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  • __ g;qM_¤.t¤.n.¢s OCR Output

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    Rakes /Que/ng: &¤.p¤

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    · Pgxcvxcms Aa.\·¢¢.l‘¤·ng OCR Output

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  • oswigvw- www M-" OCR Output

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  • A0 OCR Output

    Figure 4.1: The Cosmic Axion Search |Dc l‘:mIiIir< ct ul l987|

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    COUPLING LIMITS ASSUMING TURNER DENSITY

    ROCHESTER-BNL-FERMILAB

    COSMIC AXION SEARCH

  • Q OCR Output.. M- Wig

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  • clnvsll

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    neutrinosCooling of solar core? High _€¤€¥8>'

    LU$8 —> e5 in laboratory\

    Direct detectionTrapping in {un and planets

    Elastic Cross section

    Cosmic Rays

    ¤ $4 tt Z w YY .pCrolsing P F

    _" ` """`“‘* Eahaloofourgalaxy

    p _ \_ az , °°~"Z"“°°"`6_ _ Annihilation in the Low energy . High energyGvz Accelerator ConstraintsQ6

    W¢ihb¢¥8 me > 2 -€g,v

    Present Dark Matter Density

    Vt} ( (`T P s

  • moron ENERGY um OCR Output

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  • g 115 OCR OutputEkluwdQcuq botokqmowud

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    t Mainlg Compton =• flatdegraded)

    t Most: interaction 6n"electrons. (Neutrons can be

    + State of the art :].5 evtlkg/dag] /·94U`Radioactive background

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    trua ross sectionsc) Cosggfor heavg neutrinos with small hgpercharge)

    (e.g. vectorial coupling to neutron numberb) Ng\ etrg- charge cohgge/ngej/agtprElle MTS/k6{DPN

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    (e.g. axial vectorial coupling ¤ couples to

    factorgg{`

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  • , 0.0 10.0 20.0 30.0 40.0 50.0 GthéOCR Output

    Siiicon

    200 / ’/{ 1 Germanium

    400

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    A - ‘ 120.0 N¤n·na1is•a¥•t••-Vetwberq ___ L7`, H ` 1_ /

    Heavy NeutrinoMD .,1,. .,h_:,L*60-0

    M { Q Events/Kg/dau

    200.0

    ·0.5 10.0 20.0 30.0 40.0 50.0 66//c0.5 Event]Kg/Dau

    bone urkai evv/vt

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  • _I:>0.c\

  • zu OCR Output

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    OCR OutputOCR OutputOCR OutputOCR OutputCow l/@_vmfwv\q!2

  • 1.5 OCR Output

    Kiretic energy (keV)0.0 20.0 40.0 60.0 00.0 100.0

    0.0

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    0.6

    Fiuure lb `!°`8

    Ratio of ionisation doposiiion····1 Siliconn/0 1‘°

    Ki neiic ener9U (keV)

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  • ($7Lr OCR Output

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  • (Ballistic Phonons) OCR Output

    Cabrera etal [39] I Stanford. San Francisco State I Coherent neutrinos

    . I 1421

    Lanou, Seidel, Maris I Brown University I Solar Neutrino: (rotons)

    Sadoulet et al [35] I LBL..UC Berkeley I Dark matter

    Von Feilitasch et al [31] I Munich: Technical Unive¤ityI lnstrumentation, Neuuinos

    Dart MatterSmith etal [14] | Ruthcrford. Imperial Coll.

    Fiorini cul [14] | Milano Double Beta

    Niinikoski [41] I CERN Neuwino

    Mcudon. CERN. Aarhus. NYn I Coxon etal [12] | "Bonus' Collab. Ho (163). X Ray

    LBL. UC lrvmcX Ray Astronomyetal [40] I Livcrrmrc. QC Bcrkclcy

    X Ray AstronomyMc Canumn. Mosclcy caf:] Wisconsin. Goddard

    l'1wuou Uclcuun

    Physics InterestsInstitutions

    Bland San Francisco Snare Solar neutrinos

    Booth [16] Oxford Solar neutrinos

    InstruntcntationB:u0nc.Gr¤y [29] | N¤p0li,Axg¤nnc

    Twcxcnbold ESA X my Astronomy

    Zchndcr [30] SlN Neutrino. Instrumentation

    lnstrurncnution. Neutrino;Von Fciliusch etal [31] | Munich: Technical Univcrsicg

    Tunncl Jundium

    lnsuutnentationCabrcra ct al [25] [ Stanford, San Fmncisco Smtc

    Supcrccnducting films

    U. Souih CnmlinaDark rnattu. Double UctaDrukicrcx al [23] Briuish Columbia

    Coherent neutrino scatteringPrcuJ. Smdolsky [22] | Munich: Mu Planck lnsninuxc

    lnstrurnenutiou. NeutrinosVon Fciliusch cr al {BI] | Munich: Technical Universiu;

    Solar neuuinos. Dark MatterGonulcs :1 al [21] | Anmcy

    lnmgmg/ Solar neutrinosWaysand etal [17] | Paris VH/College dc Fmncc

    Supcrumuuwng (.ir·.u¤uI

    Phvsics lmcrcstsInsniunicns

  • sv. OCR Output

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  • 35 OCR Output

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  • 3% OCR Output

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  • Fig. 1

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    OCR OutputOCR Output1 aommsran

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    C5 OCR Output

  • his OCR Output

    _ Fig. 33

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  • MS OCR Output

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  • Lal:. OCR Output

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  • MWOCR Output

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  • is? OCR Output

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  • HQ OCR Output

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