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33 results on '"Sonbas, E."'

1. Observation Campaign of (99942) Apophis in the 2021 Apparition

Author: Lee, H.-J., Kim, M.-J., Lee, Y.-J., Marciniak, A., Urakawa, S., Kim, D.-H., Moon, H.-K., Choi, Y.-J., Kuroda, D., Okumura, S., Zoła, S., Chatelain, J., Lister, T. A., Gomez, E., Greenstreet, S., Pal, A., Szakáts, R., Erasmus, N., Lees, R., Janse van Rensburg, P., Ogłoza, W., Dróżdż, M., Żejmo, M., Kamiński, K., Kamińska, M.K., Duffard, R., Roh, D.-G., Yim, H.-S., Kim, T., Mottola, S., Yoshida, F., Reichart, D.E., Sonbas, E., Caton, D.B., Kaplan, M., Erece, O., and Yang, H.
Subjects: Asteroids, Apophis
Published: 2022

2. GRB 140102A: insight into prompt spectral evolution and early optical afterglow emission

Author: Gupta, Rahul, Oates, S. R., Pandey, S. B., Castro-Tirado, A. J., Joshi, Jagdish C., Hu, Y. -D., Valeev, A. F., Zhang, B. B., Zhang, Z., Kumar, Amit, Aryan, A., Lien, A., Kumar, B., Cui, Ch., Wang, Ch., Dimple, Bhattacharya, D., Sonbas, E., Bai, J., Tello, J. C., Gorosabel, J., Cerón, J. M. Castro, Porto, J. R. F., Misra, K., De Pasquale, M., Caballero-García, M. D., Jelínek, M., Kubánek, P., Minaev, P. Yu., Cunniffe, R., Sánchez-Ramírez, R., Guziy, S., Jeong, S., Tiwari, S. N., Razzaque, S., Bhalerao, V., Pintado, V. C., Sokolov, V. V., Zhao, X., Fan, Y., and Xin, Y.
Subjects: High Energy Astrophysical Phenomena (astro-ph.HE), shock waves, gamma-ray burst: general, gamma-ray burst: individual: GRB 140102A, methods: observational, Astrophysics::High Energy Astrophysical Phenomena, FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics - High Energy Astrophysical Phenomena, Astrophysics::Galaxy Astrophysics
Abstract: We present and perform a detailed analysis of multi-wavelength observations of \thisgrb, an optical bright GRB with an observed reverse shock (RS) signature. Observations of this GRB were acquired with the BOOTES-4 robotic telescope, the \fermi, and the \swift missions. Time-resolved spectroscopy of the prompt emission shows that changes to the peak energy (\Ep) tracks intensity and the low-energy spectral index seems to follow the intensity for the first episode, whereas this tracking behavior is less clear during the second episode. The fit to the afterglow light curves shows that the early optical afterglow can be described with RS emission and is consistent with the thin shell scenario of the constant ambient medium. The late time afterglow decay is also consistent with the prediction of the external forward shock (FS) model. We determine the properties of the shocks, Lorentz factor, magnetization parameters, and ambient density of \thisgrb, and compare these parameters with another 12 GRBs, consistent with having RS produced by thin shells in an ISM-like medium. The value of the magnetization parameter ($R_{\rm B} \approx 18$) indicates a moderately magnetized baryonic dominant jet composition for \thisgrb. We also report the host galaxy photometric observations of \thisgrb obtained with 10.4m GTC, 3.5m CAHA, and 3.6m DOT telescopes and find the host (photo $z$ = $2.8^{+0.7}_{-0.9}$) to be a high mass, star-forming galaxy with a star formation rate of $20 \pm 10 \msun$ $\rm yr^{-1}$., Comment: 27 pages, 16 figures, 12 tables, accepted for publication in MNRAS
Published: 2021

3. Spitzer Observations of the Predicted Eddington Flare from Blazar OJ 287

Author: Laine, S. Dey, L. Valtonen, M. Gopakumar, A. Zola, S. Komossa, S. Kidger, M. Pihajoki, P. Gómez, J.L. Caton, D. Ciprini, S. Drozdz, M. Gazeas, K. Godunova, V. Haque, S. Hildebrandt, F. Hudec, R. Jermak, H. Kong, A.K.H. Lehto, H. Liakos, A. Matsumoto, K. Mugrauer, M. Pursimo, T. Reichart, D.E. Simon, A. Siwak, M. Sonbas, E.
Subjects: Astrophysics::High Energy Astrophysical Phenomena, Astrophysics::Solar and Stellar Astrophysics, Astrophysics::Earth and Planetary Astrophysics
Abstract: Binary black hole (BH) central engine description for the unique blazar OJ 287 predicted that the next secondary BH impact-induced bremsstrahlung flare should peak on 2019 July 31. This prediction was based on detailed general relativistic modeling of the secondary BH trajectory around the primary BH and its accretion disk. The expected flare was termed the Eddington flare to commemorate the centennial celebrations of now-famous solar eclipse observations to test general relativity by Sir Arthur Eddington. We analyze the multi-epoch Spitzer observations of the expected flare between 2019 July 31 and 2019 September 6, as well as baseline observations during 2019 February-March. Observed Spitzer flux density variations during the predicted outburst time display a strong similarity with the observed optical pericenter flare from OJ 287 during 2007 September. The predicted flare appears comparable to the 2007 flare after subtracting the expected higher base-level Spitzer flux densities at 3.55 and 4.49 μm compared to the optical R-band. Comparing the 2019 and 2007 outburst lightcurves and the previously calculated predictions, we find that the Eddington flare arrived within 4 hr of the predicted time. Our Spitzer observations are well consistent with the presence of a nano-Hertz gravitational-wave emitting spinning massive binary BH that inspirals along a general relativistic eccentric orbit in OJ 287. These multi-epoch Spitzer observations provide a parametric constraint on the celebrated BH no-hair theorem. © 2020. The American Astronomical Society. All rights reserved..
Published: 2020

4. A Minimal Time-Scale For The Spectral States Of Gx 339-4

Author: Sonbas, E., Mohamed, K., Dhuga, K. S., Tuncer, A., and Gogus, E.
Subjects: Astrophysics::High Energy Astrophysical Phenomena
Abstract: Black hole transients are known to undergo spectral transitions that form q-shaped tracks on a hardness intensity diagram. In this work, we use the archival Rossi X-ray Timing Explorer data to extract a characteristic minimal time-scale for the spectral states in GX 339-4 for the 2002-2003 and 2010 outbursts. We use the extracted time-scale to construct an intensity variability diagram for each outburst. This new diagram is comparable to the traditional hardness intensity diagram and offers the potential for probing the underlying dynamics associated with the evolution of the relevant emission regions in black hole transients. We confirm this possibility by connecting the minimal time-scale with the inner disc radius, Rin (estimated from spectral fits), and demonstrate a positive correlation between these variables as the system evolves through its spectral transitions. Furthermore, we probe the relation between the minimal time-scale and the break frequencies extracted from the power spectral densities. Lastly, we examine a possible link between the extracted time-scale and a traditional measure of variability, i.e. the root mean square, determined directly from the power spectra.
Published: 2020

5. Stochastic Modeling of Multiwavelength Variability of the Classical BL Lac Object OJ 287 on Timescales Ranging from Decades to Hours

Author: Goyal, A. Stawarz, Ł. Zola, S. Marchenko, V. Soida, M. Nilsson, K. Ciprini, S. Baran, A. Ostrowski, M. Wiita, P.J. Gopal-Krishna Siemiginowska, A. Sobolewska, M. Jorstad, S. Marscher, A. Aller, M.F. Aller, H.D. Hovatta, T. Caton, D.B. Reichart, D. Matsumoto, K. Sadakane, K. Gazeas, K. Kidger, M. Piirola, V. Jermak, H. Alicavus, F. Baliyan, K.S. Baransky, A. Berdyugin, A. Blay, P. Boumis, P. Boyd, D. Bufan, Y. Torrent, M.C. Campos, F. Gómez, J.C. Dalessio, J. Debski, B. Dimitrov, D. Drozdz, M. Er, H. Erdem, A. Pérez, A.E. Ramazani, V.F. Filippenko, A.V. Gafton, E. Garcia, F. Godunova, V. Pinilla, F.G. Gopinathan, M. Haislip, J.B. Haque, S. Harmanen, J. Hudec, R. Hurst, G. Ivarsen, K.M. Joshi, A. Kagitani, M. Karaman, N. Karjalainen, R. Kaur, N. Kozieł-Wierzbowska, D. Kuligowska, E. Kundera, T. Kurowski, S. Kvammen, A. Lacluyze, A.P. Lee, B.C. Liakos, A. Haro, J.L.D. Moore, J.P. Mugrauer, M. Nogues, R.N. Neely, A.W. Ogloza, W. Okano, S. Pajdosz, U. Pandey, J.C. Perri, M. Poyner, G. Provencal, J. Pursimo, T. Raj, A. Rajkumar, B. Reinthal, R. Reynolds, T. Saario, J. Sadegi, S. Sakanoi, T. González, J.L.S. Sameer Simon, A.O. Siwak, M. Schweyer, T. Alfaro, F.C.S. Sonbas, E. Strobl, J. Takalo, L.O. Espasa, L.T. Valdes, J.R. Vasylenko, V.V. Verrecchia, F. Webb, J.R. Yoneda, M. Zejmo, M. Zheng, W. Zielinski, P. Janik, J. Chavushyan, V. Mohammed, I. Cheung, C.C. Giroletti, M.
Subjects: Astrophysics::High Energy Astrophysical Phenomena
Abstract: We present the results of our power spectral density analysis for the BL Lac object OJ 287, utilizing the Fermi-LAT survey at high-energy γ-rays, Swift-XRT in X-rays, several ground-based telescopes and the Kepler satellite in the optical, and radio telescopes at GHz frequencies. The light curves are modeled in terms of continuous-time autoregressive moving average (CARMA) processes. Owing to the inclusion of the Kepler data, we were able to construct for the first time the optical variability power spectrum of a blazar without any gaps across ∼6 dex in temporal frequencies. Our analysis reveals that the radio power spectra are of a colored-noise type on timescales ranging from tens of years down to months, with no evidence for breaks or other spectral features. The overall optical power spectrum is also consistent with a colored noise on the variability timescales ranging from 117 years down to hours, with no hints of any quasi-periodic oscillations. The X-ray power spectrum resembles the radio and optical power spectra on the analogous timescales ranging from tens of years down to months. Finally, the γ-ray power spectrum is noticeably different from the radio, optical, and X-ray power spectra of the source: we have detected a characteristic relaxation timescale in the Fermi-LAT data, corresponding to ∼150 days, such that on timescales longer than this, the power spectrum is consistent with uncorrelated (white) noise, while on shorter variability timescales there is correlated (colored) noise. © 2018. The American Astronomical Society. All rights reserved..
Published: 2018

6. Authenticating the Presence of a Relativistic Massive Black Hole Binary in OJ 287 Using Its General Relativity Centenary Flare: Improved Orbital Parameters

Author: Dey, L. Valtonen, M.J. Gopakumar, A. Zola, S. Hudec, R. Pihajoki, P. Ciprini, S. Matsumoto, K. Sadakane, K. Kidger, M. Nilsson, K. Mikkola, S. Sillanpää, A. Takalo, L.O. Lehto, H.J. Berdyugin, A. Piirola, V. Jermak, H. Baliyan, K.S. Pursimo, T. Caton, D.B. Alicavus, F. Baransky, A. Blay, P. Boumis, P. Boyd, D. Torrent, M.C. Campos, F. Gómez, J.C. Chandra, S. Chavushyan, V. Dalessio, J. Debski, B. Drozdz, M. Er, H. Erdem, A. Pérez, A.E. Ramazani, V.F. Filippenko, A.V. Gafton, E. Ganesh, S. Garcia, F. Gazeas, K. Godunova, V. Pinilla, F.G. Gopinathan, M. Haislip, J.B. Harmanen, J. Hurst, G. Janík, J. Jelinek, M. Joshi, A. Kagitani, M. Karjalainen, R. Kaur, N. Keel, W.C. Kouprianov, V.V. Kundera, T. Kurowski, S. Kvammen, A. Lacluyze, A.P. Lee, B.C. Liakos, A. Lindfors, E. De Haro, J.L. Mugrauer, M. Nogues, R.N. Neely, A.W. Nelson, R.H. Ogloza, W. Okano, S. Pajdosz-Śmierciak, U. Pandey, J.C. Perri, M. Poyner, G. Provencal, J. Raj, A. Reichart, D.E. Reinthal, R. Reynolds, T. Saario, J. Sadegi, S. Sakanoi, T. González, J.-L.S. Sameer Schweyer, T. Simon, A. Siwak, M. Alfaro, F.C.S. Sonbas, E. Steele, I. Stocke, J.T. Strobl, J. Tomov, T. Espasa, L.T. Valdes, J.R. Pérez, J.V. Verrecchia, F. Vasylenko, V. Webb, J.R. Yoneda, M. Zejmo, M. Zheng, W. Zielinski, P.
Subjects: Astrophysics::High Energy Astrophysical Phenomena
Abstract: Results from regular monitoring of relativistic compact binaries like PSR 1913+16 are consistent with the dominant (quadrupole) order emission of gravitational waves (GWs). We show that observations associated with the binary black hole (BBH) central engine of blazar OJ 287 demand the inclusion of gravitational radiation reaction effects beyond the quadrupolar order. It turns out that even the effects of certain hereditary contributions to GW emission are required to predict impact flare timings of OJ 287. We develop an approach that incorporates this effect into the BBH model for OJ 287. This allows us to demonstrate an excellent agreement between the observed impact flare timings and those predicted from ten orbital cycles of the BBH central engine model. The deduced rate of orbital period decay is nine orders of magnitude higher than the observed rate in PSR 1913+16, demonstrating again the relativistic nature of OJ 287's central engine. Finally, we argue that precise timing of the predicted 2019 impact flare should allow a test of the celebrated black hole "no-hair theorem" at the 10% level. © 2018. The American Astronomical Society. All rights reserved.
Published: 2018

7. Polarization and spectral energy distribution in OJ 287 during the 2016/17 outbursts

Author: Valtonen, M. Zola, S. Jermak, H. Ciprini, S. Hudec, R. Dey, L. Gopakumar, A. Reichart, D.L. Caton, D.B. Gazeas, K. Matsumoto, K. Ogloza, W. Drozdz, M. Alicavus, F. Baransky, O. Berdyugin, A. Boumis, P. Bufan, Y. Debski, B. Er, H. Erdem, A. Godunova, V. Haque, S. Hoette, V.L. Janik, J. Kidger, M. Kundera, T. Kurowski, S. Liakos, A. Mohammed, I. Nilsson, K. Pajdosz, U. Piirola, V. Pursimo, T. Rajkumar, B. Simon, A.O. Siwak, M. Sonbas, E. Steele, I.A. Vasylenko, V.V. Zejmo, M. Zielinski, P.
Subjects: Astrophysics::High Energy Astrophysical Phenomena, Astrophysics::Solar and Stellar Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics
Abstract: We report optical photometric and polarimetric observations of the blazar OJ 287 gathered during 2016/17. The high level of activity, noticed after the General Relativity Centenary flare, is argued to be part of the follow-up flares that exhibited high levels of polarization and originated in the primary black hole jet. We propose that the follow-up flares were induced as a result of accretion disk perturbations, travelling from the site of impact towards the primary SMBH. The timings inferred from our observations allowed us to estimate the propagation speed of these perturbations. Additionally, we make predictions for the future brightness of OJ 287. © 2017 by the authors.
Published: 2017

8. The size, shape, density and ring of the dwarf planet Haumea from a stellar occultation

Author: Ortiz, J.L. Santos-Sanz, P. Sicardy, B. Benedetti-Rossi, G. Bérard, D. Morales, N. Duffard, R. Braga-Ribas, F. Hopp, U. Ries, C. Nascimbeni, V. Marzari, F. Granata, V. Pál, A. Kiss, C. Pribulla, T. Komžík, R. Hornoch, K. Pravec, P. Bacci, P. Maestripieri, M. Nerli, L. Mazzei, L. Bachini, M. Martinelli, F. Succi, G. Ciabattari, F. Mikuz, H. Carbognani, A. Gaehrken, B. Mottola, S. Hellmich, S. Rommel, F.L. Fernández-Valenzuela, E. Bagatin, A.C. Cikota, S. Cikota, A. Lecacheux, J. Vieira-Martins, R. Camargo, J.I.B. Assafin, M. Colas, F. Behrend, R. Desmars, J. Meza, E. Alvarez-Candal, A. Beisker, W. Gomes, A.R. Morgado, B.E. Roques, F. Vachier, F. Berthier, J. Mueller, T.G. Madiedo, J.M. Unsalan, O. Sonbas, E. Karaman, N. Erece, O. Koseoglu, D.T. Ozisik, T. Kalkan, S. Guney, Y. Niaei, M.S. Satir, O. Yesilyaprak, C. Puskullu, C. Kabas, A. Demircan, O. Alikakos, J. Charmandaris, V. Leto, G. Ohlert, J. Christille, J.M. Szakáts, R. Farkas, A.T. Varga-Verebélyi, E. Marton, G. Marciniak, A. Bartczak, P. Santana-Ros, T. Butkiewicz-Bak, M. Dudzinski, G. Alí-Lagoa, V. Gazeas, K. Tzouganatos, L. Paschalis, N. Tsamis, V. Sánchez-Lavega, A. Pérez-Hoyos, S. Hueso, R. Guirado, J.C. Peris, V. Iglesias-Marzoa, R.
Abstract: Haumea-one of the four known trans-Neptunian dwarf planets- is a very elongated and rapidly rotating body1-3. In contrast to other dwarf planets4-6, its size, shape, albedo and density are not well constrained. The Centaur Chariklo was the first body other than a giant planet known to have a ring system7, and the Centaur Chiron was later found to possess something similar to Chariklo's rings8,9. Here we report observations from multiple Earth-based observatories of Haumea passing in front of a distant star (a multichord stellar occultation). Secondary events observed around the main body of Haumea are consistent with the presence of a ring with an opacity of 0.5, width of 70 kilometres and radius of about 2,287 kilometres. The ring is coplanar with both Haumea's equator and the orbit of its satellite Hi'iaka. The radius of the ring places it close to the 3:1 mean-motion resonance with Haumea's spin period-that is, Haumea rotates three times on its axis in the time that a ring particle completes one revolution. The occultation by the main body provides an instantaneous elliptical projected shape with axes of about 1,704 kilometres and 1,138 kilometres. Combined with rotational light curves, the occultation constrains the three-dimensional orientation of Haumea and its triaxial shape, which is inconsistent with a homogeneous body in hydrostatic equilibrium. Haumea's largest axis is at least 2,322 kilometres, larger than previously thought, implying an upper limit for its density of 1,885 kilograms per cubic metre and a geometric albedo of 0.51, both smaller than previous estimates1,10,11. In addition, this estimate of the density of Haumea is closer to that of Pluto than are previous estimates, in line with expectations. No global nitrogen- or methane-dominated atmosphere was detected. © 2017 Macmillan Publishers Limited, part of Springer Nature. All rights reserved.
Published: 2017

9. Constraining the High-energy Emission from Gamma-Ray Bursts with Fermi

Author: The, Fermi Large Area Telescope Team, Ackermann, M., Ajello, M., Baldini, L., Barbiellini, G., Baring, M. G., Bechtol, K., Bellazzini, R., Blandford, R. D., Bloom, E. D., Bonamente, E., Borgland, A. W., Bottacini, E., Bouvier, A., Brigida, M., Buehler, R., Buson, S., Caliandro, G. A., Cameron, R. A., Cecchi, C., Charles, E., Chekhtman, A., Chiang, J., Ciprini, S., Claus, R., Cohen-Tanugi, J., Cutini, S., D'Ammando, F., de, Palma F., Dermer, C. D., do, Couto e Silva E., Drell, P. S., Drlica-Wagner, A., Favuzzi, C., Fusco, P., Gargano, F., Gasparrini, D., Gehrels, N., Germani, S., Giglietto, N., Giordano, F., Giroletti, M., Glanzman, T., Granot, J., Grenier, I. A., Grove, J. E., Hadasch, D., Harding, A. K., Hays, E., Horan, D., Johannesson, G., Knodlseder, J., Kocevski, D., Kuss, M., Lande, J., Longo, F., Loparco, F., Lovellette, M. N., Lubrano, P., Mazziotta, M. N., McEnery, J., McGlynn, S., Michelson, P. F., Mitthumsiri, W., Monzani, M. E., Moretti, E., Morselli, A., Moskalenko, I. V., Murgia, S., Naumann-Godo, M., Norris, J. P., Nuss, E., Nymark, T., Omodei, N., Orlando, E., Panetta, J. H., Parent, D., Pelassa, V., Pesce-Rollins, M., Piron, F., Pivato, G., Racusin, J. L., Raino, S., Rando, R., Razzaque, S., Reimer, A., Reimer, O., Ritz, S., Ryde, F., Sgro, C., Siskind, E. J., Sonbas, E., Spandre, G., Spinelli, P., Stamatikos, M., Stawarz, Lukasz, Fukazawa, Yasushi, Hanabata, Yoshitaka, Kataoka, Jun, Ohsugi, Takashi, Okumura, Akira, High Energy Astrophys. & Astropart. Phys (API, FNWI), Ackermann M, Ajello M, Baldini L, Barbiellini G, Baring MG, Bechtol K, Bellazzini R, Blandford RD, Bloom ED, Bonamente E, Borgland AW, Bottacini E, Bouvier A, Brigida M, Buehler R, Buson S, Caliandro GA, Cameron RA, Cecchi C, Charles E, Chekhtman A, Chiang J, Ciprini S, Claus R, Cohen-Tanugi J, Cutini S, DAmmando F, de Palma F, Dermer CD, Silva EDE, Drell PS, Drlica-Wagner A, Favuzzi C, Fukazawa Y, Fusco P, Gargano F, Gasparrini D, Gehrels N, Germani S, Giglietto N, Giordano F, Giroletti M, Glanzman T, Granot J, Grenier IA, Grove JE, Hadasch D, Hanabata Y, Harding AK, Hays E, Horan D, Johannesson G, Kataoka J, Knodlseder J, Kocevski D, Kuss M, Lande J, Longo F, Loparco F, Lovellette MN, Lubrano P, Mazziotta MN, McEnery J, McGlynn S, Michelson PF, Mitthumsiri W, Monzani ME, Moretti E, Morselli A, Moskalenko IV, Murgia S, Naumann-Godo M, Norris JP, Nuss E, Nymark T, Ohsugi T, Okumura A, Omodei N, Orlando E, Panetta JH, Parent D, Pelassa V, Pesce-Rollins M, Piron F, Pivato G, Racusin JL, Raino S, Rando R, Razzaque S, Reimer A, Reimer O, Ritz S, Ryde F, Sgro C, Siskind EJ, Sonbas E, Spandre G, Spinelli P, Stamatikos M, Stawarz E, Suson DJ, Takahashi H, Tanaka T, Thayer JG, Thayer JB, Tibaldo L, Tinivella M, Tosti G, Uehara T, Vandenbroucke J, Vasileiou V, Vianello G, Vitale V, Waite AP, Connaughton V, Briggs MS, Guirec S, Goldstein A, Burgess JM, Bhat PN, Bissaldi E, Camero-Arranz A, Fishman J, Fitzpatrick G, Foley S, Gruber D, Jenke P, Kippen RM, Kouveliotou C, McBreen S, Meegan C, Paciesas WS, Preece R, Rau A, Tierney D, van der Horst AJ, von Kienlin A, Wilson-Hodge C, Xiong S, Ackermann, M., Ajello, M., Baldini, L., BARBIELLINI AMIDEI, Guido, Baring, M. G., Bechtol, K., Bellazzini, R., Blandford, R. D., Bloom, E. D., Bonamente, E., Borgland, A. W., Bottacini, E., Bouvier, A., Brigida, M., Buehler, R., Buson, S., Caliandro, G. A., Cameron, R. A., Cecchi, C., Charles, E., Chekhtman, A., Chiang, J., Ciprini, S., Claus, R., Cohen Tanugi, J., Cutini, S., D'Ammando, F., Palma, F., Dermer, C. D., E. d. C., Drell, P. S., Drlica Wagner, A., Favuzzi, C., Fukazawa, Y., Fusco, P., Gargano, F., Gasparrini, D., Gehrels, N., Germani, S., Giglietto, N., Giordano, F., Giroletti, M., Glanzman, T., Granot, J., Grenier, I. A., Grove, J. E., Hadasch, D., Hanabata, Y., Harding, A. K., Hays, E., Horan, D., Johannesson, G., Kataoka, J., Kn\odlseder, J., Kocevski, D., Kuss, M., Lande, J., Longo, Francesco, Loparco, F., Lovellette, M. N., Lubrano, P., Mazziotta, M. N., Mcenery, J., Mcglynn, S., Michelson, P. F., Mitthumsiri, W., Monzani, M. E., Moretti, E., Morselli, A., Moskalenko, I. V., Murgia, S., Naumann Godo, M., Norris, J. P., Nuss, E., Nymark, T., Ohsugi, T., Okumura, A., Omodei, N., Orlando, E., Panetta, J. H., Parent, D., Pelassa, V., Pesce Rollins, M., Piron, F., Pivato, G., Racusin, J. L., Rain\`o, S., Rando, R., Razzaque, S., Reimer, A., Reimer, O., Ritz, S., Ryde, F., Sgr\`o, C., Siskind, E. J., Sonbas, E., Spandre, G., Spinelli, P., Stamatikos, M., Stawarz, ., Suson, D. J., Takahashi, H., Tanaka, T., Thayer, J. G., Thayer, J. B., Tibaldo, L., Tinivella, M., Tosti, G., Uehara, T., Vandenbroucke, J., Vasileiou, V., Vianello, G., Vitale, V., Waite, A. P., Gamma ray, . F., Connaughton, V., Briggs, M. S., Guirec, S., Goldstein, A., Burgess, J. M., Bhat, P. N., Bissaldi, Elisabetta, Camero Arranz, A., Fishman, J., Fitzpatrick, G., Foley, S., Gruber, D., Jenke, P., Kippen, R. M., Kouveliotou, C., Mcbreen, S., Meegan, C., Paciesas, W. S., Preece, R., Rau, A., Tierney, D., Van, A. J., Kienlin, A., Wilson Hodge, C., and Xiong, S.
Subjects: Astrophysics::High Energy Astrophysical Phenomena, gamma-ray burst: general, Astrophysics, general [gamma-ray burst], Astronomical spectroscopy, Spectral line, symbols.namesake, Gamma rays: general, Physics, Astronomy, Astronomy and Astrophysics, Spectral bands, Gamma-ray astronomy, gamma rays: general, Spectral component, Space and Planetary Science, Lorentz factor, gamma-ray burst: general – gamma rays: general, symbols, ddc:520, Astrophysics - High Energy Astrophysical Phenomena, Gamma-ray burst, general [gamma rays], Astrophysics - Cosmology and Nongalactic Astrophysics, Fermi Gamma-ray Space Telescope
Abstract: 著者人数: 139名, Accepted: 2012-05-22, 資料番号: SA1004166000
Published: 2012

10. Primary black hole spin in oj 287 AS determined by the general relativity centenary flare

Author: Valtonen, M.J. Zola, S. Ciprini, S. Gopakumar, A. Matsumoto, K. Sadakane, K. Kidger, M. Gazeas, K. Nilsson, K. Berdyugin, A. Piirola, V. Jermak, H. Baliyan, K.S. Alicavus, F. Boyd, D. Torrent, M.C. Campos, F. Gómez, J.C. Caton, D.B. Chavushyan, V. Dalessio, J. Debski, B. Dimitrov, D. Drozdz, M. Er, H. Erdem, A. Pérez, A.E. Ramazani, V.F. Filippenko, A.V. Ganesh, S. Garcia, F. Gómez Pinilla, F. Gopinathan, M. Haislip, J.B. Hudec, R. Hurst, G. Ivarsen, K.M. Jelinek, M. Joshi, A. Kagitani, M. Kaur, N. Keel, W.C. Lacluyze, A.P. Lee, B.C. Lindfors, E. Lozano De Haro, J. Moore, J.P. Mugrauer, M. Naves Nogues, R. Neely, A.W. Nelson, R.H. Ogloza, W. Okano, S. Pandey, J.C. Perri, M. Pihajoki, P. Poyner, G. Provencal, J. Pursimo, T. Raj, A. Reichart, D.E. Reinthal, R. Sadegi, S. Sakanoi, T. Salto González, J.-L. Sameer Schweyer, T. Siwak, M. Soldán Alfaro, F.C. Sonbas, E. Steele, I. Stocke, J.T. Strobl, J. Takalo, L.O. Tomov, T. Tremosa Espasa, L. Valdes, J.R. Valero Pérez, J. Verrecchia, F. Webb, J.R. Yoneda, M. Zejmo, M. Zheng, W. Telting, J. Saario, J. Reynolds, T. Kvammen, A. Gafton, E. Karjalainen, R. Harmanen, J. Blay, P.
Subjects: General Relativity and Quantum Cosmology, Astrophysics::High Energy Astrophysical Phenomena
Abstract: OJ 287 is a quasi-periodic quasar with roughly 12 year optical cycles. It displays prominent outbursts that are predictable in a binary black hole model. The model predicted a major optical outburst in 2015 December. We found that the outburst did occur within the expected time range, peaking on 2015 December 5 at magnitude 12.9 in the optical R-band. Based on Swift/XRT satellite measurements and optical polarization data, we find that it included a major thermal component. Its timing provides an accurate estimate for the spin of the primary black hole, . The present outburst also confirms the established general relativistic properties of the system such as the loss of orbital energy to gravitational radiation at the 2% accuracy level, and it opens up the possibility of testing the black hole no-hair theorem with 10% accuracy during the present decade. © 2016. The American Astronomical Society. All rights reserved.
Published: 2016

11. A search for QPOs in the blazar OJ287: Preliminary results from the 2015/2016 observing campaign

Author: Zola, S. Valtonen, M. Bhatta, G. Goyal, A. Debski, B. Baran, A. Krzesinski, J. Siwak, M. Ciprini, S. Gopakumar, A. Jermak, H. Nilsson, K. Reichart, D. Matsumoto, K. Sadakane, K. Gazeas, K. Kidger, M. Piirola, V. Alicavus, F. Baliyan, K.S. Berdyugin, A. Boyd, D. Campas Torrent, M. Campos, F. Carrillo Gómez, J. Caton, D.B. Chavushyan, V. Dalessio, J. Dimitrov, D. Drozdz, M. Er, H. Erdem, A. Escartin Pérez, A. Fallah Ramazani, V. Filippenko, A.V. Garcia, F. Gómez Pinilla, F. Gopinathan, M. Haislip, J.B. Harmanen, J. Hudec, R. Hurst, G. Ivarsen, K.M. Jelinek, M. Joshi, A. Kagitani, M. Kaur, N. Keel, W.C. LaCluyze, A.P. Lee, B.C. Lindfors, E. Lozano de Haro, J. Moore, J.P. Mugrauer, M. Naves Nogues, R. Neely, A.W. Nelson, R.H. Ogloza, W. Okano, S. Pandey, J.C. Perri, M. Pihajoki, P. Poyner, G. Provencal, J. Pursimo, T. Raj, A. Reinthal, R. Sadegi, S. Sakanoi, T. Sameer González, J.-L.S. Schweyer, T. Soldán Alfaro, F.C. Karaman, N. Sonbas, E. Steele, I. Stocke, J.T. Strobl, J. Takalo, L.O. Tomov, T. Tremosa Espasa, L. Valdes, J.R. Valero Pérez, J. Verrecchia, F. Webb, J.R. Yoneda, M. Zejmo, M. Zheng, W. Telting, J. Saario, J. Reynolds, T. Kvammen, A. Gafton, E. Karjalainen, R. Blay, P.
Abstract: We analyse the light curve in the R band of the blazar OJ287, gathered during the 2015/2016 observing season. We did a search for quasi-periodic oscillations (QPOs) using several methods over a wide range of timescales. No statistically significant periods were found in the high-frequency domain both in the ground-based data and in Kepler observations. In the longer-period domain, the Lomb-Scargle periodogram revealed several peaks above the 99% significance level. The longest one-about 95 days-corresponds to the innermost stable circular orbit (ISCO) period of the more massive black hole. The 43-day period could be an alias, or it can be attributed to accretion in the form of a two-armed spiral wave. © 2016 by the authors.
Published: 2016

12. A strong optical activity of the OJ287 blazar

Author: Zoła, Stanisław, Valtonen, M., Ciprini, S., Reichart, D. E., Moore, J. P., LaCluyze, A. P., Ivarsen, K. M., Groom, R., Stranger, K., Sadakane, K., Matsumoto, K., Kagitani, M., Okano, S., Sakanoi, T., Provencal, J., Dalessio, J., Drozdz, M., Gazeas, K., Ramazani, V. Fallah, Kidger, M., Naves, R., Campas, Montse, Jermak, H., Steele, I. A., Sonbas, E., Er, H., Zejmo, M., Caton, D. B., Poyner, G., and Siwak, Michał
Subjects: optical, Black Hole, AGN, blazar
Published: 2016

13. DETECTION OF HIGH-ENERGY GAMMA-RAY EMISSION DURING THE X-RAY FLARING ACTIVITY IN GRB 100728A

Author: A. Abdo, A., Ackermann, Markus, Ajello, Marco, Baldini, Luca, Ballet, Jean, Barbiellini, Guido, G. Baring, M., Bastieri, D., Bechtol, K., Bellazzini, R., Berenji, B., N. Bhat, P., Bissaldi, E., D. Blandford, R., Bonamente, E., Bonnell, J., W. Borgland, A., Bouvier, A., Bregeon, J., Brigida, M., Bruel, Pascal, Buehler, R., Buson8, S., A. Caliandro, G., A. Cameron, R., Caraveo, P. A., M. Casandjian, J., Cecchi, C., Charles, E., Chekhtman, A., Chiang, J., Ciprini, S., Claus, R., Connaughton, V., Conrad, J., Cutini, S., De Angelis, A., De Palma, F., D. Dermer, C., Do Couto, E., S. Drell, P., Dubois, R., Favuzzi, C., Fukazawa, Y., Fusco, P., Gargano, F., Gehrels, N., Germani, S., Giglietto, N., Giommi, P., Giordano, F., Giroletti, M., Glanzman, T., Godfrey, G., Granot, J., A. Grenier, I., Guiriec, S., Hadasch, D., Hanabata, Y., E. Hughes, R., J 'Ohannesson, G., S. Johnson, A., Kamae, T., Katagiri, H., Kataoka, J., Kerr, M., Knödlseder, Jürgen, Kuss, M., Lande, J., Latronico, L., Lee, S.-H., Longo, F., Loparco, F., Lott, B., Lubrano, P., N. Mazziotta, M., E. Mcenery, J., M'Esz'Aros, P., F. Michelson, P., Mizuno, T., A. Moiseev, A., E. Monzani, M., Morselli, A., V. Moskalenko, I., Murgia, S., Nakamori, T., Naumann-Godo, M., L. Nolan, P., P. Norris, J., Nuss, E., Ohsugi, T., Okumura, A., Omodei, N., Orlando, E., S. Paciesas, W., Pelassa, V., Pesce-Rollins, M., Pierbattista, M., Piron, F., Porter, T.A., L. Racusin, J., Rain'O, S., Razzano, M., Razzaque, S., Reimer, A., Reimer, O., C. Reyes, L., Roth, M., F.-W. Sadrozinski, H., Sgr'O, C., J. Siskind, E., D. Smith, P., Sonbas, E., Spandre, G., Spinelli, P., Stamatikos, M., S. Strickman, M., Takahashi, H., Tanaka, T., Tanaka, Y., G. Thayer, J., B. Thayer, J., F. Torres, D., Tosti, G., Troja, E., Uehara, T., L. Usher, T., Vandenbroucke, J., Vasileiou, V., Vianello, G., Vilchez, N., Vitale, V., Von Kienlin, A., P. Waite, A., Wang, P., L. Winer, B., S. Wood, K., Yamazaki, R., Yang, Z., Ziegler, M., L. Piro, And, Silva, E., 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), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-École polytechnique (X)-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), 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 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), Institut de recherche en astrophysique et planétologie (IRAP), Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Observatoire Midi-Pyrénées (OMP), Abdo, A. A., Ackermann, M., Ajello, M., Baldini, L., Ballet, J., BARBIELLINI AMIDEI, Guido, Baring, M. G., Bastieri, D., Bechtol, K., Bellazzini, R., Berenji, B., Bhat, P. N., Bissaldi, Elisabetta, Blandford, R. D., Bonamente, E., Bonnell, J., Borgland, A. W., Bouvier, A., 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., Chiang, J., Ciprini, S., Claus, R., Connaughton, V., Conrad, J., Cutini, S., Angelis, A., Palma, F., Dermer, C. D., E. d. C., Drell, P. S., Dubois, R., Favuzzi, C., Fukazawa, Y., Fusco, P., Gargano, F., Gehrels, N., Germani, S., Giglietto, N., Giommi, P., Giordano, F., Giroletti, M., Glanzman, T., Godfrey, G., Granot, J., Grenier, I. A., Guiriec, S., Hadasch, D., Hanabata, Y., Hughes, R. E., Johannesson, G., Johnson, A. S., Kamae, T., Katagiri, H., Kataoka, J., Kerr, M., Kn\odlseder, J., Kuss, M., Lande, J., Latronico, L., Lee, S., Longo, Francesco, Loparco, F., Lott, B., Lubrano, P., Mazziotta, M. N., Mcenery, J. E., Meszaros, P., Michelson, P. F., Mizuno, T., Moiseev, A. A., Monzani, M. E., Morselli, A., Moskalenko, I. V., Murgia, S., Nakamori, T., Naumann Godo, M., Nolan, P. L., Norris, J. P., Nuss, E., Ohsugi, T., Okumura, A., Omodei, N., Orlando, E., Paciesas, W. S., Pelassa, V., Pesce Rollins, M., Pierbattista, M., Piron, F., Porter, T. A., Racusin, J. L., Rain\`o, S., Razzano, M., Razzaque, S., Reimer, A., Reimer, O., Reyes, L. C., Roth, M., Sadrozinski, H. F., Sgr\`o, C., Siskind, E. J., Smith, P. D., Sonbas, E., Spandre, G., Spinelli, P., Stamatikos, M., Strickman, M. S., Takahashi, H., Tanaka, T., Tanaka, Y., Thayer, J. G., Thayer, J. B., Torres, D. F., Tosti, G., Troja, E., Uehara, T., Usher, T. L., Vandenbroucke, J., Vasileiou, V., Vianello, G., Vilchez, N., Vitale, V., Kienlin, A., Waite, A. P., Wang, P., Winer, B. L., Wood, K. S., Yamazaki, R., Yang, Z., Ziegler, M., Piro, L., Collaboration, ., 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 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 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 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, 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 national des sciences de l'Univers (INSU - CNRS)-Université Toulouse III - Paul Sabatier (UT3), 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), and 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)
Subjects: High energy, [PHYS.ASTR.HE]Physics [physics]/Astrophysics [astro-ph]/High Energy Astrophysical Phenomena [astro-ph.HE], Astrophysics::High Energy Astrophysical Phenomena, FOS: Physical sciences, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, 7. Clean energy, gamma-ray burst: individual: GRB100728A, radiation mechanisms: non-thermal, 0103 physical sciences, gamma-ray burst: individual (GRB100728A), 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, Physics, High Energy Astrophysical Phenomena (astro-ph.HE), 010308 nuclear & particles physics, [SDU.ASTR.HE]Sciences of the Universe [physics]/Astrophysics [astro-ph]/High Energy Astrophysical Phenomena [astro-ph.HE], Gamma ray, X-ray, Astronomy and Astrophysics, non-thermal [radiation mechanisms], Afterglow, 13. Climate action, Space and Planetary Science, individual: GRB100728A [gamma-ray burst], Astrophysics - High Energy Astrophysical Phenomena, Fermi Gamma-ray Space Telescope
Abstract: We present the simultaneous Swift and Fermi observations of the bright GRB100728A and its afterglow. The early X-ray emission is dominated by a vigorous flaring activity continuing until 1 ks after the burst. In the same time interval high energy emission is significantly detected by the Fermi/LAT. Marginal evidence of GeV emission is observed up to later times. We discuss the broadband properties of this burst within both the internal and external shock scenarios, with a particular emphasis on the relation between X-ray flares, the GeV emission and a continued long-duration central engine activity as their power source., Comment: accepted for publication in ApJ Letters. Contact authors: E. Troja, L. Piro, V. Vasileiou, S. Cutini, J. E. McEnery
Published: 2011

14. The Afterglow Of Grb 130427A From 1 To 10(16) Ghz

Author: Perley, D. A., Cenko, S. B., Corsi, A., Tanvir, N. R., Levan, A. J., Kann, D. A., Sonbas, E., Wiersema, K., Zheng, W., Zhao, X. -H., Bai, J. -M., Bremer, M., Castro-Tirado, A. J., Chang, L., Clubb, K. I., Frail, D., Fruchter, A., Gogus, E., Greiner, J., and Guver, T.
Subjects: Astrophysics::High Energy Astrophysical Phenomena, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics::Galaxy Astrophysics
Abstract: We present multiwavelength observations of the afterglow of GRB 130427A, the brightest (in total fluence) gamma-ray burst (GRB) of the past 29 yr. Optical spectroscopy from Gemini-North reveals the redshift of the GRB to be z = 0.340, indicating that its unprecedented brightness is primarily the result of its relatively close proximity to Earth; the intrinsic luminosities of both the GRB and its afterglow are not extreme in comparison to other bright GRBs. We present a large suite of multiwavelength observations spanning from 300 s to 130 days after the burst and demonstrate that the afterglow shows relatively simple, smooth evolution at all frequencies, with no significant late-time flaring or rebrightening activity. The entire data set from 1 GHz to 10 GeV can be modeled as synchrotron emission from a combination of reverse and forward shocks in good agreement with the standard afterglow model, providing strong support to the applicability of the underlying theory and clarifying the nature of the GeV emission observed to last for minutes to hours following other very bright GRBs. A tenuous, wind-stratified circumburst density profile is required by the observations, suggesting a massive-star progenitor with a low mass-loss rate, perhaps due to low metallicity. GRBs similar in nature to GRB 130427A, inhabiting low-density media and exhibiting strong reverse shocks, are probably not uncommon but may have been difficult to recognize in the past owing to their relatively faint late-time radio emission; more such events should be found in abundance by the new generation of sensitive radio and millimeter instruments.
Published: 2014

15. GRB 130606A within a sub-DLA at redshift 5.91

Author: Castro-Tirado, A. J., Sánchez-Ramírez, R., Ellison, S. L., Jelínek, M., Martín-Carrillo, A., Bromm, V., Gorosabel, J., Bremer, M., Winters, J. M., Hanlon, L., Meegan, S., Topinka, M., Pandey, S. B., Guziy, S., Jeong, S., Sonbas, E., Pozanenko, A. S., Cunniffe, R., Fernández-Muñoz, R., Ferrero, P., Gehrels, N., Hudec, R., Kubánek, P., Lara-Gil, O., Muñoz-Martínez, V. F., Pérez-Ramírez, D., Štrobl, J., Álvarez-Iglesias, C., Inasaridze, R., Rumyantsev, V., Volnova, A., Hellmich, S., Mottola, S., Castro Cerón, J. M., Cepa, J., Göğüş, E., Tolga Guver, Önal Taş, Ö, Park, I. H., Sabau-Graziati, L., and Tejero, A.
Subjects: High Energy Astrophysical Phenomena (astro-ph.HE), Astrophysics::High Energy Astrophysical Phenomena, FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics - High Energy Astrophysical Phenomena
Abstract: Events such as GRB130606A at z=5.91, offer an exciting new window into pre-galactic metal enrichment in these very high redshift host galaxies. We study the environment and host galaxy of GRB 130606A, a high-z event, in the context of a high redshift population of GRBs. We have obtained multiwavelength observations from radio to gamma-ray, concentrating particularly on the X-ray evolution as well as the optical photometric and spectroscopic data analysis. With an initial Lorentz bulk factor in the range \Gamma_0 ~ 65-220, the X-ray afterglow evolution can be explained by a time-dependent photoionization of the local circumburst medium, within a compact and dense environment. The host galaxy is a sub-DLA (log N (HI) = 19.85+/-0.15), with a metallicity content in the range from ~1/7 to ~1/60 of solar. Highly ionized species (N V and Si IV) are also detected. This is the second highest redshift burst with a measured GRB-DLA metallicity and only the third GRB absorber with sub-DLA HI column density. GRB ' lighthouses' therefore offer enormous potential as backlighting sources to probe the ionization and metal enrichment state of the IGM at very high redshifts for the chemical signature of the first generation of stars., Comment: 10 pages, 9 figures, submitted to A&A. Typos corrected
Published: 2013

16. THE FIRST FERMI -LAT GAMMA-RAY BURST CATALOG

Author: Ackermann, M., Ajello, M., Asano, K., Axelsson, M., Baldini, L., Ballet, J., Barbiellini, G., Bastieri, D., Bechtol, K., Bellazzini, R., Bhat, P. N., Bissaldi, E., Bloom, E. D., Bonamente, E., Bonnell, J., Bouvier, A., Brandt, T. J., Bregeon, J., Brigida, M., Bruel, P., Buehler, R., Burgess, J. Michael, Buson, S., Byrne, D., Caliandro, G. A., Cameron, R. A., Caraveo, P. A., Cecchi, C., Charles, E., Chaves, R. C. G., Chekhtman, A., Chiang, J., Chiaro, G., Ciprini, S., Claus, R., Cohen-Tanugi, J., Connaughton, V., Conrad, J., Cutini, S., D'Ammando, F., de, Angelis A., de, Palma F., Dermer, C. D., Desiante, R., Digel, S. W., Dingus, B. L., Di, Venere L., Drell, P. S., Drlica-Wagner, A., Dubois, R., Favuzzi, C., Ferrara, E. C., Fitzpatrick, G., Foley, S., Franckowiak, A., Fusco, P., Gargano, F., Gasparrini, D., Gehrels, N., Germani, S., Giglietto, N., Giommi, P., Giordano, F., Giroletti, M., Glanzman, T., Godfrey, G., Goldstein, A., Granot, J., Grenier, I. A., Grove, J. E., Gruber, D., Guiriec, S., Hadasch, D., Horan, D., Hou, X., Hughes, R. E., Inoue, Y., Jackson, M. S., Jogler, T., Johannesson, G., Johnson, A. S., Johnson, W. N., Kawano, T., Kippen, R. M., Knodlseder, J., Kocevski, D., Kouveliotou, C., Kuss, M., Lande, J., Larsson, S., Latronico, L., Lee, S.-H., Longo, F., Loparco, F., Lovellette, M. N., Lubrano, P., Massaro, F., Mayer, M., Mazziotta, M. N., McBreen, S., McEnery, J. E., McGlynn, S., Michelson, P. F., Moiseev, A. A., Monte, C., Monzani, M. E., Moretti, E., Morselli, A., Murgia, S., Nemmen, R., Nuss, E., Nymark, T., Omodei, N., Orienti, M., Orlando, E., Paciesas, W. S., Paneque, D., Panetta, J. H., Pelassa, V., Perkins, J. S., Pesce-Rollins, M., Piron, F., Pivato, G., Porter, T. A., Preece, R., Racusin, J. L., Raino, S., Rando, R., Rau, A., Razzano, M., Razzaque, S., Reimer, A., Reimer, O., Reposeur, T., Ritz, S., Romoli, C., Roth, M., Ryde, F., Saz, Parkinson P. M., Schalk, T. L., Sgro, C., Siskind, E. J., Sonbas, E., Spandre, G., Spinelli, P., Suson, D. J., Takeuchi, Y., Fukazawa, Yasushi, Hanabata, Yoshitaka, Hayashida, Masaaki, Kamae, Tsuneyoshi, Kataoka, Jun, Mizuno, Tsunefumi, Ohno, Masanori, Ohsugi, Takashi, Tajima, Hiroyasu, Takahashi, Hiromitsu, Tanaka, Yasuyuki, 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 de recherche en astrophysique et planétologie (IRAP), 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), 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), Istituto Nazionale di Fisica Nucleare, sezione di Bari (INFN, sezione di Bari), Istituto Nazionale di Fisica Nucleare (INFN), IEEC-CSIC, Universitat Autònoma de Barcelona (UAB), FERMI, Centre d'Etudes Nucléaires de Bordeaux Gradignan (CENBG), 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), 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)-Centre National de la Recherche Scientifique (CNRS), Fermi-LAT, High Energy Astrophys. & Astropart. Phys (API, FNWI), Ackermann M, Ajello M, Asano K, Axelsson M, Baldini L, Ballet J, Barbiellini G, Bastieri D, Bechtol K, Bellazzini R, Bhat P N, Bissaldi E, Bloom E D, Bonamente E, Bonnell J, Bouvier A, Brandt T J, Bregeon J, Brigida M, Bruel P, Buehler R, Burgess J Michael, Buson S, Byrne D, Caliandro G A, Cameron R A, Caraveo P A, Cecchi C, Charles E, Chaves R C G, Chekhtman A, Chiang J, Chiaro G, Ciprini S, Claus R, Cohen-Tanugi J, Connaughton V, Conrad J, Cutini S, DAmmando F, de Angelis A, de Palma F, Dermer C D, Desiante R, Digel S W, Dingus B L, Di Venere L, Drell P S, Drlica-Wagner A, Dubois R, Favuzzi C, Ferrara E C, Fitzpatrick G, Foley S, Franckowiak A, Fukazawa Y, Fusco P, Gargano F, Gasparrini D, Gehrels N, Germani S, Giglietto N, Giommi P, Giordano F, Giroletti M, Glanzman T, Godfrey G, Goldstein A, Granot J, Grenier I A, Grove J E, Gruber D, Guiriec S, Hadasch D, Hanabata Y, Hayashida M, Horan D, Hou X, Hughes R E, Inoue Y, Jackson M S, Jogler T, Jóhannesson G, Johnson A S, Johnson W N, Kamae T, Kataoka J, Kawano T, Kippen R M, Knödlseder J, Kocevski D, Kouveliotou C, Kuss M, Lande J, Larsson S, Latronico L, Lee S-H, Longo F, Loparco F, Lovellette M N, Lubrano P, Massaro F, Mayer M, Mazziotta M N, McBreen S, McEnery J E, McGlynn S, Michelson P F, Mizuno T, Moiseev A A, Monte C, Monzani M E, Moretti E, Morselli A, Murgia S, Nemmen R, Nuss E, Nymark T, Ohno M, Ohsugi T, Omodei N, Orienti M, Orlando E, Paciesas W S, Paneque D, Panetta J H, Pelassa V, Perkins J S, Pesce-Rollins M, Piron F, Pivato G, Porter T A, Preece R, Racusin J L, Rainò S, Rando R, Rau A, Razzano M, Razzaque S, Reimer A, Reimer O, Reposeur T, Ritz S, Romoli C, Roth M, Ryde F, Saz Parkinson P M, Schalk T L, Sgrò C, Siskind E J, Sonbas E, Spandre G, Spinelli P, Suson D J, Tajima H, Takahashi H, Takeuchi Y, Tanaka Y, Thayer J G, Thayer J B, Thompson D J, Tibaldo L, Tierney D, Tinivella M, Torres D F, Tosti G, Troja E, Tronconi V, Usher T L, Vandenbroucke J, van der Horst A J, Vasileiou V, Vianello G, Vitale V, von Kienlin A, Winer B L, Wood K S, Wood M, Xiong S, Yang Z, Ackermann, M., Ajello, M., Asano, K., Axelsson, M., Baldini, L., Ballet, J., BARBIELLINI AMIDEI, Guido, Bastieri, D., Bechtol, K., Bellazzini, R., Bhat, P. N., Bissaldi, Elisabetta, Bloom, E. D., Bonamente, E., Bonnell, J., Bouvier, A., Brandt, T. J., Bregeon, J., Brigida, M., Bruel, P., Buehler, R., Burgess, J. M., Buson, S., Byrne, D., Caliandro, G. A., Cameron, R. A., Caraveo, P. A., Cecchi, C., Charles, E., R. C. G., Chekhtman, A., Chiang, J., Chiaro, G., Ciprini, S., Claus, R., Cohen Tanugi, J., Connaughton, V., Conrad, J., Cutini, S., D'Ammando, F., Angelis, A. d., Palma, F. d., Dermer, C. D., Desiante, R., Digel, S. W., Dingus, B. L., Venere, L. D., Drell, P. S., Drlica Wagner, A., Dubois, R., Favuzzi, C., Ferrara, E. C., Fitzpatrick, G., Foley, S., Franckowiak, A., Fukazawa, Y., Fusco, P., Gargano, F., Gasparrini, D., Gehrels, N., Germani, S., Giglietto, N., Giommi, P., Giordano, F., Giroletti, M., Glanzman, T., Godfrey, G., Goldstein, A., Granot, J., Grenier, I. A., Grove, J. E., Gruber, D., Guiriec, S., Hadasch, D., Hanabata, Y., Hayashida, M., Horan, D., Hou, X., Hughes, R. E., Inoue, Y., Jackson, M. S., Jogler, T., Johannesson, G., Johnson, A. S., Johnson, W. N., Kamae, T., Kataoka, J., Kawano, T., Kippen, R. M., Knoedlseder, J., Kocevski, D., Kouveliotou, C., Kuss, M., Lande, J., Larsson, S., Latronico, L., S. . . H., Longo, Francesco, Loparco, F., Lovellette, M. N., Lubrano, P., Massaro, F., Mayer, M., Mazziotta, M. N., Mcbreen, S., Mcenery, J. E., Mcglynn, S., Michelson, P. F., Mizuno, T., Moiseev, A. A., Monte, C., Monzani, M. E., Moretti, E., Morselli, A., Murgia, S., Nemmen, R., Nuss, E., Nymark, T., Ohno, M., Ohsugi, T., Omodei, N., Orienti, M., Orlando, E., Paciesas, W. S., Paneque, D., Panetta, J. H., Pelassa, V., Perkins, J. S., Pesce Rollins, M., Piron, F., Pivato, G., Porter, T. A., Preece, R., Racusin, J. L., Raino, S., Rando, R., Rau, A., Razzano, M., Razzaque, S., Reimer, A., Reimer, O., Reposeur, T., Ritz, S., Romoli, C., Roth, M., Ryde, F., Saz, P. M., Schalk, T. L., Sgro, C., Siskind, E. J., Sonbas, E., Spandre, G., Spinelli, P., Suson, D. J., Tajima, H., Takahashi, H., Takeuchi, Y., Tanaka, Y., Thayer, J. G., Thayer, J. B., Thompson, D. J., Tibaldo, L., Tierney, D., Tinivella, M., Torres, D. F., Tosti, G., Troja, E., Tronconi, V., Usher, T. L., Vandenbroucke, J., Van, A. J., Vasileiou, V., Vianello, G., Vitale, V., Kienlin, A. v., Winer, B. L., Wood, K. S., Wood, M., Xiong, S., Yang, Z., 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 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), Centre National de la Recherche Scientifique (CNRS)-École polytechnique (X)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3), 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), 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), 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), Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS), National Institute for Nuclear Physics (INFN), Universitat Autònoma de Barcelona [Barcelona] (UAB), 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: [PHYS.ASTR.HE]Physics [physics]/Astrophysics [astro-ph]/High Energy Astrophysical Phenomena [astro-ph.HE], Astrophysics::High Energy Astrophysical Phenomena, gamma-ray burst: general, Catalogs, methods: data analysis, Astrophysics, general [gamma-ray burst], catalogs , gamma-ray burst: general , methods: data analysis, 01 natural sciences, Spectral line, law.invention, Telescope, law, 0103 physical sciences, data analysis [methods], 010303 astronomy & astrophysics, Physics, catalogs, gamma-ray burst: general, methods: data analysis, 010308 nuclear & particles physics, [SDU.ASTR.HE]Sciences of the Universe [physics]/Astrophysics [astro-ph]/High Energy Astrophysical Phenomena [astro-ph.HE], Astrophysics::Instrumentation and Methods for Astrophysics, Astronomy, GRB 130427A, Astronomy and Astrophysics, Spectral bands, Gamma-ray astronomy, Spectral component, Space and Planetary Science, ddc:520, Catalog, Astrophysics - High Energy Astrophysical Phenomena, Gamma-ray burst, catalogs, Fermi Gamma-ray Space Telescope
Abstract: 著者人数: 180名, Accepted: 2013-07-15, 資料番号: SA1004573000
Published: 2013

17. The Afterglow of GRB 130427A from 1 to 10^16 GHz

Author: Perley, D. A., Cenko, S. B., Corsi, A., Tanvir, N. R., Levan, A. J., Kann, D. A., Sonbas, E., Wiersema, K., Zheng, W., Zhao, X. -H., Bai, J. -M., Bremer, M., Castro-Tirado, A. J., Chang, L., Clubb, K. I., Frail, D., Fruchter, A., G��, E., Greiner, J., G��ver, T., Horesh, A., Filippenko, A. V., Klose, S., Mao, J., Morgan, A. N., Pozanenko, A. S., Schmidl, S., Stecklum, B., Tanga, M., Volnova, A. A., Volvach, A. E., Wang, J. -G., Winters, J. -M., and Xin, Y. -X.
Subjects: High Energy Astrophysical Phenomena (astro-ph.HE), Astrophysics::High Energy Astrophysical Phenomena, FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics::Galaxy Astrophysics
Abstract: We present multiwavelength observations of the afterglow of GRB 130427A, the brightest (in total fluence) gamma-ray burst of the past 29 years. Optical spectroscopy from Gemini-North reveals the redshift of the GRB to be z=0.340, indicating that its unprecedented brightness is primarily the result of its relatively close proximity to Earth; the intrinsic luminosities of both the GRB and its afterglow are not extreme in comparison to other bright GRBs. We present a large suite of multiwavelength observations spanning from 300 s to 130 d after the burst and demonstrate that the afterglow shows relatively simple, smooth evolution at all frequencies with no significant late-time flaring or rebrightening activity. The entire dataset from 1 GHz to 10 GeV can be modeled as synchrotron emission from a combination of reverse and forward shocks in good agreement with the standard afterglow model, providing strong support to the applicability of the underlying theory and clarifying the nature of the GeV emission observed to last for minutes to hours following other very bright GRBs. A tenuous, wind-stratified circumburst density profile is required by the observations, suggesting a massive-star progenitor with a low mass-loss rate, perhaps due to low metallicity. GRBs similar in nature to GRB 130427A, inhabiting low-density media and exhibiting strong reverse shocks, are probably not uncommon but may have been difficult to recognize in the past due to their relatively faint late-time radio emission; more such events should be found in abundance by the new generation of sensitive radio and millimeter instruments., Accepted to ApJ. Light curves and SEDs are available at http://www.astro.caltech.edu/~dperley/grb/130427a/data/
Published: 2013
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18. X - Ray Flares and Their Connection With Prompt Emission in GRBs

Author: Sonbas, E., MacLachlan, G. A., Shenoy, A., Dhuga, K. S., and Parke, W. C.
Subjects: High Energy Astrophysical Phenomena (astro-ph.HE), Astrophysics::High Energy Astrophysical Phenomena, FOS: Physical sciences, Astrophysics - High Energy Astrophysical Phenomena
Abstract: We use a wavelet technique to investigate the time variations in the light curves from a sample of GRBs detected by Fermi and Swift. We focus primarily on the behavior of the flaring region of Swift-XRT light curves in order to explore connections between variability time scales and pulse parameters (such as rise and decay times, widths, strengths, and separation distributions) and spectral lags. Tight correlations between some of these temporal features suggest a common origin for the production of X-ray flares and the prompt emission., Comment: 7th Huntsville Gamma-Ray Burst Symposium, GRB 2013: paper 15 in eConf Proceedings C1304143
Published: 2013
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19. The Minimum Variability Time Scale and its Relation to Pulse Profiles of Fermi GRBs

Author: MacLachlan, G. A., Shenoy, A., Sonbas, E., Dhuga, K. S., Eskandarian, A., Maximon, L. C., and Parke, W. C.
Subjects: High Energy Astrophysical Phenomena (astro-ph.HE), FOS: Physical sciences, Astrophysics - High Energy Astrophysical Phenomena
Abstract: We present a direct link between the minimum variability time scales extracted through a wavelet decomposition and the rise times of the shortest pulses extracted via fits of 34 Fermi GBM GRB light curves comprised of 379 pulses. Pulses used in this study were fitted with log-normal functions whereas the wavelet technique used employs a multiresolution analysis that does not rely on identifying distinct pulses. By applying a corrective filter to published data fitted with pulses we demonstrate agreement between these two independent techniques and offer a method for distinguishing signal from noise., Comment: Accepted for publication in MNRAS Letters. 4 pages, 4 figures
Published: 2012
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20. An unusual stellar death on Christmas Day

Author: Thöne, C. C., Postigo, A. de Ugarte, Fryer, C. L., Page, K. L., Gorosabel, J., Aloy, M. A., Perley, D. A., Kouveliotou, C., Janka, H. T., Mimica, P., Racusin, J. L., Krimm, H., Cummings, J., Oates, S. R., Holland, S. T., Siegel, M. H., De Pasquale, M., Sonbas, E., Im, M., Park, W. -K., Kann, D. A., Guziy, S., Garcia, L. Hernandez, Llorente, A., Bundy, K., Choi, C., Jeong, H., Korhonen, H., Kubanek, P., Lim, J., Moskvitin, A., Darias, T. Muñoz, Pak, S., and Parrish, I.
Subjects: High Energy Astrophysical Phenomena (astro-ph.HE), Astrophysics::High Energy Astrophysical Phenomena, Astrophysics::Solar and Stellar Astrophysics, FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics - High Energy Astrophysical Phenomena, Astrophysics::Galaxy Astrophysics
Abstract: Long Gamma-Ray Bursts (GRBs) are the most dramatic examples of massive stellar deaths, usually as- sociated with supernovae (Woosley et al. 2006). They release ultra-relativistic jets producing non-thermal emission through synchrotron radiation as they interact with the surrounding medium (Zhang et al. 2004). Here we report observations of the peculiar GRB 101225A (the "Christmas burst"). Its gamma-ray emission was exceptionally long and followed by a bright X-ray transient with a hot thermal component and an unusual optical counterpart. During the first 10 days, the optical emission evolved as an expanding, cooling blackbody after which an additional component, consistent with a faint supernova, emerged. We determine its distance to 1.6 Gpc by fitting the spectral-energy distribution and light curve of the optical emission with a GRB-supernova template. Deep optical observations may have revealed a faint, unresolved host galaxy. Our proposed progenitor is a helium star-neutron star merger that underwent a common envelope phase expelling its hydrogen envelope. The resulting explosion created a GRB-like jet which gets thermalized by interacting with the dense, previously ejected material and thus creating the observed black-body, until finally the emission from the supernova dominated. An alternative explanation is a minor body falling onto a neutron star in the Galaxy (Campana et al. 2011)., Comment: 41 pages, 21 figures, accepted for publication in the original journal!
Published: 2011
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21. A Proposal to Localize Fermi GBM GRBs Through Coordinated Scanning of the GBM Error Circle via Optical Telescopes

Author: Ukwatta, T. N., Linnemann, J. T., Tollefson, K., Abeysekara, A. U., Bhat, P. N., Sonbas, E., and Gehrels, N.
Subjects: High Energy Astrophysical Phenomena (astro-ph.HE), Astrophysics::High Energy Astrophysical Phenomena, Astrophysics::Instrumentation and Methods for Astrophysics, FOS: Physical sciences, Astrophysics - High Energy Astrophysical Phenomena
Abstract: We investigate the feasibility of implementing a system that will coordinate ground-based optical telescopes to cover the Fermi GBM Error Circle (EC). The aim of the system is to localize GBM detected GRBs and facilitate multi-wavelength follow-up from space and ground. This system will optimize the observing locations in the GBM EC based on individual telescope location, Field of View (FoV) and sensitivity. The proposed system will coordinate GBM EC scanning by professional as well as amateur astronomers around the world. The results of a Monte Carlo simulation to investigate the feasibility of the project are presented., Comment: 2011 Fermi Symposium proceedings - eConf C110509
Published: 2011
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22. The Lag-Luminosity Relation in the GRB Source-Frame: An Investigation with Swift BAT Bursts

Author: Ukwatta, T. N., Dhuga, K. S., Stamatikos, M., Dermer, C. D., Sakamoto, T., Sonbas, E., Parke, W. C., Maximon, L. C., Linnemann, J. T., Bhat, P. N., Eskandarian, A., Gehrels, N., Abeysekara, U., Tollefson, K., and Norris, J. P.
Subjects: High Energy Astrophysical Phenomena (astro-ph.HE), Astrophysics::High Energy Astrophysical Phenomena, FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics - High Energy Astrophysical Phenomena
Abstract: Spectral lag, which is defined as the difference in time of arrival of high and low energy photons, is a common feature in Gamma-ray Bursts (GRBs). Previous investigations have shown a correlation between this lag and the isotropic peak luminosity for long duration bursts. However, most of the previous investigations used lags extracted in the observer-frame only. In this work (based on a sample of 43 Swift long GRBs with known redshifts), we present an analysis of the lag-luminosity relation in the GRB source-frame. Our analysis indicates a higher degree of correlation -0.82 +/- 0.05 (chance probability of ~ 5.5 x 10^-5) between the spectral lag and the isotropic peak luminosity, Liso, with a best-fit power-law index of -1.2 +/- 0.2, such that Liso proportional to lag^-1.2. In addition, there is an anti-correlation between the source-frame spectral lag and the source-frame peak energy of the burst spectrum, E_pk(1+z)., Comment: 11 pages, 6 figures, 6 table; Accepted for publication in MNRAS
Published: 2011
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23. Study of Envelope Velocity Evolution of Type Ib-c Core-Collapse Supernovae from Observations of XRF 080109 / SN 2008D and GRB 060218 / SN 2006aj with BTA

Author: Moskvitin, A. S., Sonbas, E., Sokolov, V. V., Fatkhullin, T. A., and Castro-Tirado, A. J.
Subjects: High Energy Astrophysical Phenomena (astro-ph.HE), Astrophysics::High Energy Astrophysical Phenomena, FOS: Physical sciences, Astrophysics::Solar and Stellar Astrophysics, Astrophysics - High Energy Astrophysical Phenomena
Abstract: Results of modeling the spectra of two supernovae SN 2008D and SN 2006aj related to the X-ray flash XRF 080109 and gamma-ray burst GRB / XRF 060218, respectively, are studied. The spectra were obtained with the 6-meter BTA telescope of the Special Astrophysical Observatory of the Russian Academy of Sciences in 6.48 and 27.61 days after the explosion of SN 2008D, and in 2.55 and 3.55 days after the explosion of SN 2006aj. The spectra were interpreted in the Sobolev approximation with the SYNOW code. An assumption about the presence of envelopes around the progenitor stars is confirmed by an agreement between the velocities of lines interpreted as hydrogen and helium, and the empiric power-law velocity drop with time for the envelopes of classic core-collapse supernovae. Detection of a P Cyg profile of the H-beta line in the spectra of optical afterglows of GRBs can be a determinative argument in favor of this hypothesis., 12 pages, 6 figures, accepted for publication in Astrophysical Bulletin.
Published: 2010

24. An optical search for supernova remnants in the nearby spiral galaxy NGC 2903 (research note)

Author: Sonbas E., Akyuz A., Balman S., and Çukurova Üniversitesi
Subjects: Galaxies: individual, Galaxies: spiral, ISM: supernova remnants, NGC 2903
Abstract: Aims. We present the results of an optical search for supernova remnants (SNRs) in the nearby spiral galaxy NGC 2903. Methods. Interference filter images and spectral, data were taken in March 2005 with the f/7.7 1.5 m Russian Turkish Telescope (RTT1.50) at TUBITAK National Observatory (TUG). Spectral data were obtained with the 6 m. BTA (Bolshoi Azimuthal Telescope, Russia). We used the SNR identification criterion that consists of constructing the continuum-subtracted H? and continuum-subtracted [SU]??6716, 6731 images and their ratios. Results. Five SNR candidates were identified in NGC 2903 with [SII]/H? ratios ranging from 0.41-0.74 and H? intensities ranging from 9.4 × 10-15 to 1.7 × 10 -14 erg cm-2 s-1. This work represents the first identification of SNRs by an optical survey in NGC 2903. We present the spectrum of one of the bright candidates and derive an [SII]/H? emission line ratio of 0.42 for this source. In addition, the weak [OIII]?5007/ Hß emission line ratio in the spectrum of this SNR indicates an old oxygen-deficient remnant with a low propagation velocity. © ESO 2009.
Published: 2009

25. Optical and infrared flares from a transient Galactic soft gamma-ray repeater

Author: Castro-Tirado, A. J., Postigo, A. de Ugarte, Gorosabel, J., Jelinek, M., Fatkhullin, T. A., Sokolov, V. V., Ferrero, P., Kann, D. A., Klose, S., Sluse, D., Bremer, M., Winters, J. M., Nuernberger, D., Perez-Ramirez, D., Guerrero, M. A., French, J., Melady, G., Hanlon, L., McBreen, B., Aceituno, F. J., Cunniffe, R., Kubanek, P., Vitek, S., Schulze, S., Wilson, A. C., Hudec, R., Gonzalez-Perez, J. M., Shahbaz, T., Guziy, S., Pandey, S. B., Pavlenko, L., Sonbas, E., Trushkin, S. A., Bursov, N. N., Nizhelskij, N. A., and Sabau-Graziati, L.
Subjects: Astrophysics::High Energy Astrophysical Phenomena, Astrophysics (astro-ph), FOS: Physical sciences, Astrophysics::Solar and Stellar Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, Astrophysics::Galaxy Astrophysics
Abstract: Soft gamma-ray repeaters (SGRs) are a rare type of gamma-ray transient sources that are ocasionally detected as bursts in the high-energy sky. They are thought to be produced by magnetars, young neutron stars with very strong magnetic fields of the order of 10^(14-15) G. Only three such objects are known in our Galaxy, and a fourth one is associated with the supernova remnant N49 in the Large Magellanic Cloud. In none of these cases has an optical counterpart to either the gamma-ray flares or the quiescent source been identified. Here we present multi-wavelength observations of a puzzling source, SWIFT J195509+261406, for which we detected more than 40 flaring episodes in the optical band over a time span of 3 days, plus a faint infrared flare 11 days later, after which it returned to quiescence. We propose that SWIFT J195509+261406 is a member of a subgroup of SGRs for which the long-term X-ray emission is transient in nature. Furthermore, it is the first SGR for which bursts have been detected in the optical and near-infrared bands and maybe the link between the "persistent" SGRs and the dim isolated neutron stars., Version submitted to Nature on 31 Jan 2008. A substantially revised version of this work has been published in Nature, vol. 455 issue 7212 pp 506-509 under the title "Flares from a Galactic magnetar suggest a missing link to dim isolated neutron stars"
Published: 2008

26. The stellar-wind envelope around the supernova XRF/GRB060218/SN2006aj massive progenitor star

Author: Sonbas, E., Moskvitin, A. S., Fatkhullin, T. A., Sokolov, V. V., Castro-Tirado, A., Antonio de Ugarte Postigo, Gorosabel, J., Guziy, S., Jelinek, M., Sokolova, T. N., and Chernenkov, V. N.
Subjects: Astrophysics (astro-ph), FOS: Physical sciences, Astrophysics
Abstract: In BTA spectra of the supernova SN2006aj, identified with the X-ray flash (XRF) and gamma-ray burst XRF/GRB060218/SN2006aj, we detected details interpreted as hydrogen lines, which is a sign of stellar-wind envelope around a massive progenitor star of the gamma-ray burst. Results of modeling two early spectra obtained with the BTA in 2.55 and 3.55 days after the explosion of Type Ic supernova SN2006aj (z=0.0331) are presented. The spectra were modeled in the Sobolev approximation with the SYNOW code (Branch et al. 2001; Elmhamdi et al. 2006). In the spectra of the optical afterglow of the X-ray flash XRF/GRB060218 we detected spectral features interpreted as (1) the H_alpha PCyg profile for the velocity 33000 km s$^{-1}$ -- a wide and almost unnoticeable deformation of continuum in the range of $\simeq5600 - 6600\AA$ for the first epoch (2.55 days) and (2) a part (``remnant'') of the H_alpha PCyg profile in absorption blueshifted by 24000 km s$^{-1}$ -- a wide spectral feature with a minimum at $\simeq6100\AA$ (the rest wavelength) for the second epoch (3.55 days). Taking into consideration early BTA observations and spectra obtained with other telescopes (ESO Lick, ESO VLT, NOT) before 2006 Feb. 23 UT, it can be said that we observe evolution of optical spectra of Type Ic core-collapse supernova SN 2006aj during {\it transition} from the short phase related to the shock breakout to outer layers of the stellar-wind envelope to spectra of the phase of increasing brightness corresponding to radioactive heating. Signs of hydrogen in spectra of the gamma-ray burst afterglow were detected for the first time., Comment: 26 pages, 7 figures, 3 tables, Accepted for publication in Astrophysical Bulletin, 2008, v. 63, No 3
Published: 2008
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27. GRB 101225A: a stellar murder on Christmas Day

Author: Aloy, M., Thöne, C., Ugarte-Postigo, A., Fryer, C. L., Page, K. L., Gorosabel, J., Perley, D. A., Kouveliotou, C., Janka, H. T., Petar Mimica, Racusin, J., Krimm, H., Cummings, J., Oates, S. R., Holland, S. T., Siegel, M. H., Pasquale, M., Sonbas, E., Im, M., Park, W. -K, Kann, D. A., Guziy, S., Garcia, L., Liotente, A., Bundy, K., Choi, C., Jeong, H., Korhonen, H., Kubànek, P., Lim, J., Moskvitin, A., Muñoz-Darias, T., Pak, S., and Parrish, I.

28. Optical search for supernova remnants in two-spiral galaxies

Author: Akyuz, A., SOLEN BALMAN, Bhattacharya, D., Sonbas, E., Cekmecelioglu, E., and Çukurova Üniversitesi
Subjects: Astrophysics::High Energy Astrophysical Phenomena, Astrophysics::Cosmology and Extragalactic Astrophysics, SNR, Optical Observation, Astrophysics::Galaxy Astrophysics
Abstract: X-ray Universe 2005 --26 September 2005 through 30 September 2005 -- Madrid -- We present the results of an optical search for Supernova Remnants (SNRs) in the spiral galaxies NGC6946 and NGC628. The SNR identification technique consisted of constructing continuum-subtracted H? and [SII] ?? 6716,6731 images and then using [SII] / H? ratios obtained from the image. 32 emission nebulae have been detected as SNR candidates in NGC6946. 22 of them were previously identified by Matonick et al (1997). We found five SNR candidates in the spiral galaxy NGC628. We will compare and contrast the new SNR candidates and our optical data with the existing Chandra and XMM observation of the two galaxies of interest and VLA radio observation of NGC6946. Interference-filter CCD images of two spiral galaxies were taken in 2004 September with the f/7.7 1.5 m Russian-Turkish Telescope at Turkish National Observatory.

29. GRB 110407A: Swift detection of a burst

Author: Wolf, C. W., Barthelmy, S. D., Beardmore, A. P., Campana, S., Valerio D'Elia, Evans, P. A., Gehrels, N., Gelbord, J. M., Gendre, B., Guidorzi, C., Holland, S. T., Kennea, J. A., Krimm, H. A., Littlejohns, O. M., Mangano, V., O Brien, P. T., Osborne, J. P., Pagani, C., Page, K. L., Romano, P., Siegel, M. H., Sonbas, E., Starling, R. L. C., Stratta, G., Stroh, M. C., Swenson, C. A., Tagliaferri, G., Troja, E., and Ukwatta, T. N.

30. The 2017 May 20 stellar occultation by the elongated centaur (95626) 2002 GZ32

Author: Santos-Sanz, P. Ortiz, J.L. Sicardy, B. Benedetti-Rossi, G. Morales, N. Fernández-Valenzuela, E. Duffard, R. Iglesias-Marzoa, R. Lamadrid, J.L. Maícas, N. Pérez, L. Gazeas, K. Guirado, J.C. Peris, V. Ballesteros, F.J. Organero, F. Ana-Hernández, L. Fonseca, F. Alvarez-Candal, A. Jiménez-Teja, Y. Vara-Lubiano, M. Braga-Ribas, F. Camargo, J.I.B. Desmars, J. Assafin, M. Vieira-Martins, R. Alikakos, J. Boutet, M. Bretton, M. Carbognani, A. Charmandaris, V. Ciabattari, F. Delincak, P. Fuambuena Leiva, A. González, H. Haymes, T. Hellmich, S. Horbowicz, J. Jennings, M. Kattentidt, B. Kiss, Cs. Komzík, R. Lecacheux, J. Marciniak, A. Moindrot, S. Mottola, S. Pal, A. Paschalis, N. Pastor, S. Perello, C. Pribulla, T. Ratinaud, C. Reyes, J.A. Sanchez, J. Schnabel, C. Selva, A. Signoret, F. Sonbas, E. Alí-Lagoa, V.
Abstract: We predicted a stellar occultation of the bright star Gaia DR1 4332852996360346368 (UCAC4 385-75921) (mV = 14.0 mag) by the centaur 2002 GZ32 for 2017 May 20. Our latest shadow path prediction was favourable to a large region in Europe. Observations were arranged in a broad region inside the nominal shadow path. Series of images were obtained with 29 telescopes throughout Europe and from six of them (five in Spain and one in Greece) we detected the occultation. This is the fourth centaur, besides Chariklo, Chiron, and Bienor, for which a multichord stellar occultation is reported. By means of an elliptical fit to the occultation chords, we obtained the limb of 2002 GZ32 during the occultation, resulting in an ellipse with axes of 305 ± 17 km × 146 ± 8 km. From this limb, thanks to a rotational light curve obtained shortly after the occultation, we derived the geometric albedo of 2002 GZ32 (pV = 0.043 ± 0.007) and a 3D ellipsoidal shape with axes 366 km × 306 km × 120 km. This shape is not fully consistent with a homogeneous body in hydrostatic equilibrium for the known rotation period of 2002 GZ32. The size (albedo) obtained from the occultation is respectively smaller (greater) than that derived from the radiometric technique but compatible within error bars. No rings or debris around 2002 GZ32 were detected from the occultation, but narrow and thin rings cannot be discarded. © 2021 2020 The Author(s) Published by Oxford University Press on behalf of Royal Astronomical Society.

31. MULTIWAVELENGTH OBSERVATIONS OF GRB 110731A: GeV EMISSION FROM ONSET TO AFTERGLOW

Author: T. Ohsugi, Akihiko Fukui, W. S. Paciesas, P. Fusco, Eleonora Troja, G. Godfrey, Miranda Jackson, Dario Gasparrini, Marco Ajello, J. B. Thayer, S. Rainò, Tsunefumi Mizuno, S. Murgia, J. E. Grove, Yasushi Fukazawa, Luca Latronico, I. A. Grenier, O. Littlejohns, Matthew G. Baring, Daniel Sánchez, Peter Mészáros, L. Tibaldo, Jonathan Granot, A. De Angelis, R. M. Kippen, Judith Racusin, V. Vasileiou, Elisabetta Bissaldi, R. Filgas, S. Buson, M. Tinivella, F. de Palma, G. Tosti, F. Piron, Stefano Ciprini, Sheila McBreen, P. Bruel, Jan Conrad, C. Monte, T. Jogler, Nicola Omodei, Masanori Ohno, A. P. Waite, Hiromitsu Takahashi, Melissa Pesce-Rollins, Valerie Connaughton, Giacomo Vianello, T. L. Usher, J. G. Thayer, Takashi Sako, Luca Baldini, Eda Sonbas, Alex Drlica-Wagner, E. Orlando, A. Reimer, K. S. Wood, Jürgen Knödlseder, M. Roth, J. Mehault, D. Kocevski, S. McGlynn, A. S. Johnson, S. Cutini, V. Pelassa, E. J. Siskind, A. von Kienlin, David Gruber, Johan Bregeon, T. Glanzman, J. M. Burgess, P. N. Bhat, M. Naumann-Godo, Ronaldo Bellazzini, R. Buehler, C. Romoli, E. Hays, J. S. Perkins, S. J. Fegan, Igor V. Moskalenko, Julie McEnery, Brian L Winer, Nicola Giglietto, Katsuaki Asano, M. E. Monzani, Peter F. Michelson, Marcello Giroletti, Markus Ackermann, T. Nymark, Y. Hanabata, G. Pivato, Olaf Reimer, M. N. Lovellette, M. Hayashida, Robert D. Preece, P. A. Caraveo, A. Franckowiak, R. E. Hughes, Persis S. Drell, Charles D. Dermer, E. Do Couto E Silva, Eugenio Bottacini, Denis Bastieri, E. Moretti, F. D'Ammando, F. Loparco, C. Favuzzi, T. Krühler, W. Mitthumsiri, A. J. van der Horst, R. Claus, J. Lande, Sylvain Guiriec, F. Gargano, Johann Cohen-Tanugi, Zhenwei Yang, Daniela Hadasch, Michael S. Briggs, Carmelo Sgrò, Riccardo Rando, Francesco Longo, E. Nuss, David Paneque, M. Kuss, T. N. Ukwatta, Jay P. Norris, G. A. Caliandro, R. C. G. Chaves, James Chiang, Roger Blandford, M. Razzano, Soebur Razzaque, S. R. Oates, N. Gehrels, Suzanne Foley, Arne Rau, Gudlaugur Johannesson, Claudia Cecchi, Felix Ryde, M. Stamatikos, Justin Vandenbroucke, Guido Barbiellini, M. Orienti, A. Morselli, V. Vitale, A. Chekhtman, M. N. Mazziotta, M. Brigida, W. B. Focke, P. Spinelli, Chryssa Kouveliotou, S. Larsson, Francesco Giordano, R. A. Cameron, Jochen Greiner, S. Klose, Emanuele Bonamente, A. W. Borgland, Takaaki Tanaka, Paul J. Tristram, P. Lubrano, D. A. Kann, Eric Charles, Ackermann M, Ajello M, Asano K, Baldini L, Barbiellini G, Baring MG, Bastieri D, Bellazzini R, Blandford RD, Bonamente E, Borgland AW, Bottacini E, Bregeon J, Brigida M, Bruel P, Buehler R, Buson S, Caliandro GA, Cameron RA, Caraveo PA, Cecchi C, Charles E, Chaves RCG, Chekhtman A, Chiang J, Ciprini S, Claus R, Cohen-Tanugi J, Conrad J, Cutini S, DAmmando F, de Angelis A, de Palma F, Dermer CD, Silva EDE, Drell PS, Drlica-Wagner A, Favuzzi C, Fegan SJ, Focke WB, Franckowiak A, Fukazawa Y, Fusco P, Gargano F, Gasparrini D, Gehrels N, Giglietto N, Giordano F, Giroletti M, Glanzman T, Godfrey G, Granot J, Greiner J, Grenier IA, Grove JE, Guiriec S, Hadasch D, Hanabata Y, Hayashida M, Hays E, Hughes RE, Jackson MS, Jogler T, Johannesson G, Johnson AS, Knodlseder J, Kocevski D, Kuss M, Lande J, Larsson S, Latronico L, Longo F, Loparco F, Lovellette MN, Lubrano P, Mazziotta MN, McEnery JE, Mehault J, Meszaros P, Michelson PF, Mitthumsiri W, Mizuno T, Monte C, Monzani ME, Moretti E, Morselli A, Moskalenko IV, Murgia S, Naumann-Godo M, Norris JP, Nuss E, Nymark T, Ohno M, Ohsugi T, Omodei N, Orienti M, Orlando E, Paneque D, Perkins JS, Pesce-Rollins M, Piron F, Pivato G, Racusin JL, Raino S, Rando R, Razzano M, Razzaque S, Reimer A, Reimer O, Romoli C, Roth M, Ryde F, Sanchez DA, Sgro C, Siskind EJ, Sonbas E, Spinelli P, Stamatikos M, Takahashi H, Tanaka T, Thayer JG, Thayer JB, Tibaldo L, Tinivella M, Tosti G, Troja E, Usher TL, Vandenbroucke J, Vasileiou V, Vianello G, Vitale V, Waite AP, Winer BL, Wood KS, Yang Z, Gruber D, Bhat PN, Bissaldi E, Briggs MS, Burgess JM, Connaughton V, Foley S, Kippen RM, Kouveliotou C, McBreen S, McGlynn S, Paciesas WS, Pelassa V, Preece R, Rau A, van der Horst AJ, von Kienlin A, Kann DA, Filgas R, Klose S, Kruhler T, Fukui A, Sako T, Tristram PJ, Oates SR, Ukwatta TN, Littlejohns O, High Energy Astrophys. & Astropart. Phys (API, FNWI), Ackermann, M., Ajello, M., Asano, K., Baldini, L., BARBIELLINI AMIDEI, Guido, Baring, M. G., Bastieri, D., Bellazzini, R., Blandford, R. D., Bonamente, E., Borgland, A. W., Bottacini, E., Bregeon, J., Brigida, M., Bruel, P., Buehler, R., Buson, S., Caliandro, G. A., Cameron, R. A., Caraveo, P. A., Cecchi, C., Charles, E., Chaves, R. C. G., Chekhtman, A., Chiang, J., Ciprini, S., Claus, R., Cohen Tanugi, J., Conrad, J., Cutini, S., D'Ammando, F., de Angelis, A., de Palma, F., Dermer, C. D., Silva, E. do Couto e., Drell, P. S., Drlica Wagner, A., Favuzzi, C., Fegan, S. J., Focke, W. B., Franckowiak, A., Fukazawa, Y., Fusco, P., Gargano, F., Gasparrini, D., Gehrels, N., Giglietto, N., Giordano, F., Giroletti, M., Glanzman, T., Godfrey, G., Granot, J., Greiner, J., Grenier, I. A., Grove, J. E., Guiriec, S., Hadasch, D., Hanabata, Y., Hayashida, M., Hays, E., Hughes, R. E., Jackson, M. S., Jogler, T., Jóhannesson, G., Johnson, A. S., Knödlseder, J., Kocevski, D., Kuss, M., Lande, J., Larsson, S., Latronico, L., Longo, Francesco, Loparco, F., Lovellette, M. N., Lubrano, P., Mazziotta, M. N., Mcenery, J. E., Mehault, J., Mészáros, P., Michelson, P. F., Mitthumsiri, W., Mizuno, T., Monte, C., Monzani, M. E., Moretti, E., Morselli, A., Moskalenko, I. V., Murgia, S., Naumann Godo, M., Norris, J. P., Nuss, E., Nymark, T., Ohno, M., Ohsugi, T., Omodei, N., Orienti, M., Orlando, E., Paneque, D., Perkins, J. S., Pesce Rollins, M., Piron, F., Pivato, G., Racusin, J. L., Rainò, S., Rando, R., Razzano, M., Razzaque, S., Reimer, A., Reimer, O., Romoli, C., Roth, M., Ryde, F., Sanchez, D. A., Sgrò, C., Siskind, E. J., Sonbas, E., Spinelli, P., Stamatikos, M., Takahashi, H., Tanaka, T., Thayer, J. G., Thayer, J. B., Tibaldo, L., Tinivella, M., Tosti, G., Troja, E., Usher, T. L., Vandenbroucke, J., Vasileiou, V., Vianello, G., Vitale, V., Waite, A. P., Winer, B. L., Wood, K. S., Yang, Z., Gruber, D., Bhat, P. N., Bissaldi, Elisabetta, Briggs, M. S., Burgess, J. M., Connaughton, V., Foley, S., Kippen, R. M., Kouveliotou, C., Mcbreen, S., Mcglynn, S., Paciesas, W. S., Pelassa, V., Preece, R., Rau, A., van der Horst, A. J., von Kienlin, A., Kann, D. A., Filgas, R., Klose, S., Krühler, T., Fukui, A., Sako, T., Tristram, P. J., Oates, S. R., Ukwatta, T. N., and Littlejohns, O.
Subjects: Physics, Opacity, Astrophysics::High Energy Astrophysical Phenomena, Astronomy, Astronomy and Astrophysics, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, individual (GRB110731A) [gamma-ray burst], Light curve, gamma-ray burst: individual (GRB110731A), Afterglow, law.invention, Telescope, Lorentz factor, symbols.namesake, Space and Planetary Science, law, Observatory, symbols, ddc:520, Astrophysics - High Energy Astrophysical Phenomena, Gamma-ray burst, Astrophysics::Galaxy Astrophysics, Fermi Gamma-ray Space Telescope
Abstract: The astrophysical journal 763(2), 71 (2013). doi:10.1088/0004-637X/763/2/71, We report on the multiwavelength observations of the bright, long gamma-ray burst GRB 110731A, by the Fermi and Swift observatories, and by the MOA and GROND optical telescopes. The analysis of the prompt phase reveals that GRB 110731A shares many features with bright Large Area Telescope bursts observed by Fermi during the first three years on-orbit: a light curve with short time variability across the whole energy range during the prompt phase, delayed onset of the emission above 100 MeV, extra power-law component and temporally extended high-energy emission. In addition, this is the first GRB for which simultaneous GeV, X-ray, and optical data are available over multiple epochs beginning just after the trigger time and extending for more than 800 s, allowing temporal and spectral analysis in different epochs that favor emission from the forward shock in a wind-type medium. The observed temporally extended GeV emission is most likely part of the high-energy end of the afterglow emission. Both the single-zone pair transparency constraint for the prompt signal and the spectral and temporal analysis of the forward-shock afterglow emission independently lead to an estimate of the bulk Lorentz factor of the jet Γ ~ 500-550., Published by Univ.11032, Chicago, Ill. [u.a.]
Published: 2013

32. Fermi-LAT Observations of the Gamma-Ray Burst GRB 130427A

Author: P. A. Jenke, Brian L Winer, Soebur Razzaque, A. A. Moiseev, L. R. Cominsky, Igor V. Moskalenko, Melissa Gibby, Yoshiyuki Inoue, Justin D. Finke, Olaf Reimer, Katsuaki Asano, Robert D. Preece, F. Loparco, E. Moretti, André Schulz, Akira Okumura, George Younes, Matthew G. Baring, D. Byrne, William S. Paciesas, Chryssa Kouveliotou, C. Favuzzi, Judith Racusin, Melissa Pesce-Rollins, Charles A. Meegan, Robert R. Rando, T. Jogler, S. J. Fegan, Luca Baldini, J. G. Thayer, W. B. Focke, P. Spinelli, Sylvain Guiriec, Ryo Yamazaki, P. N. Bhat, Alex Drlica-Wagner, Shuze Zhu, A. von Kienlin, Vandiver Chaplin, Francesco Giordano, Anne M. Diekmann, M. E. Monzani, Jean Ballet, T. A. Porter, Hoi-Fung Yu, A. Franckowiak, J. Michael Burgess, G. Godfrey, W. N. Johnson, W. B. Atwood, Nicola Omodei, S. Rainò, Jeffrey D. Scargle, J. R. Cummings, J. S. Perkins, R. A. Cameron, Tsunefumi Mizuno, R. E. Hughes, Denis Bastieri, Misty Giles, Nicola Giglietto, Rodrigo Nemmen, Shaolin Xiong, Stefano Ciprini, D. Hadasch, S. Germani, K. S. Wood, T. Ohsugi, Eleonora Troja, Stefan Funk, Colleen A. Wilson-Hodge, P. Bruel, G. Chiaro, D. Horan, F. de Palma, A. C. Collazzi, Julie McEnery, V. Pelassa, A. J. van der Horst, Neil Gehrels, L. Di Venere, David Gruber, J. E. Grove, Yasushi Fukazawa, E. J. Siskind, Hiromitsu Takahashi, Valerie Connaughton, A. De Angelis, Adam Goldstein, M. Mayer, V. La Parola, D. J. Thompson, Carmelo Sgrò, G. Tosti, M. N. Lovellette, P. A. Caraveo, Persis S. Drell, M. Roth, Gudlaugur Johannesson, D. Kocevski, V. Vasileiou, Marco Ajello, J. B. Thayer, J. Lande, Jonathan Granot, S. Murgia, P. Fusco, E. Nuss, David Paneque, Sheila McBreen, M. Kuss, T. L. Usher, Francesco Longo, S. Buson, F. Piron, Giacomo Vianello, Masanori Ohno, Felix Ryde, W. H. Cleveland, Emanuele Bonamente, Charles D. Dermer, Magnus Axelsson, Alice K. Harding, I. A. Grenier, Markus Ackermann, Justin Vandenbroucke, Michael S. Briggs, Vahé Petrosian, Luca Latronico, Jürgen Knödlseder, Gloria Spandre, P. M. Saz Parkinson, Ronaldo Bellazzini, Johann Cohen-Tanugi, R. Desiante, T. Kawano, M. Tinivella, Elizabeth C. Ferrara, Guido Barbiellini, Stephen F. Foley, G. A. Caliandro, C. C. Cheung, M. Deklotz, Elisabetta Bissaldi, E. Hays, A. Morselli, F. Gargano, M. Orienti, V. Vitale, J. Bregeon, R. Claus, Alberto Sartori, Y. Hanabata, L. Tibaldo, G. Pivato, A. Reimer, M. Brigida, D. Tierney, M. N. Mazziotta, Eda Sonbas, Arne Rau, Giancarlo Cusumano, Claudia Cecchi, S. Larsson, Diego F. Torres, Gerard Fitzpatrick, S. Cutini, R. M. Kippen, James Chiang, M. Hayashida, Hiroyasu Tajima, Jan Conrad, R. Buehler, Peter F. Michelson, Marcello Giroletti, Eric Charles, Steven Ritz, A. Chekhtman, P. Lubrano, Keith Bechtol, M. Razzano, Filippo D'Ammando, Ackermann M, Ajello M, Asano K, Atwood WB, Axelsson M, Baldini L, Ballet J, Barbiellini G, Baring MG, Bastieri D, Bechtol K, Bellazzini R, Bissaldi E, Bonamente E, Bregeon J, Brigida M, Bruel P, Buehler R, Burgess JM, Buson S, Caliandro GA, Cameron RA, Caraveo PA, Cecchi C, Chaplin V, Charles E, Chekhtman A, Cheung CC, Chiang J, Chiaro G, Ciprini S, Claus R, Cleveland W, Cohen-Tanugi J, Collazzi A, Cominsky LR, Connaughton V, Conrad J, Cutini S, DAmmando F, de Angelis A, DeKlotz M, de Palma F, Dermer CD, Desiante R, Diekmann A, Di Venere L, Drell PS, Drlica-Wagner A, Favuzzi C, Fegan SJ, Ferrara EC, Finke J, Fitzpatrick G, Focke WB, Franckowiak A, Fukazawa Y, Funk S, Fusco P, Gargano F, Gehrels N, Germani S, Gibby M, Giglietto N, Giles M, Giordano F, Giroletti M, Godfrey G, Granot J, Grenier IA, Grove JE, Gruber D, Guiriec S, Hadasch D, Hanabata Y, Harding AK, Hayashida M, Hays E, Horan D, Hughes RE, Inoue Y, Jogler T, Johannesson G, Johnson WN, Kawano T, Knodlseder J, Kocevski D, Kuss M, Lande J, Larsson S, Latronico L, Longo F, Loparco F, Lovellette MN, Lubrano P, Mayer M, Mazziotta MN, McEnery JE, Michelson PF, Mizuno T, Moiseev AA, Monzani ME, Moretti E, Morselli A, Moskalenko IV, Murgia S, Nemmen R, Nuss E, Ohno M, Ohsugi T, Okumura A, Omodei N, Orienti M, Paneque D, Pelassa V, Perkins JS, Pesce-Rollins M, Petrosian V, Piron F, Pivato G, Porter TA, Racusin JL, Raino S, Rando R, Razzano M, Razzaque S, Reimer A, Reimer O, Ritz S, Roth M, Ryde F, Sartori A, Parkinson PMS, Scargle JD, Schulz A, Sgro C, Siskind EJ, Sonbas E, Spandre G, Spinelli P, Tajima H, Takahashi H, Thayer JG, Thayer JB, Thompson DJ, Tibaldo L, Tinivella M, Torres DF, Tosti G, Troja E, Usher TL, Vandenbroucke J, Vasileiou V, Vianello G, Vitale V, Winer BL, Wood KS, Yamazaki R, Younes G, Yu HF, Zhu SJ, Bhat PN, Briggs MS, Byrne D, Foley S, Goldstein A, Jenke P, Kippen RM, Kouveliotou C, McBreen S, Meegan C, Paciesas WS, Preece R, Rau A, Tierney D, van der Horst AJ, von Kienlin A, Wilson-Hodge C, Xiong S, Cusumano G, La Parola V, Cummings JR, M., Ackermann, M., Ajello, K., Asano, W. B., Atwood, M., Axelsson, L., Baldini, J., Ballet, BARBIELLINI AMIDEI, Guido, M. G., Baring, D., Bastieri, K., Bechtol, R., Bellazzini, Bissaldi, Elisabetta, E., Bonamente, J., Bregeon, M., Brigida, P., Bruel, R., Buehler, J. M., Burge, S., Buson, G. A., Caliandro, R. A., Cameron, P. A., Caraveo, C., Cecchi, V., Chaplin, E., Charle, A., Chekhtman, C. C., Cheung, J., Chiang, G., Chiaro, S., Ciprini, R., Clau, W., Cleveland, J., Cohen Tanugi, A., Collazzi, L. R., Cominsky, V., Connaughton, J., Conrad, S., Cutini, F., D'Ammando, A. d., Angeli, M., Deklotz, F. d., Palma, C. D., Dermer, R., Desiante, A., Diekmann, L. D., Venere, P. S., Drell, A., Drlica Wagner, C., Favuzzi, S. J., Fegan, E. C., Ferrara, J., Finke, G., Fitzpatrick, W. B., Focke, A., Franckowiak, Y., Fukazawa, S., Funk, P., Fusco, F., Gargano, N., Gehrel, S., Germani, M., Gibby, N., Giglietto, M., Gile, F., Giordano, M., Giroletti, G., Godfrey, J., Granot, I. A., Grenier, J. E., Grove, D., Gruber, S., Guiriec, D., Hadasch, Y., Hanabata, A. K., Harding, M., Hayashida, E., Hay, D., Horan, R. E., Hughe, Y., Inoue, T., Jogler, G., Johannesson, W. N., Johnson, T., Kawano, J., Knoedlseder, D., Kocevski, M., Ku, J., Lande, S., Larsson, L., Latronico, Longo, Francesco, F., Loparco, M. N., Lovellette, P., Lubrano, M., Mayer, M. N., Mazziotta, J. E., Mcenery, P. F., Michelson, T., Mizuno, A. A., Moiseev, M. E., Monzani, E., Moretti, A., Morselli, I. V., Moskalenko, S., Murgia, R., Nemmen, E., Nu, M., Ohno, T., Ohsugi, A., Okumura, N., Omodei, M., Orienti, D., Paneque, V., Pelassa, J. S., Perkin, M., Pesce Rollin, V., Petrosian, F., Piron, G., Pivato, T. A., Porter, J. L., Racusin, S., Raino, R., Rando, M., Razzano, S., Razzaque, A., Reimer, O., Reimer, S., Ritz, M., Roth, F., Ryde, A., Sartori, P. M., Saz, J. D., Scargle, A., Schulz, C., Sgro, E. J., Siskind, E., Sonba, G., Spandre, P., Spinelli, H., Tajima, H., Takahashi, J. G., Thayer, J. B., Thayer, D. J., Thompson, L., Tibaldo, M., Tinivella, D. F., Torre, G., Tosti, E., Troja, T. L., Usher, J., Vandenbroucke, V., Vasileiou, G., Vianello, V., Vitale, B. L., Winer, K. S., Wood, R., Yamazaki, G., Youne, H. . ., F., S. J., Zhu, P. N., Bhat, M. S., Brigg, D., Byrne, S., Foley, A., Goldstein, P., Jenke, R. M., Kippen, C., Kouveliotou, S., Mcbreen, C., Meegan, W. S., Paciesa, R., Preece, A., Rau, D., Tierney, A. J., Van, A. v., Kienlin, C., Wilson Hodge, S., Xiong, G., Cusumano, V. L., Parola, J. R., Cummings, and High Energy Astrophys. & Astropart. Phys (API, FNWI)
Subjects: Astrophysics::High Energy Astrophysical Phenomena, SPECTRAL COMPONENT, Synchrotron radiation, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, LARGE-AREA TELESCOPE, HIGH-ENERGY EMISSION, AFTERGLOWS, PROMPT, law.invention, Telescope, Spitzer Space Telescope, law, Astrophysics::Galaxy Astrophysics, Physics, Multidisciplinary, Gamma ray, GRB 130427A, Astronomy, Afterglow, GRB, Fermi-LAT, ddc:500, Astrophysics - High Energy Astrophysical Phenomena, Gamma-ray burst, Fermi Gamma-ray Space Telescope
Abstract: The observations of the exceptionally bright gamma-ray burst (GRB) 130427A by the Large Area Telescope aboard the Fermi Gamma-ray Space Telescope provide constraints on the nature of such unique astrophysical sources. GRB 130427A had the largest fluence, highest-energy photon (95 GeV), longest $\gamma$-ray duration (20 hours), and one of the largest isotropic energy releases ever observed from a GRB. Temporal and spectral analyses of GRB 130427A challenge the widely accepted model that the non-thermal high-energy emission in the afterglow phase of GRBs is synchrotron emission radiated by electrons accelerated at an external shock., Comment: 30 pages, 6 figures. Accepted for publication in Science. Corresponding authors: S. Zhu (sjzhu@umd.edu); J. Chiang (jchiang@slac.stanford.edu); C. Dermer (charles.dermer@nrl.navy.mil); N. Omodei (nicola.omodei@stanford.edu); G. Vianello (giacomov@slac.stanford.edu); S. Xiong (Shaolin.Xiong@uah.edu)
Published: 2014

33. A search for supernova remnants in the nearby spiral galaxy M74 (NGC 628)

Author: Eda Sonbas, Aysun Akyüz, Solen Balman, M. E. Ozel, Çukurova Üniversitesi, and [Sonbas, E.] Univ Adiyaman, Dept Phys, TR-02040 Adiyaman, Turkey -- [Akyuz, A.] Cukurova Univ, Dept Phys, TR-01330 Adana, Turkey -- [Balman, S.] Middle E Tech Univ, Dept Phys, TR-06531 Ankara, Turkey -- [Ozel, M. E.] Cag Univ, Fac Arts & Sci, TR-33800 Tarsus, Turkey
Subjects: Physics, Spiral galaxy, Optical wavelength, FOS: Physical sciences, Flux, galaxies: groups: individual: M 74 (NGC 628), Astronomy and Astrophysics, Astrophysics, Astrophysics - Astrophysics of Galaxies, Coincidence, Luminosity, Supernova, Space and Planetary Science, Observatory, Astrophysics of Galaxies (astro-ph.GA), Ionization, galaxies: ISM, ISM: supernova remnants
Abstract: WOS: 000280929400101, An optical search was carried out for supernova remnants (SNRs) in the Sc type nearby spiral galaxy M 74, using ground-based observations at the TUBITAK National Observatory (TUG, Antalya/Turkey) and the Special Astrophysics Observatory (SAO, Russia). Observations were supplemented by the spectral analysis of archived X-ray data from XMM-Newton and Chandra. The survey of M74 covered similar to 9 arcmin(2) with [S II], H alpha, and their continuum filters. Interference filter images of M 74 were obtained the with the 1.5 m Russian Turkish Telescope (RTT150) at TUG and spectral data taken with the 6 m Bolsoi Azimuthal Telescope (BTA) at SAO. The emission nebulae with continuum-subtracted line ratio values of [S II]lambda lambda 6716,6731 /H alpha >= 0.4 are identified as SNRs. Followup spectroscopy confirmed optical SNR identifications. We have identified nine new SNR candidates in M 74 with [S II]/H alpha >= 0.4 as the basic criterion. The [S II]/H alpha ratio ranges from 0.40 to 0.91 and H alpha intensities from 2.8 x 10(-15) erg cm(-2) s(-1) to 1.7 x 10(-14) erg cm(-2) s(-1). We also present spectral follow-up observations of these SNR candidates, however, we are able to spectrally confirm only three of them (SNR2, SNR3, and SNR5). The lack of confirmation for the rest might come from contamination by the nearby H II emission regions, as well as from the inaccurate positioning of the long slit on these objects. In addition, we searched the XMM-Newton and Chandra Observatory archival data for the X-ray counterparts to the optically identified candidates. We find positional coincidence with only three SNR candidates, SNR1, SNR2, and SNR8. The spectrum of SNR2 yields a shock temperature of 10.8 keV with an ionization timescale of 1.6 x 10(10) s cm(-3), indicating a relatively young remnant in an early Sedov phase, which is not supported by our optical wavelength analysis. Given the high luminosity of 10(39) erg s(-1) and the characteristics of the X-ray spectrum, we favor an ultra luminous X-ray source interpretation for this source associated with an SNR. We calculated an X-ray flux upper limit of 9.0 x 10(-15) erg cm(-2) s(-1) for the rest of the SNRs, including spectroscopically identified SNR3 and SNR5., TUBITAK National Observatory (TUG); Special Astrophysical Observatory (SAO), We thank the TUBITAK National Observatory (TUG) and the Special Astrophysical Observatory (SAO) for their support for observing times and equipment.
Published: 2010

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33 results on '"Sonbas, E."'

1. Observation Campaign of (99942) Apophis in the 2021 Apparition

2. GRB 140102A: insight into prompt spectral evolution and early optical afterglow emission

3. Spitzer Observations of the Predicted Eddington Flare from Blazar OJ 287

4. A Minimal Time-Scale For The Spectral States Of Gx 339-4

5. Stochastic Modeling of Multiwavelength Variability of the Classical BL Lac Object OJ 287 on Timescales Ranging from Decades to Hours

6. Authenticating the Presence of a Relativistic Massive Black Hole Binary in OJ 287 Using Its General Relativity Centenary Flare: Improved Orbital Parameters

7. Polarization and spectral energy distribution in OJ 287 during the 2016/17 outbursts

8. The size, shape, density and ring of the dwarf planet Haumea from a stellar occultation

9. Constraining the High-energy Emission from Gamma-Ray Bursts with Fermi

10. Primary black hole spin in oj 287 AS determined by the general relativity centenary flare

11. A search for QPOs in the blazar OJ287: Preliminary results from the 2015/2016 observing campaign

12. A strong optical activity of the OJ287 blazar

13. DETECTION OF HIGH-ENERGY GAMMA-RAY EMISSION DURING THE X-RAY FLARING ACTIVITY IN GRB 100728A

14. The Afterglow Of Grb 130427A From 1 To 10(16) Ghz

15. GRB 130606A within a sub-DLA at redshift 5.91

16. THE FIRST FERMI -LAT GAMMA-RAY BURST CATALOG

17. The Afterglow of GRB 130427A from 1 to 10^16 GHz

18. X - Ray Flares and Their Connection With Prompt Emission in GRBs

19. The Minimum Variability Time Scale and its Relation to Pulse Profiles of Fermi GRBs

20. An unusual stellar death on Christmas Day

21. A Proposal to Localize Fermi GBM GRBs Through Coordinated Scanning of the GBM Error Circle via Optical Telescopes

22. The Lag-Luminosity Relation in the GRB Source-Frame: An Investigation with Swift BAT Bursts

23. Study of Envelope Velocity Evolution of Type Ib-c Core-Collapse Supernovae from Observations of XRF 080109 / SN 2008D and GRB 060218 / SN 2006aj with BTA

24. An optical search for supernova remnants in the nearby spiral galaxy NGC 2903 (research note)

25. Optical and infrared flares from a transient Galactic soft gamma-ray repeater

26. The stellar-wind envelope around the supernova XRF/GRB060218/SN2006aj massive progenitor star

27. GRB 101225A: a stellar murder on Christmas Day

28. Optical search for supernova remnants in two-spiral galaxies

29. GRB 110407A: Swift detection of a burst

30. The 2017 May 20 stellar occultation by the elongated centaur (95626) 2002 GZ32

31. MULTIWAVELENGTH OBSERVATIONS OF GRB 110731A: GeV EMISSION FROM ONSET TO AFTERGLOW

32. Fermi-LAT Observations of the Gamma-Ray Burst GRB 130427A

33. A search for supernova remnants in the nearby spiral galaxy M74 (NGC 628)

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