1. Cosmic Frontier at Fermilab Overview of Experiments and Strategy
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Cosmic Frontier at Fermilab
Overview of Experiments and Strategy
Craig Hogan
Fermilab PAC
June 7, 2013

2. Cosmic Frontier Experiments at Fermilab
31 staff scientists, ~28 FTEs
Dark Energy
Deep, precise surveys of the universe: map history of expansion and growth of structure to probe physics of cosmic acceleration
Dark Matter
Direct detection of WIMP dark matter particles
Highest Energy Cosmic Rays
Detailed study of rarest, largest cosmic ray showers
Quantum Geometry
Measure fidelity of space-time with Planck sensitivity
Mgmt
Initiatives
Holometer
Cosmic Rays
Dark Energy
Dark Matter

3. FCPA Scientists
33 staff scientists (22 FTEs) work on experimental particle astrophysics
Additionally:
8 experimental postdocs
5 staff and 4 postdocs in theoretical particle astrophysics

4. Theoretical Astrophysics
Vital connections between theory and experiment
Dark Matter phenomenology (Hooper, Buckley, Cholis)
Dark Energy and CMB (Dodelson, Frieman, Stebbins)
Structure formation (Gnedin, Hearin)
Theory leadership roles in science from experiments
Josh Frieman is DES director
Scott Dodelson is coordinating dark energy science from DES and LSST, and developing LSST software frameworks
Dan Hooper plays major role in interpreting results from direct and indirect dark matter detection experiments

5. Dark Energy Science Cosmic expansion is accelerating
Physics is unknown
Energy or gravity?
Experimental approach: measure the universe
Expansion history
Distribution of mass
Growth of structure
Use light from galaxies, quasars, cosmic background
Progress driven by precision

6. C. Hogan, Fermilab PAC, June 2013
Science Breakthroughs of the Year: 1998 and 2003
Cosmic acceleration
Precision cosmology ( WMAP,SDSS)
C. Hogan, Fermilab PAC, June 2013

7. C. Hogan, Fermilab PAC, June 2013
Precision Cosmology at Fermilab: a 40 year experimental campaign (almost like we planned it)
SDSS ( )
Advent of precision cosmology
Imaging and spectroscopy
Many firsts (ISW, BAO, SNe…)
DES ( )
Extends reach of wide imaging to the Hubble length for the first time
DESI ( )
Deeper, wider spectroscopy adds precision
LSST ( )
Deeper, wider, longer imaging; close to physical limits
C. Hogan, Fermilab PAC, June 2013

8. Fermilab Dark Energy Program
Dark Energy Survey ( )
Will soon extend ultra wide, precision imaging to Hubble distance for the first time; factor ~5 improvement in Dark Energy precision
Dark Energy Survey Instrument (“DESI”) (~ )
Obtain ~107 spectra to z>1, still better Dark Energy precision
Large Synoptic Survey Telescope (~ )
wider, faster, deeper imaging; total data ~100 times DES

9. Dark Energy Survey Next big step in cosmic surveys
Wide, deep (z>1), precise
DE Camera project led by Fermilab
Survey starts in 2013, runs 5 years
DECam under construction at Fermilab 6

10. Blanco Telescope at CTIO: critical instrument for discovery, and now study, of cosmic acceleration

11. C. Hogan, Fermilab PAC, June 2013
DES operations
Moving towards start of the survey this fall
Unprecedented demands on CTIO and NCSA
New plan for data management system
Operational readiness reviews complete
Fermilab active on all fronts
Installation, testing, science verification, survey operations, data management, analysis and science support
FNAL scientists transitioning effort to new tasks
C. Hogan, Fermilab PAC, June 2013

12. Dark Energy Spectroscopy
“Rocky III” panel convened by DOE to recommend a path forward
Recommended a spectroscopic survey
Deeper than SDSS: back to z>1
Volume for statistics, depth for expansion history
Economical way to achieve Stage IV Dark Energy FOM
DOE project: Mid-Scale Dark Energy Spectroscopic Instrument (now, DESI)
DESI is Fermilab’s next Dark Energy initiative

13. Why Spectroscopy Benefits of high resolution spectra
Redshifts: precise mapping in 3D, velocity structure, correlations
Character of sources
Absorption lines: line-of-sight gas
Some DE science impacts are clear (e.g. BAO)
Already BAO with BOSS shows evidence of start to acceleration
Others are more subtle (e.g. modified gravity)
Some are not yet dreamt of
Like SDSS but deeper
Proven impact of SDSS comprehensive survey
Spectra synergize with photometry
Sample selection is important

14. Basic Architecture of DESI
Positioner technology still TBD
Affects all aspects of system

15. Dark Energy Spectroscopic Instrument (DESI)
Managed and led by LBNL; CD-0 approved
Fermilab technical contributions: corrector, CCD packaging
Design choices under review
CD-1 review late in CY2013
Key choice: positioner technology
“Merger” of previous BigBOSS and DESpec teams underway
Collaboration taking shape
Collaboration meeting in July
Imaging survey needed for target selection (possibly including extended shallow survey by DECam)

16. Planning status of DESI
DOE has notified NSF that the KPNO Mayall 4-m is the preferred site for their Mid-Scale Dark Energy Spectroscopic Instrument (MS-DESI).
DOE and NSF will form a MS-DESI Joint Oversight Group (JOG). The MS-DESI JOG will negotiate how DOE and NSF might jointly execute MS-DESI at the Mayall.
DOE will proceed to a Critical Decision 1 (CD-1) review by the end of this calendar year.
If CD-1 is successful, MS-DESI will remain in Design & Development phase, DOE/NSF will review and revise their agreement(s), and the project will head towards a CD-2 in 2014.
MS-DESI enters construction phase after: (a) DOE and NSF agree on a formal MOU; (b) Major Item of Equipment (MIE) new-start appears in a future budget request; and (c) successful DOE CD-2 and CD-3a (allows long-lead item procurement) reviews.

17. LSST: like DES but more so
3x bigger field
3x bigger aperture (~9x survey speed)
6x number of pixels
3x larger share of telescope
2x survey duration
4x main survey area
(LSST includes DES survey area)
4x frame rate
Time domain: ~1000-frame movie over 10 years
>100x as much data
~10x improvement in Dark Energy precision
~10x as many scientists
~10x the budget
Nearby mountaintop
Starts ~9 years later
C. Hogan, Fermilab PAC, June 2013

18. Fermilab asset: the team of experienced survey scientists
Fermilab in LSST
DOE camera project
Led by SLAC; Fermilab participates
Fermilab technical role: still undetermined, likely small
NSF project: everything else
Led by AURA/LSSTC; Fermilab may build parts of data management system: “develop use cases, requirements, and prototypes”; also not a large technical role
LSST Dark Energy Science Collaboration
FNAL scientists active in collaboration; activity coordinated by Scott Dodelson
FNAL leading Software Working Group; hosting workshop today
Fermilab proposes to build science analysis framework
DES is a pathfinder
Individual frames comparably deep, but ~9x slower overall survey speed
Real data like LSST will be flowing this year; impacts many LSST systems
Fermilab scientists experienced in calibration, operations, etc
Interest at Fermilab is high
Typically 15 or 20 people at monthly LSST meetings
But DES dominates time and attention right now
Fermilab asset: the team of experienced survey scientists

19. Dark Energy strategy: summary
Dark Energy Science
Support (operations, computing, software, consulting, interaction) for DES collaboration
Ongoing development and integration of DM and analysis software
DES workshops, visitors program will evolve into LSST role
Project and science leadership
DESI
Fermilab participates in shaping and building DESI
Interaction with DES: target selection, joint analysis
Construction starts in ~2015, survey starts >2018
Large Synoptic Survey Telescope
Fermilab modest technical roles in camera and data management
Fermilab scientists active in LSST Dark Energy Science Collaboration
Fermilab scientists plan to contribute to execution, as in DES
Construction starts in ~2015, survey starts ~2022

20. WIMP Dark Matter Detection
Basic principle: detect collisions of Galactic Weakly Interacting Dark Matter particles with nuclei
Basic challenge: rare events require exquisite control of experimental backgrounds
Masses and detailed interactions of particles are unknown
Advances require large detector masses with zero background
Detection, confirmation, study require multiple targets and technologies
Pursue multiple technologies now, downselect later
Detectors now have sensitivity to make a discovery
Hints of detections!
Fermilab is the lead lab on four experiments, using different technologies and optimized for different kinds of WIMPs

21. WIMP Dark Matter at Fermilab
SuperCDMS: Cryogenic Ge detectors have demonstrated background rejection and have excellent sensitivity to low-mass WIMPs
G1: 10 kg, Soudan G2: 100 kg, SNOLAB G3: 1500 kg, ??
COUPP: Bubble chambers promise best spin-dependent WIMP discovery potential; allows option of various target nuclei
G1: 60kg, SNOLAB G2: 500 kg, SNOLAB G3: ??, ??
Darkside: Liquid argon has best intrinsic background rejection and may be the right path towards high-mass WIMP discovery (competes with Xenon)
G1: 50 kg (Gran Sasso) G2: 1000 kg, Gran Sasso G3: kg, ?
DAMIC: thick CCDs have exceptional sensitivity at low threshold, low mass
Prototype in operation at SNOLab; ~100g system under development
Generation 2 experiments reach the middle of the theoretical range expected for “standard WIMPs”

22. WIMP Dark Matter strategy
DOE and NSF to select experiments later this year for construction FNAL experiments are contenders Fermilab plans to stay with WIMPS at least to the G3 scale Generic Detector R&D may enable new technologies: e.g. DAMIC, low- threshold directional detectors

23. Highest Energy Cosmic Rays – Pierre Auger
World’s leading experiment on the highest energy particles, fully operational since 2008 Fermilab is the lead lab in a large international consortium Energy spectrum Seeing the GZK cutoff or learning about sources? Anisotropy Do the highest energy cosmic rays point towards matter concentrations? Can we learn about the acceleration mechanism? Composition Learning about sources, or something new in hadronic cross sections at the highest energies? Comparison with LHC: Auger center of mass collision energies up to ~100 TeV

24. Pierre Auger Observatory
Observatory: installed over a 3000 km2 site in Argentina – data taking started in 2004
24 fluorescence telescopes;
1600 surface Cherenkov detectors;
Enhancements: 3 high elevation fluorescence telescopes, 60 infill detectors,
muon counter array.
Collaboration & Partnership: Large international collaboration of 19 institutions, 463 people. Fermilab hosts the Project Office. . 24

25. Pierre Auger Observatory: Fermilab Plans
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Pierre Auger Observatory: Fermilab Plans
June 2011: DOE Fermilab institutional review asks for a plan to phase out Fermilab involvement in Auger
December 2011: Director’s review commended achievements and continued value
Recommends continued support for next 2-3 years, then review of DOE participation
August 2012: Letter from Fermilab Director to Auger principals
Requests plan by June , for transfer of lab responsibilities by end of 2015
Planning for transition now underway among Auger institutions
No current plans for Fermilab to hire additional staff in this area
Fermilab will shed management responsibility
Closeout report: rams/Auger/DirRev/2011/12_15/Closeout_ Presentation_Director's_Review_of_Auger pdf

26. Quantum Geometry
Laboratory experiments address new fundamental physics far beyond the TeV scale
Fermilab Holometer will probe fidelity of space-time with Planck sensitivity
Dual, correlated 40-meter Michelson interferometers now in commissioning, first science results expected next year
Future experiments may explore new interactions of axion-like particles, dark sector photons, or other BSM effects

27. Fermilab Holometer
Science: Probe Planck scale limits on fidelity of space-time and origin of locality
Holographic information content normalized by black hole entropy
Explores new position degrees of freedom in emergent space-time
Exotic transverse position noise predicted to grow with propagation distance
Needs large, 2D, high frequency apparatus
Basic experimental setup:
Two neighboring 40m Michelson interferometers measure
correlated beamsplitter position jitter at MHz frequency
Sensitivity limited by photon shot noise
Goal: rms < Hz-1/2
(Planck spectral density of transverse position noise)
Collaboration:
20 scientists/students from 5 institutions
Funding: DOE, NASA, NSF,
Aaron Chou DOE Early Career Award (2.5M)
NOT quantum foam! 27

28. Not a test of the holographic principle!

29. Holometer status and plans
Input mirror
North end mirror
Status:
5-arm vacuum system complete
~100W power-recycled interferometers operational
LIGO-based digital control system operational
DAQ, ~ 40MHz sampling, cross-correlation, FFT system operational
RF isolation demonstrated in ~10 hour run
Near -term plan:
Commission and operate two interferometers in nested configuration
Optimize control system for power recycling, install high quality optics
Begin to probe space-time behavior in a never-before-tested regime
Future:
Goal is sub-Planck position noise spectral density
If non-conventional noise detected, test consistency with the noise model
-- Check predicted spectral features
-- Use back-to-back configuration to null the signal
-- Check predicted scaling with interferometer length

30. Quantum Geometry strategy
Holometer experiment active for next 2 or 3 years
If signal suggests presence of quantum-geometrical fluctuations, follow up with longer arms, better null configurations, and other improvements
If no fluctuations are detected at sub-Planckian level, apply laser technology to search for axion-like particles, dark-sector photons, or other physics beyond the standard model
Experimental configurations now being explored

31. “Snowmass” (CSS 2013) Fermilab participating in community process
Fermilab scientists are active in working groups
Fermilab supports current HEP program
Current projects scientifically active for this decade
Others already planned well into the next decade
Will participate in new DM and DE experiments
Look ahead to new long-term initiatives
Explore new opportunities at the boundaries
Quantum geometry, laboratory dark energy, axion detection
Proposed Chicago-led CMB project:
Large polarization survey
Will study neutrino properties, inflation
ANL likely lead lab
SPT 3G detector collaboration being explored in FNAL MKIDs lab
New detector R&D: MKIDs, SiPM, Directional DM etc

32. Fermilab in CSS 2013 process
Fermilab convenors of Cosmic Frontier working groups
Dan Bauer: CF1, WIMP Dark Matter Direct Detection, working group A, Status and Science Case (see
Dan Hooper: CF4, Dark Matter Complementarity
Scott Dodelson: CF5, Dark Energy and CMB
Aaron Chou and Craig Hogan: CF6, subgroup C, Exploring the Basic Nature of Space and Time
Active Participants
J. Estrada: co-organizer of Argonne Instrumentation Frontier workshop
M. Soares-Santos: convenor of Snowmass Young
SLAC Cosmic Frontier meeting participation and active WG participation by: Crisler, Frieman, Hsu, Kent, Lippincott, Nord, Para, Penning, Sonnenschein, Wester
About half of the Cosmic Frontier staff

33. Cosmic Frontier Snowmass issues
Dark Matter
Manage competition between experiments and technologies
Exploit synergies with accelerator program and indirect detection
These are also internal issues at Fermilab
Dark Energy and CMB
Main DE project directions are set
Focus now on DES, DESI, LSST and their science
Considerable Fermilab effort now and in the future
No clear successor to LSST
Will DOE partner on a major CMB project for neutrino and inflation physics?
Cosmic Particles
Gamma rays, CTA: not directly a Fermilab issue
New Technologies
Cosmic Instrumentation frontier: new detectors
Health of field
Gain support of the rest of the community for the cosmic frontier

34. Cosmic Frontier Experiment Strategy
Dark Energy
Expect x5 improvement in our understanding of dark energy with DES by 2018
Follow up with spectroscopic survey (DESI) in
Significant roles in dark energy science with LSST in
Dark Matter
Expect x3 better sensitivity from current experiments by 2015
Strong G2 experiments will provide x10 additional sensitivity to WIMPs
Intend to play major role in G3 experiments to probe down to neutrino floor
Highest Energy Particles
Improved understanding of origins/composition of ultra high energy cosmic rays by 2015
Not planning for major role beyond 2015
Quantum Geometry
Unique experiment to look for Planck-scale physics
Follow on will depend on what is seen with Holometer by 2015
New Initiatives
Next generation CMB experiment
New axion-like particle searches using laser cavities and Tevatron magnets
Detector R&D leading to new experiments (mKIDs, SiPMs, Directional DM….)
C. Hogan, Fermilab PAC, June 2013

35. Big-Picture Plan Plan A: We discover something new! Plan B: We don’t
WIMP events, varying dark energy, holographic noise,…
Then discovery sets priorities
Plan B: We don’t
Choices set by potential for discovery, overall science impact
Eventually, will move on from WIMP and Dark Energy programs
Start laying the groundwork now