Particle Astrophysics at NSF (PHY and AST) NSFNSF ParticleParticle AstrophysicsAstrophysics

Jim Whitmore, Program Director for the PA program

Theme: Physics of the Universe: to support Particle Astrophysics projects doing world-leading, potentially transformative science – at any location (in/out of the US)

Outline:

- PHY Division - Underground facility - AST Division - Future Funding issues

November 22, 2011 J. Whitmore -- ASPERA Meeting 1 Particle Astrophysics at NSF (PHY and AST) Discussions with other Agencies and Advice • We work closely with DOE OHEP & ONP • We discuss projects with other International Agencies • We get advice from HEPAP (High Energy Physics Advisory Panel) and its sub-panels (PASAG, DMSAG, NUSAG,…) (SAG =Scientific Assessment Group) • Also others (ASTRO2010, AAAC, NAS,…) • International Finance Boards • OECD-GSF-Astrophysics Working Group (APIF) • Bi-national Discussions (INFN, IN2P3) • Attend Lab Scientific Committee meetings (PACs

November 22, 2011 J. Whitmore -- ASPERA Meeting 2 Particle Astrophysics at NSF (PHY and AST) Details of PHY PA funding In FY2010: 62 different institutions (may have more than 1 group) 140 PIs/Co-PIs 52 postdocs 118 graduate students 98 undergrads More than 50% of the PIs work on more than one project

PHY funding for PA in FY2011 was $19.2M

-- Search for Dark Matter (35.5% of the funding); -- Study of the particles comprising the UHE Universe (ultra-high energy cosmic rays, gamma-rays and ) (41%); -- Detection of solar neutrinos and the attempts to determine the absolute value of the mass of Neutrinos as well as some of their elusive properties (21.2%); -- Search for understanding Dark Energy, Cosmology (2.4%)

November 22, 2011 J. Whitmore -- ASPERA Meeting 3 Particle Astrophysics at NSF (PHY and AST) Location of PA projects

Of the 31 projects supported by PA, 11 are located in the US (two are planning to move out with their next upgrade) and 20 are located outside the US in Italy (underground), Canada (ug), UK (ug), Argentina, Mexico, Antarctica (ug), France (ug), China (ug), Japan (ug) and Chile. Of the 13 underground labs shown, the PA program supports activities at 9 of them.

November 22, 2011 J. Whitmore -- ASPERA Meeting 4 Particle Astrophysics at NSF (PHY and AST) Dark Matter Direct Detection WIMP searches XENON100 and CDMS have the world’s best limits as of today. S-CDMS – at Soudan/SNOLab? (Ge) XENON – 100 at LNGS Constr/Ops (Xe) X1T WARP – at LNGS (Ar) LUX – Constr at SURF (Xe) COUPP – at SNOLab PICASSO – at SNOLab CoGeNT – at Soudan MiniCLEAN – at SNOLab (Ar) DarkSide – Constr. at LNGS (DAr) DA-50 in the Borexino CTF Decay shape from 39 Directional projects: Ar in normal Ar Ar DRIFT – Constr/Ops at Boulby DMTPC – Constr only, at WIPP Xe Axion searches ADMX-HF – Axion Dark Matter eXperiment – High Frequency Depleted Ar: depletion – Constr. (Yale) factor > 100 November 22, 2011 J. Whitmore -- ASPERA Meeting 5 Particle Astrophysics UHE Cosmic Rays at NSF (PHY and AST)

S. AUGER – Constr complete/Ops (DOE-OHEP and 17 more countries) Currently have 1639 working stations and only 5 not (99.7%) All 5 fluorescence detectors are working

TA (Telescope Array) – Constr/Ops; located near Delta, south of Salt Lake City Formerly HiRes AUGER

HiRes

November 22, 2011 J. Whitmore -- ASPERA Meeting 6 Particle Astrophysics at NSF (PHY and AST) HE Cosmic Rays R&D • AMBER (Airshower Microwave Bremsstrahlung Experimental Radiometer ) The indirect observation of secondary emission from the residual tenuous gas of excited particles and plasma left when the shower of particles transits the atmosphere is currently applied only to optical fluorescence of molecular nitrogen. AUGER is studying its feasibility for observing UHE cosmic rays • Bistatic radio detection in TA:The collaboration has successfully commissioned a 2 (20) kW bistatic radar transmitter station, in Delta, Utah. The receiver station is under construction, and they have begun characterizing the transmitter output. (Ionization plasma reflects radio waves – amplitude largest in forward direction) • Askaryan Effect: When ultra-high energy neutrinos interact in a dense medium, such as ice, the enormous cascade of secondary particles emit an intense sub-nanosecond pulse of coherent Cherenkov radiation at radio wavelengths. • ARIANNA (Radio reflection in Antarctic – UHE νs) (with OPP) the first prototype for the proposed Antarctic Ross Ice Shelf Antenna Array (near McMurdo) of neutrino detectors was successfully installed. The interface between ice and liquid water below acts as an excellent surface for reflecting radio waves. • ARA (Askaryan Radio Array) R&D (MRI with OPP) To detect the RF emission from neutrino induced showers in RF transparent media. The receivers installed in IceCube boreholes were designed to be sensitive in the range of 100 MHz - 1 GHz. 14 receivers 40 m under ice and two additional ones on surface at S. Pole. November 22, 2011 J. Whitmore -- ASPERA Meeting 7 Particle Astrophysics UHE Gamma Rays at NSF (PHY and AST) VERITAS – Upgrade/Ops --Discoveries of TeV sources of γ-rays --Indirect DM limits from Dwarf Spheroidal Galaxies Science (Oct 7): “Detection of Pulsed Gamma Rays above 100 GeV from the Crab Pulsar”. They are the highest energies (by an order of magnitude) ever detected from a pulsar; their energy spectrum indicates a completely new and unexpected component; and it is coming from a new location, more than 10 stellar radii from the neutron star. HAWC started construction earlier this year: up to 300 large water Cherenkov tanks (7.3m diam, 5m deep) At high altitude (4100m, Sierra Negra) 7 tanks complete now CTA – under discussion

November 22, 2011 J. Whitmore -- ASPERA Meeting 8 Particle Astrophysics at NSF (PHY and AST) Neutrinos

IceCube (with OPP) Construction was completed at the South Pole on December 18, 2010 New Zealand time. The main IceCube detector now contains 5,160 optical sensors on 86 strings embedded two kilometers below the NSF’s Amundsen-Scott South Pole Station. Includes 6 strings of Deep Core (low energy). (with Germany, Sweden, Belgium) DOMs between 1,450 and 2,450 meters Reactor Neutrinos: (θ13) Double – Constr/Ops; taking data with 1 (far) detector since April 13, 2011 (~5000 ν)

New measurement of θ13

2 sin 2θ13 = 0.085 + 0.029(stat) + 0.042(syst)

Daya Bay – group base support only. Data-taking started August with 2 near detectors DC Outer veto (complete) Borexino – solar neutrinos at LNGS November 22, 2011 J. Whitmore -- ASPERA Meeting 9 Particle Astrophysics Neutrino Properties at NSF (PHY and AST) Neutrinoless searches: CUORE (LNGS): NSF is funding the construction, testing and installation of the electronics (Milano design) Tech support for CUORE-0 (DOE-ONP) MJD at Homestake; providing funds to import ~60 kg of germanium enriched to ~86% in 76Ge 13 in the form of GeO2, reduce it, purify it, and zone refine it to the level of ~10 electrically active impurities/cm3, normally accepted by the germanium detector manufacturers. (DOE-ONP) NSF is also funding R&D into P-type Point Contact (PPC) Ge detectors

136 21 EXO-200 WIPP (2ν DBD result: T½ ( Xe) = 2.11x10 yrs) Base support for 2 groups and Ba Tagging R&D both Liquid and Gas Xe NEMO-3 (Modane Underground Laboratory in the Fr´ejus Tunnel under the French-Italian Alps) combines tracking, calorimetry and ToF For Super-NEMO: 82Se 0.04-0.14 eV (>1.5x1026 yr) Neutrino mass measurements: Mare-II cryogenic microcalorimeters measuring beta decay of 163Ho Sensitivity goal of 0.1-0.2 eV/c2 November 22, 2011 J. Whitmore -- ASPERA Meeting 10 Particle Astrophysics at NSF (PHY and AST) Gravitational Waves

• LIGO and ADV-LIGO • Funded by MREFC (Major Research Equipment and Facility Construction) • and by Gravitation Program in PHY

November 22, 2011 J. Whitmore -- ASPERA Meeting 11 Particle Astrophysics at NSF (PHY and AST)

UndergroundUnderground PhysicsPhysics ResearchResearch atat thethe NationalNational ScienceScience FoundationFoundation

Jon Kotcher DPF Meeting 2011 Forum on Underground‐based Physics Brown University, Providence, RI August 11, 2011

November 22, 2011 J. Whitmore -- ASPERA Meeting 12 Particle Astrophysics DeepDeep UndergroundUnderground ScienceScience andand at NSF (PHY and AST) EngineeringEngineering LaboratoryLaboratory (DUSEL)(DUSEL) • DUSEL is being envisioned as a unique, dedicated international underground education & research facility that would support potentially transformational experiments in multiple disciplines. • The U.S. particle, nuclear, and astrophysics communities have selected DUSEL as central to their national programs. • Site selection was exhaustively reviewed by 22‐member world‐class • The engineering, geology and biology panel: communities are proactively engaged, and participate in all aspects of DUSEL • PHY, GEO, BIO, ENG, ES&H, planning. underground construction, geotechnical/civil engineering, mining • Development focused on the former and operations, large project Homestake Gold Mine (Lead, SD), the management, cost & schedule, E&O, deepest mine in North America. US & foreign representation.Davis Cavern November 22, 2011 J. Whitmore -- ASPERA Meeting Sep 21,13 2009 Particle Astrophysics Developing the DUSEL Experimental at NSF (PHY and AST) Program: S4

• Solicitation 4 (S4): called for proposals to develop designs and pursue targeted R&D for potential DUSEL experiments (Jan 2009)

• Nine proposals funded in physics: • Seven proposals funded in – Dark matter (4) BIO, GEO & ENG sciences: – Neutrino‐less double‐beta decay (2) – Fracture processes – Coupled processes – Large water Cerenkov detector (multipurpose) – Subsurface imaging and sensing – Fiber optic strain monitoring – Underground accelerator – CO sequestration – Assaying sub‐facility 2 – Eco‐hydrology & deep drilling • Total physics awards: $21M over – Underground monitoring 3 years. • Total BGE awards: $3M.

November 22, 2011 J. Whitmore -- ASPERA Meeting 14 Particle Astrophysics SouthSouth DakotaDakota DevelopmentDevelopment at NSF (PHY and AST) ofof SanfordSanford LaboratoryLaboratory

• South Dakota Science and Technology Authority (SDSTA) holds $124M for development of Sanford Laboratory. – $70M private benefactor (Sanford), $44M state SD, $10M HUD. • Funds to support: – Education center. – Reentry and partial refurbishment of 4850L & 7400L. – Operations & maintenance of Sanford Laboratory activities. • Approximately 85 staff. • SDSTA began mine re‐entry late July 2007. Dewatering & treatment began 21 April 2008. • Various BGE experiments have been deployed since reentry. • 4850L dry since May 2009 and being prepared to support early physics experiments (LUX, MJD). November 22, 2011 J. Whitmore -- ASPERA Meeting 15 Particle Astrophysics Current Status (1) at NSF (PHY and AST) Current Status (1)

• In December 2010, the Committee on Programs and Plans (CPP) of the National Science Board (NSB) voted to discontinue further DUSEL design funding. • The National Academy study was released in July 2011. It contains a strong endorsement of both the DUSEL research program, and the US pursuit of an on‐shore leadership role in underground science. (See next slide) • NSF subsequently provided an additional $4M in FY11 to continue dewatering and maintain security in the mine for the remainder of the fiscal year (June – September); plus $2M in FY2012.

November 22, 2011 J. Whitmore -- ASPERA Meeting 16 Particle Astrophysics at NSF (PHY and AST) National Academy of Sciences Report

National Academy of Sciences: An Assessment of the Deep Underground Science and Engineering Laboratory (Board on Physics and Astronomy, July 2011) Laboratories located deep under the surface provide a unique environment where scientists can study the behavior of the smallest subatomic components of matter, shielded from the cosmic rays and other environmental “noise” that permeate the environment on the surface. ….. The research pursued in these laboratories has the potential to make profound contributions to our understanding of nuclear and particle physics. ….. This study … identifies the most important questions and experiments that could be addressed by the proposed program of research. From the list of proposed experiments, the study identified three as the top priorities: • The direct detection dark matter experiment; • The long baseline experiment; and • The neutrinoless double beta decay experiment Because these three experiments address fundamental questions at the forefront of physics research, all could produce a breakthrough discovery upon which the future of particle, nuclear, and astrophysics will be built. For this reason, and to foster future U.S. leadership in the expanding field of underground science, the committee concluded that United States should proceed with plans to conduct the above three experiments, even if they must take place in a facility other than DUSEL. November 22, 2011 J. Whitmore -- ASPERA Meeting 17 Particle Astrophysics at NSF (PHY and AST) SanfordSanford LaboratoryLaboratory DevelopmentDevelopment atat 48504850 levellevel Davis Cavern and associated spaces Ray Davis being outfitted to house LUX (DM) and 1965 MAJORANA demonstrator (DBD) for early science. Davis Cavern Excavated and Shotcreted May 2, 2011

Majorana Clean Room May 31, 2011 November 22, 2011 J. Whitmore -- ASPERA Meeting Davis Cavern18 Sep 21, 2009 Particle AstrophysicsTheThe LongLong BaselineBaseline ExperimentExperiment at NSF (PHY and AST)

NOvA (off-axis) MINOS (on-axis)

Homestake DUSEL 735 km Hig h Inte Large Detector at DUSEL: ensity y Neu CP violation, Proton Decay, 1 trino 1300 k o Bea Supernovae m am

Fermilab

The configuration of a Mega-Detector at Homestake, greater than 1,000 km from a high intensity source, offers a discovery opportunity that is unique in the world.

November 22, 2011 J. Whitmore -- ASPERA Meeting 19 Particle Astrophysics at NSF (PHY and AST) TheThe CurrentCurrent StatusStatus (2)(2)

• The viability and future of Fermilab, DUSEL and U.S. particle physics are intimately linked. • The project continues to be the focus of much discussion and activity in government circles. • Re‐engagement of NSF as a secondary partner, with DOE as the lead, is a possibility.

November 22, 2011 J. Whitmore -- ASPERA Meeting 20 Particle Astrophysics at NSF (PHY and AST)

Division of Astronomical Sciences Jim Ulvestad Division Director, AST AAAC, October 13, 2011

November 22, 2011 J. Whitmore -- ASPERA Meeting 21 Particle Astrophysics Antennae, NGC 4038/9 at NSF (PHY and AST) ALMA HST • Atacama Large Millimeter/ submillimeter Array • Science observations started on 30 Sept. – 112 projects selected from over 900 proposals for observation in Cycle 0 ALMA Bands 3,6,7 • 44 antennas now in Chile with 27 accepted; current delivery rate is ~2/month • Final North American deliverables (antennas and receivers) on course for ~Sept 2012

Brodwin et al. 2010, ApJ, 721, 90

November 22, 2011 J. Whitmore -- ASPERA Meeting 22 10/13/2011 22 Particle Astrophysics at NSF (PHY and AST) Other AST Facility News

• EVLA (Expanded Very Large Array) completion expected on time and on budget in 2012 • ATST (Advanced Technology Solar Telescope) • Still aiming for end of commissioning in late 2018 • Impact on operations budget and structure of grants program • Dark Energy Survey at NOAO/CTIO 4m (Blanco) telescope scheduled to start in September 2012 • NSF/DOE collaboration on telescope/camera • BigBOSS under discussion; possible execution at 4m Mayall telescope at NOAO/KPNO • NSF funding dependent on mid-scale competition

November 22, 2011 J. Whitmore -- ASPERA Meeting 23 10/13/2011 23 Particle Astrophysics Mid-Scale Instrumentation at NSF (PHY and AST)

• Currently supporting – PAPER (Precision Array to Probe Epoch of Re- ionization) – POLARBEAR –ACTPOL – SDSS-III – LSST D&D POLARBEAR – VAO (Virtual Astron. Obs) – HETDEX (Hobby-Eberley Telescope Dark Energy Expt – CCAT D&D (Cornell-CalTech Atacama Telescope) • No new starts in FY12

November 22, 2011 J. Whitmore -- ASPERA Meeting 24 10/13/2011 24 Particle Astrophysics at NSF (PHY and AST) South Pole Astronomy

• Primarily supported by NSF Office of Polar Programs (OPP), with (very) minor shared AST funding – South Pole Telescope, BICEP2, SPIDER2, etc. • Funding for Particle Astrophysics, primarily IceCube operations and science, shared 50/50 with PHY • In constrained budget environment, with IceCube in full operations, maintenance of South Pole astronomy program will be a challenge – Balance/tradeoff against other AST mid-scale projects?

November 22, 2011 J. Whitmore -- ASPERA Meeting 25 10/13/2011 25 Particle Astrophysics at NSF (PHY and AST) NWNH Actions—Large Programs • Continuing LSST D&D funding, aiming for possibility of MREFC start in FY 2014 or later – Increased D&D and required operations funding both will require significant funding reallocation • Mid-Scale Innovations Program – discussions ongoing about more general NSF/MPS program • GSMT selection solicitation under consideration – Would have stringent conditions: No MREFC funding possible before 2020, no ops funding before 2023 – Congress expects “..a solicitation …[by] the end of CY2011 and a result announced no later than July 31,2012.” • CTA: possible proposal opportunity if Mid-Scale program is initiated November 22, 2011 J. Whitmore -- ASPERA Meeting 26 10/13/2011 26 Particle Astrophysics at NSF (PHY and AST) AST will have a Portfolio Review

• New Worlds, New Horizons (NWNH) advised: “If …budget is truly flat…there is no possibility of implementing …the recommended program…without…enacting the recommendations of the first 2006 senior review and/or …a second more drastic…review before mid-decade.” (p. 240)

• Not a repeat of Senior Review, which was confined to facilities.

• Examine balance across entire portfolio of activities AST supports.

• AIM: Maximize progress on central science questions, balancing recommendations for new facilities, instrumentation and program enhancements with capabilities enabled by existing facilities and programs.

November 22, 2011 J. Whitmore -- ASPERA Meeting 27 10/13/2011 27 Particle Astrophysics FY2012 Funding at NSF (PHY and AST) for NSF R&RA Current status: Research and Related Activities The FY 2010 appropriation was $5,615.3 M The FY 2011 appropriation was $5,563.9 M The FY 2012 Administration request was $6,253.5 M On Friday: The FY2012 approved budget provides $5,719M an increase of $155.1 million or +2.8% “By accepting NSF’s proposal to eliminate funding for the Deep Underground Science and Engineering Laboratory (DUSEL), the conference agreement completes a multi-year phase-out of NSF involvement in this project. NSF is directed to report to the Committees on Appropriations about future efforts or commitments, if any, to collaborate with the Department of Energy on a deep underground lab.”

November 22, 2011 J. Whitmore -- ASPERA Meeting 28 Particle Astrophysics at NSF (PHY and AST) MPS FY2012 Budget Request

FY 2012 NSF request was $7,767M ;13% above the FY2010 Enacted amount FY11 CR PHY (+3.7%)

ARRA AST (+1.4%)

FY 2012 President’s Budget under Terminations, Reductions and Savings NSF will continue to solicit grant proposals for future particle physics research, including small-scale underground experiments that might be conducted at Homestake (should DOE decide to support the core infrastructure there) or at other existing sites in the United States and around the world. November 22, 2011 J. Whitmore -- ASPERA Meeting 29 Particle Astrophysics at NSF (PHY and AST) PHY: Comments/ Future

• Oversight – periodic reviews of fabrication projects (usually with DOE, both OHEP and ONP) • To start new projects, under flat funding, we obviously need to end others • With DOE/OHEP, we are starting to review all major projects to re- evaluate: – their science – their goals – the length of running needed to achieve those goals Looking ahead to FY2013: OMB Issues Budget Guidance: An Office of Management and Budget memo instructed the heads of departments and agencies to submit FY 2013 budget requests lower than FY 2011 levels, while stressing the importance of investments critical to job creation and economic growth.

November 22, 2011 J. Whitmore -- ASPERA Meeting 30 Particle Astrophysics AST: Principles for Budget at NSF (PHY and AST) Decisions

• Protect high priority facilities with international and interagency commitments; • Maintain a robust individual investigator program to enable a broad base of astronomical research across the country; • Initiate significant long-term reductions in existing facilities in order to enable operation of the newest generation of NSF astronomy facilities, such as ALMA, as well as (future) ATST and LSST; • To the extent possible, defer the divestment of major observing capabilities until after the report of the MPS/AST Portfolio Review, scheduled to be completed in summer 2012. • No new unsolicited mid-scale proposals will be funded in FY 2012

November 22, 2011 J. Whitmore -- ASPERA Meeting 31 10/13/2011 31