M. Yamanaka - Department of Physical Science, Hiroshima University

M. Yamanaka
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M. Yamanaka
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Department of Physical Science, Hiroshima University
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High Energy Astrophysical Phenomena (21)
 
High Energy Physics - Phenomenology (20)
 
Solar and Stellar Astrophysics (15)
 
Cosmology and Nongalactic Astrophysics (11)
 
High Energy Physics - Experiment (3)
 
Nuclear Theory (2)
 
Astrophysics of Galaxies (1)
 
Physics - Accelerator Physics (1)

Publications Authored By M. Yamanaka

We revisit charged lepton flavor violating (CLFV) scattering processes $\ell_{i} N \to \tau X \, (\ell_{i} \ni e, \mu)$ mediated by Higgs. We point out that a new subprocess $\ell_{i} g \to \tau g$ via the effective interactions of Higgs and gluon gives the dominant contribution to $\ell_{i} N \to \tau X$ for an incident beam energy of $E_{\ell} \lesssim 1\,\text{TeV}$ in fixed target experiments. Furthermore, in the light of quark number conservation, we consider quark pair-production processes $\ell_{i} g \to \tau q \bar{q}$ ($q$ denotes quarks) instead of $\ell_{i} q \to \tau q$. Read More

The nature of progenitors of the so-called super-Chandrasekhar candidate Type Ia supernovae (SC-SNe Ia) has been actively debated. Recently, Yamanaka et al. (2016) reported a near-infrared (NIR) excess for SN 2012dn, and proposed that the excess originates from an echo by circumstellar (CS) dust. Read More

Blazars are highly variable active galactic nuclei which emit radiation at all wavelengths from radio to gamma-rays. Polarized radiation from blazars is one key piece of evidence for synchrotron radiation at low energies and it also varies dramatically. The polarization of blazars is of interest for understanding the origin, confinement, and propagation of jets. Read More

2016Aug
Authors: The CLIC, CLICdp collaborations, :, M. J. Boland, U. Felzmann, P. J. Giansiracusa, T. G. Lucas, R. P. Rassool, C. Balazs, T. K. Charles, K. Afanaciev, I. Emeliantchik, A. Ignatenko, V. Makarenko, N. Shumeiko, A. Patapenka, I. Zhuk, A. C. Abusleme Hoffman, M. A. Diaz Gutierrez, M. Vogel Gonzalez, Y. Chi, X. He, G. Pei, S. Pei, G. Shu, X. Wang, J. Zhang, F. Zhao, Z. Zhou, H. Chen, Y. Gao, W. Huang, Y. P. Kuang, B. Li, Y. Li, J. Shao, J. Shi, C. Tang, X. Wu, L. Ma, Y. Han, W. Fang, Q. Gu, D. Huang, X. Huang, J. Tan, Z. Wang, Z. Zhao, T. Laštovička, U. Uggerhoj, T. N. Wistisen, A. Aabloo, K. Eimre, K. Kuppart, S. Vigonski, V. Zadin, M. Aicheler, E. Baibuz, E. Brücken, F. Djurabekova, P. Eerola, F. Garcia, E. Haeggström, K. Huitu, V. Jansson, V. Karimaki, I. Kassamakov, A. Kyritsakis, S. Lehti, A. Meriläinen, R. Montonen, T. Niinikoski, K. Nordlund, K. Österberg, M. Parekh, N. A. Törnqvist, J. Väinölä, M. Veske, W. Farabolini, A. Mollard, O. Napoly, F. Peauger, J. Plouin, P. Bambade, I. Chaikovska, R. Chehab, M. Davier, W. Kaabi, E. Kou, F. LeDiberder, R. Pöschl, D. Zerwas, B. Aimard, G. Balik, J. -P. Baud, J. -J. Blaising, L. Brunetti, M. Chefdeville, C. Drancourt, N. Geoffroy, J. Jacquemier, A. Jeremie, Y. Karyotakis, J. M. Nappa, S. Vilalte, G. Vouters, A. Bernard, I. Peric, M. Gabriel, F. Simon, M. Szalay, N. van der Kolk, T. Alexopoulos, E. N. Gazis, N. Gazis, E. Ikarios, V. Kostopoulos, S. Kourkoulis, P. D. Gupta, P. Shrivastava, H. Arfaei, M. K. Dayyani, H. Ghasem, S. S. Hajari, H. Shaker, Y. Ashkenazy, H. Abramowicz, Y. Benhammou, O. Borysov, S. Kananov, A. Levy, I. Levy, O. Rosenblat, G. D'Auria, S. Di Mitri, T. Abe, A. Aryshev, T. Higo, Y. Makida, S. Matsumoto, T. Shidara, T. Takatomi, Y. Takubo, T. Tauchi, N. Toge, K. Ueno, J. Urakawa, A. Yamamoto, M. Yamanaka, R. Raboanary, R. Hart, H. van der Graaf, G. Eigen, J. Zalieckas, E. Adli, R. Lillestøl, L. Malina, J. Pfingstner, K. N. Sjobak, W. Ahmed, M. I. Asghar, H. Hoorani, S. Bugiel, R. Dasgupta, M. Firlej, T. A. Fiutowski, M. Idzik, M. Kopec, M. Kuczynska, J. Moron, K. P. Swientek, W. Daniluk, B. Krupa, M. Kucharczyk, T. Lesiak, A. Moszczynski, B. Pawlik, P. Sopicki, T. Wojtoń, L. Zawiejski, J. Kalinowski, M. Krawczyk, A. F. Żarnecki, E. Firu, V. Ghenescu, A. T. Neagu, T. Preda, I-S. Zgura, A. Aloev, N. Azaryan, J. Budagov, M. Chizhov, M. Filippova, V. Glagolev, A. Gongadze, S. Grigoryan, D. Gudkov, V. Karjavine, M. Lyablin, A. Olyunin, A. Samochkine, A. Sapronov, G. Shirkov, V. Soldatov, A. Solodko, E. Solodko, G. Trubnikov, I. Tyapkin, V. Uzhinsky, A. Vorozhtov, E. Levichev, N. Mezentsev, P. Piminov, D. Shatilov, P. Vobly, K. Zolotarev, I. Bozovic Jelisavcic, G. Kacarevic, S. Lukic, G. Milutinovic-Dumbelovic, M. Pandurovic, U. Iriso, F. Perez, M. Pont, J. Trenado, M. Aguilar-Benitez, J. Calero, L. Garcia-Tabares, D. Gavela, J. L. Gutierrez, D. Lopez, F. Toral, D. Moya, A. Ruiz Jimeno, I. Vila, T. Argyropoulos, C. Blanch Gutierrez, M. Boronat, D. Esperante, A. Faus-Golfe, J. Fuster, N. Fuster Martinez, N. Galindo Muñoz, I. García, J. Giner Navarro, E. Ros, M. Vos, R. Brenner, T. Ekelöf, M. Jacewicz, J. Ögren, M. Olvegård, R. Ruber, V. Ziemann, D. Aguglia, N. Alipour Tehrani, A. Andersson, F. Andrianala, F. Antoniou, K. Artoos, S. Atieh, R. Ballabriga Sune, M. J. Barnes, J. Barranco Garcia, H. Bartosik, C. Belver-Aguilar, A. Benot Morell, D. R. Bett, S. Bettoni, G. Blanchot, O. Blanco Garcia, X. A. Bonnin, O. Brunner, H. Burkhardt, S. Calatroni, M. Campbell, N. Catalan Lasheras, M. Cerqueira Bastos, A. Cherif, E. Chevallay, B. Constance, R. Corsini, B. Cure, S. Curt, B. Dalena, D. Dannheim, G. De Michele, L. De Oliveira, N. Deelen, J. P. Delahaye, T. Dobers, S. Doebert, M. Draper, F. Duarte Ramos, A. Dubrovskiy, K. Elsener, J. Esberg, M. Esposito, V. Fedosseev, P. Ferracin, A. Fiergolski, K. Foraz, A. Fowler, F. Friebel, J-F. Fuchs, C. A. Fuentes Rojas, A. Gaddi, L. Garcia Fajardo, H. Garcia Morales, C. Garion, L. Gatignon, J-C. Gayde, H. Gerwig, A. N. Goldblatt, C. Grefe, A. Grudiev, F. G. Guillot-Vignot, M. L. Gutt-Mostowy, M. Hauschild, C. Hessler, J. K. Holma, E. Holzer, M. Hourican, D. Hynds, Y. Inntjore Levinsen, B. Jeanneret, E. Jensen, M. Jonker, M. Kastriotou, J. M. K. Kemppinen, R. B. Kieffer, W. Klempt, O. Kononenko, A. Korsback, E. Koukovini Platia, J. W. Kovermann, C-I. Kozsar, I. Kremastiotis, S. Kulis, A. Latina, F. Leaux, P. Lebrun, T. Lefevre, L. Linssen, X. Llopart Cudie, A. A. Maier, H. Mainaud Durand, E. Manosperti, C. Marelli, E. Marin Lacoma, R. Martin, S. Mazzoni, G. Mcmonagle, O. Mete, L. M. Mether, M. Modena, R. M. Münker, T. Muranaka, E. Nebot Del Busto, N. Nikiforou, D. Nisbet, J-M. Nonglaton, F. X. Nuiry, A. Nürnberg, M. Olvegard, J. Osborne, S. Papadopoulou, Y. Papaphilippou, A. Passarelli, M. Patecki, L. Pazdera, D. Pellegrini, K. Pepitone, E. Perez Codina, A. Perez Fontenla, T. H. B. Persson, M. Petrič, F. Pitters, S. Pittet, F. Plassard, R. Rajamak, S. Redford, Y. Renier, S. F. Rey, G. Riddone, L. Rinolfi, E. Rodriguez Castro, P. Roloff, C. Rossi, V. Rude, G. Rumolo, A. Sailer, E. Santin, D. Schlatter, H. Schmickler, D. Schulte, N. Shipman, E. Sicking, R. Simoniello, P. K. Skowronski, P. Sobrino Mompean, L. Soby, M. P. Sosin, S. Sroka, S. Stapnes, G. Sterbini, R. Ström, I. Syratchev, F. Tecker, P. A. Thonet, L. Timeo, H. Timko, R. Tomas Garcia, P. Valerio, A. L. Vamvakas, A. Vivoli, M. A. Weber, R. Wegner, M. Wendt, B. Woolley, W. Wuensch, J. Uythoven, H. Zha, P. Zisopoulos, M. Benoit, M. Vicente Barreto Pinto, M. Bopp, H. H. Braun, M. Csatari Divall, M. Dehler, T. Garvey, J. Y. Raguin, L. Rivkin, R. Zennaro, A. Aksoy, Z. Nergiz, E. Pilicer, I. Tapan, O. Yavas, V. Baturin, R. Kholodov, S. Lebedynskyi, V. Miroshnichenko, S. Mordyk, I. Profatilova, V. Storizhko, N. Watson, A. Winter, J. Goldstein, S. Green, J. S. Marshall, M. A. Thomson, B. Xu, W. A. Gillespie, R. Pan, M. A Tyrk, D. Protopopescu, A. Robson, R. Apsimon, I. Bailey, G. Burt, D. Constable, A. Dexter, S. Karimian, C. Lingwood, M. D. Buckland, G. Casse, J. Vossebeld, A. Bosco, P. Karataev, K. Kruchinin, K. Lekomtsev, L. Nevay, J. Snuverink, E. Yamakawa, V. Boisvert, S. Boogert, G. Boorman, S. Gibson, A. Lyapin, W. Shields, P. Teixeira-Dias, S. West, R. Jones, N. Joshi, R. Bodenstein, P. N. Burrows, G. B. Christian, D. Gamba, C. Perry, J. Roberts, J. A. Clarke, N. A. Collomb, S. P. Jamison, B. J. A. Shepherd, D. Walsh, M. Demarteau, J. Repond, H. Weerts, L. Xia, J. D. Wells, C. Adolphsen, T. Barklow, M. Breidenbach, N. Graf, J. Hewett, T. Markiewicz, D. McCormick, K. Moffeit, Y. Nosochkov, M. Oriunno, N. Phinney, T. Rizzo, S. Tantawi, F. Wang, J. Wang, G. White, M. Woodley

The Compact Linear Collider (CLIC) is a multi-TeV high-luminosity linear e+e- collider under development. For an optimal exploitation of its physics potential, CLIC is foreseen to be built and operated in a staged approach with three centre-of-mass energy stages ranging from a few hundred GeV up to 3 TeV. The first stage will focus on precision Standard Model physics, in particular Higgs and top-quark measurements. Read More

We study the $\mu$-$e$ conversion in muonic atoms via an exchange of family gauge boson (FGB) $A_{2}^{\ 1}$ in a $U(3)$ FGB model. Within the class of FGB model, we consider three types of family-number assignments for quarks. We evaluate the $\mu$-$e$ conversion rate for various target nuclei, and find that next generation $\mu$-$e$ conversion search experiments can cover entire energy scale of the model for all of types of the quark family-number assignments. Read More

The relic abundance of the dark matter (DM) particle $d$ is studied in a secluded DM scenario, in which the $d$ number decreasing process dominantly occurs not through the pair annihilation of $d$ into the standard model particles, but via the $dd \to mm$ scattering process with a subsequently decaying mediator particle $m$. It is pointed out that the cosmologically observed relic abundance of DM can be accomplished even with a massive mediator having a mass $m_m$ non-negligibly heavy compared with the DM particle mass $m_d$. In the degenerated $d$-$m$ case ($m_d=m_m$), the DM relic abundance is realized by adjusting the $dd \to mm$ scattering amplitude large enough and by choosing an appropriate mediator particle life-time. Read More

We review a non-standard Big-Bang nucleosynthesis (BBN) scenario within the minimal supersymmetric standard model, and propose an idea to solve both ${}^{7}$Li and ${}^{6}$Li problems. Each problem is a discrepancy between the predicted abundance in the standard BBN and observed one. We focus on the stau, a supersymmetric partner of tau lepton, which is a long-lived charged particle when it is the next lightest supersymmetric particle and is degenerate in mass with the lightest supersymmetric particle. Read More

We present extensively dense observations of the super-Chandrasekhar supernova (SC SN) candidate SN 2012dn from $-11$ to $+140$ days after the date of its $B$-band maximum in the optical and near-infrared (NIR) wavelengths conducted through the OISTER ToO program. The NIR light curves and color evolutions up to 35 days after the $B$-band maximum provided an excellent match with those of another SC SN 2009dc, providing a further support to the nature of SN 2012dn as a SC SN. We found that SN 2012dn exhibited strong excesses in the NIR wavelengths from $30$ days after the $B$-band maximum. Read More

The charged lepton flavor violating (CLFV) processes of $\mu^-e^-\rightarrow e^-e^-$ decay by four Fermi contact interactions in a muonic atom for various atoms are investigated. The wave functions of bound and scattering state leptons are properly treated by solving Dirac equations with Coulomb interaction of the finite nuclear charge distributions. This new effect contributes significantly in particular for heavier atoms, where the obtained decay rate is about one order of magnitude larger than the previous estimation for $^{208}$Pb. Read More

Na I D absorbing systems toward Type Ia supernovae (SNe Ia) have been intensively studied over the last decade with the aim of finding circumstellar material (CSM), which is an indirect probe of the progenitor system. However, it is difficult to deconvolve CSM components from non-variable, and often dominant, components created by interstellar material (ISM). We present a series of high-resolution spectra of SN Ia 2014J from before maximum brightness to ~250 days after maximum brightness. Read More

We study the thermal leptogenesis in the $E_6\times U(1)_A$ SUSY GUT model in which realistic masses and mixings of quarks and leptons can be realized. We show that the sufficient baryon number can be produced by the leptogenesis in the model, in which the mass parameter of the lightest right-handed neutrino is predicted to be smaller than $10^8$ GeV. The essential point is that the mass of the lightest right-handed neutrino can be enhanced in the model because it has a lot of mass terms whose mass parameters are predicted to be the same order of magnitude which is smaller than $10^8$ GeV. Read More

Koike et al. proposed the charged lepton flavor violation (CLFV) decay of the muonic atom $\mu^-e^-\rightarrow e^-e^-$ as one of the promising processes to search for new physics beyond the standard model. It was found that the attractive interaction of leptons with the nucleus enhances the transition rate of the $\mu^-e^-\rightarrow e^-e^-$ process. Read More

We consider the case that $\mu$-$e$ conversion signal is discovered but other charged lepton flavor violating (cLFV) processes will never be found. In such a case, we need other approaches to confirm the $\mu$-$e$ conversion and its underlying physics without conventional cLFV searches. We study R-parity violating (RPV) SUSY models as a benchmark. Read More

Family gauge boson production at the LHC is investigated according to a $U(3)$ family gauge model with twisted family number assignment. In the model we study, a family gauge boson with the lowest mass, $A_1^{\ 1}$, interacts only with the first generation leptons and the third generation quarks. (The family numbers are assigned, for example, as $(e_1, e_2, e_3)= (e^-, \mu^-, \tau^-)$ and $(d_1, d_2, d_3)=(b, d, s) $[or $(d_1, d_2, d_3)=(b, s, d)$]). Read More

We report observations of the Type Iax supernova (SN Iax) 2012Z at optical and near-infrared wavelengths from immediately after the explosion until $\sim$ $260$ days after the maximum luminosity using the Optical and Infrared Synergetic Telescopes for Education and Research (OISTER) Target-of-Opportunity (ToO) program and the Subaru telescope. We found that the near-infrared (NIR) light curve evolutions and color evolutions are similar to those of SNe Iax 2005hk and 2008ha. The NIR absolute magnitudes ($M_{J}\sim-18. Read More

We report the late-time evolution of Type IIb Supernova (SN IIb) 2013df. SN 2013df showed a dramatic change in its spectral features at ~1 year after the explosion. Early on it showed typical characteristics shared by SNe IIb/Ib/Ic dominated by metal emission lines, while later on it was dominated by broad and flat-topped Halpha and He I emissions. Read More

We propose an $SO(10)$ supersymmetric grand unified theory (SUSY GUT), where the $SO(10)$ gauge symmetry breaks down to $SU(3)_c \times SU(2)_L \times U(1)_Y\times U(1)_{X}$ at the GUT scale and $U(1)_X$ is radiatively broken at the SUSY-braking scale. In order to achieve the observed Higgs mass around $126$ GeV and also to satisfy constraints on flavor- and/or CP-violating processes, we assume that the SUSY-breaking scale is $O(100)$ TeV, so that the $U(1)_X$ breaking scale is also $O(100)$ TeV. One big issue in the SO(10) GUTs is how to realize realistic Yukawa couplings. Read More

We report on long-term multi-wavelength monitoring of blazar Mrk~421 from 2010 to 2011. The source exhibited extreme X-ray flares in 2010. Our research group performed optical photopolarimetric follow-up observations using the Kanata telescope. Read More

We consider the case that $\mu$-$e$ conversion signal is discovered but other charged lepton flavor violating (cLFV) processes will never be found. In such a case, we need other approaches to confirm the $\mu$-$e$ conversion and its underlying physics without conventional cLFV searches. We study R-parity violating (RPV) SUSY models as a benchmark. Read More

We consider the case that $\mu$-$e$ conversion signal is discovered but other charged lepton flavor violating (cLFV) processes will never be found. In such a case, we need other approaches to confirm the $\mu$-$e$ conversion and its underlying physics without conventional cLFV searches. We study R-parity violating (RPV) SUSY models as a benchmark. Read More

2014Jun
Affiliations: 1Kyoto U

Continuing the project described by Kato et al. (2009, PASJ, 61, S395, arXiv:0905.1757), we collected times of superhump maxima for 56 SU UMa-type dwarf novae mainly observed during the 2013-2014 season and characterized these objects. Read More

We show that the Li problems can be solved in the next-to-minimal supersymmetric standard model where the slepton as the next-to-lightest SUSY particle is very long-lived. Such a long-lived slepton induces exotic nuclear reactions in big-bang nucleosynthesis, and destroys and produces the $^7$Li and $^6$Li nuclei via bound state formation. We study cases where the lightest SUSY particle is singlino-like neutralino and bino-like neutralino to present allowed regions in the parameter space which is consistent with the observations on the dark matter and the Higgs mass. Read More

Previously unremarkable, the extragalactic radio source GB 1310+487 showed a gamma-ray flare on 2009 November 18, reaching a daily flux of ~10^-6 photons/cm^2/s at energies E>100 MeV and becoming one of the brightest GeV sources for about two weeks. Its optical spectrum is not typical for a blazar, instead, it resembles those of narrow emission-line galaxies. We investigate changes of the object's radio-to-GeV spectral energy distribution (SED) during and after the prominent GeV flare with the aim to determine the nature of the object and constrain the origin of the variable high-energy emission. Read More

Using the non-equilibrium Green function method (Kadanoff-Baym equations) in the expanding universe, we investigate evolution of the lepton number asymmetry when the right-handed (RH) neutrinos have almost degenerate masses $|M_i^2-M_j^2| \ll M_i^2$. The resonantly enhanced $CP$-violating parameter $\varepsilon_i$ associated with the decay of the RH neutrino $N_i$ is obtained. It is proportional to an enhancement factor $(M_i^2-M_j^2) M_i \Gamma_j/ ((M_i^2-M_j^2)^2 +R_{ij}^2)$ with the regulator $R_{ij}=M_i \Gamma_i+M_j \Gamma_j$. Read More

We apply the axion-photon conversion mechanism to the 130 GeV $\gamma$-ray line observed by the Fermi satellite. Near the Galactic center, some astrophysical sources and/or particle dark matter can produce energetic axions (or axionlike particles), and the axions convert to $\gamma$ rays in Galactic magnetic fields along their flight to the Earth. Since continuum $\gamma$-ray and antiproton productions are sufficiently suppressed in axion production, the scenario fits the 130 GeV $\gamma$-ray line without conflicting with cosmic ray measurements. Read More

We explore the coannihilation region of the constrained minimal supersymmetric standard model (CMSSM) being consistent with current experimental/observational results. The requirements from the experimental/observational results are the 125GeV Higgs mass and the relic abundances of both the dark matter and light elements, especially the lithium-7. We put these requirements on the caluculated values, and thus we obtain allowed region. Read More

Supernovae (SNe) have been proposed to be the main production sites of dust grains in the Universe. Our knowledge on their importance to dust production is, however, limited by observationally poor constraints on the nature and amount of dust particles produced by individual SNe. In this paper, we present a spectrum covering optical through near-Infrared (NIR) light of the luminous Type IIn supernova (SN IIn) 2010jl around one and half years after the explosion. Read More

We present a set of photometric and spectroscopic observations of a bright Type Ib supernova SN 2012au from -6d until ~+150d after maximum. The shape of its early R-band light curve is similar to that of an average Type Ib/c supernova. The peak absolute magnitude is M_R=-18. Read More

We present multi-color light curves and optical spectra of V1280 Scorpii obtained from 2007 to 2012. It is shown that V1280 Sco is the extremely slow nova and the mass of white dwarf appears to be $\sim$ 0.6 M$\odot$ or lower. Read More

We present a study of SN 2009js in NGC 918. Multi-band Kanata optical photometry covering the first ~120 days show the source to be a Type IIP SN. Reddening is dominated by that due to our Galaxy. Read More

3C 66A is an intermediate-frequency-peaked BL Lac object detected by the Large Area Telescope onboard the Fermi Gamma-ray Space Telescope. We present a study of the long-term variations of this blazar seen over 2 years at GeV energies with Fermi and in the optical (flux and polarization) and near infrared with the Kanata telescope. In 2008, the first year of the study, we find a correlation between the gamma-ray flux and the measurements taken with the Kanata telescope. Read More

We propose helium-4 spallation processes induced by long-lived stau in supersymmetric standard models, and investigate an impact of the processes on light elements abundances. We show that, as long as the phase space of helium-4 spallation processes is open, they are more important than stau-catalyzed fusion and hence constrain the stau property. This talk is based on works (Jittoh et al. Read More

We studied allowed region on the intergenerational mixing parameters of sleptons from a viewpoint of big-bang nucleosynthesis in a slepton-neutralino coannihilation scenario. In this scenario, $^7$Li and $^6$Li problems can be solved by considering exotic reactions caused by bound-state effects with a long-lived slepton. Light element abundances are calculated as functions of the relic density and lifetime of the slepton which considerably depend on the intergenerational mixing parameters. Read More

2012Jul
Authors: M. Ackermann1, M. Ajello2, J. Ballet3, G. Barbiellini4, D. Bastieri5, R. Bellazzini6, R. D. Blandford7, E. D. Bloom8, E. Bonamente9, A. W. Borgland10, E. Bottacini11, J. Bregeon12, M. Brigida13, P. Bruel14, R. Buehler15, S. Buson16, G. A. Caliandro17, R. A. Cameron18, P. A. Caraveo19, J. M. Casandjian20, E. Cavazzuti21, C. Cecchi22, E. Charles23, A. Chekhtman24, J. Chiang25, S. Ciprini26, R. Claus27, J. Cohen-Tanugi28, S. Cutini29, F. D'Ammando30, F. de Palma31, C. D. Dermer32, E. do Couto e Silva33, P. S. Drell34, A. Drlica-Wagner35, R. Dubois36, C. Favuzzi37, S. J. Fegan38, E. C. Ferrara39, W. B. Focke40, P. Fortin41, L. Fuhrmann42, Y. Fukazawa43, P. Fusco44, F. Gargano45, D. Gasparrini46, N. Gehrels47, S. Germani48, N. Giglietto49, P. Giommi50, F. Giordano51, M. Giroletti52, T. Glanzman53, G. Godfrey54, I. A. Grenier55, S. Guiriec56, D. Hadasch57, M. Hayashida58, R. E. Hughes59, R. Itoh60, G. Johannesson61, A. S. Johnson62, H. Katagiri63, J. Kataoka64, J. Knodlseder65, M. Kuss66, J. Lande67, S. Larsson68, S. -H. Lee69, F. Longo70, F. Loparco71, B. Lott72, M. N. Lovellette73, P. Lubrano74, G. M. Madejski75, M. N. Mazziotta76, J. E. McEnery77, J. Mehault78, P. F. Michelson79, W. Mitthumsiri80, T. Mizuno81, C. Monte82, M. E. Monzani83, A. Morselli84, I. V. Moskalenko85, S. Murgia86, M. Naumann-Godo87, S. Nishino88, J. P. Norris89, E. Nuss90, T. Ohsugi91, A. Okumura92, N. Omodei93, E. Orlando94, M. Ozaki95, D. Paneque96, J. H. Panetta97, V. Pelassa98, M. Pesce-Rollins99, M. Pierbattista100, F. Piron101, G. Pivato102, T. A. Porter103, S. Raino104, R. Rando105, D. Rastawicki106, M. Razzano107, A. Readhead108, A. Reimer109, O. Reimer110, L. C. Reyes111, J. L. Richards112, C. Sbarra113, C. Sgro114, E. J. Siskind115, G. Spandre116, P. Spinelli117, A. Szostek118, H. Takahashi119, T. Tanaka120, J. G. Thayer121, J. B. Thayer122, D. J. Thompson123, M. Tinivella124, D. F. Torres125, G. Tosti126, E. Troja127, T. L. Usher128, J. Vandenbroucke129, V. Vasileiou130, G. Vianello131, V. Vitale132, A. P. Waite133, B. L. Winer134, K. S. Wood135, Z. Yang136, S. Zimmer137, R. Moderski138, K. Nalewajko139, M. Sikora140, M. Villata141, C. M. Raiteri142, H. D. Aller143, M. F. Aller144, A. A. Arkharov145, E. Benitez146, A. Berdyugin147, D. A. Blinov148, M. Boettcher149, O. J. A. Bravo Calle150, C. S. Buemi151, D. Carosati152, W. P. Chen153, C. Diltz154, A. Di Paola155, M. Dolci156, N. V. Efimova157, E. Forn\'158, M. A. Gurwell159, J. Heidt160, D. Hiriart161, B. Jordan162, G. Kimeridze163, T. S. Konstantinova164, E. N. Kopatskaya165, E. Koptelova166, O. M. Kurtanidze167, A. Lahteenmaki168, E. G. Larionova169, L. V. Larionova170, V. M. Larionov171, P. Leto172, E. Lindfors173, H. C. Lin174, D. A. Morozova175, M. G. Nikolashvili176, K. Nilsson177, M. Oksman178, P. Roustazadeh179, A. Sievers180, L. A. Sigua181, A. Sillanpaa182, T. Takahashi183, L. O. Takalo184, M. Tornikoski185, C. Trigilio186, I. S. Troitsky187, G. Umana188, E. Angelakis189, T. P. Krichbaum190, I. Nestoras191, D. Riquelme192, M. Krips193, S. Trippe194, A. Arai195, K. S. Kawabata196, K. Sakimoto197, M. Sasada198, S. Sato199, M. Uemura200, M. Yamanaka201, M. Yoshida202, T. Belloni203, G. Tagliaferri204, E. W. Bonning205, J. Isler206, C. M. Urry207, E. Hoversten208, A. Falcone209, C. Pagani210, M. Stroh211
Affiliations: 1the Fermi-LAT Collaboration, 2the Fermi-LAT Collaboration, 3the Fermi-LAT Collaboration, 4the Fermi-LAT Collaboration, 5the Fermi-LAT Collaboration, 6the Fermi-LAT Collaboration, 7the Fermi-LAT Collaboration, 8the Fermi-LAT Collaboration, 9the Fermi-LAT Collaboration, 10the Fermi-LAT Collaboration, 11the Fermi-LAT Collaboration, 12the Fermi-LAT Collaboration, 13the Fermi-LAT Collaboration, 14the Fermi-LAT Collaboration, 15the Fermi-LAT Collaboration, 16the Fermi-LAT Collaboration, 17the Fermi-LAT Collaboration, 18the Fermi-LAT Collaboration, 19the Fermi-LAT Collaboration, 20the Fermi-LAT Collaboration, 21the Fermi-LAT Collaboration, 22the Fermi-LAT Collaboration, 23the Fermi-LAT Collaboration, 24the Fermi-LAT Collaboration, 25the Fermi-LAT Collaboration, 26the Fermi-LAT Collaboration, 27the Fermi-LAT Collaboration, 28the Fermi-LAT Collaboration, 29the Fermi-LAT Collaboration, 30the Fermi-LAT Collaboration, 31the Fermi-LAT Collaboration, 32the Fermi-LAT Collaboration, 33the Fermi-LAT Collaboration, 34the Fermi-LAT Collaboration, 35the Fermi-LAT Collaboration, 36the Fermi-LAT Collaboration, 37the Fermi-LAT Collaboration, 38the Fermi-LAT Collaboration, 39the Fermi-LAT Collaboration, 40the Fermi-LAT Collaboration, 41the Fermi-LAT Collaboration, 42the Fermi-LAT Collaboration, 43the Fermi-LAT Collaboration, 44the Fermi-LAT Collaboration, 45the Fermi-LAT Collaboration, 46the Fermi-LAT Collaboration, 47the Fermi-LAT Collaboration, 48the Fermi-LAT Collaboration, 49the Fermi-LAT Collaboration, 50the Fermi-LAT Collaboration, 51the Fermi-LAT Collaboration, 52the Fermi-LAT Collaboration, 53the Fermi-LAT Collaboration, 54the Fermi-LAT Collaboration, 55the Fermi-LAT Collaboration, 56the Fermi-LAT Collaboration, 57the Fermi-LAT Collaboration, 58the Fermi-LAT Collaboration, 59the Fermi-LAT Collaboration, 60the Fermi-LAT Collaboration, 61the Fermi-LAT Collaboration, 62the Fermi-LAT Collaboration, 63the Fermi-LAT Collaboration, 64the Fermi-LAT Collaboration, 65the Fermi-LAT Collaboration, 66the Fermi-LAT Collaboration, 67the Fermi-LAT Collaboration, 68the Fermi-LAT Collaboration, 69the Fermi-LAT Collaboration, 70the Fermi-LAT Collaboration, 71the Fermi-LAT Collaboration, 72the Fermi-LAT Collaboration, 73the Fermi-LAT Collaboration, 74the Fermi-LAT Collaboration, 75the Fermi-LAT Collaboration, 76the Fermi-LAT Collaboration, 77the Fermi-LAT Collaboration, 78the Fermi-LAT Collaboration, 79the Fermi-LAT Collaboration, 80the Fermi-LAT Collaboration, 81the Fermi-LAT Collaboration, 82the Fermi-LAT Collaboration, 83the Fermi-LAT Collaboration, 84the Fermi-LAT Collaboration, 85the Fermi-LAT Collaboration, 86the Fermi-LAT Collaboration, 87the Fermi-LAT Collaboration, 88the Fermi-LAT Collaboration, 89the Fermi-LAT Collaboration, 90the Fermi-LAT Collaboration, 91the Fermi-LAT Collaboration, 92the Fermi-LAT Collaboration, 93the Fermi-LAT Collaboration, 94the Fermi-LAT Collaboration, 95the Fermi-LAT Collaboration, 96the Fermi-LAT Collaboration, 97the Fermi-LAT Collaboration, 98the Fermi-LAT Collaboration, 99the Fermi-LAT Collaboration, 100the Fermi-LAT Collaboration, 101the Fermi-LAT Collaboration, 102the Fermi-LAT Collaboration, 103the Fermi-LAT Collaboration, 104the Fermi-LAT Collaboration, 105the Fermi-LAT Collaboration, 106the Fermi-LAT Collaboration, 107the Fermi-LAT Collaboration, 108the Fermi-LAT Collaboration, 109the Fermi-LAT Collaboration, 110the Fermi-LAT Collaboration, 111the Fermi-LAT Collaboration, 112the Fermi-LAT Collaboration, 113the Fermi-LAT Collaboration, 114the Fermi-LAT Collaboration, 115the Fermi-LAT Collaboration, 116the Fermi-LAT Collaboration, 117the Fermi-LAT Collaboration, 118the Fermi-LAT Collaboration, 119the Fermi-LAT Collaboration, 120the Fermi-LAT Collaboration, 121the Fermi-LAT Collaboration, 122the Fermi-LAT Collaboration, 123the Fermi-LAT Collaboration, 124the Fermi-LAT Collaboration, 125the Fermi-LAT Collaboration, 126the Fermi-LAT Collaboration, 127the Fermi-LAT Collaboration, 128the Fermi-LAT Collaboration, 129the Fermi-LAT Collaboration, 130the Fermi-LAT Collaboration, 131the Fermi-LAT Collaboration, 132the Fermi-LAT Collaboration, 133the Fermi-LAT Collaboration, 134the Fermi-LAT Collaboration, 135the Fermi-LAT Collaboration, 136the Fermi-LAT Collaboration, 137the Fermi-LAT Collaboration, 138the GASP-WEBT consortium, 139the GASP-WEBT consortium, 140the GASP-WEBT consortium, 141the GASP-WEBT consortium, 142the GASP-WEBT consortium, 143the GASP-WEBT consortium, 144the GASP-WEBT consortium, 145the GASP-WEBT consortium, 146the GASP-WEBT consortium, 147the GASP-WEBT consortium, 148the GASP-WEBT consortium, 149the GASP-WEBT consortium, 150the GASP-WEBT consortium, 151the GASP-WEBT consortium, 152the GASP-WEBT consortium, 153the GASP-WEBT consortium, 154the GASP-WEBT consortium, 155the GASP-WEBT consortium, 156the GASP-WEBT consortium, 157the GASP-WEBT consortium, 158the GASP-WEBT consortium, 159the GASP-WEBT consortium, 160the GASP-WEBT consortium, 161the GASP-WEBT consortium, 162the GASP-WEBT consortium, 163the GASP-WEBT consortium, 164the GASP-WEBT consortium, 165the GASP-WEBT consortium, 166the GASP-WEBT consortium, 167the GASP-WEBT consortium, 168the GASP-WEBT consortium, 169the GASP-WEBT consortium, 170the GASP-WEBT consortium, 171the GASP-WEBT consortium, 172the GASP-WEBT consortium, 173the GASP-WEBT consortium, 174the GASP-WEBT consortium, 175the GASP-WEBT consortium, 176the GASP-WEBT consortium, 177the GASP-WEBT consortium, 178the GASP-WEBT consortium, 179the GASP-WEBT consortium, 180the GASP-WEBT consortium, 181the GASP-WEBT consortium, 182the GASP-WEBT consortium, 183the GASP-WEBT consortium, 184the GASP-WEBT consortium, 185the GASP-WEBT consortium, 186the GASP-WEBT consortium, 187the GASP-WEBT consortium, 188the GASP-WEBT consortium, 189F-GAMMA, 190F-GAMMA, 191F-GAMMA, 192F-GAMMA, 193Iram-PdBI, 194Iram-PdBI, 195Kanata, 196Kanata, 197Kanata, 198Kanata, 199Kanata, 200Kanata, 201Kanata, 202Kanata, 203RXTE, 204RXTE, 205SMARTS, 206SMARTS, 207SMARTS, 208Swift-XRT, 209Swift-XRT, 210Swift-XRT, 211Swift-XRT

The blazar AO 0235+164 (z = 0.94) has been one of the most active objects observed by Fermi Large Area Telescope (LAT) since its launch in Summer 2008. In addition to the continuous coverage by Fermi, contemporaneous observations were carried out from the radio to {\gamma} -ray bands between 2008 September and 2009 February. Read More

2012Jun
Affiliations: 1INAF/IAPS, Via Fosso del Cavaliere, Italy, 2INAF/IAPS, Via Fosso del Cavaliere, Italy, 3Marie Curie Fellow, Dark Cosmology Center, Niels Bohr Institute, University of Copenhagen, Copenhagen, Denmark, 4NASA Postdoctoral Program fellow at the Jet Propulsion Laboratory, California Institute of Technology, 5Department of Physical Science, Hiroshima University, Japan, 6Department of Physical Science, Hiroshima University, Japan, 7Hiroshima Astrophysical Science Center, Hiroshima University, Japan, 8Centro de Astrobiología, 9ASI Science Data Center, Italy, 10INAF-OAC, localita' Poggio dei Pini, Italy, 11ASI Science Data Center, Italy, 12Dip. Fisica, Univ Trieste and INFN Trieste, Italy, 13Istituto Nazionale di Fisica Nucleare, Sezione di Bari, Italy, 14INAF/IAPS, Via Fosso del Cavaliere, Italy, 15INAF-IASF Palermo, Italy, 16INAF/IASF-Milano, Italy, 17INAF/IAPS, Via Fosso del Cavaliere, Italy, 18INAF/IAPS, Via Fosso del Cavaliere, Italy, 19INAF/IAPS, Via Fosso del Cavaliere, Italy, 20Agenzia Spaziale Italiana, Viale Liegi, Italy, 21INAF/IASF-Milano, Italy, 22ENEA Frascati, Italy, 23INAF/IAPS, Via Fosso del Cavaliere, Italy, 24Dip. Fisica, Univ Trieste and INFN Trieste, Italy, 25INAF/IASF-Milano, Italy, 26INFN-Pavia, Italy, 27INAF-OAR, Italy, 28INAF/IAPS, Via Fosso del Cavaliere, Italy, 29INAF/IAPS, Via Fosso del Cavaliere, Italy, 30INAF/IAPS, Via Fosso del Cavaliere, Italy, 31INAF/IASF-Bologna, Italy, 32INAF/IAPS, Via Fosso del Cavaliere, Italy, 33Dip. Fisica, Universitá di Torino, Italy, 34INAF/IAPS, Via Fosso del Cavaliere, Italy, 35INAF/IASF-Milano, Italy, 36INAF/IASF-Bologna, Italy, 37ENEA-Bologna, Italy, 38INAF/IASF-Bologna, Italy, 39INAF/IASF-Bologna, Italy, 40INAF/IAPS, Via Fosso del Cavaliere, Italy, 41INAF/IAPS, Via Fosso del Cavaliere, Italy, 42INFN-Roma La Sapienza, Italy, 43INAF/IASF-Bologna, Italy, 44INAF/IASF-Milano, Italy, 45INAF/IASF-Bologna, Italy, 46Dip. Fisica, Univ Trieste and INFN Trieste, Italy, 47INFN Roma Tor Vergata, Italy, 48INAF-OAC, localita' Poggio dei Pini, Italy, 49INAF/IASF-Milano, Italy, 50INAF/IAPS, Via Fosso del Cavaliere, Italy, 51Dip. di Fisica, Univ. Tor Vergata, Italy, 52Dip. di Fisica, Univ. Dell'Insubria, Italy, 53Dip. di Fisica, Univ. Dell'Insubria, Italy, 54ENEA Frascati, Italy, 55INFN-Pavia, Italy, 56INAF/IAPS, Via Fosso del Cavaliere, Italy, 57INAF/IAPS, Via Fosso del Cavaliere, Italy, 58INAF/IAPS, Via Fosso del Cavaliere, Italy, 59INAF/IASF-Bologna, Italy, 60INAF-OAC, localita' Poggio dei Pini, Italy, 61Dip. Fisica, Univ Trieste and INFN Trieste, Italy, 62INFN-Roma La Sapienza, Italy, 63ASI Science Data Center, Italy, 64ASI Science Data Center, Italy, 65ASI Science Data Center, Italy, 66Agenzia Spaziale Italiana, Viale Liegi, Italy, 67Agenzia Spaziale Italiana, Viale Liegi, Italy

In 2008 AGILE and Fermi detected gamma-ray flaring activity from the unidentified EGRET source 3EG J1236+0457, recently associated with a flat spectrum radio quasar GB6 J1239+0443 at z=1.762. The optical counterpart of the gamma-ray source underwent a flux enhancement of a factor 15-30 in 6 years, and of ~10 in six months. Read More

We present time-resolved broad-band observations of the quasar 3C 279 obtained from multi-wavelength campaigns conducted during the first two years of the Fermi Gamma-ray Space Telescope mission. While investigating the previously reported gamma-ray/optical flare accompanied by a change in optical polarization, we found that the optical emission appears delayed with respect to the gamma-ray emission by about 10 days. X-ray observations reveal a pair of `isolated' flares separated by ~90 days, with only weak gamma-ray/optical counterparts. Read More

We present optical ($B$, $V$, $R_{\rm c}$, $I_{\rm c}$ and $y$) and near infrared ($J$, $H$ and $K_{\rm s}$) photometric and spectroscopic observations of a classical nova V1280 Scorpii for five years from 2007 to 2011. Our photometric observations show a declining event in optical bands shortly after the maximum light which continues $\sim$ 250 days. The event is most probably caused by a dust formation. Read More

In December 2009, the bright blazar, 3C 454.3 exhibited a strong outburst in the optical, X-ray and gamma-ray regions. We performed photometric and polarimetric monitoring of this outburst in the optical and near-infrared bands with TRISPEC and HOWPol attached to the Kanata telescope. Read More

We propose helium-4 spallation processes induced by long-lived stau in supersymmetric standard models, and investigate an impact of the processes on light elements abundances. We show that, as long as the phase space of helium-4 spallation processes is open, they are more important than stau-catalyzed fusion and hence constrain the stau property. Read More

We report on the correlation between the flux, color and polarization variations on time scales of days--months in blazars, and discuss their universal aspects. We performed monitoring of 42 blazars in the optical and near-infrared bands from 2008 to 2010 using TRISPEC attached to the "Kanata" 1.5-m telescope. Read More

We investigate flavour violating decays of the long-lived lightest slepton and the tau lepton in the coannihilation region of the Minimal Supersymmetric Standard Model with a Seesaw mechanism to generate neutrino masses. We consider a situation where the mass difference between the lightest neutralino, as the Lightest Supersymmetric particle (LSP), and the lightest slepton, as the Next-to-LSP, is smaller than the mass of tau lepton. In this situation, the lifetime of the lightest slepton is very long and it is determined by lepton flavour violating (LFV) couplings because the slepton mainly consists of the lighter stau and the flavour conserving 2-body decay is kinematically forbidden. Read More

We report on multi-band photometric and polarimetric observations of the blazars AO 0235+164 and PKS 1510-089. These two blazars were active in 2008 and 2009, respectively. In these active states, prominent short flares were observed in both objects, having amplitudes of >1 mag within 10 d. Read More