The SuperTiger-1 instrument and its long-duration Antarctic balloon - - PowerPoint PPT Presentation

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The SuperTiger-1 instrument and its long-duration Antarctic balloon - - PowerPoint PPT Presentation

Nov 02, 2022 257 likes •412 views

The SuperTiger-1 instrument and its long-duration Antarctic balloon flight J.T. LINK 2,6 , W.R. BINNS 1 , R.G. BOSE 1 , D.L. BRAUN 1 , T.J. BRANT 2 , W.M. DANIELS 2 , P.F. DOWKONTT 1 , S.P. FITZSIMMONS 2 , D.J. HAHNE 2 , T. HAMS 2,6 , M.H. ISRAEL 1

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SLIDE 1

The SuperTiger-1 instrument and its long-duration Antarctic balloon flight

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J.T. LINK2,6, W.R. BINNS1, R.G. BOSE1, D.L. BRAUN1, T.J. BRANT2, W.M. DANIELS2, P.F. DOWKONTT1, S.P. FITZSIMMONS2, D.J. HAHNE2, T. HAMS2,6, M.H. ISRAEL1, J. KLEMIC3, A.W. LABRADOR3, R.A. MEWALDT3, J.W. MITCHELL2, P. MOORE1, R.P. MURPHY1, M.A. OLEVITCH1, B.F. RAUCH1, K. SAKAI2,6, F. SAN SEBASTIAN2, M. SASAKI2,6, G.E. SIMBURGER1, E.C. STONE3, C.J. WADDINGTON4, N.E. WALSH1, J.E. WARD1, M.E. WIEDENBECK5

  • 1. Washington University in St. Louis, St. Louis, MO 63130 USA
  • 2. NASA/Goddard Space Flight Center, Greenbelt, MD 2077 USA
  • 3. California Institute of Technology, Pasadena, CA 91125 USA
  • 4. University of Minnesota, Minneapolis, MN 55455 USA
  • 5. Jet Propulsion Laboratory, California Institute of Technology, Pasadena,

CA 91109

  • 6. Center for Research in Space Sciences and Technology, Greenbelt, MD 20771 USA
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SLIDE 2

What can Ultra-Heavy GCRs Tell Us

  • How are GCRs accelerated?
  • What are the source materials

for the GCR nuclei?

Henize 70 Superbubble in the LMC (FORS/VLT Telescopes, ESO) Nebula surrounding Wolf Rayet Star WR124 in Saggetarius

  • constellation. (Hubble Wide

Field Planetary Camera 2)

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  • Ultra-Heavy nuclei (those with a Z >30) are produced by the s- and

r-processes in stars and supernova explosions. These nuclei are then accelerated to cosmic-ray energies most likely by supernova explosions in OB associations.

  • Recent work suggests that an additional source of ultra-heavy

nuclei may be needed for particles above ~Z=54. Binary neutron star mergers are one possibility.

  • These particles are excellent probes of the material source

and acceleration process of cosmic-rays.

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SLIDE 3

Elemental Abundances in the Galactic Cosmic Radiation

♦Elements in the upper 2/3rds of the periodic table, are extremely rare compared to lighter elements. ♦Measurement requires large instruments at the top of the atmosphere for long exposure times.

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SLIDE 4

SuperTIGER Instrument

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Hodo_top Scintillator 1 Aerogel Cherenkov Acrylic Cherenkov Scintillator 2 Scintillator 3

  • Stack of 7 detectors

– 3 Scintillation counters – 2 Scintillating Fiber Hodoscopes – 2 Cherenkov Detectors

  • Aerogel, n =1.043 or 1.025 (2.5 or 3.3

GeV/nucleon)

  • Acrylic, n = 1.49 (0.3 GeV/nucleon)
  • Two nearly identical modules
  • Effective area 2.9 m2sr, 7.2 times that of

TIGER.

  • See instrument paper: Binns et al. ApJ (2014)

788:18 Hodo_bottom

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SLIDE 5

Super-TIGER Detectors

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SLIDE 6

SuperTIGER-1 Instrument

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SLIDE 7

SuperTIGER-1 Balloon Flight and Recovery

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  • December 8, 2012-February 1, 2013
  • 55 day flight--(NASA Heavy-Lift Scientific

Balloon Record!)

  • Collected 4.7 x 106 iron events
  • Detectors and electronics completely

recovered in 2014-2015 season. Team

  • f 4 camped for 31 days at landing site.
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SLIDE 8

Data Analysis Technique

High Energies: Acrylic C vs Aerogel C Low Energies: Scintillator vs Acrylic C Energy> 800 MeV/nuc at top of atmosphere

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SLIDE 9

Data Analysis Technique

Low Energy Branch

High Energy Branch High Energies: Acrylic C vs Aerogel C Low Energies: Scintillator vs Acrylic C Energy> 800 MeV/nuc at top of atmosphere

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SLIDE 10

Resolution for Z≤30

Low Energy (below C0) High Energy (above C0) Combined

Fe Co Ni Cu Zn Ca

Si S

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SLIDE 11

HEAO 3 Heavy Nuclei Experiment Data 30 < Z < 62

Source: Binns et. al. Astrophysical Journal , 346, 1989

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SLIDE 12

Charge histogram for 30≤Z≤40 nuclei

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Abundances of 30 ≤ Z ≤ 40. We get well-defined charge peaks

for every element from Z= 30 to 40 (Bin size 0.125 cu).

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SuperTIGER-II Improvements

  • SuperTIGER selected for a second flight in 2017-2018

Antarctic season.

  • Instrument currently in Palestine Texas for final integration
  • Improvements over SuperTIGER-1

– Additional storage and disk drive redundancy – Will use open port iridium in addition to TDRSS telemetry which will give us complete high-priority data coverage for entire flight – Improved scintillator PMT/WLSB mounting scheme to address damage to PMTs most likely caused when we wintered over on the ice. – Redesigned HV power supplies and testing procedures to address the issues we saw with a small number of supplies in ST-1 Flight

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SLIDE 14

Summary

  • The first flight of SuperTIGER in 2012-2013 was

highly successful

–55 day flight duration (44 days equivalent data due to telemetry outages) –Paper on elemental abundances published (ApJ 831:148, 2016)

  • SuperTIGER-II flying December, 2017
  • Future flights of SuperTIGER a possibility as are

space missions on ISS (TIGERISS) or free flying sattelites (HNX).

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SLIDE 15

SuperTIGER Related Presentations at this conference

  • CRD105 (Alan Labrador) Galactic Cosmic Ray

Energy Spectra for Ne through Cu from 0.8 to 10 GeV/nuc with the SuperTIGER instrument

  • CRD047 (Nathan Walsh) Preliminary

SuperTIGER Abundances of Galactic Cosmic Rays for the Charge Interval Z=41-56 and Prospects For SuperTIGER-II

  • CRD138 (John Krizmanic) Ultra-Heavy GCR

Measurements Beyond SuperTIGER: HNX and TIGERISS