Clusters can be seen at any distance.***

## SZ State-of-the-Art TODAY

- Carlstrom et al, ARAA, 2002

- SuZIE (W. Holzapfel et al.)

- Simulations from M. White.

- Sunyaev Zeldovich effect in *KNOWN* galaxy clusters observed.
- No clusters have been *DISCOVERED* with SZ yet.
- No observation of kinetic SZ yet.

**Notes:**
Point out that this was first measured in the mm band by Holzapfel in his Suzie thesis.

## SZ Effect

**SZ Effect**

- Growth of structure depends on cosmology.
- SZ cluster counts together with redshifts determine cluster dN/dz
- constrain dark energy equation of state, w
- constrain matter density, ΩM
- Complementary to DEEP & SNAP results
- different systematics
- different correlations

**Notes:**
This physics is so profound, we need to go at it with very different observational techniques.

- Instrumentation development #1:
***Large Scale Bolometer Arrays manufactured Photolithographically***
- Implementation:
***APEX-SZ Galaxy Cluster Survey***

## APEX Sunyaev Zel’dovich Receiver

- Bolometer technology is approaching the photon statistics limit.
- We can’t do better by building a better bolometer.
- Increase integration time by going to ground based observations.
- Make many measurements at once using large scale arrays
- APEX-SZ: 320 Element superconducting transition edge sensor array
- Noise: 250 μK √s   at 2mm.
- will thus measure one square degree of sky to an RMS of 10 μK per three hours of observation!
- discover ≈ 5000 Galaxy Clusters in 250 degrees2
- Mass limit of 4x1014 Solar Masses

## Atacama Pathfinder Experiment (APEX)

**Atacama Pathfinder Experiment (APEX)**

- _Telescope_
- Located at 16,500 feet in the Chilean Andes.
- 12m on-axis ALMA prototype
- 45” resolution at 150 GHz
- 30’ field-of-view
- Telescope funded and under construction by **MPIfR/ESO/Onsala.**
- _Berkeley SZ Receiver_ **funded by NSF astronomy.**
**First Light *****Fall 2004*****.**

**Mechanical **
**Installation **
**in Chile **
**Completed.**

- _Since last year’s review:_
- Pulse tube cooler technology proven
- noise characteristics carefully studied and understood
- eliminates need for liquid cryogens   remote operation
- 55 element Spider-web TES Bolometer array fabricated and tested.
- demonstrates our abilities for large scale photolithographic production
- Prototypes for each element of readout system tested.

- Instrumentation development #2:
***Frequency Domain Multiplexing***
- Implementation:
***South Pole Telescope***

## SQUID Readout Multiplexing

- Key Element:    Readout Multiplexing
- maintain sensor sensitivity, continuous readout
- test chip of 8-channel Multiplexer (LBNL, UCB, TRW)
**cited as a Physics Highlight in APS *****Physics News in 2001***
- April 2002: **MUX demonstrated together with **
**LLNL in x-ray bands** (Cunningham et al., APL 2002 (LBNL-50193))
- LTD 2003: **noise properties of MUX demonstrated with CMB bolometer**

**Bolometer Array**

- frequency

- _Since last year’s review:_
- Prototype readout electronics fabricated and tested.
- “Module Zero” SQUID controllers in hand and operating.
- Prototype Osc/Demod board tested
- “Module Zero” Osc/Demod boards in layout phase
- in hand in ~ month

**Computer controlled mixed Analog / Digital SQUID readout Electronics**
**Exploit unique capabilities of LBL for large scale detector development.**

## South Pole Telescope

- 1000 pixel focal plane (multiplexed)
- 8m, off-axis design
- 1.3’ resolution
- 1 deg. Field of view
- 100% time SZ observations
- Best mm-wave site
- First light 2006
- Funded by NSF Polar Programs (Chicago, Berkeley, Case Western, SAO)

**APEX/SPT are complementary: APEX will be operational 2-3 years**
**before SPT, but SPT will have ~5x faster cluster finding rate.**

## New Instrumentation↔New Experiments

*Readout *
*Multiplexing*

_**South Pole Telescope**_ 2006
- Discover 104s of Galaxy Clusters—Measure ***w, Ω******M***

_**CMBPol**_ 2014?
- Polarization Satellite

*Large Format Bolometer Arrays*
*Manufactured Photolithographically*

_**APEX-SZ **_2004
- Discover 103s of Galaxy Clusters—Measure ***w, Ω******M***

- time

_**Polarbear I**_ 2005
- Polarization from ground
- Early IGW sensitivity, proof of concept

*Polarization*
*Sensitive Planar Antennae*

_**Polarbear II**_ 2006/7
- Polarization from ground
- Excellent IGW sensitivity

## Why measure CMB Polarization?

- scalar, vector & tensor fields carry
- 	more information than the
- 	temperature anisotropies alone.
-  measure cosmo parameters better
- measure the reionization epoch, which produces a large degeneracy in the Temp spectrum
- measure gravity wave amplitude... the smoking gun of inflationary models.

**DASI 2002**

## Inflationary Gravity Waves

- Just as the CMB gives the fingerprint of the universe at the surface of last scattering,
- the fingerprint at the time of inflation (10-38? s) is encoded on the ***inflationary gravity wave background*** (IGB).

**IGB**

## Polarization Power Spectrum

**W. Hu et al. astro-ph/0210096**

**~100 ****μ****K RMS**

**~4 ****μ****K RMS**

** ≤****300 nK RMS**

**1 degree**

**Temperature**

**E-modes**

**B-modes**

- B-mode amplitude is characterized
- by the tensor to scalar ratio.
- T/S < 0.71 from WMAP.
- Determined only by the energy scale of inflation.

- Instrumentation development #3:
***Polarization Sensitive Antenna Coupled Bolometers***
- Implementation:
***POLARBEAR I***
- Instrumentation development #1+2+3:
***POLARBEAR II***

## Antenna-coupled Bolometer Diagram

- Simulated Bands

**Antenna provides directivity**
**antenna, filters, bolometers packaged together below lens**
**Multicolor ******** multiple bands per pixel.**
**Polarization sensitive**
**dual polarization by placing 2 crossed dipole arrays in same pixel**

- 1 mm

**Prototype pixel fabricated, **
_**being tested now**_

## POLARBEAR Focal Plane

- Polarbear I Focal plane
- 150 pixels x 2 polarizations =300 bolo’s at 300 mK
- 3 bands, 150,250,350 GHz
- Polarbear II Focal plane
- 900 pixels, 3000 bolometers
- Full use of 150 GHz Field-of-view

- 6 inches

- _Since last year’s review:_
- dipole slot antenna coupled bolometer has been successfully fabricated
-  beginning testing phase.
- Optics design complete.
- Candidate telescope designs assessed.
- Site selection & evaluation.
- White Mtn– good observing conditions, easily accessible to Berkeley for Bolo-array prototyping.

## Could achieve first light in 2005 from White Mountain, CA with a ~3m primary
atmospheric emission is nearly unpolarized.
large sky coverage for primordial gravity waves
sufficient resolution to measure and subtract out gravitational lensing signal.
staged deployment – 300 elements, upgrade to fMUX 1000s of elements.
multi-frequency polarization sensitive antenna coupled toTransition Edge Sensor bolometers
testing facility for future satellite technologies, systematics, and foreground measurements.

- atmospheric emission is nearly unpolarized.
- large sky coverage for primordial gravity waves
- sufficient resolution to measure and subtract out gravitational lensing signal.
- staged deployment – 300 elements, upgrade to fMUX 1000s of elements.
- multi-frequency polarization sensitive antenna coupled toTransition Edge Sensor bolometers
- testing facility for future satellite technologies, systematics, and foreground measurements.

**POLARBEAR**

## POLARBEAR Performance

**3 yrs x 25% duty **
****** ****200 nK/pixel on 10 x 10 deg****2**

- POLARBEAR-II Sensitivity

**3 years observing**
**(Assuming a Tensor to Scalar ratio r=T/S=0.35)**

- POLARBEAR-I Sensitivity

** ****Characterize E-modes**
** ****Search for B-modes, the **
**  “****smoking gun” of inflation**

## Einstein Probe Satellite: CMBPOL

**Einstein Probe Satellite: CMBPOL**

- SPACE: the final-frontier
- Are POLARBEARs space-worthy?
- Proposals for concept studies submitted.
- Five Berkeley collaborators (Lee = CO-I) on joint JPL/Berkeley/Caltech/Chicago proposal
- 2013-16 launch with cost cap ~$500M
- lots of R&D between now and then
- upcoming polarization facilities (e.g. POLARBEAR) will be test-beds for CMBPOL instrumentation.

**Notes:**
Analogy  SCP SNAP   vs.   POLARBEAR  CMBPol

## (a few of) The Polarization Experiments

- DASI  (interferometer at the South Pole)
- Boomerang / MAXIPOL  Balloon based telescopes
- WMAP NASA Satellite  2001-5
- Bicep  (South Pole 2004/5)
- POLARBEAR  (California 2005-) 3m ground based
- QUAD (South Pole 2004/5) ground based
- Planck  ESA/NASA Satellite (2007-)
- CMBPOL Einstein Probe Satellite (2013/16)

- now

- Competition is fierce.

- In terms of technology and leveraging,
- Berkeley is positioned as a leader.

## Computing & Data Analysis

**NERSC ****expertise and computing power is used extensively by CMB community **
**Seaborg: ~6000 processor (1.5 GFlops,  1-4 GB each) IBM SP3 Massively Parallel Computer**
**HPSS Storage, 850 TB**
**Since Last Year, MADCAP3 Released:**
**Microwave Anisotropy Dataset Comp Analysis Package, Ver 3 implemented for SP3**
**polarization capability**
**multiple datasets, Planck size datasets**
**Planck Surveyor, 2007**
- responsibility for software, algorithm development, calibration, and treatment of systematics
- ESA/NASA has recognized importance of NERSC
**2 Planck funded NERSC positions +postdoc**
**50 team members using NERSC facilities**

**NERSC CMB Users**
** ****and Collaborators**

**Notes:**
Having these guys in the same building is a huge resource.

Maxipol – real data with real glitches
Planck- enormous size data.

## The Polarization sensitive balloon-borne followup to MAXIMA flew in May 2003

**E-mode POLARIZATION with MaxiPOL**

- GOAL: detection of
- 	E-mode polarization
- First half-wave plate polarimeter
- modulated polarization key for systematics
- NERSC Facilities and staff currently analyzing data
- 	 Expect results soon.

## Technology Development is Crucial

**Berkeley CMB Group is a world leader in CMB instrumentation, observations, analysis and results.**
**excellent synergy between Campus & LBL.**
**NASA/NSF is funding basic Bolometer development**
**no funding for engineering large scale systems / production facilities.**
**Berkeley National Lab’s unique contribution is expertise in large detector systems.**
**large scale integrated sensor arrays & readout multiplexing.**
**experienced engineers are essential**
**Superconducting Detector Fabrication Facility progressing:**
**Identified Space, Floor plan, & equipment requirements**
**Start date deferred to 2005.**

## LDRD Funding for CMB Technology

- from Director’s Review Last year:
- “technology development relies heavily on LDRD funds from LBNL... require a significant infusion of LDRD funds in 2003 and 2004... We recommend that LBNL use LDRD funds toseed the technology development for the approved experiments.”
- Rated as “highest priority LDRD” by the physics division.

- 2001

- 2002

- 2004

- 2003

- 10/2000

- $ 100K

- $ 0

**LDRD **
**Funding**

- SC Detector Array Technology
- Strategic LDRD Rejected

- Polarized Arrays
- LDRD Rejected

**Notes:**
2002: “noted the Division’s ability to react quickly to new scientific opportunities, notably in astrophysics.”

## Summary

**strong ongoing CMB program that combines the strengths of university and National Lab.**
**Science goals of CMB program have been endorsed by two National Advisory Panels and given the highest priority by the community.**
**LBL has a focused instrumentation development path, providing key cosmology measurements at each step**
**next generation CMB measurements rely on technology development**
**Physics Div’s unique contributions to this field need lab support. **
**Berkeley is in a unique position to take leadership role in Polarization science.**
**modest increase in funding will allow POLARBEAR to proceed expeditiously**
**positions LBL to play major role in (post-SNAP) future CMBpol satellite**