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Cosmic Frontier at FermilabOverview of Experiments and Strategy

Craig HoganFermilab PACJune 7, 2013

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Cosmic Frontier Experiments at Fermilab

Dark Energy

Dark Matter

Cosmic Rays

Holometer

Initiatives

Mgmt

31 staff scientists, ~28 FTEsDark EnergyDeep, precise surveys of the universe: map history of expansion and growth of structure to probe physics of cosmic acceleration

Dark MatterDirect detection of WIMP dark matter particles

Highest Energy Cosmic RaysDetailed study of rarest, largest cosmic ray showers

Quantum GeometryMeasure fidelity of space-time with Planck sensitivity

FCPA Scientists

33 staff scientists (22 FTEs) work on experimental particle astrophysics

Additionally:8 experimental postdocs5 staff and 4 postdocs in theoretical particle astrophysics

Dark Energy

Dark Matter

Cosmic Rays

Holometer

Other

Management

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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

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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

Science Breakthroughs of the Year: 1998 and 2003

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Cosmic acceleration Precision cosmology ( WMAP,SDSS)

C. Hogan, Fermilab PAC, June 2013

Precision Cosmology at Fermilab: a 40 year experimental campaign(almost like we planned it)

SDSS (1990- 2010)Advent of precision cosmology

Imaging and spectroscopy

Many firsts (ISW, BAO, SNe…)

DES (2013-2018)Extends reach of wide imaging to the Hubble length for the first time

DESI (2018-20)Deeper, wider spectroscopy adds precision

LSST (2020-2030)Deeper, wider, longer imaging; close to physical limits

7C. Hogan, Fermilab PAC, June 2013

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Fermilab Dark Energy Program

Dark Energy Survey (2013-2018)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”) (~2018-2020)

Obtain ~107 spectra to z>1, still better Dark Energy precision

Large Synoptic Survey Telescope (~2020-2030) wider, faster, deeper imaging; total data ~100 times DES

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Dark Energy SurveyNext big step in cosmic surveys

Wide, deep (z>1), precise

DE Camera project led by Fermilab

Survey starts in 2013, runs 5 years

6DECam under construction at Fermilab

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

DES operations

Moving towards start of the survey this fallUnprecedented demands on CTIO and NCSA

New plan for data management system

Operational readiness reviews complete

Fermilab active on all frontsInstallation, testing, science verification, survey operations, data management, analysis and science support

FNAL scientists transitioning effort to new tasks

C. Hogan, Fermilab PAC, June 201311

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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

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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 deeperProven impact of SDSS comprehensive survey

Spectra synergize with photometrySample selection is important

Basic Architecture of DESI

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Positioner technology still TBDAffects all aspects of system

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Dark Energy Spectroscopic Instrument (DESI)

Managed and led by LBNL; CD-0 approved

Fermilab technical contributions: corrector, CCD packaging

Design choices under reviewCD-1 review late in CY2013Key choice: positioner technology

“Merger” of previous BigBOSS and DESpec teams underwayCollaboration taking shape

Collaboration meeting in July

Imaging survey needed for target selection (possibly including extended shallow survey by DECam)

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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.

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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

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Fermilab in LSST

DOE camera projectLed by SLAC; Fermilab participatesFermilab technical role: still undetermined, likely small

NSF project: everything elseLed 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 CollaborationFNAL scientists active in collaboration; activity coordinated by Scott DodelsonFNAL leading Software Working Group; hosting workshop todayFermilab proposes to build science analysis framework

DES is a pathfinderIndividual frames comparably deep, but ~9x slower overall survey speedReal data like LSST will be flowing this year; impacts many LSST systemsFermilab scientists experienced in calibration, operations, etc

Interest at Fermilab is highTypically 15 or 20 people at monthly LSST meetingsBut DES dominates time and attention right now

Fermilab asset: the team of experienced survey scientists

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Dark Energy strategy: summary

Dark Energy ScienceSupport (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

DESIFermilab participates in shaping and building DESI

Interaction with DES: target selection, joint analysis

Construction starts in ~2015, survey starts >2018

Large Synoptic Survey TelescopeFermilab 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

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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 unknownAdvances 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

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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: 10000 kg, ?

DAMIC: thick CCDs have exceptional sensitivity at low threshold, low massPrototype in operation at SNOLab; ~100g system under development

Generation 2 experiments reach the middle of the theoretical range expected for “standard WIMPs”

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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

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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

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Pierre Auger Observatory

Observatory: installed over a 3000 km2 site in Argentina – data taking started in 200424 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.

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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 principalsRequests plan by June 1 2013, for transfer of lab responsibilities by end of 2015

Planning for transition now underway among Auger institutionsNo current plans for Fermilab to hire additional staff in this area

Fermilab will shed management responsibility

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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

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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 frequencySensitivity limited by photon shot noise Goal: rms <10-22 Hz-1/2 (Planck spectral density of transverse position noise)

Collaboration: 20 scientists/students from 5 institutionsFunding: DOE, NASA, NSF, Aaron Chou DOE Early Career Award (2.5M)

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NOT quantum foam!

Not a test of the holographic principle!

Status:5-arm vacuum system complete~100W power-recycled interferometers operationalLIGO-based digital control system operationalDAQ, ~ 40MHz sampling, cross-correlation, FFT system operationalRF isolation demonstrated in ~10 hour runNear -term plan:Commission and operate two interferometers in nested configurationOptimize control system for power recycling, install high quality opticsBegin to probe space-time behavior in a never-before-tested regimeFuture: 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

Input mirror North end mirror

Holometer status and plans

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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

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“Snowmass” (CSS 2013)

Fermilab participating in community processFermilab scientists are active in working groups

Fermilab supports current HEP programCurrent 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 initiativesExplore 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

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Fermilab in CSS 2013 process

Fermilab convenors of Cosmic Frontier working groupsDan Bauer: CF1, WIMP Dark Matter Direct Detection, working group A, Status and Science Case (see http://arxiv.org/abs/1305.1605)

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

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Cosmic Frontier Snowmass issues

Dark MatterManage competition between experiments and technologies

Exploit synergies with accelerator program and indirect detection

These are also internal issues at Fermilab

Dark Energy and CMBMain 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 ParticlesGamma rays, CTA: not directly a Fermilab issue

New TechnologiesCosmic Instrumentation frontier: new detectors

Health of fieldGain support of the rest of the community for the cosmic frontier

Cosmic Frontier Experiment Strategy

Dark EnergyExpect x5 improvement in our understanding of dark energy with DES by 2018Follow up with spectroscopic survey (DESI) in 2018-2020Significant roles in dark energy science with LSST in 2020-2030

Dark MatterExpect x3 better sensitivity from current experiments by 2015Strong G2 experiments will provide x10 additional sensitivity to WIMPsIntend to play major role in G3 experiments to probe down to neutrino floor

Highest Energy ParticlesImproved understanding of origins/composition of ultra high energy cosmic rays by 2015Not planning for major role beyond 2015

Quantum GeometryUnique experiment to look for Planck-scale physicsFollow on will depend on what is seen with Holometer by 2015

New InitiativesNext generation CMB experimentNew axion-like particle searches using laser cavities and Tevatron magnetsDetector R&D leading to new experiments (mKIDs, SiPMs, Directional DM….)

C. Hogan, Fermilab PAC, June 201334

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Big-Picture Plan

• Plan A: We discover something new!WIMP events, varying dark energy, holographic noise,…

Then discovery sets priorities

• Plan B: We don’tChoices set by potential for discovery, overall science impact

Eventually, will move on from WIMP and Dark Energy programs

Start laying the groundwork now