T. Mizuno

Hiroshima University

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Co-Authors

H. Takahashi

Hiroshima University

Y. Fukazawa

Hiroshima University

H. Katagiri

Toyohashi University of Technology

A. Morselli

Istituto Nazionale di Fisica Nucleare, Sezione di Roma I

J. Kataoka

Waseda University

N. Giglietto

Polytechnic University of Bari

R. Rando

University of Padua

T. Ohsugi

Hiroshima University

H. Tajima

Nagoya University

L. Baldini

Sapienza University of Rome

Cooperative Institutions

Centre National de la Recherche Scientifique

292

Universitat de Barcelona

228

Institut d'Estudis Espacials de Catalunya

221

Max Planck Institute for Physics

189

University of Turku

187

Stanford University

173

SLAC National Accelerator Laboratory

162

Kavli Institute for Particle Astrophysics and Cosmology

161

The University of Tokyo

157

TU Dortmund University

146

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Modulated High-Energy Gamma-Ray Emission from the Microquasar Cygnus X-3

Science (2009)

A. A. Abdo M. Ackermann M. Ajello M. Axelsson L. Baldini

Microquasar Spotted Microquasars are binary star systems where a normal star sheds matter onto a neutron star or a black hole, generating x-ray radiation and jets of material moving at relativistic speeds. Microquasars have proved difficult to detect in high-energy gamma rays (> 100 megaelectron volts). Using the Fermi Large Area Telescope, Abdo et al. (p. 1512 , published online 26 November; see the Perspective by Bignami ) now report the detection of variable gamma-ray emission from the microquasar Cygnus X-3. The gamma-ray flux is modulated at the orbital period of Cygnus X-3, and its variation is correlated with the radio emission originating from the microquasar's relativistic jets.

Black hole (networking)

X-ray binary

Astrophysical jet

Star (game theory)

10.1126/science.1182174

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Citations (231)

Three Advantages of the KANATA 1.5-m Telescope as a Powerful Partner for GLAST

AIP conference proceedings (2007)

Makoto Uemura T. Ohsugi Tsukasa Yamashita K. Kawabata Akira Arai

KANATA is a 1.5‐m optical—near infrared telescope of Hiroshima University, which has been developed for observations of astronomical transients and variables, such as γ‐ray bursts, blazars. X‐ray transients, and cataclysmic variables. Here, we introduce three characteristics of KANATA with examples of observations, that is, i) high ability for prompt observations, ii) simultaneous optical and infrared observations, and iii) polarimetric observations. Collaborating with GLAST, we are planning to perform follow‐up optical—infrared observations of γ‐ray sources with KANATA.

Infrared telescope

10.1063/1.2757301

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Citations (1)

VizieR Online Data Catalog: Fermi-LAT flaring gamma-ray sources from FAVA (Ackermann+, 2013)

yCat (2015)

M. Ackermann M. Ajello A. Albert A. Allafort E. Antolini

Ackermann function

Source

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GLAST simulation study of an extended TeV-emitting supernova remnant for the origin of cosmic-ray nuclei

AIP conference proceedings (2007)

H. Katagiri H. Yoshida T. Mizuno H. Takahashi Y. Fukazawa

We extracted the gamma‐ray emission of the π0‐decay, which will be a decisive evidence of cosmic‐ray proton acceleration, from the one‐year data of an extended TeV‐emitting supernova remnant, generated by the GLAST full detector simulation, although many assumptions were oversimplified.

10.1063/1.2757370

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SECOND CATALOG OF ACTIVE GALACTIC NUCLEI DETECTED BY THE FERMI LARGE AREA TELESCOPE (vol 743, 171, 2011)

The Astrophysical Journal (2015)

M. Ackermann M. Ajello A. Allafort E. Antolini W. B. Atwood

Source

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Citations (2)

A gamma-ray determination of the Universe’s star formation history

Science (2018)

S. Abdollahi M. Ackermann M. Ajello W. B. Atwood L. Baldini

Gamma rays reveal the Universe's history How many stars have formed in the Universe, and when did they do so? These fundamental questions are difficult to answer because there are systematic uncertainties in converting the light we observe into the total mass of stars in galaxies. The Fermi-LAT Collaboration addressed these questions by exploiting the way that gamma rays from distant blazars propagate through intergalactic space, which depends on the total amount of light emitted by all galaxies. The collaboration found that star formation peaked about 3 billion years after the Big Bang (see the Perspective by Prandini). Although this is similar to previous estimates from optical and infrared observations, the results provide valuable confirmation because they should be affected by different systematic effects. Science , this issue p. 1031 ; see also p. 995

Intergalactic dust

Intergalactic star

10.1126/science.aat8123

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Citations (141)

Cosmic‐Ray Background Flux Model Based on aGamma‐Ray Large Area Space TelescopeBalloon Flight Engineering Model

The Astrophysical Journal (2004)

T. Mizuno T. Kamae G. Godfrey T. Handa D. J. Thompson

Cosmic-ray background fluxes were modeled on the basis of existing measurements and theories and are presented here. The model, originally developed for the Gamma-Ray Large Area Space Telescope (GLAST) balloon experiment, covers the entire solid angle (4π sr), the sensitive energy range of the instrument (~10 MeV to 100 GeV), and the abundant components (proton, alpha particle, e-, e+, μ-, μ+, and gamma ray). It is expressed in analytic functions in which modulations due to solar activity and the Earth's geomagnetism are parameterized. Although the model is intended to be used primarily for the GLAST balloon experiment, model functions in low Earth orbit are also presented and can be used for other high-energy astrophysical missions. The model has been validated via comparison with the data of the GLAST balloon experiment.

Orbit (dynamics)

Spitzer Space Telescope

Earth's orbit

Gamma-Ray Astronomy

10.1086/423801

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Citations (87)

FERMIOBSERVATIONS OF GRB 090510: A SHORT-HARD GAMMA-RAY BURST WITH AN ADDITIONAL, HARD POWER-LAW COMPONENT FROM 10 keV TO GeV ENERGIES

The Astrophysical Journal (2010)

M. Ackermann Katsuaki Asano W. B. Atwood M. Axelsson L. Baldini

We present detailed observations of the bright short-hard gamma-ray burst GRB 090510 made with the Gamma-ray Burst Monitor (GBM) and Large Area Telescope (LAT) on board the Fermi observatory. GRB 090510 is the first burst detected by the LAT that shows strong evidence for a deviation from a Band spectral fitting function during the prompt emission phase. The time-integrated spectrum is fit by the sum of a Band function with $\Epeak = 3.9\pm 0.3$\,MeV, which is the highest yet measured, and a hard power-law component with photon index $-1.62\pm 0.03$ that dominates the emission below $\approx$\,20\,keV and above $\approx$\,100\,MeV. The onset of the high-energy spectral component appears to be delayed by $\sim$\,0.1\,s with respect to the onset of a component well fit with a single Band function. A faint GBM pulse and a LAT photon are detected 0.5\,s before the main pulse. During the prompt phase, the LAT detected a photon with energy $30.5^{+5.8}_{-2.6}$ GeV, the highest ever measured from a short GRB. Observation of this photon sets a minimum bulk outflow Lorentz factor, $\Gamma\ga$\,1200, using simple $\gamma\gamma$ opacity arguments for this GRB at redshift $z = 0.903$ and a variability time scale on the order of tens of ms for the $\approx$\,100\,keV--few MeV flux. Stricter high confidence estimates imply $\Gamma \ga 1000$ and still require that the outflows powering short GRBs are at least as highly relativistic as those of long duration GRBs. Implications of the temporal behavior and power-law shape of the additional component on synchrotron/synchrotron self-Compton (SSC), external-shock synchrotron, and hadronic models are considered.

Spectral index

10.1088/0004-637x/716/2/1178

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Citations (334)

Performance of large-area avalanche photodiode for low-energy X-rays and γ-rays scintillation detection

Nuclear Instruments and Methods in Physics Research Section A Accelerators Spectrometers Detectors and Associated Equipment (2003)

T. Ikagawa J. Kataoka Yoichi Yatsu N. Kawai Kunishiro Mori

Photodiode

X-ray detector

Biasing

10.1016/j.nima.2003.07.024

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Citations (51)

Gamma-ray burst monitoring with the hard X-ray detector onboard the ASTRO-E mission

AIP conference proceedings (1996)

Atsushi Yoshida H. Ezawa Y. Fukazawa M. Hirayama E. Idesawa

ASTRO-E is the fifth Japanese X-ray astronomy satellite scheduled to be launched in year 2000. The satellite will carry three scientific instruments, one of which is the Hard X-ray Detector (HXD). HXD will cover the 10–600 keV band with low background of several×10−6c/s/cm2/keV. This will be achieved by the well-type phoswich counter technique together with large active shield counters of BGO (about 1200 cm2/side), which are also capable to detect GRBs in the 100–2000 keV band. About 100 GRBs are expected to be detected per year with HXD.

X-ray detector

Launched

10.1063/1.51609

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