1 / 16

- Functional Requirements - Background - Examples of expected Signal Track

EUSO-BALLOON DESIGN REVIEW, 18.12.2012, CNES TOULOUSE. Performances of the EUSO-Balloon. Andrea Santangelo IAAT, Eberhard-Karls Univerität Tübingen. - Functional Requirements - Background - Examples of expected Signal Track - An “idea” of angular resolution .

jennis
Download Presentation

- Functional Requirements - Background - Examples of expected Signal Track

An Image/Link below is provided (as is) to download presentation Download Policy: Content on the Website is provided to you AS IS for your information and personal use and may not be sold / licensed / shared on other websites without getting consent from its author. Content is provided to you AS IS for your information and personal use only. Download presentation by click this link. While downloading, if for some reason you are not able to download a presentation, the publisher may have deleted the file from their server. During download, if you can't get a presentation, the file might be deleted by the publisher.

E N D

Presentation Transcript

  1. EUSO-BALLOON DESIGN REVIEW, 18.12.2012, CNES TOULOUSE Performances of the EUSO-Balloon Andrea Santangelo IAAT, Eberhard-KarlsUniverität Tübingen • - Functional Requirements • - Background • - Examples ofexpected Signal Track • - An “idea” of angular resolution

  2. Functional requirements R-4.1-1 Background imaging The Instrument shall image the UV sky background in the bandwidth used by the JEM-EUSO mission observational technique. The background includes star light, airglow, light from artificial sources. Test of the trigger algorithms, switch between observational modes R-4.1-2 Detection of EAS (from the edge of space) The Instrument shall trigger, detect and image EAS with energy above 1018 eV that might develop in the field of view. R-4.1-3 Technology demonstrator All key components and the relative sub-assembly items should be tested according to the configuration foreseen for the JEM-EUSO mission. This is needed to test the JEM-EUSO detection chain. UPDATE: Test capability of the IR-CAM; Test of laser induced EAS. Performances of the EUSO-Balloon

  3. On the night-sky background. Nightglow background: 100 - 500 photons/m2/ns/sr Sakaki, BABY, NIGHTGLOW, Tatiana increases by ~1.5 with clouds Airglow (~100 km height): 250 - 600 photons/m2/ns/sr Moon phases (<25%): <100 ph/m2/ns/sr Background measurements with coarseresolution (~200 km FoV) ph/m2/ns/sr 2000 1000 500 From Tatiana Universitetsky Satellite. aand b = large cities Performances of the EUSO-Balloon

  4. Baby vs. Tatiana and the EUSO-Balloon • The Baby (Balloon) Experiment had a reduced field of view with respect to Tatiana  stronger contrast, fluctuations Balloon trajectory O.Catalano et al., NIMA 480 (2002) 547 • EUSO-Balloon: • willhavefinerresolutionatground(~200m) • b) willimplement a control on background variationsto keep a stable trigger rate (~7 Hz) Performances of the EUSO-Balloon

  5. Background simulation • An exampleofbackgroundobservation • 250 photons / m^2 nssr • Uniform distribution • Simulatedatelectronicslevel The EUSO Simulation and Anlaysis Framework has been used for the simulation Performances of the EUSO-Balloon

  6. Testingswitches • The logic of switchesof EUSO-Balloon will be tested to verify: • Capability of protecting the detector from brightevents • Measuretheir light curve and intensity WITH SWITCHES 250 pC Performances of the EUSO-Balloon

  7. The observation principle of JEM-EUSO duration ~ 50 – 150 ms Simulation of the light profile observed at the entrance pupil (above) and throught the instrument using the ESAF code 7 Performances of the EUSO-Balloon

  8. EUSO-BALLOON vs. JEM-EUSO Maximize performance of EUSO-Balloon keepingparametersascloseaspossible to JEM-EUSO Performances of the EUSO-Balloon

  9. Simulations BalloonConfiguration modified „AlcalaConfig“, thatismodified JEM-EUSO • ISS altitude 400 km  40 km • New focalsurfaceparametrization • 3. New pixel angle map • 5. New opticalsystem • 6. Changed FOV: 2*30°  12*12° • 7. Background estimation ~ 50% of JEM-EUSO 9 Performances of the EUSO-Balloon

  10. ExampleShower: 1e19 eV, Theta=20° 10 Performances of the EUSO-Balloon

  11. Example Signal Track • Proton • 1e19 eV • Theta= 20° • Phi= 135° 11 Performances of the EUSO-Balloon

  12. Example Signal Track • Proton • 1e18 eV • Theta= 30° • Phi=120° • Proton • 1e19 eV • Theta= 30° • Phi=120° 12 Performances of the EUSO-Balloon

  13. phe/GTU So called: “Saitama” code Typicaleventobservable by EUSO-Balloon: other code Proton: E = 4·1018eV q = 57.5 f= 188.7 X0 = 9.3 km Y0 = 3.1 km Ypix Xpix Time(GTU) Time(GTU) phe/GTU Ypix Eventlandingoutside the FoV Time(GTU) Xpix 13

  14. Angular Resolution Testingmode: „Debugmode“  a priori knoweldhgeofthetrack Performances of the EUSO-Balloon 14

  15. Trigger Efficiency EUSO-B. & <B>=1.4 phe/pix/GTU EUSO-B. & <B> =2.8 phe/pix/GTU 7 Hz/PDM ● 80 Hz fake trig. o 7 Hz faketrig. Integrated N. Events [1018,E]eV in 10h Trigger efficiency (%) Efficiency=1 & 1.5 x Aug. flux Efficiency=1 & Auger flux EB & A.fl. & <B>=1.4 phe EB & 1.5xA.fl. & <B>=1.4 phe EB & A.fl. & <B> =2.8 phe Energy(eV) Energy(eV) LEFT PLOT: Trigger efficiency curve for events with impact point inside FoV. RIGHT PLOT: Black, red and bluecurvesgivepreliminaryresults on the performance from a 10 h durationflightfor differentassumptions of background and cosmicrayflux. Performances of the EUSO-Balloon

  16. Conclusions • EUSO-Balloowill IMAGE the UV sky background (star light, airglow, TLEs, artificial lights) in the bandwidth used by the JEMEUSO mission observational technique. • All key components and the relative sub-assembly items will be tested according to the configuration foreseen for the JEM-EUSO mission: in particular the trigger scheme and its capability to cope with the variable sky conditions (EXTREMELY IMPORTANT). • Simulationstudieshavebeenperformed: to understand the structure of the expectedsignal and the effectiveenergythreshold of EUSO-Balloon and itspossibility to detectshowers. Resultsconfirm the capability of the instrument of detectingprimarycosmicrays of energy E>1018eV. • Due to the lowcosmicrayflux the detection of a couple of eventswillrequirefewdaysexposuretime  thereforethe detection of the first air shower from the edge of the spacewillmostprobablyrequire more thanoneflight. 16 Performances of the EUSO-Balloon

More Related