Possibilities for AMS experiments at ATLAS

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Possibilities for AMS experiments at ATLAS

• Philippe Collon, University of Notre Dame

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Present status of AMS experiments at ATLAS

• A number of AMS experiments have been performed
  at ATLAS
• Environmental science (39Ar, 81Kr, )
• Stellar nucleosynthesis (59Ni, 62Ni(n,g)63Ni,
  146Sm, 182Hf,)
• WIMP dark matter detector development (39Ar)
• AMS relies on a number of factors
• Good isobaric separation
• Stability of the entire system
• High overall transmission

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146Sm t1/2 measurement using AMS
146Sm-146Nd separation
146Sm22/146Nd22 840 MeV
146Sm/147Sm 10-12
Detection of live 146Sm in meteorites may also be
an interesting capability
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High sensitivity 59Ni AMS using full stripping
59Ni-59Co separation ECR 59Ni16 (3) 630
MeV 1mg/cm2 C stripper foil 10 fully
stripped
Natural production of 59Ni (t1/2 76 kyr) occurs
by interaction of cosmic-ray particles with
matter. This production is signficant only in
extraterrestrial matter and concentrations of the
order of 59Ni/Ni 10-11 10-12 have been
measured in iron meteorites by AMS
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List of commonly classified p-nuclides
Nucleus abundance Nucleus abundance nucleus abundance
74Se 0.55 114Sn 0.0252 156Dy 0.000221
78Kr 0.153 115Sn 0.0129 158Dy 0.000378
84Sr 0.132 120Te 0.0043 162Er 0.000351
92Mo 0.378 124Xe 0.00571 164Er 0.00404
94Mo 0.236 126Xe 0.00509 168Yb 0.000322
96Ru 0.103 130Ba 0.00476 174Hf 0.000249
98Ru 0.035 132Ba 0.00453 180Ta 2.4e-06
102Pd 0.0142 138La 0.000409 180W 0.000173
106Cd 0.0201 136Ce 0.00216 184Os 0.000122
108Cd 0.0143 138Ce 0.00284 190Pt 0.00017
113In 0.0079 144Sm 0.008 196Hg 0.00048
112Sn 0.0372 152Gd 0.00066 -------- ----------
Stellar production rates can be studied using the
inverse (a, g) reactions followed by AMS counting
of produced nuclei
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Short-lived cosmogenic radionuclides
A Isotope D t1/2 (years) Mass
10 10Be 12606.6 1.51E06 10.01353
26 26Al -12210.3 7.39E05 25.98689
36 36Cl -29521.9 3.00E05 35.96831
41 41Ca -35137.5 1.03E05 40.96228
53 53Mn -54683.6 3.73E06 52.9413
60 60Fe -61407 1.50E06 59.93408
79 79Se -75916.9 6.46E05 78.9185
81 81Kr -77693.6 2.29E05 80.91659
93 93Zr -87117.4 1.53E06 92.90648
97 97Tc -87221 2.60E06 96.90637
98 98Tc -86428 4.19E06 97.90722
99 99Tc -87323.3 2.11E05 98.90626
126 126Sn -86020 2.07E05 125.9077
135 135Cs -87587 2.30E06 134.906
146 146Sm -81002 1.0308 145.9234
150 150Gd -75772 1.79E06 149.9187
154 154Dy -70400 2.99E06 153.9244
182 182Hf -46059 9.00E06 181.9632
208 208Bi -18884 3.67E05 207.9797
210 210Bim -14535 3.03E06 209.9844
233 233U 36913.4 1.59E05 233.0396
234 234U 38140.6 2.45E05 234.0409
236 236Np 43370 1.54E05 236.0466
237 237Np 44867.5 2.14E06 237.0482
242 242Pu 54713 3.73E05 242.0587
248 248Cm 67386 3.39E05 248.0723
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AMS possibilities with the upgraded facility

• A number of the radionuclides can be detected
  using smaller accelerators however a large number
  of very exciting nuclides will benefit from an
  ATLAS upgrade
• Higher beam currents
• Reduce count times (less stability requirements)
• Allow access to lower reaction cross sections
• Improve sensitivity
• Higher beam energies (? improved isobaric
  separation)
• Improved separation for gas-filled magnet
  techniques
• Higher full-stripping probabilities

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182Hf as an supernova indicator
182Hf is a r-process radionuclides with a rapid
s-process component in massive stars. During
supervovae events it can be injected into the
interstellar medium t1/2 9x109 years Its
signal should be detectable in geological
material Needs separation from 182W
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Possible needs for upcoming AMS experiments at
ATLAS

• Possibility of clean ion sources with the
  development of plasma chamber liner (Quartz)
  and/or the development of a dedicated quartz
  lined ECR source
• Development of a new detector that can
  accommodate higher count rates
• Improved continuous beam monitoring (both for
  transmission and primary beam intensity)
• Further development of calibrated beam
  attenuation (tested during recent 146Sm
  experiments)
• ..