Fluxes of Galactic Cosmic Rays

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2 o n m l p Flues o alactic Cosmic Rays sr s m - ev Flu - solar Modulation: Φ = 550 MV proton helium positron electron antiproton photon galde 50080/60080 (γ) Status o Cosmic Ray Measurements: good agreement beteen cosmic ray propagation/production model and data in bacground lues (, nuclei) general model ors!,, other heavy - - AMS-0 electrons AMS-0 positrons AT 9/5 positrons AMS-0 protons AMS-0 helium MAX antiprotons Caprice 9 antiprotons Caprice 98 antiprotons SS 95/9 antiprotons SS 0 antiprotons inetic nergy [ev] d bd aaeg 9ih DC[ QSRT DC

3 o n m l p q m s p Flues o alactic Cosmic Rays sr s m - ev Flu solar Modulation: Φ = 550 MV AMS-0 electrons AMS-0 positrons AT 9/5 positrons AMS-0 protons AMS-0 helium MAX antiprotons Caprice 9 antiprotons Caprice 98 antiprotons SS 95/9 antiprotons SS 0 antiprotons proton helium positron electron antiproton photon inetic nergy [ev] galde 50080/60080 (γ) Status o Cosmic Ray Measurements: good agreement beteen cosmic ray propagation/production model and data in bacground lues (, nuclei) general model ors!,, r l,, other heavy are sensitive to dar matter signals (annihilation) and lues/ractions sho some uneplained eatures need precise measurement o lues up to high energies! d bd aaeg 9ih DC[ QSRT DC

4 o n m l p q m s p u t Flues o alactic Cosmic Rays sr s m - ev Flu solar Modulation: Φ = 550 MV AMS-0 electrons AMS-0 positrons AT 9/5 positrons AMS-0 protons AMS-0 helium MAX antiprotons Caprice 9 antiprotons Caprice 98 antiprotons SS 95/9 antiprotons SS 0 antiprotons proton helium positron electron antiproton photon inetic nergy [ev] galde 50080/60080 (γ) Status o Cosmic Ray Measurements: good agreement beteen cosmic ray propagation/production model and data in bacground lues (, nuclei) general model ors!,, r l,, other heavy are sensitive to dar matter signals (annihilation) and lues/ractions sho some uneplained eatures need precise measurement o lues up to high energies! alloon periment: nvestigate inluence o atmosphere on lu measurements! d bd aaeg 9ih DC[ QSRT DC

5 T Requirements or positron lu measurements electron : antiproton proton : positron 5 solar Modulation: Φ = 550 MV Flu Ratio galde 50080/60080 (γ) inetic nergy [ev] total rejection is made up o the single rejections o the dierent subdetectors bd` ` bd aaeg 9ih \S] Z DC[ QSRT DC

6 v bd aaeg 9ih T Air shoer in arth s atmosphere \S] Z DC[ QSRT DC

7 y z ANTOCOSMCS Simulation o the arth s atmosphere and magnetic ield ith ANTOCOSMCS (developed by. Desorgher, Uni. ern laurent/planetocosmics) general properties: based on ANT atmospheric model: NRMSS magnetic ield: RF solar modulation: mean ield approimation { bd aaeg 9ih DC[ QSRT DC

8 y z p z ANTOCOSMCS Simulation o the arth s atmosphere and magnetic ield ith ANTOCOSMCS (developed by. Desorgher, Uni. ern laurent/planetocosmics) general properties: based on ANT atmospheric model: NRMSS magnetic ield: RF solar modulation: mean ield approimation properties o this simulation: input spectra are the lues o the conventional alprop model tuned in the loer energy region to match the data (galde astro-ph/0065) detection planes in several altitudes around the earth particle gun in m height starting positions are choosen to produce a isotropic distribution o cosmic rays only primaries that can hit the detection planes are started { bd aaeg 9ih DC[ QSRT DC

9 Scheme o simulations and analysis ANTOCOSMCS simulate at South ole etract galactic lues calculate errors compare secondary muons ith SS Ft. Sumner, TX veriy simulation solar Modulation orce ield approimation isotropic distribution in 0m height arth s magnetic ield and atmosphere (RF, NRMSS00) produce spectra o galactic cosmic ray ARO DarSUSY e bd aaeg 9ih DC[ QSRT DC

10 ƒ m ƒ m ƒ t ƒ y y z y T Solar Modulation taen rom: Journal o geophysical Research, Vol. : Usosin et. al., A physical reconstruction o cosmic ray intensity since 6 solar modulated lu, mean ield approimation: Œ Ž Œ } S } ˆ Š Œ S S }~ Œ Ž S MV D : / Ft. Sumner MV z : / South ole bd aaeg 9ih \S] Z DC[ QSRT DC

11 z c bd aaeg 9ih T sotropic distribution o cosmic rays m starting plane sin(latitude) longitude [deg] entries [#] entries [#] 5 5 azimuth [deg] cos(zenith) \S] Z DC[ QSRT DC

12 c bd aaeg 9ih T sotropic distribution o cosmic rays m detection plane sin(latitude) longitude [deg] entries [#] entries [#] 5 5 azimuth [deg] cos(zenith) \S] Z DC[ QSRT DC

13 t œ NRMSS atmospheric model & depth NRMSS properties: atmospheric model itted to. data o satellite accelerometers and orbit determination (mass density). data o incoherent scatter radar (temperature). data o solar ultraviolet occulatation (O Œ mass density) dependency on date/solar and magnetic parameters deintion o atmospheric depth: } } œ š d } altitude dependent atmospheric density, provided by the NASA via: detection altitude ž bd aaeg 9ih DC[ QSRT DC

14 T Temperature & depth proile ].5.5 depth [g/cm.5 latitude [deg] longitude [deg] latitude [deg] Depth Temperature Calculations done ith the olloing parameters: m altitude or the solar and magnetic parameters : Ÿ y Ÿ date: aj \S] Z C[ Q RT C temperature [K] 0 longitude [deg]

15 t z ƒ t u t Depth over time on South ole ] depth [g/cm year [a] m altitude latitude deg, longitude solar and magnetic parameters or each day deg: mean trajectory on South ole time has the largest inluence on the atmospheric depth (only small dependency on solar and magnetic parameters) jj C[ Q RT C

16 z ƒ T ) roperties o arth s Atmosphere (NRMSS deg), deg, long.: Calculation at mean balloon trajectory at south pole (lat.: y z Dec Temperature [deg Celsius] Altitude [m] inetic energy/temperature o atmosphere (ideal gas) dj \S] Z C[ Q RT C

17 Mean radiation length in Dec. at the South ole entries [#] number o radiation lengths calculated ith the atmospheric model and the trajectory o the cosmic rays mean number o crossed radiation lengths o all cosmic rays beore % because o the angular distribution o cosmic rays m is bd`j ` C[ Q RT C

18 vj T Rigidity Cuto ith RF \S] Z C[ Q RT C

19 j { T nluence o magnetic ield to secondary muon lues ev Ÿ - energy range o primaries: total, 0000 m, D primary, 0000 m, D secondary, 0000 m, D sr s m - ] Flu [ev - - SS. g/cm nergy [ev] \S] Z C[ Q RT C

20 z nluence o magnetic ield to secondary muon lues energy range o primaries: - ev sr s m - ] Flu [ev total, 0000 m, D primary, 0000 m, D secondary, 0000 m, D sin(latitude) secondary, 0000 m, D ] s m - deg Flu [sr SS. g/cm nergy [ev] longitude [deg] - j { C[ Q RT C

21 z z nluence o magnetic ield to secondary muon lues energy range o primaries: - ev sr s m - ] Flu [ev total, 0000 m, D primary, 0000 m, D secondary, 0000 m, D sin(latitude) secondary, 0000 m, D ] s m - deg Flu [sr SS. g/cm nergy [ev] longitude [deg] - j { C[ Q RT C

22 z nluence o magnetic ield to secondary muon lues energy range o primaries: - ev sr s m - ] Flu [ev total, 0000 m, D primary, 0000 m, D secondary, 0000 m, D sin(latitude) secondary, 0000 m, D ] s m - deg Flu [sr SS. g/cm nergy [ev] longitude [deg] - j { C[ Q RT C

23 nluence o magnetic ield to secondary muon lues energy range o primaries: - ev sr s m - ] Flu [ev total, 0000 m, D primary, 0000 m, D secondary, 0000 m, D sin(latitude) secondary, 0000 m, D ] s m - deg Flu [sr SS. g/cm nergy [ev] longitude [deg] - j { C[ Q RT C

24 y ej T Veriication o atmospheric physics model 000 m,. g/cm sr s m - ] 0000 m, g/cm Flu [ev SS. g/cm SS.68 g/cm - nergy [ev] ). / Comparison o simulations ith SS data in Ft. Sumner, TX ( Simulation seems to or ithin the errors! \S] Z C[ Q RT C

25 ositron lues in m South ole Dec. sr s m - ] Flu [ev primary generated, D total, 0000 m, D primary, 0000 m, D secondary, 0000 m, D Ratio total, 0000 m, D primary gen. primary, 0000 m, D primary gen nergy [ev] - nergy [ev] simulations done in the same ay as or Ft. Sumner, ecept o date and location j C[ Q RT C

26 Š Š Š Š t» t º ositron lues in m corrections S prim S atmo meaning o quantities: sec S tot ª «ª tot (all quantities are energy dependent) S number o particles (alrop, ANTOCOSMCS): S,, sec, ª, tot tot prim detection eiciency (detector simulation): to tae loer acceptance o TRD into account: S z Š Ÿ ev µ } Ž ³ ² q ± proton Rejection (detector simulation): ¼ t «ª or all energies ev Ž q ¹ n j loss o particles in atmosphere (ANTOCOSMCS): atmo energy dependent tracer misidentiication (detector simulation): S energy dependent cj C[ Q RT C

27 Š Š Š Š t» t º ½ z ositron lues in m corrections S prim S atmo meaning o quantities: sec S tot ª «ª tot (all quantities are energy dependent) S number o particles (alrop, ANTOCOSMCS): S,, sec, ª, tot tot prim detection eiciency (detector simulation): to tae loer acceptance o TRD into account: S z Š Ÿ ev µ } Ž ³ ² q ± proton Rejection (detector simulation): ¼ t «ª or all energies ev Ž q ¹ n j loss o particles in atmosphere (ANTOCOSMCS): atmo energy dependent tracer misidentiication (detector simulation): S energy dependent error estimates: statistical errors: systematic errors or atmospheric physics: systematic errors or detector properties: % % cj C[ Q RT C

28 Á À ¾ Š Š Š t p à  T m corrections ositron lues in tot tot tot S tot ª «ª S sec atmo S prim Š S «À «(all quantities are energy dependent) Rejections: presentation. ast roton rejections o Cal and Tracer -eiciencies o detector -/ not yet: consider general: use energy dependent rejections (to be done... ) cj \S] Z C[ Q RT C

29 Å Ä m qæ m Œ žj T n) S -lues ( - and ƒ Ä Total counts o 6 [#], S, 0 days, S, 0 days + - total e total e S N 5 nergy [ev] counts ith detector eiciencies and atmospheric loss! sr m Ÿ days S ith acceptance \S] Z C[ Q RT C

30 ad T days S lectron and ositron lues ith ] 9 Counts [ev 8 sr s m - ] 6 Flu [ev 5 e, S, 0 days e -, S, 0 days conv. alprop + AMS-0 electrons AMS-0 positrons AT 9/5 positrons nergy [ev] all corrections applied \S] Z C[ Q RT C

31 q n m m u t lectron and ositron lues ith days S sr s m - ] Flu [ev AMS-0 electrons AMS-0 positrons AT 9/5 positrons + e, S, 0 days - e, S, 0 days conv. alprop nergy [ev] ] Counts [ev - e + e + +e ositron Fraction - S, 0 days AT AMS0 conv. alprop nergy [ev] all corrections applied assumptions or and same behaviour in atmosphere same rejection same tracer resolution smaller errors ( atmo cancels in raction) : a d C[ Q RT C

32 lectron and ositron lues ith days S sr s m - ] Flu [ev AMS-0 electrons AMS-0 positrons AT 9/5 positrons + e, S, 0 days - e, S, 0 days conv. alprop nergy [ev] ] Counts [ev - e + e + +e ositron Fraction - S, 0 days AT AMS0 conv. alprop nergy [ev] all corrections applied S errors are dominated by statistics at higher energies this S has ca. AT ŒÈÇ statistics o a d C[ Q RT C

33 lectron and ositron lues ith days S sr s m - ] Flu [ev AMS-0 electrons AMS-0 positrons AT 9/5 positrons + e, S, 0 days - e, S, 0 days conv. alprop nergy [ev] ] Counts [ev - e + e + +e ositron Fraction - m / = 500 ev, m = 00 ev 0 tanβ= 5, µ>0, A = 0 0 DM signal boost actor: 5.0 S, 0 days AT AMS0 alprop + DM DM, DarSUSY conv. alprop nergy [ev] all corrections applied this dar matter signal is probably distinguishable ith a light in m altitude days S a d C[ Q RT C

34 ΠAntiproton lues in m (counts or days ith acceptance ٠m sr and ithout detector eiencies) sr s m - ] Flu [ev primary generated, D - total, 0000 m, D - primary, 0000 m, D - secondary, 0000 m, D nergy [ev] inluence o atmosphere seems to be in the same order as or positrons! j d C[ Q RT C

35 Œ É m u t Antiproton lues in m (counts or days ith acceptance Ÿ m sr and ithout detector eiencies) sr s m - ] Flu [ev primary generated, D - total, 0000 m, D - primary, 0000 m, D - secondary, 0000 m, D - ] + Antiproton Fraction [p/p - - MAX Caprice 98 Caprice 9 SS 95/9 SS 0 eat S, 0 days conv. alprop -6 - nergy [ev] nergy [ev] inluence o atmosphere seems to be in the same order as or positrons! same assumptions or detector eiciencies as or room or improvement! j d C[ Q RT C

36 Œ Antiproton lues in m (counts or days ith acceptance Ÿ m sr and ithout detector eiencies) sr s m - ] Flu [ev primary generated, D - total, 0000 m, D - primary, 0000 m, D - secondary, 0000 m, D - ] + Antiproton Fraction [p/p - - m / = 500 ev, m = 00 ev 0 tanβ= 5, µ>0, A = 0 0 DM signal boost actor:.0 MAX Caprice 98 Caprice 9 SS 95/9 SS 0 eat S, 0 days alprop + DM DM, DarSUSY conv. alprop -6 - nergy [ev] nergy [ev] inluence o atmosphere seems to be in the same order as or positrons! dar matter contribution j d C[ Q RT C

37 Πs hoton lues in m (counts or days ith acceptance ٠m sr and ithout detector eiencies) sr s m - ] Flu [ev primary generated, D total, 0000 m, D primary, 0000 m, D secondary, 0000 m, D nergy [ev] diuse s, averaged over all directions in the galay d d C[ Q RT C

38 Πs T m hoton lues in sr and ithout detector eiencies) m ٠days ith acceptance (counts or s, averaged over all directions in the galay diuse too many secondaries, lu measurement not possible! dd \S] Z C[ Q RT C

39 Ê Ì Ë Ê Ê Î K Ì Í Ê Summary & Outloo What have been done: simulation o the positron raction measurement on the South ole in m altitude ith S error estimation including the correction o the main uncertainties good measurement o positron raction possible (ca. statistics o AT) good measurement o antiproton ratio possible bd` ` d C[ Q RT C

40 Ê Ì Ë Ê Ê Î K Ì Í Ê Ê Ê Ê Ê Summary & Outloo What have been done: simulation o the positron raction measurement on the South ole in m altitude ith S error estimation including the correction o the main uncertainties good measurement o positron raction possible (ca. statistics o AT) good measurement o antiproton ratio possible What should be done: use more precise properties o S detector ind a better implementation o high energetic alphas ind out about the detecabilty o heavy ions to measure e.g. /C ratio chec or detectibility o other dar matter signals bd` ` d C[ Q RT C