X-ray polarimetry small satellite TSUBAME

Arimoto, M.; Tsubuku, Y.; Toizumi, T.; Kobayashi, M.; Yatsu, Yoichi; Shimokawabe, Takashi; Kataoka, J.; Kawai, N.; Omagari, Kuniyuki; Fujiwara, Ken; Konda, Yasumi; Tanaka, Yohei; Maeno, Masaki; Yamanaka, Tateo; Ashida, Hiroki; Nishida, Jun‐ichi; Fujihashi, Kouta; Ikeda, T.; Inagawa, Shinichi; Miura, Yoshio; Matunaga, Saburo; Galassi, M.; Palmer, D. M.; Fenimore, E.

doi:10.1063/1.2943543

Cited by 3 publications

(3 citation statements)

References 2 publications

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“…During the first four years of operation, CHASE has produced more than 130 supernovae, being the most successful project of its type in the southern hemisphere (Hamuy et al, 2012). c) TSUBAME is an interesting example of a micro-satellite developed by the students of Tokyo Institute of Technology (Arimoto et al, 2008). The name Tsubame means "swift" in Japanese, referring to the fast spacecraft attitude changes for event monitoring; it also connotes a certain relationship to NASA's gamma-ray mission, Swift.…”

Section: Pos(multif2023)001mentioning

confidence: 99%

A Journey to Understand Our Universe

Giovannelli

2024

Proceedings of Multifrequency Behaviour of High Energy Cosmic Sources XIV — PoS(MULTIF2023)

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A Journey into the Universe Franco Giovannelli 4.10 Extragalactic background light 4.11 Unified model for compact sources 4.12 Jets in astrophysics 4.13 The tidal disruption of stars by massive black holes 4.14 Neutrinos 5. The challenge to know our universe 5.1 Big experiments 5.2 Small experiments 5.3 Active physics experiments 5.3.1 The Large Hadron Collider (LHC) 5.4 Passive physics experiments 5.4.1 The Cherenkov Telescope Array 5.4.2 ESO-Extremely Large Telescope 5.4.3 Canadian Hydrogen Intensity Mapping Experiment: CHIME 5.4.4 e-ASTROGAM observatory 5.4.5 Imaging X-ray Polarimetry Explorer (IXPE) 5.4.6 The James Webb Space Telescope (JWST) 5.4.7 The GAMMA-400 gamma-ray telescope 5.4.8 The BICEP (Background Imaging of Cosmic Extragalactic Polarization) and the Keck Array 5.4.9 LSPE (Large Scale Polarization Explorer) 5.4.10 QUBIC experiment 5.4.11 Square Kilometer Array 5.5 Cosmic Ray physics experiments 5.5.1 HAWC (High-Altitude Water Cherenkov Gamma-ray Observatory) 5.5.2 LHAASO (Large High Altitude Air Shower Observatory) 5.5.3 TAIGA (Tunka Advanced Instrument for cosmic ray physics and Gamma Astronomy) 6. Habitable zone in the Milky Way and exoplanets 7. Origin of terrestrial life 7.1 The Cambrian explosion 7.2 Plant life 7.3 Animal life 7.4 The evolution of humans 7.5 What intelligent humanity is doing? 8. Great examples of synergy between astrophysics and history 9. The use of wisdom in physics 9.1 The classical T Tauri star RU Lupi 9.2 The cataclysmic variable SS Cygni 9.3 X-ray/Be systems PoS(MULTIF2023)001A Journey into the Universe Franco Giovannelli Conclusions and perspectivesA Journey into the Universe Franco Giovannelli Drouart et al. (1999) starting from the fact that each nebula disk is characterized by its initial mass M D , its initial radius R D , and the coefficient of turbulent viscosity α, they show that these parameters may be constrained by comparing temperature-density profiles to properly chosen physical and chemical Solar System data. They developed an analytical model that permits fruitful comparisons with available Solar System data and helpful constraints on the structure of the primitive solar nebula, as summarized below:• Theories of the formation of giant planets provide relatively weak constraints on the main parameters which define the nebula, namely the initial mass M D , the initial radius R D , and the coefficient of turbulent diffusion α. However, they conclude that forming the cores of giant planets in a time compatible with the lifetime of the nebula requires a α value equal to at least a few 10 −4 .• The enrichment in fossil deuterium enrichment in water with respect to the protosolar abundance is by far more constraining. At t = 0, R D must be between 8 and 28 AU, M D between 0.03 and 0.3 M ⊙ , and α must be between 0.003 and 1.• The high viscosity disks they infer (0.02 < α < 1) are characterized by a magnetohydrodynamic (MHD) turbulence while their low viscosity models (0.003 < α < 0.02) are charaterized by hydrodynamical turbulence. Other mechanisms susceptible ...

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Section: Pos(multif2023)001mentioning

confidence: 99%

A Journey to Understand Our Universe

Giovannelli

2024

Proceedings of Multifrequency Behaviour of High Energy Cosmic Sources XIV — PoS(MULTIF2023)

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“…Tsubame is a microsatellite developed at the Tokyo Institute of Technology that was placed into orbit in November, 2014 (Yatsu et al, 2014(Yatsu et al, , 2011Arimoto et al, 2008). The satellite uses a nearly cubic platform measuring 50 cm × 50 cm × 47 cm.…”

Section: Tsubamementioning

confidence: 99%

High energy polarimetry of prompt GRB emission

McConnell

2017

New Astronomy Reviews

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Evidence of polarized γ-ray emission (> 50 keV) from Gamma-Ray Bursts (GRBs) has been accumulated in recent years. Measurements have been reported with levels in the range of 30-80%, typically with limited statistical significance. No clear picture has yet emerged with regards to the polarization properties of GRBs. Taken at face value, the data suggest that most GRBs have a relatively large level of polarization (typically, > 50%), which may suggest synchrotron emission associated with an ordered magnetic field structure within the GRB jet. But these results are far from conclusive. Here, we review the observations that have been made, concentrating especially on the instrumental issues and the lessons that might be learned from these data.

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“…We performed a Monte Carlo simulation of Compton scattering to determine the signal and background levels of the HXCP and the detectability of the polarization from GRBs using the Geant4 simulator 6) . As an indicator of the performance of the HXCP, we use the modulation factor.…”

Section: Hxcp Simulationmentioning

confidence: 99%

TSUBAME: toward the Frontier of X-ray/Gamma-ray Polarimetry in Astronomy

Toizumi

Kataoka

Tsubuku

et al. 2009

Trans. JSASS Space Tech. Japan

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"TSUBAME" is a university-built small satellite mission to measure polarization of hard X-ray photons (30-200 keV) from gamma-ray bursts (GRBs) using azimuthal anisotropy of Compton-scattered photons. Polarimetry in the hard X-ray and soft γ-ray bands should provide crucial information for understanding the high-energy emission mechanisms and the distribution of magnetic fields and radiation fields in the astrophysical sources. TSUBAME has two instruments: the Wide-field Burst Monitor (WBM) and the Hard X-ray Compton Polarimeter (HXCP). The WBM determines on board the direction of the burst occurrence with an accuracy of 10 degrees, then using a high speed attitude control device, the HXCP is pointed to the GRB within 15 seconds after the burst occurrence to promptly detect polarized X-ray photons from the GRB. We present an overview of the TSUBAME mission, its estimated scientific capability for detecting GRBs and measuring their X-ray polarization, development of multi-anode photomultiplier tubes that use ultra bi-alkali photocathodes, and the future plans of this mission.

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X-ray polarimetry small satellite TSUBAME

Cited by 3 publications

References 2 publications

A Journey to Understand Our Universe

A Journey to Understand Our Universe

High energy polarimetry of prompt GRB emission

TSUBAME: toward the Frontier of X-ray/Gamma-ray Polarimetry in Astronomy

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