143 results on '"Tohuvavohu A"'
Search Results
102. Rapid spectral variability of a giant flare from a magnetar in NGC 253
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Roberts, O. J., primary, Veres, P., additional, Baring, M. G., additional, Briggs, M. S., additional, Kouveliotou, C., additional, Bissaldi, E., additional, Younes, G., additional, Chastain, S. I., additional, DeLaunay, J. J., additional, Huppenkothen, D., additional, Tohuvavohu, A., additional, Bhat, P. N., additional, Göğüş, E., additional, van der Horst, A. J., additional, Kennea, J. A., additional, Kocevski, D., additional, Linford, J. D., additional, Guiriec, S., additional, Hamburg, R., additional, Wilson-Hodge, C. A., additional, and Burns, E., additional
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- 2021
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103. Swift-XRT follow-up of gravitational wave triggers during the third aLIGO/Virgo observing run
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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
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- 2020
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104. Rotation Optimized Filter for Longevity (ROFL): Increasing the Lifetime of Swift/UVOT Simply
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Tohuvavohu, Aaron, primary
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- 2020
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105. Gamma-Ray Urgent Archiver for Novel Opportunities (GUANO): Swift/BAT Event Data Dumps on Demand to Enable Sensitive Subthreshold GRB Searches
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Tohuvavohu, Aaron, primary, Kennea, Jamie A., additional, DeLaunay, James, additional, Palmer, David M., additional, Cenko, S. Bradley, additional, and Barthelmy, Scott, additional
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- 2020
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106. Multimessenger observations of counterparts to IceCube-190331A
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Krauß, Felicia, primary, Calamari, Emily, additional, Keivani, Azadeh, additional, Coleiro, Alexis, additional, Evans, Phil A, additional, Fox, Derek B, additional, Kennea, Jamie A, additional, Mészáros, Peter, additional, Murase, Kohta, additional, Russell, Thomas D, additional, Santander, Marcos, additional, and Tohuvavohu, Aaron, additional
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- 2020
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107. The Gravitational Wave Treasure Map: A Tool to Coordinate, Visualize, and Assess the Electromagnetic Follow-up of Gravitational-wave Events
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Wyatt, Samuel D., primary, Tohuvavohu, Aaron, additional, Arcavi, Iair, additional, Lundquist, Michael J., additional, Howell, D. Andrew, additional, and Sand, David J., additional
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- 2020
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108. Multi-epoch Modeling of TXS 0506+056 and Implications for Long-term High-energy Neutrino Emission
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Petropoulou, Maria, primary, Murase, Kohta, additional, Santander, Marcos, additional, Buson, Sara, additional, Tohuvavohu, Aaron, additional, Kawamuro, Taiki, additional, Vasilopoulos, Georgios, additional, Negoro, Hiroshi, additional, Ueda, Yoshihiro, additional, Siegel, Michael H., additional, Keivani, Azadeh, additional, Kawai, Nobuyuki, additional, Mastichiadis, Apostolos, additional, and Dimitrakoudis, Stavros, additional
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- 2020
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109. GW170817: Swift UV detection of a blue kilonova, and improving the search in O3
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A. Tohuvavohu and J. A. Kennea
- Subjects
Swift ,Physics ,010308 nuclear & particles physics ,Gravitational wave ,media_common.quotation_subject ,Astronomy and Astrophysics ,Field (mathematics) ,Astrophysics ,Kilonova ,01 natural sciences ,Galaxy ,Space and Planetary Science ,Sky ,0103 physical sciences ,Sensitivity (control systems) ,Uv detection ,010303 astronomy & astrophysics ,computer ,computer.programming_language ,media_common - Abstract
Swift’s rapid slewing, flexible planning, and multi-wavelength instruments make it the most capable space-based follow-up engine for finding poorly localized sources. During O1 and O2 Swift successfully tiled hundreds of square-degrees of sky in the LVC localization regions, searching for, and identifying, possible X-ray and UV/O transients in the field. Swift made important contributions to the discovery and characterization of the kilonova AT 2017gfo, discovering the UV emission and providing the deepest X-ray upper limits in the first 24 hours after the trigger, strongly constraining the dynamics and geometry of the counterpart. Swift tiled 92% of the galaxy convolved error region down to average X-ray flux sensitivities of 10−12 erg cm−2 s−1, significantly increasing our confidence that AT 2017gfo is indeed the counterpart to GW 170817 and sGRB 170817. However, there remains significant room for improvement of Swift’s follow-up in preparation for O3. This will take the form of both revised observation strategy based on detailed analysis of the results from O2, and significant changes to Swift’s operational capabilities. These improvements are necessary both for maximizing the likelihood that Swift finds a counterpart, and minimizing the impact that follow-up activities have on other Swift science priorities. We outline areas of improvement to the observing strategy itself for optimal tiling of the LVC localization regions. We also discuss ongoing work on operational upgrades that will decrease latency in our response time, and minimize impact on pre-planned observations, while maintaining spacecraft health and safety.
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- 2017
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110. The Gravitational Wave Treasure Map: A Tool to Coordinate, Visualize, and Assess the Electromagnetic Follow-Up of Gravitational Wave Events
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Iair Arcavi, D. Andrew Howell, David J. Sand, Michael J. Lundquist, S. Wyatt, and A. Tohuvavohu
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High Energy Astrophysical Phenomena (astro-ph.HE) ,Physics ,010504 meteorology & atmospheric sciences ,Interface (Java) ,Gravitational wave ,Stochastic game ,FOS: Physical sciences ,Astronomy ,Astronomy and Astrophysics ,01 natural sciences ,Gravitational-wave astronomy ,Square (algebra) ,Space and Planetary Science ,0103 physical sciences ,Treasure ,Astrophysics - High Energy Astrophysical Phenomena ,Astrophysics - Instrumentation and Methods for Astrophysics ,Instrumentation and Methods for Astrophysics (astro-ph.IM) ,010303 astronomy & astrophysics ,0105 earth and related environmental sciences ,Overall efficiency - Abstract
We present the Gravitational Wave Treasure Map, a tool to coordinate, visualize, and assess the electromagnetic follow-up of gravitational wave (GW) events. With typical GW localization regions of hundreds to thousands of square degrees and dozens of active follow-up groups, the pursuit of electromagnetic (EM) counterparts is a challenging endeavor, but the scientific payoff for early discovery of any counterpart is clear. With this tool, we provide a website and API interface that allows users to easily see where other groups have searched and better inform their own follow-up search efforts. A strong community of Treasure Map users will increase the overall efficiency of EM counterpart searches and will play a fundamental role in the future of multi-messenger astronomy., 14 pages, 8 figures, Accepted to ApJ
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- 2020
111. Multi-epoch Modeling of TXS 0506+056 and Implications for Long-term High-energy Neutrino Emission
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Petropoulou, Maria Murase, Kohta Santander, Marcos Buson, Sara Tohuvavohu, Aaron Kawamuro, Taiki Vasilopoulos, Georgios Negoro, Hiroshi Ueda, Yoshihiro Siegel, Michael H. and Keivani, Azadeh Kawai, Nobuyuki Mastichiadis, Apostolos and Dimitrakoudis, Stavros
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Astrophysics::High Energy Astrophysical Phenomena ,Astrophysics::Cosmology and Extragalactic Astrophysics - Abstract
The IceCube report of a 3.5s excess of 13.+/-.5 neutrino events in the direction of the blazar TXS.0506+056 in 2014-2015 and the 2017 detection of a high-energy neutrino event, IceCube-170922A, during a gamma-ray flare from the same blazar, have revived the interest in scenarios for neutrino production in blazars. We perform comprehensive analyses on the long-term electromagnetic emission of TXS.0506+056 using optical, X-ray, and gamma-ray data from the All-Sky Automated Survey for Supernovae, the Neil Gehrels Swift Observatory, Monitor of All-sky X-ray Image, and the Fermi Large Area Telescope. We also perform numerical modeling of the spectral energy distributions (SEDs) in four epochs prior to 2017 with contemporaneous gamma-ray and lower-energy (optical and/or X-ray) data. We find that the multi-epoch SEDs are consistent with a hybrid leptonic scenario, where the gamma-rays are produced in the blazar zone via external inverse Compton scattering of accelerated electrons, and high-energy neutrinos are produced via the photomeson production process of co-accelerated protons. The multi-epoch SEDs can be satisfactorily explained with the same jet parameters and variable external photon density and electron luminosity. Using the maximal neutrino flux derived for each epoch, we put an upper limit of 0.4-2 on the muon neutrino number in 10 years of IceCube observations. Our results are consistent with the IceCube-170922A detection, which can be explained as an upper fluctuation from the average neutrino rate expected from the source, but in strong tension with the 2014-2015 neutrino flare.
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- 2020
112. Multi-Epoch Modeling of TXS 0506+056 and Implications for Long-Term High-Energy Neutrino Emission
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Apostolos Mastichiadis, Azadeh Keivani, Sara Buson, A. Tohuvavohu, Yoshihiro Ueda, Stavros Dimitrakoudis, Taiki Kawamuro, Michael H. Siegel, H. Negoro, Kohta Murase, Marcos Santander, Georgios Vasilopoulos, Nobuyuki Kawai, and Maria Petropoulou
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010504 meteorology & atmospheric sciences ,Astrophysics::High Energy Astrophysical Phenomena ,FOS: Physical sciences ,Astrophysics ,Astrophysics::Cosmology and Extragalactic Astrophysics ,7. Clean energy ,01 natural sciences ,law.invention ,Luminosity ,law ,0103 physical sciences ,Muon neutrino ,Blazar ,010303 astronomy & astrophysics ,Astrophysics::Galaxy Astrophysics ,0105 earth and related environmental sciences ,High Energy Astrophysical Phenomena (astro-ph.HE) ,Physics ,Compton scattering ,Astronomy and Astrophysics ,Supernova ,13. Climate action ,Space and Planetary Science ,Neutrino ,Astrophysics - High Energy Astrophysical Phenomena ,Flare ,Fermi Gamma-ray Space Telescope - Abstract
The IceCube report of a $\sim 3.5\sigma$ excess of $13\pm5$ neutrino events in the direction of the blazar TXS 05056+056 in 2014-2015 and the 2017 detection of a high-energy neutrino, IceCube-170922A, during a gamma-ray flare from the same blazar, have revived the interest in scenarios for neutrino production in blazars. We perform comprehensive analyses on the long-term electromagnetic emission of TXS 05056+056 using optical, X-ray, and gamma-ray data from the All-Sky Automated Survey for Supernovae (ASAS-SN), the Neil Gehrels Swift Observatory (Swift), the Monitor of All-sky X-ray Image (MAXI), and the Fermi Large Area Telescope (Fermi-LAT). We also perform numerical modeling of the spectral energy distributions (SEDs) in four epochs prior to 2017 with contemporaneous gamma-ray and lower energy (optical and/or X-ray) data. We find that the multi-epoch SEDs are consistent with a hybrid leptonic scenario, where the gamma-rays are produced in the blazar zone via external inverse Compton scattering of accelerated electrons, and high-energy neutrinos are produced via the photomeson production process of co-accelerated protons. The multi-epoch SEDs can be satisfactorily explained with the same jet parameters and variable external photon density and electron luminosity. Using the maximal neutrino flux derived for each epoch, we put an upper limit of $\sim0.4-2$ on the muon neutrino number in ten years of IceCube observations. Our results are consistent with the IceCube-170922A detection, which can be explained as an upper fluctuation from the average neutrino rate expected from the source, but in strong tension with the 2014-2015 neutrino flare., Comment: 24 pages, 8 figures, 11 tables, accepted for publication in ApJ
- Published
- 2019
113. A Vision for Canadian Leadership in Multi-Messenger Astrophysics in the Next Decade
- Author
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Ruan, John J., Afsari, Niloufar, Brunner, Thomas, Carlberg, Raymond, Doyon, Rene, Drout, Maria, Dykaar, Hannah, Fernandez, Rodrigo, Gaensler, Bryan, Haggard, Daryl, Kaspi, Victoria, Lafreniere, David, McIver, Jess, Moon, Dae-Sik, Ni, Yuan Chris, Safi-Harb, Samar, Spekkens, Kristine, Tohuvavohu, Aaron, Vieira, Nicholas, and Virtue, Clarence J.
- Subjects
astrophysics - Abstract
Multi-messenger astronomy is currently entering a golden era of discovery. Our new abilities to detect individual sources using combinations of electromagnetic emission, gravitational waves, and cosmic neutrinos enable novel probes of matter at extreme densities, the origin of the elements, and the acceleration of cosmic rays. Over the next decade, the pace of multi-messenger discoveries will rapidly accelerate, thanks to planned upgrades to current GW detectors and new GW facilities that will come online. For several classes of new GW sources (e.g., core collapse supernovae), additional multi-messenger observations of neutrinos may be expected. The Canadian multi-messenger astrophysics community has reached a critical mass, and is well-poised to take a leadership role in upcoming landmark discoveries. Our efforts will utilize new Canadian telescope facilities that are scheduled to come online over the next decade such as JWST, LSST, TMT, SKA, and CASTOR. These new facilities will enable multi-messenger studies of GW events at progressively larger distances, in lockstep with planned sensitivity upgrades to GW detectors. However, challenges await, and we make recommendations that will ensure Canadian leadership in the next breakthrough discoveries in this burgeoning field., White paper identifier W042
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- 2019
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114. Fermi and Swift Observations of GRB 190114C : Tracing the Evolution of High-energy Emission from Prompt to Afterglow
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Ajello, M., Arimoto, M., Axelsson, Magnus, Baldini, L., Barbiellini, G., Bastieri, D., Bellazzini, R., Berretta, A., Bissaldi, E., Blandford, R. D., Bonino, R., Bottacini, E., Bregeon, J., Bruel, P., Buehler, R., Burns, E., Buson, S., Cameron, R. A., Caputo, R., Caraveo, P. A., Cavazzuti, E., Chen, S., Chiaro, G., Ciprini, S., Cohen-Tanugi, J., Costantin, D., Cutini, S., D'Ammando, F., DeKlotz, M., Luque, P. de la Torre, de Palma, F., Desai, A., Di Lalla, N., Di Venere, L., Dirirsa, F. Fana, Fegan, S. J., Franckowiak, A., Fukazawa, Y., Funk, S., Fusco, P., Gargano, F., Gasparrini, D., Giglietto, N., Gill, R., Giordano, F., Giroletti, M., Granot, J., Green, D., Grenier, I. A., Grondin, M. -H., Guiriec, S., Hays, E., Horan, D., Jóhannesson, Guðlaugur, Kocevski, D., Kovac'evic', M., Kuss, M., Larsson, S., Latronico, L., Lemoine-Goumard, M., Li, J., Liodakis, I., Longo, F., Loparco, F., Lovellette, M. N., Lubrano, P., Maldera, S., Malyshev, D., Manfreda, A., Marti-Devesa, G., Mazziotta, M. N., McEnery, J. E., Mereu, I., Meyer, M., Michelson, P. F., Mitthumsiri, W., Mizuno, T., Monzani, M. E., Moretti, E., Morselli, A., Moskalenko, I. V., Negro, M., Nuss, E., Omodei, N., Orienti, M., Orlando, E., Palatiello, M., Paliya, V. S., Paneque, D., Pei, Z., Persic, M., Pesce-Rollins, M., Petrosian, V., Piron, F., Poon, H., Porter, T. A., Principe, G., Racusin, J. L., Raino, S., Rando, R., Rani, B., Razzano, M., Razzaque, S., Reimer, A., Reimer, O., Ryde, F., Parkinson, P. M. Saz, Serini, D., Sgro, C., Siskind, E. J., Spandre, G., Spinelli, P., Tajima, H., Takagi, K., Takahashi, M. N., Tak, D., Thayer, J. B., Thompson, D. J., Torres, D. F., Troja, E., Valverde, J., Van Klaveren, B., Wood, K., Yassine, M., Zaharijas, G., Mailyan, B., Bhat, P. N., Briggs, M. S., Cleveland, W., Giles, M., Goldstein, A., Hui, M., Malacaria, Christian, Preece, R., Roberts, O. J., Veres, P., Wilson-Hodge, C., von Kienlin, A., Cenko, S. B., O'Brien, P., Beardmore, A. P., Lien, A., Osborne, J. P., Tohuvavohu, A., D'Elia, V., D'Ai, A., Perri, M., Gropp, J., Klingler, N., Capalbi, M., Tagliaferri, G., Stamatikos, M., De Pasquale, M., Ajello, M., Arimoto, M., Axelsson, Magnus, Baldini, L., Barbiellini, G., Bastieri, D., Bellazzini, R., Berretta, A., Bissaldi, E., Blandford, R. D., Bonino, R., Bottacini, E., Bregeon, J., Bruel, P., Buehler, R., Burns, E., Buson, S., Cameron, R. A., Caputo, R., Caraveo, P. A., Cavazzuti, E., Chen, S., Chiaro, G., Ciprini, S., Cohen-Tanugi, J., Costantin, D., Cutini, S., D'Ammando, F., DeKlotz, M., Luque, P. de la Torre, de Palma, F., Desai, A., Di Lalla, N., Di Venere, L., Dirirsa, F. Fana, Fegan, S. J., Franckowiak, A., Fukazawa, Y., Funk, S., Fusco, P., Gargano, F., Gasparrini, D., Giglietto, N., Gill, R., Giordano, F., Giroletti, M., Granot, J., Green, D., Grenier, I. A., Grondin, M. -H., Guiriec, S., Hays, E., Horan, D., Jóhannesson, Guðlaugur, Kocevski, D., Kovac'evic', M., Kuss, M., Larsson, S., Latronico, L., Lemoine-Goumard, M., Li, J., Liodakis, I., Longo, F., Loparco, F., Lovellette, M. N., Lubrano, P., Maldera, S., Malyshev, D., Manfreda, A., Marti-Devesa, G., Mazziotta, M. N., McEnery, J. E., Mereu, I., Meyer, M., Michelson, P. F., Mitthumsiri, W., Mizuno, T., Monzani, M. E., Moretti, E., Morselli, A., Moskalenko, I. V., Negro, M., Nuss, E., Omodei, N., Orienti, M., Orlando, E., Palatiello, M., Paliya, V. S., Paneque, D., Pei, Z., Persic, M., Pesce-Rollins, M., Petrosian, V., Piron, F., Poon, H., Porter, T. A., Principe, G., Racusin, J. L., Raino, S., Rando, R., Rani, B., Razzano, M., Razzaque, S., Reimer, A., Reimer, O., Ryde, F., Parkinson, P. M. Saz, Serini, D., Sgro, C., Siskind, E. J., Spandre, G., Spinelli, P., Tajima, H., Takagi, K., Takahashi, M. N., Tak, D., Thayer, J. B., Thompson, D. J., Torres, D. F., Troja, E., Valverde, J., Van Klaveren, B., Wood, K., Yassine, M., Zaharijas, G., Mailyan, B., Bhat, P. N., Briggs, M. S., Cleveland, W., Giles, M., Goldstein, A., Hui, M., Malacaria, Christian, Preece, R., Roberts, O. J., Veres, P., Wilson-Hodge, C., von Kienlin, A., Cenko, S. B., O'Brien, P., Beardmore, A. P., Lien, A., Osborne, J. P., Tohuvavohu, A., D'Elia, V., D'Ai, A., Perri, M., Gropp, J., Klingler, N., Capalbi, M., Tagliaferri, G., Stamatikos, M., and De Pasquale, M.
- Abstract
We report on the observations of gamma-ray burst (GRB) 190114C by the Fermi Gamma -ray Space Telescope and the Neil Gehrels Swift Observatory. The prompt gamma-ray emission was detected by the Fermi GRB Monitor (GBM), the Fermi Large Area Telescope (LAT), and the Swift Burst Alert Telescope (BAT) and the long-lived afterglow emission was subsequently observed by the GBM, LAT, Swift X-ray Telescope (XRT), and Swift UV Optical Telescope. The early -time observations reveal multiple emission components that evolve independently, with a delayed power-law component that exhibits significant spectral attenuation above 40 MeV in the first few seconds of the burst. This power-law component transitions to a harder spectrum that is consistent with the afterglow emission observed by the XRT at later times. This afterglow component is clearly identifiable in the GBM and BAT light curves as a slowly fading emission component on which the rest of the prompt emission is superimposed. As a result, we are able to observe the transition from internal-shock- to external-shock-dominated emission. We find that the temporal and spectral evolution of the broadband afterglow emission can be well modeled as synchrotron emission from a forward shock propagating into a wind -like circumstellar environment. We estimate the initial bulk Lorentz factor using the observed high-energy spectral cutoff. Considering the onset of the afterglow component, we constrain the deceleration radius at which this forward shock begins to radiate in order to estimate the maximum synchrotron energy as a function of time. We find that even in the LAT energy range, there exist high-energy photons that are in tension with the theoretical maximum energy that can be achieved through synchrotron emission from a shock. These violations of the maximum synchrotron energy are further compounded by the detection of very high-energy (VHE) emission above 300 GeV by MAGIC concurrent with our observations. We conclude that the
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- 2020
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115. ON THE 2014-15 NEUTRINO EXCESS FROM TXS 0506+056
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M Petropoulou, K Murase, M Santander, A Tohuvavohu, S Buson, G Vasilopoulos, T Kawamuro, Y Ueda, H Negoro, D Fox, and N Kawai
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- 2019
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116. Fermi and Swift Observations of GRB 190114C: Tracing the Evolution of High-energy Emission from Prompt to Afterglow
- Author
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Ajello, M., primary, Arimoto, M., additional, Axelsson, M., additional, Baldini, L., additional, Barbiellini, G., additional, Bastieri, D., additional, Bellazzini, R., additional, Berretta, A., additional, Bissaldi, E., additional, Blandford, R. D., additional, Bonino, R., additional, Bottacini, E., additional, Bregeon, J., additional, Bruel, P., additional, Buehler, R., additional, Burns, E., additional, Buson, S., additional, Cameron, R. A., additional, Caputo, R., additional, Caraveo, P. A., additional, Cavazzuti, E., additional, Chen, S., additional, Chiaro, G., additional, Ciprini, S., additional, Cohen-Tanugi, J., additional, Costantin, D., additional, Cutini, S., additional, D’Ammando, F., additional, DeKlotz, M., additional, Torre Luque, P. de la, additional, Palma, F. de, additional, Desai, A., additional, Lalla, N. Di, additional, Venere, L. Di, additional, Fana Dirirsa, F., additional, Fegan, S. J., additional, Franckowiak, A., additional, Fukazawa, Y., additional, Funk, S., additional, Fusco, P., additional, Gargano, F., additional, Gasparrini, D., additional, Giglietto, N., additional, Gill, R., additional, Giordano, F., additional, Giroletti, M., additional, Granot, J., additional, Green, D., additional, Grenier, I. A., additional, Grondin, M.-H., additional, Guiriec, S., additional, Hays, E., additional, Horan, D., additional, Jóhannesson, G., additional, Kocevski, D., additional, Kovac’evic’, M., additional, Kuss, M., additional, Larsson, S., additional, Latronico, L., additional, Lemoine-Goumard, M., additional, Li, J., additional, Liodakis, I., additional, Longo, F., additional, Loparco, F., additional, Lovellette, M. N., additional, Lubrano, P., additional, Maldera, S., additional, Malyshev, D., additional, Manfreda, A., additional, Martí-Devesa, G., additional, Mazziotta, M. N., additional, McEnery, J. E., additional, Mereu, I., additional, Meyer, M., additional, Michelson, P. F., additional, Mitthumsiri, W., additional, Mizuno, T., additional, Monzani, M. E., additional, Moretti, E., additional, Morselli, A., additional, Moskalenko, I. V., additional, Negro, M., additional, Nuss, E., additional, Omodei, N., additional, Orienti, M., additional, Orlando, E., additional, Palatiello, M., additional, Paliya, V. S., additional, Paneque, D., additional, Pei, Z., additional, Persic, M., additional, Pesce-Rollins, M., additional, Petrosian, V., additional, Piron, F., additional, Poon, H., additional, Porter, T. A., additional, Principe, G., additional, Racusin, J. L., additional, Rainò, S., additional, Rando, R., additional, Rani, B., additional, Razzano, M., additional, Razzaque, S., additional, Reimer, A., additional, Reimer, O., additional, Ryde, F., additional, Saz Parkinson, P. M., additional, Serini, D., additional, Sgrò, C., additional, Siskind, E. J., additional, Spandre, G., additional, Spinelli, P., additional, Tajima, H., additional, Takagi, K., additional, Takahashi, M. N., additional, Tak, D., additional, Thayer, J. B., additional, Thompson, D. J., additional, Torres, D. F., additional, Troja, E., additional, Valverde, J., additional, Klaveren, B. Van, additional, Wood, K., additional, Yassine, M., additional, Zaharijas, G., additional, Mailyan, B., additional, Bhat, P. N., additional, Briggs, M. S., additional, Cleveland, W., additional, Giles, M., additional, Goldstein, A., additional, Hui, M., additional, Malacaria, Christian, additional, Preece, R., additional, Roberts, O. J., additional, Veres, P., additional, Wilson-Hodge, C., additional, Kienlin, A. von, additional, Cenko, S. B., additional, O’Brien, P., additional, Beardmore, A. P., additional, Lien, A., additional, Osborne, J. P., additional, Tohuvavohu, A., additional, D’Elia, V., additional, D’Aì, A., additional, Perri, M., additional, Gropp, J., additional, Klingler, N., additional, Capalbi, M., additional, Tagliaferri, G., additional, Stamatikos, M., additional, and De Pasquale, M., additional
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- 2020
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117. A Multimessenger Picture of the Flaring Blazar TXS 0506+056: implications for High-Energy Neutrino Emission and Cosmic Ray Acceleration
- Author
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J. A. Kennea, Apostolos Mastichiadis, Kohta Murase, J. P. Osborne, Phil Evans, A. Tohuvavohu, J. J. DeLaunay, Frank Marshall, Sylvain Chaty, Marcos Santander, Derek B. Fox, C. F. Turley, Azadeh Keivani, Stavros Dimitrakoudis, Maria Petropoulou, S. B. Cenko, Alexis Coleiro, 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), AstroParticule et Cosmologie (APC (UMR_7164)), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Université de Paris (UP), 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), Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Astrophysique Interprétation Modélisation (AIM (UMR7158 / UMR_E_9005 / UM_112)), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Observatoire de Paris, and PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)
- Subjects
Astrophysics::High Energy Astrophysical Phenomena ,Hadron ,galaxies: active ,FOS: Physical sciences ,Cosmic ray ,Astrophysics ,Astrophysics::Cosmology and Extragalactic Astrophysics ,blazar: emission ,7. Clean energy ,01 natural sciences ,GLAST ,IceCube ,emission: model ,X-ray ,particle: acceleration ,neutrino: production ,cascade: electromagnetic ,Acceleration ,neutrino: energy ,0103 physical sciences ,gamma rays: galaxies ,cosmic radiation: UHE ,cosmic radiation: acceleration ,Blazar ,010303 astronomy & astrophysics ,BL Lacertae objects: individual ,Physics ,High Energy Astrophysical Phenomena (astro-ph.HE) ,COSMIC cancer database ,hybrid ,010308 nuclear & particles physics ,hadronic component ,neutrinos ,Astronomy and Astrophysics ,BL Lacertae objects: general ,radiation mechanisms: non-thermal ,Particle acceleration ,messenger ,observatory ,monitoring ,Compton scattering: inverse ,13. Climate action ,Space and Planetary Science ,gamma ray ,High Energy Physics::Experiment ,Neutrino ,[PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph] ,Astrophysics - High Energy Astrophysical Phenomena ,Fermi Gamma-ray Space Telescope - Abstract
Detection of the IceCube-170922A neutrino coincident with the flaring blazar TXS 0506+056, the first and only 3-sigma high-energy neutrino source association to date, offers a potential breakthrough in our understanding of high-energy cosmic particles and blazar physics. We present a comprehensive analysis of TXS 0506+056 during its flaring state, using newly collected Swift, NuSTAR, and X-shooter data with Fermi observations and numerical models to constrain the blazar's particle acceleration processes and multimessenger (electromagnetic and high-energy neutrino) emissions. Accounting properly for electromagnetic cascades in the emission region, we find a physically-consistent picture only within a hybrid leptonic scenario, with gamma-rays produced by external inverse-Compton processes and high-energy neutrinos via a radiatively-subdominant hadronic component. We derive robust constraints on the blazar's neutrino and cosmic-ray emissions and demonstrate that, because of cascade effects, the 0.1-100keV emissions of TXS 0506+056 serve as a better probe of its hadronic acceleration and high-energy neutrino production processes than its GeV-TeV emissions. If the IceCube neutrino association holds, physical conditions in the TXS 0506+056 jet must be close to optimal for high-energy neutrino production, and are not favorable for ultra-high-energy cosmic-ray acceleration. Alternatively, the challenges we identify in generating a significant rate of IceCube neutrino detections from TXS 0506+056 may disfavor single-zone models. In concert with continued operations of the high-energy neutrino observatories, we advocate regular X-ray monitoring of TXS 0506+056 and other blazars in order to test single-zone blazar emission models, clarify the nature and extent of their hadronic acceleration processes, and carry out the most sensitive possible search for additional multimessenger sources., 23 pages, 6 figures, 9 tables, submitted to ApJ
- Published
- 2018
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118. Swift-XRT Follow-up of Gravitational-wave Triggers in the Second Advanced LIGO/Virgo Observing Run
- Author
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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
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- 2019
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119. Observation of inverse Compton emission from a long γ-ray burst
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Acciari, V. A., Ansoldi, S., Antonelli, L. A., Engels, A. Arbet, Baack, D., Babić, A., Banerjee, B., Barres de Almeida, U., Barrio, J. A., González, J. Becerra, Bednarek, W., Bellizzi, L., Bernardini, E., Berti, A., Besenrieder, J., Bhattacharyya, W., Bigongiari, C., Biland, A., Blanch, O., Bonnoli, G., Bošnjak, Ž., Busetto, G., Carosi, R., Ceribella, G., Chai, Y., Chilingaryan, A., Cikota, S., Colak, S. M., Colin, U., Colombo, E., Contreras, J. L., Cortina, J., Covino, S., D’Elia, V., Da Vela, P., Dazzi, F., De Angelis, A., De Lotto, B., Delfino, M., Delgado, J., Depaoli, D., Di Pierro, F., Di Venere, L., Espiñeira, E. Do Souto, Prester, D. Dominis, Donini, A., Dorner, D., Doro, M., Elsaesser, D., Ramazani, V. Fallah, Fattorini, A., Ferrara, G., Fidalgo, D., Foffano, L., Fonseca, M. V., Font, L., Fruck, C., Fukami, S., López, R. J. García, Garczarczyk, M., Gasparyan, S., Gaug, M., Giglietto, N., Giordano, F., Godinović, N., Green, D., Guberman, D., Hadasch, D., Hahn, A., Herrera, J., Hoang, J., Hrupec, D., Hütten, M., Inada, T., Inoue, S., Ishio, K., Iwamura, Y., Jouvin, L., Kerszberg, D., Kubo, H., Kushida, J., Lamastra, A., Lelas, D., Leone, F., Lindfors, E., Lombardi, S., Longo, F., López, M., López-Coto, R., López-Oramas, A., Loporchio, S., de Oliveira Fraga, B. Machado, Maggio, C., Majumdar, P., Makariev, M., Mallamaci, M., Maneva, G., Manganaro, M., Mannheim, K., Maraschi, L., Mariotti, M., Martínez, M., Mazin, D., Mićanović, S., Miceli, D., Minev, M., Miranda, J. M., Mirzoyan, R., Molina, E., Moralejo, A., Morcuende, D., Moreno, V., Moretti, E., Munar-Adrover, P., Neustroev, V., Nigro, C., Nilsson, K., Ninci, D., Nishijima, K., Noda, K., Nogués, L., Nozaki, S., Paiano, S., Palatiello, M., Paneque, D., Paoletti, R., Paredes, J. M., Peñil, P., Peresano, M., Persic, M., Moroni, P. G. Prada, Prandini, E., Puljak, I., Rhode, W., Ribó, M., Rico, J., Righi, C., Rugliancich, A., Saha, L., Sahakyan, N., Saito, T., Sakurai, S., Satalecka, K., Schmidt, K., Schweizer, T., Sitarek, J., Šnidarić, I., Sobczynska, D., Somero, A., Stamerra, A., Strom, D., Strzys, M., Suda, Y., Surić, T., Takahashi, M., Tavecchio, F., Temnikov, P., Terzić, T., Teshima, M., Torres-Albà, N., Tosti, L., Vagelli, V., van Scherpenberg, J., Vanzo, G., Acosta, M. Vazquez, Vigorito, C. F., Vitale, V., Vovk, I., Will, M., Zarić, D., Nava, L., Veres, P., Bhat, P. N., Briggs, M. S., Cleveland, W. H., Hamburg, R., Hui, C. M., Mailyan, B., Preece, R. D., Roberts, O. J., von Kienlin, A., Wilson-Hodge, C. A., Kocevski, D., Arimoto, M., Tak, D., Asano, K., Axelsson, M., Barbiellini, G., Bissaldi, E., Dirirsa, F. Fana, Gill, R., Granot, J., McEnery, J., Omodei, N., Razzaque, S., Piron, F., Racusin, J. L., Thompson, D. J., Campana, S., Bernardini, M. G., Kuin, N. P. M., Siegel, M. H., Cenko, S. B., O’Brien, P., Capalbi, M., Daì, A., De Pasquale, M., Gropp, J., Klingler, N., Osborne, J. P., Perri, M., Starling, R. L. C., Tagliaferri, G., Tohuvavohu, A., Ursi, A., Tavani, M., Cardillo, M., Casentini, C., Piano, G., Evangelista, Y., Verrecchia, F., Pittori, C., Lucarelli, F., Bulgarelli, A., Parmiggiani, N., Anderson, G. E., Anderson, J. P., Bernardi, G., Bolmer, J., Caballero-García, M. D., Carrasco, I. M., Castellón, A., Segura, N. Castro, Castro-Tirado, A. J., Cherukuri, S. V., Cockeram, A. M., D’Avanzo, P., Di Dato, A., Diretse, R., Fender, R. P., Fernández-García, E., Fynbo, J. P. U., Fruchter, A. S., Greiner, J., Gromadzki, M., Heintz, K. E., Heywood, I., van der Horst, A. J., Hu, Y.-D., Inserra, C., Izzo, L., Jaiswal, V., Jakobsson, P., Japelj, J., Kankare, E., Kann, D. A., Kouveliotou, C., Klose, S., Levan, A. J., Li, X. Y., Lotti, S., Maguire, K., Malesani, D. B., Manulis, I., Marongiu, M., Martin, S., Melandri, A., Michałowski, M. J., Miller-Jones, J. C. A., Misra, K., Moin, A., Mooley, K. P., Nasri, S., Nicholl, M., Noschese, A., Novara, G., Pandey, S. B., Peretti, E., del Pulgar, C. J. Pérez, Pérez-Torres, M. A., Perley, D. A., Piro, L., Ragosta, F., Resmi, L., Ricci, R., Rossi, A., Sánchez-Ramírez, R., Selsing, J., Schulze, S., Smartt, S. J., Smith, I. A., Sokolov, V. V., Stevens, J., Tanvir, N. R., Thöne, C. C., Tiengo, A., Tremou, E., Troja, E., de Ugarte Postigo, A., Collaboration, MAGIC, Acciari, V. A., Ansoldi, S., Antonelli, L. A., Engels, A. Arbet, Baack, D., Babić, A., Banerjee, B., Barres de Almeida, U., Barrio, J. A., González, J. Becerra, Bednarek, W., Bellizzi, L., Bernardini, E., Berti, A., Besenrieder, J., Bhattacharyya, W., Bigongiari, C., Biland, A., Blanch, O., Bonnoli, G., Bošnjak, Ž., Busetto, G., Carosi, R., Ceribella, G., Chai, Y., Chilingaryan, A., Cikota, S., Colak, S. M., Colin, U., Colombo, E., Contreras, J. L., Cortina, J., Covino, S., D’Elia, V., Da Vela, P., Dazzi, F., De Angelis, A., De Lotto, B., Delfino, M., Delgado, J., Depaoli, D., Di Pierro, F., Di Venere, L., Espiñeira, E. Do Souto, Prester, D. Dominis, Donini, A., Dorner, D., Doro, M., Elsaesser, D., Ramazani, V. Fallah, Fattorini, A., Ferrara, G., Fidalgo, D., Foffano, L., Fonseca, M. V., Font, L., Fruck, C., Fukami, S., López, R. J. García, Garczarczyk, M., Gasparyan, S., Gaug, M., Giglietto, N., Giordano, F., Godinović, N., Green, D., Guberman, D., Hadasch, D., Hahn, A., Herrera, J., Hoang, J., Hrupec, D., Hütten, M., Inada, T., Inoue, S., Ishio, K., Iwamura, Y., Jouvin, L., Kerszberg, D., Kubo, H., Kushida, J., Lamastra, A., Lelas, D., Leone, F., Lindfors, E., Lombardi, S., Longo, F., López, M., López-Coto, R., López-Oramas, A., Loporchio, S., de Oliveira Fraga, B. Machado, Maggio, C., Majumdar, P., Makariev, M., Mallamaci, M., Maneva, G., Manganaro, M., Mannheim, K., Maraschi, L., Mariotti, M., Martínez, M., Mazin, D., Mićanović, S., Miceli, D., Minev, M., Miranda, J. M., Mirzoyan, R., Molina, E., Moralejo, A., Morcuende, D., Moreno, V., Moretti, E., Munar-Adrover, P., Neustroev, V., Nigro, C., Nilsson, K., Ninci, D., Nishijima, K., Noda, K., Nogués, L., Nozaki, S., Paiano, S., Palatiello, M., Paneque, D., Paoletti, R., Paredes, J. M., Peñil, P., Peresano, M., Persic, M., Moroni, P. G. Prada, Prandini, E., Puljak, I., Rhode, W., Ribó, M., Rico, J., Righi, C., Rugliancich, A., Saha, L., Sahakyan, N., Saito, T., Sakurai, S., Satalecka, K., Schmidt, K., Schweizer, T., Sitarek, J., Šnidarić, I., Sobczynska, D., Somero, A., Stamerra, A., Strom, D., Strzys, M., Suda, Y., Surić, T., Takahashi, M., Tavecchio, F., Temnikov, P., Terzić, T., Teshima, M., Torres-Albà, N., Tosti, L., Vagelli, V., van Scherpenberg, J., Vanzo, G., Acosta, M. Vazquez, Vigorito, C. F., Vitale, V., Vovk, I., Will, M., Zarić, D., Nava, L., Veres, P., Bhat, P. N., Briggs, M. S., Cleveland, W. H., Hamburg, R., Hui, C. M., Mailyan, B., Preece, R. D., Roberts, O. J., von Kienlin, A., Wilson-Hodge, C. A., Kocevski, D., Arimoto, M., Tak, D., Asano, K., Axelsson, M., Barbiellini, G., Bissaldi, E., Dirirsa, F. Fana, Gill, R., Granot, J., McEnery, J., Omodei, N., Razzaque, S., Piron, F., Racusin, J. L., Thompson, D. J., Campana, S., Bernardini, M. G., Kuin, N. P. M., Siegel, M. H., Cenko, S. B., O’Brien, P., Capalbi, M., Daì, A., De Pasquale, M., Gropp, J., Klingler, N., Osborne, J. P., Perri, M., Starling, R. L. C., Tagliaferri, G., Tohuvavohu, A., Ursi, A., Tavani, M., Cardillo, M., Casentini, C., Piano, G., Evangelista, Y., Verrecchia, F., Pittori, C., Lucarelli, F., Bulgarelli, A., Parmiggiani, N., Anderson, G. E., Anderson, J. P., Bernardi, G., Bolmer, J., Caballero-García, M. D., Carrasco, I. M., Castellón, A., Segura, N. Castro, Castro-Tirado, A. J., Cherukuri, S. V., Cockeram, A. M., D’Avanzo, P., Di Dato, A., Diretse, R., Fender, R. P., Fernández-García, E., Fynbo, J. P. U., Fruchter, A. S., Greiner, J., Gromadzki, M., Heintz, K. E., Heywood, I., van der Horst, A. J., Hu, Y.-D., Inserra, C., Izzo, L., Jaiswal, V., Jakobsson, P., Japelj, J., Kankare, E., Kann, D. A., Kouveliotou, C., Klose, S., Levan, A. J., Li, X. Y., Lotti, S., Maguire, K., Malesani, D. B., Manulis, I., Marongiu, M., Martin, S., Melandri, A., Michałowski, M. J., Miller-Jones, J. C. A., Misra, K., Moin, A., Mooley, K. P., Nasri, S., Nicholl, M., Noschese, A., Novara, G., Pandey, S. B., Peretti, E., del Pulgar, C. J. Pérez, Pérez-Torres, M. A., Perley, D. A., Piro, L., Ragosta, F., Resmi, L., Ricci, R., Rossi, A., Sánchez-Ramírez, R., Selsing, J., Schulze, S., Smartt, S. J., Smith, I. A., Sokolov, V. V., Stevens, J., Tanvir, N. R., Thöne, C. C., Tiengo, A., Tremou, E., Troja, E., de Ugarte Postigo, A., and Collaboration, MAGIC
- Abstract
Long-duration γ-ray bursts (GRBs) originate from ultra-relativistic jets launched from the collapsing cores of dying massive stars. They are characterized by an initial phase of bright and highly variable radiation in the kiloelectronvolt-to-megaelectronvolt band, which is probably produced within the jet and lasts from milliseconds to minutes, known as the prompt emission1,2. Subsequently, the interaction of the jet with the surrounding medium generates shock waves that are responsible for the afterglow emission, which lasts from days to months and occurs over a broad energy range from the radio to the gigaelectronvolt bands1,2,3,4,5,6. The afterglow emission is generally well explained as synchrotron radiation emitted by electrons accelerated by the external shock7,8,9. Recently, intense long-lasting emission between 0.2 and 1 teraelectronvolts was observed from GRB 190114C10,11. Here we report multi-frequency observations of GRB 190114C, and study the evolution in time of the GRB emission across 17 orders of magnitude in energy, from 5 × 10−6 to 1012 electronvolts. We find that the broadband spectral energy distribution is double-peaked, with the teraelectronvolt emission constituting a distinct spectral component with power comparable to the synchrotron component. This component is associated with the afterglow and is satisfactorily explained by inverse Compton up-scattering of synchrotron photons by high-energy electrons. We find that the conditions required to account for the observed teraelectronvolt component are typical for GRBs, supporting the possibility that inverse Compton emission is commonly produced in GRBs.
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- 2019
120. A Multimessenger Picture of the Flaring Blazar TXS 0506+056: Implications for High-energy Neutrino Emission and Cosmic-Ray Acceleration
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Keivani, A. Murase, K. Petropoulou, M. Fox, D.B. Cenko, S.B. Chaty, S. Coleiro, A. Delaunay, J.J. Dimitrakoudis, S. Evans, P.A. Kennea, J.A. Marshall, F.E. Mastichiadis, A. Osborne, J.P. Santander, M. Tohuvavohu, A. Turley, C.F.
- Subjects
Astrophysics::High Energy Astrophysical Phenomena ,High Energy Physics::Experiment ,Astrophysics::Cosmology and Extragalactic Astrophysics - Abstract
Detection of the IceCube-170922A neutrino coincident with the flaring blazar TXS 0506+056, the first and only ∼3σ high-energy neutrino source association to date, offers a potential breakthrough in our understanding of high-energy cosmic particles and blazar physics. We present a comprehensive analysis of TXS 0506+056 during its flaring state, using newly collected Swift, NuSTAR, and X-shooter data with Fermi observations and numerical models to constrain the blazar's particle acceleration processes and multimessenger (electromagnetic (EM) and high-energy neutrino) emissions. Accounting properly for EM cascades in the emission region, we find a physically consistent picture only within a hybrid leptonic scenario, with γ-rays produced by external inverse-Compton processes and high-energy neutrinos via a radiatively subdominant hadronic component. We derive robust constraints on the blazar's neutrino and cosmic-ray emissions and demonstrate that, because of cascade effects, the 0.1-100 keV emissions of TXS 0506+056 serve as a better probe of its hadronic acceleration and high-energy neutrino production processes than its GeV-TeV emissions. If the IceCube neutrino association holds, physical conditions in the TXS 0506+056 jet must be close to optimal for high-energy neutrino production, and are not favorable for ultrahigh-energy cosmic-ray acceleration. Alternatively, the challenges we identify in generating a significant rate of IceCube neutrino detections from TXS 0506+056 may disfavor single-zone models, in which γ-rays and high-energy neutrinos are produced in a single emission region. In concert with continued operations of the high-energy neutrino observatories, we advocate regular X-ray monitoring of TXS 0506+056 and other blazars in order to test single-zone blazar emission models, clarify the nature and extent of their hadronic acceleration processes, and carry out the most sensitive possible search for additional multimessenger sources. © 2018. The American Astronomical Society. All rights reserved..
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- 2018
121. GRB171205A/SN2017iuk: A local low-luminosity gamma-ray burst
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A. Tsvetkova, Antonino D'Ai, A. Tohuvavohu, Dmitry S. Svinkin, M. de Pasquale, Valerio D'Elia, P. T. O'Brien, S. W. K. Emery, J. P. Osborne, A. Melandri, S. R. Oates, Peter J. Brown, D. D. Frederiks, Sergio Campana, David N. Burrows, S. B. Cenko, R. L. C. Starling, M. H. Siegel, A. Y. Lien, A. A. Breeveld, G. Tagliaferri, K. L. Page, ITA, USA, GBR, and TUR
- Subjects
Physics ,High Energy Astrophysical Phenomena (astro-ph.HE) ,media_common.quotation_subject ,Astrophysics::High Energy Astrophysical Phenomena ,FOS: Physical sciences ,Astronomy and Astrophysics ,Context (language use) ,Astrophysics ,Astrophysics::Cosmology and Extragalactic Astrophysics ,Light curve ,01 natural sciences ,Universe ,Redshift ,Galaxy ,Luminosity ,Supernova ,Space and Planetary Science ,0103 physical sciences ,Astrophysics - High Energy Astrophysical Phenomena ,010306 general physics ,Gamma-ray burst ,010303 astronomy & astrophysics ,media_common - Abstract
Gamma-ray bursts (GRBs) occurring in the local Universe constitute an interesting sub-class of the GRB family, since their luminosity is on average lower than that of their cosmological analogs. We aim to contribute to the study of local bursts by reporting the case of GRB 171205A. This source was discovered by Swift Burst Alert Telescope (BAT) on 2017, December 5 and soon associated with a low redshift host galaxy (z=0.037), and an emerging SN (SN 2017iuk). We analyzed the full Swift, dataset, comprising the UV-Optical Telescope (UVOT), X-ray Telescope (XRT) and BAT data. In addition, we employed the Konus-Wind high energy data as a valuable extension at gamma-ray energies. The photometric SN signature is clearly visible in the UVOT u, b and v filters. The maximum emission is reached at ~ 13 (rest frame) days, and the whole bump resembles that of SN 2006aj, but lower in magnitude and with a shift in time of +2 d. A prebump in the v-band is also clearly visible, and this is the first time that such a feature is not observed achromatically in GRB-SNe. Its physical origin cannot be easily explained. The X-ray spectrum shows an intrinsic Hydrogen column density N_H,int = 7.4(+4.1 -3.6) X 10^20 / cm^2$, which is at the low end of the N_H,int, even considering just low redshift GRBs. The spectrum also features a thermal component, which is quite common in GRBs associated with SNe, but whose origin is still a matter of debate. Finally, the isotropic energy in the gamma-ray band, E_iso = 2.18(+0.63 -0.50) X 10^49 erg, is lower than those of cosmological GRBs. Combining this value with the peak energy in the same band, E_p=125(+141 -37) keV, implies that GRB 171205A is an outlier of the Amati relation, as are some other low redshift GRBs, and its emission mechanism should be different from that of canonical, farther away GRBs., Comment: 13 pages, 10 figures, A&A in press
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- 2018
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122. Swift spectra of AT2018cow: a white dwarf tidal disruption event?
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Kuin, N Paul M, primary, Wu, Kinwah, additional, Oates, Samantha, additional, Lien, Amy, additional, Emery, Sam, additional, Kennea, Jamie A, additional, de Pasquale, Massimiliano, additional, Han, Qin, additional, Brown, Peter J, additional, Tohuvavohu, Aaron, additional, Breeveld, Alice, additional, Burrows, David N, additional, Cenko, S Bradley, additional, Campana, Sergio, additional, Levan, Andrew, additional, Markwardt, Craig, additional, Osborne, Julian P, additional, Page, Mat J, additional, Page, Kim L, additional, Sbarufatti, Boris, additional, Siegel, Michael, additional, and Troja, Eleonora, additional
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- 2019
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123. GRB 171205A/SN 2017iuk: A local low-luminosity gamma-ray burst
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D’Elia, V., primary, Campana, S., additional, D’Aì, A., additional, De Pasquale, M., additional, Emery, S. W. K., additional, Frederiks, D. D., additional, Lien, A., additional, Melandri, A., additional, Page, K. L., additional, Starling, R. L. C., additional, Burrows, D. N., additional, Breeveld, A. A., additional, Oates, S. R., additional, O’Brien, P. T., additional, Osborne, J. P., additional, Siegel, M. H., additional, Tagliaferri, G., additional, Brown, P. J., additional, Cenko, S. B., additional, Svinkin, D. S., additional, Tohuvavohu, A., additional, and Tsvetkova, A. E., additional
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- 2018
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124. Improving science yield for NASA Swift with automated planning technologies
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Tohuvavohu, A, primary
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- 2018
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125. A Multimessenger Picture of the Flaring Blazar TXS 0506+056: Implications for High-energy Neutrino Emission and Cosmic-Ray Acceleration
- Author
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Keivani, A., primary, Murase, K., additional, Petropoulou, M., additional, Fox, D. B., additional, Cenko, S. B., additional, Chaty, S., additional, Coleiro, A., additional, DeLaunay, J. J., additional, Dimitrakoudis, S., additional, Evans, P. A., additional, Kennea, J. A., additional, Marshall, F. E., additional, Mastichiadis, A., additional, Osborne, J. P., additional, Santander, M., additional, Tohuvavohu, A., additional, and Turley, C. F., additional
- Published
- 2018
- Full Text
- View/download PDF
126. Multimessenger observations of a flaring blazar coincident with high-energy neutrino IceCube-170922A
- Author
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Aartsen, M. G., Ackermann, M., Adams, J., Aguilar, J. A., Ahlers, M., Ahrens, M., Al Samarai, I., Altmann, D., Andeen, K., Anderson, T., Ansseau, I., Anton, G., Arguelles, C., Auffenberg, J., Axani, S., Bagherpour, H., Bai, X., Barron, J. P., Barwick, S. W., Baum, V., Bay, R., Beatty, J. J., Tjus, J. Becker, Becker, K. -H, BenZvi, S., Berley, D., Bernardini, E., Besson, D. Z., Binder, G., Bindig, D., Blaufuss, E., Blot, S., Bohm, C., Borner, M., Bos, F., Boser, S., Botner, Olga, Bourbeau, E., Bourbeau, J., Bradascio, F., Braun, J., Brenzke, M., Bretz, H. -P, Bron, S., Brostean-Kaiser, J., Burgman, Alexander, Busse, R. S., Carver, T., Cheung, E., Chirkin, D., Christov, A., Clark, K., Classen, L., Coenders, S., Collin, G. H., Conrad, J. M., Coppin, P., Correa, P., Cowen, D. F., Cross, R., Dave, P., Day, M., de Andre, J. P. A. M., De Clercq, C., DeLaunay, J. J., Dembinski, H., De Ridder, S., Desiati, P., de Vries, K. D., de Wasseige, G., de With, M., DeYoung, T., Diaz-Velez, J. C., di Lorenzo, V., Dujmovic, H., Dumm, J. P., Dunkman, M., Dvorak, E., Eberhardt, B., Ehrhardt, T., Eichmann, B., Eller, P., Evenson, P. A., Fahey, S., Fazely, A. R., Felde, J., Filimonov, K., Finley, C., Flis, S., Franckowiak, A., Friedman, E., Fritz, A., Gaisser, T. K., Gallagher, J., Gerhardt, L., Ghorbani, K., Glauch, T., Glusenkamp, T., Goldschmidt, A., Gonzalez, J. G., Grant, D., Griffith, Z., Haack, C., Hallgren, Allan, Halzen, F., Hanson, K., Hebecker, D., Heereman, D., Helbing, K., Hellauer, R., Hickford, S., Hignight, J., Hill, G. C., Hoffman, K. D., Hoffmann, R., Hoinka, T., Hokanson-Fasig, B., Hoshina, K., Huang, F., Huber, M., Hultqvist, K., Hunnefeld, M., Hussain, R., In, S., Iovine, N., Ishihara, A., Jacobi, E., Japaridze, G. S., Jeong, M., Jero, K., Jones, B. J. P., Kalaczynski, P., Kang, W., Kappes, A., Kappesser, D., Karg, T., Karle, A., Katz, U., Kauer, M., Keivani, A., Kelley, J. L., Kheirandish, A., Kim, J., Kim, M., Kintscher, T., Kiryluk, J., Kittler, T., Klein, S. R., Koirala, R., Kolanoski, H., Kopke, L., Kopper, C., Kopper, S., Koschinsky, J. P., Koskinen, D. J., Kowalski, M., Krings, K., Kroll, M., Kruckl, G., Kunwar, S., Kurahashi, N., Kuwabara, T., Kyriacou, A., Labare, M., Lanfranchi, J. L., Larson, M. J., Lauber, F., Leonard, K., Lesiak-Bzdak, M., Leuermann, M., Liu, Q. R., Mariscal, C. J. Lozano, Lu, L., Lunemann, J., Luszczak, W., Madsen, J., Maggi, G., Mahn, K. B. M., Mancina, S., Maruyama, R., Mase, K., Maunu, R., Meagher, K., Medici, M., Meier, M., Menne, T., Merino, G., Meures, T., Miarecki, S., Micallef, J., Momente, G., Montaruli, T., Moore, R. W., Morse, R., Moulai, M., Nahnhauer, R., Nakarmi, P., Naumann, U., Neer, G., Niederhausen, H., Nowicki, S. C., Nygren, D. R., Pollmann, A. Obertacke, Olivas, A., O'Murchadha, A., O'Sullivan, E., Palczewski, T., Pandya, H., Pankova, D. V., Peiffer, P., Pepper, J. A., de los Heros, Carlos, Pieloth, D., Pinat, E., Plum, M., Price, P. B., Przybylski, G. T., Raab, C., Radel, L., Rameez, M., Rauch, L., Rawlins, K., Rea, I. C., Reimann, R., Relethford, B., Relich, M., Resconi, E., Rhode, W., Richman, M., Robertson, S., Rongen, M., Rott, C., Ruhe, T., Ryckbosch, D., Rysewyk, D., Safa, I., Salzer, T., Herrera, S. E. Sanchez, Sandrock, A., Sandroos, J., Santander, M., Sarkar, S., Satalecka, K., Schlunder, P., Schmidt, T., Schneider, A., Schoenen, S., Schoneberg, S., Schumacher, L., Sclafani, S., Seckel, D., Seunarine, S., Soedingrekso, J., Soldin, D., Song, M., Spiczak, G. M., Spiering, C., Stachurska, J., Stamatikos, M., Stanev, T., Stasik, A., Stein, R., Stettner, J., Steuer, A., Stezelberger, T., Stokstad, R. G., Stossl, A., Strotjohann, N. L., Stuttard, T., Sullivan, G. W., Sutherland, M., Taboada, I., Tatar, J., Tenholt, F., Ter-Antonyan, S., Terliuk, A., Tilav, S., Toale, P. A., Tobin, M. N., Toennis, C., Toscano, S., Tosi, D., Tselengidou, M., Tung, C. F., Turcati, A., Turley, C. F., Ty, B., Unger, Elisabeth, Usner, M., Vandenbroucke, J., Van Driessche, W., van Eijk, D., van Eijndhoven, N., Vanheule, S., van Santen, J., Vogel, E., Vraeghe, M., Walck, C., Wallace, A., Mallraff, M., Wandler, F. D., Wandkowsky, N., Waza, A., Weaver, C., Weiss, M. J., Wendt, C., Werthebach, J., Westerhoff, S., Whelan, B. J., Whitehorn, N., Wiebe, K., Wiebusch, C. H., Wille, L., Williams, D. R., Wills, L., Wolf, M., Wood, J., Wood, T. R., Woschnagg, K., Xu, D. L., Xu, X. W., Xu, Y., Yanez, J. P., Yodh, G., Yoshida, S., Yuan, T., Abdollahi, S., Ajello, M., Angioni, R., Baldini, L., Ballet, J., Barbiellini, G., Bastieri, D., Bechtol, K., Bellazzini, R., Berenji, B., Bissaldi, E., Blandford, R. D., Bonino, R., Bottacini, E., Bregeon, J., Bruel, P., Buehler, R., Burnett, T. H., Burns, E., Buson, S., Cameron, R. A., Caputo, R., Caraveo, P. A., Cavazzuti, E., Charles, E., Chen, S., Cheung, C. C., Chiang, J., Chiaro, G., Ciprini, S., Cohen-Tanugi, J., Conrad, J., Costantin, D., Cutini, S., D'Ammando, F., de Palma, F., Digel, S. W., Di Lalla, N., Di Mauro, M., Di Venere, L., Dominguez, A., Favuzzi, C., Fukazawa, Y., Funk, S., Fusco, P., Gargano, F., Gasparrini, D., Giglietto, N., Giomi, M., Giommi, P., Giordano, F., Giroletti, M., Glanzman, T., Green, D., Grenier, I. A., Grondin, M. -H, Guiriec, S., Harding, A. K., Hayashida, M., Hays, E., Hewitt, J. W., Horan, D., Johannesson, G., Kadler, M., Kensei, S., Kocevski, D., Krauss, F., Kreter, M., Kuss, M., La Mura, G., Larsson, S., Latronico, L., Lemoine-Goumard, M., Li, J., Longo, F., Loparco, F., Lovellette, M. N., Lubrano, P., Magill, J. D., Maldera, S., Malyshev, D., Manfreda, A., Mazziotta, M. N., McEnery, J. E., Meyer, M., Michelson, P. F., Mizuno, T., Monzani, M. E., Morselli, A., Moskalenko, I. V., Negro, M., Nuss, E., Ojha, R., Omodei, N., Orienti, M., Orlando, E., Palatiello, M., Paliya, V. S., Perkins, J. S., Persic, M., Pesce-Rollins, M., Piron, F., Porter, T. A., Principe, G., Raino, S., Rando, R., Rani, B., Razzano, M., Razzaque, S., Reimer, A., Reimer, O., Renault-Tinacci, N., Ritz, S., Rochester, L. S., Parkinson, P. M. Saz, Sgro, C., Siskind, E. J., Spandre, G., Spinelli, P., Suson, D. J., Tajima, H., Takahashi, M., Tanaka, Y., Thayer, J. B., Thompson, D. J., Tibaldo, L., Torres, D. F., Torresi, E., Tosti, G., Troja, E., Valverde, J., Vianello, G., Vogel, M., Wood, K., Wood, M., Zaharijas, G., Ahnen, M. L., Ansoldi, S., Antonelli, L. A., Arcaro, C., Baack, D., Babic, A., Banerjee, B., Bangale, P., de Almeida, U. Barres, Barrio, J. A., Gonzalez, J. Becerra, Bednarek, W., Berti, A., Bhattacharyya, W., Biland, A., Blanch, O., Bonnoli, G., Carosi, A., Carosi, R., Ceribella, G., Chatterjee, A., Colak, S. M., Colin, P., Colombo, E., Contreras, J. L., Cortina, J., Covino, S., Cumani, P., Da Vela, P., Dazzi, F., De Angelis, A., De Lotto, B., Delfino, M., Delgado, J., Di Pierro, F., Prester, D. . Dominis, Dorner, D., Doro, M., Einecke, S., Elsaesser, D., Ramazani, V. Fallah, Fernandez-Barral, A., Fidalgo, D., Foffano, L., Pfrang, K., Fonseca, M. V., Font, L., Franceschini, A., Fruck, C., Galindo, D., Gallozzi, S., Lopez, R. J. Garcia, Garczarczyk, M., Gaug, M., Giammaria, P., Godinovic, N., Gora, D., Guberman, D., Hadasch, D., Hahn, A., Hassan, T., Herrera, J., Hose, J., Hrupec, D., Inoue, S., Ishio, K., Konno, Y., Kubo, H., Kushida, J., Lelas, D., Lindfors, E., Lombardi, S., Lopez, M., Maggio, C., Majumdar, P., Makariev, M., Maneva, G., Manganaro, M., Mannheim, K., Maraschi, L., Mariotti, M., Martinez, M., Masuda, S., Mazin, D., Minev, M., M, J. M., Mirzoyan, R., Moralejo, A., Moreno, V., Moretti, E., Nagayoshi, T., Neustroev, V., Niedzwiecki, A., Rosillo, M. Nievas, Nigro, C., Nilsson, K., Ninci, D., Nishijima, K., Noda, K., Nogues, L., Paiano, S., Palacio, J., Paneque, D., Paoletti, R., Paredes, J. M., Pedaletti, G., Peresano, M., Moroni, P. G. Prada, Prandini, E., Puljak, I., Garcia, J. Rodriguez, Reichardt, I., Ribo, M., Rico, J., Righi, C., Rugliancich, A., Saito, T., Schweizer, T., Sitarek, J., Snidaric, I., Sobczynska, D., Stamerra, A., Strzys, M., Suric, T., Tavecchio, F., Temnikov, P., Terzic, T., Teshima, M., Torres-Alba, N., Treves, A., Tsujimoto, S., Vanzo, G., Acosta, M. Vazquez, Vovk, I., Ward, J. E., Will, M., Zaric, D., Lucarelli, F., Tavani, M., Piano, G., Donnarumma, I., Pittori, C., Verrecchia, F., Bulgarelli, A., Caraveo, P., Cattaneo, P. W., Colafrancesco, S., Costa, E., Di Cocco, G., Ferrari, A., Gianotti, F., Giuliani, A., Lipari, P., Mereghetti, S., Pacciani, L., Paoletti, F., Parmiggiani, N., Pellizzoni, A., Picozza, P., Pilia, M., Rappoldi, A., Trois, A., Vercellone, S., Vittorini, V., Stanek, K. Z., Kochanek, C. S., Beacom, J. F., Thompson, T. A., Holoien, W. -S, Dong, S., Prieto, J. L., Shappee, B. J., Holmbo, S., Abeysekara, A. U., Albert, A., Alfaro, R., Alvarez, C., Arceo, R., Arteaga-Velazquez, J. C., Rojas, D. Avila, Solares, H. A. Ayala, Becerril, A., Belmont-Moreno, E., Bernal, A., Caballero-Mora, K. S., Capistran, T., Carraminana, A., Casanova, S., Castillo, M., Cotti, U., Cotzomi, J., de Leon, S. Coutino, De Leon, C., De la Fuente, E., Hernandez, R. Diaz, Dichiara, S., Dingus, B. L., DuVernois, M. A., Ellsworth, R. W., Engel, K., Fiorino, D. W., Fleischhack, H., Fraija, N., Garcia-Gonzalez, J. A., Garfias, F., Munoz, A. Gonzalez, Gonzalez, M. M., Goodman, J. A., Hampel-Arias, Z., Harding, J. P., Hernandez, S., Hona, B., Hueyotl-Zahuantitla, F., Hui, C. M., Huntemeyer, P., Iriarte, A., Jardin-Blicq, A., Joshi, V., Kaufmann, S., Kunde, G. J., Lara, A., Lauer, R. J., Lee, W. H., Lennarz, D., Vargas, H. Leon, Linnemann, J. T., Longinotti, A. L., Luis-Raya, G., Luna-Garcia, R., Malone, K., Marinelli, S. S., Martinez, O., Martinez-Castellanos, I., Martinez-Castro, J., Martinez-Huerta, H., Matthews, J. A., Miranda-Romagnoli, P., Moreno, E., Mostafa, M., Nayerhoda, A., Nellen, L., Newbold, M., Nisa, M. U., Noriega-Papaqui, R., Pelayo, R., Pretz, J., Perez-Perez, E. G., Ren, Z., Rho, C. D., Riviere, C., Rosa-Gonzalez, D., Rosenberg, M., Ruiz-Velasco, E., Greus, F. Salesa, Sandoval, A., Schneider, M., Schoorlemmer, H., Sinnis, G., Smith, A. J., Springer, R. W., Surajbali, P., Tibolla, O., Tollefson, K., Torres, I., Villasenor, L., Weisgarber, T., Werner, F., Yapici, T., Gaurang, Y., Zepeda, A., Zhou, H., Alvarez, J. D., Abdalla, H., Anguner, E. O., Armand, C., Backes, M., Becherini, Y., Berge, D., Bottcher, M., Boisson, C., Bolmont, J., Bonnefoy, S., Bordas, P., Brun, F., Buchele, M., Bulik, T., Caroff, S., Cerruti, M., Chakraborty, N., Chandra, S., Chen, A., Davids, I. D., Deil, C., Devin, J., Djannati-Atai, A., Egberts, K., Emery, G., Eschbach, S., Fiasson, A., Fontaine, G., Fussling, M., Gallant, Y. A., Gate, F., Giavitto, G., Glawion, D., Glicenstein, J. F., Gottschall, D., Haupt, M., Henri, G., Hinton, J. A., Hoischen, C., Holch, T. L., Huber, D., Jamrozy, M., Jankowsky, D., Jankowsky, F., Jouvin, L., Jung-Richardt, I., Kerszberg, D., Khelifi, B., King, J., Klepser, S., Kluzniak, W., Komin, Nu., Kraus, M., Lefaucheur, J., Lemiere, A., Lenain, J. -P, Leser, E., Lohse, T., Lopez-Coto, R., Lorentz, M., Lypova, I., Marandon, V., Marti-Devesa, G. Guillem, Maurin, G., Mitchell, A. M. W., Moderski, R., Mohamed, M., Mohrmann, L., Moulin, E., Murach, T., de Naurois, M., Niederwanger, F., Niemiec, J., Oakes, L., O'Brien, P., Ohm, S., Ostrowski, M., Oya, I., Panter, M., Parsons, R. D., Perennes, C., Piel, Q., Pita, S., Poireau, V., Noel, A. Priyana, Prokoph, H., Puhlhofer, G., Quirrenbach, A., Raab, S., Rauth, R., Renaud, M., Rieger, F., Rinchiuso, L., Romoli, C., Rowell, G., Rudak, B., Sanchez, D. A., Sasaki, M., Schlickeiser, R., Schussler, F., Schulz, A., Schwanke, U., Seglar-Arroyo, M., Shafi, N., Simoni, R., Sol, H., Stegmann, C., Steppa, C., Tavernier, T., Taylor, A. M., Tiziani, D., Trichard, C., Tsirou, M., van Eldik, C., van Rensburg, C., van Soelen, B., Veh, J., Vincent, P., Voisin, F., Wagner, S. J., Wagner, R. M., Wierzcholska, A., Zanin, R., Zdziarski, A. A., Zech, A., Ziegler, A., Zorn, J., Zywucka, N., Savchenko, V., Ferrigno, C., Bazzano, A., Diehl, R., Kuulkers, E., Laurent, P., Natalucci, L., Panessa, F., Rodi, J., Ubertini, P., Morokuma, T., Ohta, K., Tanaka, Y. T., Mori, H., Yamanaka, M., Kawabata, K. S., Utsumi, Y., Nakaoka, T., Kawabata, M., Nagashima, H., Yoshida, M., Matsuoka, Y., Itoh, R., Keel, W., Copperwheat, C., Steele, I., Cenko, S. B., Evans, P. A., Fox, D. B., Kennea, J. A., Marshall, F. E., Osborne, J. P., Tohuvavohu, A., Archer, A., Benbow, W., Bird, R., Brill, A., Brose, R., Buchovecky, M., Buckley, J. H., Bugaev, V., Christiansen, J. L., Connolly, M. P., Cui, W., Daniel, M. K., Errando, M., Falcone, A., Feng, Q., Finley, J. P., Fortson, L., Furniss, A., Gueta, O., Hutten, M., Hervet, O., Hughes, G., Humensky, T. B., Johnson, C. A., Kaaret, P., Kar, P., Kelley-Hoskins, N., Kertzman, M., Kieda, D., Krause, M., Krennrich, F., Kumar, S., Lang, M. J., Lin, T. T. Y., Maier, G., McArthur, S., Moriarty, P., Mukherjee, R., Nieto, D., O'Brien, S., Ong, R. A., Otte, A. N., Park, N., Petrashyk, A., Pohl, M., Popkow, A., Pueschel, E., Quinn, J., Ragan, K., Reynolds, P. T., Richards, G. T., Roache, E., Rulten, C., Sadeh, I., Scott, S. S., Sembroski, G. H., Shahinyan, K., Sushch, I., Trepanier, S., Tyler, J., Vassiliev, V. V., Wakely, S. P., Weinstein, A., Wells, R. M., Wilcox, P., Wilhelm, A., Williams, D. A., Zitzer, B., Tetarenko, A. J., Kimball, A. E., Miller-Jones, J. C. A., Sivakoff, G. R., Aartsen, M. G., Ackermann, M., Adams, J., Aguilar, J. A., Ahlers, M., Ahrens, M., Al Samarai, I., Altmann, D., Andeen, K., Anderson, T., Ansseau, I., Anton, G., Arguelles, C., Auffenberg, J., Axani, S., Bagherpour, H., Bai, X., Barron, J. P., Barwick, S. W., Baum, V., Bay, R., Beatty, J. J., Tjus, J. Becker, Becker, K. -H, BenZvi, S., Berley, D., Bernardini, E., Besson, D. Z., Binder, G., Bindig, D., Blaufuss, E., Blot, S., Bohm, C., Borner, M., Bos, F., Boser, S., Botner, Olga, Bourbeau, E., Bourbeau, J., Bradascio, F., Braun, J., Brenzke, M., Bretz, H. -P, Bron, S., Brostean-Kaiser, J., Burgman, Alexander, Busse, R. S., Carver, T., Cheung, E., Chirkin, D., Christov, A., Clark, K., Classen, L., Coenders, S., Collin, G. H., Conrad, J. M., Coppin, P., Correa, P., Cowen, D. F., Cross, R., Dave, P., Day, M., de Andre, J. P. A. M., De Clercq, C., DeLaunay, J. J., Dembinski, H., De Ridder, S., Desiati, P., de Vries, K. D., de Wasseige, G., de With, M., DeYoung, T., Diaz-Velez, J. C., di Lorenzo, V., Dujmovic, H., Dumm, J. P., Dunkman, M., Dvorak, E., Eberhardt, B., Ehrhardt, T., Eichmann, B., Eller, P., Evenson, P. A., Fahey, S., Fazely, A. R., Felde, J., Filimonov, K., Finley, C., Flis, S., Franckowiak, A., Friedman, E., Fritz, A., Gaisser, T. K., Gallagher, J., Gerhardt, L., Ghorbani, K., Glauch, T., Glusenkamp, T., Goldschmidt, A., Gonzalez, J. G., Grant, D., Griffith, Z., Haack, C., Hallgren, Allan, Halzen, F., Hanson, K., Hebecker, D., Heereman, D., Helbing, K., Hellauer, R., Hickford, S., Hignight, J., Hill, G. C., Hoffman, K. D., Hoffmann, R., Hoinka, T., Hokanson-Fasig, B., Hoshina, K., Huang, F., Huber, M., Hultqvist, K., Hunnefeld, M., Hussain, R., In, S., Iovine, N., Ishihara, A., Jacobi, E., Japaridze, G. S., Jeong, M., Jero, K., Jones, B. J. P., Kalaczynski, P., Kang, W., Kappes, A., Kappesser, D., Karg, T., Karle, A., Katz, U., Kauer, M., Keivani, A., Kelley, J. L., Kheirandish, A., Kim, J., Kim, M., Kintscher, T., Kiryluk, J., Kittler, T., Klein, S. R., Koirala, R., Kolanoski, H., Kopke, L., Kopper, C., Kopper, S., Koschinsky, J. P., Koskinen, D. J., Kowalski, M., Krings, K., Kroll, M., Kruckl, G., Kunwar, S., Kurahashi, N., Kuwabara, T., Kyriacou, A., Labare, M., Lanfranchi, J. L., Larson, M. J., Lauber, F., Leonard, K., Lesiak-Bzdak, M., Leuermann, M., Liu, Q. R., Mariscal, C. J. Lozano, Lu, L., Lunemann, J., Luszczak, W., Madsen, J., Maggi, G., Mahn, K. B. M., Mancina, S., Maruyama, R., Mase, K., Maunu, R., Meagher, K., Medici, M., Meier, M., Menne, T., Merino, G., Meures, T., Miarecki, S., Micallef, J., Momente, G., Montaruli, T., Moore, R. W., Morse, R., Moulai, M., Nahnhauer, R., Nakarmi, P., Naumann, U., Neer, G., Niederhausen, H., Nowicki, S. C., Nygren, D. R., Pollmann, A. Obertacke, Olivas, A., O'Murchadha, A., O'Sullivan, E., Palczewski, T., Pandya, H., Pankova, D. V., Peiffer, P., Pepper, J. A., de los Heros, Carlos, Pieloth, D., Pinat, E., Plum, M., Price, P. B., Przybylski, G. T., Raab, C., Radel, L., Rameez, M., Rauch, L., Rawlins, K., Rea, I. C., Reimann, R., Relethford, B., Relich, M., Resconi, E., Rhode, W., Richman, M., Robertson, S., Rongen, M., Rott, C., Ruhe, T., Ryckbosch, D., Rysewyk, D., Safa, I., Salzer, T., Herrera, S. E. Sanchez, Sandrock, A., Sandroos, J., Santander, M., Sarkar, S., Satalecka, K., Schlunder, P., Schmidt, T., Schneider, A., Schoenen, S., Schoneberg, S., Schumacher, L., Sclafani, S., Seckel, D., Seunarine, S., Soedingrekso, J., Soldin, D., Song, M., Spiczak, G. M., Spiering, C., Stachurska, J., Stamatikos, M., Stanev, T., Stasik, A., Stein, R., Stettner, J., Steuer, A., Stezelberger, T., Stokstad, R. G., Stossl, A., Strotjohann, N. L., Stuttard, T., Sullivan, G. W., Sutherland, M., Taboada, I., Tatar, J., Tenholt, F., Ter-Antonyan, S., Terliuk, A., Tilav, S., Toale, P. A., Tobin, M. N., Toennis, C., Toscano, S., Tosi, D., Tselengidou, M., Tung, C. F., Turcati, A., Turley, C. F., Ty, B., Unger, Elisabeth, Usner, M., Vandenbroucke, J., Van Driessche, W., van Eijk, D., van Eijndhoven, N., Vanheule, S., van Santen, J., Vogel, E., Vraeghe, M., Walck, C., Wallace, A., Mallraff, M., Wandler, F. D., Wandkowsky, N., Waza, A., Weaver, C., Weiss, M. J., Wendt, C., Werthebach, J., Westerhoff, S., Whelan, B. J., Whitehorn, N., Wiebe, K., Wiebusch, C. H., Wille, L., Williams, D. R., Wills, L., Wolf, M., Wood, J., Wood, T. R., Woschnagg, K., Xu, D. L., Xu, X. W., Xu, Y., Yanez, J. P., Yodh, G., Yoshida, S., Yuan, T., Abdollahi, S., Ajello, M., Angioni, R., Baldini, L., Ballet, J., Barbiellini, G., Bastieri, D., Bechtol, K., Bellazzini, R., Berenji, B., Bissaldi, E., Blandford, R. D., Bonino, R., Bottacini, E., Bregeon, J., Bruel, P., Buehler, R., Burnett, T. H., Burns, E., Buson, S., Cameron, R. A., Caputo, R., Caraveo, P. A., Cavazzuti, E., Charles, E., Chen, S., Cheung, C. 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A., and Sivakoff, G. R.
- Abstract
INTRODUCTION Neutrinos are tracers of cosmic-ray acceleration: electrically neutral and traveling at nearly the speed of light, they can escape the densest environments and may be traced back to their source of origin. High-energy neutrinos are expected to be produced in blazars: intense extragalactic radio, optical, x-ray, and, in some cases, γ-ray sources characterized by relativistic jets of plasma pointing close to our line of sight. Blazars are among the most powerful objects in the Universe and are widely speculated to be sources of high-energy cosmic rays. These cosmic rays generate high-energy neutrinos and γ-rays, which are produced when the cosmic rays accelerated in the jet interact with nearby gas or photons. On 22 September 2017, the cubic-kilometer IceCube Neutrino Observatory detected a ~290-TeV neutrino from a direction consistent with the flaring γ-ray blazar TXS 0506+056. We report the details of this observation and the results of a multiwavelength follow-up campaign. RATIONALE Multimessenger astronomy aims for globally coordinated observations of cosmic rays, neutrinos, gravitational waves, and electromagnetic radiation across a broad range of wavelengths. The combination is expected to yield crucial information on the mechanisms energizing the most powerful astrophysical sources. That the production of neutrinos is accompanied by electromagnetic radiation from the source favors the chances of a multiwavelength identification. In particular, a measured association of high-energy neutrinos with a flaring source of γ-rays would elucidate the mechanisms and conditions for acceleration of the highest-energy cosmic rays. The discovery of an extraterrestrial diffuse flux of high-energy neutrinos, announced by IceCube in 2013, has characteristic properties that hint at contributions from extragalactic sources, although the individual sources remain as yet unidentified. Continuously monitoring the entire sky for astrophysical neutrinos, IceCube provides
- Published
- 2018
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127. Multi-messenger Observations of a Binary Neutron Star Merger
- Author
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Abbott, B. P., Abbott, R., Abbott, T. D., Acernese, F., Ackley, K., Adams, C., Adams, T., Addesso, P., Adhikari, R. X., Adya, V. B., Affeldt, C., Afrough, M., Agarwal, B., Agathos, M., Agatsuma, K., Aggarwal, N., Aguiar, O. D., Aiello, L., Ain, A., Ajith, P., Allen, B., Allen, G., Allocca, A., Altin, P. A., Amato, A., Ananyeva, A., Anderson, S. B., Anderson, W. G., Angelova, S. V., Antier, S., Appert, S., Arai, K., Araya, M. C., Areeda, J. S., Arnaud, N., Arun, K. G., Ascenzi, S., Ashton, G., Ast, M., Aston, S. M., Astone, P., Atallah, D. V., Aufmuth, P., Aulbert, C., AultONeal, K., Austin, C., Avila-Alvarez, A., Babak, S., Bacon, P., Bader, M. K. M., Bae, S., Baker, P. T., Baldaccini, F., Ballardin, G., Ballmer, S. W., Banagiri, S., Barayoga, J. C., Barclay, S. E., Barish, B. C., Barker, D., Barkett, K., Barone, F., Barr, B., Barsotti, L., Barsuglia, M., Barta, D., Barthelmy, S. D., Bartlett, J., Bartos, I., Bassiri, R., Basti, A., Batch, J. C., Bawaj, M., Bayley, J. C., Bazzan, M., Bécsy, B., Beer, C., Bejger, M., Belahcene, I., Bell, A. S., Berger, B. K., Bergmann, G., Bero, J. J., Berry, C. P. L., Bersanetti, D., Bertolini, A., Betzwieser, J., Bhagwat, S., Bhandare, R., Bilenko, I. A., Billingsley, G., Billman, C. R., Birch, J., Birney, R., Birnholtz, O., Biscans, S., Biscoveanu, S., Bisht, A., Bitossi, M., Biwer, C., Bizouard, M. A., Blackburn, J. K., Blackman, J., Blair, C. D., Blair, D. G., Blair, R. M., Bloemen, S., Bock, O., Bode, N., Boer, M., Bogaert, G., Bohe, A., Bondu, F., Bonilla, E., Bonnand, R., Boom, B. A., Bork, R., Boschi, V., Bose, S., Bossie, K., Bouffanais, Y., Bozzi, A., Bradaschia, C., Brady, P. R., Branchesi, M., Brau, J. E., Briant, T., Brillet, A., Brinkmann, Markus, Brisson, V., Brockill, P., Broida, J. E., Brooks, A. F., Brown, D. A., Brown, D. D., Brunett, S., Buchanan, C. C., Buikema, A., Bulik, T., Bulten, H. J., Buonanno, A., Buskulic, D., Buy, C., Byer, R. 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- Abstract
59 Seiten : Illustrationen, Tabellen, Diagramme (2017).
- Published
- 2017
- Full Text
- View/download PDF
128. Swift and NuSTAR observations of GW170817: Detection of a blue kilonova
- Author
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Eleonora Troja, M. Perri, David Palmer, Sean N. Pike, A. Y. Lien, A. P. Beardmore, Javier A. García, J. P. Osborne, Hans A. Krimm, Mansi M. Kasliwal, Stephan Rosswog, Judith Racusin, Giancarlo Cusumano, Chris L. Fryer, M. de Pasquale, Karl Forster, Fiona A. Harrison, David N. Burrows, T. Sakamoto, Ryan Wollaeger, Gianpiero Tagliaferri, Frank Marshall, A. A. Breeveld, S. R. Oates, Oleg Korobkin, Michael H. Siegel, P. D'Avanzo, S. W. K. Emery, Andrew J. Levan, A. Tohuvavohu, J. A. Kennea, Sergio Campana, Y. Xu, B. Sbarufatti, Aimee Hungerford, Kenta Hotokezaka, Christopher J. Fontes, Nial R. Tanvir, D. B. Malesani, Wesley Even, Brian W. Grefenstette, S. B. Cenko, C. Pagani, Valerio D'Elia, P. T. O'Brien, A. Melandri, Phil Evans, Paolo Giommi, Caryl Gronwall, K. K. Madsen, Antonino D'Ai, J. A. Nousek, N. P. M. Kuin, Marianne Heida, Scott Barthelmy, Hiromasa Miyasaka, Ehud Nakar, Dieter H. Hartmann, K. L. Page, ITA, USA, GBR, DNK, SWE, and TUR
- Subjects
Physics ,High Energy Astrophysical Phenomena (astro-ph.HE) ,Solar mass ,Multidisciplinary ,Orbital plane ,010308 nuclear & particles physics ,Gravitational wave ,Astrophysics::High Energy Astrophysical Phenomena ,FOS: Physical sciences ,Astrophysics ,Astrophysics::Cosmology and Extragalactic Astrophysics ,Kilonova ,Compact star ,01 natural sciences ,law.invention ,Afterglow ,Telescope ,Neutron star ,law ,0103 physical sciences ,Astrophysics::Solar and Stellar Astrophysics ,Astrophysics - High Energy Astrophysical Phenomena ,010303 astronomy & astrophysics ,Astrophysics::Galaxy Astrophysics ,QB - Abstract
With the first direct detection of merging black holes in 2015, the era of gravitational wave (GW) astrophysics began. A complete picture of compact object mergers, however, requires the detection of an electromagnetic (EM) counterpart. We report ultraviolet (UV) and X-ray observations by Swift and the Nuclear Spectroscopic Telescope ARray (NuSTAR) of the EM counterpart of the binary neutron star merger GW170817. The bright, rapidly fading ultraviolet emission indicates a high mass ($\approx0.03$ solar masses) wind-driven outflow with moderate electron fraction ($Y_{e}\approx0.27$). Combined with the X-ray limits, we favor an observer viewing angle of $\approx 30^{\circ}$ away from the orbital rotation axis, which avoids both obscuration from the heaviest elements in the orbital plane and a direct view of any ultra-relativistic, highly collimated ejecta (a gamma-ray burst afterglow)., Science, in press; 56 pages, 12 figures
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- 2017
129. Multi-messenger Observations of a Binary Neutron Star Merger
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Abbott, B. P., Abbott, R., Abbott, T. D., Acernese, F., Ackley, K., Adams, C., Adams, T., Addesso, P., Adhikari, R. X., Adya, V. B., Affeldt, C., Afrough, M., Agarwal, B., Agathos, M., Agatsuma, K., Aggarwal, N., Aguiar, O. D., Aiello, L., Ain, A., Ajith, P., Allen, B., Allen, G., Allocca, A., Altin, P. A., Amato, A., Ananyeva, A., Anderson, S. B., Anderson, W. G., Angelova, S. V., Antier, S., Appert, S., Arai, K., Araya, M. C., Areeda, J. S., Arnaud, N., Arun, K. G., Ascenzi, S., Ashton, G., Ast, M., Aston, S. M., Astone, P., Atallah, D. V., Aufmuth, P., Aulbert, C., AultONeal, K., Austin, C., Avila-Alvarez, A., Babak, S., Bacon, P., Bader, M. K. M., Bae, S., Baker, P. T., Baldaccini, F., Ballardin, G., Ballmer, S. W., Banagiri, S., Barayoga, J. C., Barclay, S. E., Barish, B. C., Barker, D., Barkett, K., Barone, F., Barr, B., Barsotti, L., Barsuglia, M., Barta, D., Barthelmy, S. D., Bartlett, J., Bartos, I., Bassiri, R., Basti, A., Batch, J. C., Bawaj, M., Bayley, J. C., Bazzan, M., Bécsy, B., Beer, C., Bejger, M., Belahcene, I., Bell, A. S., Berger, B. K., Bergmann, G., Bero, J. J., Berry, C. P. L., Bersanetti, D., Bertolini, A., Betzwieser, J., Bhagwat, S., Bhandare, R., Bilenko, I. A., Billingsley, G., Billman, C. R., Birch, J., Birney, R., Birnholtz, O., Biscans, S., Biscoveanu, S., Bisht, A., Bitossi, M., Biwer, C., Bizouard, M. A., Blackburn, J. K., Blackman, J., Blair, C. D., Blair, D. G., Blair, R. M., Bloemen, S., Bock, O., Bode, N., Boer, M., Bogaert, G., Bohe, A., Bondu, F., Bonilla, E., Bonnand, R., Boom, B. A., Bork, R., Boschi, V., Bose, S., Bossie, K., Bouffanais, Y., Bozzi, A., Bradaschia, C., Brady, P. R., Branchesi, M., Brau, J. E., Briant, T., Brillet, A., Brinkmann, M., Brisson, V., Brockill, P., Broida, J. E., Brooks, A. F., Brown, D. A., Brown, D. D., Brunett, S., Buchanan, C. C., Buikema, A., Bulik, T., Bulten, H. J., Buonanno, A., Buskulic, D., Buy, C., Byer, R. 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D., Verzi, V., Vicha, J., Villaseñor, L., Vorobiov, S., Wahlberg, H., Wainberg, O., Walz, D., Watson, A. A., Weber, M., Weindl, A., Wiedeński, M., Wiencke, L., Wilczyński, H., Wirtz, M., Wittkowski, D., Wundheiler, B., Yushkov, A., Zas, E., Zavrtanik, D., Zavrtanik, M., Zepeda, A., Zimmermann, B., Ziolkowski, M., Zong, Z., Zuccarello, F., Kim, S., Schulze, S., Corral-Santana, J. M., de Gregorio-Monsalvo, I., González-López, J., Hartmann, D. H., Ishwara-Chandra, C. H., Martín, S., Mehner, A., Misra, K., Michałowski, M. J., Resmi, L., Paragi, Z., Agudo, I., An, T., Beswick, R., Casadio, C., Frey, S., Jonker, P., Kettenis, M., Marcote, B., Moldon, J., Szomoru, A., van Langevelde, H. J., Cwiek, A., Cwiok, M., Czyrkowski, H., Dabrowski, R., Kasprowicz, G., Mankiewicz, L., Nawrocki, K., Opiela, R., Piotrowski, L. W., Wrochna, G., Zaremba, M., Żarnecki, A. F., Haggard, D., Nynka, M., Ruan, J. J., Bland, P. A., Booler, T., Devillepoix, H. A. R., Gois, J. S. de, Hancock, P. J., Howie, R. M., Paxman, J., Sansom, E. K., Towner, M. C., Tonry, J., Coughlin, M., Stubbs, C. W., Denneau, L., Heinze, A., Stalder, B., Weiland, H., Eatough, R. P., Kramer, M., Kraus, A., Piro, L., González, J. Becerra, Butler, N. R., Khandrika, H. G., Kutyrev, A., Lee, W. H., Ricci, R., Ryan Jr., R. E., Sánchez-Ramírez, R., Veilleux, S., Watson, A. M., Wieringa, M. H., Burgess, J. M., Eerten, H. van, Fontes, C. J., Korobkin, O., Wollaeger, R. T., Camilo, F., Foley, A. R., Goedhart, S., Makhathini, S., Oozeer, N., Smirnov, O. M., and Woudt, P. A.
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ddc - Published
- 2016
130. Swift and NuSTAR observations of GW170817: Detection of a blue kilonova
- Author
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Evans, P. A., primary, Cenko, S. B., additional, Kennea, J. A., additional, Emery, S. W. K., additional, Kuin, N. P. M., additional, Korobkin, O., additional, Wollaeger, R. T., additional, Fryer, C. L., additional, Madsen, K. K., additional, Harrison, F. A., additional, Xu, Y., additional, Nakar, E., additional, Hotokezaka, K., additional, Lien, A., additional, Campana, S., additional, Oates, S. R., additional, Troja, E., additional, Breeveld, A. A., additional, Marshall, F. E., additional, Barthelmy, S. D., additional, Beardmore, A. P., additional, Burrows, D. N., additional, Cusumano, G., additional, D’Aì, A., additional, D’Avanzo, P., additional, D’Elia, V., additional, de Pasquale, M., additional, Even, W. P., additional, Fontes, C. J., additional, Forster, K., additional, Garcia, J., additional, Giommi, P., additional, Grefenstette, B., additional, Gronwall, C., additional, Hartmann, D. H., additional, Heida, M., additional, Hungerford, A. L., additional, Kasliwal, M. M., additional, Krimm, H. A., additional, Levan, A. J., additional, Malesani, D., additional, Melandri, A., additional, Miyasaka, H., 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, Pike, S., additional, Racusin, J. L., additional, Rosswog, S., additional, Siegel, M. H., additional, Sakamoto, T., additional, Sbarufatti, B., additional, Tagliaferri, G., additional, Tanvir, N. R., additional, and Tohuvavohu, A., additional
- Published
- 2017
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131. Swift and NuSTAR observations of GW170817:Detection of a blue kilonova
- Author
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Evans, P. A., Cenko, S. B., Kennea, J. A., Emery, S. W. K., Kuin, N. P. M., Korobkin, O., Wollaeger, R. T., Fryer, C. L., Madsen, K. K., Harrison, F. A., Xu, Y., Nakar, E., Hotokezaka, K., Lien, A., Campana, S., Oates, S. R., Troja, E., Breeveld, A. A., Marshall, F. E., Barthelmy, S. D., Beardmore, A. P., Burrows, D. N., Cusumano, G., D'Ai, A., D'Avanzo, P., D'Elia, V., De Pasquale, M., Even, W. P., Fontes, C. J., Forster, K., Garcia, J., Giommi, P., Grefenstette, B., Gronwall, C., Hartmann, D. H., Heida, M., Hungerford, A. L., Kasliwal, M. M., Krimm, H. A., Levan, A. J., Malesani, D., Melandri, A., Miyasaka, H., Nousek, J. A., O'Brien, P. T., Osborne, J. P., Pagani, C., Page, K. L., Palmer, D. M., Perri, M., Pike, S., Racusin, J. L., Rosswog, S., Siegel, M. H., Sakamoto, T., Sbarufatti, B., Tagliaferri, G., Tanvir, N. R., Tohuvavohu, A., Evans, P. A., Cenko, S. B., Kennea, J. A., Emery, S. W. K., Kuin, N. P. M., Korobkin, O., Wollaeger, R. T., Fryer, C. L., Madsen, K. K., Harrison, F. A., Xu, Y., Nakar, E., Hotokezaka, K., Lien, A., Campana, S., Oates, S. R., Troja, E., Breeveld, A. A., Marshall, F. E., Barthelmy, S. D., Beardmore, A. P., Burrows, D. N., Cusumano, G., D'Ai, A., D'Avanzo, P., D'Elia, V., De Pasquale, M., Even, W. P., Fontes, C. J., Forster, K., Garcia, J., Giommi, P., Grefenstette, B., Gronwall, C., Hartmann, D. H., Heida, M., Hungerford, A. L., Kasliwal, M. M., Krimm, H. A., Levan, A. J., Malesani, D., Melandri, A., Miyasaka, H., Nousek, J. A., O'Brien, P. T., Osborne, J. P., Pagani, C., Page, K. L., Palmer, D. M., Perri, M., Pike, S., Racusin, J. L., Rosswog, S., Siegel, M. H., Sakamoto, T., Sbarufatti, B., Tagliaferri, G., Tanvir, N. R., and Tohuvavohu, A.
- Published
- 2017
132. Multi-messenger observations of a binary neutron star merger
- Author
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Abbott, B., Abbott, R., Abbott, T., Acernese, F., Ackley, K., Adams, C., Adams, T., Addesso, P., Adhikari, R., Adya, V., Affeldt, C., Afrough, M., Agarwal, B., Agathos, M., Agatsuma, K., Aggarwal, N., Aguiar, O., Aiello, L., Ain, A., Ajith, P., Allen, B., Allen, G., Allocca, A., Altin, P., Amato, A., Ananyeva, A., Anderson, S., Anderson, W., Angelova, S., Antier, S., Appert, S., Arai, K., Araya, M., Areeda, J., Arnaud, N., Arun, K., Ascenzi, S., Ashton, G., Ast, M., Aston, S., Astone, P., Atallah, D., Aufmuth, P., Aulbert, C., AultONeal, K., Austin, C., Avila-Alvarez, A., Babak, S., Bacon, P., Bader, M., Bae, S., Baker, P., Baldaccini, F., Ballardin, G., Ballmer, S., Banagiri, S., Barayoga, J., Barclay, S., Barish, B., Barker, D., Barkett, K., Barone, F., Barr, B., Barsotti, L., Barsuglia, M., Barta, D., Barthelmy, S., Bartlett, J., Bartos, I., Bassiri, R., Basti, A., Batch, J., Bawaj, M., Bayley, J., Bazzan, M., Becsy, B., Beer, C., Bejger, M., Belahcene, I., Bell, A., Berger, B., 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Etchegoyen, A., Falcke, H., Farmer, J., Farrar, G., Fauth, A., Fazzini, N., Feldbusch, F., Fenu, F., Fick, B., Figueira, J., Filipcic, A., Freire, M., Fujii, T., Fuster, A., Gaior, R., Garcia, B., Gemmeke, H., Gherghel-Lascu, A., Ghia, P., Giaccari, U., Giammarchi, M., Giller, M., Glas, D., Glaser, C., Golup, G., Berisso, M., Vitale, P., Gonzlez, N., Gorgi, A., Gottowik, M., Grillo, A., Grubb, T., Guarino, F., Guedes, G., Halliday, R., Hampel, M., Hansen, P., Harari, D., Harrison, T., Harvey, V., Haungs, A., Hebbeker, T., Heck, D., Heimann, P., Herve, A., Hojvat, C., Holt, E., Homola, P., Horandel, J., Horvath, P., Hrabovsky, M., Huege, T., Hulsman, J., Insolia, A., Isar, P., Jandt, I., Johnsen, J., Josebachuili, M., Jurysek, J., Kaapa, A., Kampert, K., Keilhauer, B., Kemmerich, N., Kemp, J., Kieckhafer, R., Klages, H., Kleifges, M., Kleinfeller, J., Krause, R., Krohm, N., Kuempel, D., Mezek, G., Kunka, N., Awad, A., Lago, B., LaHurd, D., Lauscher, M., Legumina, R., De Oliveira, M., Letessier-Selvon, A., Lhenry-Yvon, I., Link, K., Lo Presti, D., Lopes, L., Lopez, R., Casado, A., Lorek, R., Luce, Q., Lucero, A., Malacari, M., Mallamaci, M., Mandat, D., Mantsch, P., Mariazzi, A., Maris, I., Marsella, G., Martello, D., Martinez, H., Bravo, O., Meza, J., Mathes, H., Mathys, S., Matthiae, G., Mayotte, E., Mazur, P., Medina, C., Medina-Tanco, G., Melo, D., Menshikov, A., Merenda, K., Michal, S., Micheletti, M., Middendorf, L., Miramonti, L., Mitrica, B., Mockler, D., Mollerach, S., Montanet, F., Morello, C., Morlino, G., Mueller, M., Mueller, S., Mussa, R., Naranjo, I., Niculescu-Oglinzanu, M., Niechciol, M., Niemietz, L., Niggemann, T., Nitz, D., Nosek, D., Novotny, V., Nozka, L., Nunez, L., Oikonomou, F., Olinto, A., Palatka, M., Pallotta, J., Papenbreer, P., Parente, G., Parra, A., Paul, T., Pech, M., Pedreira, F., Kala, J., Pea-Rodriguez, J., Pereira, L., Perlin, M., Perrone, L., Peters, C., Petrera, S., Phuntsok, J., Pierog, T., Pimenta, M., Pirronello, V., Platino, M., Plum, M., Poh, J., Porowski, C., Prado, R., Privitera, P., Prouza, M., Quel, E., Querchfeld, S., Quinn, S., Ramos-Pollan, R., Rautenberg, J., Ravignani, D., Ridky, J., Riehn, F., Risse, M., Ristori, P., Rizi, V., De Carvalho, W., Fernandez, G., Rojo, J., Roncoroni, M., Roth, M., Roulet, E., Rovero, A., Ruehl, P., Saffi, S., Saftoiu, A., Salamida, F., Saleh, A., Salina, G., Sanchez, F., Sanchez-Lucas, P., Santos, E., Sarazin, F., Sarmento, R., Sarmiento-Cano, C., Sato, R., Schauer, M., Scherini, V., Schieler, H., Schimp, M., Schmidt, D., Scholten, O., Schovnek, P., Schroder, F., Schumacher, J., Sciutto, S., Segreto, A., Shadkam, A., Shellard, R., Sigl, G., Silli, G., Smida, R., Snow, G., Sommers, P., Sonntag, S., Soriano, J., Squartini, R., Stanca, D., Stanic, S., Stasielak, J., Stassi, P., Stolpovskiy, M., Strafella, F., Streich, A., Suarez, F., Suarez-Duran, M., Sudholz, T., Suomijarvi, T., Supanitsky, A., Supik, J., Swain, J., Szadkowski, Z., Taboada, A., Taborda, O., Timmermans, C., Peixoto, C., Tomankova, L., Tome, B., Elipe, G., Travnicek, P., Trini, M., Tueros, M., Ulrich, R., Unger, M., Urban, M., Galicia, J., Valio, I., Valore, L., Van Aar, G., Van Bodegom, P., Van den Berg, A., Van Vliet, A., Varela, E., Cardenas, B., Vazquez, R., Veberic, D., Ventura, C., Quispe, I., Verzi, V., Vicha, J., Villaseor, L., Vorobiov, S., Wahlberg, H., Wainberg, O., Walz, D., Watson, A., Weber, M., Weindl, A., Wiedenski, M., Wiencke, L., Wilczynski, H., Wirtz, M., Wittkowski, D., Wundheiler, B., Yushkov, A., Zas, E., Zavrtanik, D., Zavrtanik, M., Zepeda, A., Zimmermann, B., Ziolkowski, M., Zong, Z., Zuccarello, F., Schulze, S., Corral-Santana, J., De Gregorio-Monsalvo, I., Gonzlez-Lopez, J., Hartmann, D., Ishwara-Chandra, C., Martin, S., Mehner, A., Misra, K., Michalowski, M., Resmi, L., Paragi, Z., Agudo, I., An, T., Beswick, R., Casadio, C., Frey, S., Kettenis, M., Marcote, B., Moldon, J., Szomoru, A., Langevelde, H., Cwiek, A., Cwiok, M., Czyrkowski, H., Dabrowski, R., Kasprowicz, G., Mankiewicz, L., Nawrocki, K., Opiela, R., Piotrowski, L., Wrochna, G., Zaremba, M., Zarnecki, A., Haggard, D., Nynka, M., Ruan, J., Bland, Phil, Booler, T., Devillepoix, H., De Gois, J., Hancock, Paul, Howie, Robert, Paxman, Jonathan, Sansom, Eleanor, Towner, Martin, Tonry, J., Stubbs, C., Denneau, L., Heinze, A., Stalder, B., Weiland, H., Eatough, R., Kramer, M., Kraus, A., Piro, L., Gonzlez, J., Butler, N., Khandrika, H., Kutyrev, A., Lee, W., Ricci, R., Ryan, R., Sanchez-Ramirez, R., Veilleux, S., Wieringa, M., Burgess, J., Van Eerten, H., Fontes, C., Korobkin, O., Wollaeger, R., Camilo, F., Foley, A., Goedhart, S., Makhathini, S., Oozeer, N., Smirnov, O., and Woudt, P.
- Abstract
© 2017. The American Astronomical Society. All rights reserved. On 2017 August 17 a binary neutron star coalescence candidate (later designated GW170817) with merger time 12:41:04 UTC was observed through gravitational waves by the Advanced LIGO and Advanced Virgo detectors. The Fermi Gamma-ray Burst Monitor independently detected a gamma -ray burst (GRB 170817A) with a time delay of ~1.7 s with respect to the merger time. From the gravitational-wave signal, the source was initially localized to a sky region of 31 deg2 at a luminosity distance of 40 8 8-+ Mpc and with component masses consistent with neutron stars. The component masses were later measured to be in the range 0.86 to 2.26 M. An extensive observing campaign was launched across the electromagnetic spectrum leading to the discovery of a bright optical transient (SSS17a, now with the IAU identification of AT 2017gfo) in NGC 4993 (at ~40 Mpc) less than 11 hours after the merger by the One-Meter, Two Hemisphere (1M2H) team using the 1 m Swope Telescope. The optical transient was independently detected by multiple teams within an hour. Subsequent observations targeted the object and its environment. Early ultraviolet observations revealed a blue transient that faded within 48 hours. Optical and infrared observations showed a redward evolution over ~10 days. Following early non-detections, X-ray and radio emission were discovered at the transient's position ~9 and ~16 days, respectively, after the merger. Both the X-ray and radio emission likely arise from a physical process that is distinct from the one that generates the UV/optical/near-infrared emission. No ultra-high-energy gamma-rays and no neutrino candidates consistent with the source were found in follow-up searches. These observations support the hypothesis that GW170817 was produced by the merger of two neutron stars in NGC4993 followed by a short gamma-ray burst (GRB 170817A) and a kilonova/macronova powered by the radioactive decay of r-process nu
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- 2017
133. Observation of inverse Compton emission from a long γ-ray burst
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Veres, P., Bhat, P. N., Briggs, M. S., Cleveland, W. H., Hamburg, R., Hui, C. M., Mailyan, B., Preece, R. D., Roberts, O. J., von Kienlin, A., Wilson-Hodge, C. A., Kocevski, D., Arimoto, M., Tak, D., Asano, K., Axelsson, M., Barbiellini, G., Bissaldi, E., Dirirsa, F. Fana, Gill, R., Granot, J., McEnery, J., Omodei, N., Razzaque, S., Piron, F., Racusin, J. L., Thompson, D. J., Campana, S., Bernardini, M. G., Kuin, N. P. M., Siegel, M. H., Cenko, S. B., O’Brien, P., Capalbi, M., Daì, A., De Pasquale, M., Gropp, J., Klingler, N., Osborne, J. P., Perri, M., Starling, R. L. C., Tagliaferri, G., Tohuvavohu, A., Ursi, A., Tavani, M., Cardillo, M., Casentini, C., Piano, G., Evangelista, Y., Verrecchia, F., Pittori, C., Lucarelli, F., Bulgarelli, A., Parmiggiani, N., Anderson, G. E., Anderson, J. P., Bernardi, G., Bolmer, J., Caballero-García, M. D., Carrasco, I. M., Castellón, A., Segura, N. Castro, Castro-Tirado, A. J., Cherukuri, S. V., Cockeram, A. M., D’Avanzo, P., Di Dato, A., Diretse, R., Fender, R. P., Fernández-García, E., Fynbo, J. P. U., Fruchter, A. S., Greiner, J., Gromadzki, M., Heintz, K. E., Heywood, I., van der Horst, A. J., Hu, Y.-D., Inserra, C., Izzo, L., Jaiswal, V., Jakobsson, P., Japelj, J., Kankare, E., Kann, D. A., Kouveliotou, C., Klose, S., Levan, A. J., Li, X. Y., Lotti, S., Maguire, K., Malesani, D. B., Manulis, I., Marongiu, M., Martin, S., Melandri, A., Michałowski, M. J., Miller-Jones, J. C. A., Misra, K., Moin, A., Mooley, K. P., Nasri, S., Nicholl, M., Noschese, A., Novara, G., Pandey, S. B., Peretti, E., del Pulgar, C. J. Pérez, Pérez-Torres, M. A., Perley, D. A., Piro, L., Ragosta, F., Resmi, L., Ricci, R., Rossi, A., Sánchez-Ramírez, R., Selsing, J., Schulze, S., Smartt, S. J., Smith, I. A., Sokolov, V. V., Stevens, J., Tanvir, N. R., Thöne, C. C., Tiengo, A., Tremou, E., Troja, E., de Ugarte Postigo, A., Valeev, A. F., Vergani, S. D., Wieringa, M., Woudt, P. A., Xu, D., Yaron, O., and Young, D. R.
- Abstract
Long-duration γ-ray bursts (GRBs) originate from ultra-relativistic jets launched from the collapsing cores of dying massive stars. They are characterized by an initial phase of bright and highly variable radiation in the kiloelectronvolt-to-megaelectronvolt band, which is probably produced within the jet and lasts from milliseconds to minutes, known as the prompt emission1,2. Subsequently, the interaction of the jet with the surrounding medium generates shock waves that are responsible for the afterglow emission, which lasts from days to months and occurs over a broad energy range from the radio to the gigaelectronvolt bands1–6. The afterglow emission is generally well explained as synchrotron radiation emitted by electrons accelerated by the external shock7–9. Recently, intense long-lasting emission between 0.2 and 1 teraelectronvolts was observed from GRB 190114C10,11. Here we report multi-frequency observations of GRB 190114C, and study the evolution in time of the GRB emission across 17 orders of magnitude in energy, from 5 × 10−6to 1012electronvolts. We find that the broadband spectral energy distribution is double-peaked, with the teraelectronvolt emission constituting a distinct spectral component with power comparable to the synchrotron component. This component is associated with the afterglow and is satisfactorily explained by inverse Compton up-scattering of synchrotron photons by high-energy electrons. We find that the conditions required to account for the observed teraelectronvolt component are typical for GRBs, supporting the possibility that inverse Compton emission is commonly produced in GRBs.
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- 2019
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134. GW170817: Swift UV detection of a blue kilonova, and improving the search in O3.
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Tohuvavohu, Aaron, Kennea, Jamie A., González, G., and Hynes, R.
- Abstract
Swift 's rapid slewing, flexible planning, and multi-wavelength instruments make it the most capable space-based follow-up engine for finding poorly localized sources. During O1 and O2 Swift successfully tiled hundreds of square-degrees of sky in the LVC localization regions, searching for, and identifying, possible X-ray and UV/O transients in the field. Swift made important contributions to the discovery and characterization of the kilonova AT 2017gfo, discovering the UV emission and providing the deepest X-ray upper limits in the first 24 hours after the trigger, strongly constraining the dynamics and geometry of the counterpart. Swift tiled 92% of the galaxy convolved error region down to average X-ray flux sensitivities of 10
−12 erg cm−2 s−1 , significantly increasing our confidence that AT 2017gfo is indeed the counterpart to GW 170817 and sGRB 170817. However, there remains significant room for improvement of Swift's follow-up in preparation for O3. This will take the form of both revised observation strategy based on detailed analysis of the results from O2, and significant changes to Swift 's operational capabilities. These improvements are necessary both for maximizing the likelihood that Swift finds a counterpart, and minimizing the impact that follow-up activities have on other Swift science priorities. We outline areas of improvement to the observing strategy itself for optimal tiling of the LVC localization regions. We also discuss ongoing work on operational upgrades that will decrease latency in our response time, and minimize impact on pre-planned observations, while maintaining spacecraft health and safety. [ABSTRACT FROM AUTHOR]- Published
- 2018
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135. GW170817: Swift UV detection of a blue kilonova, and improving the search in O3.
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Tohuvavohu, Aaron, Kennea, Jamie A., González, G., and Hynes, R.
- Abstract
Swift 's rapid slewing, flexible planning, and multi-wavelength instruments make it the most capable space-based follow-up engine for finding poorly localized sources. During O1 and O2 Swift successfully tiled hundreds of square-degrees of sky in the LVC localization regions, searching for, and identifying, possible X-ray and UV/O transients in the field. Swift made important contributions to the discovery and characterization of the kilonova AT 2017gfo, discovering the UV emission and providing the deepest X-ray upper limits in the first 24 hours after the trigger, strongly constraining the dynamics and geometry of the counterpart. Swift tiled 92% of the galaxy convolved error region down to average X-ray flux sensitivities of 10
−12 erg cm−2 s−1 , significantly increasing our confidence that AT 2017gfo is indeed the counterpart to GW 170817 and sGRB 170817. However, there remains significant room for improvement of Swift's follow-up in preparation for O3. This will take the form of both revised observation strategy based on detailed analysis of the results from O2, and significant changes to Swift 's operational capabilities. These improvements are necessary both for maximizing the likelihood that Swift finds a counterpart, and minimizing the impact that follow-up activities have on other Swift science priorities. We outline areas of improvement to the observing strategy itself for optimal tiling of the LVC localization regions. We also discuss ongoing work on operational upgrades that will decrease latency in our response time, and minimize impact on pre-planned observations, while maintaining spacecraft health and safety. [ABSTRACT FROM AUTHOR]- Published
- 2017
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136. A low-cost ultraviolet-to-infrared absolute quantum efficiency characterization system of detectors
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Holland, Andrew D., Beletic, James, Gill, Ajay S., Shaaban, Mohamed M., Tohuvavohu, Aaron, Sivanandam, Suresh, Abraham, Roberto G., Chen, Seery, Drout, Maria R., Lokhorst, Deborah, Matzner, Christopher D., Mochnacki, Stefan W., and Netterfield, Calvin B.
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- 2022
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137. Multi-epoch Modeling of TXS 0506+056 and Implications for Long-term High-energy Neutrino Emission.
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Maria Petropoulou, Kohta Murase, Marcos Santander, Sara Buson, Aaron Tohuvavohu, Taiki Kawamuro, Georgios Vasilopoulos, Hiroshi Negoro, Yoshihiro Ueda, Michael H. Siegel, Azadeh Keivani, Nobuyuki Kawai, Apostolos Mastichiadis, and Stavros Dimitrakoudis
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NEUTRINOS ,SPECTRAL energy distribution ,COMPTON scattering ,ELECTRON density ,ELECTRON scattering - Abstract
The IceCube report of a excess of 13 ± 5 neutrino events in the direction of the blazar TXS 0506+056 in 2014–2015 and the 2017 detection of a high-energy neutrino event, IceCube-170922A, during a gamma-ray flare from the same blazar, have revived the interest in scenarios for neutrino production in blazars. We perform comprehensive analyses on the long-term electromagnetic emission of TXS 0506+056 using optical, X-ray, and gamma-ray data from the All-Sky Automated Survey for Supernovae, the Neil Gehrels Swift Observatory, Monitor of All-sky X-ray Image, and the Fermi Large Area Telescope. We also perform numerical modeling of the spectral energy distributions (SEDs) in four epochs prior to 2017 with contemporaneous gamma-ray and lower-energy (optical and/or X-ray) data. We find that the multi-epoch SEDs are consistent with a hybrid leptonic scenario, where the gamma-rays are produced in the blazar zone via external inverse Compton scattering of accelerated electrons, and high-energy neutrinos are produced via the photomeson production process of co-accelerated protons. The multi-epoch SEDs can be satisfactorily explained with the same jet parameters and variable external photon density and electron luminosity. Using the maximal neutrino flux derived for each epoch, we put an upper limit of ∼0.4–2 on the muon neutrino number in 10 years of IceCube observations. Our results are consistent with the IceCube-170922A detection, which can be explained as an upper fluctuation from the average neutrino rate expected from the source, but in strong tension with the 2014–2015 neutrino flare. [ABSTRACT FROM AUTHOR]
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- 2020
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138. Swift-XRT Follow-up of Gravitational-wave Triggers in the Second Advanced LIGO/Virgo Observing Run.
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N. J. Klingler, J. A. Kennea, P. A. Evans, A. Tohuvavohu, S. B. Cenko, S. D. Barthelmy, A. P. Beardmore, A. A. Breeveld, P. J. Brown, D. N. Burrows, S. Campana, G. Cusumano, A. D’Aì, P. D’Avanzo, V. D’Elia, M. de Pasquale, S. W. K. Emery, J. Garcia, P. Giommi, and C. Gronwall
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- 2019
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139. Fermi and Swift Observations of GRB 190114C: Tracing the Evolution of High-Energy Emission from Prompt to Afterglow
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Ajello, M., Arimoto, M., Axelsson, M., Baldini, L., Barbiellini, G., Bastieri, D., Bellazzini, R., Berretta, A., Bissaldi, E., Blandford, R. D., Bonino, R., Bottacini, E., Bregeon, J., Bruel, P., Buehler, R., Burns, E., Buson, S., Cameron, R. A., Caputo, R., Caraveo, P. A., Cavazzuti, E., Chen, S., Chiaro, G., Ciprini, S., Cohen-Tanugi, J., Costantin, D., Cutini, S., D'Ammando, F., DeKlotz, M., Luque, P. De La Torre, De Palma, F., Desai, A., Di Lalla, N., Di Venere, L., Dirirsa, F. Fana, Fegan, S. J., Franckowiak, A., Fukazawa, Y., Funk, S., Fusco, P., Gargano, F., Gasparrini, D., Giglietto, N., Gill, R., Giordano, F., Giroletti, M., Granot, J., Green, D., Grenier, I. A., Grondin, M. H., Guiriec, S., Hays, E., Horan, D., Jóhannesson, G., Kocevski, D., Kovac'evic', M., Kuss, M., Larsson, S., Latronico, L., Lemoine-Goumard, M., Li, Jian, Liodakis, I., Longo, F., Loparco, F., Lovellette, M. N., Lubrano, P., Maldera, S., Malyshev, D., Manfreda, A., Martí-Devesa, G., Mazziotta, M. N., McEnery, J. E., Mereu, I., Meyer, M., Michelson, P. F., Mitthumsiri, W., Mizuno, T., Monzani, M. E., Moretti, E., Morselli, A., Moskalenko, I. V., Negro, M., Nuss, E., Omodei, N., Orienti, M., Orlando, E., Palatiello, M., Paliya, V. S., Paneque, D., Pei, Z., Persic, M., Pesce-Rollins, M., Petrosian, V., Piron, F., Poon, H., Porter, T. A., Principe, G., Racusin, J. L., Rainò, S., Rando, R., Rani, B., Razzano, M., Razzaque, S., Reimer, A., Reimer, O., Ryde, F., Saz Parkinson, P. M., Serini, D., Sgrò, C., Siskind, E. J., Spandre, G., Spinelli, P., Tajima, H., Takagi, K., Takahashi, M. N., Tak, D., Thayer, J. B., Thompson, D. J., Torres, D. F., Troja, E., Valverde, J., Van Klaveren, B., Wood, K., Yassine, M., Zaharijas, G., Bhat, P. N., Briggs, M. S., Cleveland, W., Giles, M., Goldstein, A., Hui, M., Malacaria, C., Preece, R., Roberts, O., Veres, P., Von Kienlin, A., Cenko, S. B., O'Brien, P., Beardmore, A. P., Lien, A., Osborne, J. P., Tohuvavohu, A., D'Elia, V., D'A, A., Perri, M., Gropp, J., Klingler, N., Capalbi, M., Tagliaferri, G., and Stamatikos, M.
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13. Climate action - Abstract
The astrophysical journal 890(1), 9 (2020). doi:10.3847/1538-4357/ab5b05, We report on the observations of gamma-ray burst (GRB) 190114C by the Fermi Gamma-ray Space Telescope and the Neil Gehrels Swift Observatory. The early-time observations reveal multiple emission components that evolve independently, with a delayed power-law component that exhibits significant spectral attenuation above 40 MeV in the first few seconds of the burst. This power-law component transitions to a harder spectrum that is consistent with the afterglow emission observed at later times. This afterglow component is clearly identifiable in the GBM and BAT light curves as a slowly fading emission component on which the rest of the prompt emission is superimposed. As a result, we are able to constrain the transition from internal shock to external shock dominated emission. We find that the temporal and spectral evolution of the broadband afterglow emission can be well modeled as synchrotron emission from a forward shock propagating into a wind-like circumstellar environment and find that high-energy photons observed by Fermi LAT are in tension with the theoretical maximum energy that can be achieved through synchrotron emission from a shock. These violations of the maximum synchrotron energy are further compounded by the detection of very high energy (VHE) emission above 300 GeV by MAGIC concurrent with our observations. We conclude that the observations of VHE photons from GRB 190114C necessitates either an additional emission mechanism at very high energies that is hidden in the synchrotron component in the LAT energy range, an acceleration mechanism that imparts energy to the particles at a rate that is faster than the electron synchrotron energy loss rate, or revisions of the fundamental assumptions used in estimating the maximum photon energy attainable through the synchrotron process., Published by Chicago, Ill. [u.a.]
140. Observation Locator Table Access Protocol Version 1.0
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Salgado, Jesús, primary, Ibarra, Aitor, additional, Ehle, Matthias, additional, Gabriel, Carlos, additional, Kretschmar, Peter, additional, Kuulkers, Erik, additional, Merín, Bruno, additional, Ness, Jan-Uwe, additional, Salazar, Emilio, additional, Saxton, Richard, additional, Cecconi, Baptiste, additional, Foster, Karl, additional, Demleitner, Markus, additional, Dempsey, James, additional, Molinaro, Marco, additional, Sánchez, Celia, additional, Taylor, Mark, additional, Díaz Trigo, María, additional, Fernández, Mónica, additional, Kennea, Jaime, additional, Kettenis, Mark, additional, Matt, Giorgio, additional, Osborne, Julian, additional, de Oña Wilhelmi, Emma, additional, Salbol, Edward J., additional, Sivakoff, Gregory, additional, Tao, Lian, additional, Tohuvavohu, Aaron, additional, Tibbetts, Michael, additional, and Workman, Bill, additional
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141. Improving science yield for NASA Swift with automated planning technologies.
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A Tohuvavohu
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- 2018
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142. A Multimessenger Picture of the Flaring Blazar TXS 0506+056: Implications for High-energy Neutrino Emission and Cosmic-Ray Acceleration.
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A. Keivani, K. Murase, M. Petropoulou, D. B. Fox, S. B. Cenko, S. Chaty, A. Coleiro, J. J. DeLaunay, S. Dimitrakoudis, P. A. Evans, J. A. Kennea, F. E. Marshall, A. Mastichiadis, J. P. Osborne, M. Santander, A. Tohuvavohu, and C. F. Turley
- Subjects
SOLAR neutrinos ,SOLAR flares ,BL Lacertae objects ,COSMIC rays ,PARTICLE acceleration - Abstract
Detection of the IceCube-170922A neutrino coincident with the flaring blazar TXS 0506+056, the first and only ∼3σ high-energy neutrino source association to date, offers a potential breakthrough in our understanding of high-energy cosmic particles and blazar physics. We present a comprehensive analysis of TXS 0506+056 during its flaring state, using newly collected Swift, NuSTAR, and X-shooter data with Fermi observations and numerical models to constrain the blazar’s particle acceleration processes and multimessenger (electromagnetic (EM) and high-energy neutrino) emissions. Accounting properly for EM cascades in the emission region, we find a physically consistent picture only within a hybrid leptonic scenario, with γ-rays produced by external inverse-Compton processes and high-energy neutrinos via a radiatively subdominant hadronic component. We derive robust constraints on the blazar’s neutrino and cosmic-ray emissions and demonstrate that, because of cascade effects, the 0.1–100 keV emissions of TXS 0506+056 serve as a better probe of its hadronic acceleration and high-energy neutrino production processes than its GeV–TeV emissions. If the IceCube neutrino association holds, physical conditions in the TXS 0506+056 jet must be close to optimal for high-energy neutrino production, and are not favorable for ultrahigh-energy cosmic-ray acceleration. Alternatively, the challenges we identify in generating a significant rate of IceCube neutrino detections from TXS 0506+056 may disfavor single-zone models, in which γ-rays and high-energy neutrinos are produced in a single emission region. In concert with continued operations of the high-energy neutrino observatories, we advocate regular X-ray monitoring of TXS 0506+056 and other blazars in order to test single-zone blazar emission models, clarify the nature and extent of their hadronic acceleration processes, and carry out the most sensitive possible search for additional multimessenger sources. [ABSTRACT FROM AUTHOR]
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- 2018
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143. Heavy-element production in a compact object merger observed by JWST.
- Author
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Levan AJ, Gompertz BP, Salafia OS, Bulla M, Burns E, Hotokezaka K, Izzo L, Lamb GP, Malesani DB, Oates SR, Ravasio ME, Rouco Escorial A, Schneider B, Sarin N, Schulze S, Tanvir NR, Ackley K, Anderson G, Brammer GB, Christensen L, Dhillon VS, Evans PA, Fausnaugh M, Fong WF, Fruchter AS, Fryer C, Fynbo JPU, Gaspari N, Heintz KE, Hjorth J, Kennea JA, Kennedy MR, Laskar T, Leloudas G, Mandel I, Martin-Carrillo A, Metzger BD, Nicholl M, Nugent A, Palmerio JT, Pugliese G, Rastinejad J, Rhodes L, Rossi A, Saccardi A, Smartt SJ, Stevance HF, Tohuvavohu A, van der Horst A, Vergani SD, Watson D, Barclay T, Bhirombhakdi K, Breedt E, Breeveld AA, Brown AJ, Campana S, Chrimes AA, D'Avanzo P, D'Elia V, De Pasquale M, Dyer MJ, Galloway DK, Garbutt JA, Green MJ, Hartmann DH, Jakobsson P, Kerry P, Kouveliotou C, Langeroodi D, Le Floc'h E, Leung JK, Littlefair SP, Munday J, O'Brien P, Parsons SG, Pelisoli I, Sahman DI, Salvaterra R, Sbarufatti B, Steeghs D, Tagliaferri G, Thöne CC, de Ugarte Postigo A, and Kann DA
- Abstract
The mergers of binary compact objects such as neutron stars and black holes are of central interest to several areas of astrophysics, including as the progenitors of gamma-ray bursts (GRBs)
1 , sources of high-frequency gravitational waves (GWs)2 and likely production sites for heavy-element nucleosynthesis by means of rapid neutron capture (the r-process)3 . Here we present observations of the exceptionally bright GRB 230307A. We show that GRB 230307A belongs to the class of long-duration GRBs associated with compact object mergers4-6 and contains a kilonova similar to AT2017gfo, associated with the GW merger GW170817 (refs.7-12 ). We obtained James Webb Space Telescope (JWST) mid-infrared imaging and spectroscopy 29 and 61 days after the burst. The spectroscopy shows an emission line at 2.15 microns, which we interpret as tellurium (atomic mass A = 130) and a very red source, emitting most of its light in the mid-infrared owing to the production of lanthanides. These observations demonstrate that nucleosynthesis in GRBs can create r-process elements across a broad atomic mass range and play a central role in heavy-element nucleosynthesis across the Universe., (© 2023. The Author(s).)- Published
- 2024
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