# Presentation: 051170

## DMSAG Presentation to HEPAP

- Hank Sobel
- For the DMSAG Panel
- July 13, 2007

## Changes to Document

- Comments from AAAC & HEPAP
- Suggestions/corrections from individual members
- Send report to outside reviewers for comments.
- Distribute findings and recommendations throughout the report in appropriate locations.
- More discussion of DUSEL
- More detail in priorities.

## Send report to outside reviewers for comments

- Request to review sent to eleven people selected from lists supplied by HEPAP, AAAC, DOE
- Eight accepted, seven returned remarks. Theoretical astrophysics, HEP theory, Particle astrophysics, Experimentalists.

## Results

- Comments:
-  typos, wording, style, content
- New executive summary stating charge questions and short answers. (Page 4)
- New glossary with experimental acronyms, basic techniques, status and index to location in document. (Page 91)

## Extracts From Executive Summary

## What are the most promising experimental approaches for the direct detection of dark matter using particle detectors in underground laboratories?

- Cryogenic techniques based on solid state (phonons and ionization in Ge and Si) and noble liquids (in two-phase systems of both liquid Xe and liquid Ar) are presently leading the field and showing the greatest promise for coherent scattering of WIMPs.
- Methods with single phase liquid argon and warm liquids or gases are showing significant promise for the future.

## What is the optimum strategy to operate at the sensitivity frontier in the short and immediate term while making the investments required to reach the ultimate sensitivity by scaling up to some realistic size in the long term (5-10 year horizon)?

- We suggest as an optimal strategy a near-term push to construct at least two experiments of differing target materials with a goal of improving sensitivity at least a factor 10 over present limits. The technologies to be chosen from those presently with the most promise to carry them out in a timely and cost effective manner.
- At the same time, aiming for the longer term and next level of sensitivity, R&D should be conducted on all techniques with potential for scalability to at least tonne-scale and/or background control (such as true directionality).

## What is the present state of the worldwide program? Does the US program have the potential to make unique contributions in the future?

- In addition to the U.S.-led experiments, there are presently between 7-10 dark matter direct detection experiments principally in Europe, Canada and Japan. Those programs are also making significant progress and expect to field additional experiments.
- The U.S. experiments are presently leading the field in sensitivity in two or more of the major techniques (e.g., ADMX, CDMS, XENON10).

## Changes to Findings and Recommendations

## Recent XENON 10 Results

- Better than current CDMS limits, but  although they are working to reduce or eliminate it, current version of experiment has background.

- CDMS expects to finish analysis of latest data set this summer. They expect to reach a  sensitivity of ~4x10-44 cm2 with no background.

## Recommendation: CDMS(old version)

- The sub-panel recommends the completion and operation of CDMS-II and funding of two SuperCDMS supertowers, to be tested at the Soudan site.
- If the dark matter experimental funding is increased to the range of that suggested in Recommendation 1, then we support the design and construction of the necessary refrigeration system for SNOLAB. If not, and funding is not sufficient for the rest of the program we have outlined, then we recommend that the decision to go forward with Super-CDMS in SNOLAB be contingent upon a full evaluation of the field to be completed by mid-2009.

## Problems with this

- In this version the panel did not support going forward with the full 7 ST even if the full funding we suggested was available.
- Main reason was that panel felt strongly that it was necessary to demonstrate background reduction in the first two ST before recommending ST 3-7...factor of ~ 20 required over CDMS II.
- In addition...funding procedure implies >2009 before initial funding. 2ST is fastest way to proceed .
- However, this uncertainty could lead to unfortunate delays.

## Recommendation 3: CDMS (revised)

- The sub-panel recommends that the CDMS Collaboration be supported to continue its outstanding direct-detection program. In order to accomplish this, we recommend the completion and operation of CDMS-II and the funding of two SuperCDMS supertowers at the Soudan site. Additionally, if dark matter funding is sufficient to permit the significant starts on the other portions of the U.S. program that we describe, and if the collaboration demonstrates the necessary control of the backgrounds, we support the completion and operation of the SuperCDMS detector with 7 supertowers at SNOLAB.
- If funding is not sufficient for the rest of the program we have outlined, we recommend that the decision to go forward with supertowers 3-7 and installation of SuperCDMS in SNOLAB be considered in the broad context of a full evaluation of the field to be completed by mid-2009.

## Reasoning...

- If required background reduction is demonstrated, then the panel recommends that SuperCDMS goes forward...if funding allows...see priorities.
- Positive statement allows review process to start at the agencies immediately.
- Estimated 1 1⁄2 year total timescale for DOE review.
- If review is positive, and funding available (MIE in DOE), funding could start immediately after 2009 review.

## Expanded Section on DUSEL

- While other countries have developed a number of underground sites, the total amount of deep experimental space is still far below that which will be required.
- Presently, there is no U.S. site or collection of sites suitable or capable of accommodating the evolving dark matter program alone.
- An underground facility such as DUSEL is essential for these large detectors and could also serve as a cooperative center and shared infrastructure for the entire U.S. direct detection program.
- Money for initial suite of experiments will be important new source of experimental funding.

## Recommendation 8: Priorities (old version)

- Following on the above recommendations, we recommend that the funding priorities during this window of opportunity be aimed equally towards continuing the on-going CDMS and ADMX experiments, at the levels indicated above, and funding the expansion of the noble liquid experimental efforts to their next level. The development of superheated liquid detectors and detectors capable of determining WIMP direction should be supported with a lower priority since, although they have great promise, they still have significant R&D questions remaining to be answered.
- We believe that many of the uncertainties associated with the longer-term direction of the experimental efforts will be resolved during the next few years and that a program review in or around 2009 will be necessary.

## Asked to Expand This...

- Here, we tried to carefully word it so that we didn’t do any damage...

## Recommendation 8: Priorities (revised)

- Following on the above recommendations, if the comprehensive program we have
- described above is not able to be fully funded, then we recommend that the funding
- priorities during the next few years be allocated as follows. In establishing these priorities,
- we have considered both the experimental evidence of promise in a particular technique
- and our estimation of its readiness for producing significant experimental results. In
- addition, all else being equal, predominantly US efforts are given somewhat higher
- priority.
- 1. Equal priorities between (A) and (B):
- A) Continuing the on-going CDMS and ADMX experiments and the initial construction of SuperCDMS in Soudan with two super-towers.
- B) Funding the expansion of the noble liquids with priorities i), ii) and iii):
- i) The expansion of the liquid Xenon experimental efforts to their next level.
- ii) The U.S. participation in the WARP detector development.
- iii) The next stage of the CLEAN Argon/Neon detector development.
**(***Note on funding guidance: As we have noted elsewhere, we do not yet know which technique is the best route to the ton and larger scale. Consequently, there is a need to keep the three noble liquid techniques moving in parallel to that goal. As progress is achieved in each project, the levels of relative funding may need to change, independent of present priorities, in order to make fair evaluation of potential.)*

## Priorities Continued...

- 2. The development of superheated liquid detectors and detectors capable of determining WIMP direction. Although these ideas have great promise, they still have significant R&D questions remaining to be answered.
- We believe that many of the questions associated
- with the longer-term direction of the experimental
- efforts will be resolved during the next few years
- and that a program review in or around 2009 will
- be necessary.

## Recommendation 1: Program and Funding

-   To realize this program on an optimal time scale, the committee recommends that DOE and NSF increase funding for the direct detection of dark matter from the present ~$2-3M to ~$10M annually as soon as possible. The prospect of detecting dark matter while the LHC is operating amply justifies this increase. Such a figure is also consistent with the recommendations of P5 and EPP2010.

## Outside Reviewers

- Marcela Carena - Fermilab (HEP theory, P5)- _[carena@fnal.gov](mailto:carena@fnal.gov)_
- Bob McKeown - Caltech (Daya Bay, Kamland)- _[bmck@krl.caltech.edu](mailto:bmck@krl.caltech.edu)_
- Ted Baltz - SLAC (Particle astrophysics)- _[eabaltz@slac.stanford.edu](mailto:eabaltz@slac.stanford.edu)_
- Gina Rameika - Fermilab (LAr, Minos)- _[rameika](mailto:rameika@fnal.gov)__[@fnal.gov](mailto:rameika@fnal.gov)_
- Ira Wasserman - Cornell (Theoretical Astrophysics)- _[ira@astro.cornell.edu](mailto:ira@astro.cornell.edu)_
- John Swain - Northeastern (Astroparticle experiment, Auger)- _[j.swain@neu.edu](mailto:j.swain@neu.edu)_
- Paolo Gondolo – Utah (Cosmology, Astrophysics) _[paolo@physics.utah.edu](mailto:paolo@physics.utah.edu)_
- Frank Avignone - (Double beta decay) - _[avignone@sc.edu](mailto:avignone@sc.edu)_