GRIPS - Gamma-Ray Imaging, Polarimetry and Spectroscopy

Greiner, J.; Mannheim, K.; Aharonian, F.; Ajello, M.; Balasz, L. G.; Barbiellini, G.; Bellazzini, R.; Bishop, S.; Bisnovatij-Kogan, G. S.; Boggs, Steven E.; Bykov, A. M.; DiCocco, G.; Diehl, R.; Elsässer, Dominik; Foley, S.; Fransson, Claes; Gehrels, N.; Hanlon, L.; Hartmann, D. H.; Hermsen, W.; Hillebrandt, W.; Hudec, R.; Iyudin, A. F.; José, J.; Kadler, M.; Kanbach, G.; Klamra, W.; Kiener, J.; Klose, S.; Kreykenbohm, I.; Kuiper, L.; Kylafis, N. D.; Labanti, C.; Langanke, K.; Langer, N.; Larsson, Stefan; Leibundgut, B.; Laux, U.; Longo, F.; Maeda, Keiichi; Marcinkowski, R.; Marisaldi, M.; McBreen, B.; McBreen, Sheila; Mészáros, A.; Nomoto, K.; Pearce, Mark; Pe’er, Asaf; Pian, E.; Prantzos, Nikos; Raffelt, Georg G.; Reimer, O.; Rhode, W.; Ryde, F.; Schmidt, Ch.; Silk, Joseph; Шустов, Б. М.; Strong, A. W.; Tanvir, N. R.; Thielemann, F. K.; Tibolla, O.; Tierney, D.; Trümper, J.; Варшалович, Д. А.; Wilms, J.; Wrochna, G.; Zdziarski, A. A.; Zoglauer, Andreas

doi:10.1007/s10686-011-9255-0

Cited by 55 publications

(38 citation statements)

References 42 publications

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“…The achieved spatial resolution is of order 2-3 degrees only, while spectral resolution, however, is sufficient for astrophysical detail studies from line shapes and centroid shifts for several lines and sources of interest [22]. Examples for proposed next-generation instruments [23,24] have demonstrated that about one order of magnitude improvements or more would be feasible, affordability assessment by the scientific funding communities set aside.…”

Section: Measuring Cosmic Gamma-ray Linesmentioning

confidence: 99%

About cosmic gamma ray lines

Diehl

2017

AIP Conference Proceedings

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Abstract. Gamma ray lines from cosmic sources convey the action of nuclear reactions in cosmic sites and their impacts on astrophysical objects. Gamma rays at characteristic energies result from nuclear transitions following radioactive decays or highenergy collisions with excitation of nuclei. The gamma-ray line from the annihilation of positrons at 511 keV falls into the same energy window, although of different origin. We present here the concepts of cosmic gamma ray spectrometry and the corresponding instruments and missions, followed by a discussion of recent results and the challenges and open issues for the future. Among the lessons learned are the diffuse radioactive afterglow of massive-star nucleosynthesis in 26 Al and 60 Fe gamma rays, which is now being exploited towards the cycle of matter driven by massive stars and their supernovae; large interstellar cavities and superbubbles have been recognised to be of key importance here. Also, constraints on the complex processes making stars explode as either thermonuclear or core-collapse supernovae are being illuminated by gamma-ray lines, in this case from shortlived radioactivities from 56 Ni and 44 Ti decays. In particular, the three-dimensionality and asphericities that have recently been recognised as important are enlightened in different ways through such gamma-ray line spectroscopy. Finally, the distribution of positron annihilation gamma ray emission with its puzzling bulge-dominated intensity disctribution is measured through spatially-resolved spectra, which indicate that annihilation conditions may differ in different parts of our Galaxy. But it is now understood that a variety of sources may feed positrons into the interstellar medium, and their characteristics largely get lost during slowing down and propagation of positrons before annihilation; a recent microquasar flare was caught as an opportunity to see positrons annihilate at a source.

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Section: Measuring Cosmic Gamma-ray Linesmentioning

confidence: 99%

About cosmic gamma ray lines

Diehl

2017

AIP Conference Proceedings

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“…Greiner et al 2012;Summa et al 2011), the mission with the highest sensitivities at these energies was the COMPTEL instrument aboard the CGRO satellite in the mid-nineties. One possible successor with an enhanced sensitivity of a factor 40 is the proposed GRIPS (Gamma-Ray Imaging, Polarimetry and Spectroscopy) mission (Greiner et al 2009(Greiner et al , 2012. The focus of this section is on the progress that could be made in the future concerning the detection of gamma-ray emission from SNe Ia, using the GRIPS instrument as an example.…”

Section: Detection Prospectsmentioning

confidence: 99%

“…The model of the GRM detector used in this study corresponds to the setup described in Greiner et al (2012).…”

Section: Detection Prospectsmentioning

confidence: 99%

“…In this paper, we explore the additional benefits from analyzing gamma-ray spectra towards a more sound theoretical understanding of SNe Ia and discuss the detection limits of proposed next-generation gamma-ray observatories. For this aim to be achieved, we ran full detector simulations of the proposed MeV satellite GRIPS (Greiner et al 2012).…”

Section: Introductionmentioning

confidence: 99%

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Gamma-ray diagnostics of Type Ia supernovae

Summa

Ulyanov

Kromer

et al. 2013

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Context. Although the question of progenitor systems and detailed explosion mechanisms still remains a matter of discussion, it is commonly believed that Type Ia supernovae (SNe Ia) are production sites of large amounts of radioactive nuclei. Even though the gamma-ray emission due to radioactive decays is responsible for powering the light curves of SNe Ia, gamma rays themselves are of particular interest as a diagnostic tool because they directly lead to deeper insight into the nucleosynthesis and the kinematics of these explosion events. Aims. We study the evolution of gamma-ray line and continuum emission of SNe Ia with the objective of analyzing the relevance of observations in this energy range. We seek to investigate the chances for the success of future MeV missions regarding their capabilities for constraining the intrinsic properties and the physical processes of SNe Ia. Methods. Focusing on two of the most broadly discussed SN Ia progenitor scenarios -a delayed detonation in a Chandrasekhar-mass white dwarf (WD) and a violent merger of two WDs -we used three-dimensional explosion models and performed radiative transfer simulations to obtain synthetic gamma-ray spectra. Both chosen models produce the same mass of 56 Ni and have similar optical properties that are in reasonable agreement with the recently observed supernova SN 2011fe. We examine the gamma-ray spectra with respect to their distinct features and draw connections to certain characteristics of the explosion models. Applying diagnostics, such as line and hardness ratios, the detection prospects for future gamma-ray missions with higher sensitivities in the MeV energy range are discussed. Results. In contrast to the optical regime, the gamma-ray emission of our two chosen models proves to be quite different. The almost direct connection of the emission of gamma rays to fundamental physical processes occurring in SNe Ia permits additional constraints concerning several explosion model properties that are not easily accessible within other wavelength ranges. Proposed future MeV missions such as GRIPS will resolve all spectral details only for nearby SNe Ia, but hardness ratio and light curve measurements still allow for a distinction of the two different models at 10 Mpc and 16 Mpc for an exposure time of 10 6 s. The possibility of detecting the strongest line features up to the Virgo distance will offer the opportunity to build up a first sample of SN Ia detections in the gamma-ray energy range and underlines the importance of future space observatories for MeV gamma rays.

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“…for GRIPS [12], Si + CsI(Tl) for TIGRE [13]), semiconductor pixel detectors (CIPHER [14]) and liquid xenon (LXeGRIT [15]) time projection chambers (TPC). In most Compton telescopes the reconstruction of the direction of the incident photon provides an uncertainty area which has the shape of a thin cone arc.…”

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Compton polarimetry revisited

Bernard

2015

Nuclear Instruments and Methods in Physics Research Section A:

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We compute the average polarisation asymmetry from the Klein-Nishina differential cross section on free electrons at rest. As expected from the expression for the asymmetry, the average asymmetry is found to decrease like the inverse of the incident photon energy asymptotically at high energy. We then compute a simple estimator of the polarisation fraction that makes optimal use of all the kinematic information present in an event final state, by the use of "moments" method, and we compare its statistical power to that of a simple fit of the azimuthal distribution. In contrast to polarimetry with pair creation, for which we obtained an improvement by a factor of larger than two in a previous work, here for Compton scattering the improvement is only of 10-20 %.Key words: Hard X-ray, gamma-ray, Compton scattering, polarimeter, polarisation asymmetry, optimal variable 1. Cosmic-source polarimetry: the high-energy frontier Polarimetry is a powerful diagnostic of specific phenomena at work in cosmic sources in the radio-wave and optical energy bands, but very few results are available at high photon energies: the only significant observation in the X-gamma energy range, to date, is the measurement of a linear polarisation fraction of P = 19 ± 1% of the 2.6 keV emission of the Crab nebula by a Bragg polarimeter on board . At higher energies, hard-X-ray and soft-gamma-ray telescopes that have flown to space in the past (COMPTEL

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GRIPS - Gamma-Ray Imaging, Polarimetry and Spectroscopy

Cited by 55 publications

References 42 publications

About cosmic gamma ray lines

About cosmic gamma ray lines

Gamma-ray diagnostics of Type Ia supernovae

Compton polarimetry revisited

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