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Богомолов, А. В.; Denisov, Yu. I.; Kuznetsov, S. N.; Lisin, D. V.; Logachev, Yu. I.; Morozov, O. V.; Myagkova, I. N.; Свертилов, С. И.; Zhitnik, I. A.; Ignat'ev, A. P.; Oparin, S. N.; Pertsov, A. A.; Stepanov, A. I.; Tindo, I. P.

doi:10.1023/a:1023332408371

Cited by 14 publications

(5 citation statements)

References 7 publications

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“…The instrument is expected to provide an MDP level of 2 − 3 % for a 50 mCrab source in 10 6 s of exposure. SPR-N (Bogomolov et al, 2003) on board solar mission CORONAS-F exploits Rayleigh scattering on a 5 cm thick and 50 cm 2 collecting area Beryllium packed inside a hexahedral prism with 3 pairs of scintillation detectors surrounding the scatterer. Because of the use of scintillators, SPR-N polarimeter is sensitive in 20 − 100 keV range.…”

Section: Scattering Polarimetry Configurations: Instrumentation In Ha...mentioning

confidence: 99%

“…The field of hard X-ray polarimetry has been quite active in the last 10 − 15 years which can be seen through the new developments of dedicated polarimeters like SPR-N (Bogomolov et al, 2003;Zhitnik et al, 2006), POLAR (Sun et al, 2016), PoGOLite and PoGO+ , X-Calibur (Guo et al, 2011(Guo et al, , 2013, GRAPE (Bloser et al, 2009;Mc-Connell et al, 2009), GAP (Yonetoku et al, 2006), PENGUIN-M (Dergachev et al, 2009), COSI (Yang et al, 2018;Lowell et al, 2017) and a large number of new proposals to develop hard X-ray polarimeters, e.g. COSI-2 (Tomsick et al, 2019), POLAR-2 (Kole, 2019), Daksha 1 , AMEGO (McEnery et al, 2019) etc.…”

Section: Introductionmentioning

confidence: 99%

“…They measured a polarization fraction ranging from 2 − 54 % for M and X class flares that oc-curred from Sun's center to limb. SPR-N, a dedicated Thomson polarimeter sensitive in 20 − 100 keV(Bogomolov et al, 2003), on board CORONAS-F, on the other hand reported polarization measurement for 25 M and X class flares with an upper limit of 8 − 40 %(Zhitnik et al, 2006). For one of the flares occurred on 29 th October 2003, they detected a significant polarization degree that increases from about 50 % at 20 − 40 keV energy band to more than 70 % in the 60 − 100 keV band.…”

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confidence: 99%

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Hard X-ray Polarimetry -- An overview of the method, science drivers and recent findings

Chattopadhyay

2021

Preprint

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The last decade has seen a leapfrog in the interest in X-ray polarimetry with a number of new polarization measurements in hard X-rays from AstroSat, POLAR, GAP, and PoGO+. The measurements provide some interesting insights into various astrophysical phenomena such as coronal geometry and disk-jet connection in black hole X-ray binaries, hard X-ray emission mechanism in pulsars and Gamma Ray Bursts (GRB). They also highlight an increase in polarization with energy which makes hard X-ray polarimetry extremely appealing. There is a number of confirmed hard X-ray polarimetry experiments which along with the existing instruments (AstroSat and INTEGRAL) makes this field further exciting. Polarization experiments may also see a significant progress in sensitivity with new developments in scintillator readouts, active pixel sensors, CZT detectors. In particular, the advent of hard X-ray focusing optics, will enable designing of compact focal plane polarimeters with a multifold enhancement in sensitivity. In this review, we will focus on the recent polarimetry findings, science potential of hard X-ray polarimetry along with possible improvements in the measurement techniques.

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Section: Scattering Polarimetry Configurations: Instrumentation In Ha...mentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

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confidence: 99%

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Hard X-ray Polarimetry -- An overview of the method, science drivers and recent findings

Chattopadhyay

2021

Preprint

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“…The best energy range for polarimetric observations is thus the window between 50 keV and 1 MeV. First tentative detections of the X-ray polarization of solar flares were reported by Bogomolov et al [97], Boggs et al [98], Suarez-Garcia et al [99], Zhitnik et al [100]. During a solar flare, the direction of the polarization vector relative to the magnetic field direction will depend on the pitch angle distribution of the emitting electrons and on the viewing angle.…”

Section: Solar and Stellar Hard X-ray Flaresmentioning

confidence: 99%

Scientific prospects for hard X-ray polarimetry

Krawczynski

Garson

Guo

et al. 2011

Astroparticle Physics

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X-ray polarimetry promises to give qualitatively new information about highenergy sources. Examples of interesting source classes are binary black hole systems, rotation and accretion powered neutron stars, Microquasars, Active Galactic Nuclei and Gamma-Ray Bursts. Furthermore, X-ray polarimetry affords the possibility for testing fundamental physics, e.g. to observe signatures of light bending in the strong gravitational field of a black hole, to detect third order Quantum Electrodynamic effects in the magnetosphere of Magnetars, and to perform sensitive tests of Lorentz Invariance. In this paper we discuss scientific drivers of hard (>10 keV) X-ray polarimetry emphasizing how observations in the hard band can complement observations at lower energies (0.1 -10 keV). Subsequently, we describe four different technical realizations of hard X-ray polarimeters suitable for small to medium sized space borne missions, and study their performance in the signal-dominated case based on Monte Carlo simulations. We end with confronting the instrument requirements for accomplishing the science goals with the capabilities of the four polarimeters.

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“…Thus far, there has been no systematic study of polarization in high-energy astrophysics due to the lack of sensitivity, and polarization at hard X-ray and soft gamma-ray energies, where non-thermal processes are likely to produce a high degree of polarization, is yet to be explored. We note that, on the other hand, there has been a long history of attempts to measure polarization of hard X-rays in solar flares followed by recent missions of SPR-N on CORONAS-F [8] and RHESSI [9]. See an introduction section in [9] and references therein for a review.…”

Section: Introductionmentioning

confidence: 99%

Beam test of a prototype detector array for the PoGO astronomical hard X-ray/soft gamma-ray polarimeter

Mizuno

Kamae

et al. 2005

Nuclear Instruments and Methods in Physics Research Section A:

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Polarization measurements in the X-ray and gamma-ray energy range can provide crucial information on massive compact objects such as black holes and neutron stars. The Polarized Gamma-ray Observer (PoGO) is a new balloon-borne instrument designed to measure polarization from astrophysical objects in the 30-100 keV range, under development by an international collaboration with members from United States, Japan, Sweden and France. To examine PoGO's capability, a beam test of a simplified prototype detector array was conducted at the Argonne National Laboratory Advanced Photon Source. The detector array consisted of seven plastic scintillators, and was irradiated by polarized photon beams at 60, 73, and 83 keV. The data showed a clear polarization signal, with a measured modulation factor of 0.42 ± 0.01. This was successfully reproduced at the 10% level by the computer simulation package Geant4 after modifications to its implementation of polarized Compton/Rayleigh scattering. Details of the beam test and the validation of the Geant4 simulations are presented.

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Cited by 14 publications

References 7 publications

Hard X-ray Polarimetry -- An overview of the method, science drivers and recent findings

Hard X-ray Polarimetry -- An overview of the method, science drivers and recent findings

Scientific prospects for hard X-ray polarimetry

Beam test of a prototype detector array for the PoGO astronomical hard X-ray/soft gamma-ray polarimeter

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