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2. EXPERIMENTAL DETERMINATION OF ANISOTROPIC EMISSION OF NEUTRONS FROM 252CF NEUTRON SOURCE WITH THE SPHERICAL PROTECTION CASE

Author

Hiroshi Yoshitomi, Sho Nishino, Kristine Marie D. Romallosa, Tetsuya Ohishi, Yoshihiko Tanimura, and Munehiko Kowatari

Subjects
Neutrons, Range (particle radiation), Radiation, Materials science, Radiological and Ultrasound Technology, Monte Carlo method, Californium, Public Health, Environmental and Occupational Health, chemistry.chemical_element, General Medicine, Computational physics, chemistry, Aluminium, Neutron source, Anisotropy, Radiology, Nuclear Medicine and imaging, Neutron, Radiometry, Casing, Monte Carlo Method, Zenith
Abstract

The anisotropic emission of neutrons from a cylindrical X1 252Cf source with the spherical external casing was experimentally determined. The influence of metal materials and shapes of the external casing to the anisotropy factor, FI(θ), was assessed by the Monte Carlo calculation, before performing the measurement. The results of the calculation implied that light- and spherical-shaped external casing decreases the anisotropic emission of neutrons from a cylindrical source and the nature of the material does not affect the anisotropic emission to a large extent. The experimental results obtained when a spherical-shaped aluminum protection case was employed also revealed that the anisotropy factor was close to 1.0 with a wide zenith angle range. Considering the source handling and measures against mechanical impact to the source, we designed an SUS304-made spherical protection case for a renovated source delivering apparatus. With the SUS304-made spherical protection case, the measured anisotropy factor FI(90) was determined to be 1.002 ± 0.002 (k = 1). Results from the experiments also indicated that the measured anisotropy factor has a flat distribution from 55 to 125° with zenith angle.

Published
2020

3. Development of the high-energy neutron fluence rate standard field in Japan with a peak energy of 45 MeV using the 7Li(p,n)7Be reaction at TIARA

Author

Yoshihiko Tanimura, Satoshi Kurashima, Michio Yoshizawa, Hideki Harano, Sho Nishino, Jun Nishiyama, Masayuki Hagiwara, Hajime Seito, Yoshiaki Shikaze, Yasuhiro Unno, Tetsuro Matsumoto, Hiroshi Yoshitomi, and Akihiko Masuda

Subjects
010302 applied physics, Bonner sphere, Physics, Nuclear and High Energy Physics, High energy, Field (physics), 010308 nuclear & particles physics, Astrophysics::High Energy Astrophysical Phenomena, Physics::Medical Physics, Nuclear Theory, 01 natural sciences, Nuclear physics, Nuclear Energy and Engineering, Neutron flux, 0103 physical sciences, Neutron cross section, Physics::Accelerator Physics, Neutron detection, Neutron, Nuclear Experiment, Energy (signal processing)
Abstract

In this study, we developed a 45 MeV neutron fluence rate standard of Japan. Quasi-monoenergetic neutrons with a peak energy of 45 MeV in the neutron standard field were produced by the 7Li(p,n)7Be...

Published
2017

5. Development of the Graphite-Moderated Neutron Calibration Fields Using 241Am-Be Sources in JAEA-FRS

Author

Sho Nishino, Yoshihiko Tanimura, Michio Yoshizawa, and Yoshiaki Ebata

Subjects
Radiation, Materials science, Spectrometer, Equivalent dose, Astrophysics::High Energy Astrophysical Phenomena, Health, Toxicology and Mutagenesis, Nuclear Theory, Radiochemistry, Public Health, Environmental and Occupational Health, Neutron temperature, Nuclear physics, Measuring instrument, Calibration, Neutron detection, Radiology, Nuclear Medicine and imaging, Neutron, Nuclear Experiment
Abstract

Background: The moderated neutron calibration fields using 241Am-Be sources and a graphite moderator have been constructed at the Facility of Radiation Standard (FRS) in the Japan Atomic Energy Agency (JAEA). Materials and Methods: The neutron spectra of the fields were evaluated by the Monte-Carlo calculations and measurements using the Bonner Multi-sphere Spectrometer. Results and Discussion: The fields have continuous neutron spectra from several MeV to thermal neutron energy, with fluence-averaged energies of 0.84 MeV and 0.60 MeV. Reference values of fluence rates and ambient/personal dose equivalent rates were determined from neutron spectra by measurements. Conclusion: Currently, the fields are available for calibration or performance test of neutron measuring instruments.

Published
2016

6. Background correction method for portable thyroid dose monitor using gamma-ray spectrometer developed at JAEA in high dose rate environment

Author

M. Takahashi, Sho Nishino, Yoshihiko Tanimura, and Hiroshi Yoshitomi

Subjects
010302 applied physics, Physics, Radiation, Photon, Point source, Gamma ray spectrometer, business.industry, Equivalent dose, equipment and supplies, 01 natural sciences, Dose monitoring, Imaging phantom, 030218 nuclear medicine & medical imaging, 03 medical and health sciences, 0302 clinical medicine, Optics, 0103 physical sciences, Background Correction Method, Dose rate, business, Instrumentation
Abstract

A portable thyroid dose monitoring system has been developed at the Japan Atomic Energy Agency (JAEA) to assess the thyroid equivalent dose for workers and members of the public in a high dose rate environment. The background (B.G.) photon correction is required for an accurate measurement in a high dose rate environment at an early stage after a nuclear accident. The responses of the system to the B.G. photons were calculated with the simplified cylindrical phantoms made of PMMA or the voxel phantoms using the PHITS code. Then they were compared each other among the respective age groups. It was found that the cylindrical phantom with an appropriate size and properly arrangement can mimic the human body in the high dose rate caused by 131I sources. As such we successfully developed the B.G. photon correction method using the cylindrical phantoms; one of those is used as an effective way to calibrate the monitoring system by inserting a133Ba point source into it. As an additional phantom is not required, this method has a great advantage in the practical operation of the B.G. photon correction.

Published
2020

8. Prototype test of a portable thyroid dose monitoring system using gamma-ray spectrometers

Author

Yoshihiko Tanimura, Hiroshi Yoshitomi, Sho Nishino, and M. Takahashi

Subjects
010302 applied physics, Radiation, Spectrometer, business.industry, Thyroid, Gamma ray, Radiation shield, 01 natural sciences, Dose monitoring, 030218 nuclear medicine & medical imaging, 03 medical and health sciences, 0302 clinical medicine, medicine.anatomical_structure, 0103 physical sciences, medicine, Environmental science, Nuclear medicine, business, Instrumentation, Background radiation
Abstract

In case of a severe nuclear accident, radioiodine monitoring of the thyroid must be carried out for a large number of residents and emergency workers. In the present study, we developed a portable thyroid dose monitoring system consisting of two independent gamma-ray spectrometers and a radiation shield, which could be used under high background radiation conditions. Two types of prototype thyroid monitors were realized; one utilizing CdZnTe detectors for emergency workers and the other employing LaBr3(Ce) detectors for members of the public. As a result of the performance test, it was confirmed that both monitors effectively assess thyroid equivalent doses of

Published
2020

9. A study of a calibration technique for a newly developed thyroid monitor and its uncertainties due to body size for radioiodine measurements

Author

Yoshihiko Tanimura, M. Takahashi, Sho Nishino, and Hiroshi Yoshitomi

Subjects
010302 applied physics, Accuracy and precision, Measure (data warehouse), Radiation, Monte Carlo method, Thyroid, Body size, computer.software_genre, 01 natural sciences, Emergency situations, 030218 nuclear medicine & medical imaging, 03 medical and health sciences, 0302 clinical medicine, medicine.anatomical_structure, Voxel, 0103 physical sciences, Calibration, medicine, Environmental science, Instrumentation, computer, Remote sensing
Abstract

We have developed a portable thyroid monitoring system to measure thyroid doses for members of the public in a nuclear emergency. It is assumed that a large number of these monitoring systems are deployed and maintained for emergency situations. Hence, the calibration performed should be performed as simple as possible. We proposed a new calibration method based on standard voxel phantoms using a point source. By applying this method to the thyroid monitoring system, the counting efficiencies were evaluated. Although this monitor is properly calibrated, any differences between the phantoms used in the calibration and the monitored subjects can affect the measurement accuracy. Therefore, the influence of the anatomical features of the subjects on the detection efficiencies was investigated in detail by Monte Carlo calculations. The effects of the body size on the counting efficiencies of the thyroid monitoring system were estimated using several voxel phantoms. Consequently, the uncertainties in the counting efficiencies due to the body size were found to be within 25%.

Published
2020

10. Time-of-Flight Measurements for Low-Energy Components of 45-MeV Quasi-Monoenergetic High-Energy Neutron Field from <formula formulatype='inline'><tex Notation='TeX'>${^7{\rm Li}({\rm p}, {\rm n})}$</tex></formula> Reaction

Author

Jun Nishiyama, Tetsuro Matsumoto, Yasuhiro Unno, H. Seito, Masayuki Hagiwara, Sho Nishino, Yoshiaki Shikaze, Akihiko Masuda, S. Kurashima, Michio Yoshizawa, Yoshihiko Tanimura, Hideki Harano, and Hiroshi Yoshitomi

Subjects
Physics, Nuclear and High Energy Physics, Physics::Instrumentation and Detectors, Astrophysics::High Energy Astrophysical Phenomena, Nuclear Theory, Physics::Medical Physics, Liquid scintillation counting, Cyclotron, Detector, Scintillator, Fluence, law.invention, Nuclear physics, Time of flight, Nuclear Energy and Engineering, law, Neutron detection, Neutron, Electrical and Electronic Engineering, Nuclear Experiment
Abstract

A quasi-monoenergetic neutron field generated in the ${^7{\rm Li}({\rm p}, {\rm n})}$ reaction consists of a high-energy monoenergetic peak and a continuum to the low-energy region. In this study, the spectral fluence of the continuum was measured with the time-of-flight (TOF) method using a ${^6{\rm Li}}$ -glass scintillation detector and an organic liquid scintillation detector for the keV and MeV region, respectively. The neutron spectral fluence was determined down to the keV region by implementing a new beam chopping system and the results showed that the neutrons that came directly from the target had a lower energy limit about 100 keV. Discussions were made also on the effect of the time-independent neutrons which are assumed to be room-scattered neutrons. The obtained information is expected to contribute to understanding the quasi-monoenergetic high-energy neutron field and improvements of calibrating neutron detectors in the field.

Published
2015

11. CHARACTERIZATION OF AN IN-HOUSE DEVELOPED MULTI-CYLINDRICAL MODERATOR NEUTRON SPECTROMETER

Author

J. Channuie, T. Liamsuwan, Sho Nishino, Munehiko Kowatari, and S. Wonglee

Subjects
Field (physics), Nuclear Theory, Monte Carlo method, Proportional counter, Radiation Dosage, Helium, 030218 nuclear medicine & medical imaging, Nuclear physics, Matrix (chemical analysis), 03 medical and health sciences, 0302 clinical medicine, Humans, Radiology, Nuclear Medicine and imaging, Neutron, Nuclear Experiment, Radiometry, Physics, Neutrons, Range (particle radiation), Radiation, Radiological and Ultrasound Technology, Spectrometer, Public Health, Environmental and Occupational Health, General Medicine, Characterization (materials science), 030220 oncology & carcinogenesis, Monte Carlo Method
Abstract

This article describes the characterization of an in-house developed multi-cylindrical moderator neutron spectrometer, which consists of a cylindrical 3He proportional counter and cylindrical moderator shells of different sizes. The response matrix of the spectrometer was calculated by Monte Carlo simulations for neutron energies from 1 × 10−8 to 10 MeV and verified with measurements in 0.144 MeV, 1.2 MeV and 241AmBe neutron standard fields. Influence of scattered neutrons was properly eliminated from the measured response using the shadow cone technique. The calculated and measured responses were in good agreement in most cases. Differences were

Published
2017

12. Constraint of Non-Thermal X-Ray Emission from the On-Going Merger Cluster Abell 3376 with Suzaku

Author

Naomi Kawano, Kazuhiro Nakazawa, Ann Hornschemeier, Takaya Ohashi, Tadayuki Takahashi, Takao Kitaguchi, J. Patrick Henry, Sho Nishino, Yasushi Fukazawa, Motohide Kokubun, Kazuo Makishima, Naoki Isobe, and Naomi Ota

Subjects
Physics, Astrophysics::High Energy Astrophysical Phenomena, Astrophysics (astro-ph), Imaging spectrometer, Center (category theory), FOS: Physical sciences, Flux, Astronomy and Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, Galaxy, Relativistic particle, Particle acceleration, X-rays: galaxies, Space and Planetary Science, galaxies: clusters: individual (Abell 3376), Thermal, Cluster (physics), X-rays: non-thermal emission, Astrophysics::Galaxy Astrophysics
Abstract

Clusters of galaxies are among the best candidates for particle acceleration sources in the universe, a signature of which is non-thermal hard X-ray emission from the accelerated relativistic particles. We present early results on Suzaku observations of non-thermal emission from Abell 3376, which is a nearby on-going merger cluster. Suzaku observed the cluster twice, focusing on the cluster center containing the diffuse radio emission to the east, and cluster peripheral region to the west. For both observations, we detect no excess hard X-ray emission above the thermal cluster emission. An upper limit on the non-thermal X-ray flux of $2.1\times10^{-11}$ erg cm$^{-2}$ s$^{-1}$ (15--50 keV) at the 3$\sigma$ level from a $34\times34$ arcmin$^2$ region, derived with the Hard X-ray Detector (HXD), is similar to that obtained with the BeppoSAX/PDS. Using the X-ray Imaging Spectrometer (XIS) data, the upper limit on the non-thermal emission from the West Relic is independently constrained to be $0.03\mu$G (HXD) and $>0.10\mu$G (XIS)., Comment: 19pages, 10 figures, accepted in the PASJ

Published
2009

13. Spectral measurement of quasi-monoenergetic high-energy neutron field by combination of TOF and Bonner unfolding methods

Author

Masayuki Hagiwara, Tetsuro Matsumoto, Yoshihiko Tanimura, Hideki Harano, H. Seito, Yoshiaki Shikaze, Jun Nishiyama, Yasuhiro Unno, S. Kurashima, Michio Yoshizawa, Hiroshi Yoshitomi, Akihiko Masuda, and Sho Nishino

Subjects
Nuclear physics, Bonner sphere, Physics, High energy, Spectrometer, Field (physics), Physics::Instrumentation and Detectors, Neutron flux, Astrophysics::High Energy Astrophysical Phenomena, Detector, Neutron, Nuclear Experiment, Particle detector
Abstract

The spectral neutron fluence was measured by a combination of the TOF method (above keV region) and the Bonner unfolding method (whole energy region), for a 45-MeV quasi-monoenergetic high-energy neutron field. The extrapolated TOF-based spectrum information was used as a default spectrum for the Bonner unfolding method. The Bonner measurements were performed using the 3He-counter based Bonner sphere spectrometer (BSS) and the gold-activation BSS. While both unfolding reproduced reasonable solutions, difference in amount of the low-energy neutrons was observed between the types of BSS.

Published
2015

14. ERRATUM: 'FERMI LARGE AREA TELESCOPE STUDY OF COSMIC-RAYS AND THE INTERSTELLAR MEDIUM IN NEARBY MOLECULAR CLOUDS' (2012, ApJ, 755, 22)

Author

P. Lubrano, Denis Bastieri, Hartmut Sadrozinski, Sho Nishino, J. Lande, Sylvain Guiriec, Charles D. Dermer, F. Gargano, Rodrigo Nemmen, A. Chekhtman, D. Horan, Tadayuki Takahashi, M. Tinivella, M. Roth, Francesco Longo, Elizabeth C. Ferrara, W. B. Focke, P. Spinelli, Pierrick Martin, Francesco Giordano, Igor V. Moskalenko, I. A. Grenier, Olaf Reimer, A. Tramacere, E. J. Siskind, Takaaki Tanaka, C. Favuzzi, Stephan Zimmer, J. H. Panetta, Alice Allafort, Gloria Spandre, Markus Ackermann, R. A. Cameron, T. J. Brandt, P. Bruel, S. Murgia, Johann Cohen-Tanugi, T. L. Usher, Hiromitsu Takahashi, F. Piron, T. A. Porter, G. Busetto, Brian L Winer, G. A. Caliandro, J. M. Casandjian, Yasunobu Uchiyama, M. Razzano, Y. Hanabata, Masanori Ohno, A. Morselli, V. Vasileiou, V. Vitale, Stefan Funk, M. E. Monzani, E. Orlando, Zhenwei Yang, G. Pivato, A. A. Moiseev, R. Claus, J. Bregeon, Carmelo Sgrò, Riccardo Rando, E. Nuss, David Paneque, X. Hou, M. Kuss, T. Kamae, T. Ohsugi, Eleonora Troja, Miranda Jackson, Alice K. Harding, A. W. Borgland, A. De Angelis, T. Uehara, L. Falletti, G. Tosti, Eugenio Bottacini, Daniel Sánchez, S. J. Fegan, B. Berenji, M. H. Grondin, Gudlaugur Johannesson, Seth Digel, F. Loparco, Giacomo Vianello, O. Tibolla, W. Mitthumsiri, M. Naumann-Godo, Claudia Cecchi, Jürgen Knödlseder, Justin Vandenbroucke, R. E. Hughes, Eric Charles, Andrew W. Strong, Guido Barbiellini, Alex Drlica-Wagner, K. Hayashi, D. J. Suson, Nicola Giglietto, Keith Bechtol, Shiu-Hang Lee, Marianne Lemoine-Goumard, Dario Gasparrini, A. P. Waite, M. Ozaki, C. Monte, Ronaldo Bellazzini, T. Glanzman, M. N. Lovellette, P. A. Caraveo, Persis S. Drell, P. Wang, Nicola Omodei, D. J. Thompson, M. Brigida, Emanuele Bonamente, T. Sada, Jun Kataoka, S. Germani, K. S. Wood, A. S. Johnson, S. Larsson, Jay P. Norris, James Chiang, Roger Blandford, S. Rainò, Tsunefumi Mizuno, J. E. Grove, Yasushi Fukazawa, P. Fusco, Hiroaki Yamamoto, A. Reimer, J. F. Ormes, J. G. Thayer, J. Mehault, Carla Sbarra, Julie McEnery, Marco Ajello, J. B. Thayer, L. Tibaldo, S. Buson, D. Parent, Yasuo Fukui, Melissa Pesce-Rollins, Luca Baldini, M. Pierbattista, Diego F. Torres, Mn Mazziotta, C. Romoli, E. Do Couto E Silva, Jean Ballet, Stefano Ciprini, Elliott D. Bloom, R. Buehler, Peter F. Michelson, Marcello Giroletti, Hideaki Katagiri, F. D'Ammando, Akira Okumura, Daniela Hadasch, Jan Conrad, G. Godfrey, F. de Palma, and Ryosuke Itoh

Subjects
Physics, Molecular cloud, Astronomy, Astronomy and Astrophysics, Cosmic ray, Astrophysics, law.invention, Interstellar medium, Telescope, Space and Planetary Science, law, ddc:520, Fermi Gamma-ray Space Telescope
Abstract

The astrophysical journal 778(1), 82 (2013). doi:10.1088/0004-637X/778/1/82, This is an Erratum for the article 2012 ApJ 755 22, Published by Univ.11032, Chicago, Ill. [u.a.]

Published
2013
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15. Determination of the Point-spread Function for the Fermi Large Area Telescope from On-orbit Data and Limits on Pair Halos of Active Galactic Nuclei

Author

G. Busetto, Brian L Winer, S. Cutini, A. A. Moiseev, Katsuaki Asano, Francesco Longo, Gudlaugur Johannesson, F. Loparco, E. Do Couto E Silva, W. Mitthumsiri, T. A. Porter, A. P. Waite, T. J. Brandt, Jean Ballet, Stefan Funk, Daniel Sánchez, Claudia Lavalley, Sho Nishino, Alex Drlica-Wagner, Justin Vandenbroucke, T. E. Stephens, A. Morselli, V. Vitale, Jeffrey D. Scargle, P. Fusco, Stefano Ciprini, Igor V. Moskalenko, Matthew Kerr, A. W. Borgland, I. A. Grenier, S. Germani, T. Ohsugi, Eleonora Troja, Miranda Jackson, Nicola Omodei, Guido Barbiellini, S. J. Fegan, Olaf Reimer, Zhenwei Yang, Elliott D. Bloom, G. Godfrey, Kent S. Wood, T. Jogler, Carmelo Sgrò, Riccardo Rando, Soebur Razzaque, Jay P. Norris, M. Razzano, P. Fortin, L. S. Rochester, C. Favuzzi, V. Vasileiou, R. Claus, Matthew Wood, Stephan Zimmer, J. F. Ormes, N. Gehrels, James Chiang, Hiroyasu Tajima, Gino Tosti, Jan Conrad, F. de Palma, R. E. Hughes, E. Wallace, Dario Gasparrini, Patrick Weltevrede, E. Nuss, Paola Grandi, P. Lubrano, Hiromitsu Takahashi, M. Brigida, Sylvain Chaty, A. Chekhtman, David Paneque, Claudia Cecchi, S. Rainò, J. G. Thayer, T. Kamae, Tsunefumi Mizuno, Randall P. Johnson, Rodrigo Nemmen, R. Dubois, E. Orlando, J. M. Casandjian, D. Horan, F. D'Ammando, W. B. Focke, M. Kuss, C. Monte, M. E. Monzani, Gloria Spandre, P. Spinelli, M. N. Mazziotta, Jun Kataoka, Pascal Bruel, J. Mehault, Emanuele Bonamente, R. Buehler, J. E. Grove, S. Larsson, T. L. Usher, Francesco Giordano, D. J. Thompson, Daniela Hadasch, M. Roth, Yasushi Fukazawa, T. H. Burnett, A. S. Johnson, M. Orienti, S. Murgia, O. Tibolla, Benoit Lott, Peter F. Michelson, Marcello Giroletti, Takaaki Tanaka, F. Piron, A. Snyder, Keith Bechtol, Johan Bregeon, Johann Cohen-Tanugi, Alice Allafort, Roberto Mignani, Eric Charles, Julie McEnery, Morihiro Hayashida, E. Hays, Steven Ritz, D. J. Suson, C. C. Cheung, W. McConville, L. C. Reyes, Marco Ajello, J. B. Thayer, M. Naumann-Godo, L. Tibaldo, W. B. Atwood, J. S. Perkins, Nicola Giglietto, F. Gargano, Luca Latronico, G. A. Caliandro, H. Poon, S. Colafrancesco, M. N. Lovellette, P. A. Caraveo, Persis S. Drell, M. Tinivella, Elizabeth C. Ferrara, V. Pelassa, E. J. Siskind, J. H. Panetta, Markus Ackermann, A. N. Cillis, R. A. Cameron, Luca Baldini, M. Pierbattista, Denis Bastieri, A. von Kienlin, C. Romoli, J. Lande, Sylvain Guiriec, A. Reimer, S. Buson, P. M. Saz Parkinson, Suk-Han Lee, Melissa Pesce-Rollins, T. Glanzman, Jürgen Knödlseder, G. Pivato, Eugenio Bottacini, Charles D. Dermer, X. Hou, Giacomo Vianello, Ronaldo Bellazzini, Astrophysique Interprétation Modélisation (AIM (UMR_7158 / UMR_E_9005 / UM_112)), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris Diderot - Paris 7 (UPD7), Laboratoire Leprince-Ringuet (LLR), Centre National de la Recherche Scientifique (CNRS)-École polytechnique (X)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3), Commonwealth Scientific and Industrial Research Organisation [Canberra] (CSIRO), Istituto Nazionale di Fisica Nucleare, sezione di Bari (INFN, sezione di Bari), Istituto Nazionale di Fisica Nucleare (INFN), GLAST, Centre d'Etudes Nucléaires de Bordeaux Gradignan (CENBG), Université Sciences et Technologies - Bordeaux 1-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Université Sciences et Technologies - Bordeaux 1-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Laboratoire Univers et Particules de Montpellier (LUPM), Université Montpellier 2 - Sciences et Techniques (UM2)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université de Montpellier (UM)-Centre National de la Recherche Scientifique (CNRS), Ackermann, M., Ajello, M., Allafort, A., Asano, K., Atwood, W. B., Baldini, L., Ballet, J., BARBIELLINI AMIDEI, Guido, Bastieri, D., Bechtol, K., Bellazzini, R., Bloom, E. D., Bonamente, E., Borgland, A. W., Bottacini, E., Brandt, T. J., Bregeon, J., Brigida, M., Bruel, P., Buehler, R., Burnett, T. H., Busetto, G., Buson, S., Caliandro, G. A., Cameron, R. A., Caraveo, P. A., Casandjian, J. M., Cecchi, C., Charles, E., Chaty, S., Chekhtman, A., Cheung, C. C., Chiang, J., Cillis, A. N., Ciprini, S., Claus, R., Cohen Tanugi, J., Colafrancesco, S., Conrad, J., Cutini, S., D'Ammando, F., de Palma, F., Dermer, C. D., Silva, E. do Couto e., Drell, P. S., Drlica Wagner, A., Dubois, R., Favuzzi, C., Fegan, S. J., Ferrara, E. C., Focke, W. B., Fortin, P., Fukazawa, Y., Funk, S., Fusco, P., Gargano, F., Gasparrini, D., Gehrels, N., Germani, S., Giglietto, N., Giordano, F., Giroletti, M., Glanzman, T., Godfrey, G., Grandi, P., Grenier, I. A., Grove, J. E., Guiriec, S., Hadasch, D., Hayashida, M., Hays, E., Horan, D., Hou, X., Hughes, R. E., Jackson, M. S., Jogler, T., Jóhannesson, G., Johnson, R. P., Johnson, A. S., Kamae, T., Kataoka, J., Kerr, M., Knödlseder, J., Kuss, M., Lande, J., Larsson, S., Latronico, L., Lavalley, C., Lee, S. H., Longo, Francesco, Loparco, F., Lott, B., Lovellette, M. N., Lubrano, P., Mazziotta, M. N., Mcconville, W., Mcenery, J. E., Mehault, J., Michelson, P. F., Mignani, R. P., Mitthumsiri, W., Mizuno, T., Moiseev, A. A., Monte, C., Monzani, M. E., Morselli, A., Moskalenko, I. V., Murgia, S., Naumann Godo, M., Nemmen, R., Nishino, S., Norris, J. P., Nuss, E., Ohsugi, T., Omodei, N., Orienti, M., Orlando, E., Ormes, J. F., Paneque, D., Panetta, J. H., Pelassa, V., Perkins, J. S., Pesce Rollins, M., Pierbattista, M., Piron, F., Pivato, G., Poon, H., Porter, T. A., Rainò, S., Rando, R., Razzano, M., Razzaque, S., Reimer, A., Reimer, O., Reyes, L. C., Ritz, S., Rochester, L. S., Romoli, C., Roth, M., Sanchez, D. A., Saz Parkinson, P. M., Scargle, J. D., Sgrò, C., Siskind, E. J., Snyder, A., Spandre, G., Spinelli, P., Stephens, T. E., Suson, D. J., Tajima, H., Takahashi, H., Tanaka, T., Thayer, J. G., Thayer, J. B., Thompson, D. J., Tibaldo, L., Tibolla, O., Tinivella, M., Tosti, G., Troja, E., Usher, T. L., Vandenbroucke, J., Vasileiou, V., Vianello, G., Vitale, V., von Kienlin, A., Waite, A. P., Wallace, E., Weltevrede, P., Winer, B. L., Wood, K. S., Wood, M., Yang, Z., Zimmer, S., Astrophysique Interprétation Modélisation (AIM (UMR7158 / UMR_E_9005 / UM_112)), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-École polytechnique (X)-Centre National de la Recherche Scientifique (CNRS), Université Sciences et Technologies - Bordeaux 1 (UB)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Université Sciences et Technologies - Bordeaux 1 (UB)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Université Montpellier 2 - Sciences et Techniques (UM2)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Ackermann M, Ajello M, Allafort A, Asano K, Atwood WB, Baldini L, Ballet J, Barbiellini G, Bastieri D, Bechtol K, Bellazzini R, Bloom ED, Bonamente E, Borgland AW, Bottacini E, Brandt TJ, Bregeon J, Brigida M, Bruel P, Buehler R, Burnett TH, Busetto G, Buson S, Caliandro GA, Cameron RA, Caraveo PA, Casandjian JM, Cecchi C, Charles E, Chaty S, Chekhtman A, Cheung CC, Chiang J, Cillis AN, Ciprini S, Claus R, Cohen-Tanugi J, Colafrancesco S, Conrad J, Cutini S, DAmmando F, de Palma F, Dermer CD, Silva EDE, Drell S, Drlica-Wagner A, Dubois R, Favuzzi C, Fegan SJ, Ferrara EC, Focke WB, Fortin P, Fukazawa Y, Funk S, Fusco P, Gargano F, Gasparrini D, Gehrels N, Germani S, Giglietto N, Giordano F, Giroletti M, Glanzman T, Godfrey G, Grandi P, Grenier IA, Grove JE, Guiriec S, Hadasch D, Hayashida M, Hays E, Horan D, Hou X, Hughes RE, Jackson MS, Jogler T, Johannesson G, Johnson RP, Johnson AS, Kamae T, Kataoka J, Kerr M, Knodlseder J, Kuss M, Lande J, Larsson S, Latronico L, Lavalley C, Lee SH, Longo F, Loparco F, Lott B, Lovellette MN, Lubrano P, Mazziotta MN, McConville W, McEnery JE, Mehault J, Michelson PF, Mignani RP, Mitthumsiri W, Mizuno T, Moiseev AA, Monte C, Monzani ME, Morselli A, Moskalenko IV, Murgia S, Naumann-Godo M, Nemmen R, Nishino S, Norris JP, Nuss E, Ohsugi T, Omodei N, Orienti M, Orlando E, Ormes JF, Paneque D, Panetta JH, Pelassa V, Perkins JS, Pesce-Rollins M, Pierbattista M, Piron F, Pivato G, Poon H, Porter TA, Raino S, Rando R, Razzano M, Razzaque S, Reimer A, Reimer O, Reyes LC, Ritz S, Rochester LS, Romoli C, Roth M, Sanchez DA, Parkinson PMS, Scargle JD, Sgro C, Siskind EJ, Snyder A, Spandre G, Spinelli P, Stephens TE, Suson DJ, Tajima H, Takahashi H, Tanaka T, Thayer JG, Thayer JB, Thompson DJ, Tibaldo L, Tibolla O, Tinivella M, Tosti G, Troja E, Usher TL, Vandenbroucke J, Vasileiou V, Vianello G, Vitale V, von Kienlin A, Waite AP, Wallace E, Weltevrede P, Winer BL, Wood KS, Wood M, Yang Z, Zimmer S, National Institute for Nuclear Physics (INFN), and Université de Montpellier (UM)-Université Montpellier 2 - Sciences et Techniques (UM2)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)

Subjects
Ciencias Físicas, EXTRAGALACTIC MAGNETIC-FIELDS, halo [galaxies], galaxies: halos, Astrophysics, 01 natural sciences, galaxies, [gamma rays], law.invention, Spitzer Space Telescope, law, 1ES 0229+200, SPACE-TELESCOPE, 010303 astronomy & astrophysics, Physics, TEV BLAZARS, detector [instrumentation], [SDU.ASTR.HE]Sciences of the Universe [physics]/Astrophysics [astro-ph]/High Energy Astrophysical Phenomena [astro-ph.HE], Astrophysics::Instrumentation and Methods for Astrophysics, detectors, intergalactic medium [instrumentation], VHE GAMMA-RAYS, galaxies: active – galaxies: halos – gamma rays: galaxies – instrumentation: detectors – intergalactic medium, halos [galaxies], active [galaxies], intergalactic medium, Astrophysics - High Energy Astrophysical Phenomena, CIENCIAS NATURALES Y EXACTAS, Point spread function, [PHYS.ASTR.HE]Physics [physics]/Astrophysics [astro-ph]/High Energy Astrophysical Phenomena [astro-ph.HE], Active galactic nucleus, Astrophysics::High Energy Astrophysical Phenomena, galaxies: active, Astrophysics::Cosmology and Extragalactic Astrophysics, Telescope, 0103 physical sciences, gamma rays: galaxies, instrumentation: detectors, galaxie [gamma rays], Blazar, SOURCE CATALOG, Astrophysics::Galaxy Astrophysics, BACKGROUND LIGHT, 010308 nuclear & particles physics, Astronomy, CONSTRAINTS, Astronomy and Astrophysics, Quasar, PULSAR, Galaxy, DISCOVERY, Astronomía, Space and Planetary Science, ddc:520, Fermi Gamma-ray Space Telescope
Abstract

The astrophysical journal 765(1), 54 (2013). doi:10.1088/0004-637X/765/1/54, The Large Area Telescope (LAT) on the Fermi Gamma-ray Space Telescope is a pair-conversion telescope designed to detect photons with energies from ≈20 MeV to >300 GeV. The pre-launch response functions of the LAT were determined through extensive Monte Carlo simulations and beam tests. The point-spread function (PSF) characterizing the angular distribution of reconstructed photons as a function of energy and geometry in the detector is determined here from two years of on-orbit data by examining the distributions of γ rays from pulsars and active galactic nuclei (AGNs). Above 3 GeV, the PSF is found to be broader than the pre-launch PSF. We checked for dependence of the PSF on the class of γ-ray source and observation epoch and found none. We also investigated several possible spatial models for pair-halo emission around BL Lac AGNs. We found no evidence for a component with spatial extension larger than the PSF and set upper limits on the amplitude of halo emission in stacked images of low- and high-redshift BL Lac AGNs and the TeV blazars 1ES0229+200 and 1ES0347–121, Published by Univ.11032, Chicago, Ill. [u.a.]

Published
2013

16. FERMI LARGE AREA TELESCOPE OBSERVATIONS OF THE SUPERNOVA REMNANT G8.7-0.1

Author

Hartmut Sadrozinski, R. A. Cameron, Stefano Ciprini, Marco Ajello, J. B. Thayer, Sho Nishino, Jay P. Norris, Akira Okumura, T. A. Porter, Pascal Bruel, T. Ohsugi, Eleonora Troja, Gloria Spandre, Gudlaugur Johannesson, Elliott D. Bloom, Alex Drlica-Wagner, K. Hayashi, D. Parent, S. Buson, E. Hays, R. Buehler, Luca Latronico, T. Glanzman, Johann Cohen-Tanugi, S. Murgia, Stephan Zimmer, Roger Blandford, F. Piron, Peter F. Michelson, Marcello Giroletti, Justin Vandenbroucke, M. Roth, Guido Barbiellini, Nicola Omodei, G. Godfrey, Zhenwei Yang, Carmelo Sgrò, Riccardo Rando, Yasuo Fukui, A. De Angelis, G. Tosti, R. Dubois, W. B. Focke, V. Pelassa, E. Nuss, David Paneque, M. Ohno, M. E. Monzani, M. Kuss, Alice K. Harding, P. Spinelli, Francesco Giordano, Hideaki Katagiri, F. de Palma, Melissa Pesce-Rollins, A. Van Etten, Igor V. Moskalenko, M. Frailis, Elizabeth C. Ferrara, G. A. Caliandro, Jonathan F. Ormes, Olaf Reimer, E. Do Couto E Silva, B. Berenji, Ryo Yamazaki, Giacomo Vianello, A. Morselli, Hiromitsu Takahashi, V. Vitale, D. Hadasch, Keith Bechtol, S. Rainò, M. Brigida, Tsunefumi Mizuno, Hajimu Yasuda, Francesco Longo, C. Favuzzi, Jürgen Knödlseder, E. Orlando, Takeshi Nakamori, J. M. Casandjian, A. Tramacere, R. Claus, Hiroaki Yamamoto, Hiroyasu Tajima, J. Bregeon, Ryosuke Itoh, Nicola Giglietto, P. L. Nolan, J. E. Grove, Yasushi Fukazawa, Takaaki Tanaka, A. P. Waite, S. Germani, Brian L Winer, Shiu-Hang Lee, Ronaldo Bellazzini, Andrea Lionetto, M. N. Lovellette, Dario Gasparrini, Diego F. Torres, Hidetoshi Kubo, P. A. Caraveo, Alice Allafort, P. Fusco, Persis S. Drell, Paolo Giommi, C. Monte, T. Kamae, V. Vasileiou, J. G. Thayer, T. L. Usher, A. A. Moiseev, Yasunobu Uchiyama, Jun Kataoka, S. J. Fegan, J. Mehault, Luca Baldini, A. Reimer, M. Naumann-Godo, Charles D. Dermer, E. J. Siskind, M. Pierbattista, A. S. Johnson, S. Cutini, Claudia Cecchi, F. Loparco, P. Wang, Denis Bastieri, Emanuele Bonamente, J. Lande, Sylvain Guiriec, K. S. Wood, L. Tibaldo, O. Tibolla, N. Vilchez, Y. Hanabata, F. Gargano, P. D. Smith, T. Reposeur, A. W. Borgland, T. Uehara, M. Ziegler, M. N. Mazziotta, A. Chekhtman, P. Lubrano, Eric Charles, D. J. Suson, Jean Ballet, Ajello, M., Allafort, A., Baldini, L., Ballet, J., Barbiellini, G., Bastieri, D., Bechtol, K., Bellazzini, R., Berenji, B., Blandford, R. D., Bloom, E. D., Bonamente, E., Borgland, A. W., Bregeon, J., Brigida, M., Bruel, P., Buehler, R., Buson, S., Caliandro, G. A., Cameron, R. A., Caraveo, P. A., Casandjian, J. M., Cecchi, C., Charles, E., Chekhtman, A., Ciprini, S., Claus, R., Cohen Tanugi, J., Cutini, S., Angelis, A., Palma, F., Dermer, C. D., E. d. C., Drell, P. S., Drlica Wagner, A., Dubois, R., Favuzzi, C., Fegan, S. J., Ferrara, E. C., Focke, W. B., Frailis, M., Fukazawa, Y., Fukui, Y., Fusco, P., Gargano, F., Gasparrini, D., Germani, S., Giglietto, N., Giommi, P., Giordano, F., Giroletti, M., Glanzman, T., Godfrey, G., Grove, J. E., Guiriec, S., Hadasch, D., Hanabata, Y., Harding, A. K., Hayashi, K., Hays, E., Itoh, R., Johannesson, G., Johnson, A. S., Kamae, T., Katagiri, H., Kataoka, J., Kn\odlseder, J., Kubo, H., Kuss, M., Lande, J., Latronico, L., Lee, S., Lionetto, A. M., Longo, Francesco, Loparco, F., Lovellette, M. N., Lubrano, P., Mazziotta, M. N., Mehault, J., Michelson, P. F., Mizuno, T., Moiseev, A. A., Monte, C., Monzani, M. E., Morselli, A., Moskalenko, I. V., Murgia, S., Nakamori, T., Naumann Godo, M., Nishino, S., Nolan, P. L., Norris, J. P., Nuss, E., Ohno, M., Ohsugi, T., Okumura, A., Omodei, N., Orlando, E., Ormes, J. F., Paneque, D., Parent, D., Pelassa, V., Pesce Rollins, M., Pierbattista, M., Piron, F., Porter, T. A., Rain\`o, S., Rando, R., Reimer, A., Reimer, O., Reposeur, T., Roth, M., Sadrozinski, H. F., Sgr\`o, C., Siskind, E. J., Smith, P. D., Spandre, G., Spinelli, P., Suson, D. J., Tajima, H., Takahashi, H., Tanaka, T., Thayer, J. G., Thayer, J. B., Tibaldo, L., Tibolla, O., Torres, D. F., Tosti, G., Tramacere, A., Troja, E., Uchiyama, Y., Uehara, T., Usher, T. L., Vandenbroucke, J., Etten, A., Vasileiou, V., Vianello, G., Vilchez, N., Vitale, V., Waite, A. P., Wang, P., Winer, B. L., Wood, K. S., Yamamoto, H., Yamazaki, R., Yang, Z., Yasuda, H., Ziegler, M., Zimmer, S., Astrophysique Interprétation Modélisation (AIM (UMR_7158 / UMR_E_9005 / UM_112)), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris Diderot - Paris 7 (UPD7), Laboratoire Leprince-Ringuet (LLR), Centre National de la Recherche Scientifique (CNRS)-École polytechnique (X)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3), Laboratoire Univers et Particules de Montpellier (LUPM), Centre National de la Recherche Scientifique (CNRS)-Université de Montpellier (UM)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Montpellier 2 - Sciences et Techniques (UM2), Institut de recherche en astrophysique et planétologie (IRAP), Institut national des sciences de l'Univers (INSU - CNRS)-Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Observatoire Midi-Pyrénées (OMP), Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Centre National de la Recherche Scientifique (CNRS), GLAST, Centre d'Etudes Nucléaires de Bordeaux Gradignan (CENBG), Université Sciences et Technologies - Bordeaux 1-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Université Sciences et Technologies - Bordeaux 1-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Université Montpellier 2 - Sciences et Techniques (UM2)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université de Montpellier (UM)-Centre National de la Recherche Scientifique (CNRS), Astrophysique Interprétation Modélisation (AIM (UMR7158 / UMR_E_9005 / UM_112)), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-École polytechnique (X)-Centre National de la Recherche Scientifique (CNRS), Université Montpellier 2 - Sciences et Techniques (UM2)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire Midi-Pyrénées (OMP), Institut de Recherche pour le Développement (IRD)-Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Institut de Recherche pour le Développement (IRD)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Centre National de la Recherche Scientifique (CNRS), Université Sciences et Technologies - Bordeaux 1 (UB)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Université Sciences et Technologies - Bordeaux 1 (UB)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Université de Montpellier (UM)-Université Montpellier 2 - Sciences et Techniques (UM2)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), and Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)

Subjects
[PHYS.ASTR.HE]Physics [physics]/Astrophysics [astro-ph]/High Energy Astrophysical Phenomena [astro-ph.HE], Astrophysics::High Energy Astrophysical Phenomena, Cosmic ray, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, acceleration of particles, cosmic rays, gamma rays, ISM, ISM: individual objects (G8.7–0.1, HESS J1804–216), ISM: supernova remnants, Spectral line, Particle decay, individual objects: G8.7{\ndash}0.1 HESS J1804{\ndash}216 [ISM], gamma rays: ISM, ISM: individual objects (G8.7?0.1, ISM [gamma rays], ISM: individual objects (G8.7?0.1, HESS J1804?216), Astronomy and Astrophysics, Space and Planetary Science, 0103 physical sciences, 14. Life underwater, Supernova remnant, ISM: individual objects (G8.7-0.1, 010303 astronomy & astrophysics, acceleration of particle, cosmic ray, Astrophysics::Galaxy Astrophysics, Acceleration of particles, ISM: individual objects (G8.7-0.1, HESS J1804-216), Physics, Spectral index, HESS J1804-216), 010308 nuclear & particles physics, [SDU.ASTR.HE]Sciences of the Universe [physics]/Astrophysics [astro-ph]/High Energy Astrophysical Phenomena [astro-ph.HE], supernova remnants [ISM], Astronomy, Gamma-ray astronomy, ISM: individual objects: G8.7{\ndash}0.1 HESS J1804{\ndash}216, Interstellar medium, HESS J1804?216), High Energy Physics::Experiment, Astrophysics - High Energy Astrophysical Phenomena, Fermi Gamma-ray Space Telescope
Abstract

We present a detailed analysis of the GeV gamma-ray emission toward the supernova remnant (SNR) G8.7-0.1 with the Large Area Telescope (LAT) onboard the \emph{Fermi} Gamma-ray Space Telescope. An investigation of the relationship among G8.7-0.1 and the TeV unidentified source HESS J1804-216 provides us with an important clue on diffusion process of cosmic rays if particle acceleration operates in the SNR. The GeV gamma-ray emission is extended with most of the emission in positional coincidence with the SNR G8.7-0.1 and a lesser part located outside the western boundary of G8.7-0.1. The region of the gamma-ray emission overlaps spatially-connected molecular clouds, implying a physical connection for the gamma-ray structure. The total gamma-ray spectrum measured with LAT from 200 MeV--100 GeV can be described by a broken power-law function with a break of 2.4 $\pm$ 0.6 (stat) $\pm$ 1.2 (sys) GeV, and photon indices of 2.10 $\pm$ 0.06 (stat) $\pm$ 0.10 (sys) below the break and 2.70 $\pm$ 0.12 (stat) $\pm$ 0.14 (sys) above the break. Given the spatial association among the gamma rays, the radio emission of G8.7$-$0.1, and the molecular clouds, the decay of $\pi^{0}$s produced by particles accelerated in the SNR and hitting the molecular clouds naturally explains the GeV gamma-ray spectrum. We also find that the GeV morphology is not well represented by the TeV emission from HESS J1804$-$216 and that the spectrum in the GeV band is not consistent with the extrapolation of the TeV gamma-ray spectrum. The spectral index of the TeV emission is consistent with the particle spectral index predicted by a theory that assumes energy-dependent diffusion of particles accelerated in an SNR. We discuss the possibility that the TeV spectrum originates from the interaction of particles accelerated in G8.7$-$0.1 with molecular clouds, and we constrain the diffusion coefficient of the particles., Comment: 42 pages, 5 figures. Accepted for publication in the Astrophysical Journal. Corresponding authors: Y. Hanabata, H. Katagiri

Published
2012

17. Suzaku view of X-ray Spectral Variability of the Radio Galaxy Centaurus A : Partial Covering Absorber, Reflector, and Possible Jet Component

Author

Yasushi Fukazawa, Kazuyoshi Hiragi, Syoko Yamazaki, Motohiro Mizuno, Kazuma Hayashi, Katsuhiro Hayashi, Sho Nishino, Hiromitsu Takahashi, and Masanori Ohno

Subjects
Photon, Radio galaxy, Astrophysics::High Energy Astrophysical Phenomena, Centaurus A, galaxies: active, FOS: Physical sciences, Astrophysics, galaxies: individual (Centaurus A), Spectral line, Seyfert [galaxies], Active phase, Physics, High Energy Astrophysical Phenomena (astro-ph.HE), individual (Centaurus A) [galaxies], X-ray, Astronomy and Astrophysics, galaxies: Seyfert, galaxies [X-rays], X-rays: galaxies, Space and Planetary Science, active [galaxies], Linear relation, Astrophysics - High Energy Astrophysical Phenomena, Fermi Gamma-ray Space Telescope
Abstract

We observed a nearby radio galaxy, the Centaurus A (Cen A), three times with Suzaku in 2009, and measured the wide-band X-ray spectral variability more accurately than the previous measurements. The Cen A was in the active phase in 2009, and the flux became higher by a factor of 1.5--2.0 and the spectrum became harder than that in 2005. The Fe-K line intensity increased by 20--30% from 2005 to 2009. The correlation of the count rate between the XIS 3--8 keV and PIN 15--40 keV band showed a complex behavior with a deviation from a linear relation. The wide-band X-ray continuum in 2--200 keV can be fitted with an absorbed powerlaw model plus a reflection component, or a powerlaw with a partial covering Compton-thick absorption. The difference spectra between high and low flux periods in each observation were reproduced by a powerlaw with a partial covering Compton-thick absorption. Such a Compton-thick partial covering absorber was for the first time observed for the Cen A. The powerlaw photon index of the difference spectra in 2009 is almost the same as that of the time-averaged spectra in 2005, but steeper by $\sim0.2$ than that of the time-averaged spectra in 2009. This suggests an additional hard powerlaw component with a photon index of $, 43 pages, 16 figures, will appear in the ApJ

Published
2011

18. On-orbit calibration status of the hard x-ray detector (HXD) onboard Suzaku

Author

Shinya Yamada, Hiromitsu Takahashi, Sho Nishino, Yukikatsu Terada, Tsunefumi Mizuno, K. Hayashi, Yasushi Fukazawa, Shigeto Watanabe, Madoka Kawaharada, Motohide Kokubun, M. Mizuno, Koji Nakazawa, Kazuyoshi Hiragi, and Takaaki Tanaka

Subjects
Physics, Physics::Instrumentation and Detectors, business.industry, Astrophysics::High Energy Astrophysical Phenomena, Detector, X-ray detector, Shields, Scintillator, Orbital mechanics, Optics, Observatory, Calibration, business, Diode
Abstract

Hard X-ray Detector (HXD) onboard Suzaku, the Japanese 5th X-ray observatory, consists of 64 PIN photo diodes with 2 mm thickness (10-70 keV) and 16 phoswich detectors using 5 mm-thick GSO scintillators and BGO active collimators (40-600 keV), and these are surrounded by 20 units of BGO Active shields. All the detector units have been working well with no significant troubles in four and a half years since the launch on July 2005, and given many important scientific results. In this paper, we report the recent status of on-orbit calibrations for PIN/GSO detectors. For the PIN, analog/digital threshold levels of both in-orbit and on-ground are raised up to avoid the increasing noise events due to in-orbit radiation damage. For the GSO, the accuracy of the energy scale and modeling of gain variations are improved, and newly calibrated data set including background files and response matrices are released on April 2010.

Published
2010

19. Study of the Large-scale Temperature Structure of the Perseus Cluster with Suzaku

Author

Yasushi Fukazawa, Sho Nishino, Takaaki Tanaka, Kazuhiro Nakazawa, and Katsuhiro Hayashi

Subjects
Physics, Perseus Cluster, Astrophysics::High Energy Astrophysical Phenomena, FOS: Physical sciences, Astronomy and Astrophysics, Collimator, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, Central region, Astrophysics - Astrophysics of Galaxies, law.invention, Cluster of Galaxies, X-ray, Suzaku, Space and Planetary Science, law, Astrophysics of Galaxies (astro-ph.GA), Spectral analysis, Galaxy cluster, Astrophysics::Galaxy Astrophysics
Abstract

The 3rd Suzaku international Conference "Energetic Cosmos : from Suzaku to ASTRO-H" (June 29-July 2, 2009. Grand Park Otaru Hotel), Otaru, Hokkaido Japan, We report the study of the large-scale temperature structure of the Perseus cluster with Suzaku. We performed Suzaku observations of the Perseus cluster with four pointings of 30' offset from the cluster center, together with the observation of the central region, in order to investigate the temperature of the outer region, with the Hard X-ray Detector (HXD: 10 - 60 keV). We performed the spectral analysis of the Perseus cluster with a model of the temperature structure, by considering the collimator response of the PIN correctly. As a result, we found that the upper limit of the temperature in the outer region is approximately 14 keV, and an extreme hot gas, that was reported for RXJ 1347.5-1145 and A 3667, was not found in the Perseus cluster. This indicates that the Perseus cluster has not recently experienced a major merger., Meeting sponsors: The University of Tokyo, The Institute of Physical and Chemical Research, The Japan Society for the Promotion of Science, 資料番号: AA0064574034, レポート番号: JAXA-SP-09-008E

Published
2010

20. Gamma -ray Spectral Evolution of NGC 1275 observed with Fermi large area telescope

Author

Yasushi Fukazawa, Sho Nishino, E. Cavazzuti, D. J. Thompson, Jun Kataoka, Annalisa Celotti, C. C. Cheung, G. Tosti, Lukasz Stawarz, and W. McConville

Subjects
Physics, Photon, Radio galaxy, Astrophysics::High Energy Astrophysical Phenomena, individual (NGC 1275) [galaxies], galaxies: active, Gamma ray, jets [galaxies], Flux, Astronomy and Astrophysics, galaxies: individual (NGC 1275), galaxies: jets, gamma rays: general, radiation mechanisms: non-thermal, Radius, Astrophysics, Photon energy, non-thermal [radiation mechanisms], Settore FIS/05 - Astronomia e Astrofisica, Space and Planetary Science, active [galaxies], Blazar, general [gamma rays], Fermi Gamma-ray Space Telescope
Abstract

We report on a detailed investigation of the high-energy gamma-ray emission from NGC\,1275, a well-known radio galaxy hosted by a giant elliptical located at the center of the nearby Perseus cluster. With the increased photon statistics, the center of the gamma-ray emitting region is now measured to be separated by only 0.46' from the nucleus of NGC1275, well within the 95% confidence error circle with radius ~1.5'. Early Fermi-LAT observations revealed a significant decade-timescale brightening of NGC1275 at GeV photon energies, with a flux about seven times higher than the one implied by the upper limit from previous EGRET observations. With the accumulation of one-year of Fermi-LAT all-sky-survey exposure, we now detect flux and spectral variations of this source on month timescales, as reported in this paper. The average >100 MeV gamma-ray spectrum of NGC1275 shows a possible deviation from a simple power-law shape, indicating a spectral cut-off around an observed photon energy of E = 42.2+-19.6 GeV, with an average flux of F = (2.31+-0.13) X 10^{-7} ph/cm^2/s and a power-law photon index, Gamma = 2.13+-0.02. The largest gamma-ray flaring event was observed in April--May 2009 and was accompanied by significant spectral variability above E > 1-2 GeV. The gamma-ray activity of NGC1275 during this flare can be described by a hysteresis behavior in the flux versus photon index plane. The highest energy photon associated with the gamma-ray source was detected at the very end of the observation, with the observed energy of E = 67.4GeV and an angular separation of about 2.4' from the nucleus. In this paper we present the details of the Fermi-LAT data analysis, and briefly discuss the implications of the observed gamma-ray spectral evolution of NGC1275 in the context of gamma-ray blazar sources in general.

Published
2010

21. The On-orbit Calibrations for the Fermi Large Area Telescope

Author

Luca Baldini, M. Hakimi, N. Saggini, Wlodzimierz Klamra, Roger W. Romani, Staffan Carius, G. Busetto, Brian L Winer, M. Ceccanti, Carmelo Sgrò, L. Guillemot, S. Cutini, A. A. Moiseev, David Paneque, M. Campell, M. Kuss, M. Mongelli, P. Fleury, Michele Pinchera, J. M. Casandjian, C. Meurer, A. Makeev, F. Belli, G. Mazzenga, Melissa Pesce-Rollins, N. Virmani, H. Kelly, Hiromitsu Takahashi, F. Gargano, M. E. Monzani, Luca Latronico, R. E. Hughes, F. Loparco, W. Mitthumsiri, David Sanchez, Keith Bechtol, S. Ritz, Charles D. Dermer, P. Bourgeois, R. Chipaux, E. Do Couto E Silva, G. Godfrey, P. Dizon, Francesco Longo, P. Picozza, Hartmut Sadrozinski, A. Sacchetti, Shiu-Hang Lee, Elena Moretti, A. P. Waite, F. Bellardi, Stefan Funk, Elizabeth C. Ferrara, M.M. Massai, E. Orlando, Brandon Anderson, Sho Nishino, A. Kavelaars, Y. Edmonds, Jean Ballet, A. Tramacere, D. Fabiani, D. L. Wood, Christian Farnier, Takaaki Tanaka, Stefano Ciprini, M. Ozaki, Nicola Omodei, B. Marangelli, T. H. Burnett, Denis Bastieri, D. J. Thompson, Elliott D. Bloom, B. M. Baughman, F. de Palma, J. Bartelt, E. J. Siskind, J. R. Bogart, J. Goodman, T. Ylinen, D. Freytag, M. Ziegler, W. N. Johnson, D. Parent, S. Murgia, T. Ohsugi, Dario Bisello, Massimo Minuti, Alessandro Brez, A. Chekhtman, J. H. Panetta, F. Kuehn, P. L. Nolan, Magnus Axelsson, V. Pelassa, N. Vilchez, Markus Ackermann, S. Germani, F. Piron, G. M. Madejski, A. N. Cillis, Masanori Ohno, S. McGlynn, R. Dubois, Marianne Lemoine-Goumard, Robin H. D. Corbet, W. B. Focke, D. L. Flath, Sylvain Guiriec, A. Sander, T. A. Porter, P. Spinelli, M. Razzano, Eric Nuss, David A. Smith, S. Condamoor, Julie McEnery, L. C. Reyes, S. Robinson, Francesco Giordano, Neil Gehrels, P. Hascall, A. Reimer, L.L. Wai, W. Raynor, Tyrel J. Johnson, T. Kamae, R. A. Cameron, Ronaldo Bellazzini, K. Fouts, P. Lubrano, P. M. Saz Parkinson, P. Bruel, M. Turri, K. S. Wood, C. C. Cheung, M. Roth, O. Ferreira, Martin Kocian, A. De Angelis, Jürgen Knödlseder, G. Tosti, N. Mirizzi, M. Brigida, Y. Hanabata, Igor V. Moskalenko, P. Mitra, J. G. Thayer, Olaf Reimer, T. E. Stephens, D. Bédérède, B. Giebels, B. Berenji, T. Reposeur, D. Dumora, M. Huffer, A. W. Borgland, C. Lavalley, Gudlaugur Johannesson, Elisabetta Bissaldi, J. Ampe, Felix Ryde, G. A. Caliandro, Andrew W. Strong, Guido Barbiellini, C. Favuzzi, M. Frailis, L. S. Rochester, Marco Ajello, J. B. Thayer, A. Tenze, O. Tibolla, L. Tibaldo, P. Wang, G. Bogaert, Emanuele Bonamente, T. L. Usher, Eric Charles, A. Y. Rodriguez, David S. Davis, D. J. Suson, Tadayuki Takahashi, B. Leas, Z. Fewtrell, W. B. Atwood, Seth Digel, Nicola Giglietto, M. N. Mazziotta, P. A. Hart, Alessandro Paccagnella, L. Nilsson, A. Sellerholm, E. Hays, James Chiang, P. Carlson, M. N. Lovellette, P. A. Caraveo, Persis S. Drell, Gunther Haller, Hideaki Katagiri, Claudia Cecchi, D. Nelson, Johann Cohen-Tanugi, M. S. Strickman, Jean-Luc Starck, R. Claus, E. Rapposelli, A. Morselli, V. Vitale, M.-H. Grondin, J. F. Ormes, J. Bregeon, Hiroyasu Tajima, B. Lee, Jan Conrad, L. Sapozhnikov, M. Marchetti, P. D. Smith, Peter F. Michelson, A. A. Abdo, R. Bagagli, D. May, A. Bouvier, Dario Gasparrini, C. Monte, D.K. Lung, Jun Kataoka, M. Deklotz, Diego F. Torres, I. A. Grenier, A. S. Johnson, E. Cavazzuti, Robert R. Rando, M. Dormody, T. Glanzman, Benoit Lott, M. Pepe, P. Fusco, M. Sugizaki, Gloria Spandre, Matthew Kerr, S. Rainò, Tsunefumi Mizuno, Hajimu Yasuda, R. P. Johnson, J. E. Grove, Yasushi Fukazawa, O.H. Saxton, Astrophysique Interprétation Modélisation (AIM (UMR_7158 / UMR_E_9005 / UM_112)), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris Diderot - Paris 7 (UPD7), Institut de Recherches sur les lois Fondamentales de l'Univers (IRFU), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay, Laboratoire Leprince-Ringuet (LLR), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-École polytechnique (X)-Centre National de la Recherche Scientifique (CNRS), Laboratoire de Physique Théorique et Astroparticules (LPTA), Université Montpellier 2 - Sciences et Techniques (UM2)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Centre d'Etudes Nucléaires de Bordeaux Gradignan (CENBG), Université Sciences et Technologies - Bordeaux 1-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Centre d'étude spatiale des rayonnements (CESR), Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire Midi-Pyrénées (OMP), Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS), Fermi-LAT, Centre National de la Recherche Scientifique (CNRS)-École polytechnique (X)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3), Observatoire Midi-Pyrénées (OMP), Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées, Abdo, A. A., Ackermann, M., Ajello, M., Ampe, J., Anderson, B., Atwood, W. B., Axelsson, M., Bagagli, R., Baldini, L., Ballet, J., BARBIELLINI AMIDEI, Guido, Bartelt, J., Bastieri, D., Baughman, B. M., Bechtol, K., Bederede, D., Bellardi, F., Bellazzini, R., Belli, F., Berenji, B., Bisello, D., Bissaldi, Elisabetta, Bloom, E. D., Bogaert, G., Bogart, J. R., Bonamente, E., Borgland, A. W., Bourgeois, P., Bouvier, A., Bregeon, J., Brez, A., Brigida, M., Bruel, P., Burnett, T. H., Busetto, G., Caliandro, G. A., Cameron, R. A., Campell, M., Caraveo, P. A., Carius, S., Carlson, P., Casandjian, J. M., Cavazzuti, E., Ceccanti, M., Cecchi, C., Charles, E., Chekhtman, A., Cheung, C. C., Chiang, J., Chipaux, R., Cillis, A. N., Ciprini, S., Claus, R., Cohen Tanugi, J., Condamoor, S., Conrad, J., Corbet, R., Cutini, S., Davis, D. S., Deklotz, M., Dermer, C. D., Angelis, A. d., Palma, F. d., Digel, S. W., Dizon, P., Dormody, M., Silva, E. D. E., Drell, P. S., Dubois, R., Dumora, D., Edmonds, Y., Fabiani, D., Farnier, C., Favuzzi, C., Ferrara, E. C., Ferreira, O., Fewtrell, Z., Flath, D. L., Fleury, P., Focke, W. B., Fouts, K., Frailis, M., Freytag, D., Fukazawa, Y., Funk, S., Fusco, P., Garganov, F., Gasparrini, D., Gehrelscao, N., Germani, S., Giebels, B., Giglietto, N., Giordano, F., Glanzman, T., Godfrey, G., Goodman, J., Grenier, I. A., Grondin, M. H., Grove, J. E., Guillemot, L., Guiriec, S., Hakimi, M., Haller, G., Hanabata, Y., Hart, P. A., Hascall, P., Hays, E., Huffer, M., Hughes, R. E., Johannesson, G., Johnson, A. S., Johnson, R. P., Johnson, T. J., Johnson, W. N., Kamae, T., Katagiri, H., Kataoka, J., Kavelaars, A., Kelly, H., Kerr, M., Klamra, W., Knodlseder, J., Kocian, M. L., Kuehn, F., Kuss, M., Latronico, L., Lavalley, C., Leas, B., Lee, B., Lee, S. H., Lemoine Goumard, M., Longo, Francesco, Loparco, F., Lott, B., Lovellette, M. N., Lubrano, P., Lung, D. K., Madejski, G. M., Makeev, A., Marangelli, B., Marchetti, M., Massai, M. M., May, D., Mazzenga, G., Mazziotta, M. N., Mcenery, J. E., Mcglynn, S., Meurer, C., Michelson, P. F., Minuti, M., Mirizzi, N., Mitra, P., Mitthumsiri, W., Mizuno, T., Moiseev, A. A., Mongelli, M., Monte, C., Monzani, M. E., Moretti, E., Morselli, A., Moskalenko, I. V., Murgia, S., Nelson, D., Nilsson, L., Nishino, S., Nolan, P. L., Nuss, E., Ohno, M., Ohsugi, T., Omodei, N., Orlando, E., Ormes, J. F., Ozaki, M., Paccagnella, A., Paneque, D., Panetta, J. H., Parent, D., Pelassa, V., Pepe, M., Pesce Rollins, M., Picozza, P., Pinchera, M., Piron, F., Porter, T. A., Raino, S., Rando, R., Rapposelli, E., Raynor, W., Razzano, M., Reimer, A., Reimer, O., Reposeur, T., Reyes, L. C., Ritz, S., Robinson, S., Rochester, L. S., Rodriguez, A. Y., Romani, R. W., Roth, M., Ryde, F., Sacchetti, A., Sadrozinski, H. F. W., Saggini, N., Sanchez, D., Sander, A., Sapozhnikov, L., Saxton, O. H., Parkinson, P. M. S., Sellerholm, A., Sgro, C., Siskind, E. J., Smith, D. A., Smith, P. D., Spandre, G., Spinelli, P., Starck, J. L., Stephens, T. E., Strickman, M. S., Strong, A. W., Sugizaki, M., Suson, D. J., Tajima, H., Takahashi, H., Takahashi, T., Tanaka, T., Tenze, A., Thayer, J. B., Thayer, J. G., Thompson, D. J., Tibaldo, L., Tibolla, O., Torres, D. F., Tosti, G., Tramacere, A., Turri, M., Usher, T. L., Vilchez, N., Virmani, N., Vitale, V., Wai, L. L., Waite, A. P., Wang, P., Winer, B. L., Wood, D. L., Wood, K. S., Yasuda, H., Ylinen, T., Ziegler, M., Astrophysique Interprétation Modélisation (AIM (UMR7158 / UMR_E_9005 / UM_112)), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Université Sciences et Technologies - Bordeaux 1 (UB)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire Midi-Pyrénées (OMP), Institut de Recherche pour le Développement (IRD)-Université Toulouse III - Paul Sabatier (UT3), and Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Institut de Recherche pour le Développement (IRD)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Centre National de la Recherche Scientifique (CNRS)

Subjects
[PHYS.ASTR.HE]Physics [physics]/Astrophysics [astro-ph]/High Energy Astrophysical Phenomena [astro-ph.HE], [PHYS.ASTR.IM]Physics [physics]/Astrophysics [astro-ph]/Instrumentation and Methods for Astrophysic [astro-ph.IM], Astrophysics::High Energy Astrophysical Phenomena, FOS: Physical sciences, Cosmic ray, Fermi satellite, 01 natural sciences, High Energy Gamma-ray Astronomy, GLAST, law.invention, Gamma-ray, Telescope, Spitzer Space Telescope, law, 07.87.+v, 95.55.Ka, 0103 physical sciences, Calibration, FGST, 010303 astronomy & astrophysics, Instrumentation and Methods for Astrophysics (astro-ph.IM), Fermi, LAT, Calibrations, Physics, High Energy Astrophysical Phenomena (astro-ph.HE), Spacecraft, 010308 nuclear & particles physics, business.industry, [SDU.ASTR.HE]Sciences of the Universe [physics]/Astrophysics [astro-ph]/High Energy Astrophysical Phenomena [astro-ph.HE], Detector, Astrophysics::Instrumentation and Methods for Astrophysics, Astronomy, Astronomy and Astrophysics, Detectors, South Atlantic Anomaly, [SDU.ASTR.IM]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Instrumentation and Methods for Astrophysic [astro-ph.IM], business, Astrophysics - Instrumentation and Methods for Astrophysics, Astrophysics - High Energy Astrophysical Phenomena, Fermi Gamma-ray Space Telescope
Abstract

The Large Area Telescope (LAT) on--board the Fermi Gamma ray Space Telescope began its on--orbit operations on June 23, 2008. Calibrations, defined in a generic sense, correspond to synchronization of trigger signals, optimization of delays for latching data, determination of detector thresholds, gains and responses, evaluation of the perimeter of the South Atlantic Anomaly (SAA), measurements of live time, of absolute time, and internal and spacecraft boresight alignments. Here we describe on orbit calibration results obtained using known astrophysical sources, galactic cosmic rays, and charge injection into the front-end electronics of each detector. Instrument response functions will be described in a separate publication. This paper demonstrates the stability of calibrations and describes minor changes observed since launch. These results have been used to calibrate the LAT datasets to be publicly released in August 2009., 60 pages, 34 figures, submitted to Astroparticle Physics

Published
2009

22. The Soft Gamma-ray Detector for the ASTRO-H mission

Author

J. Harayama, S. Sasaki, H. Tajima, T. Miura, Roger Blandford, S. Sugimoto, Kazutaka Yamaoka, T. Takahashi, Hiroyuki Nishioka, Jun Kataoka, Yuichi Yaji, Grzegorz Madejski, K. Nakajima, Takayuki Yuasa, Koji Nakazawa, Motohide Kokubun, Tsunefumi Mizuno, K. Hayashi, Takanori Endo, Hirofumi Noda, Yasushi Fukazawa, R. Sato, Kazuyoshi Hiragi, Masao Yoshino, K. Doutsu, Kazuo Makishima, M. Matsuoka, K. Fukami, Yasunobu Uchiyama, Sei-ichiro Watanabe, Teruaki Enoto, T. Fukuyama, Takaaki Tanaka, Takao Kitaguchi, Satoshi Nakahira, T. Kozu, S. Torii, Y. Hanabata, Shinya Saito, Makoto Tashiro, J. Katsuta, Hirokazu Odaka, Sho Nishino, Y. Umeki, M. Koseki, Shinya Yamada, Shin-nosuke Ishikawa, and Yukikatsu Terada

Subjects
Physics, Photon, business.industry, Astrophysics::High Energy Astrophysical Phenomena, Compton telescope, Detector, Astrophysics::Instrumentation and Methods for Astrophysics, Compton scattering, Cadmium telluride photovoltaics, Semiconductor detector, Optics, Angular resolution, business, Energy (signal processing)
Abstract

The Soft Gamma-ray Detector (SGD) on board ASTRO-H (Japanese next high-energy astrophysics mission) is a Compton telescope with narrow fleld-of-view, which utilizes Compton kinematics to enhance its background rejection capabilities. It is realized as a hybrid semiconductor detector system which consists of silicon and CdTe (cadmium telluride) detectors. It can detect photons in a wide energy band (50-600 keV) at a background level 10 times better than that of the Suzaku Hard X-ray Detector, and is complimentary to the Hard X-ray Imager on board ASTRO-H with an energy coverage of 5-80 keV. Excellent energy resolution is the key feature of the SGD, allowing it to achieve good background rejection capability taking advantage of good angular resolution. An additional capability of the SGD, its ability to measure gamma-ray polarization, opens up a new window to study properties of gamma-ray emission processes. Here we describe the instrument design of the SGD, its expected performance, and its development status.

Published
2009

23. Suzaku Observation of the Metallicity Distribution in the Elliptical Galaxy NGC 4636

Author

Kyoko Matsushita, Katsuhiro Hayashi, Keith A. Arnaud, Yasushi Fukazawa, Yoh Takei, Miyako Tozuka, and Sho Nishino

Subjects
Physics, galaxies: elliptical and lenticular, cD - X-rays: galaxies - X-rays: ISM, Metallicity, Resolution (electron density), FOS: Physical sciences, Astronomy and Astrophysics, Astrophysics, Central region, Galaxy, Distribution (mathematics), Astrophysics - Solar and Stellar Astrophysics, Space and Planetary Science, Elliptical galaxy, Resonance scattering, Solar and Stellar Astrophysics (astro-ph.SR), Line (formation)
Abstract

The 3rd Suzaku international Conference "Energetic Cosmos : from Suzaku to ASTRO-H" (June 29-July 2, 2009. Grand Park Otaru Hotel), Otaru, Hokkaido Japan, NGC 4636, an X-ray bright elliptical galaxy, was observed with Suzaku. Thanks to low background and good energy resolution of the XIS, we succeeded to estimate the foreground Galactic emission accurately, and measure the metal abundance distributions out to approximately 28 arcmin (approximately equal to 140 kpc) for O, Mg, Si and Fe for the first time. Metal abundances are as high as > 1 solar within 4' and decreases by approximately 50 % from the center toward the outer region. In addition, the O to Fe abundance ratio is about from 0.6 to 1.0 solar in all analyzed regions, indicating that metal products by SNe II and SNe Ia have mixed and diffused to the outer region of the galaxy. Furthermore, comparing distribution of metal mass and mass-to-light-ratio with those of other galaxies, we found that metal distributions in NGC 4636 are less extended, possibly due to environmental factors, such as frequency of galaxy interaction. We also confirmed a signature of the resonance scattering of the Fe(sub XVII) line in the central region, as reported with the XMM-Newton RGS observation., Meeting sponsors: The University of Tokyo, The Institute of Physical and Chemical Research, The Japan Society for the Promotion of Science, 資料番号: AA0064574149, レポート番号: JAXA-SP-09-008E

Published
2009

24. ERRATUM: 'CONSTRAINTS ON THE COSMIC-RAY DENSITY GRADIENT BEYOND THE SOLAR CIRCLE FROM FERMI γ-RAY OBSERVATIONS OF THE THIRD GALACTIC QUADRANT' (2011, ApJ, 726, 81)

Author

Francesco Longo, A. Chekhtman, J. Mehault, R. Dubois, A. W. Borgland, W. B. Focke, Eric Charles, P. L. Nolan, D. Parent, P. Spinelli, T. Uehara, D. J. Suson, Francesco Giordano, Nicola Omodei, M. Ziegler, Pierrick Martin, Joachim Ripken, R. A. Cameron, Hiromitsu Takahashi, S. Murgia, Jean Ballet, Andrey Vladimirov, P. Wang, P. Bruel, F. Piron, P. Lubrano, Julie McEnery, Yasunobu Uchiyama, E. Orlando, Stefano Ciprini, R. Buehler, P. Fusco, Emanuele Bonamente, Hartmut Sadrozinski, Melissa Pesce-Rollins, R. Claus, Alice K. Harding, J. M. Casandjian, Peter F. Michelson, Tadayuki Takahashi, Marcello Giroletti, Ryosuke Itoh, Marco Ajello, Sho Nishino, J. B. Thayer, Elliott D. Bloom, Luca Baldini, A. Tramacere, G. Godfrey, Ronaldo Bellazzini, Hideaki Katagiri, A. Makeev, Takaaki Tanaka, T. J. Brandt, K. Hayashi, Igor V. Moskalenko, M. E. Monzani, S. Rainò, Zhenwei Yang, Tsunefumi Mizuno, Mn Mazziotta, Carmelo Sgrò, Riccardo Rando, T. Ohsugi, F. de Palma, F. Loparco, Olaf Reimer, S. Buson, Yasushi Fukazawa, Jan Conrad, T. A. Porter, R. E. Hughes, Shiu-Hang Lee, V. Pelassa, E. Nuss, Seth Digel, Charles D. Dermer, Claudia Cecchi, L. Tibaldo, M. Kuss, Diego F. Torres, Daniela Hadasch, M. Ozaki, D. J. Thompson, J. F. Ormes, A. P. Waite, C. Favuzzi, J. P. Norris, A. Morselli, V. Vitale, J. Bregeon, M. Razzano, T. Sada, Stefan Funk, S. Germani, K. S. Wood, T. Kamae, W. N. Johnson, B. Berenji, Keith Bechtol, A. Reimer, Gudlaugur Johannesson, Justin Vandenbroucke, Guido Barbiellini, M. Brigida, E. J. Siskind, M. Hayashida, C. Monte, N. Vilchez, Jun Kataoka, Markus Ackermann, M. Llena-Garde, Andrew W. Strong, A. S. Johnson, M. Pepe, T. Glanzman, Jürgen Knödlseder, Y. Hanabata, V. Vasileiou, F. Gargano, Luca Latronico, Nicola Giglietto, Denis Bastieri, M. N. Lovellette, P. A. Caraveo, James Chiang, Elizabeth C. Ferrara, Alessandro Brez, Persis S. Drell, I. A. Grenier, T. L. Usher, Atsushi Okumura, Gloria Spandre, J. Lande, Sylvain Guiriec, Johann Cohen-Tanugi, M. Naumann-Godo, M. S. Strickman, and G. A. Caliandro

Subjects
Physics, Density gradient, Space and Planetary Science, Galactic quadrant, Astronomy, Astronomy and Astrophysics, Cosmic ray, Astrophysics, Fermi Gamma-ray Space Telescope
Published
2013

25. X-Ray and Optical Monitoring of a Gamma-Ray-Emitting Radio Galaxy, NGC 1275

Author

Katsutoshi Takaki, Hiromitsu Takahashi, Sho Nishino, Koji S. Kawabata, Makoto Uemura, Ryosuke Itoh, Syoko Yamazaki, Mahito Sasada, Yasushi Fukazawa, and Michitoshi Yoshida

Subjects
Physics, Space and Planetary Science, Radio galaxy, Detector, X-ray, Gamma ray, Astronomy, Astronomy and Astrophysics, Astrophysics, Instrumentation (computer programming)
Published
2013

27. Fe-K LINE PROBING OF MATERIAL AROUND THE ACTIVE GALACTIC NUCLEUS CENTRAL ENGINE WITHSUZAKU

Author

Masanori Ohno, Hiromitsu Takahashi, Sho Nishino, Katsuhiro Hayashi, Tomonori Yamasaki, Yasushi Fukazawa, M. Mizuno, Kazuyoshi Hiragi, and Hirohisa Shirai

Subjects
Physics, Astrophysics::High Energy Astrophysical Phenomena, Solid angle, Flux, Astronomy and Astrophysics, Torus, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, K-line, Galaxy, Interstellar medium, Space and Planetary Science, Equivalent width, Astrophysics::Galaxy Astrophysics, Line (formation)
Abstract

We systematically analyzed the high-quality Suzaku data of 88 Seyfert galaxies. We obtained a clear relation between the absorption column density and the equivalent width of the 6.4 keV line above 10$^{23}$ cm$^{-2}$, suggesting a wide-ranging column density of $10^{23-24.5}$ cm$^{-2}$ with a similar solid and a Fe abundance of 0.7--1.3 solar for Seyfert 2 galaxies. The EW of the 6.4 keV line for Seyfert 1 galaxies are typically 40--120 eV, suggesting the existence of Compton-thick matter like the torus with a column density of $>10^{23}$ cm$^{-2}$ and a solid angle of $(0.15-0.4)*4pi$, and no difference of neutral matter is visible between Seyfert 1 and 2 galaxies. An absorber with a lower column density of $10^{21-23}$ cm$^{-2}$ for Compton-thin Seyfert 2 galaxies is suggested to be not a torus but an interstellar medium. These constraints can be understood by the fact that the 6.4 keV line intensity ratio against the 10--50 keV flux is almost identical within a range of 2--3 in many Seyfert galaxies. Interestingly, objects exist with a low EW, 10--30 eV, of the 6.4 keV line, suggesting that those torus subtends only a small solid angle of $ 10^{23}$ cm$^{-2}$ is found, like that of the cold material. It is found that these features seem to change for brighter objects with more than several $10^{44}$ erg/s such that the Fe-K line features become weak. We discuss this feature, together with the torus structure.

Published
2010

28. Modeling and reproducibility of suzaku HXD PIN/GSO background

Author

M. Ushio, Masanori Ohno, Tomonori Yamasaki, Shinya Yamada, Motohide Kokubun, Tadayuki Takahashi, Kazuo Nakazawa, Tsunefumi Mizuno, Takaaki Tanaka, Hiromitsu Takahashi, Takuya Takahashi, Yasushi Fukazawa, Kazuhiro Makishima, Kazutaka Yamaoka, Hirohisa Shirai, Madoka Kawaharada, Naomi Kawano, Makoto Tashiro, Takayuki Yuasa, Mahito Sasada, Teruaki Enoto, Takao Kitaguchi, Shin Watanabe, Yukikatsu Terada, Tomonori Yasuda, Aya Bamba, Yuichi Uehara, Naoki Isobe, Sho Nishino, and Y. Umeki

Subjects
Time delay and integration, Physics, Reproducibility, instrumentation: detectors, business.industry, Astrophysics::High Energy Astrophysical Phenomena, Detector, Shields, Astronomy and Astrophysics, Scintillator, X-rays: general, methods: data analysis, Photodiode, law.invention, Event selection, Optics, Space and Planetary Science, law, Satellite, business
Abstract

Suzaku Hard X-ray Detector (HXD) achieved the lowest background level than any other previously or currently operational missions sensitive in the energy range of 10–600 keV, by utilizing PIN photodiodes and GSO scintillators mounted in BGO active shields to reject particle background and Compton-scattered events as much as possible. Because it does not have an imaging capability nor rocking mode for the background monitor, the sensitivity is limited by the reproducibility of the non X-ray background (NXB) model. We modeled the HXD NXB, which varies with time as well as other satellites with a low-Earth orbit, by utilizing several parameters, including particle monitor counts and satellite orbital/attitude information. The model background is supplied as an event file in which the background events are generated by random numbers, and can be analyzed in the same way as the real data. The reproducibility of the NXB model depends on the event selection criteria (such as cut-off rigidity and energy band) and the integration time, and the 1 systematic error is estimated to be less than 3% (PIN 15–40 keV) and 1% (GSO 50–100 keV) for more than 10 ks exposure.

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