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934 results on '"Oates, S"'

151. OPTICAL SPECTROSCOPY OF CANDIDATES IN THE LIGO/VIRGO BINARY MERGER ERROR BOXES

Author

Valeev, A. F., primary, Castro-Tirado, A. J., additional, Hu, Y. -D., additional, Sokolov, V. V., additional, Agudo, I., additional, Caballero-García, M. D., additional, Cepa, J., additional, Font, J. A., additional, Jeong, S., additional, Martin-Carrillo, A., additional, Pandey, S. B., additional, Pian, E., additional, Oates, S. R., additional, Sánchez-Ramírez, R., additional, Sintes, A. M., additional, Zhang, B.-B., additional, and Fernandez-Garcia, E., additional

Published
2021
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152. Swift/UVOT follow-up of gravitational wave alerts in the O3 era

Author

Oates, S R, primary, Marshall, F E, additional, Breeveld, A A, additional, Kuin, N P M, additional, Brown, P J, additional, De Pasquale, M, additional, Evans, P A, additional, Fenney, A J, additional, Gronwall, C, additional, Kennea, J A, additional, Klingler, N J, additional, Page, M J, additional, Siegel, M H, additional, Tohuvavohu, A, additional, Ambrosi, E, additional, Barthelmy, S D, additional, Beardmore, A P, additional, Bernardini, M G, additional, Campana, S, additional, Caputo, R, additional, Cenko, S B, additional, Cusumano, G, additional, D’Aì, A, additional, D’Avanzo, P, additional, D’Elia, V, additional, Giommi, P, additional, Hartmann, D H, additional, Krimm, H A, additional, Laha, S, additional, Malesani, D B, additional, Melandri, A, additional, Nousek, J A, additional, O’Brien, P T, additional, Osborne, J P, additional, Pagani, C, additional, Page, K L, additional, Palmer, D M, additional, Perri, M, additional, Racusin, J L, additional, Sakamoto, T, additional, Sbarufatti, B, additional, Schlieder, J E, additional, Tagliaferri, G, additional, and Troja, E, additional

Published
2021
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153. Publisher Correction: Transition from fireball to Poynting-flux-dominated outflow in the three-episode GRB 160625B

Author

Zhang, B.-B., Zhang, B., Castro-Tirado, A. J., Dai, Z. G., Tam, P.-H. T., Wang, X.-Y., Hu, Y.-D., Karpov, S., Pozanenko, A., Zhang, F.-W., Mazaeva, E., Minaev, P., Volnova, A., Oates, S., Gao, H., Wu, X.-F., Shao, L., Tang, Q.-W., Beskin, G., Biryukov, A., Bondar, S., Ivanov, E., Katkova, E., Orekhova, N., Perkov, A., Sasyuk, V., Mankiewicz, L., Żarnecki, A. F., Cwiek, A., Opiela, R., Zadrożny, A., Aptekar, R., Frederiks, D., Svinkin, D., Kusakin, A., Inasaridze, R., Burhonov, O., Rumyantsev, V., Klunko, E., Moskvitin, A., Fatkhullin, T., Sokolov, V. V., Valeev, A. F., Jeong, S., Park, I. H., Caballero-García, M. D., Cunniffe, R., Tello, J. C., Ferrero, P., Pandey, S. B., Jelínek, M., Peng, F. K., Sánchez-Ramírez, R., and Castellón, A.

Published
2018
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154. The Central Engine of GRB 130831A and the Energy Breakdown of a Relativistic Explosion

Author

Pasquale, M. De, Oates, S. R, Racusin, J. L, Kann, D. A, Zhang, B, Pozanenko, A, Volnova, A.A, Trotter, A, Frank, N, and Cucchiara, A

Subjects
Astrophysics
Abstract

Gamma-ray bursts (GRBs) are the most luminous explosions in the Universe, yet the nature and physical properties of their energy sources are far from understood. Very important clues, however, can be inferred by studying the afterglows of these events. We present optical and X-ray observations of GRB 130831A obtained by Swift, Chandra, Skynet, Reionization And Transients Infra-Red camera, Maidanak, International Scientific Optical-Observation Network, Nordic Optical Telescope, Liverpool Telescope and Gran Telescopio Canarias. This burst shows a steep drop in the X-ray light curve at asymptotically equal to 10(exp 5) s after the trigger, with a power-law decay index of alpha that is approximately 6. Such a rare behaviour cannot be explained by the standard forward shock (FS) model and indicates that the emission, up to the fast decay at 10(exp 5) s, must be of internal origin, produced by a dissipation process within an ultrarelativistic outflow. We propose that the source of such an outflow, which must produce the X-ray flux for an asymptotically equal to 1 d in the cosmological rest frame, is a newly born magnetar or black hole. After the drop, the faint X-ray afterglow continues with a much shallower decay. The optical emission, on the other hand, shows no break across the X-ray steep decrease, and the late-time decays of both the X-ray and optical are consistent. Using both the X-ray and optical data, we show that the emission after an asymptotically equal to 10(exp 5) scan be explained well by the FS model. We model our data to derive the kinetic energy of the ejecta and thus measure the efficiency of the central engine of a GRB with emission of internal origin visible for a long time. Furthermore, we break down the energy budget of this GRB into the prompt emission, the late internal dissipation, the kinetic energy of the relativistic ejecta,and compare it with the energy of the associated supernova, SN 2013 fu.

Published
2014
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155. Swift Multiwavelength Follow-Up Of Lvc S200224Ca And The Implications For Binary Black Hole Mergers

Author

Klingler, N. J., Lien, A., Oates, S. R., Kennea, J. A., Evans, P. A., Tohuvavohu, A., Zhang, B., Page, K. L., Cenko, S. B., Barthelmy, S. D., Beardmore, A. P., Bernardini, M. G., Breeveld, A. A., Brown, P. J., Burrows, D. N., Campana, S., Cusumano, G., D'Ai, A., D'Avanzo, P., and D'Elia, V.

Abstract

On 2020 February 24, during their third observing run ("O3"), the Laser Interferometer Gravitational-wave Observatory and Virgo Collaboration detected S200224ca: a candidate gravitational wave (GW) event produced by a binary black hole (BBH) merger. This event was one of the best-localized compact binary coalescences detected in O3 (with 50%/ 90% error regions of 13/72 deg(2)), and so the Neil Gehrels Swift Observatory performed rapid near-UV/X-ray followup observations. Swift-XRT and UVOT covered approximately 79.2% and 62.4% (respectively) of the GWerror region, making S200224ca the BBH event most thoroughly followed-up in near-UV (u-band) and X-ray to date. No likely EM counterparts to the GW event were found by the Swift BAT, XRT, or UVOT, nor by other observatories. Here, we report on the results of our searches for an EM counterpart, both in the BAT data near the time of the merger, and in follow-up UVOT/XRT observations. We also discuss the upper limits we can place on EM radiation from S200224ca, as well as the implications these limits have on the physics of BBH mergers. Namely, we place a shallow upper limit on the dimensionless BH charge, (q) over cap < 1.4 x 10(-4), and an upper limit on the isotropic-equivalent energy of a blast wave E< 4.1x10(51) erg (assuming typical GRB parameters).

Published
2021

156. Swift Multiwavelength Follow-up of LVC S200224ca and the Implications for Binary Black Hole Mergers

Author

Klingler, N. J., primary, Lien, A., additional, Oates, S. R., additional, Kennea, J. A., additional, Evans, P. A., additional, Tohuvavohu, A., additional, Zhang, B., additional, Page, K. L., additional, Cenko, S. B., additional, Barthelmy, S. D., additional, Beardmore, A. P., additional, Bernardini, M. G., additional, Breeveld, A. A., additional, Brown, P. J., additional, Burrows, D. N., additional, Campana, S., additional, Cusumano, G., additional, D’Aì, A., additional, D’Avanzo, P., additional, D’Elia, V., additional, Pasquale, M. de, additional, Emery, S. W. K., additional, Garcia, J., additional, Giommi, P., additional, Gronwall, C., additional, Hartmann, D. H., additional, Krimm, H. A., additional, Kuin, N. P. M., additional, Malesani, D. B., additional, Marshall, F. E., additional, Melandri, A., additional, Nousek, J. A., additional, O’Brien, P. T., additional, Osborne, J. P., additional, Palmer, D. M., additional, Page, M. J., additional, Perri, M., additional, Racusin, J. L., additional, Sakamoto, T., additional, Sbarufatti, B., additional, Schlieder, J. E., additional, Siegel, M. H., additional, Tagliaferri, G., additional, and Troja, E., additional

Published
2021
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157. 10.4 m GTC observations of the nearby VHE-detected GRB 190829A/SN 2019oyw

Author

Hu, Y.-D., primary, Castro-Tirado, A. J., additional, Kumar, A., additional, Gupta, R., additional, Valeev, A. F., additional, Pandey, S. B., additional, Kann, D. A., additional, Castellón, A., additional, Agudo, I., additional, Aryan, A., additional, Caballero-García, M. D., additional, Guziy, S., additional, Martin-Carrillo, A., additional, Oates, S. R., additional, Pian, E., additional, Sánchez-Ramírez, R., additional, Sokolov, V. V., additional, and Zhang, B.-B., additional

Published
2021
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158. Transient Puzzles

Author

Kouveliotou, Chryssa, Granot, J, Racusin, J. L, Bellm, E, Vianello, G, Oates, S, Fryer, C. L, Boggs, S. E, Christensen, F. E, Craig, W. W, Dermer, C. D, Gehrels, N, Hailey, C. J, Harrison, F. A, Melandri, A, McEnery, J. E, Mundell, C. G, Stern, D. K, Tagliaferri, G, and Zhang, W. W

Subjects
Astronomy, Astrophysics
Published
2014

159. Prompt Emission of GRB 121217A from Gamma-Rays to the Near-Infrared

Author

Elliott, J, Yu, H.-F, Schmidl, S, Greiner, J, Gruber, D, Oates, S, Kobayashi, S, Zhang, B, Cummings, J. R, Filgas, R, and Gehrels, N

Subjects
Astrophysics
Abstract

The mechanism that causes the prompt-emission episode of gamma-ray bursts (GRBs) is still widely debated despite there being thousands of prompt detections. The favoured internal shock model relates this emission to synchrotron radiation. However, it does not always explain the spectral indices of the shape of the spectrum, which is often fit with empirical functions, such as the Band function. Multi-wavelength observations are therefore required to help investigate the possible underlying mechanisms that causes the prompt emission. We present GRB 121217A, for which we were able to observe its near-infrared (NIR) emission during a secondary prompt-emission episode with the Gamma-Ray burst Optical Near-infrared Detector (GROND) in combination with the Swift and Fermi satellites, which cover an energy range of 5 orders of magnitude (10(exp −3) keV to 100 keV). We determine a photometric redshift of z = 3.1 +/- 0.1 with a line-of-sight with little or no extinction (AV approx. 0 mag) utilising the optical/NIR SED. From the afterglow, we determine a bulk Lorentz factor of Gamma(sub 0) approx. 250 and an emission radius of R < 1018 cm. The prompt-emission broadband spectral energy distribution is well fit with a broken power law with beta1 = −0.3 +/- 0.1 and beta2 = 0.6 +/- 0.1 that has a break at E = 6.6 +/- 0.9 keV, which can be interpreted as the maximum injection frequency. Self-absorption by the electron population below energies of Ea < 6 keV suggest a magnetic field strength of B approx. 10(exp 5) G. However, all the best fit models underpredict the flux observed in the NIR wavelengths, which also only rebrightens by a factor of approx. 2 during the second prompt emission episode, in stark contrast to the X-ray emission, which rebrightens by a factor of approx. 100. This suggests an afterglow component is dominating the emission. We present GRB 121217A, one of the few GRBs that has multi-wavelength observations of the prompt-emission period and shows that it can be understood with a synchrotron radiation model. However, due to the complexity of the GRB's emission, other mechanisms that result in Band-like spectra cannot be ruled out.

Published
2014
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160. Observational constraints on the optical and near-infrared emission from the neutron star-black hole binary merger candidate S190814bv

Author

Ackley, K., Amati, L., Barbieri, C., Bauer, F. E., Benetti, S., Bernardini, M. G., Bhirombhakdi, K., Botticella, M. T., Branchesi, M., Brocato, E., Bruun, S. H., Bulla, Mattia, Campana, S., Cappellaro, E., Castro-Tirado, A. J., Chambers, K. C., Chaty, S., Chen, Ting-Wan, Ciolfi, R., Coleiro, A., Copperwheat, C. M., Covino, S., Cutter, R., D'Ammando, F., D'Avanzo, P., De Cesare, G., D'Elia, V., Della Valle, M., Denneau, L., De Pasquale, M., Dhillon, V. S., Dyer, M. J., Elias-Rosa, N., Evans, P. A., Eyles-Ferris, R. A. J., Fiore, A., Fraser, M., Fruchter, A. S., Fynbo, J. P. U., Galbany, L., Gall, C., Galloway, D. K., Getman, F., Ghirlanda, G., Gillanders, J. H., Gomboc, A., Gompertz, B. P., Gonzalez-Fernandez, C., Gonzalez-Gaitan, S., Grado, A., Greco, G., Gromadzki, M., Groot, P. J., Gutierrez, C. P., Heikkila, T., Heintz, K. E., Hjorth, J., Hu, Y.-D., Huber, M. E., Inserra, C., Izzo, L., Japelj, J., Jerkstrand, Anders, Jin, Z. P., Jonker, P. G., Kankare, E., Kann, D. A., Kennedy, M., Kim, S., Klose, S., Kool, Erik C., Kotak, R., Kuncarayakti, H., Lamb, G. P., Leloudas, G., Levan, A. J., Longo, F., Lowe, T. B., Lyman, J. D., Magnier, E., Maguire, K., Maiorano, E., Mandel, I., Mapelli, M., Mattila, S., McBrien, O. R., Melandri, A., Michalowski, M. J., Milvang-Jensen, B., Moran, S., Nicastro, L., Nicholl, M., Nicuesa Guelbenzu, A., Nuttal, L., Oates, S. R., O'Brien, P. T., Onori, F., Palazzi, E., Patricelli, B., Perego, A., Torres, M. A. P., Perley, D. A., Pian, E., Pignata, G., Piranomonte, S., Poshyachinda, S., Possenti, A., Pumo, M. L., Quirola-Vasquez, J., Ragosta, F., Ramsay, G., Rau, A., Rest, A., Reynolds, T. M., Rosetti, S. S., Rossi, A., Rosswog, Stephan, Sabha, N. B., Sagués Carracedo, Ana, Salafia, O. S., Salmon, L., Salvaterra, R., Savaglio, S., Sbordone, L., Schady, P., Schipani, P., Schultz, A. S. B., Schweyer, Tassilo, Smartt, S. J., Smith, K. W., Smith, M., Sollerman, Jesper, Srivastav, S., Stanway, E. R., Starling, R. L. C., Steeghs, D., Stratta, G., Stubbs, C. W., Tanvir, N. R., Testa, V., Thrane, E., Tonry, J. L., Turatto, M., Ulaczyk, K., van der Horst, A. J., Vergani, S. D., Walton, N. A., Watson, D., Wiersema, K., Wiik, K., Wyrzykowski, L., Yang, Sheng, Yi, S.-X., Young, D. R., Ackley, K., Amati, L., Barbieri, C., Bauer, F. E., Benetti, S., Bernardini, M. G., Bhirombhakdi, K., Botticella, M. T., Branchesi, M., Brocato, E., Bruun, S. H., Bulla, Mattia, Campana, S., Cappellaro, E., Castro-Tirado, A. J., Chambers, K. C., Chaty, S., Chen, Ting-Wan, Ciolfi, R., Coleiro, A., Copperwheat, C. M., Covino, S., Cutter, R., D'Ammando, F., D'Avanzo, P., De Cesare, G., D'Elia, V., Della Valle, M., Denneau, L., De Pasquale, M., Dhillon, V. S., Dyer, M. J., Elias-Rosa, N., Evans, P. A., Eyles-Ferris, R. A. J., Fiore, A., Fraser, M., Fruchter, A. S., Fynbo, J. P. U., Galbany, L., Gall, C., Galloway, D. K., Getman, F., Ghirlanda, G., Gillanders, J. H., Gomboc, A., Gompertz, B. P., Gonzalez-Fernandez, C., Gonzalez-Gaitan, S., Grado, A., Greco, G., Gromadzki, M., Groot, P. J., Gutierrez, C. P., Heikkila, T., Heintz, K. E., Hjorth, J., Hu, Y.-D., Huber, M. E., Inserra, C., Izzo, L., Japelj, J., Jerkstrand, Anders, Jin, Z. P., Jonker, P. G., Kankare, E., Kann, D. A., Kennedy, M., Kim, S., Klose, S., Kool, Erik C., Kotak, R., Kuncarayakti, H., Lamb, G. P., Leloudas, G., Levan, A. J., Longo, F., Lowe, T. B., Lyman, J. D., Magnier, E., Maguire, K., Maiorano, E., Mandel, I., Mapelli, M., Mattila, S., McBrien, O. R., Melandri, A., Michalowski, M. J., Milvang-Jensen, B., Moran, S., Nicastro, L., Nicholl, M., Nicuesa Guelbenzu, A., Nuttal, L., Oates, S. R., O'Brien, P. T., Onori, F., Palazzi, E., Patricelli, B., Perego, A., Torres, M. A. P., Perley, D. A., Pian, E., Pignata, G., Piranomonte, S., Poshyachinda, S., Possenti, A., Pumo, M. L., Quirola-Vasquez, J., Ragosta, F., Ramsay, G., Rau, A., Rest, A., Reynolds, T. M., Rosetti, S. S., Rossi, A., Rosswog, Stephan, Sabha, N. B., Sagués Carracedo, Ana, Salafia, O. S., Salmon, L., Salvaterra, R., Savaglio, S., Sbordone, L., Schady, P., Schipani, P., Schultz, A. S. B., Schweyer, Tassilo, Smartt, S. J., Smith, K. W., Smith, M., Sollerman, Jesper, Srivastav, S., Stanway, E. R., Starling, R. L. C., Steeghs, D., Stratta, G., Stubbs, C. W., Tanvir, N. R., Testa, V., Thrane, E., Tonry, J. L., Turatto, M., Ulaczyk, K., van der Horst, A. J., Vergani, S. D., Walton, N. A., Watson, D., Wiersema, K., Wiik, K., Wyrzykowski, L., Yang, Sheng, Yi, S.-X., and Young, D. R.

Abstract

Context. Gravitational wave (GW) astronomy has rapidly reached maturity, becoming a fundamental observing window for modern astrophysics. The coalescences of a few tens of black hole (BH) binaries have been detected, while the number of events possibly including a neutron star (NS) is still limited to a few. On 2019 August 14, the LIGO and Virgo interferometers detected a high-significance event labelled S190814bv. A preliminary analysis of the GW data suggests that the event was likely due to the merger of a compact binary system formed by a BH and a NS. Aims. In this paper, we present our extensive search campaign aimed at uncovering the potential optical and near infrared electromagnetic counterpart of S190814bv. We found no convincing electromagnetic counterpart in our data. We therefore use our non-detection to place limits on the properties of the putative outflows that could have been produced by the binary during and after the merger. Methods. Thanks to the three-detector observation of S190814bv, and given the characteristics of the signal, the LIGO and Virgo Collaborations delivered a relatively narrow localisation in low latency - a 50% (90%) credible area of 5 deg(2) (23 deg(2)) - despite the relatively large distance of 26752 Mpc. ElectromagNetic counterparts of GRAvitational wave sources at the VEry Large Telescope collaboration members carried out an intensive multi-epoch, multi-instrument observational campaign to identify the possible optical and near infrared counterpart of the event. In addition, the ATLAS, GOTO, GRAWITA-VST, Pan-STARRS, and VINROUGE projects also carried out a search on this event. In this paper, we describe the combined observational campaign of these groups. Results. Our observations allow us to place limits on the presence of any counterpart and discuss the implications for the kilonova (KN), which was possibly generated by this NS-BH merger, and for the strategy of future searches. The typical depth of our wide-field observat

Published
2020
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162. An outflow powers the optical rise of the nearby, fast-evolving tidal disruption event AT2019qiz

Author

Nicholl, M, Wevers, T, Oates, S R, Alexander, K D, Leloudas, G, Onori, F, Jerkstrand, A, Gomez, S, Campana, S, Arcavi, I, Charalampopoulos, P, Gromadzki, M, Ihanec, N, Jonker, P G, Lawrence, A, Mandel, I, Schulze, S, Short, P, Burke, J, McCully, C, Hiramatsu, D, Howell, D A, Pellegrino, C, Abbot, H, Anderson, J P, Berger, E, Blanchard, P K, Cannizzaro, G, Chen, T-W, Dennefeld, M, Galbany, L, González-Gaitán, S, Hosseinzadeh, G, Inserra, C, Irani, I, Kuin, P, Müller-Bravo, T, Pineda, J, Ross, N P, Roy, R, Smartt, S J, Smith, K W, Tucker, B, Wyrzykowski, Ł, Young, D R, Nicholl, M, Wevers, T, Oates, S R, Alexander, K D, Leloudas, G, Onori, F, Jerkstrand, A, Gomez, S, Campana, S, Arcavi, I, Charalampopoulos, P, Gromadzki, M, Ihanec, N, Jonker, P G, Lawrence, A, Mandel, I, Schulze, S, Short, P, Burke, J, McCully, C, Hiramatsu, D, Howell, D A, Pellegrino, C, Abbot, H, Anderson, J P, Berger, E, Blanchard, P K, Cannizzaro, G, Chen, T-W, Dennefeld, M, Galbany, L, González-Gaitán, S, Hosseinzadeh, G, Inserra, C, Irani, I, Kuin, P, Müller-Bravo, T, Pineda, J, Ross, N P, Roy, R, Smartt, S J, Smith, K W, Tucker, B, Wyrzykowski, Ł, and Young, D R

Abstract

At 66 Mpc, AT2019qiz is the closest optical tidal disruption event (TDE) to date, with a luminosity intermediate between the bulk of the population and the faint-and-fast event iPTF16fnl. Its proximity allowed a very early detection and triggering of multiwavelength and spectroscopic follow-up well before maximum light. The velocity dispersion of the host galaxy and fits to the TDE light curve indicate a black hole mass ≈106 M⊙, disrupting a star of ≈1 M⊙. By analysing our comprehensive UV, optical, and X-ray data, we show that the early optical emission is dominated by an outflow, with a luminosity evolution L ∝ t2, consistent with a photosphere expanding at constant velocity (≳2000 km s−1), and a line-forming region producing initially blueshifted H and He ii profiles with v = 3000–10 000 km s−1. The fastest optical ejecta approach the velocity inferred from radio detections (modelled in a forthcoming companion paper from K. D. Alexander et al.), thus the same outflow may be responsible for both the fast optical rise and the radio emission – the first time this connection has been observed in a TDE. The light-curve rise begins 29 ± 2 d before maximum light, peaking when the photosphere reaches the radius where optical photons can escape. The photosphere then undergoes a sudden transition, first cooling at constant radius then contracting at constant temperature. At the same time, the blueshifts disappear from the spectrum and Bowen fluorescence lines (N iii) become prominent, implying a source of far-UV photons, while the X-ray light curve peaks at ≈1041 erg s−1. Assuming that these X-rays are from prompt accretion, the size and mass of the outflow are consistent with the reprocessing layer needed to explain the large optical to X-ray ratio in this and other optical TDEs, possibly favouring accretion-powered over collision-powered outflow models.

Published
2020

163. Liquefaction Hazard in the Groningen Region of the Netherlands due to Induced Seismicity

Author

Civil and Environmental Engineering, Green, Russell A., Bommer, J. J., Stafford, Peter J., Maurer, B. W., Kruiver, P. P., Edwards, B., Rodriguez-Marek, Adrian, de Lange, Ger, Oates, S. J., Storck, T., Omidi, P., Bourne, S. J., van Elk, J., Civil and Environmental Engineering, Green, Russell A., Bommer, J. J., Stafford, Peter J., Maurer, B. W., Kruiver, P. P., Edwards, B., Rodriguez-Marek, Adrian, de Lange, Ger, Oates, S. J., Storck, T., Omidi, P., Bourne, S. J., and van Elk, J.

Abstract

The operator of the Groningen gas field is leading an effort to quantify the seismic hazard and risk of the region due to induced earthquakes, including overseeing one of the most comprehensive liquefaction hazard studies performed globally to date. Due to the unique characteristics of the seismic hazard and the geologic deposits in Groningen, efforts first focused on developing relationships for a Groningen-specific liquefaction triggering model. The liquefaction hazard was then assessed using a Monte Carlo method, wherein a range of credible event scenarios were considered in computing liquefaction damage-potential hazard curves. This effort entailed the use of a regional stochastic seismic source model, ground motion prediction equation, site response model, and geologic model that were developed as part of the broader regional seismic hazard assessment. No to minor surficial liquefaction manifestations are predicted for most sites across the study area for a 2475-year return period. The only sites where moderate surficial liquefaction manifestations are predicted are in the town of Zandeweer, with only some of the sites in the town being predicted to experience this severity of liquefaction for this return period. This work is made available under the terms of the Creative Commons Attribution 4.0 International license, https://creativecommons.org/licenses/by/4.0/.

Published
2020

164. The Optical Luminosity-Time Correlation for More than 100 Gamma-Ray Burst Afterglows

Author

Ministerio de Ciencia, Innovación y Universidades (España), European Commission, Australian Research Council, Department of Energy (US), Dainotti, M. G., Livermore, S., Kann, D.A., Li, L., Oates, S., Yi, S., Zhang, B., Gendre, B., Cenko, B., Fraija, N., Ministerio de Ciencia, Innovación y Universidades (España), European Commission, Australian Research Council, Department of Energy (US), Dainotti, M. G., Livermore, S., Kann, D.A., Li, L., Oates, S., Yi, S., Zhang, B., Gendre, B., Cenko, B., and Fraija, N.

Abstract

Gamma-ray bursts (GRBs) are fascinating events due to their panchromatic nature. Their afterglow emission is observed from sub-TeV energies to radio wavelengths. We investigate GRBs that present an optical plateau, leveraging on the resemblance with the X-ray plateau shown in many GRB light curves (LCs). We comprehensively analyze all published GRBs with known redshifts and optical plateau observed mostly by the Neil Gehrels Swift Observatory (Swift). We fit 267 optical LCs and show the existence of the plateau in 102 cases, which is the largest compilation so far of optical plateaus. For 56 Swift GRBs with optical and X-ray plateaus, we compare the rest-frame end time at both wavelengths (T*opt, T*x), and conclude that the plateau is achromatic between T*opt and T*x. We also confirm the existence of the two-dimensional relations between T*opt and T*x and the optical luminosity at the end of the plateau emission, which resembles the same luminosity-time correlation in X-rays (Dainotti et al. 2013). The existence of this optical correlation has been demonstrated for the largest sample of optical plateaus in the literature to date. The squared scatter in this optical correlation is smallest for the subset of the Gold GRBs with a decrease in the scatter equivalent to 52.4% when compared to the scatter of the entire GRB sample. © 2020. The American Astronomical Society. All rights reserved.

Published
2020

168. Observational constraints on the optical and near-infrared emission from the neutron star–black hole binary merger candidate S190814bv

Author

Ackley, K., primary, Amati, L., additional, Barbieri, C., additional, Bauer, F. E., additional, Benetti, S., additional, Bernardini, M. G., additional, Bhirombhakdi, K., additional, Botticella, M. T., additional, Branchesi, M., additional, Brocato, E., additional, Bruun, S. H., additional, Bulla, M., additional, Campana, S., additional, Cappellaro, E., additional, Castro-Tirado, A. J., additional, Chambers, K. C., additional, Chaty, S., additional, Chen, T.-W., additional, Ciolfi, R., additional, Coleiro, A., additional, Copperwheat, C. M., additional, Covino, S., additional, Cutter, R., additional, D’Ammando, F., additional, D’Avanzo, P., additional, De Cesare, G., additional, D’Elia, V., additional, Della Valle, M., additional, Denneau, L., additional, De Pasquale, M., additional, Dhillon, V. S., additional, Dyer, M. J., additional, Elias-Rosa, N., additional, Evans, P. A., additional, Eyles-Ferris, R. A. J., additional, Fiore, A., additional, Fraser, M., additional, Fruchter, A. S., additional, Fynbo, J. P. U., additional, Galbany, L., additional, Gall, C., additional, Galloway, D. K., additional, Getman, F. I., additional, Ghirlanda, G., additional, Gillanders, J. H., additional, Gomboc, A., additional, Gompertz, B. P., additional, González-Fernández, C., additional, González-Gaitán, S., additional, Grado, A., additional, Greco, G., additional, Gromadzki, M., additional, Groot, P. J., additional, Gutiérrez, C. P., additional, Heikkilä, T., additional, Heintz, K. E., additional, Hjorth, J., additional, Hu, Y.-D., additional, Huber, M. E., additional, Inserra, C., additional, Izzo, L., additional, Japelj, J., additional, Jerkstrand, A., additional, Jin, Z. P., additional, Jonker, P. G., additional, Kankare, E., additional, Kann, D. A., additional, Kennedy, M., additional, Kim, S., additional, Klose, S., additional, Kool, E. C., additional, Kotak, R., additional, Kuncarayakti, H., additional, Lamb, G. P., additional, Leloudas, G., additional, Levan, A. J., additional, Longo, F., additional, Lowe, T. B., additional, Lyman, J. D., additional, Magnier, E., additional, Maguire, K., additional, Maiorano, E., additional, Mandel, I., additional, Mapelli, M., additional, Mattila, S., additional, McBrien, O. R., additional, Melandri, A., additional, Michałowski, M. J., additional, Milvang-Jensen, B., additional, Moran, S., additional, Nicastro, L., additional, Nicholl, M., additional, Nicuesa Guelbenzu, A., additional, Nuttal, L., additional, Oates, S. R., additional, O’Brien, P. T., additional, Onori, F., additional, Palazzi, E., additional, Patricelli, B., additional, Perego, A., additional, Torres, M. A. P., additional, Perley, D. A., additional, Pian, E., additional, Pignata, G., additional, Piranomonte, S., additional, Poshyachinda, S., additional, Possenti, A., additional, Pumo, M. L., additional, Quirola-Vásquez, J., additional, Ragosta, F., additional, Ramsay, G., additional, Rau, A., additional, Rest, A., additional, Reynolds, T. M., additional, Rosetti, S. S., additional, Rossi, A., additional, Rosswog, S., additional, Sabha, N. B., additional, Sagués Carracedo, A., additional, Salafia, O. S., additional, Salmon, L., additional, Salvaterra, R., additional, Savaglio, S., additional, Sbordone, L., additional, Schady, P., additional, Schipani, P., additional, Schultz, A. S. B., additional, Schweyer, T., additional, Smartt, S. J., additional, Smith, K. W., additional, Smith, M., additional, Sollerman, J., additional, Srivastav, S., additional, Stanway, E. R., additional, Starling, R. L. C., additional, Steeghs, D., additional, Stratta, G., additional, Stubbs, C. W., additional, Tanvir, N. R., additional, Testa, V., additional, Thrane, E., additional, Tonry, J. L., additional, Turatto, M., additional, Ulaczyk, K., additional, van der Horst, A. J., additional, Vergani, S. D., additional, Walton, N. A., additional, Watson, D., additional, Wiersema, K., additional, Wiik, K., additional, Wyrzykowski, Ł., additional, Yang, S., additional, Yi, S.-X., additional, and Young, D. R., additional

Published
2020
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169. The unusual γ-ray burst GRB 101225A from a helium star/neutron star merger at redshift 0.33

Author

Thöne, C. C., de Ugarte Postigo, A., 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., García, L. Hernández, Llorente, A., Bundy, K., Choi, C., Jeong, H., Korhonen, H., Kubànek, P., Lim, J., Moskvitin, A., Muñoz-Darias, T., Pak, S., and Parrish, I.

Published
2011
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171. An outflow powers the optical rise of the nearby, fast-evolving tidal disruption event AT2019qiz

Author

Nicholl, M, primary, Wevers, T, additional, Oates, S R, additional, Alexander, K D, additional, Leloudas, G, additional, Onori, F, additional, Jerkstrand, A, additional, Gomez, S, additional, Campana, S, additional, Arcavi, I, additional, Charalampopoulos, P, additional, Gromadzki, M, additional, Ihanec, N, additional, Jonker, P G, additional, Lawrence, A, additional, Mandel, I, additional, Schulze, S, additional, Short, P, additional, Burke, J, additional, McCully, C, additional, Hiramatsu, D, additional, Howell, D A, additional, Pellegrino, C, additional, Abbot, H, additional, Anderson, J P, additional, Berger, E, additional, Blanchard, P K, additional, Cannizzaro, G, additional, Chen, T-W, additional, Dennefeld, M, additional, Galbany, L, additional, González-Gaitán, S, additional, Hosseinzadeh, G, additional, Inserra, C, additional, Irani, I, additional, Kuin, P, additional, Müller-Bravo, T, additional, Pineda, J, additional, Ross, N P, additional, Roy, R, additional, Smartt, S J, additional, Smith, K W, additional, Tucker, B, additional, Wyrzykowski, Ł, additional, and Young, D R, additional

Published
2020
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172. Swift-XRT follow-up of gravitational wave triggers during the third aLIGO/Virgo observing run

Author

Page, K L, primary, Evans, P A, additional, Tohuvavohu, A, additional, Kennea, J A, additional, Klingler, N J, additional, Cenko, S B, additional, Oates, S R, additional, Ambrosi, E, additional, Barthelmy, S D, additional, Beardmore, A P, additional, Bernardini, M G, additional, Breeveld, A A, additional, Brown, P J, additional, Burrows, D N, additional, Campana, S, additional, Caputo, R, additional, Cusumano, G, additional, D’Aì, A, additional, D’Avanzo, P, additional, D’Elia, V, additional, De Pasquale, M, additional, Emery, S W K, additional, Giommi, P, additional, Gronwall, C, additional, Hartmann, D H, additional, Krimm, H A, additional, Kuin, N P M, additional, Malesani, D B, additional, Marshall, F E, additional, Melandri, A, additional, Nousek, J A, additional, O’Brien, P T, additional, Osborne, J P, additional, Pagani, C, additional, Page, M J, additional, Palmer, D M, additional, Perri, M, additional, Racusin, J L, additional, Sakamoto, T, additional, Sbarufatti, B, additional, Schlieder, J E, additional, Siegel, M H, additional, Tagliaferri, G, additional, and Troja, E, additional

Published
2020
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175. Multi-Wavelength Observations of the Type IIb Supernova 2009mg

Author

Oates, S. R, Bayless, A. J, Stritzinger, M. D, Prichard, T, Prieto, J. L, Immler, S, Brown, P. J, Breeveld, A. A, DePasquale, M, Kuin, N. P. M, Hamuy, M, Holland, S. T, Taddia, F, and Roming, P. W. A

Subjects
Astronomy
Abstract

We present Swift UVOT and XRT observations, and visual wavelength spectroscopy of the Type IIb supernova (SN) 2009mg, discovered in the Sb galaxy ESO 121-G26. The observational properties of SN 2009mg are compared to the prototype Type IIb SNe 1993J and 2008ax, with which we find many similarities. However,minor differences are discernible including SN 2009mg not exhibiting an initial fast decline or micro-band upturn as observed in the comparison objects, and its rise to maximum is somewhat slower leading to slightly broader light curves. The late-time temporal index of SN 2009mg, determined from 40 days post-explosion, is consistent with the decay rate of SN 1993J, but inconsistent with the decay of Co-56. This suggests leakage of gamma-rays out of the ejecta and a stellar mass on the small side of the mass distribution. Our XRT nondetection provides an upper limit on the mass-loss rate of the progenitor of M less than 1.5 x 10(exp -5) solar mass yr(exp -1). Modelling of the SN light curve indicates a kinetic energy of 0.15 sup +0.02 sub -0.13 x 10(exp 51) erg, an ejecta mass of 0.56 sup+0.10 sub -.26 solar mass and a Ni-56 mass of 0.10 plus or minus 0.01 solar mass.

Published
2012

176. Broadband Study of GRB 091127: A Sub-Energetic Burst at Higher Redshift?

Author

Troja, E, Sakamoto, T, Guidorzi, C, Norris, J. P, Panaitescu, A, Kobayashi, S, Omodei, N, Brown, J. C, Burrows, D. N, Evans, P. A, Gehrels, N, Marshall, F. E, Mawson, N, Melandri, Mundell, C. G, Oates, S. R, Pal'shin, V, Preece, R. D, Racusin, J. L, Steele, I. A, Tanvir, N. R, Vasileiou, V, and Wilson-Hodge, C

Subjects
Astrophysics
Abstract

GRB 091127 is a bright gamma-ray burst (GRB) detected by Swift at a redshift z=0.49 and associated with SN 2009nz. We present the broadband analysis of the GRB prompt and afterglow emission and study its high-energy properties in the context of the GRB/SN association. While the high luminosity of the prompt emission and standard afterglow behavior are typical of cosmological long GRBs, its low energy release (E(sub gamma),<3x10(exp 49) erg), soft spectrum and unusual spectral lag connect this GRB to the class of sub-energetic bursts. We discuss the suppression of high-energy emission in this burst, and investigate whether this behavior could be connected with the sub-energetic nature of the explosion. Subject headings: gamma-ray bursts: individual (GRB 091127)

Published
2012

177. Gamma-Ray Emission Concurrent with the Nova in the Symbiotic Binary V407 Cygni

Author

Abdo, A. A., Ackermann, M., Ajello, M., Atwood, W. B., Baldini, L., Ballet, J., Barbiellini, G., Bastieri, D., Bechtol, K., Bellazzini, R., Berenji, B., Blandford, R. D., Bloom, E. D., Bonamente, E., Borgland, A. W., Bouvier, A., Brandt, T. J., Bregeon, J., Brez, A., Brigida, M., Bruel, P., Buehler, R., Burnett, T. H., Buson, S., Caliandro, G. A., Cameron, R. A., Caraveo, P. A., Carrigan, S., Casandjian, J. M., Cecchi, C., Celik, O., Charles, E., Chaty, S., Chekhtman, A., Cheung, C. C., Chiang, J., Ciprini, S., Claus, R., Cohen-Tanugi, J., Conrad, J., Corbel, S., Corbet, R., DeCesar, M. E., den Hartog, P. R., Dermer, C. D., de Palma, F., Digel, S. W., Donato, D., do Couto e Silva, E., Drell, P. S., Dubois, R., Dubus, G., Dumora, D., Favuzzi, C., Fegan, S. J., Ferrara, E. C, Fortin, P., Frailis, M., Fuhrmann, L., Fukazawa, Y., Funk, S., Fusco, P., Gargano, F., Gaspamini, D., Gehrels, N., Germani, S., Giglietto, N., Giordano, F., Giroletti, M., Glanzman, T., Godfrey, G., Grenier, I. A., Grondin, M.-H., Grove, J. E., Guiriec, S., Hadasch, D., Harding, A. K., Hayashida, M., Hays, E., Healey, S. E., Hill, A. B., Horan, D., Hughes, R. E., Itoh, R., Jean, P., Jóhannesson, G., Johnson, A. S., Johnson, R. P., Johnson, T. J., Johnson, W. N., Kamae, T., Katagiri, H., Kataoka, J., Kerr, M., Knödlseder, J., Koerding, E., Kuss, M., Lande, J., Latronico, L., Lee, S.-H., Lemoine-Goumard, M., Garde, Llena M., Longo, F., Loparco, F., Lott, B., Lovellette, M. N., Lubrano, P., Makeev, A., Mazziotta, M. N., McConville, W., McEnery, J. E., Mehault, J., Michelson, P. F., Mizuno, T., Moiseev, A. A., Monte, C., Monzani, M. E., Morselli, A., Moskalenko, I. V., Murgia, S., Nakamori, T., Naumann-Godo, M., Nestoras, I., Nolan, P. L., Norris, J. P., Nuss, E., Ohno, M., Ohsugi, T., Okumura, A., Omodei, N., Orlando, E., Ormes, J. F., Ozaki, M., Paneque, D., Panetta, J. H., Parent, D., Pelassa, V., Pepe, M., Pesce-Rollins, M., Piron, F., Porter, T. A, Raino, S., Rando, R., Ray, P. S., Razzano, M., Razzaque, S., Rea, N., Reimer, A., Reimer, O., Reposeur, T., Ripken, J., Ritz, S., Romani, R. W., Roth, M., Sadrozinski, H. F.-W., Sander, A., Saz Parkinson, P. M., Scargle, J. D., Schinzel, F. K., Sgrò, C., Shaw, M. S., Siskind, E. J., Smith, D. A., Smith, P. D., Sokolovsky, K. V., Spandre, G., Spinelli, P., Stawarz, L., Strickman, M. S., Suson, D. J., Takahashi, H., Takahashi, T., Tanaka, T., Tanaka, Y., Thayer, J. B., Thayer, J. G., Thompson, D. J., Tibaldo, L., Torres, D. F., Tosti, G., Tramacere, A., Uchiyama, Y., Usher, T. L, Vandenbroucke, J., Vasileiou, V., Vilchez, N., Vitale, V., Waite, A. P., Wallace, E., Wang, P., Winer, B. L, Wolff, M. T., Wood, K. S., Yang, Z., Ylinen, T., Ziegler, M., Maehara, H., Nishiyama, K., Kabashima, F., Bach, U., Bower, G. C., Falcone, A., Forster, J. R., Henden, A., Kawabata, K. S., Koubsky, P., Mukai, K., Nelson, T., Oates, S. R., Sakimoto, K., Sasada, M., Shenavrin, V. I., Shore, S. N., Skinner, G. K., Sokoloski, J., Stroh, M., Tatarnikov, A. M., Uemura, M., Wahlgren, G. M., and Yamanaka, M.

Published
2010
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178. Multiwavelength observations of GRB 140629A

Author

Hu, Y.-D., primary, Oates, S. R., additional, Lipunov, V. M., additional, Zhang, B.-B., additional, Castro-Tirado, A. J., additional, Jeong, S., additional, Sánchez-Ramírez, R., additional, Tello, J. C., additional, Cunniffe, R., additional, Gorbovskoy, E., additional, Caballero-García, M. D., additional, Pandey, S. B., additional, Kornilov, V. G., additional, Tyurina, N. V., additional, Kuznetsov, A. S., additional, Balanutsa, P. V., additional, Gress, O. A., additional, Gorbunov, I., additional, Vlasenko, D. M., additional, Vladimirov, V. V., additional, Budnev, N. M., additional, Balakin, F., additional, Ershova, O., additional, Krushinski, V. V., additional, Gabovich, A. V., additional, Yurkov, V. V., additional, Gorosabel, J., additional, Moskvitin, A. S., additional, Burenin, R. A., additional, Sokolov, V. V., additional, Delgado, I., additional, Guziy, S., additional, Fernandez-García, E. J., additional, and Park, I. H., additional

Published
2019
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179. Swift-XRT Follow-up of Gravitational-wave Triggers in the Second Advanced LIGO/Virgo Observing Run

Author

Klingler, N. J., primary, Kennea, J. A., additional, Evans, P. A., additional, Tohuvavohu, A., additional, Cenko, S. B., additional, Barthelmy, S. D., additional, Beardmore, A. P., additional, Breeveld, A. A., additional, Brown, P. J., additional, Burrows, D. N., additional, Campana, S., additional, Cusumano, G., additional, D’Aì, A., additional, D’Avanzo, P., additional, D’Elia, V., additional, de Pasquale, M., additional, Emery, S. W. K., additional, Garcia, J., additional, Giommi, P., additional, Gronwall, C., additional, Hartmann, D. H., additional, Krimm, H. A., additional, Kuin, N. P. M., additional, Lien, A., additional, Malesani, D. B., additional, Marshall, F. E., additional, Melandri, A., additional, Nousek, J. A., additional, Oates, S. R., additional, O’Brien, P. T., additional, Osborne, J. P., additional, Page, K. L., additional, Palmer, D. M., additional, Perri, M., additional, Racusin, J. L., additional, Siegel, M. H., additional, Sakamoto, T., additional, Sbarufatti, B., additional, Tagliaferri, G., additional, and Troja, E., additional

Published
2019
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181. An Unusual Stellar Death on Christmas Day

Author

Thone, C. C, de Ugarte Postigo, A, 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, Hernandez Garcia, L, Llorente, A, and Bundy, K

Subjects
Astronomy
Abstract

Long Gamma-Ray Bursts (GRBs) are the most dramatic examples of massive stellar deaths, usually associated with supernovae. They release ultra-relativistic jets producing non-thermal emission through synchrotron radiation as they interact with the surrounding medium. 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 couuterpart. 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 io the Galaxy

Published
2011

182. Fermi and Swift Gamma-Ray Burst Afterglow Population Studies

Author

Racusin, Judith L, Oates, S. R, Schady, P, Burrows, D. N, dePasquale, M, Donato, D, Gehrels, N, Koch, S, McEnery, J, Piran, T, Roming, P, Sakamoto, T, Swenson, C, Troja, E, Vasileiou, V, Virgili, F, Wanderman, D, and Zhang, B

Subjects
Astrophysics
Abstract

The new and extreme population of GRBs detected by Fermi -LAT shows several new features in high energy gamma-rays that are providing interesting and unexpected clues into GRB prompt and afterglow emission mechanisms. Over the last 6 years, it has been Swift that has provided the robust dataset of UV/optical and X-ray afterglow observations that opened many windows into components of GRB emission structure. The relationship between the LAT detected GRBs and the well studied, fainter, less energetic GRBs detected by Swift -BAT is only beginning to be explored by multi-wavelength studies. We explore the large sample of GRBs detected by BAT only, BAT and Fermi -GBM, and GBM and LAT, focusing on these samples separately in order to search for statistically significant differences between the populations, using only those GRBs with measured redshifts in order to physically characterize these objects. We disentangle which differences are instrumental selection effects versus intrinsic properties, in order to better understand the nature of the special characteristics of the LAT bursts.

Published
2011

183. Fermi and Swift Gamma-Ray Burst Afterglow Population Studies

Author

Racusin, J. L, Oates, S. R, Schady, P, Burrows, D. N, de Pasquale, M, Donato, D, Gehrels, N, Koch, S, McEnery, J, Piran, T, Roming, P, Sakamoto, T, Swenson, C, Virgili, F, Wanderman, D, and Zhang, B

Subjects
Astronomy
Abstract

The new and extreme population of GRBs detected by Fermi-LAT shows several new features in high energy gamma-rays that are providing interesting and unexpected clues into GRB prompt and afterglow emission mechanisms. Over the last 6 years, it has been Swift that has provided the robust data set of UV/optical and X-ray afterglow observations that opened many windows into components of GRB emission structure. The relationship between the LAT GRBs and the well studied, fainter, less energetic GRBs detected by Swift-BAT is only beginning to be explored by multiwavelength studies. We explore the large sample of GRBs detected by BAT only, BAT and Fermi-GBM, and GBM and LAT, focusing on these samples separately in order to search for statistically significant differences between the populations, using only those GRBs with measured redshifts in order to physically characterize these objects. We disentangle which differences are instrumental selection effects versus intrinsic properties, in order to better understand the nature of the special characteristics of the LAT bursts.

Published
2011

184. Afterglow Population Studies from Swift Follow-Up Observations of Fermi LAT GRBs

Author

Racusin, Judith L, Oates, S. R, McEnery, J, Vasileiou, V, Troja, E, and Gehrels, N

Subjects
Astronomy
Abstract

The small population of Fermi LAT detected GRBs discovered over the last year has been providing interesting and unexpected clues into GRB prompt and afterglow emission mechanisms. Over the last 5 years, it has been Swift that has provided the robust data set of UV/optical and X-ray afterglow observations that opened many windows into other components of GRB emission structure. We explore the new ability to utilize both of these observatories to study the same GRBs over 10 orders of magnitude in energy, although not always concurrently. Almost all LAT GRBs that have been followed-up by Swift within 1-day have been clearly detected and carefully observed. We will present the context of the lower-energy afterglows of this special subset of GRBs that has > 100 MeV emission compared to the hundreds in the Swift database that may or may not have been observed by LAT, and theorize upon the relationship between these properties and the origin of the high energy gamma-ray emission.

Published
2010

185. Broadband observations of the naked-eye γ-ray burst GRB 080319B

Author

Racusin, J. L., Karpov, S. V., Sokolowski, M., Granot, J., Wu, X. F., Pal'shin, V., Covino, S., van der Horst, A. J., Oates, S. R., Schady, P., Smith, R. J., Cummings, J., Starling, R. L. C., Piotrowski, L. W., Zhang, B., Evans, P. A., Holland, S. T., Malek, K., Page, M. T., Vetere, L., Margutti, R., Guidorzi, C., Kamble, A. P., Curran, P. A., Beardmore, A., Kouveliotou, C., Mankiewicz, L., Melandri, A., O'Brien, P. T., Page, K. L., Piran, T., Tanvir, N. R., Wrochna, G., Aptekar, R. L., Barthelmy, S., Bartolini, C., Beskin, G. M., Bondar, S., Bremer, M., Campana, S., Castro-Tirado, A., Cucchiara, A., Cwiok, M., D'Avanzo, P., D'Elia, V., Valle, M. Della, Postigo, A. de Ugarte, Dominik, W., Falcone, A., Fiore, F., Fox, D. B., Frederiks, D. D., Fruchter, A. S., Fugazza, D., Garrett, M. A., Gehrels, N., Golenetskii, S., Gomboc, A., Gorosabel, J., Greco, G., Guarnieri, A., Immler, S., Jelinek, M., Kasprowicz, G., La Parola, V., Levan, A. J., Mangano, V., Mazets, E. P., Molinari, E., Moretti, A., Nawrocki, K., Oleynik, P. P., Osborne, J. P., Pagani, C., Pandey, S. B., Paragi, Z., Perri, M., Piccioni, A., Ramirez-Ruiz, E., Roming, P. W. A., Steele, I. A., Strom, R. G., Testa, V., Tosti, G., Ulanov, M. V., Wiersema, K., Wijers, R. A. M. J., Winters, J. M., Zarnecki, A. F., Zerbi, F., Mészáros, P., Chincarini, G., and Burrows, D. N.

Published
2008
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186. Clinical spectrum of STX1B-related epileptic disorders

Author

Wolking, S, May, P, Mei, D, Møller, RS, Balestrini, S, Helbig, KL, Altuzarra, CD, Chatron, N, Kaiwar, C, Stöhr, K, Widdess-Walsh, P, Mendelsohn, BA, Numis, A, Cilio, MR, Van Paesschen, W, Svendsen, LL, Oates, S, Hughes, E, Goyal, S, Brown, K, Saenz, M, Dorn, T, Muhle, H, Pagnamenta, AT, Vavoulis, DV, Knight, SJL, Taylor, JC, Canevini, MP, Darra, F, Gavrilova, RH, Powis, Z, Tang, S, Marquetand, J, Armstrong, M, McHale, D, Klee, EW, Kluger, GJ, Lowenstein, DH, Weckhuysen, S, Pal, DK, Helbig, I, Guerrini, R, Thomas, RH, Rees, MI, Lesca, G, Sisodiya, SM, Weber, YG, Lal, D, Marini, C, Lerche, H, and Schubert, J

Subjects
Male, Drug Resistant Epilepsy, Adolescent, Developmental Disabilities, Mutation, Missense, Clinical Neurology, FEBRILE SEIZURES PLUS, GENERALIZED EPILEPSY, Syntaxin 1, PROTEIN, Article, Seizures, Febrile, Young Adult, Loss of Function Mutation, Humans, HETEROGENEITY, SCN1A, Child, Epilepstic disorders, Science & Technology, Learning Disabilities, Infant, Newborn, High-Throughput Nucleotide Sequencing, Infant, GENETIC-VARIATION, Electroencephalography, Sequence Analysis, DNA, SODIUM-CHANNEL, Epilepstic disorders, STX1B, Phenotype, DE-NOVO MUTATIONS, Child, Preschool, ONSET, STXBP1, STX1B, Anticonvulsants, Female, Human medicine, Epilepsies, Partial, Neurosciences & Neurology, Epileptic Syndromes, Life Sciences & Biomedicine
Abstract

OBJECTIVE: The aim of this study was to expand the spectrum of epilepsy syndromes related to STX1B, encoding the presynaptic protein syntaxin-1B, and establish genotype-phenotype correlations by identifying further disease-related variants. METHODS: We used next-generation sequencing in the framework of research projects and diagnostic testing. Clinical data and EEGs were reviewed, including already published cases. To estimate the pathogenicity of the variants, we used established and newly developed in silico prediction tools. RESULTS: We describe 17 new variants in STX1B, which are distributed across the whole gene. We discerned 4 different phenotypic groups across the newly identified and previously published patients (49 patients in 23 families): (1) 6 sporadic patients or families (31 affected individuals) with febrile and afebrile seizures with a benign course, generally good drug response, normal development, and without permanent neurologic deficits; (2) 2 patients with genetic generalized epilepsy without febrile seizures and cognitive deficits; (3) 13 patients or families with intractable seizures, developmental regression after seizure onset and additional neuropsychiatric symptoms; (4) 2 patients with focal epilepsy. More often, we found loss-of-function mutations in benign syndromes, whereas missense variants in the SNARE motif of syntaxin-1B were associated with more severe phenotypes. CONCLUSION: These data expand the genetic and phenotypic spectrum of STX1B-related epilepsies to a diverse range of epilepsies that span the International League Against Epilepsy classification. Variants in STX1B are protean and contribute to many different epilepsy phenotypes, similar to SCN1A, the most important gene associated with fever-associated epilepsies. ispartof: NEUROLOGY vol:92 issue:11 pages:E1238-E1249 ispartof: location:United States status: published

Published
2019

187. A Multiwavelength Analysis Of A Collection Of Short-Duration Grbs Observed Between 2012 And 2015

Author

Pandey, S. B., Hu, Y., Castro-Tirado, Ao J., Pozanenko, A. S., Sanchez-Ramirez, R., Gorosabel, J., Guziy, S., Jelinek, M., Tello, J. C., Jeong, S., Oates, S. R., Zhang, B. -B., Mazaeva, E. D., Volnova, A. A., Minaev, P. Yu., van Eerten, H. J., Caballero-Garcia, M. D., Perez-Ramirez, D., Bremer, M., and Winters, J. -M.

Abstract

We investigate the prompt emission and the afterglow properties of short-duration gamma-ray burst (sGRB) 130603B and another eight sGRB events during 2012-2015, observed by several multiwavelength facilities including the Gran Canarias Telescope 10.4m telescope. Prompt emission high energy data of the events were obtained by INTEGRAL-SPI-ACS, Swift-BAT, and Fermi-GBM satellites. The prompt emission data by INTEGRAL in the energy range of 0.1-10 MeV for sGRB 130603B, sGRB 140606A, sGRB 140930B, sGRB 141212A, and sGRB 151228A do not show any signature of the extended emission or precursor activity and their spectral and temporal properties are similar to those seen in case of other short bursts. For sGRB 130603B, our new afterglow photometric data constrain the pre-jet-break temporal decay due to denser temporal coverage. For sGRB130603B, the afterglowlight curve, containing both our new and previously published photometric data is broadly consistent with the ISMafterglowmodel. Modeling of the host galaxies of sGRB 130603B and sGRB 141212A using the LePHARE software supports a scenario in which the environment of the burst is undergoing moderate star formation activity. From the inclusion of our late-time data for eight other sGRBs we are able to: place tight constraints on the non-detection of the afterglow, host galaxy, or any underlying 'kilonova' emission. Our late-time afterglow observations of the sGRB 170817A/GW170817 are also discussed and compared with the sub-set of sGRBs.

Published
2019

188. Multiwavelength observations of GRB 140629A. A long burst with an achromatic jet break in the optical and X-ray afterglow

Author

Hu, Y. -D., Oates, S. R., Lipunov, V. M., Zhang, B. -B., Castro-Tirado, A. J., Jeong, S., Sánchez-Ramírez, R., Tello, J. C., Cunniffe, R., Gorbovskoy, E., Caballero-García, M. D., Pandey, S. B., Kornilov, V. G., Tyurina, N. V., Kuznetsov, A. S., Balanutsa, P. V., Gress, O. A., Gorbunov, I., Vlasenko, D. M., Vladimirov, V. V., Budnev, N. M., Balakin, F., Ershova, O., Krushinski, V. V., Gabovich, A. V., Yurkov, V. V., Gorosabel, J., Moskvitin, A. S., Burenin, R. A., Sokolov, V. V., Delgado, I., Guziy, S., Fernandez-García, E. J., Park, I. H., Hu, Y. -D., Oates, S. R., Lipunov, V. M., Zhang, B. -B., Castro-Tirado, A. J., Jeong, S., Sánchez-Ramírez, R., Tello, J. C., Cunniffe, R., Gorbovskoy, E., Caballero-García, M. D., Pandey, S. B., Kornilov, V. G., Tyurina, N. V., Kuznetsov, A. S., Balanutsa, P. V., Gress, O. A., Gorbunov, I., Vlasenko, D. M., Vladimirov, V. V., Budnev, N. M., Balakin, F., Ershova, O., Krushinski, V. V., Gabovich, A. V., Yurkov, V. V., Gorosabel, J., Moskvitin, A. S., Burenin, R. A., Sokolov, V. V., Delgado, I., Guziy, S., Fernandez-García, E. J., and Park, I. H.

Abstract

We investigate the long GRB140629A through multiwavelength observations, which cover optical, infrared and X-rays between 40s and 3yr after the burst, to derive the properties of the dominant jet and its host galaxy. Polarisation observations by the MASTER telescope indicate that this burst is weakly polarised. The optical spectrum contains absorption features, from which we confirm the redshift of the GRB as originating at z=2.276. We performed spectral fitting of the X-rays to optical afterglow data and find there is no strong spectral evolution. We determine the hydrogen column density to be 7.2x10^21cm^-2 along the line of sight. The afterglow in this burst can be explained by a blast wave jet with a long-lasting central engine expanding into a uniform medium in the slow cooling regime. At the end of energy injection, a normal decay phase is observed in both the optical and X-ray bands. An achromatic jet break is also found in the afterglow light curves 0.4d after trigger. We fit the multiwavelength data simultaneously with a model based on a numerical simulation and find that the observations can be explained by a narrow uniform jet in a dense environment with an opening angle of 6.7deg viewed 3.8deg off-axis, which released a total energy of 1.4x10^54erg. Using the redshift and opening angle, we find GRB 140629A follows both the Ghirlanda and Amati relations. From the peak time of the light curve, identified as the onset of the forward shock (181s after trigger), the initial Lorentz factor is constrained in the range 82-118. Fitting the host galaxy photometry, we find the host to be a low mass, star-forming galaxy with a star formation rate of logSFR=1.1^+0.9_-0.4Myr^-1. We obtain a value of the neutral hydrogen density by fitting the optical spectrum, logN(HI)=21.0+-0.3, classifying this host as a damped Lyman-alpha. High ionisation lines are also detected in the spectrum., Comment: 18 pages, 13 figures, 8 tables, accepted for publication in A&A

Published
2019
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189. A study of gamma-ray burst afterglows as they first come into view of the Swift Ultraviolet and Optical Telescope

Author

Page, M. J., Oates, S. R., De Pasquale, M., Breeveld, A. A., Emery, S. W. K., Kuin, N. P. M., Marshall, F. E., Siegel, M. H., Roming, P. W. A., Page, M. J., Oates, S. R., De Pasquale, M., Breeveld, A. A., Emery, S. W. K., Kuin, N. P. M., Marshall, F. E., Siegel, M. H., and Roming, P. W. A.

Abstract

We examine the the emission from optically bright gamma-ray burst (GRB) afterglows as the Ultraviolet and Optical Telescope (UVOT) on the Neil Gehrels Swift Observatory first begins observing, following the slew to target the GRB, while the pointing of the Swift satellite is still settling. We verify the photometric quality of the UVOT settling data using bright stars in the field of view. In the majority of cases we find no problems with the settling exposure photometry, but in one case we excise the first second of the exposure to mitigate a spacecraft attitude reconstruction issue, and in a second case we exclude the first second of the exposure in which the UVOT photocathode voltage appears to be ramping up. Of a sample of 23 afterglows which have peak V magnitudes <16, we find that all are detected in the settling exposures, when Swift arrives on target. For 9 of the GRBs the UVOT settling exposure took place before the conclusion of the prompt gamma-ray emission. Five of these GRBs have well defined optical peaks after the settling exposures, with rises of >0.5 mag in their optical lightcurves, and there is a marginal trend for these GRBs to have long T90. Such a trend is expected for thick-shell afterglows, but the temporal indices of the optical rises and the timing of the optical peaks appear to rule out thick shells., Comment: accepted for publication in MNRAS

Published
2019
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190. A multi-wavelength analysis of a collection of short-duration GRBs observed between 2012-2015

Author

Pandey, S. B., Hu, Y., Castro-Tirado, A. J., Pozanenko, A. S., Sánchez-Ramírez, R., Gorosabel, J., Guziy, 5 S., Jelinek, M., Tello, J. C., Jeong, S., Oates, S. R., Zhang, B. -B., Mazaeva, E. D., Volnova, A. A., Minaev, P. Yu., van Eerten, H. J., Caballero-García, M. D., Pérez-Ramírez, D., Bremer, M., Winters, J. -M., Park, I. H., Guelbenzu, A. Nicuesa, Klose, S., Moskvitin, A., Sokolov, V. V., Sonbas, E., Ayala, A., Cepa, J., Butler, N., Troja, E., Chernenko, A. M., Molkov, S. V., Volvach, A. E., Inasaridze, R. Ya., Egamberdiyev, Sh. A., Burkhonov, O., Reva, I. V., Polyakov, K. A., Matkin, A. A., Ivanov, A. L., Molotov, I., Guver, T., Watson, A. M., Kutyrev, A., Lee, W. H., Fox, O., Littlejohns, O., Cucchiara, A., Gonzalez, J., Richer, M. G., Román-Zúñiga, C. G., Tanvir, N. R., Bloom, J. S., Prochaska, J. X., Gehrels, N., Moseley, H., de Diego, J. A., Ramírez-Ruiz, E., Klunko, E. V., Fan, Y., Zhao, X., Bai, J., Wang, Ch., Xin, Y., Cui, Ch., Tungalag, N., Peng, Z. -K., Kumar, Amit, Gupta, Rahul, Aryan, Amar, Kumar, Brajesh, Volvach, L. N., Lamb, G. P., Valeev, A. F., Pandey, S. B., Hu, Y., Castro-Tirado, A. J., Pozanenko, A. S., Sánchez-Ramírez, R., Gorosabel, J., Guziy, 5 S., Jelinek, M., Tello, J. C., Jeong, S., Oates, S. R., Zhang, B. -B., Mazaeva, E. D., Volnova, A. A., Minaev, P. Yu., van Eerten, H. J., Caballero-García, M. D., Pérez-Ramírez, D., Bremer, M., Winters, J. -M., Park, I. H., Guelbenzu, A. Nicuesa, Klose, S., Moskvitin, A., Sokolov, V. V., Sonbas, E., Ayala, A., Cepa, J., Butler, N., Troja, E., Chernenko, A. M., Molkov, S. V., Volvach, A. E., Inasaridze, R. Ya., Egamberdiyev, Sh. A., Burkhonov, O., Reva, I. V., Polyakov, K. A., Matkin, A. A., Ivanov, A. L., Molotov, I., Guver, T., Watson, A. M., Kutyrev, A., Lee, W. H., Fox, O., Littlejohns, O., Cucchiara, A., Gonzalez, J., Richer, M. G., Román-Zúñiga, C. G., Tanvir, N. R., Bloom, J. S., Prochaska, J. X., Gehrels, N., Moseley, H., de Diego, J. A., Ramírez-Ruiz, E., Klunko, E. V., Fan, Y., Zhao, X., Bai, J., Wang, Ch., Xin, Y., Cui, Ch., Tungalag, N., Peng, Z. -K., Kumar, Amit, Gupta, Rahul, Aryan, Amar, Kumar, Brajesh, Volvach, L. N., Lamb, G. P., and Valeev, A. F.

Abstract

We investigate the prompt emission and the afterglow properties of short duration gamma-ray burst (sGRB) 130603B and another eight sGRB events during 2012-2015, observed by several multi-wavelength facilities including the GTC 10.4m telescope. Prompt emission high energy data of the events were obtained by INTEGRAL/SPI/ACS, Swift/BAT and Fermi/GBM satellites. The prompt emission data by INTEGRAL in the energy range of 0.1-10 MeV for sGRB 130603B, sGRB 140606A, sGRB 140930B, sGRB 141212A and sGRB 151228A do not show any signature of the extended emission or precursor activity and their spectral and temporal properties are similar to those seen in case of other short bursts. For sGRB130603B, our new afterglow photometric data constraints the pre jet-break temporal decay due to denser temporal coverage. For sGRB 130603B, the afterglow light curve, containing both our new as well as previously published photometric data is broadly consistent with the ISM afterglow model. Modeling of the host galaxies of sGRB 130603B and sGRB 141212A using the LePHARE software supports a scenario in which the environment of the burst is undergoing moderate star formation activity. From the inclusion of our late-time data for 8 other sGRBs we are able to; place tight constraints on the non-detection of the afterglow, host galaxy or any underlying kilonova emission. Our late-time afterglow observations of the sGRB 170817A/GW170817 are also discussed and compared with the sub-set of sGRBs., Comment: 24 pages, 22 figures, Accepted to MNRAS, 2019 February 19. Received 2019 February 19; in original form 2018 August 30

Published
2019
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191. Swift-XRT Follow-up of Gravitational-wave Triggers in the Second Advanced LIGO/Virgo Observing Run

Author

Klingler, N. J., Kennea, J. A., Evans, P. A., Tohuvavohu, A., Cenko, S. B., Barthelmy, S. D., Beardmore, A. P., Breeveld, A. A., Brown, P. J., Burrows, D. N., Campana, S., Cusumano, G., D'Ai, A., D'Avanzo, P., D'Elia, V, de Pasquale, M., Emery, S. W. K., Garcia, J., Giommi, P., Gronwall, C., Hartmann, D. H., Krimm, H. A., Kuin, N. P. M., Lien, A., Malesani, D. B., Marshall, F. E., Melandri, A., Nousek, J. A., Oates, S. R., O'Brien, P. T., Osborne, J. P., Page, K. L., Palmer, D. M., Perri, M., Racusin, J. L., Siegel, M. H., Sakamoto, T., Sbarufatti, B., Tagliaferri, G., Troja, E., Klingler, N. J., Kennea, J. A., Evans, P. A., Tohuvavohu, A., Cenko, S. B., Barthelmy, S. D., Beardmore, A. P., Breeveld, A. A., Brown, P. J., Burrows, D. N., Campana, S., Cusumano, G., D'Ai, A., D'Avanzo, P., D'Elia, V, de Pasquale, M., Emery, S. W. K., Garcia, J., Giommi, P., Gronwall, C., Hartmann, D. H., Krimm, H. A., Kuin, N. P. M., Lien, A., Malesani, D. B., Marshall, F. E., Melandri, A., Nousek, J. A., Oates, S. R., O'Brien, P. T., Osborne, J. P., Page, K. L., Palmer, D. M., Perri, M., Racusin, J. L., Siegel, M. H., Sakamoto, T., Sbarufatti, B., Tagliaferri, G., and Troja, E.

Published
2019

192. The Optical Afterglow of GW170817 at One Year Post-merger

Author

Lamb, G. P., Lyman, J. D., Levan, A. J., Tanvir, N. R., Kangas, T., Fruchter, A. S., Gompertz, B., Hjorth, J., Mandel, I., Oates, S. R., Steeghs, D., Wiersema, K., Lamb, G. P., Lyman, J. D., Levan, A. J., Tanvir, N. R., Kangas, T., Fruchter, A. S., Gompertz, B., Hjorth, J., Mandel, I., Oates, S. R., Steeghs, D., and Wiersema, K.

Published
2019

193. GRB161219B/SN2016jca:a powerful stellar collapse

Author

Ashall, C., Mazzali, P. A., Pian, E., Woosley, S. E., Palazzi, E., Prentice, S. J., Kobayashi, S., Holmbo, S., Levan, A., Perley, D., Stritzinger, M. D., Bufano, F., Filippenko, A. V., Melandri, A., Oates, S., Rossi, A., Selsing, J., Zheng, W., Castro-Tirado, A. J., Chincarini, G., D'Avanzo, P., De Pasquale, M., Emery, S., Fruchter, A. S., Hurley, K., Moller, P., Nomoto, K., Tanaka, M., Valeev, A. F., Ashall, C., Mazzali, P. A., Pian, E., Woosley, S. E., Palazzi, E., Prentice, S. J., Kobayashi, S., Holmbo, S., Levan, A., Perley, D., Stritzinger, M. D., Bufano, F., Filippenko, A. V., Melandri, A., Oates, S., Rossi, A., Selsing, J., Zheng, W., Castro-Tirado, A. J., Chincarini, G., D'Avanzo, P., De Pasquale, M., Emery, S., Fruchter, A. S., Hurley, K., Moller, P., Nomoto, K., Tanaka, M., and Valeev, A. F.

Published
2019

194. GRB 161219B/SN 2016jca: a powerful stellar collapse

Author

Independent Research Fund Denmark, Instrument Center for Danish Astrophysics, Leverhulme Trust, Istituto Nazionale di Astrofisica, National Science Foundation (US), Ministerio de Economía y Competitividad (España), European Commission, National Aeronautics and Space Administration (US), Russian Science Foundation, Villum Fonden, Ashall, Chris, Mazzali, Paolo A., Pian, E., Woosley, S.E., Palazzi, E., Prentice, S.J., Kobayashi, S., Holmbo, S., Levan, A., Perley, D., Stritzinger, Maximilian, Bufano, F., Filippenko, Alexei V., Melandri, A., Oates, S., Rossi, A., Selsing, J., Zheng, W., Castro-Tirado, Alberto J., Chincarini, G., D'Avanzo, P., De Pasquale, M., Emery, S., Fruchter, Andrew S., Hurley, K., Moller, P., Nomoto, K., Tanaka, M., Valeev, A.F., Independent Research Fund Denmark, Instrument Center for Danish Astrophysics, Leverhulme Trust, Istituto Nazionale di Astrofisica, National Science Foundation (US), Ministerio de Economía y Competitividad (España), European Commission, National Aeronautics and Space Administration (US), Russian Science Foundation, Villum Fonden, Ashall, Chris, Mazzali, Paolo A., Pian, E., Woosley, S.E., Palazzi, E., Prentice, S.J., Kobayashi, S., Holmbo, S., Levan, A., Perley, D., Stritzinger, Maximilian, Bufano, F., Filippenko, Alexei V., Melandri, A., Oates, S., Rossi, A., Selsing, J., Zheng, W., Castro-Tirado, Alberto J., Chincarini, G., D'Avanzo, P., De Pasquale, M., Emery, S., Fruchter, Andrew S., Hurley, K., Moller, P., Nomoto, K., Tanaka, M., and Valeev, A.F.

Abstract

We report observations and analysis of the nearby gamma-ray burst GRB 161219B (redshift z = 0.1475) and the associated Type Ic supernova (SN) 2016jca. GRB 161219B had an isotropic gamma-ray energy of ∼1.6 × 10 erg. Its afterglow is likely refreshed at an epoch preceding the first photometric points (0.6 d), which slows down the decay rates. Combined analysis of the SN light curve and multiwavelength observations of the afterglow suggest that the GRB jet was broad during the afterglow phase (full opening angle ∼42° ± 3°). Our spectral series shows broad absorption lines typical of GRB supernovae (SNe), which testify to the presence of material with velocities up to ∼0.25c. The spectrum at 3.73 d allows for the very early identification of an SN associated with a GRB. Reproducing it requires a large photospheric velocity (35000 ± 7000 km s). The kinetic energy of the SN is estimated through models to be E≈4 × 10 erg in spherical symmetry. The ejected mass in the explosion was M≈6.5 ± 1.5 M⊙, much less than that of other GRB-SNe, demonstrating diversity among these events. The total amount of Ni in the explosion was 0.27 ± 0.05 M⊙. The observed spectra require the presence of freshly synthesized Ni at the highest velocities, at least three times more than a standard GRB-SN. We also find evidence for a decreasing Ni abundance as a function of decreasing velocity. This suggests that SN 2016jca was a highly aspherical explosion viewed close to on-axis, powered by a compact remnant. Applying a typical correction for asymmetry, the energy of SN 2016jca was ∼(1-3) × 10 erg, confirming that most of the energy produced by GRB-SNe goes into the kinetic energy of the SN ejecta.© 2019 The Author(s).

Published
2019

195. 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, and Tello, J C

Subjects
*GAMMA ray bursts, *RADIANT intensity, *INTERSTELLAR medium, *EMISSION spectroscopy, *OPTICAL telescopes, *TIME-resolved spectroscopy
Abstract

We present and perform a detailed analysis of multiwavelength observations of GRB 140102A, 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 (E p) tracks intensity and the low-energy spectral index seems to follow the intensity for the first episode, whereas this tracking behaviour 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 model. We determine the properties of the shocks, Lorentz factor, magnetization parameters, and ambient density of GRB 140102A, and compare these parameters with another 12 GRBs, consistent with having RS produced by thin shells in an interstellar medium like medium. The value of the magnetization parameter (R B ≈ 18) indicates a moderately magnetized baryonic dominant jet composition for GRB 140102A. We also report the host galaxy photometric observations of GRB 140102A obtained with 10.4 m GTC, 3.5 m Calar Alto Astronomical Observatory, and 3.6 m Devasthal optical telescope 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 |$20 \pm 10 {\rm ~M_{\odot }}\, \rm yr^{-1}$|⁠. [ABSTRACT FROM AUTHOR]

Published
2021
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196. Swift UVOT observations of the 2015 outburst of V404 Cygni

Author

Oates, S R, primary, Motta, S, additional, Beardmore, A P, additional, Russell, D M, additional, Gandhi, P, additional, Kuin, N P M, additional, De Pasquale, M, additional, Altamirano, D, additional, Breeveld, A A, additional, Castro-Tirado, A J, additional, Knigge, C, additional, Page, M J, additional, and Steeghs, D, additional

Published
2019
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198. GRB 161219B/SN 2016jca: a powerful stellar collapse

Author

Ashall, C, primary, Mazzali, P A, primary, Pian, E, primary, Woosley, S E, primary, Palazzi, E, primary, Prentice, S J, primary, Kobayashi, S, primary, Holmbo, S, primary, Levan, A, primary, Perley, D, primary, Stritzinger, M D, primary, Bufano, F, primary, Filippenko, A V, primary, Melandri, A, primary, Oates, S, primary, Rossi, A, primary, Selsing, J, primary, Zheng, W, primary, Castro-Tirado, A J, primary, Chincarini, G, primary, D’Avanzo, P, primary, De Pasquale, M, primary, Emery, S, primary, Fruchter, A S, primary, Hurley, K, primary, Moller, P, primary, Nomoto, K, primary, Tanaka, M, primary, and Valeev, A F, primary

Published
2019
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199. A multiwavelength analysis of a collection of short-duration GRBs observed between 2012 and 2015

Author

Pandey, S B, primary, Hu, Y, primary, Castro-Tirado, Ao J, primary, Pozanenko, A S, primary, Sánchez-Ramírez, R, primary, Gorosabel, J, primary, Guziy, S, primary, Jelinek, M, primary, Tello, J C, primary, Jeong, S, primary, Oates, S R, primary, Zhang, B-B, primary, Mazaeva, E D, primary, Volnova, A A, primary, Minaev, P Yu, primary, van Eerten, H J, primary, Caballero-García, M D, primary, Pérez-Ramírez, D, primary, Bremer, M, primary, Winters, J-M, primary, Park, I H, primary, Guelbenzu, A Nicuesa, primary, Klose, S, primary, Moskvitin, A, primary, Sokolov, V V, primary, Sonbas, E, primary, Ayala, A, primary, Cepa, J, primary, Butler, N, primary, Troja, E, primary, Chernenko, A M, primary, Molkov, S V, primary, Volvach, A E, primary, Inasaridze, R Ya, primary, Egamberdiyev, Sh A, primary, Burkhonov, O, primary, Reva, I V, primary, Polyakov, K A, primary, Matkin, A A, primary, Ivanov, A L, primary, Molotov, I, primary, Guver, T, primary, Watson, A M, primary, Kutyrev, A, primary, Lee, W H, primary, Fox, O, primary, Littlejohns, O, primary, Cucchiara, A, primary, Gonzalez, J, primary, Richer, M G, primary, Román-Zúñiga, C G, primary, Tanvir, N R, primary, Bloom, J S, primary, Prochaska, J X, primary, Gehrels, N, primary, Moseley, H, primary, de Diego, J A, primary, Ramírez-Ruiz, E, primary, Klunko, E V, primary, Fan, Y, primary, Zhao, X, primary, Bai, J, primary, Wang, Ch, primary, Xin, Y, primary, Cui, Ch, primary, Tungalag, N, primary, Peng, Z-K, primary, Kumar, Amit, primary, Gupta, Rahul, primary, Aryan, Amar, primary, Kumar, Brajesh, primary, Volvach, L N, primary, Lamb, G P, primary, and Valeev, A F, primary

Published
2019
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