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Base Grant Status at NSF

Base Grant Status at NSF. Presentation for P5 at Fermilab, Sept 24-25, 2007. J. Whitmore, Ani Aprahamian (PNA) F. Cooper (Theory) J. Kotcher (DUSEL) M. Pripstein (LHC) M. Goldberg, *J. Reidy , + R. Ruchti (EPP). + Until Oct 17. *After Oct 1. Topics. NSF Budgets FY2003-08 (Request)

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Base Grant Status at NSF

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  1. Base Grant Status at NSF Presentation for P5 at Fermilab, Sept 24-25, 2007 J. Whitmore, Ani Aprahamian (PNA) F. Cooper (Theory) J. Kotcher (DUSEL) M. Pripstein (LHC) M. Goldberg, *J. Reidy, +R. Ruchti (EPP) +Until Oct 17 *After Oct 1

  2. Topics • NSF Budgets FY2003-08 (Request) • EPP Underlying Themes/Scope • PNA Program Scope/Highlights • Recommendations of UGPS • Possible Future Projects • Summary NSF EPP+ PNA Programs @ P5 Meeting, 24-25 Sept 2007

  3. House and Senate Action For FY08: Current status (from FYI #93, Sept 5, 2007): FY2007 NSF budget: $5,917.2 M For 2008, Bush Admin requested $6,429.0M, increase of 8.7% SENATE Appropriations Committee (FYI#71,July 9): Sent to the floor a bill that would increase NSF by 10.8% to $6,553.4M HOUSE (Details in FYI#78,July 24): Has passed a bill that would increase NSF by 10% to $6,509.0M: The House Appropriations Committee report stated: “This level of funding will support the doubling of the NSF budget in 10 years as part of a long-term, sustained commitment to investment in basic research and development which provides the foundation for innovation and future technologies.” NSF EPP+ PNA Programs @ P5 Meeting, 24-25 Sept 2007

  4. NSF Budget by Directorate NSF EPP+ PNA Programs @ P5 Meeting, 24-25 Sept 2007

  5. MPS Funding by Division NSF EPP+ PNA Programs @ P5 Meeting, 24-25 Sept 2007

  6. MPS 10-Year Funding History Request PHY NSF EPP+ PNA Programs @ P5 Meeting, 24-25 Sept 2007

  7. Physics Division Funding *Centers, MRI, other = $33.8M PI programs = $130.8M # +$1M from OPP NSF EPP+ PNA Programs @ P5 Meeting, 24-25 Sept 2007

  8. EPP + PNA Portfolio • University Program • EPP Accelerator based physics • Hadron Colliders: CDF, DØ, CMS, ATLAS, LHCb • Electron Positron Colliders: CLEO-c, BaBar,… • Neutrinos: MINOS, NOVA, MINERvA, MiniBooNE • Particle and Nuclear Astrophysics • Dark Matter:CDMS, COUPP, XENON10, DRIFT-II, ZEPLIN-II • UltraHigh Energy Universe: HiRes/TA, Pierre Auger, VERITAS, MILAGRO • Neutrinos: Double Chooz, Super-K, Borexino, CUORE • Other • Theory • Computational physics • LHC Experiments: Maintenance and Operations • DUSEL and DUSEL R&D • CESR/CLEO-c • Accelerator and Detector R&D • ILC Accelerator and Detector R&D • MICE • Advanced Technologies • Partnerships & Broader Impacts NSF EPP+ PNA Programs @ P5 Meeting, 24-25 Sept 2007

  9. EPP+PNA Funding History NSF EPP+ PNA Programs @ P5 Meeting, 24-25 Sept 2007

  10. Base + Allied Funding NSF EPP+ PNA Programs @ P5 Meeting, 24-25 Sept 2007

  11. EPP(1): Allied Funding FY07 NSF EPP+ PNA Programs @ P5 Meeting, 24-25 Sept 2007

  12. EPP(2): Underlying Themes • Empowering University-Based Investigators • Adding Value • Partnerships • Building Interdisciplinary Collaboration • Broadening Participation • Single Investigators • Non-traditional/Underrepresented participants • Research at Undergraduate Institutions • Education, Outreach and Broader Impacts NSF EPP+ PNA Programs @ P5 Meeting, 24-25 Sept 2007

  13. EPP(3): Partnerships • Cyberscience • Tier 2c – with OCI • UltraLight – with OCI • OSG – with OCI and DOE • Education with research • QuarkNet – with OMA, EHR and DOE/HEP • CHEPREO – with OMA, OCI, EHR, OISE • I2U2 – with OMA, EHR, PHY • Mariachi – OCI funded • CyberBridges – OCI funded • PIRE (UK,KSU,UNL,UIC, UPRM) – with OISE • ILC Outreach – with OISE NSF EPP+ PNA Programs @ P5 Meeting, 24-25 Sept 2007

  14. EPP(4): FY07 Funding Actions 85 Total Funding Actions Mean of $237k based on 70 actions 2 Actions > $1M 13 small awards for conferences and workshops. NSF EPP+ PNA Programs @ P5 Meeting, 24-25 Sept 2007

  15. EPP(5): University Support NSF EPP+ PNA Programs @ P5 Meeting, 24-25 Sept 2007

  16. EPP(6): Distribution of Univ Group FY05 NSF EPP+ PNA Programs @ P5 Meeting, 24-25 Sept 2007

  17. PNA(1) Program Funding I II III IV Note: all of these values include base group funding From FY02 to FY07, increase by 64% (excl. DUSEL R&D) NSF EPP+ PNA Programs @ P5 Meeting, 24-25 Sept 2007

  18. PNA(2) Funding in FY07 Note: in $k Note: all of these values include base group funding NSF EPP+ PNA Programs @ P5 Meeting, 24-25 Sept 2007

  19. PNA(3): Ultra-High Energy Universe UHE Neutrinos IceCube 22 strings $$ NSF/…. UHE Cosmic Rays HiRes S. Auger TA UHE Gamma-Rays STACEE VERITAS MILAGRO Highlights from HiRes and Auger: S.AUGER $$ HiRes/TA - NSF Auger – NSF/DOE/… (From P. Mazur, 2007) NSF EPP+ PNA Programs @ P5 Meeting, 24-25 Sept 2007

  20. PNA(4): Ultra-High Energy Universe Highlights from VERITAS: • Detection of TeV gamma-ray emission from microquasar LSI +61 303. Fascinating binary system with neutron star/BH and companion. S.AUGER Discovery of supernova remnant IC 443 as a very high-energy source. This is one of the “prototypical” SNRs, thought to be the origin of cosmic rays. $$ VERITAS – NSF/DOE/… NSF EPP+ PNA Programs @ P5 Meeting, 24-25 Sept 2007

  21. PNA(5): Ultra-High Energy Universe Highlights from MILAGRO: (RA = 70, Dec = 15) • Signal (A) disappears when their cosmic-ray rejection is applied • MILAGRO notes it is a charged particle shower and not single high energy gamma rays hitting the pond • Signal (A) maintains significance when energy cut is raised • (Expected 7; observed 13) => hard energy spectrum • Anisotropy due to hard (<2.6) spectrum cosmic rays: WHAT IS IT? • These are probably the highest energy gamma rays detected > 100 TeV (1014 eV) • Indicative of a hard spectrum (2.05) of gamma rays up to 100 TeV MGRO J1908 +06 S.AUGER $$ MILAGRO – NSF/DOE NSF EPP+ PNA Programs @ P5 Meeting, 24-25 Sept 2007

  22. PNA(6): Neutrinos 300 tons of pseudocumene-based scintillator – 100 tons fiducial volume Observe: the first real-time spectral measurement of sub-MeV solar neutrinos from 7Be; the result (47±7±12 cts/day per 100 tons) is consistent with predictions of the Standard Solar Models and neutrino oscillations with the LMA-MSW parameters: • Highlights from Borexino (49±4 with osc./75±4 no osc.) 2 MeV $$ Borexino – NSF/INFN/.. 800 keV NSF EPP+ PNA Programs @ P5 Meeting, 24-25 Sept 2007

  23. PNA(7): 0nbb • NuSAG (Sept 1, 2005): “The following three experiments, listed in alphabetical order, have the highest priority for funding: CUORE, EXO, Majorana.” For Super-NEMO, “Support is not a priority.” (From S. Katsanevas, TAUP2007) • With DOE-ONP; NSF will fund the electronics for CUORE – presently in the CD-1 approval process • NSF has a small involvement with NEMO-3 and EXO NSF EPP+ PNA Programs @ P5 Meeting, 24-25 Sept 2007

  24. UGPS(1) • The primary recommendation is • (1) $$ The University Grants Program must be strengthened in order to achieve the goals of the national high energy physics program, as articulated by EPP2010. This requires increased investment and careful attention to building and sustaining levels of personnel and infrastructure necessary for successful university research groups. • I note that 11 of the 15 recommendations involve a request for more $$ • I note that as far as I can tell no priority to them • PHY has a strategic portfolio balance established in consultation with the community through discussions with our COV every three years that no less than 50% of the Divisional funds will be devoted to PI support (< 10% to centers, ~35% to facility OPS, as shown in slide on PHY funding) NSF EPP+ PNA Programs @ P5 Meeting, 24-25 Sept 2007

  25. UGPS(2) • 2) $$ A higher priority in the overall HEP program should be given to funding directed at university-based theoretical particle physics for the purpose of increasing the number of grant-supported graduate students. Support for students and postdocs doing calculations related to upcoming experiments is particularly urgent. • The NSF has been addressing this issue long before the UGPS report: • Fred Cooper has been working with the phenomenology community to organize and figure out the best way to prepare for the LHC... this started around 3 years ago at the 2004 DPF meeting! • The present LHC initiative group started organizing at the Madison Phenomenology Meeting in May 2005. • Special funding for students and post-docs was initiated through the LHC Theory initiative: • The funding profile planned is: • FY 2007 $100K (thru’ supplement to JHU) • FY 2008 $250K (50% from OMA) • FY 2009 $450K • FY 2010 $500K • This funding will also be augmented as allowed by the Physics funding profile increases to allow for more funding for proposals in the area of phenomenology. NSF EPP+ PNA Programs @ P5 Meeting, 24-25 Sept 2007

  26. UGPS(3) • (3) $$ Group sizes should be sustained, and increased where appropriate and supported by peer review. The agencies should make a special effort to support long-term research scientists as an integral part of this group structure, particularly when they provide expertise essential to the experimental program or leadership at a remote laboratory. • All proposals to NSF are MERIT-reviewed • Group sizes are decreased or increased where appropriate and supported by merit-review • Funds are allocated to a PI and can be (mostly) spent as they see fit • Issue with long–term research scientists on “soft” money is a concern for their future – up to the PI to make this decision; this issue is evaluated carefully in the merit-review process • (4) $$ University-based technical development should be funded at a level commensurate with its great importance. The investment should be adequate to provide the necessary equipment and technical and engineering support. • All proposals to the NSF are merit reviewed, and most are also discussed, compared and prioritized by a peer-composed panel each year. We believe that this does enable us to fund each university group at the “appropriate level”, consistent with the overall funding levels of the agency. NSF EPP+ PNA Programs @ P5 Meeting, 24-25 Sept 2007

  27. UGPS(4) • (5) As much as possible, universities should be funded through merit-based peer-reviewed proposals, rather than through specific project-based funds. • Nearly all proposals to the NSF are merit reviewed (the exceptions being Workshop proposals, supplements, creative extensions and SGER, Small Grants for Exploratory Research), as they have been since the NSF was founded • These same proposals are also discussed, compared and prioritized by a peer-composed panel each year • The larger requests are now reviewed by a site visit panel of 3-4 external peer reviewers • Note the next recommendation says that “Project managers should utilize university resources”; are these recommendations completely consistent? • (6) $$ The agencies should support university technical infrastructure, including hardware development, through grants. In addition, project managers should utilize university resources which are economical and effective, and they should report on this optimization at major project reviews. • See comments on previous recommendation • We provide extensive funds to the various projects (eg ATLAS/CMS, AUGER, VERITAS, IceCube to name a few). It is the responsibility of the managers to allocate the funds as they see fit. We should not be micro-managing them; however, we do have major reviews of these projects as part of our oversight responsibilities: from the ATLAS RP through FY06, $42M went to labs, $25M to universities • For the LHC this year (FY07), the earlier slides (#9-10) show a 34.7% increase NSF EPP+ PNA Programs @ P5 Meeting, 24-25 Sept 2007

  28. UGPS(5) • Three recommendations directly address issues that arise from overseas operations: • (7) The agencies should continue their efforts to ensure that the vision for LHC computing is realized. This includes working across and within agencies to ensure sufficient network and computing capacity. • The agencies do appreciate these two issues and we are working with US ATLAS and US CMS to encourage them to set up their internal committees to make recommendations of this issue; a US LHC committee is being convened • Additionally, Open Science Grid is being supported strongly by both NSF and DOE – LHC benefits as well as other sciences • (8) $$ The agencies should support the increased travel and subsistence costs of university researchers participating in the LHC and other overseas experiments. • We merit-review all proposals, including the PI’s request for travel funds • These same proposals are also discussed, compared and prioritized by a peer-composed panel each year • The larger requests are now reviewed by a site visit panel of 3-4 external reviewers • This year, FY07, we have started having reverse site visits, with a peer-composed external panel, to specifically look at the LHC contributions in each proposal • (9) $$ The agencies should support efforts to ensure that both U.S. sites and key sites abroad are equipped with remote videoconferencing systems that are reliable, robust, and readily available. • The agencies do appreciate this issue and we are working with US ATLAS and US CMS to encourage them to set up their internal committees to make recommendations of this issue (see above) NSF EPP+ PNA Programs @ P5 Meeting, 24-25 Sept 2007

  29. UGPS(6) • (10) The Scientific Assessment Groups (SAGs) should regularize their role in reviewing projects. • o Each SAG should actively monitor and prioritize the experiments and R&D in its area. It should evaluate both physics goals and technical design. • o The SAGs should report to P5, timing their reports so that they are available to • P5 when needed. • o The SAGs should review all experiments with expected construction costs above $5M, along with smaller ones seeking review. This includes both experiments that are affiliated with a U.S. laboratory and those that are not. Additional SAGs should be created as needed to cover all areas (taking care to avoid proliferation). • o HEPAP should establish mechanisms for prioritizing experiments whose cost is above $5M but below the P5 threshold. The prioritization process should take advantage of input from the SAGs and should reflect the breadth of the field. • In PNA, we have already announced (see program description on the NSF web page) that for larger requests (ie above $1M) at the program officer’s discretion, the proposal will be subjected to a cost review, including scientific goals, and examining the degree to which the proposed project can achieve these goals • (11) $$ The University Grants Program should fund the development and mounting of small and mid-scale university-based experiments that are highly rated by peer review and, where appropriate, by the SAGs and P5. This may require supplements to the University Grants Program. • MRI • APPI NSF EPP+ PNA Programs @ P5 Meeting, 24-25 Sept 2007

  30. UGPS(7) • (12) A University Grants Program Committee (UGPC) should be formed to consult with University Grants Program managers of both agencies on the issues facing the University Grants Program. The chair of this committee should be chosen cooperatively by both agencies and by the chairs of the HEPAP, DPF, DAP, and DPB and should serve as a spokesperson for the university community. • We are discussing between the agencies how to implement this; needs a careful charge; note: 14 of the 23 members of HEPAP are Univ. • (13) We applaud the COV process and endorse its continuation. Among the issues that future COVs should address are: • o Mechanisms for the consistent review of lab- and university-based researchers • o The competitive review of proposals, through panels or other means, within the University Grants Program • o The workload of University Grants Program staff • o Implementation of a DOE database comparable to the one used by NSF that makes institutional, funding, demographic, and programmatic information readily available • The NSF has been using the COV process for many years (at least 20) and it does consider the first three points noted above NSF EPP+ PNA Programs @ P5 Meeting, 24-25 Sept 2007

  31. UGPS(8) • (14) $$ Additional support should be made available to enable undergraduates and high school teachers to participate in experiments offshore. In addition, support should be continued for an REU program at CERN, following discussion of its structure with representatives of interested university groups. • NSF and DOE provide funds for QuarkNet to work with teachers and undergraduates • The REU-site and RET programs accept proposals which are then merit reviewed • (15) $$ The agencies should foster outreach by, for example, funding new positions dedicated to facilitating and coordinating university outreach efforts. • We have increased the funding for QuarkNet over the last several years • We have provided funds to many projects, many of which have staff funded, either through university funds or through NSF grant funds, to work on Broader Impacts and E&O • Some examples are I2U2, CHEPREO, ASPIRE, LIGO, IceCube, Cornell U, VERITAS • We provide value-added though working with DOE and others at NSF NSF EPP+ PNA Programs @ P5 Meeting, 24-25 Sept 2007

  32. Future PNA Projects • 3 Projects have been ended in 2006-7: • HiRes, STACEE and MILAGRO • → TA/(LE), VERITAS, (HAWC) • Dark Matter: • DEAP/CLEAN • LUX • UHE Cosmic Rays: • TALE • N. AUGER • UHE Gamma-Rays: • HAWC • AGIS • Neutrino-less Double Beta Decay: MAJORANA • DUSEL activities NSF EPP+ PNA Programs @ P5 Meeting, 24-25 Sept 2007

  33. Summary • We have a vested interest in University Groups – PI support > 50% in PHY • NSF has a successful history of partnerships with DOE/OHEP and DOE/ONP • NSF vision of partnerships for the Future • ILC: DOE is lead, with NSF in supporting role • DUSEL: NSF is lead, with DOE in supporting role • We take advice from the community seriously (Merit and Panel reviews) • Merit review is a cornerstone of our decision process. • “We respond to proposals” NSF EPP+ PNA Programs @ P5 Meeting, 24-25 Sept 2007

  34. The BIG Picture (From S. Katsanevas, TAUP2007) NSF EPP+ PNA Programs @ P5 Meeting, 24-25 Sept 2007

  35. Additional Slides

  36. DARK MATTER: DEAP/CLEAN DEAP 0initial R&D detector Pico-CLEANinitial R&D detector • Single phase LAr/LNe DEAP I7 kg LAr2 warm PMTsSNOLab 2007 Micro-CLEAN4 kg LAr and LNe 2 cold PMTssurface tests at Yale 10-44 cm2 $960k Mini-CLEAN 360360 kg LAr/LNe (100 kg fiducial mass)80 cold PMTsunderground DUSEL or SNOLab late 2008 topics of this meeting 10-45 cm2 DEAP/CLEAN 36003600 kg LAr/LNe (1000 kg fiducial mass)266 cold PMTs*underground at SNOLab late 2008 $5,824k 10-46 cm2 WIMP ssensitivity 10-100 ton LNe Detectorpp solar n, supernova, dark matter 10-46 cm2proposals ~ 2011 NSF EPP+ PNA Programs @ P5 Meeting, 24-25 Sept 2007

  37. Timelines for DEAP/CLEAN Project DARK MATTER: DEAP/CLEAN DUSEL EIP 2nd DMSAGReview NSF EPP+ PNA Programs @ P5 Meeting, 24-25 Sept 2007

  38. UHE Cosmic Rays: TALE • TALE: Telescope Array Low energy Extension • Target energy range is 1017-19 eV • With a SD infill array • And tower FD (for higher altitude) • Goal: to study the primary CR composition in the low energy region NSF EPP+ PNA Programs @ P5 Meeting, 24-25 Sept 2007

  39. UHE Cosmic Rays: N. AUGER • Chosen site is SE Colorado, initial area is 4,000 sq miles (10,370 km2), 3.3 times SPAO • Same latitude and elevation as SPAO • Possible for future expansion • SD located on a square-mile grid covering a 84x48 mile area • FD would be split into 3 half-eyes, in order to maximize the number of hybrid events • # PMTs/tank will be reduced from 3 to 1 • Requesting Construction starting in 2009, completion in 2012 • • Expecting to submit an R&D proposal in Fall 2007 • Comments taken from D. Nitz, ICRC2007/arXiv:0706.3940v1 NSF EPP+ PNA Programs @ P5 Meeting, 24-25 Sept 2007

  40. UHE g-rays: HAWC • High Altitude Water Cherenkov detector • 4100 m above sea level • At Sierra Negra, MX • Est. ~$6M total • 15x Milagro sensitivity • Expecting a proposal in September, 2007 • VERITAS, HESS, MAGIC, Whipple sensitivity in 50 hours, (~0.2 sr/yr) • GLAST sensitivity in 1 year (4p sr) • HAWC, Milagro, sensitivity in 1 year (2p sr) NSF EPP+ PNA Programs @ P5 Meeting, 24-25 Sept 2007

  41. UHE g-rays: AGIS • AGIS: Advanced Gamma-ray Imaging System • U.S. (AGIS) and European groups (CTA) are currently in the planning stages for a next generation gamma-ray experiment (50-100 ACTs) • With 1 km2 effective area, 10% energy resolution, arcmin angular resolution, and energy thresholds as low as 40 GeV. • Such instruments could achieve sensitivities of 10-13 down to 10-10 erg cm-2 sec-1 at 200 GeV; energy range from GLAST up to 50 TeV • Open to new technologies. • • Submit joint R&D proposal (~$6M) to NSF/DOE by 9/26/07 • Aiming at ~$100M level project ($1M/telescope) • • New technologies required to reduce cost • Managing institutions: • Univ. of Chicago (NSF) and ANL (DOE). • SLAC plan to participate in camera development. CTA ~ $100-$200M NSF EPP+ PNA Programs @ P5 Meeting, 24-25 Sept 2007

  42. Double Beta Decay Expts NSF EPP+ PNA Programs @ P5 Meeting, 24-25 Sept 2007

  43. Summary of DM Projects (From P. Belli, TAUP2007) NSF EPP+ PNA Programs @ P5 Meeting, 24-25 Sept 2007

  44. High Energy Gamma-Rays (From Hofmann, TAUP2007/Hinton ICRC2007) NSF EPP+ PNA Programs @ P5 Meeting, 24-25 Sept 2007

  45. High Energy Gamma-Rays: MILAGRO • Milagro has discovered3 new & 4 candidate sources in the Galaxy. • 5/7 of these TeV sources have GeV counterparts (only 13 GeV counterparts in this region - excluding Crab) J and C NSF EPP+ PNA Programs @ P5 Meeting, 24-25 Sept 2007

  46. UHE Neutrinos: IceCube • The main goal of the experiment is to detect neutrinos in the energy range from 1011 eV to about 1021 eV. • The sources of neutrinos coming "up" from below could be black holes, GRBs, or supernova remnants. • The IceCube In-Ice detector will consist of a minimum of 4200 DOMs (optical modules) deployed on 70 vertical strings buried 1450 to 2450 meters under the surface of the ice, and an IceTop surface air-shower detector array comprised of a minimum of 280 optical modules. NSF EPP+ PNA Programs @ P5 Meeting, 24-25 Sept 2007

  47. Neutrino properties: Double Chooz • The Double Chooz experiment goal is to search for a non-vanishing value of the θ13 neutrino mixing angle. This is the last step to accomplish prior moving towards a new era of precision measurements in the lepton sector. • Double Chooz will use two identical detectors, one at 300 m and another at 1.05 km distance from the Chooz nuclear cores. • The plan is to start operation in 2007 with one detector and to have both detectors operating by the end of 2008. In this scenario, Double Chooz will reach a sin2(2θ13) sensitivity of 0.07 after 1 year with 1 detector, and 0.03-0.02 after 3 years of operation with both detectors. • NSF will fund outer muon shield veto $2.3M NSF EPP+ PNA Programs @ P5 Meeting, 24-25 Sept 2007

  48. Neutrino-less Double Beta Decay: CUORE • With DOE-NP, Spain, and INFN in LNGS • NSF will help fund the electronics ~$1.3M • Cryogenic bolometer of 988, 750 g-TeO2 crystals • Effective mass of 200 kg of 130Te w/o enrichment • Will search for 0nbb with sensitivity to well below 100 meV in the effective Majorana mass or, in the “inverted hierarchy,” can prove n is a Dirac particle by putting stringent limits on the 0nbb lifetime. • Start data-taking in 2011, reaching T1/2 = 2.1x1026 yr in 5 years, corresponding to <mn> = 19-100 meV, depending on nuclear matrix elements NSF EPP+ PNA Programs @ P5 Meeting, 24-25 Sept 2007

  49. Acronyms - I NSF EPP+ PNA Programs @ P5 Meeting, 24-25 Sept 2007

  50. Acronyms - II NSF EPP+ PNA Programs @ P5 Meeting, 24-25 Sept 2007

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