Compton Large Area Silicon Timing Tracker for Cosmic Vision M3

Lebrun, F.; Aharonian, F.; Beckmann, V.; Bertoli, W.; Brom, J. M.; Bykov, A.; Brandt, S.; Bulik, T.; Budtz-Jørgensen, Carl; Caballero, I.; Cohen‐Tanugi, J.; Daigne, F.; Denis, M.; Drury, L. O’c.; Gallant, Y. A.; Gehrels, N.; Goerlach, U.; Götz, D.; Hamadache, C.; Hermsen, W.; Kiener, J.; Kuiper, L.; Lamanna, G.; Laurent, Philippe; Limousin, O.; Mattana, F.; Marcowith, A.; Neubert, Torsten; Olivetto, C.; Orleański, P.; Parizot, E.; Pinçon, Jean-Louis; Pradier, T.; Schanne, S.; Séréville, N. de; Soldi, S.; Renaud, M.; Tagger, M.; Tatischeff, V.; Terrier, R.; Walter, R.; Watanabe, S.; Heras, J. A. Zurita

doi:10.22323/1.115.0034

Cited by 6 publications

(6 citation statements)

References 3 publications

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“…Using a series of silicon wafer active targets placed at a distance of each other, at the same time the material in which the photon converts and in which the tracks are tracked, enables an improvement of ≈ a factor of three in the angular resolution at 100 MeV with respect to the LAT [2][3][4][5][6][7][8][9] at the cost of a lower average active target density. Similar values of the angular resolution are achieved using a high-spatial-resolution, homogeneous, high-density material such as an emulsion [10].…”

Section: γ-Ray Astronomymentioning

confidence: 99%

Charged particle tracking without magnetic field: Optimal measurement of track momentum by a Bayesian analysis of the multiple measurements of deflections due to multiple scattering

Frosini

Bernard

2017

Nuclear Instruments and Methods in Physics Research Section A:

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Section: γ-Ray Astronomymentioning

confidence: 99%

Charged particle tracking without magnetic field: Optimal measurement of track momentum by a Bayesian analysis of the multiple measurements of deflections due to multiple scattering

Frosini

Bernard

2017

Nuclear Instruments and Methods in Physics Research Section A:

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“…For thick wafers (≈ 500 µm [47,48,49,50,51,52]), the effective polarization asymmetry, and therefore the dilution factor, are still low because multiple scattering remains an issue. It's only if very thin wafers can be made, held and launched (≈ 150 µm [53]) that there is some hope of a sizeable sensitivity to polarization (see Figs.…”

Section: γ-Ray Polarimetry With Pairs: Techniquesmentioning

confidence: 99%

γ-Ray polarimetry with conversions to e+e− pairs: Polarization asymmetry and the way to measure it

Gros

Bernard

2017

Astroparticle Physics

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We revisit the measurement of the polarization fraction, P , and the measurement of the polarization angle of partially linearly-polarized gamma rays using their conversion to e + e − pairs in the field of a nucleus. We show that an inappropriate definition of the azimuthal angle, ϕ, used to reference the orientation of the final state degrades the precision of the measurement of P , by comparison to the optimal case where the bisector angle of the electron and of the positron momenta is used. We then focus on the lowest part of the energy spectrum, below ≈ 10 MeV, where a large part of the statistics lie for a cosmic source. We obtain the value of the polarization asymmetry, A, of pair conversion at threshold and we show that in the case where the correct expression is used for ϕ, the measured value of A tends to the limit.

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“…A significant advance in sensitivity is needed to not depend only on luck with sufficiently nearby events, to below 10 −6 ph cm −2 s −1 as shown in several proposed mission concepts (see ESA's Cosmic-Vision program selection, e.g. [39,137,72]). …”

Section: Supernovae Of Type Iamentioning

confidence: 99%

Cosmic Gamma-Ray Spectroscopy

Diehl

2013

Astronomical Review

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Penetrating gamma-rays require complex instrumentation for astronomical spectroscopy measurements of gamma-rays from cosmic sources. Multiple-interaction detectors in space combined with sophisticated postprocessing of detector events on ground have lead to a spectroscopy performance which is now capable to provide new astrophysical insights. Spectral signatures in the MeV regime originate from transitions in the nuclei of atoms (rather than in their electron shell). Nuclear transitions are stimulated by either radioactive decays or high-energy nuclear collisions such as with cosmic rays. Gamma-ray lines have been detected from radioactive isotopes produced in nuclear burning inside stars and supernovae, and from energetic-particle interactions in solar flares. Radioactive-decay gamma-rays from 56 Ni directly reflect the source of supernova light. 44 Ti is produced in core-collapse supernova interiors, and the paucity of corresponding 44 Ti gamma-ray line sources reflects the variety of dynamical conditions herein. 26 Al and 60 Fe are dispersed in interstellar space from massive-star nucleosynthesis over millions of years. Gamma-rays from their decay are measured in detail by gamma-ray telescopes, astrophysical interpretations reach from massive-star interiors to dynamical processes in the interstellar medium. Nuclear de-excitation gamma-ray lines have been found in solar-flare events, and convey information about energetic-particle production in these events, and their interaction in the solar atmosphere. The annihilation of positrons leads to another type of cosmic gamma-ray source. The characteristic annihilation gamma-rays at 511 keV have been measured long ago in solar flares, and now throughout the interstellar medium of our Milky Way galaxy. But now a puzzle has appeared, as a surprising predominance of the central bulge region was determined. This requires either new positron sources or transport processes not yet known to us. In this paper we discuss instrumentation and data processing for cosmic gamma-ray spectroscopy, and the astrophysical issues and insights from these measurements.

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Compton Large Area Silicon Timing Tracker for Cosmic Vision M3

Cited by 6 publications

References 3 publications

Charged particle tracking without magnetic field: Optimal measurement of track momentum by a Bayesian analysis of the multiple measurements of deflections due to multiple scattering

Charged particle tracking without magnetic field: Optimal measurement of track momentum by a Bayesian analysis of the multiple measurements of deflections due to multiple scattering

γ-Ray polarimetry with conversions to e+e− pairs: Polarization asymmetry and the way to measure it

Cosmic Gamma-Ray Spectroscopy

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