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Pearce, M., Eliasson, L., Iyer, N., Kiss, M., Kushwah, R., Larsson, J., . . . Xie, E. (2019). Science prospects for SPHiNX - A small satellite GRB polarimetry mission. Astroparticle physics, 104, 54-63
Open this publication in new window or tab >>Science prospects for SPHiNX - A small satellite GRB polarimetry mission
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2019 (English)In: Astroparticle physics, ISSN 0927-6505, E-ISSN 1873-2852, Vol. 104, p. 54-63Article in journal (Refereed) Published
Abstract [en]

Gamma-ray bursts (GRBs) are exceptionally bright electromagnetic events occurring daily on the sky. The prompt emission is dominated by X-/gamma-rays. Since their discovery over 50 years ago, GRBs are primarily studied through spectral and temporal measurements. The properties of the emission jets and underlying processes are not well understood. A promising way forward is the development of missions capable of characterising the linear polarisation of the high-energy emission. For this reason, the SPHiNX mission has been developed for a small-satellite platform. The polarisation properties of incident high-energy radiation (50-600 keV) are determined by reconstructing Compton scattering interactions in a segmented array of plastic and Gd3Al2Ga3O12(Ce) (GAGG(Ce)) scintillators. During a two-year mission, similar to 200 GRBs will be observed, with similar to 50 yielding measurements where the polarisation fraction is determined with a relative error <= 10%. This is a significant improvement compared to contemporary missions. This performance, combined with the ability to reconstruct GRB localisation and spectral properties, will allow discrimination between leading classes of emission models. 

Place, publisher, year, edition, pages
ELSEVIER SCIENCE BV, 2019
Keywords
Polarimetry, X-ray, Gamma-ray burst, Small satellite
National Category
Physical Sciences
Identifiers
urn:nbn:se:kth:diva-238522 (URN)10.1016/j.astropartphys.2018.08.007 (DOI)000447479300004 ()
Funder
Swedish National Space Board, 232/16
Note

QC 20181106

Available from: 2018-11-06 Created: 2018-11-06 Last updated: 2018-11-06Bibliographically approved
Pearce, M., Eliasson, L., Iyer, N., Kiss, M., Kushwah, R., Larsson, J., . . . Xie, F. (2019). Science prospects for SPHiNX – A small satellite GRB polarimetry mission. Astroparticle physics, 104, 54-63
Open this publication in new window or tab >>Science prospects for SPHiNX – A small satellite GRB polarimetry mission
Show others...
2019 (English)In: Astroparticle physics, ISSN 0927-6505, E-ISSN 1873-2852, Vol. 104, p. 54-63Article in journal (Refereed) Published
Abstract [en]

Gamma-ray bursts (GRBs) are exceptionally bright electromagnetic events occurring daily on the sky. The prompt emission is dominated by X-/γ-rays. Since their discovery over 50 years ago, GRBs are primarily studied through spectral and temporal measurements. The properties of the emission jets and underlying processes are not well understood. A promising way forward is the development of missions capable of characterising the linear polarisation of the high-energy emission. For this reason, the SPHiNX mission has been developed for a small-satellite platform. The polarisation properties of incident high-energy radiation (50–600 keV) are determined by reconstructing Compton scattering interactions in a segmented array of plastic and Gd3Al2Ga3O12(Ce) (GAGG(Ce)) scintillators. During a two-year mission, ∼ 200 GRBs will be observed, with ∼ 50 yielding measurements where the polarisation fraction is determined with a relative error ≤ 10%. This is a significant improvement compared to contemporary missions. This performance, combined with the ability to reconstruct GRB localisation and spectral properties, will allow discrimination between leading classes of emission models.

Place, publisher, year, edition, pages
Elsevier, 2019
Keywords
Gamma-ray burst, Polarimetry, Small satellite, X-ray, Ellipsometry, Polarimeters, Polarization, Satellites, Stars, X rays, Gamma ray bursts, Gamma-ray bursts (GRBs), High energy emission, High energy radiation, Linear polarisation, Scattering interactions, Small-satellite, Temporal measurements, Gamma rays
National Category
Physical Sciences
Identifiers
urn:nbn:se:kth:diva-236345 (URN)10.1016/j.astropartphys.2018.08.007 (DOI)2-s2.0-85052499332 (Scopus ID)
Funder
Swedish National Space Board, 232/16
Note

QC 20181108

Available from: 2018-11-08 Created: 2018-11-08 Last updated: 2018-11-08Bibliographically approved
Li, L., Wu, X.-F., Lei, W.-H., Dai, Z.-G., Lian, E.-W. & Ryde, F. (2018). Constraining the Type of Central Engine of GRBs with Swift Data. Astrophysical Journal Supplement Series, 236(2), Article ID 26.
Open this publication in new window or tab >>Constraining the Type of Central Engine of GRBs with Swift Data
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2018 (English)In: Astrophysical Journal Supplement Series, ISSN 0067-0049, E-ISSN 1538-4365, Vol. 236, no 2, article id 26Article in journal (Refereed) Published
Abstract [en]

The central engine of gamma-ray bursts (GRBs) is poorly constrained. There exist two main candidates: a fast-rotating black hole and a rapidly spinning magnetar. Furthermore, X-ray plateaus are widely accepted to be the energy injection into the external shock. In this paper, we systematically analyze the Swift/XRT light curves of 101 GRBs having plateau phases and known redshifts (before 2017 May). Since a maximum energy budget (similar to 2 x 10(52) erg) exists for magnetars but not for black holes, this provides a good clue to identifying the type of GRB central engine. We calculate the isotropic kinetic energy E-K,(iso) and the isotropic X-ray energy release E-X,E-iso for individual GRBs. We identify three categories based on how likely a black hole harbors a central engine: "Gold" (9 out of 101; both E-X,E-iso and E-K,E-iso exceed the energy budget), "Silver" (69 out of 101; E-X,E-iso less than the limit but E-K,E-iso greater than the limit), and "Bronze" (23 out of 101; the energies are not above the limit). We then derive and test the black hole parameters with the Blandford-Znajek mechanism, and find that the observations of the black hole candidate ("Gold" + "Silver") samples are consistent with the expectations of the black hole model. Furthermore, we also test the magnetar candidate ("Bronze") sample with the magnetar model, and find that the magnetar surface magnetic field (B-p) and initial spin period (P-0) fall into reasonable ranges. Our analysis indicates that if the magnetar wind is isotropic, a magnetar central engine is possible for 20% of the analyzed GRBs. For most GRBs, a black hole is most likely operating.

Place, publisher, year, edition, pages
IOP PUBLISHING LTD, 2018
Keywords
methods: statistical, reference systems, X-rays: ISM
National Category
Astronomy, Astrophysics and Cosmology
Identifiers
urn:nbn:se:kth:diva-230421 (URN)10.3847/1538-4365/aabaf3 (DOI)000432546100002 ()
Note

QC 20180619

Available from: 2018-06-19 Created: 2018-06-19 Last updated: 2018-06-19Bibliographically approved
Li, L., Wu, X.-F., Lei, W.-H., Dai, Z.-G., Lian, E.-W. & Ryde, F. (2018). Constraining the Type of Central Engine of GRBs with Swift Data. Astrophysical Journal Supplement Series, 236(2), Article ID 26.
Open this publication in new window or tab >>Constraining the Type of Central Engine of GRBs with Swift Data
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2018 (English)In: Astrophysical Journal Supplement Series, ISSN 0067-0049, E-ISSN 1538-4365, Vol. 236, no 2, article id 26Article in journal (Refereed) Published
Abstract [en]

The central engine of gamma-ray bursts (GRBs) is poorly constrained. There exist two main candidates: a fast-rotating black hole and a rapidly spinning magnetar. Furthermore, X-ray plateaus are widely accepted to be the energy injection into the external shock. In this paper, we systematically analyze the Swift/XRT light curves of 101 GRBs having plateau phases and known redshifts (before 2017 May). Since a maximum energy budget (similar to 2 x 10(52) erg) exists for magnetars but not for black holes, this provides a good clue to identifying the type of GRB central engine. We calculate the isotropic kinetic energy E-K,(iso) and the isotropic X-ray energy release E-X,E-iso for individual GRBs. We identify three categories based on how likely a black hole harbors a central engine: "Gold" (9 out of 101; both E-X,E-iso and E-K,E-iso exceed the energy budget), "Silver" (69 out of 101; E-X,E-iso less than the limit but E-K,E-iso greater than the limit), and "Bronze" (23 out of 101; the energies are not above the limit). We then derive and test the black hole parameters with the Blandford-Znajek mechanism, and find that the observations of the black hole candidate ("Gold" + "Silver") samples are consistent with the expectations of the black hole model. Furthermore, we also test the magnetar candidate ("Bronze") sample with the magnetar model, and find that the magnetar surface magnetic field (B-p) and initial spin period (P-0) fall into reasonable ranges. Our analysis indicates that if the magnetar wind is isotropic, a magnetar central engine is possible for 20% of the analyzed GRBs. For most GRBs, a black hole is most likely operating.

Place, publisher, year, edition, pages
Institute of Physics (IOP), 2018
Keywords
methods: statistical, reference systems, X-rays: ISM
National Category
Physical Sciences
Identifiers
urn:nbn:se:kth:diva-230489 (URN)10.3847/1538-4365/aabaf3 (DOI)000432546100002 ()2-s2.0-85051213360 (Scopus ID)
Note

QC 20180614

Available from: 2018-06-14 Created: 2018-06-14 Last updated: 2018-10-16Bibliographically approved
Ajello, M., Allafort, A., Axelsson, M., Baldini, L., Barbiellini, G., Baring, M. G., . . . Zaharijas, G. (2018). Fermi-LAT Observations of LIGO/Virgo Event GW170817. Astrophysical Journal, 861(2), Article ID 88.
Open this publication in new window or tab >>Fermi-LAT Observations of LIGO/Virgo Event GW170817
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2018 (English)In: Astrophysical Journal, ISSN 0004-637X, E-ISSN 1538-4357, Vol. 861, no 2, article id 88Article in journal (Refereed) Published
Abstract [en]

We present the Fermi Large Area Telescope (LAT) observations of the binary neutron star merger event GW170817 and the associated short gamma-ray burst (SGRB) GRB 170817A detected by the Fermi Gamma-ray Burst Monitor. The LAT was entering the South Atlantic Anomaly at the time of the LIGO/Virgo trigger (t(GW)) and therefore cannot place constraints on the existence of high-energy (E > 100 MeV) emission associated with the moment of binary coalescence. We focus instead on constraining high-energy emission on longer timescales. No candidate electromagnetic counterpart was detected by the LAT on timescales of minutes, hours, or days after the LIGO/Virgo detection. The resulting flux upper bound (at 95% C. L.) from the LAT is 4.5. x. 10(-10) erg cm(-2) s(-1) in the 0.1-1 GeV range covering a period from tGW. +. 1153 s to t(GW). +. 2027 s. At the distance of GRB 170817A, this flux upper bound corresponds to a luminosity upper bound of 9.7. x. 10(43) erg s(-1), which is five orders of magnitude less luminous than the only other LAT SGRB with known redshift, GRB 090510. We also discuss the prospects for LAT detection of electromagnetic counterparts to future gravitational-wave events from Advanced LIGO/Virgo in the context of GW170817/GRB 170817A.

Place, publisher, year, edition, pages
Institute of Physics (IOP), 2018
Keywords
gamma-ray burst: general, gamma rays: general, gravitational waves
National Category
Physical Sciences
Identifiers
urn:nbn:se:kth:diva-232611 (URN)10.3847/1538-4357/aac515 (DOI)000437822700010 ()2-s2.0-85050685077 (Scopus ID)
Note

QC 20180801

Available from: 2018-08-01 Created: 2018-08-01 Last updated: 2018-10-16Bibliographically approved
Amati, L., O'Brien, P., Gotz, D., Bozzo, E., Tenzer, C., Frontera, F., . . . Zicha, J. (2018). The THESEUS space mission concept: science case, design and expected performances. Advances in Space Research, 62(1), 191-244
Open this publication in new window or tab >>The THESEUS space mission concept: science case, design and expected performances
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2018 (English)In: Advances in Space Research, ISSN 0273-1177, E-ISSN 1879-1948, Vol. 62, no 1, p. 191-244Article in journal (Refereed) Published
Abstract [en]

THESEUS is a space mission concept aimed at exploiting Gamma-Ray Bursts for investigating the early Universe and at providing a substantial advancement of multi-messenger and time-domain astrophysics. These goals will be achieved through a unique combination of instruments allowing GRB and X-ray transient detection over a broad field of view (more than 1 sr) with 0.5-1 arcmin localization, an energy band extending from several MeV down to 0.3 keV and high sensitivity to transient sources in the soft X-ray domain, as well as on-board prompt (few minutes) follow-up with a 0.7 m class IR telescope with both imaging and spectroscopic capabilities. THESEUS will be perfectly suited for addressing the main open issues in cosmology such as, e.g., star formation rate and metallicity evolution of the inter-stellar and intra-galactic medium up to redshift similar to 10, signatures of Pop III stars, sources and physics of re-ionization, and the faint end of the galaxy luminosity function. In addition, it will provide unprecedented capability to monitor the X-ray variable sky, thus detecting, localizing, and identifying the electromagnetic counterparts to sources of gravitational radiation, which may be routinely detected in the late '20s/early '30s by next generation facilities like aLIGO/ aVirgo, eLISA, KAGRA, and Einstein Telescope. THESEUS will also provide powerful synergies with the next generation of multi-wavelength observatories (e.g., LSST, ELT, SKA, CTA, ATHENA).

Place, publisher, year, edition, pages
ELSEVIER SCI LTD, 2018
Keywords
Gamma-ray: bursts, Cosmology: observations, Dark ages, Re-ionization, First stars
National Category
Astronomy, Astrophysics and Cosmology
Identifiers
urn:nbn:se:kth:diva-232234 (URN)10.1016/j.asr.2018.03.010 (DOI)000436889000016 ()2-s2.0-85046789580 (Scopus ID)
Note

QC 20180718

Available from: 2018-07-18 Created: 2018-07-18 Last updated: 2018-07-18Bibliographically approved
Pe'er, A. & Ryde, F. (2017). Photospheric emission in gamma-ray bursts. International Journal of Modern Physics D, 26(10), Article ID 1730018.
Open this publication in new window or tab >>Photospheric emission in gamma-ray bursts
2017 (English)In: International Journal of Modern Physics D, ISSN 0218-2718, Vol. 26, no 10, article id 1730018Article, review/survey (Refereed) Published
Abstract [en]

A major breakthrough in our understanding of gamma-ray bursts (GRB) prompt emission physics occurred in the last few years, with the realization that a thermal component accompanies the over-all nonthermal prompt spectra. This thermal part is important by itself, as it provides direct probe of the physics in the innermost outflow regions. It further has an indirect importance, as a source of seed photons for inverse-Compton scattering, thereby it contributes to the nonthermal part as well. In this short review, we highlight some key recent developments. Observationally, although so far it was clearly identified only in a minority of bursts, there is indirect evidence that a thermal component exists in a very large fraction of GRBs, possibly close to 100%. Theoretically, the existence of a thermal component has a large number of implications as a probe of underlying GRB physics. Some surprising implications include its use as a probe of the jet dynamics, geometry and magnetization.

Place, publisher, year, edition, pages
WORLD SCIENTIFIC PUBL CO PTE LTD, 2017
Keywords
Gamma-rays bursts, hydrodynamics, radiation mechanism: nonthermal, radiation mechanism: thermal
National Category
Physical Sciences
Identifiers
urn:nbn:se:kth:diva-214321 (URN)10.1142/S021827181730018X (DOI)000407996000001 ()2-s2.0-85017454452 (Scopus ID)
Note

QC 20170918

Available from: 2017-09-18 Created: 2017-09-18 Last updated: 2017-09-18Bibliographically approved
Dong, Y., Pearce, M., Ryde, F., Zhang, S. & et al., . (2016). Experimental verification of the HERD prototype at CERN SPS. In: Proceedings of SPIE: SPACE TELESCOPES AND INSTRUMENTATION 2016: ULTRAVIOLET TO GAMMA RAY: . Paper presented at Conference on Space Telescopes and Instrumentation - Ultraviolet to Gamma Ray, Edinburgh, SCOTLAND, JUN 26-JUL 01, 2016. SPIE - International Society for Optical Engineering
Open this publication in new window or tab >>Experimental verification of the HERD prototype at CERN SPS
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2016 (English)In: Proceedings of SPIE: SPACE TELESCOPES AND INSTRUMENTATION 2016: ULTRAVIOLET TO GAMMA RAY, SPIE - International Society for Optical Engineering, 2016Conference paper, Published paper (Refereed)
Abstract [en]

The High Energy cosmic-Radiation Detection (HERD) facility is one of several space astronomy payloads of the cosmic light house program onboard China's Space Station, which is planned for operation starting around 2020 for about 10 years. Beam test with a HERD prototype, to verify the HERD specifications and the reading out method of wavelength shifting fiber and image intensified CCD, was taken at CERN SPS in November, 2015. The prototype is composed of an array of 5∗5∗10 LYSO crystals, which is 1/40th of the scale of HERD calorimeter. Experimental results on the performances of the calorimeter are discussed.

Place, publisher, year, edition, pages
SPIE - International Society for Optical Engineering, 2016
Keywords
3d imaging, Calorimeter, Cosmic ray, Dark matter, Gamma ray, ICCD, Shower, WLSF
National Category
Accelerator Physics and Instrumentation
Identifiers
urn:nbn:se:kth:diva-202109 (URN)10.1117/12.2231804 (DOI)000387731500178 ()2-s2.0-85003633069 (Scopus ID)
Conference
Conference on Space Telescopes and Instrumentation - Ultraviolet to Gamma Ray, Edinburgh, SCOTLAND, JUN 26-JUL 01, 2016
Note

QC 20170217

Available from: 2017-02-17 Created: 2017-02-17 Last updated: 2017-02-17Bibliographically approved
Chauvin, M., Floren, H.-G. -., Jackson, M., Kamae, T., Kawano, T., Kiss, M., . . . Pearce, M. (2016). Observation of polarized hard X-ray emission from the Crab by the PoGOLite Pathfinder. Monthly notices of the Royal Astronomical Society, 456(1), L84-L88
Open this publication in new window or tab >>Observation of polarized hard X-ray emission from the Crab by the PoGOLite Pathfinder
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2016 (English)In: Monthly notices of the Royal Astronomical Society, ISSN 0035-8711, E-ISSN 1365-2966, Vol. 456, no 1, p. L84-L88Article in journal (Refereed) Published
Abstract [en]

We have measured the linear polarization of hard X-ray emission from the Crab in a previously unexplored energy interval, 20-120 keV. The introduction of two new observational parameters, the polarization fraction and angle stands to disentangle geometrical and physical effects, thereby providing information on the pulsar wind geometry and magnetic field environment. Measurements are conducted using the PoGOLite Pathfinder - a balloon-borne polarimeter. Polarization is determined by measuring the azimuthal Compton scattering angle of incident X-rays in an array of plastic scintillators housed in an anticoincidence well. The polarimetric response has been characterized prior to flight using both polarized and unpolarized calibration sources. We address possible systematic effects through observations of a background field. The measured polarization fraction for the integrated Crab light curve is 18.4(-10.6)(+9.8) per cent, corresponding to an upper limit (99 per cent credibility) of 42.4 per cent, for a polarization angle of (149.2 +/- 16.0)degrees.

Place, publisher, year, edition, pages
Oxford University Press, 2016
Keywords
instrumentation: polarimeters, techniques: polarimetric, stars: neutron, pulsars: individual: the Crab pulsar
National Category
Astronomy, Astrophysics and Cosmology
Identifiers
urn:nbn:se:kth:diva-182840 (URN)10.1093/mnrasl/slv177 (DOI)000368010000018 ()2-s2.0-84959175886 (Scopus ID)
Note

QC 20160224

Available from: 2016-02-24 Created: 2016-02-23 Last updated: 2018-05-21Bibliographically approved
Topchiev, N. P., Pearce, M., Ryde, F., Zverev, V. G. & et al., . (2016). Perspectives of the GAMMA-400 space observatory for high-energy gamma rays and cosmic rays measurements. In: INTERNATIONAL CONFERENCE ON PARTICLE PHYSICS AND ASTROPHYSICS (ICPPA-2015), PTS 1-4: . Paper presented at International Conference on Particle Physics and Astrophysics (ICPPA), Moscow, 2015. Institute of Physics (IOP)
Open this publication in new window or tab >>Perspectives of the GAMMA-400 space observatory for high-energy gamma rays and cosmic rays measurements
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2016 (English)In: INTERNATIONAL CONFERENCE ON PARTICLE PHYSICS AND ASTROPHYSICS (ICPPA-2015), PTS 1-4, Institute of Physics (IOP), 2016Conference paper, Published paper (Refereed)
Abstract [en]

The GAMMA-400 gamma-ray telescope is intended to measure the fluxes of gamma-rays and cosmic-ray electrons and positrons in the energy range from 100 MeV to several TeV. Such measurements concern the following scientific tasks: investigation of point sources of gamma-rays, studies of the energy spectra of Galactic and extragalactic diffuse emission, studies of gamma-ray bursts and gamma-ray emission from the Sun, as well as high precision measurements of spectra of high-energy electrons and positrons. Also the GAMMA-400 instrument provides the possibility for protons and nuclei measurements up to knee. But the main goal for the GAMMA-400 mission is to perform a sensitive search for signatures of dark matter particles in high-energy gamma-ray emission. To fulfill these measurements the GAMMA-400 gamma-ray telescope possesses unique physical characteristics in comparison with previous and present experiments. The major advantage of the GAMMA-400 instrument is excellent angular and energy resolution for gamma-rays above 10 GeV. The GAMMA-400 experiment will be installed onboard of the Navigator space platform, manufactured by the NPO Lavochkin Association. The expected orbit will be a highly elliptical orbit (with apogee 300.000 km and perigee 500 km) with 7 days orbital period. An important profit of such an orbit is the fact that the full sky coverage will always be available for gamma ray astronomy.

Place, publisher, year, edition, pages
Institute of Physics (IOP), 2016
Series
Journal of Physics Conference Series ; 675
National Category
Astronomy, Astrophysics and Cosmology
Identifiers
urn:nbn:se:kth:diva-185738 (URN)10.1088/1742-6596/675/3/032010 (DOI)000372460100076 ()2-s2.0-84964720786 (Scopus ID)
Conference
International Conference on Particle Physics and Astrophysics (ICPPA), Moscow, 2015
Note

QC 20160426

Available from: 2016-04-26 Created: 2016-04-26 Last updated: 2016-11-03Bibliographically approved
Organisations
Identifiers
ORCID iD: ORCID iD iconorcid.org/0000-0002-9769-8016

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