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1. Validation of the dispositional adult hyperfocus questionnaire (AHQ-D)

Author

K. E. Hupfeld, J. B. Osborne, Q. T. Tran, H. W. Hyatt, T. R. Abagis, and P. Shah

Subjects
Adult hyperfocus questionnaire (AHQ), Hyperfocus, Flow, Attention-deficit/hyperactivity disorder (ADHD), Medicine, Science
Abstract

Abstract Hyperfocus (HF), or intense, deep concentration on a task, has gained significant research attention in recent years, particularly in regard to clinical populations such as Attention-Deficit/Hyperactivity Disorder (ADHD). The present work aims to provide validation of the 12-item dispositional adult hyperfocus questionnaire (AHQ-D) as a quantitative metric of HF in adults. We preregistered the study design and hypotheses. We administered the AHQ-D and several additional questionnaires to 347 adults (mean ± SD age: 33 ± 11 years; 47% female). Exploratory factor analysis revealed high factor loadings (0.57–0.81) on a single HF factor; item response theory analysis suggested that the questionnaire items had high discrimination and covered a wide range of responses; and we report strong internal consistency metrics (Cronbach’s alpha 0.93, mean split-half reliability 0.93). Replicating our previous work, HF was positively correlated with Conners’ Adult ADHD Rating Scale (CAARS) scores (r(345) = 0.53), suggesting that HF may be related to ADHD traits (though in this sample we did not specifically recruit individuals with ADHD). The AHQ-D demonstrated the hypothesized convergent validity; HF on the AHQ-D was positively correlated with HF measured using a different HF scale (r(344) = 0.69), as well as flow (r(345) = 0.12) and mind wandering (r(345) = 0.39) scores. AHQ-D HF scores showed a weak negative correlation with grit (r(345) = − 0.29). Though there was a weak negative correlation between HF and social desirability response tendency (r(345) = − 0.24), suggesting that those who care more about what others think may report less HF, there was no relationship between HF and extrasensory perception beliefs (r(345) = 0.01), suggesting that participants were not simply biased in their response tendencies. Taken together, we demonstrate strong scale metrics for the AHQ-D, the expected convergent validity, and a general lack of response bias, in addition to replicating our previous association of HF with ADHD traits. We suggest that the AHQ-D can be confidently used in future work as a valid way to measure HF in adults.

Published
2024
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2. Predictive Identification of At-Risk Students: Using Learning Management System Data

Author

J Bryan Osborne and Andrew S.I.D. Lang

Subjects
at-risk students, early detection, LMS data, machine learning, student retention, student success, Special aspects of education, LC8-6691
Abstract

This paper describes a neural network model that can be used to detect at-risk students failing a particular course using only grade book data from a learning management system. By analyzing data extracted from the learning management system at the end of week 5, the model can predict with an accuracy of 88% whether the student will pass or fail a specific course. Data from the grade books from all course shells from the Spring 2022 semester (N = 22,041 rows) were analyzed, and four factors were found to be significant predictors of student success/failure: the current course grade after the fifth week of the semester and the presence of missing grades in weeks 3, 4, and 5. Several models were investigated before concluding that a neural network model had the best overall utility for the purpose of an early alert system. By categorizing students who are predicted to fail more than one course as being generally at risk, we provide a metric for those who use early warning systems to target resources to the most at-risk students and intervene before students drop out. Seventy-four percent of the students whom our model classified as being generally at risk ended up failing at least one course.

Published
2023
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3. Swift/UVOT follow-up of gravitational wave alerts in the O3 era

Author

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

Published
2021
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5. Meta-analysis reveals that pollinator functional diversity and abundance enhance crop pollination and yield

Author

B. A. Woodcock, M. P. D. Garratt, G. D. Powney, R. F. Shaw, J. L. Osborne, J. Soroka, S. A. M. Lindström, D. Stanley, P. Ouvrard, M. E. Edwards, F. Jauker, M. E. McCracken, Y. Zou, S. G. Potts, M. Rundlöf, J. A. Noriega, A. Greenop, H. G. Smith, R. Bommarco, W. van der Werf, J. C. Stout, I. Steffan-Dewenter, L. Morandin, J. M. Bullock, and R. F. Pywell

Subjects
Science
Abstract

Pollinator communities could have nuanced effects on crop yield depending on their species and functional trait compositions. Here, the authors use a meta-analysis to show that, in addition to pollinator abundance, functional trait divergence also positively impacts yield of oilseed rape crops.

Published
2019
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6. A simple tool for refining GCM water availability projections, applied to Chinese catchments

Author

J. M. Osborne and F. H. Lambert

Subjects
Technology, Environmental technology. Sanitary engineering, TD1-1066, Geography. Anthropology. Recreation, Environmental sciences, GE1-350
Abstract

There is a growing desire for reliable 21st-century projections of water availability at the regional scale. Global climate models (GCMs) are typically used together with global hydrological models (GHMs) to generate such projections. GCMs alone are unsuitable, especially if they have biased representations of aridity. The Budyko framework represents how water availability varies as a non-linear function of aridity and is used here to constrain projections of runoff from GCMs, without the need for computationally expensive GHMs. Considering a Chinese case study, we first apply the framework to observations to show that the contribution of direct human impacts (water consumption) to the significant decline in Yellow River runoff was greater than the contribution of aridity change by a factor of approximately 2, although we are unable to rule out a significant contribution from the net effect of all other factors. We then show that the Budyko framework can be used to narrow the range of Yellow River runoff projections by 34 %, using a multi-model ensemble and the high-end Representative Concentration Pathway (RCP8.5) emissions scenario. This increases confidence that the Yellow River will see an increase in runoff due to aridity change by the end of the 21st century. Yangtze River runoff projections change little, since aridity biases in GCMs are less substantial. Our approach serves as a quick and inexpensive tool to rapidly update and correct projections from GCMs alone. This could serve as a valuable resource when determining the water management policies required to alleviate water stress for future generations.

Published
2018
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9. A real-time transient detector and the living Swift-XRT point source catalogue

Author

P A Evans, K L Page, A P Beardmore, R A J Eyles-Ferris, J P Osborne, S Campana, J A Kennea, and S B Cenko

Subjects
High Energy Astrophysical Phenomena (astro-ph.HE), Space and Planetary Science, FOS: Physical sciences, Astronomy and Astrophysics, Astrophysics - High Energy Astrophysical Phenomena
Abstract

We present the Living Swift-XRT Point Source catalogue (LSXPS) and real-time transient detector. This system allows us for the first time to carry out low-latency searches for new transient X-ray events fainter than those available to the current generation of wide-field imagers, and report their detection in near real-time. Previously, such events could only be found in delayed searches, e.g. of archival data; our low-latency analysis now enables rapid and ongoing follow up of these events, enabling the probing of timescales previously inaccessible. The LSXPS is, uniquely among X-ray catalogues, updated in near real-time, making this the first up-to-date record of the point sources detected by a sensitive X-ray telescope: the Swift-X-ray Telescope (XRT). The associated upper limit calculator likewise makes use of all available data allowing contemporary upper limits to be rapidly produced on-demand. These facilities, which enable the low-latency transient system are also fully available to the community, providing a powerful resource for time-domain and multi-messenger astrophysics., Comment: Replaced with post-refereeing accepted version of the paper. To appear in MNRAS. 12 pages, plus 18 of appendices. For the sake of rainforests, printing the appendices is not advised. For the sake of sanity, nor is reading them

Published
2022

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

Author

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

Subjects
Astronomy
Abstract

On 2020 February 24, during their third observing run (“O3”), the Laser Interferometer Gravitational-wave Observatory and Virgo Collaboration detected S200224ca: a candidate gravitational wave (GW) event produced by a binary black hole (BBH) merger. This event was one of the best-localized compact binary coalescences detected in O3 (with 50%/90% error regions of 13/72 deg2), and so the Neil Gehrels Swift Observatory performed rapid near-UV/X-ray follow-up observations. Swift-XRT and UVOT covered approximately 79.2% and 62.4% (respectively) of the GW error region, making S200224ca the BBH event most thoroughly followed-up in near-UV (u-band) and X-ray to date. No likely EM counterparts to the GW event were found by the Swift BAT, XRT, or UVOT, nor by other observatories. Here, we report on the results of our searches for an EM counterpart, both in the BAT data near the time of the merger, and in follow-up UVOT/XRT observations. We also discuss the upper limits we can place on EM radiation from S200224ca, as well as the implications these limits have on the physics of BBH mergers. Namely, we place a shallow upper limit on the dimensionless BH charge, qˆ < 1.4 x 10-4, and an upper limit on the isotropic-equivalent energy of a blast wave E<4.1×1051 erg (assuming typical GRB parameters).

Published
2021
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11. 2SXPS: An Improved and Expanded Swift X-Ray Telescope Point-source Catalog

Author

P. A. Evans, Kim Page, J. P. Osborne, A. P. Beardmore, R. Willingale, D. N. Burrows, J A Kennea, M. Perri, M. Capalbi, G. Tagliaferri, and S. B. Cenko

Subjects
Astronomy
Abstract

We present the 2SXPS (Swift-XRT Point Source) catalog, containing 206,335 point sources detected by the Swift X-ray Telescope (XRT) in the 0.3–10 keV energy range. This catalog represents a significant improvement over 1SXPS, with double the sky coverage (now 3790 deg2), and several significant developments in source detection and classification. In particular, we present for the first time techniques to model the effect of stray light—significantly reducing the number of spurious sources detected. These techniques will be very important for future, large effective area X-ray missions, such as the forthcoming Athena X-ray observatory. We also present a new model of the XRT point-spread function and a method for correctly localizing and characterizing piled-up sources. We provide light curves—in four energy bands, two hardness ratios, and two binning timescales—for every source, and from these deduce that over 80,000 of the sources in 2SXPS are variable in at least one band or hardness ratio. The catalog data can be queried or downloaded via a web interface at https://www.swift.ac.uk/2SXPS, via HEASARC, or in Vizier (IX/58).

Published
2020
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12. Fermi and Swift Observations of GRB 190114C: Tracing the Evolution of High-energy Emission from Prompt to Afterglow

Author

M. Ajello, M. Arimoto, M. Axelsson, L. Baldini, G. Barbiellini, D. Bastieri, R. Bellazzini, A. Berretta, E. Bissaldi, R. D. Blandford, R. Bonino, E. Bottacini, J. Bregeon, P. Bruel, R. Buehler, E. Burns, S. Buson, R. A. Cameron, R. Caputo, P. A. Caraveo, E. Cavazzuti, S. Chen, G. Chiaro, S. Ciprini, J. Cohen-Tanugi, D. Costantin, S. Cutini, F.D’Ammando, M. DeKlotz, P. de la Torre Luque, F. de Palma, A. Desai, N. Di Lalla, L. Di Venere, F. Fana Dirirsa, S. J. Fegan, A. Franckowiak, Y. Fukazawa, S. Funk, P. Fusco, F. Gargano, D. Gasparrini, N. Giglietto, R. Gill, F. Giordano, M. Giroletti, J. Granot, D. Green, I. A. Grenier, M.-H. Grondin, S. Guiriec, E. Hays, D. Horan, G. Jóhannesson, D. Kocevski, M. Kovac’evic’, M. Kuss, S. Larsson, L. Latronico, M. Lemoine-Goumard, J.Li, I. Liodakis, F. Longo, F. Loparco, M. N. Lovellette, P. Lubrano, S. Maldera, D. Malyshev, A. Manfreda, G. Martí-Devesa, M. N. Mazziotta, J. E. McEnery, I. Mereu, M. Meyer, P. F. Michelson, W. Mitthumsiri, T. Mizuno, M. E. Monzani, E. Moretti, A. Morselli, I. V. Moskalenko, M. Negro, E. Nuss, N. Omodei, M. Orienti, E. Orlando, M. Palatiello, V. S. Paliya, D. Paneque, Z. Pei, M. Persic, M. Pesce-Rollins, V. Petrosian, F. Piron, H. Poon, T. A. Porter, G. Principe, J. L. Racusin, S. Rainò, R. Rando, B. Rani, M. Razzano, S. Razzaque, A. Reimer, O. Reimer, F. Ryde, P. M. Saz Parkinson, D. Serini, C. Sgrò, E. J. Siskind, G. Spandre, P. Spinelli, H. Tajima, K. Takagi, M. N. Takahashi, D. Tak, J. B. Thayer, D. J. Thompson, D. F. Torres, E. Troja, J. Valverde, B. Van Klaveren, K. Wood, M. Yassine, G. Zaharijas, B. Mailyan, P. N. Bhat, M. S. Briggs, W. Cleveland, M. Giles, A. Goldstein, M. Hui, Christian Malacaria, R. Preece, O. J. Roberts, P. Veres, C. Wilson-Hodge, A. von Kienlin, S. B. Cenko, P. O’Brien, A. P. Beardmore, A. Lien, J. P. Osborne, A. Tohuvavohu, V. D’Elia, A.D’Aì, M. Perri, J. Gropp, N. Klingler, M. Capalbi, G. Tagliaferri, M. Stamatikos, and M. De Pasquale

Subjects
Astronomy
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 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
2020
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13. Observation of inverse Compton emission from a long γ-ray burst

Author

P. Veres, P. N. Bhat, M. S. Briggs, W. H. Cleveland, R. Hamburg, C. M. Hui, B. Mailyan, R. D. Preece, O. J. Roberts, A. von Kienlin, C. A. Wilson-Hodge, D. Kocevski, M. Arimoto, D. Tak, K. Asano, M. Axelsson, G. Barbiellini, E. Bissaldi, F.Fana Dirirsa, R. Gill, J. Granot, J. McEnery, N. Omodei, S. Razzaque, F. Piron, J. L. Racusin, D. J. Thompson, S. Campana, M. G. Bernardini, N. P. M. Kuin, M. H. Siegel, S. B. Cenko, P. O’Brien, M. Capalbi, A. Daì, M. De Pasquale, J. Gropp, N. Klingler, J. P. Osborne, M. Perri, R. L. C. Starling, G. Tagliaferri, A. Tohuvavohu, A. Ursi, M.Tavani, M. Cardillo, C. Casentini, G. Piano, Y. Evangelista, F. Verrecchia, C. Pittori, F. Lucarelli, A. Bulgarelli, N. Parmiggiani, G. E. Anderson, J. P. Anderson, G. Bernardi, J. Bolmer, M. D. Caballero-García, I. M. Carrasco, A. Castellón, N. Castro Segura, A. J. Castro-Tirado, S. V. Cherukuri, A. M. Cockeram, P. D’Avanzo, A. Di Dato, R. Diretse, R. P. Fender, E. Fernández-García, J. P. U. Fynbo, A. S.Fruchter, J. Greiner, M. Gromadzki, K. E. Heintz, I. Heywood, A. J. van der Horst, Y.-D. Hu, C. Inserra, L. Izzo, V. Jaiswal, P. Jakobsson, J. Japelj, E. Kankare, D. A.Kann, C. Kouveliotou, S. Klose, A. J. Levan, X. Y. Li, S. Lotti, K. Maguire, D. B. Malesani, I. Manulis, M. Marongiu, S. Martin, A. Melandri, M. J.Michałowski, J. C. A. Miller-Jones, K. Misra, A. Moin, K. P. Mooley, S. Nasri, M. Nicholl, A. Noschese, G. Novara, S. B. Pandey, E. Peretti, C. J. Pérez del Pulgar, M. A. Pérez-Torres, D. A. Perley, L. Piro, F. Ragosta, L. Resmi, R. Ricci, A. Rossi, R. Sánchez-Ramírez, J. Selsing, S. Schulze, S. J. Smartt, I. A. Smith, V. V. Sokolov, J. Stevens, N. R. Tanvir, C. C. Thöne, A. Tiengo, E. Tremou, E. Troja, A. de Ugarte Postigo, A. F. Valeev, S. D. Vergani, M. Wieringa, P. A. Woudt, D. Xu, O. Yaron, D. R. Young, V. A. Acciari, S. Ansoldi, L. A. Antonelli, A. Arbet Engels, D. Baack, A. Babić, B. Banerjee, U. Barres de Almeida, J. A. Barrio, J. Becerra González, W. Bednarek, L. Bellizzi, E. Bernardini, A. Berti, J. Besenrieder, W. Bhattacharyya, C. Bigongiari, A. Biland, O. Blanch, G. Bonnoli, Ž. Bošnjak, G. Busetto, R. Carosi, G. Ceribella, Y. Chai, A. Chilingaryan, S. Cikota, S. M. Colak, U. Colin, E. Colombo, J. L. Contreras, J. Cortina, S. Covino, V. D’Elia, P. Da Vela, F. Dazzi, A. De Angelis, B. De Lotto, M. Delfino, J. Delgado, D. Depaoli, F. Di Pierro, L. Di Venere, E. Do Souto Espiñeira, D. Dominis Prester, A. Donini, D. Dorner, M. Doro, D. Elsaesser, V. Fallah Ramazani, A. Fattorini, G. Ferrara, D. Fidalgo, L. Foffano, M. V. Fonseca, L. Font, C. Fruck, S. Fukami, R. J. García López, M. Garczarczyk, S.Gasparyan, M. Gaug, N. Giglietto, F. Giordano, N. Godinović, D. Green, D. Guberman, D. Hadasch, A. Hahn, J. Herrera, J. Hoang, D. Hrupec, M. Hütten, T. Inada, S. Inoue, K. Ishio, Y. Iwamura, L. Jouvin, D. Kerszberg, H. Kubo, J. Kushida, A. Lamastra, D. Lelas, F. Leone, E. Lindfors, S. Lombardi, F. Longo, M. López, R. López-Coto, A. López-Oramas, S. Loporchio, B. Machado de Oliveira Fraga, C. Maggio, P. Majumdar, M. Makariev, M. Mallamaci, G. Maneva, M. Manganaro, K. Mannheim, L. Maraschi, M. Mariotti, M. Martínez, D. Mazin, S. Mićanović, D. Miceli, M. Minev, J. M. Miranda, R. Mirzoyan, E. Molina, A. Moralejo, D. Morcuende, V. Moreno, E. Moretti, P. Munar-Adrover, V. Neustroev, C. Nigro, K. Nilsson, D. Ninci, K. Nishijima, K. Noda, L. Nogués, S. Nozaki, S. Paiano, M. Palatiello, D. Paneque, R. Paoletti, J. M. Paredes, P. Peñil, M. Peresano, M. Persic, P. G. Prada Moroni, E. Prandini, I. Puljak, W. Rhode, M. Ribó, J. Rico, C. Righi, A. Rugliancich, L. Saha, N. Sahakyan, T. Saito, S. Sakurai, K. Satalecka, K. Schmidt, T. Schweizer, J. Sitarek, I. Šnidarić, D. Sobczynska, A. Somero, A. Stamerra, D. Strom, M. Strzys, Y. Suda, T. Surić, M. Takahashi, F. Tavecchio, P. Temnikov, T. Terzić, M. Teshima, N. Torres-Albà, L. Tosti, V. Vagelli, J. van Scherpenberg, G. Vanzo, M. Vazquez Acosta, C. F. Vigorito, V. Vitale, I. Vovk, M. Will, D. Zarić, and L. Nava

Subjects
Space Sciences (General)
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 emission. 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 bands. The afterglow emission is generally well explained as synchrotron radiation emitted by electrons accelerated by the external shock. Recently, intense long-lasting emission between 0.2 and 1 teraelectronvolts was observed from GRB 190114C. Here we report multifrequency 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 10^(12) 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.

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

Author

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, C. Gronwall, D. H. Hartmann, H. A. Krimm, N. P. M. Kuin, A. Lien, D. B. Malesani, F. E. Marshall, A. Melandri, J. A. Nousek, S. R. Oates, P. T. O’Brien, J. P. Osborne, K. L. Page, D. M. Palmer, M. Perri, J. L. Racusin, M. H. Siegel, T. Sakamoto, B. Sbarufatti, Gianpiero Tagliaferri, and E. Troja

Subjects
Astrophysics, Astronomy
Abstract

The Neil Gehrels Swift Observatory carried out prompt searches for gravitational-wave (GW) events detected by the LIGO/Virgo Collaboration (LVC) during the second observing run ("O2"). Swift performed extensive tiling of eight LVC triggers, two of which had very low false-alarm rates (GW170814 and the epochal GW170817), indicating a high confidence of being astrophysical in origin; the latter was the first GW event to have an electromagnetic counterpart detected. In this paper we describe the follow-up performed during O2 and the results of our searches. No GW electromagnetic counterparts were detected; this result is expected, as GW170817 remained the only astrophysical event containing at least one neutron star after LVC's later retraction of some events. A number of X-ray sources were detected, with the majority of identified sources being active galactic nuclei. We discuss the detection rate of transient X-ray sources and their implications in the O2 tiling searches. Finally, we describe the lessons learned during O2 and how these are being used to improve the Swift follow-up of GW events. In particular, we simulate a population of gamma-ray burst afterglows to evaluate our source ranking system's ability to differentiate them from unrelated and uncataloged X-ray sources. We find that ≈60%–70% of afterglows whose jets are oriented toward Earth will be given high rank (i.e., "interesting" designation) by the completion of our second follow-up phase (assuming that their location in the sky was observed), but that this fraction can be increased to nearly 100% by performing a third follow-up observation of sources exhibiting fading behavior.

Published
2019
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15. Constraints on the X-ray luminosity function of AGN at z = 5.7–6.4 with the Extragalactic Serendipitous Swift Survey

Author

C L Barlow-Hall, J Delaney, J Aird, P A Evans, J P Osborne, and M G Watson

Subjects
High Energy Astrophysical Phenomena (astro-ph.HE), Astrophysics::High Energy Astrophysical Phenomena, supermassive black holes [quasars], FOS: Physical sciences, Astronomy and Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, luminosity function, mass function [galaxies], Astrophysics - Astrophysics of Galaxies, galaxies [X-rays], Space and Planetary Science, Astrophysics of Galaxies (astro-ph.GA), active [galaxies], Astrophysics - High Energy Astrophysical Phenomena, Astrophysics::Galaxy Astrophysics, evolution [galaxies]
Abstract

X-ray luminosity functions (XLFs) of Active Galactic Nuclei (AGN) trace the growth and evolution of supermassive black hole populations across cosmic time, however, current XLF models are poorly constrained at redshifts of z>6, with a lack of spectroscopic constraints at these high redshifts. In this work we \redit{place limits} on the bright-end of the XLF at z=5.7-6.4 using high-redshift AGN identified within the Extragalactic Serendipitous Swift Survey (ExSeSS) catalogue. Within ExSeSS we find one serendipitously X-ray detected z>6 AGN, ATLAS J025.6821-33.4627, with an X-ray luminosity of $L_\mathrm{X}=8.47^{+3.40}_{-3.13}\times10^{44}\mathrm{erg.s^{-1}}$ and $z=6.31\pm0.03$ making it the highest redshift, spectroscopically confirmed, serendipitously X-ray detected quasar known to date. We also calculate an upper limit on the space density at higher luminosities where no additional sources are found, enabling us to place constraints on the shape of the XLF. Our results are consistent with the rapid decline in the space densities of high-luminosity AGN toward high redshift as predicted by extrapolations of existing parametric models of the XLF. We also find that our X-ray based measurements are consistent with estimates of the bolometric quasar luminosity function based on UV measurements at $z\gtrsim6$, although they require a large X-ray to bolometric correction factor at these high luminosities., 10pages, 6 figures. Resubmitted to MNRAS, following referee comments

Published
2023

16. The 2021 outburst of the recurrent nova RS Ophiuchi observed in X-rays by the Neil Gehrels Swift Observatory: a comparative study

Author

K L Page, A P Beardmore, J P Osborne, U Munari, J-U Ness, P A Evans, M F Bode, M J Darnley, J J Drake, N P M Kuin, T J O’Brien, M Orio, S N Shore, S Starrfield, and C E Woodward

Subjects
High Energy Astrophysical Phenomena (astro-ph.HE), Space and Planetary Science, individual: RS Oph [stars], novae, cataclysmic variables, FOS: Physical sciences, Astronomy and Astrophysics, Astrophysics - High Energy Astrophysical Phenomena, QC, QB, stars [X-rays]
Abstract

On 2021 August 8, the recurrent nova RS Ophiuchi erupted again, after an interval of 15.5 yr. Regular monitoring by the Neil Gehrels Swift Observatory began promptly, on August 9.9 (0.37 day after the optical peak), and continued until the source passed behind the Sun at the start of November, 86 days later. Observations then restarted on day 197, once RS Oph emerged from the Sun constraint. This makes RS Oph the first Galactic recurrent nova to have been monitored by Swift throughout two eruptions. Here we investigate the extensive X-ray datasets from 2006 and 2021, as well as the more limited data collected by EXOSAT in 1985. The hard X-rays arising from shock interactions between the nova ejecta and red giant wind are similar following the last two eruptions. In contrast, the early super-soft source (SSS) in 2021 was both less variable and significantly fainter than in 2006. However, 0.3-1 keV light-curves from 2021 reveal a 35 s quasi-periodic oscillation consistent in frequency with the 2006 data. The Swift X-ray spectra from 2021 are featureless, with the soft emission typically being well parametrized by a simple blackbody, while the 2006 spectra showed much stronger evidence for superimposed ionized absorption edges. Considering the data after day 60 following each eruption, during the supersoft phase the 2021 spectra are hotter, with smaller effective radii and lower wind absorption, leading to an apparently reduced bolometric luminosity. We explore possible explanations for the gross differences in observed SSS behaviour between the 2006 and 2021 outbursts., 21 pages, 16 colour figures, accepted for publication in MNRAS. Table 1 in full is included as an ancillary PDF (will be supplementary online material when published by MNRAS)

Published
2022

17. The 2019 eruption of recurrent nova V3890 Sgr: observations by Swift, NICER, and SMARTS

Author

A. P. Beardmore, N. P. M. Kuin, J. P. Osborne, J. U. Ness, F. M. Walter, C. B. Markwardt, Marina Orio, Kirill Sokolovsky, and K. L. Page

Subjects
High Energy Astrophysical Phenomena (astro-ph.HE), Physics, 010504 meteorology & atmospheric sciences, Red giant, Astrophysics::High Energy Astrophysical Phenomena, FOS: Physical sciences, White dwarf, Astronomy and Astrophysics, Astrophysics, 01 natural sciences, Spectral line, Amplitude, 13. Climate action, Space and Planetary Science, Observatory, 0103 physical sciences, Astrophysics::Solar and Stellar Astrophysics, Black-body radiation, Emission spectrum, Astrophysics - High Energy Astrophysical Phenomena, Ejecta, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, 0105 earth and related environmental sciences
Abstract

V3890 Sgr is a recurrent nova which has been seen in outburst three times so far, with the most recent eruption occurring on 2019 August 27 UT. This latest outburst was followed in detail by the Neil Gehrels Swift Observatory, from less than a day after the eruption until the nova entered the Sun observing constraint, with a small number of additional observations after the constraint ended. The X-ray light-curve shows initial hard shock emission, followed by an early start of the super-soft source phase around day 8.5, with the soft emission ceasing by day 26. Together with the peak blackbody temperature of the super-soft spectrum being ~100 eV, these timings suggest the white dwarf mass to be high, ~1.3 M_sun. The UV photometric light-curve decays monotonically, with the decay rate changing a number of times, approximately simultaneously with variations in the X-ray emission. The UV grism spectra show both line and continuum emission, with emission lines of N, C, Mg and O being notable. These UV spectra are best dereddened using an SMC extinction law. Optical spectra from SMARTS show evidence of interaction between the nova ejecta and wind from the donor star, as well as the extended atmosphere of the red giant being flash-ionized by the super-soft X-ray photons. Data from NICER reveal a transient 83 s quasi-periodic oscillation, with a modulation amplitude of 5 per cent, adding to the sample of novae which show such short variabilities during their super-soft phase., Comment: 20 pages, 13 figures (9 in colour). The full version of Table 2 is provided as a PDF within the source file download

Published
2020

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

Author

M. H. Siegel, J. A. Kennea, M. J. Page, E. Troja, Dieter H. Hartmann, B. Sbarufatti, P. T. O'Brien, M. Perri, T. Sakamoto, Regina Caputo, S. R. Oates, Phil Evans, N. P. M. Kuin, P. D'Avanzo, Hans A. Krimm, D. Malesani, Paolo Giommi, Valerio D'Elia, Peter J. Brown, N. J. Klingler, Scott Barthelmy, Giancarlo Cusumano, S. B. Cenko, J. L. Racusin, M. G. Bernardini, Sergio Campana, David Palmer, M. de Pasquale, E. Ambrosi, C. Pagani, A. Melandri, David N. Burrows, S. W. K. Emery, J. A. Nousek, A. A. Breeveld, Antonino D'Ai, Caryl Gronwall, F. E. Marshall, Gianpiero Tagliaferri, A. P. Beardmore, Joshua E. Schlieder, A. Tohuvavohu, J. P. Osborne, and K. L. Page

Subjects
High Energy Astrophysical Phenomena (astro-ph.HE), Physics, Gravitational wave, FOS: Physical sciences, Binary number, Astronomy and Astrophysics, Astrophysics, LIGO, Neutron star, Wavelength, Binary black hole, Space and Planetary Science, Observatory, general [X-rays], ROSAT, Astrophysics - High Energy Astrophysical Phenomena
Abstract

The Neil Gehrels Swift Observatory followed up 18 gravitational wave (GW) triggers from the LIGO/Virgo collaboration during the O3 observing run in 2019/2020, performing approximately 6500 pointings in total. Of these events, four were finally classified (if real) as binary black hole (BH) triggers, six as binary neutron star (NS) events, two each of NSBH and Mass Gap triggers, one an unmodelled (Burst) trigger, and the remaining three were subsequently retracted. Thus far, four of these O3 triggers have been formally confirmed as real gravitational wave events. While no likely electromagnetic counterparts to any of these GW events have been identified in the X-ray data (to an average upper limit of 3.60 x 10^{-12} erg cm^{-2} s^{-1} over 0.3-10 keV), or at other wavelengths, we present a summary of all the Swift-XRT observations performed during O3, together with typical upper limits for each trigger observed. The majority of X-ray sources detected during O3 were previously uncatalogued; while some of these will be new (transient) sources, others are simply too faint to have been detected by earlier survey missions such as ROSAT. The all-sky survey currently being performed by eROSITA will be a very useful comparison for future observing runs, reducing the number of apparent candidate X-ray counterparts by up to 95 per cent., Comment: 23 pages (including 4 pages of references, and a 4 page table in the appendix), 5 figures (4 in colour), accepted for publication in MNRAS. (Replaced due to annoying spelling typo in the abstract.)

Published
2020

19. High Resolution X-ray Spectra of RS Ophiuchi (2006 and 2021): Revealing the cause of SSS variability

Author

J.-U. Ness, A. P. Beardmore, M. F. Bode, M. J. Darnley, A. Dobrotka, J. J. Drake, J. Magdolen, U. Munari, J. P. Osborne, M. Orio, K. L. Page, and S. Starrfield

Subjects
High Energy Astrophysical Phenomena (astro-ph.HE), Astrophysics - Solar and Stellar Astrophysics, Space and Planetary Science, FOS: Physical sciences, Astronomy and Astrophysics, Astrophysics - High Energy Astrophysical Phenomena, Solar and Stellar Astrophysics (astro-ph.SR)
Abstract

Context. The ~ 10–20 yr recurrent symbiotic nova RS Oph exploded on 2021 August 9, the seventh confirmed recorded outburst since 1898. During the previous outburst in 2006, the current fleet of X-ray space observatories was already in operation, and thanks to the longevity of Swift, XMM-Newton, and Chandra, a direct comparison between these two outbursts is possible. The Swift monitoring campaign revealed similar behaviour during the early shock phase but very different behaviour during the super-soft source (SSS) phase. Two XMM-Newton observations were made during the 2021 SSS phase on days 37.1 and 55.6 after the 2021 optical peak. We focus in this work on the bright SSS observation on day 55.6 and compare to SSS Chandra and XMM-Newton grating observations made on days 39.7, 54, and 66.9 after the 2006 optical peak. Aims. By exploring the reasons for the differences between the 2006 and 2021 outbursts, we aim to obtain a better general understanding of the emission and absorption mechanisms. While the emission mechanisms hold the key to the physics of novae and nuclear burning, absorption processes may dominate what we observe, and we aim to explore the cause of the gross initial variability in the observed SSS emission. Methods. We present a novel approach to down-scaling the observed (brighter) 2006 SSS spectra to match the 2021 day 55.6 spectrum by parameter optimisation of: (1) a constant factor (representing fainter source emission, smaller radius, eclipses, etc.), (2) a multi-ionisation photoelectric absorption model (representing different line-of-sight absorption), and (3) scaling with a ratio of two blackbody models with different effective temperatures (representing different brightness and colours). This model approach does not depend on a source model assuming the intrinsic source to be the same. It is therefore more sensitive to incremental changes than modelling approaches where source and absorption are modelled simultaneously. Results. The 2021d55.6 spectrum can be reproduced remarkably well by multiplying the (brighter) 2006d39.7 and 2006d54 spectra with the absorption model, while the 2006d66.9 spectrum requires additional colour changes to match the 2021.d55.6 spectrum. The 2006d39.7 spectrum much more closely resembles the 2021d55.6 spectrum in shape and structure than the same-epoch 2006d54 spectrum: The spectra on days 2006d39.7 and 2021d55.6 are richer in absorption lines with a deeper O I absorption edge, and blueshifts are higher (~1200 km s−1) than on day 2006d54 (~700 km s−1). In the SSS light curves on days 2006d39.7, 2006d54, and 2021d55.6, brightness and hardness variations are correlated, indicating variations of the O I column density. Only on day 2006d39.7, a 1000 s lag is observed. The 35 s period was detected on day 2021d55.6 with lower significance compared to 2006d54. Conclusions. We conclude that the central radiation source is the same, while absorption is the principal reason for observing lower soft-X-ray emission in 2021 than in 2006. This is consistent with a similar 2006 and 2021 [Fe X] line-flux evolution. We explain the reduction in line blueshift, depth in O I edge, and number of absorption lines from day 2006d39.7 to 2006d54 by deceleration and heating of the ejecta within the stellar wind of the companion. In 2021, less such deceleration and heating was observed, which we interpret as due to viewing at different angles through an inhomogeneous density distribution of the stellar wind, allowing free expansion in some directions (probed in 2021) and a higher degree of deceleration in others (probed in 2006). The higher absorption in 2021 can then be explained by the lower-temperature absorbing plasma being more opaque to soft X-rays. Our approach of scaling observations against observations is free of ambiguities from imperfect source models and can be applied to other grating spectra with complex continuum sources.

Published
2022
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20. First Wide Field-of-view X-Ray Observations by a Lobster-eye Focusing Telescope in Orbit

Author

C. Zhang, Z. X. Ling, X. J. Sun, S. L. Sun, Y. Liu, Z. D. Li, Y. L. Xue, Y. F. Chen, Y. F. Dai, Z. Q. Jia, H. Y. Liu, X. F. Zhang, Y. H. Zhang, S. N. Zhang, F. S. Chen, Z. W. Cheng, W. Fu, Y. X. Han, H. Li, J. F. Li, Y. Li, P. R. Liu, X. H. Ma, Y. J. Tang, C. B. Wang, R. J. Xie, A. L. Yan, Q. Zhang, B. W. Jiang, G. Jin, L. H. Li, X. B. Qiu, D. T. Su, J. N. Sun, Z. Xu, S. K. Zhang, Z. Zhang, N. Zhang, X. Z. Bi, Z. M. Cai, J. W. He, H. Q. Liu, X. C. Zhu, H. Q. Cheng, C. Z. Cui, D. W. Fan, H. B. Hu, M. H. Huang, C. C. Jin, D. Y. Li, H. W. Pan, W. X. Wang, Y. F. Xu, X. Yang, B. Zhang, M. Zhang, W. D. Zhang, D. H. Zhao, M. Bai, Z. Ji, Y. R. Liu, F. L. Ma, J. Su, J. Z. Tong, Y. S. Wang, Z. J. Zhao, C. Feldman, P. O’Brien, J. P. Osborne, R. Willingale, V. Burwitz, G. Hartner, A. Langmeier, T. Müller, S. Rukdee, T. Schmidt, E. Kuulkers, and W. Yuan

Subjects
High Energy Astrophysical Phenomena (astro-ph.HE), Space and Planetary Science, FOS: Physical sciences, Astronomy and Astrophysics, Astrophysics - High Energy Astrophysical Phenomena, Astrophysics - Instrumentation and Methods for Astrophysics, Instrumentation and Methods for Astrophysics (astro-ph.IM)
Abstract

As a novel X-ray focusing technology, lobster eye micro-pore optics (MPO) feature both a wide observing field of view and true imaging capability, promising sky monitoring with significantly improved sensitivity and spatial resolution in soft X-rays. Since first proposed by Angel (1979), the optics have been extensively studied, developed and trialed over the past decades. In this Letter, we report on the first-light results from a flight experiment of the Lobster Eye Imager for Astronomy ($LEIA$), a pathfinder of the wide-field X-ray telescope of the Einstein Probe mission. The piggyback imager, launched in July 2022, has a mostly un-vignetted field of view of $18.6^\circ \times 18.6^\circ $. Its spatial resolution is in the range of 4$-$7 arcmin in FWHM and the focal spot effective area is 2$-$3 cm$^2$, both showing only mild fluctuations across the field of view. We present images of the Galactic center region, Sco X-1 and the diffuse Cygnus Loop nebular taken in snapshot observations over 0.5$-$4 keV. These are truly wide-field X-ray images of celestial bodies observed, for the first time, by a focusing imaging telescope. Initial analyses of the in-flight data show excellent agreement between the observed images and the on-ground calibration and simulations. The instrument and its characterization are briefly described, as well as the flight experiment. The results provide a solid basis for the development of the present and proposed wide-field X-ray missions using lobster eye MPO., Comment: 11 pages, 4 figures. Accepted for publication in Astrophysical Journal Letter

Published
2022

21. Swift follow-up of gravitational wave triggers: results from the first aLIGO run and optimization for the future

Author

P. A. Evans, J. A. Kennea, D. M. Palmer, M. Bilicki, J. P. Osborne, P. T. O'Brien, N. R. Tanvir, A. Y. Lien, S. D. Barthelmy, D. N. Burrows, S. Campana, S. B. Cenko, V. D'Elia, N. Gehrels, F. E. Marshall, K. L. Page, M. Perri, B. Sbarufatti, M. H. Siegel, G. Tagliaferri, and E. Troja

Subjects
Astronomy
Abstract

During its first observing run, in late 2015, the advanced Laser Interferometer Gravitational-wave Observatory facility announced three gravitational wave (GW) triggers to electromagnetic follow-up partners. Two of these have since been confirmed as being of astrophysical origin: both are binary black hole mergers at ∼500 Mpc; the other trigger was later found not to be astrophysical. In this paper, we report on the Swift follow-up observations of the second and third triggers, including details of 21 X-ray sources detected; none of which can be associated with the GW event. We also consider the challenges that the next GW observing run will bring as the sensitivity and hence typical distance of GW events will increase. We discuss how to effectively use galaxy catalogues to prioritize areas for follow-up, especially in the presence of distance estimates from the GW data. We also consider two galaxy catalogues and suggest that the high completeness at larger distances of the 2MASS Photometric Redshift catalogue makes it very well suited to optimize Swift follow-up observations.

Published
2016
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22. Gamma ray burst studies with THESEUS

Author

Lara Nava, Gor Oganesyan, Lorenzo Amati, Diego Götz, Enrico Bozzo, Giancarlo Ghirlanda, P. T. O'Brien, M. Topinka, S. Ascenzi, M. E. Ravasio, A. Melandri, Sandro Mereghetti, A. E. Camisasca, M. Hafizi, M. Toffano, Andrew Blain, Giulia Stratta, Silvia Zane, A. I. Bogomazov, S. Ronchini, Piero Rosati, Ruben Salvaterra, E. Le Floc'h, Marica Branchesi, P. D'Avanzo, M. G. Bernardini, A. J. Castro-Tirado, S. D. Vergani, Nial R. Tanvir, J. P. Osborne, S. Mandhai, C. Guidorzi, Asaf Pe'er, Istituto Nazionale di Astrofisica, Ghirlanda, G, Salvaterra, R, Toffano, M, Ronchini, S, Guidorzi, C, Oganesyan, G, Ascenzi, S, Bernardini, M, Camisasca, A, Mereghetti, S, Nava, L, Ravasio, M, Branchesi, M, Castro-Tirado, A, Amati, L, Blain, A, Bozzo, E, O'Brien, P, Gotz, D, Le Floch, E, Osborne, J, Rosati, P, Stratta, G, Tanvir, N, Bogomazov, A, D'Avanzo, P, Hafizi, M, Mandhai, S, Melandri, A, Peer, A, Topinka, M, Vergani, S, Zane, S, Astrophysique Interprétation Modélisation (AIM (UMR7158 / UMR_E_9005 / UM_112)), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Galaxies, Etoiles, Physique, Instrumentation (GEPI), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS), 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), and Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS)

Subjects
Gamma ray burst, Jet structure, Astrophysics::High Energy Astrophysical Phenomena, FOS: Physical sciences, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, Gamma ray bursts, Synchrotron radiation, Jet structure, Spectral line, Gamma ray bursts, NO, Astrophysical jet, 0103 physical sciences, Emission spectrum, [PHYS.PHYS.PHYS-INS-DET]Physics [physics]/Physics [physics]/Instrumentation and Detectors [physics.ins-det], 010306 general physics, 010303 astronomy & astrophysics, Instrumentation and Methods for Astrophysics (astro-ph.IM), Luminosity function, Astrophysics::Galaxy Astrophysics, Physics, Synchrotron radiation, Astronomy and Astrophysics, Redshift, Afterglow, Stars, Space and Planetary Science, Gamma-ray burst, Astrophysics - Instrumentation and Methods for Astrophysics
Abstract

Gamma-ray Bursts (GRBs) are the most powerful transients in the Universe, over-shining for a few seconds all other $\gamma$-ray sky sources. Their emission is produced within narrowly collimated relativistic jets launched after the core-collapse of massive stars or the merger of compact binaries. THESEUS will open a new window for the use of GRBs as cosmological tools by securing a statistically significant sample of high-$z$ GRBs, as well as by providing a large number of GRBs at low-intermediate redshifts extending the current samples to low luminosities. The wide energy band and unprecedented sensitivity of the Soft X-ray Imager (SXI) and X-Gamma rays Imaging Spectrometer (XGIS) instruments provide us a new route to unveil the nature of the prompt emission. For the first time, a full characterisation of the prompt emission spectrum from 0.3 keV to 10 MeV with unprecedented large count statistics will be possible revealing the signatures of synchrotron emission. SXI spectra, extending down to 0.3 keV, will constrain the local metal absorption and, for the brightest events, the progenitors' ejecta composition. Investigation of the nature of the internal energy dissipation mechanisms will be obtained through the systematic study with XGIS of the sub-second variability unexplored so far over such a wide energy range. THESEUS will follow the spectral evolution of the prompt emission down to the soft X-ray band during the early steep decay and through the plateau phase with the unique ability of extending above 10 keV the spectral study of these early afterglow emission phases., Comment: Submitted to Experimental Astronomy

Published
2021

23. Swift spectra of AT2018cow: a white dwarf tidal disruption event?

Author

Craig B. Markwardt, S. Bradley Cenko, N. Paul M. Kuin, J. A. Kennea, S. R. Oates, Sam Emery, A. Y. Lien, Eleonora Troja, Kinwah Wu, Andrew J. Levan, Michael H. Siegel, Qin Han, J. P. Osborne, A. Tohuvavohu, Massimiliano De Pasquale, Mat Page, K. L. Page, Peter J. Brown, A. A. Breeveld, Sergio Campana, David N. Burrows, B. Sbarufatti, ITA, USA, GBR, and TUR

Subjects
Opacity, Infrared, Astrophysics::High Energy Astrophysical Phenomena, FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, 01 natural sciences, Spectral line, Tidal disruption event, 0103 physical sciences, Astrophysics::Solar and Stellar Astrophysics, 010303 astronomy & astrophysics, Solar and Stellar Astrophysics (astro-ph.SR), Astrophysics::Galaxy Astrophysics, Line (formation), High Energy Astrophysical Phenomena (astro-ph.HE), Physics, Photosphere, 010308 nuclear & particles physics, White dwarf, Astronomy and Astrophysics, Galaxy, Astrophysics - Solar and Stellar Astrophysics, 13. Climate action, Space and Planetary Science, Astrophysics::Earth and Planetary Astrophysics, Astrophysics - High Energy Astrophysical Phenomena
Abstract

The bright transient AT2018cow has been unlike any other known type of transient. Its high brightness, rapid rise and decay and initially nearly featureless spectrum are unprecedented and difficult to explain using models for similar burst sources. We present evidence for faint gamma-ray emission continuing for at least 8 days, and featureless spectra in the ultraviolet bands -- both unusual for eruptive sources. The X-ray variability of the source has a burst-like character. The UV-optical spectrum does not show any CNO line but is well described by a blackbody. We demonstrate that a model invoking the tidal disruption of a 0.1 - 0.4 Msun Helium White Dwarf (WD) by a 100,000 to one million solar mass Black Hole (BH) located in the outskirts of galaxy Z~137-068 could provide an explanation for most of the characteristics shown in the multi-wavelength observations. A blackbody-like emission is emitted from an opaque photosphere, formed by the debris of the WD disruption. Broad features showing up in the optical/infrared spectra in the early stage are probably velocity broadened lines produced in a transient high-velocity outward moving cocoon. The asymmetric optical/infrared lines that appeared at a later stage are emission from an atmospheric layer when it detached from thermal equilibrium with the photosphere, which undergoes more rapid cooling. The photosphere shrinks when its temperature drops, and the subsequent infall of the atmosphere produced asymmetric line profiles. Additionally, a non-thermal jet might be present, emitting X-rays in the 10-150 keV band.

Published
2019

24. The semen microbiome and its relationship with local immunology and viral load in HIV infection.

Author

Cindy M Liu, Brendan J W Osborne, Bruce A Hungate, Kamnoosh Shahabi, Sanja Huibner, Richard Lester, Michael G Dwan, Colin Kovacs, Tania L Contente-Cuomo, Erika Benko, Maliha Aziz, Lance B Price, and Rupert Kaul

Subjects
Immunologic diseases. Allergy, RC581-607, Biology (General), QH301-705.5
Abstract

Semen is a major vector for HIV transmission, but the semen HIV RNA viral load (VL) only correlates moderately with the blood VL. Viral shedding can be enhanced by genital infections and associated inflammation, but it can also occur in the absence of classical pathogens. Thus, we hypothesized that a dysregulated semen microbiome correlates with local HIV shedding. We analyzed semen samples from 49 men who have sex with men (MSM), including 22 HIV-uninfected and 27 HIV-infected men, at baseline and after starting antiretroviral therapy (ART) using 16S rRNA gene-based pyrosequencing and quantitative PCR. We studied the relationship of semen bacteria with HIV infection, semen cytokine levels, and semen VL by linear regression, non-metric multidimensional scaling, and goodness-of-fit test. Streptococcus, Corynebacterium, and Staphylococcus were common semen bacteria, irrespective of HIV status. While Ureaplasma was the more abundant Mollicutes in HIV-uninfected men, Mycoplasma dominated after HIV infection. HIV infection was associated with decreased semen microbiome diversity and richness, which were restored after six months of ART. In HIV-infected men, semen bacterial load correlated with seven pro-inflammatory semen cytokines, including IL-6 (p = 0.024), TNF-α (p = 0.009), and IL-1b (p = 0.002). IL-1b in particular was associated with semen VL (r(2) = 0.18, p = 0.02). Semen bacterial load was also directly linked to the semen HIV VL (r(2) = 0.15, p = 0.02). HIV infection reshapes the relationship between semen bacteria and pro-inflammatory cytokines, and both are linked to semen VL, which supports a role of the semen microbiome in HIV sexual transmission.

Published
2014
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25. Swift multiwavelength follow-up of LVC S200224ca and the implications for binary black hole mergers

Author

S. R. Oates, Antonino D'Ai, K. L. Page, P. T. O'Brien, Caryl Gronwall, Sergio Campana, Gianpiero Tagliaferri, Scott Barthelmy, J. A. Kennea, N. P. M. Kuin, Michael H. Siegel, Phil Evans, David Palmer, B. Sbarufatti, M. J. Page, Paolo Giommi, Valerio D'Elia, Javier A. García, S. W. K. Emery, Peter J. Brown, Bing Zhang, M. de Pasquale, Noel Klingler, Frank Marshall, Dieter H. Hartmann, M. Perri, Giancarlo Cusumano, A. Y. Lien, Eleonora Troja, A. P. Beardmore, Joshua E. Schlieder, David N. Burrows, A. Tohuvavohu, A. A. Breeveld, Maria Grazia Bernardini, J. P. Osborne, Hans A. Krimm, A. Melandri, J. A. Nousek, Judith Racusin, D. B. Malesani, P. D'Avanzo, T. Sakamoto, and S. B. Cenko

Subjects
Physics, High Energy Astrophysical Phenomena (astro-ph.HE), X-ray astronomy, 010504 meteorology & atmospheric sciences, Gravitational wave, High-energy astronomy, Astrophysics::High Energy Astrophysical Phenomena, FOS: Physical sciences, Astronomy and Astrophysics, Astrophysics, Gamma-ray astronomy, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, Binary black hole, Space and Planetary Science, Observatory, 0103 physical sciences, Astrophysics - High Energy Astrophysical Phenomena, Gamma-ray burst, 010303 astronomy & astrophysics, 0105 earth and related environmental sciences, Dimensionless quantity
Abstract

On 2020 February 24, during their third observing run ("O3"), the Laser Interferometer Gravitational-wave Observatory and Virgo Collaboration (LVC) detected S200224ca: a candidate gravitational wave (GW) event produced by a binary black hole (BBH) merger. This event was one of the best-localized compact binary coalescences detected in O3 (with 50%/90% error regions of 13/72 deg$^2$), and so the Neil Gehrels Swift Observatory performed rapid near-UV/X-ray follow-up observations. Swift-XRT and UVOT covered approximately 79.2% and 62.4% (respectively) of the GW error region, making S200224ca the BBH event most thoroughly followed-up in near-UV (u-band) and X-ray to date. No likely EM counterparts to the GW event were found by the Swift BAT, XRT, or UVOT, nor by other observatories. Here we report on the results of our searches for an EM counterpart, both in the BAT data near the time of the merger, and in follow-up UVOT/XRT observations. We also discuss the upper limits we can place on EM radiation from S200224ca, and the implications these limits have on the physics of BBH mergers. Namely, we place a shallow upper limit on the dimensionless BH charge, $\hat{q} < 1.4 \times10^{-4}$, and an upper limit on the isotropic-equivalent energy of a blast wave $E < 4.1\times10^{51}$ erg (assuming typical GRB parameters)., 14 pages, 6 figures, accepted for publication in ApJ

Published
2021

26. The THESEUS space mission: science goals, requirements and mission concept

Author

M. Branchesi, E. Le Floc'h, Sandro Mereghetti, Victor Reglero, Andrew Blain, Riccardo Ciolfi, A. de Rosa, P. Heddermann, S. Basa, Lise Christensen, Ian Hutchinson, Claudio Labanti, Andrea Santangelo, E. Bozzo, A. J. Castro-Tirado, P. T. O'Brien, Victor Doroshenko, Nial Tanvir, Hannah Natasha Lerman, S. Paltani, D. Gotz, J. P. Osborne, C. Tenzer, Luciano Burderi, Piero Rosati, M. D. Caballero-Garcia, G. Stratta, Lorenzo Amati, Lorraine Hanlon, G. Ghirlanda, Ruben Salvaterra, F. Frontera, Luciano Rezzolla, Andrea Ferrara, Institut de Recherches sur les lois Fondamentales de l'Univers (IRFU), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay, Laboratoire d'Astrophysique de Marseille (LAM), Aix Marseille Université (AMU)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS), THESEUS, Istituto Nazionale di Astrofisica, European Commission, Ministerio de Economía y Competitividad (España), and Ministerio de Ciencia e Innovación (España)

Subjects
cosmological model, transients, Computer science, X-rays: survey, X-rays: transients, X-rays: instrumentation, Gamma-rays: bursts, Cosmology: early Universe, Gamma-rays: instrumentation, NIR: instrumentation, NIR: transients, Space (commercial competition), 01 natural sciences, 7. Clean energy, NIR: instrumentation, star, X-rays: survey, Gamma-rays: bursts, 010303 astronomy & astrophysics, instrumentation [Gamma-rays], instrumentation, X-rays: instrumentation, bursts, redshift: high, Astrophysics::Instrumentation and Methods for Astrophysics, early Universe, solar system, Cosmology, neutrino: detector, AFTERGLOW, Cosmology: early Universe, Systems engineering, Astrophysics - Instrumentation and Methods for Astrophysics, Gamma-rays, instrumentation [X-rays], Astrophysics::High Energy Astrophysical Phenomena, interferometer, REDSHIFT, FOS: Physical sciences, galaxy: luminosity, Astrophysics::Cosmology and Extragalactic Astrophysics, gamma ray: burst, transients [X-rays], GAMMA-RAY BURST, electromagnetic field: production, NO, neutrino: production, X-rays, 0103 physical sciences, ionization, NIR: transients, gamma ray: detector, galaxy: mass, survey, Gamma-rays: instrumentation, [PHYS.PHYS.PHYS-INS-DET]Physics [physics]/Physics [physics]/Instrumentation and Detectors [physics.ins-det], AGN, Instrumentation and Methods for Astrophysics (astro-ph.IM), transients [NIR], 010308 nuclear & particles physics, survey [X-rays], Astronomy and Astrophysics, early Universe [Cosmology], NIR, instrumentation [NIR], gravitational radiation detector, bursts [Gamma-rays], LUMINOSITY FUNCTION, Space and Planetary Science, gravitational radiation: emission, X-rays: transients, gravitational radiation: localization, galaxy, X-ray: detector
Abstract

Full list of authors: Amati, L.; O'Brien, P. T.; Götz, D.; Bozzo, E.; Santangelo, A.; Tanvir, N. ; Frontera, F.; Mereghetti, S.; Osborne, J. P.; Blain, A.; Basa, S.; Branchesi, M.; Burderi, L.; Caballero-García, M.; Castro-Tirado, A. J.; Christensen, L.; Ciolfi, R.; De Rosa, A.; Doroshenko, V.; Ferrara, A.; Ghirlanda, G.; Hanlon, L.; Heddermann, P.; Hutchinson, I.; Labanti, C.; Le Floch, E.; Lerman, H.; Paltani, S.; Reglero, V.; Rezzolla, L.; Rosati, P.; Salvaterra, R.; Stratta, G.; Tenzer, C.; Theseus Consortium.--This Open Access article is licensed under a Creative Commons Attribution 4.0 International License, which permits use, sharing, adaptation, distribution and reproduction in any medium or format, as long as you give appropriate credit to the original author(s) and the source, provide a link to the Creative Commons licence, and indicate if changes were made. The images or other third party material in this article are included in the article's Creative Commons licence, unless indicated otherwise in a credit line to the material. If material is not included in the article's Creative Commons licence and your intended use is not permitted by statutory regulation or exceeds the permitted use, you will need to obtain permission directly from the copyright holder. To view a copy of this licence, visit http://creativecommons.org/licenses/by/4.0/., THESEUS, one of the two space mission concepts being studied by ESA as candidates for next M5 mission within its Comsic Vision programme, aims at fully exploiting Gamma-Ray Bursts (GRB) to solve key questions about the early Universe, as well as becoming a cornerstone of multi-messenger and time-domain astrophysics. By investigating the first billion years of the Universe through high-redshift GRBs, THESEUS will shed light on the main open issues in modern cosmology, such as the population of primordial low mass and luminosity galaxies, sources and evolution of cosmic re-ionization, SFR and metallicity evolution up to the “cosmic dawn” and across Pop-III stars. At the same time, the mission will provide a substantial advancement of multi-messenger and time-domain astrophysics by enabling the identification, accurate localisation and study of electromagnetic counterparts to sources of gravitational waves and neutrinos, which will be routinely detected in the late ‘20s and early ‘30s by the second and third generation Gravitational Wave (GW) interferometers and future neutrino detectors, as well as of all kinds of GRBs and most classes of other X/gamma-ray transient sources. Under all these respects, THESEUS will provide great synergies with future large observing facilities in the multi-messenger domain. A Guest Observer programme, comprising Target of Opportunity (ToO) observations, will expand the science return of the mission, to include, e.g., solar system minor bodies, exoplanets, and AGN. © 2021, The Author(s)., The authors, on behalf of the entire THESEUS consortium, are grateful to the ESA-appointed THESEUS Study Scientist Matteo Guainazzi, as well as the entire ESA Study Team for all their work and support across the mission assessment phase (2018-2021). Authors from the Italian National Institute of Astrophysics (INAF) are grateful for the support received through the agreement ASI-INAF n. 2n. 2018-29-HH.0. Open access funding provided by Istituto Nazionale di Astrofisica within the CRUI-CARE Agreement., With funding from the Spanish government through the Severo Ochoa Centre of Excellence accreditation SEV-2017-0709.

Published
2021

27. Exploration of the high-redshift universe enabled by THESEUS

Author

Lajos G. Balázs, E. Le Floc'h, René Hudec, Ehud Behar, Giancarlo Ghirlanda, Valentina D'Odorico, Silvia Zane, J. P. Osborne, P. T. O'Brien, Stéphane Paltani, Dorottya Szécsi, A. Gomboc, B. Ciardi, Lise Christensen, U. Maio, Yuji Urata, Sandro Mereghetti, Ruben Salvaterra, F. Frontera, E. Piedipalumbo, Sergio Campana, Joseph Caruana, Olga Sergijenko, Pasquier Noterdaeme, A. De Cia, Lorenzo Amati, Diego Götz, Elizabeth R. Stanway, L. V. Toth, S. D. Vergani, M. de Pasquale, Nial R. Tanvir, Z. Bagoly, L. Graziani, M. Della Valle, S. Basa, Piero Rosati, István T. Horváth, Astrophysique Interprétation Modélisation (AIM (UMR7158 / UMR_E_9005 / UM_112)), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Institut d'Astrophysique de Paris (IAP), Institut national des sciences de l'Univers (INSU - CNRS)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Laboratoire d'Astrophysique de Marseille (LAM), Aix Marseille Université (AMU)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS), Institut de Recherches sur les lois Fondamentales de l'Univers (IRFU), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay, Galaxies, Etoiles, Physique, Instrumentation (GEPI), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS), Tanvir, N. R., Le Floc'h, E., Christensen, L., Caruana, J., Salvaterra, R., Ghirlanda, G., Ciardi, B., Maio, U., D'Odorico, V., Piedipalumbo, E., Campana, S., Noterdaeme, P., Graziani, L., Amati, L., Bagoly, Z., Balazs, L. G., Basa, S., Behar, E., De Cia, A., Valle, M. D., De Pasquale, M., Frontera, F., Gomboc, A., Gotz, D., Horvath, I., Hudec, R., Mereghetti, S., O'Brien, P. T., Osborne, J. P., Paltani, S., Rosati, P., Sergijenko, O., Stanway, E. R., Szecsi, D., Toth, L. V., Urata, Y., Vergani, S., Zane, S., Astrophysique Interprétation Modélisation (AIM (UMR_7158 / UMR_E_9005 / UM_112)), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris Diderot - Paris 7 (UPD7), and Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS)

Subjects
Abundances, Gamma-ray bursts, Reionization, Star forming galaxies, Abundances, Gamma-ray bursts, Reionization, Star forming galaxies, PEAK ENERGY, Metallicity, media_common.quotation_subject, MASS-METALLICITY RELATION, Astrophysics::High Energy Astrophysical Phenomena, FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, DUST FORMATION, 01 natural sciences, 7. Clean energy, NO, GAMMA-RAY BURST, X-ray astronomy, NEUTRAL FRACTION, LY-ALPHA, Abundance, 0103 physical sciences, LYMAN-ALPHA EMISSION, Astrophysics::Solar and Stellar Astrophysics, [PHYS.PHYS.PHYS-INS-DET]Physics [physics]/Physics [physics]/Instrumentation and Detectors [physics.ins-det], 010303 astronomy & astrophysics, Instrumentation and Methods for Astrophysics (astro-ph.IM), Gamma-ray burst, Astrophysics::Galaxy Astrophysics, Luminosity function (astronomy), media_common, Physics, 010308 nuclear & particles physics, Star formation, Astronomy, Astronomy and Astrophysics, Redshift, Galaxy, Universe, Cosmology, Stars, 13. Climate action, Space and Planetary Science, POPULATION III, NO EVIDENCE, Astrophysics - Instrumentation and Methods for Astrophysics, COSMIC REIONIZATION
Abstract

At peak, long-duration gamma-ray bursts are the most luminous sources of electromagnetic radiation known. Since their progenitors are massive stars, they provide a tracer of star formation and star-forming galaxies over the whole of cosmic history. Their bright power-law afterglows provide ideal backlights for absorption studies of the interstellar and intergalactic medium back to the reionization era. The proposed THESEUS mission is designed to detect large samples of GRBs at $z>6$ in the 2030s, at a time when supporting observations with major next generation facilities will be possible, thus enabling a range of transformative science. THESEUS will allow us to explore the faint end of the luminosity function of galaxies and the star formation rate density to high redshifts; constrain the progress of re-ionisation beyond $z\gtrsim6$; study in detail early chemical enrichment from stellar explosions, including signatures of Population III stars; and potentially characterize the dark energy equation of state at the highest redshifts., Submitted to Experimental Astronomy

Published
2021

28. Synergies of THESEUS with the large facilities of the 2030s and guest observer opportunities

Author

Stefan Grimm, Enrico Bozzo, P. T. O'Brien, Antonio Martin-Carrillo, Andrea Ferrara, Sandro Mereghetti, Piero Rosati, G. Oganesyan, G. Guidorzi, Nikolaos Stergioulas, S. Turriziani, Francesco Longo, Marica Branchesi, J. P. Osborne, D. Porquet, Lorenzo Amati, S. Basa, Stéphane Paltani, Giancarlo Ghirlanda, Dafne Guetta, Solen Balman, M. H. Erkut, Sarah L. Casewell, Olga Sergijenko, Ruben Salvaterra, Joseph Caruana, Andrew Blain, S. D. Vergani, Giulia Stratta, Michele Maggiore, R. Ciolfi, Maurizio Spurio, E. Le Floc'h, Andreja Gomboc, Andrea Rossi, Lise Christensen, Nial R. Tanvir, Filippo Frontera, F. Schüssler, Jan Harms, Laboratoire d'Astrophysique de Marseille (LAM), Aix Marseille Université (AMU)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS), Institut de Recherches sur les lois Fondamentales de l'Univers (IRFU), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay, Astrophysique Interprétation Modélisation (AIM (UMR7158 / UMR_E_9005 / UM_112)), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Galaxies, Etoiles, Physique, Instrumentation (GEPI), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS), 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), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris Diderot - Paris 7 (UPD7)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL), Rosati, P, Basa, S, Blain, A W, Bozzo, E, Branchesi, M, Christensen, L, Ferrara, A, Gomboc, A, O'Brien, P T, Osborne, J P, Rossi, A, Schüssler, F, Spurio, M, Stergioulas, N, Stratta, G, Amati, L, Casewell, S, Ciolfi, R, Ghirlanda, G, Grimm, S, Guetta, D, Harms, J, Le Floc'h, E, Longo, F, Maggiore, M, Mereghetti, S, Oganesyan, G, Salvaterra, R, Tanvir, N R, Turriziani, S, Vergani, S D, Balman, S, Caruana, J, Erkut, M H, Guidorzi, G, Frontera, F, Martin-Carrillo, A, Paltani, S, Porquet, D, Sergijenko, O, Rosati P., Basa S., Blain A.W., Bozzo E., Branchesi M., Christensen L., Ferrara A., Gomboc A., O'Brien P.T., Osborne J.P., Rossi A., Schussler F., Spurio M., Stergioulas N., Stratta G., Amati L., Casewell S., Ciolfi R., Ghirlanda G., Grimm S., Guetta D., Harms J., Le Floc'h E., Longo F., Maggiore M., Mereghetti S., Oganesyan G., Salvaterra R., Tanvir N.R., Turriziani S., Vergani S.D., Balman S., Caruana J., Erkut M.H., Guidorzi G., Frontera F., Martin-Carrillo A., Paltani S., Porquet D., and Sergijenko O.

Subjects
cosmological model, neutron star: binary, Cherenkov Telescope Array, Computer science, 01 natural sciences, 7. Clean energy, Cosmology, GW170817, multi-messenger astrophysics, 010303 astronomy & astrophysics, media_common, COSMIC cancer database, gamma-ray bursts, REIONIZATION, gravitation wave sources, star: formation, AFTERGLOWS, neutrino: detector, Neutrino detector, Gravitation wave sources, Gamma-ray bursts, Astrophysics - Instrumentation and Methods for Astrophysics, Exploit, media_common.quotation_subject, FOS: Physical sciences, gamma ray: burst, Observer (physics), X-ray sources, NO, electromagnetic field: production, neutrino: production, binary: coalescence, Neutrino sources, 0103 physical sciences, gamma ray: detector, X-ray: emission, [PHYS.PHYS.PHYS-INS-DET]Physics [physics]/Physics [physics]/Instrumentation and Detectors [physics.ins-det], Instrumentation and Methods for Astrophysics (astro-ph.IM), Gamma-ray burst, Neutrino source, Multi-messenger astrophysics, 010308 nuclear & particles physics, Gravitational wave, Astronomy and Astrophysics, Multi-messenger astrophysic, neutrino: particle source, binary: compact, Data science, Universe, gravitational radiation detector, detector: sensitivity, black hole: binary, Space and Planetary Science, gravitational radiation: emission, Gravitation wave source, gravitational radiation: localization, X-ray: detector
Abstract

The proposed THESEUS mission will vastly expand the capabilities to monitor the high-energy sky, and will exploit large samples of gamma-ray bursts to probe the early Universe back to the first generation of stars, and to advance multi-messenger astrophysics by detecting and localizing the counterparts of gravitational waves and cosmic neutrino sources. The combination and coordination of these activities with multi-wavelength, multi-messenger facilities expected to be operating in the thirties will open new avenues of exploration in many areas of astrophysics, cosmology and fundamental physics, thus adding considerable strength to the overall scientific impact of THESEUS and these facilities. We discuss here a number of these powerful synergies., Revised version after submission to Experimental Astronomy

Published
2021

29. Sensitivity of the Cherenkov Telescope Array for probing cosmology and fundamental physics with gamma-ray propagation

Author

J.-P. Lenain, A. Domínguez, Jonathan Ivor Davies, T. Armstrong, A. A. Zdziarski, F. Gianotti, M. Balbo, E. O. Angüner, M. Marculewicz, Alasdair E. Gent, Alice Donini, Olivier Hervet, Henry Przybilski, Giacomo Principe, G. Leto, M. Peresano, Stefano Covino, P. A. Caraveo, Gianpiero Tagliaferri, D. de Martino, V. V. Vassiliev, D. Cauz, F. R. Pantaleo, U. Barres de Almeida, Pietro Bruno, E. Lindfors, M. Zavrtanik, G. Hughes, Miriam Lucio Martinez, P. Bordas, Y. Suda, G. S. Varner, R. Rando, K. Cerny, S. Pita, Csaba Balázs, E. Fiandrini, Michael Backes, Tomohiko Oka, Massimo Persic, Andrea Chiavassa, Johannes Veh, A. Stamerra, Fabrizio Tavecchio, B. Biasuzzi, Michael Punch, Soebur Razzaque, F. D'Ammando, P. I. Batista, Bruna Bertucci, F. Longo, Francesco Gabriele Saturni, Michael G. Burton, Bohdan Hnatyk, P. Sangiorgi, E. M. Santos, D. Nosek, Gagik Tovmassian, J. L. Dournaux, Pedro L. Luque-Escamilla, A. Aguirre-Santaella, M. Orienti, Lluis Font, Andreas Quirrenbach, Philippe Laporte, Ralf Kissmann, Francesco Lucarelli, K. Noda, I. Jiménez Martínez, G. Romeo, Wystan Benbow, P. Romano, B. Bi, J. Grube, H.-S. Zechlin, Giacomo Bonnoli, Martin White, J. P. Osborne, Enrico Cascone, Marek Jamrozy, C. Alispach, Miroslav Pech, O. Cuevas, Petr Schovanek, K. Hayashi, V. I. Zhdanov, Javier Coronado-Blázquez, D. Medina Miranda, Barbara Balmaverde, E. de Ona Wilhelmi, Frank M. Rieger, A. Shalchi, J. M. Paredes, Ruben Alfaro, N. Giglietto, Diego Falceta-Gonçalves, Helene Sol, Rodolfo Carosi, Ayan Acharyya, Dominik Elsässer, S. Vercellone, D. Pimentel, T. Mizuno, Alessandro Bruno, Juan Abel Barrio, K. Kosack, Mauro Orlandini, Rodrigo Guedes Lang, P. Marquez, Adrian Biland, Y. Kobayashi, Nicholas F. H Tothill, M. de Naurois, Daniele Spiga, Lili Yang, L. Tibaldo, Pavel Horvath, M. Lopez, I. Sadeh, Marek Nikolajuk, F. Schüssler, Reshmi Mukherjee, Gianpaolo Vettolani, Jürgen Knödlseder, Daniel Nieto, R. Hnatyk, German Martinez, Diego F. Torres, Farinaldo S. Queiroz, N. Parmiggiani, G. Lamanna, Marcos Santander, S. Fegan, I. Vovk, M. Sánchez-Conde, Wiphu Rujopakarn, Norita Kawanaka, R. C. Shellard, Michael C. B. Ashley, J. Jurysek, Francisco J. Franco, Samuel Timothy Spencer, E. Rebert, J. Morales Merino, M. Pecimotika, Marco Berton, Regis Terrier, G. A. Beck, Carlos Díaz, J. L. Contreras, G. Zaharijas, R. Moderski, José-María Martí, A. Insolia, D. Zavrtanik, K. Kohri, Ladislav Chytka, T. Grabarczyk, A. Zech, M. Garczarczyk, Anastasia Sokolenko, J. Lefaucheur, R. A. Cameron, Moritz Hütten, S. Karkar, K. Pfrang, V. Poireau, Asaf Pe'er, A. Reimer, Fabio Acero, L. Freixas Coromina, David Sánchez, Jonathan S. Lapington, Konstantinos N. Gourgouliatos, J.R. Hörandel, Mario Buscemi, Francesco Dazzi, Abelardo Moralejo, J. Bolmont, R. White, A. Rosales de Leon, J. Prast, Sabrina Einecke, Roberto Aloisio, Yvonne Becherini, Andreas Specovius, Shohei Yanagita, Juan Cortina, Miroslav Hrabovsky, Petr Janecek, D. Depaoli, Lucas Taylor, U. Schwanke, H. Abdalla, S. Recchia, Manuela Mallamaci, M. K. Daniel, Q. Feng, L. Baroncelli, Hiromitsu Takahashi, Susumu Inoue, U. Straumann, Masatoshi Ohishi, Roberto Capuzzo-Dolcetta, Nu. Komin, Federico Russo, R. de Cássia dos Anjos, Y. Ohira, Ferdinando Giordano, Nagisa Hiroshima, E. Garcia, Gavin Rowell, V. Bozhilov, Maxim V. Barkov, Dario Hrupec, I. Oya, F. Salesa Greus, Anna Wolter, M. Živec, R. Belmont, R. Adam, T. Reposeur, J. Rico, A. W. Chen, G. Pühlhofer, H. Prokoph, Stefan Wagner, F. Di Pierro, Fabrizio Bocchino, M. de Bony de Lavergne, A. Kong, Masha Chernyakova, M. Pohl, M. Vazquez Acosta, A. Nagai, A. Brill, Dusan Mandat, Jonathan Biteau, Martin Makariev, Catherine Boisson, E. Lyard, Gilles Maurin, H. Martínez-Huerta, Oscar Blanch, Bernd Schleicher, M. Minev, A. Berti, James E. M. Watson, Talvikki Hovatta, M. Valentino, Luis Ángel Tejedor, Elena Amato, M. V. Fonseca, Anderson Caproni, L. Mohrmann, P. Reichherzer, R. L. C. Starling, M. Seglar Arroyo, E. Orlando, B. Rudak, G. Emery, J. A. Green, Salvo Scuderi, M. Prouza, Tom Richtler, Bartłomiej Pilszyk, A. Carosi, Jacek Niemiec, Wolfgang Rhode, G. Ambrosi, D. Ribeiro, A. Wierzcholska, A. Ghalumyan, Eugenio Bottacini, Sylvain Chaty, A. Baquero Larriva, Olaf Reimer, D. Horan, Fabian Leuschner, T. Di Girolamo, Alessandro Caccianiga, Martin Will, Saverio Lombardi, A. Fiasson, Mitsunari Takahashi, J. J. Rodríguez Vázquez, B. De Lotto, V. De Caprio, Stefano Truzzi, Dirk L. Hoffmann, M. Vecchi, Antonio Pagliaro, Jose J. Gonzalez, Wenwu Tian, R. Della Ceca, J. Becerra González, S. Nozaki, T. Vuillaume, S. L. Lloyd, Maria Ionica, Elisabetta Bissaldi, Petr Travnicek, Y. Ascasibar, Carlo Vigorito, F. Tuossenel, Malcolm Fairbairn, O. Martinez, Marco Iarlori, Serena Loporchio, Alessandro Costa, R. Pillera, A. Morselli, M. Heller, Jaime Rosado, E. M. de Gouveia Dal Pino, V. Vitale, A. M. Brown, E. Molina, Takashi Saito, A. De Angelis, Thomas Murach, R. A. Ong, J. Bregeon, P. T. O'Brien, Mikael Jacquemont, P. Cristofari, Francesco Conte, Lab Saha, R. Walter, Vitalii Sliusar, W. Jin, Vito Conforti, N. Produit, H. Siejkowski, Lovro Pavletić, Carole Mundell, G. Rodriguez Fernandez, J. F. Glicenstein, Paresh Sharma, C. Delgado, Vladimír Karas, Luca Foffano, J. Granot, Manuel Meyer, Reiko Orito, G. Umana, G. Chiaro, D. Tonev, R. Wiemann, G. Manicò, J.C. Rodriguez Ramirez, Luca Tosti, Markus Böttcher, Andrea Bulgarelli, C. Díaz-Bahamondes, I. Jung-Richardt, Karol Seweryn, P. Piatteli, Agnieszka Slowikowska, Jan Ebr, M. Ostrowski, J. L. Rodriguez, D. della Volpe, Ermanno Pietropaolo, M. Caprai, T. Montaruli, A. Lopez, Rodrigo Nemmen, R. R. Prado, L. Arrabito, Atreyee Sinha, C. van Eldik, Serguei Vorobiov, Hidetoshi Sano, J. Alfaro, Sabrina Casanova, G. Maneva, B. Vallage, Valentina Fioretti, Carmelo Evoli, P. Kaaret, B. A. W. Mode, Agnieszka Majczyna, Sebastian Diebold, A. Scherer, F. de Palma, S. Hernández Cadena, V. Beshley, T.R.N. Ekoume, David A. Williams, M. Capasso, A. Halim, Alison Mitchell, Tomislav Terzić, Paola Grandi, Lorenzo Amati, Christopher Eckner, David Gascon, K. Nishijima, J. Becker Tjus, B. Khélifi, G. Galanti, Jamie Holder, Vincenzo Rizi, Orel Gueta, Daniele Gaggero, F. Pintore, Utane Sawangwit, Vassil Verguilov, Heide Costantini, F. Arqueros, Daniel Kerszberg, P. M. Chadwick, D. Zarić, Marc Ribó, Olga Sergijenko, Dario Grasso, Hidetoshi Kubo, Daniela Dorner, T. Stolarczyk, M. Gaug, R. Alves Batista, Elisa Bernardini, Vikram V. Dwarkadas, Jim Hinton, Jelena Strišković, Andreu Sanuy, M. Servillat, V. Barbosa Martins, Giovanni Bonanno, S. Gunji, R. Wischnewski, S. Sarkar, Gianluca Giavitto, Takeshi Nakamori, M. Palatka, Maria Letizia Pumo, Camilla Maggio, M. Zacharias, Katsuaki Asano, Valerio Vagelli, Anton Dmytriiev, Ryo Yamazaki, M. Vacula, P. Goldoni, Gilles Fontaine, Hiroshi Muraishi, D. Mazin, Samo Stanič, G. Ghirlanda, M. Polo, M. Nievas, M. Lemoine-Goumard, Oleh Petruk, Jose Miguel Miranda, M. Iori, A. Marcowith, Y. Renier, Satoshi Fukami, M. Roncadelli, F. Leone, Takanori Yoshikoshi, Ana Luiza d'Ávila Viana, Y. Fukui, Max Harvey, Sera Markoff, I. Agudo, P. Temnikov, Vincenzo Testa, R. López-Coto, J.D. Mbarubucyeye, Tjark Miener, David Paneque, V. Gammaldi, T. Hassan Collado, H. Abe, L. Bonneau Arbeletche, S. D. Vergani, Sasa Micanovic, P. Vallania, Marina Manganaro, Elena Torresi, M. Giarrusso, G. Ferrand, Paweł Świerk, B. Patricelli, Matteo Cerruti, N. La Palombara, D. Morcuende-Parrilla, V. de Souza, Toshiaki Inada, Yasushi Fukazawa, Werner Hofmann, Michele Doro, E. Pueschel, A. Araudo, E. Sciacca, Thomas Lohse, A. Djannati-Ataï, Abdalla, H., Abe, H., Acero, F., Acharyya, A., Adam, R., Agudo, I., Aguirre-Santaella, A., Alfaro, R., Alfaro, J., Alispach, C., Aloisio, R., Alves Batista, R., Amati, L., Amato, E., Ambrosi, G., Ang??ner, E. O., Araudo, A., Armstrong, T., Arqueros, F., Arrabito, L., Asano, K., Ascas??bar, Y., Ashley, M., Backes, M., Balazs, C., Balbo, M., Balmaverde, B., Baquero Larriva, A., Barbosa Martins, V., Barkov, M., Baroncelli, L., Barres de Almeida, U., Barrio, J. A., Batista, P. -I., Becerra Gonz??lez, J., Becherini, Y., Beck, G., Becker Tjus, J., Belmont, R., Benbow, W., Bernardini, E., Berti, A., Berton, M., Bertucci, B., Beshley, V., Bi, B., Biasuzzi, B., Biland, A., Bissaldi, E., Biteau, J., Blanch, O., Bocchino, F., Boisson, C., Bolmont, J., Bonanno, G., Bonneau Arbeletche, L., Bonnoli, G., Bordas, P., Bottacini, E., B??ttcher, M., Bozhilov, V., Bregeon, J., Brill, A., Brown, A. M., Bruno, P., Bruno, A., Bulgarelli, A., Burton, M., Buscemi, M., Caccianiga, A., Cameron, R., Capasso, M., Caprai, M., Caproni, A., Capuzzo-Dolcetta, R., Caraveo, P., Carosi, R., Carosi, A., Casanova, S., Cascone, E., Cauz, D., Cerny, K., Cerruti, M., Chadwick, P., Chaty, S., Chen, A., Chernyakova, M., Chiaro, G., Chiavassa, A., Chytka, L., Conforti, V., Conte, F., Contreras, J. L., Coronado-Blazquez, J., Cortina, J., Costa, A., Costantini, H., Covino, S., Cristofari, P., Cuevas, O., D'Ammando, F., Daniel, M. K., Davies, J., Dazzi, F., De Angelis, A., de Bony de Lavergne, M., De Caprio, V., de C??ssia dos Anjos, R., de Gouveia Dal Pino, E. M., De Lotto, B., De Martino, D., de Naurois, M., de O??a Wilhelmi, E., De Palma, F., de Souza, V., Delgado, C., Della Ceca, R., della Volpe, D., Depaoli, D., Di Girolamo, T., Di Pierro, F., D??az, C., D??az-Bahamondes, C., Diebold, S., Djannati-Ata??, A., Dmytriiev, A., Dom??nguez, A., Donini, A., Dorner, D., Doro, M., Dournaux, J., Dwarkadas, V. V., Ebr, J., Eckner, C., Einecke, S., Ekoume, T. R. N., Els??sser, D., Emery, G., Evoli, C., Fairbairn, M., Falceta-Goncalves, D., Fegan, S., Feng, Q., Ferrand, G., Fiandrini, E., Fiasson, A., Fioretti, V., Foffano, L., Fonseca, M. V., Font, L., Fontaine, G., Franco, F. J., Freixas Coromina, L., Fukami, S., Fukazawa, Y., Fukui, Y., Gaggero, D., Galanti, G., Gammaldi, V., Garcia, E., Garczarczyk, M., Gascon, D., Gaug, M., Gent, A., Ghalumyan, A., Ghirlanda, G., Gianotti, F., Giarrusso, M., Giavitto, G., Giglietto, N., Giordano, F., Glicenstein, J., Goldoni, P., Gonz??lez, J. M., Gourgouliatos, K., Grabarczyk, T., Grandi, P., Granot, J., Grasso, D., Green, J., Grube, J., Gueta, O., Gunji, S., Halim, A., Harvey, M., Hassan Collado, T., Hayashi, K., Heller, M., Hern??ndez Cadena, S., Hervet, O., Hinton, J., Hiroshima, N., Hnatyk, B., Hnatyk, R., Hoffmann, D., Hofmann, W., Holder, J., Horan, D., H??randel, J., Horvath, P., Hovatta, T., Hrabovsky, M., Hrupec, D., Hughes, G., H??tten, M., Iarlori, M., Inada, T., Inoue, S., Insolia, A., Ionica, M., Iori, M., Jacquemont, M., Jamrozy, M., Janecek, P., Jim??nez Mart??nez, I., Jin, W., Jung-Richardt, I., Jurysek, J., Kaaret, P., Karas, V., Karkar, S., Kawanaka, N., Kerszberg, D., Kh??lifi, B., Kissmann, R., Kn??dlseder, J., Kobayashi, Y., Kohri, K., Komin, N., Kong, A., Kosack, K., Kubo, H., La Palombara, N., Lamanna, G., Lang, R. G., Lapington, J., Laporte, P., Lefaucheur, J., Lemoine-Goumard, M., Lenain, J., Leone, F., Leto, G., Leuschner, F., Lindfors, E., Lloyd, S., Lohse, T., Lombardi, S., Longo, F., Lopez, A., L??pez, M., L??pez-Coto, R., Loporchio, S., Lucarelli, F., Luque-Escamilla, P. L., Lyard, E., Maggio, C., Majczyna, A., Makariev, M., Mallamaci, M., Mandat, D., Maneva, G., Manganaro, M., Manic??, G., Marcowith, A., Marculewicz, M., Markoff, S., Marquez, P., Mart??, J., Martinez, O., Mart??nez, M., Mart??nez, G., Mart??nez-Huerta, H., Maurin, G., Mazin, D., Mbarubucyeye, J. D., Medina Miranda, D., Meyer, M., Micanovic, S., Miener, T., Minev, M., Miranda, J. M., Mitchell, A., Mizuno, T., Mode, B., Moderski, R., Mohrmann, L., Molina, E., Montaruli, T., Moralejo, A., Morales Merino, J., Morcuende-Parrilla, D., Morselli, A., Mukherjee, R., Mundell, C., Murach, T., Muraishi, H., Nagai, A., Nakamori, T., Nemmen, R., Niemiec, J., Nieto, D., Nievas, M., Nikolajuk, M., Nishijima, K., Noda, K., Nosek, D., Nozaki, S., O'Brien, P., Ohira, Y., Ohishi, M., Oka, T., Ong, R. A., Orienti, M., Orito, R., Orlandini, M., Orlando, E., Osborne, J. P., Ostrowski, M., Oya, I., Pagliaro, A., Palatka, M., Paneque, D., Pantaleo, F. R., Paredes, J. M., Parmiggiani, N., Patricelli, B., Pavleti??, L., Pe'Er, A., Pech, M., Pecimotika, M., Peresano, M., Persic, M., Petruk, O., Pfrang, K., Piatteli, P., Pietropaolo, E., Pillera, R., Pilszyk, B., Pimentel, D., Pintore, F., Pita, S., Pohl, M., Poireau, V., Polo, M., Prado, R. R., Prast, J., Principe, G., Produit, N., Prokoph, H., Prouza, M., Przybilski, H., Pueschel, E., P??hlhofer, G., Pumo, M. L., Punch, M., Queiroz, F., Quirrenbach, A., Rando, R., Razzaque, S., Rebert, E., Recchia, S., Reichherzer, P., Reimer, O., Reimer, A., Renier, Y., Reposeur, T., Rhode, W., Ribeiro, D., Rib??, M., Richtler, T., Rico, J., Rieger, F., Rizi, V., Rodriguez, J., Rodriguez Fernandez, G., Rodriguez Ramirez, J. C., Rodr??guez V??zquez, J. J., Romano, P., Romeo, G., Roncadelli, M., Rosado, J., Rosales de Leon, A., Rowell, G., Rudak, B., Rujopakarn, W., Russo, F., Sadeh, I., Saha, L., Saito, T., Salesa Greus, F., Sanchez, D., S??nchez-Conde, M., Sangiorgi, P., Sano, H., Santander, M., Santos, E. M., Sanuy, A., Sarkar, S., Saturni, F. G., Sawangwit, U., Scherer, A., Schleicher, B., Schovanek, P., Schussler, F., Schwanke, U., Sciacca, E., Scuderi, S., Seglar Arroyo, M., Sergijenko, O., Servillat, M., Seweryn, K., Shalchi, A., Sharma, P., Shellard, R. C., Siejkowski, H., Sinha, A., Sliusar, V., Slowikowska, A., Sokolenko, A., Sol, H., Specovius, A., Spencer, S., Spiga, D., Stamerra, A., Stani??, S., Starling, R., Stolarczyk, T., Straumann, U., Stri??kovi??, J., Suda, Y., wierk, P., Tagliaferri, G., Takahashi, H., Takahashi, M., Tavecchio, F., Taylor, L., Tejedor, L. A., Temnikov, P., Terrier, R., Terzic, T., Testa, V., Tian, W., Tibaldo, L., Tonev, D., Torres, D. F., Torresi, E., Tosti, L., Tothill, N., Tovmassian, G., Travnicek, P., Truzzi, S., Tuossenel, F., Umana, G., Vacula, M., Vagelli, V., Valentino, M., Vallage, B., Vallania, P., van Eldik, C., Varner, G. S., Vassiliev, V., V??zquez Acosta, M., Vecchi, M., Veh, J., Vercellone, S., Vergani, S., Verguilov, V., Vettolani, G. P., Viana, A., Vigorito, C. F., Vitale, V., Vorobiov, S., Vovk, I., Vuillaume, T., Wagner, S. J., Walter, R., Watson, J., White, M., White, R., Wiemann, R., Wierzcholska, A., Will, M., Williams, D. A., Wischnewski, R., Wolter, A., Yamazaki, R., Yanagita, S., Yang, L., Yoshikoshi, T., Zacharias, M., Zaharijas, G., Zaric, D., Zavrtanik, M., Zavrtanik, D., Zdziarski, A. A., Zech, A., Zechlin, H., Zhdanov, V. I., ivec, M., Comisión Nacional de Investigación Científica y Tecnológica (Chile), Ministry of Education, Youth and Sports (Czech Republic), Academy of Finland, Istituto Nazionale di Astrofisica, National Science Centre (Poland), Slovenian Research Agency, European Commission, Ministerio de Economía y Competitividad (España), Ministerio de Ciencia e Innovación (España), Junta de Andalucía, Astrophysique Interprétation Modélisation (AIM (UMR_7158 / UMR_E_9005 / UM_112)), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris Diderot - Paris 7 (UPD7), Laboratoire Leprince-Ringuet (LLR), Centre National de la Recherche Scientifique (CNRS)-École polytechnique (X)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3), Centre de Physique des Particules de Marseille (CPPM), Aix Marseille Université (AMU)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Laboratoire Univers et Particules de Montpellier (LUPM), Centre National de la Recherche Scientifique (CNRS)-Université de Montpellier (UM)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Montpellier 2 - Sciences et Techniques (UM2), Laboratoire de Physique des 2 Infinis Irène Joliot-Curie (IJCLab), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Paris-Saclay-Centre National de la Recherche Scientifique (CNRS), Laboratoire Univers et Théories (LUTH (UMR_8102)), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Diderot - Paris 7 (UPD7), Laboratoire de Physique Nucléaire et de Hautes Énergies (LPNHE (UMR_7585)), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-Université de Paris (UP), Laboratoire d'Annecy de Physique des Particules (LAPP), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS), 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), Institut de Recherches sur les lois Fondamentales de l'Univers (IRFU), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay, Institut de recherche en astrophysique et planétologie (IRAP), Institut national des sciences de l'Univers (INSU - CNRS)-Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Observatoire Midi-Pyrénées (OMP), Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Centre National de la Recherche Scientifique (CNRS), Centre d'Etudes Nucléaires de Bordeaux Gradignan (CENBG), Université Sciences et Technologies - Bordeaux 1-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), CTA, UAM. Departamento de Física Teórica, Batista, R. A., Anguner, E. O., Ascasibar, Y., Larriva, A. B., Martins, V. B., De Almeida, U. B., Gonzalez, J. B., Tjus, J. B., Arbeletche, L. B., Bottcher, M., Angelis, A. D., De Lavergne, M. D. B., Caprio, V. D., De Dos Anjos, R. C., De Gouveia Dal Pino, E. M., Lotto, B. D., Martino, D. D., De Naurois, M., Wilhelmi, E. D. O., DE PALMA, F., De Souza, V., Ceca, R. D., Volpe, D. D., Girolamo, T. D., Pierro, F. D., Diaz, C., Diaz-Bahamondes, C., Djannati-Atai, A., Dominguez, A., Elsasser, D., Coromina, L. F., Gonzalez, J. M., Collado, T. H., Cadena, S. H., Horandel, J., Hutten, M., Martinez, I. J., Khelifi, B., Knodlseder, J., Palombara, N. L., Lopez, M., Lopez-Coto, R., Manico, G., Marti, J., Martinez, M., Martinez, G., Martinez-Huerta, H., Miranda, D. M., Merino, J. M., Pavletic, L., Puhlhofer, G., Ribo, M., Fernandez, G. R., Ramirez, J. C. R., Vazquez, J. J. R., De Leon, A. R., Greus, F. S., Sanchez-Conde, M., Arroyo, M. S., Stanic, S., Striskovic, J., Swierk, P., Eldik, C. V., Acosta, M. V., Zivec, M., Astrophysique Interprétation Modélisation (AIM (UMR7158 / UMR_E_9005 / UM_112)), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-École polytechnique (X)-Centre National de la Recherche Scientifique (CNRS), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université de Montpellier (UM)-Centre National de la Recherche Scientifique (CNRS), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité), Galaxies, Etoiles, Physique, Instrumentation (GEPI), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS), Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire Midi-Pyrénées (OMP), Institut de Recherche pour le Développement (IRD)-Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Institut de Recherche pour le Développement (IRD)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Centre National de la Recherche Scientifique (CNRS), Université Sciences et Technologies - Bordeaux 1 (UB)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Abdalla H., Abe H., Acero F., Acharyya A., Adam R., Agudo I., Aguirre-Santaella A., Alfaro R., Alfaro J., Alispach C., Aloisio R., Batista R.A., Amati L., Amato E., Ambrosi G., Anguner E.O., Araudo A., Armstrong T., Arqueros F., Arrabito L., Asano K., Ascasibar Y., Ashley M., Backes M., Balazs C., Balbo M., Balmaverde B., Larriva A.B., Martins V.B., Barkov M., Baroncelli L., De Almeida U.B., Barrio J.A., Batista P.-I., Gonzalez J.B., Becherini Y., Beck G., Tjus J.B., Belmont R., Benbow W., Bernardini E., Berti A., Berton M., Bertucci B., Beshley V., Bi B., Biasuzzi B., Biland A., Bissaldi E., Biteau J., Blanch O., Bocchino F., Boisson C., Bolmont J., Bonanno G., Arbeletche L.B., Bonnoli G., Bordas P., Bottacini E., Bottcher M., Bozhilov V., Bregeon J., Brill A., Brown A.M., Bruno P., Bruno A., Bulgarelli A., Burton M., Buscemi M., Caccianiga A., Cameron R., Capasso M., Caprai M., Caproni A., Capuzzo-Dolcetta R., Caraveo P., Carosi R., Carosi A., Casanova S., Cascone E., Cauz D., Cerny K., Cerruti M., Chadwick P., Chaty S., Chen A., Chernyakova M., Chiaro G., Chiavassa A., Chytka L., Conforti V., Conte F., Contreras J.L., Coronado-Blazquez J., Cortina J., Costa A., Costantini H., Covino S., Cristofari P., Cuevas O., D'Ammando F., Daniel M.K., Davies J., Dazzi F., Angelis A.D., De Lavergne M.D.B., Caprio V.D., De Dos Anjos R.C., De Gouveia Dal Pino E.M., Lotto B.D., Martino D.D., De Naurois M., Wilhelmi E.D.O., Palma F.D., De Souza V., Delgado C., Ceca R.D., Volpe D.D., Depaoli D., Girolamo T.D., Pierro F.D., Diaz C., Diaz-Bahamondes C., Diebold S., Djannati-Atai A., Dmytriiev A., Dominguez A., Donini A., Dorner D., Doro M., Dournaux J., Dwarkadas V.V., Ebr J., Eckner C., Einecke S., Ekoume T.R.N., Elsasser D., Emery G., Evoli C., Fairbairn M., Falceta-Goncalves D., Fegan S., Feng Q., Ferrand G., Fiandrini E., Fiasson A., Fioretti V., Foffano L., Fonseca M.V., Font L., Fontaine G., Franco F.J., Coromina L.F., Fukami S., Fukazawa Y., Fukui Y., Gaggero D., Galanti G., Gammaldi V., Garcia E., Garczarczyk M., Gascon D., Gaug M., Gent A., Ghalumyan A., Ghirlanda G., Gianotti F., Giarrusso M., Giavitto G., Giglietto N., Giordano F., Glicenstein J., Goldoni P., Gonzalez J.M., Gourgouliatos K., Grabarczyk T., Grandi P., Granot J., Grasso D., Green J., Grube J., Gueta O., Gunji S., Halim A., Harvey M., Collado T.H., Hayashi K., Heller M., Cadena S.H., Hervet O., Hinton J., Hiroshima N., Hnatyk B., Hnatyk R., Hoffmann D., Hofmann W., Holder J., Horan D., Horandel J., Horvath P., Hovatta T., Hrabovsky M., Hrupec D., Hughes G., Hutten M., Iarlori M., Inada T., Inoue S., Insolia A., Ionica M., Iori M., Jacquemont M., Jamrozy M., Janecek P., Martinez I.J., Jin W., Jung-Richardt I., Jurysek J., Kaaret P., Karas V., Karkar S., Kawanaka N., Kerszberg D., Khelifi B., Kissmann R., Knodlseder J., Kobayashi Y., Kohri K., Komin N., Kong A., Kosack K., Kubo H., Palombara N.L., Lamanna G., Lang R.G., Lapington J., Laporte P., Lefaucheur J., Lemoine-Goumard M., Lenain J., Leone F., Leto G., Leuschner F., Lindfors E., Lloyd S., Lohse T., Lombardi S., Longo F., Lopez A., Lopez M., Lopez-Coto R., Loporchio S., Lucarelli F., Luque-Escamilla P.L., Lyard E., Maggio C., Majczyna A., Makariev M., Mallamaci M., Mandat D., Maneva G., Manganaro M., Manico G., Marcowith A., Marculewicz M., Markoff S., Marquez P., Marti J., Martinez O., Martinez M., Martinez G., Martinez-Huerta H., Maurin G., Mazin D., Mbarubucyeye J.D., Miranda D.M., Meyer M., Micanovic S., Miener T., Minev M., Miranda J.M., Mitchell A., Mizuno T., Mode B., Moderski R., Mohrmann L., Molina E., Montaruli T., Moralejo A., Merino J.M., Morcuende-Parrilla D., Morselli A., Mukherjee R., Mundell C., Murach T., Muraishi H., Nagai A., Nakamori T., Nemmen R., Niemiec J., Nieto D., Nievas M., Nikolajuk M., Nishijima K., Noda K., Nosek D., Nozaki S., O'Brien P., Ohira Y., Ohishi M., Oka T., Ong R.A., Orienti M., Orito R., Orlandini M., Orlando E., Osborne J.P., Ostrowski M., Oya I., Pagliaro A., Palatka M., Paneque D., Pantaleo F.R., Paredes J.M., Parmiggiani N., Patricelli B., Pavletic L., Pe'Er A., Pech M., Pecimotika M., Peresano M., Persic M., Petruk O., Pfrang K., Piatteli P., Pietropaolo E., Pillera R., Pilszyk B., Pimentel D., Pintore F., Pita S., Pohl M., Poireau V., Polo M., Prado R.R., Prast J., Principe G., Produit N., Prokoph H., Prouza M., Przybilski H., Pueschel E., Puhlhofer G., Pumo M.L., Punch M., Queiroz F., Quirrenbach A., Rando R., Razzaque S., Rebert E., Recchia S., Reichherzer P., Reimer O., Reimer A., Renier Y., Reposeur T., Rhode W., Ribeiro D., Ribo M., Richtler T., Rico J., Rieger F., Rizi V., Rodriguez J., Fernandez G.R., Ramirez J.C.R., Vazquez J.J.R., Romano P., Romeo G., Roncadelli M., Rosado J., De Leon A.R., Rowell G., Rudak B., Rujopakarn W., Russo F., Sadeh I., Saha L., Saito T., Greus F.S., Sanchez D., Sanchez-Conde M., Sangiorgi P., Sano H., Santander M., Santos E.M., Sanuy A., Sarkar S., Saturni F.G., Sawangwit U., Scherer A., Schleicher B., Schovanek P., Schussler F., Schwanke U., Sciacca E., Scuderi S., Arroyo M.S., Sergijenko O., Servillat M., Seweryn K., Shalchi A., Sharma P., Shellard R.C., Siejkowski H., Sinha A., Sliusar V., Slowikowska A., Sokolenko A., Sol H., Specovius A., Spencer S., Spiga D., Stamerra A., Stanic S., Starling R., Stolarczyk T., Straumann U., Striskovic J., Suda Y., Swierk P., Tagliaferri G., Takahashi H., Takahashi M., Tavecchio F., Taylor L., Tejedor L.A., Temnikov P., Terrier R., Terzic T., Testa V., Tian W., Tibaldo L., Tonev D., Torres D.F., Torresi E., Tosti L., Tothill N., Tovmassian G., Travnicek P., Truzzi S., Tuossenel F., Umana G., Vacula M., Vagelli V., Valentino M., Vallage B., Vallania P., Eldik C.V., Varner G.S., Vassiliev V., Acosta M.V., Vecchi M., Veh J., Vercellone S., Vergani S., Verguilov V., Vettolani G.P., Viana A., Vigorito C.F., Vitale V., Vorobiov S., Vovk I., Vuillaume T., Wagner S.J., Walter R., Watson J., White M., White R., Wiemann R., Wierzcholska A., Will M., Williams D.A., Wischnewski R., Wolter A., Yamazaki R., Yanagita S., Yang L., Yoshikoshi T., Zacharias M., Zaharijas G., Zaric D., Zavrtanik M., Zavrtanik D., Zdziarski A.A., Zech A., Zechlin H., Zhdanov V.I., Zivec M., ITA, USA, GBR, FRA, DEU, ESP, AUS, BRA, BGR, CHL, HRV, FIN, JPN, IRL, MEX, NAM, NLD, POL, CZE, SVN, SWE, CHE, UKR, Astronomy, High Energy Astrophys. & Astropart. Phys (API, FNWI), and Université Montpellier 2 - Sciences et Techniques (UM2)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université de Montpellier (UM)-Centre National de la Recherche Scientifique (CNRS)

Subjects
Gamma ray Astronomy, Cherenkov Telescope Array, axions, MATÉRIA ESCURA, redshift: dependence, Astronomy, Gamma ray experiments, gamma ray experiments, Astrophysics, 01 natural sciences, Cosmology, Observatory, cosmological model: parameter space, gamma ray experiment, High Energy Astrophysical Phenomena (astro-ph.HE), astro-ph.HE, Physics, Cherenkov telescopes, IACT technique, Gamma rays, Cosmic rays, new physics, 4. Education, Settore FIS/01 - Fisica Sperimentale, Astrophysics::Instrumentation and Methods for Astrophysics, Gamma-ray astronomy, violation: Lorentz, 3. Good health, observatory, Extragalactic background light, astro-ph.CO, axion-like particles, Física nuclear, Astrophysics - High Energy Astrophysical Phenomena, Astrophysics - Cosmology and Nongalactic Astrophysics, gamma ray: propagation, Cosmology and Nongalactic Astrophysics (astro-ph.CO), Active galactic nucleus, Axions, Astrophysics::High Energy Astrophysical Phenomena, Dark matter, FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, invariance: Lorentz, jet: relativistic, dark matter: halo, 0103 physical sciences, active galactic nuclei, extragalactic magnetic fields, AGN, Blazar, background, 010308 nuclear & particles physics, Física, Astronomy and Astrophysics, sensitivity, axion, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], absorption, statistical, Blazars, Telescopes
Abstract

Full list of authors: Abdalla, H.; Abe, H.; Acero, F.; Acharyya, A.; Adam, R.; Agudo, I; Aguirre-Santaella, A.; Alfaro, R.; Alfaro, J.; Alispach, C.; Aloisio, R.; Batista, R. Alves; Amati, L.; Amato, E.; Ambrosi, G.; Anguner, E. O.; Araudo, A.; Armstrong, T.; Arqueros, F.; Arrabito, L.; Asano, K.; Ascasibar, Y.; Ashley, M.; Backes, M.; Balazs, C.; Balbo, M.; Balmaverde, B.; Baquero Larriva, A.; Martins, V. Barbosa; Barkov, M.; Baroncelli, L.; de Almeida, U. Barres; Barrio, J. A.; Batista, P-, I; Becerra Gonzalez, J.; Becherini, Y.; Beck, G.; Tjus, J. Becker; Belmont, R.; Benbow, W.; Bernardini, E.; Berti, A.; Berton, M.; Bertucci, B.; Beshley, V; Bi, B.; Biasuzzi, B.; Biland, A.; Bissaldi, E.; Biteau, J.; Blanch, O.; Bocchino, F.; Boisson, C.; Bolmont, J.; Bonanno, G.; Arbeletche, L. Bonneau; Bonnoli, G.; Bordas, P.; Bottacini, E.; Bottcher, M.; Bozhilov, V; Bregeon, J.; Brill, A.; Brown, A. M.; Bruno, P.; Bruno, A.; Bulgarelli, A.; Burton, M.; Buscemi, M.; Caccianiga, A.; Cameron, R.; Capasso, M.; Caprai, M.; Caproni, A.; Capuzzo-Dolcetta, R.; Caraveo, P.; Carosi, R.; Carosi, A.; Casanova, S.; Cascone, E.; Cauz, D.; Cerny, K.; Cerruti, M.; Chadwick, P.; Chaty, S.; Chen, A.; Chernyakova, M.; Chiaro, G.; Chiavassa, A.; Chytka, L.; Conforti, V; Conte, F.; Contreras, J. L.; Coronado-Blazquez, J.; Cortina, J.; Costa, A.; Costantini, H.; Covino, S.; Cristofari, P.; Cuevas, O.; D'Ammando, F.; Daniel, M. K.; Davies, J.; Dazzi, F.; De Angelis, A.; de Lavergne, M. de Bony; De Caprio, V; dos Anjos, R. de Cassia; Dal Pino, E. M. de Gouveia; De Lotto, B.; De Martino, D.; de Naurois, M.; Wilhelmi, E. de Ona; De Palma, F.; de Souza, V; Delgado, C.; Della Ceca, R.; della Volpe, D.; Depaoli, D.; Di Girolamo, T.; Di Pierro, F.; Diaz, C.; Diaz-Bahamondes, C.; Diebold, S.; Djannati-Atai, A.; Dmytriiev, A.; Dominguez, A.; Donini, A.; Dorner, D.; Doro, M.; Dournaux, J.; Dwarkadas, V. V.; Ebr, J.; Eckner, C.; Einecke, S.; Ekoume, T. R. N.; Elsaesser, D.; Emery, G.; Evoli, C.; Fairbairn, M.; Falceta-Goncalves, D.; Fegan, S.; Feng, Q.; Ferrand, G.; Fiandrini, E.; Fiasson, A.; Fioretti, V; Foffano, L.; Fonseca, M., V; Font, L.; Fontaine, G.; Franco, F. J.; Freixas Coromina, L.; Fukami, S.; Fukazawa, Y.; Fukui, Y.; Gaggero, D.; Galanti, G.; Gammaldi, V; Garcia, E.; Garczarczyk, M.; Gascon, D.; Gaug, M.; Gent, A.; Ghalumyan, A.; Ghirlanda, G.; Gianotti, F.; Giarrusso, M.; Giavitto, G.; Giglietto, N.; Giordano, F.; Glicenstein, J.; Goldoni, P.; Gonzalez, J. M.; Gourgouliatos, K.; Grabarczyk, T.; Grandi, P.; Granot, J.; Grasso, D.; Green, J.; Grube, J.; Gueta, O.; Gunji, S.; Halim, A.; Harvey, M.; Collado, T. Hassan; Hayashi, K.; Heller, M.; Cadena, S. Hernandez; Hervet, O.; Hinton, J.; Hiroshima, N.; Hnatyk, B.; Hnatyk, R.; Hoffmann, D.; Hofmann, W.; Holder, J.; Horan, D.; Horandel, J.; Horvath, P.; Hovatta, T.; Hrabovsky, M.; Hrupec, D.; Hughes, G.; Hutten, M.; Iarlori, M.; Inada, T.; Inoue, S.; Insolia, A.; Ionica, M.; Iori, M.; Jacquemont, M.; Jamrozy, M.; Janecek, P.; Jimenez Martinez, I; Jin, W.; Jung-Richardt, I; Jurysek, J.; Kaaret, P.; Karas, V; Karkar, S.; Kawanaka, N.; Kerszberg, D.; Khelifi, B.; Kissmann, R.; Knodlseder, J.; Kobayashi, Y.; Kohri, K.; Komin, N.; Kong, A.; Kosack, K.; Kubo, H.; La Palombara, N.; Lamanna, G.; Lang, R. G.; Lapington, J.; Laporte, P.; Lefaucheur, J.; Lemoine-Goumard, M.; Lenain, J.; Leone, F.; Leto, G.; Leuschner, F.; Lindfors, E.; Lloyd, S.; Lohse, T.; Lombardi, S.; Longo, F.; Lopez, A.; Lopez, M.; Lopez-Coto, R.; Loporchio, S.; Lucarelli, F.; Luque-Escamilla, P. L.; Lyard, E.; Maggio, C.; Majczyna, A.; Makariev, M.; Mallamaci, M.; Mandat, D.; Maneva, G.; Manganaro, M.; Manico, G.; Marcowith, A.; Marculewicz, M.; Markoff, S.; Marquez, P.; Marti, J.; Martinez, O.; Martinez, M.; Martinez, G.; Martinez-Huerta, H.; Maurin, G.; Mazin, D.; Mbarubucyeye, J. D.; Miranda, D. Medina; Meyer, M.; Micanovic, S.; Miener, T.; Minev, M.; Miranda, J. M.; Mitchell, A.; Mizuno, T.; Mode, B.; Moderski, R.; Mohrmann, L.; Molina, E.; Montaruli, T.; Moralejo, A.; Morales Merino, J.; Morcuende-Parrilla, D.; Morselli, A.; Mukherjee, R.; Mundell, C.; Murach, T.; Muraishi, H.; Nagai, A.; Nakamori, T.; Nemmen, R.; Niemiec, J.; Nieto, D.; Nievas, M.; Nikolajuk, M.; Nishijima, K.; Noda, K.; Nosek, D.; Nozaki, S.; Ohira, Y.; Ohishi, M.; Oka, T.; Ong, R. A.; Orienti, M.; Orito, R.; Orlandini, M.; Orlando, E.; Osborne, J. P.; Ostrowski, M.; Oya, I; Pagliaro, A.; Palatka, M.; Paneque, D.; Pantaleo, F. R.; Paredes, J. M.; Parmiggiani, N.; Patricelli, B.; Pavletic, L.; Pe'er, A.; Pech, M.; Pecimotika, M.; Peresano, M.; Persic, M.; Petruk, O.; Pfrang, K.; Piatteli, P.; Pietropaolo, E.; Pillera, R.; Pilszyk, B.; Pimentel, D.; Pintore, F.; Pita, S.; Pohl, M.; Poireau, V; Polo, M.; Prado, R. R.; Prast, J.; Principe, G.; Produit, N.; Prokoph, H.; Prouza, M.; Przybilski, H.; Pueschel, E.; Puehlhofer, G.; Pumo, M. L.; Punch, M.; Queiroz, F.; Quirrenbach, A.; Rando, R.; Razzaque, S.; Rebert, E.; Recchia, S.; Reichherzer, P.; Reimer, O.; Reimer, A.; Renier, Y.; Reposeur, T.; Rhode, W.; Ribeiro, D.; Ribo, M.; Richtler, T.; Rico, J.; Rieger, F.; Rizi, V; Rodriguez, J.; Fernandez, G. Rodriguez; Ramirez, J. C. Rodriguez; Rodriguez Vazquez, J. J.; Romano, P.; Romeo, G.; Roncadelli, M.; Rosado, J.; de Leon, A. Rosales; Rowell, G.; Rudak, B.; Rujopakarn, W.; Russo, F.; Sadeh, I; Saha, L.; Saito, T.; Greus, F. Salesa; Sanchez, D.; Sanchez-Conde, M.; Sangiorgi, P.; Sano, H.; Santander, M.; Santos, E. M.; Sanuy, A.; Sarkar, S.; Saturni, F. G.; Sawangwit, U.; Scherer, A.; Schleicher, B.; Schovanek, P.; Schussler, F.; Schwanke, U.; Sciacca, E.; Scuderi, S.; Arroyo, M. Seglar; Sergijenko, O.; Servillat, M.; Seweryn, K.; Shalchi, A.; Sharma, P.; Shellard, R. C.; Siejkowski, H.; Sinha, A.; Sliusar, V; Slowikowska, A.; Sokolenko, A.; Sol, H.; Specovius, A.; Spencer, S.; Spiga, D.; Stamerra, A.; Starling, R.; Stolarczyk, T.; Straumann, U.; Striskovic, J.; Suda, Y.; Tagliaferri, G.; Takahashi, H.; Takahashi, M.; Tavecchio, F.; Taylor, L.; Tejedor, L. A.; Temnikov, P.; Terrier, R.; Terzic, T.; Testa, V; Tian, W.; Tibaldo, L.; Tonev, D.; Torres, D. F.; Torresi, E.; Tosti, L.; Tothill, N.; Tovmassian, G.; Travnicek, P.; Truzzi, S.; Tuossenel, F.; Umana, G.; Vacula, M.; Vagelli, V.; Valentino, M.; Vallage, B.; Vallania, P.; van Eldik, C.; Varner, G. S.; Vassiliev, V.; Vazquez Acosta, M.; Vecchi, M.; Veh, J.; Vercellone, S.; Vergani, S.; Verguilov, V.; Vettolani, G. P.; Viana, A.; Vigorito, C. F.; Vitale, V.; Vorobiov, S.; Vovk, I; Vuillaume, T.; Wagner, S. J.; Walter, R.; Watson, J.; White, M.; White, R.; Wiemann, R.; Wierzcholska, A.; Will, M.; Williams, D. A.; Wischnewski, R.; Wolter, A.; Yamazaki, R.; Yanagita, S.; Yang, L.; Yoshikoshi, T.; Zacharias, M.; Zaharijas, G.; Zaric, D.; Zavrtanik, M.; Zavrtanik, D.; Zdziarski, A. A.; Zech, A.; Zechlin, H.; Zhdanov, V., I; Zivec, M., The Cherenkov Telescope Array (CTA), the new-generation ground-based observatory for γ astronomy, provides unique capabilities to address significant open questions in astrophysics, cosmology, and fundamental physics. We study some of the salient areas of γ cosmology that can be explored as part of the Key Science Projects of CTA, through simulated observations of active galactic nuclei (AGN) and of their relativistic jets. Observations of AGN with CTA will enable a measurement of γ absorption on the extragalactic background light with a statistical uncertainty below 15% up to a redshift z=2 and to constrain or detect γ halos up to intergalactic-magnetic-field strengths of at least 0.3 pG . Extragalactic observations with CTA also show promising potential to probe physics beyond the Standard Model. The best limits on Lorentz invariance violation from γ astronomy will be improved by a factor of at least two to three. CTA will also probe the parameter space in which axion-like particles could constitute a significant fraction, if not all, of dark matter. We conclude on the synergies between CTA and other upcoming facilities that will foster the growth of γ cosmology. © 2021 IOP Publishing Ltd and Sissa Medialab., We gratefully acknowledge financial support from the following agencies and organizations: State Committee of Science of Armenia, Armenia; The Australian Research Council, Astronomy Australia Ltd, The University of Adelaide, Australian National University, Monash University, The University of New South Wales, The University of Sydney, Western Sydney University, Australia; Federal Ministry of Education, Science and Research, and Innsbruck University, Austria; Conselho Nacional de Desenvolvimento Científico e Tecnológico (CNPq), Fundação de Amparo à Pesquisa do Estado do Rio de Janeiro (FAPERJ), Fundação de Amparo à Pesquisa do Estado de São Paulo (FAPESP), Ministry of Science, Technology, Innovations and Communications (MCTIC), Brasil; Ministry of Education and Science, National RI Roadmap Project DO1-153/28.08.2018, Bulgaria; The Natural Sciences and Engineering Research Council of Canada and the Canadian Space Agency, Canada; CONICYT-Chile grants CATA AFB 170002, ANID PIA/APOYO AFB 180002, ACT 1406, FONDECYT-Chile grants, 1161463, 1170171, 1190886, 1171421, 1170345, 1201582, Gemini-ANID 32180007, Chile; Croatian Science Foundation, Rudjer Boskovic Institute, University of Osijek, University of Rijeka, University of Split, Faculty of Electrical Engineering, Mechanical Engineering and Naval Architecture, University of Zagreb, Faculty of Electrical Engineering and Computing, Croa tia; Ministry of Education, Youth and Sports, MEYS M2015046, LM2018105, LTT17006, EU/MEYS CZ.02.1.01/0.0/0.0/16_013/0001403, CZ.02.1.01/0.0/0.0/18_046/0016007 and CZ.02.1.01/0.0/0.0/16_019/0000754, Czech Republic; Academy of Finland (grant nr.317636 and 320045), Finland; Ministry of Higher Education and Research, CNRS-INSU and CNRS-IN2P3, CEA-Irfu, ANR, Regional Council Ile de France, Labex ENIGMASS, OCEVU, OSUG2020 and P2IO, France; Max Planck Society, BMBF, DESY, Helmholtz Association, Germany; Department of Atomic Energy, Department of Science and Technology, India; Istituto Nazionale di Astrofisica (INAF), Istituto Nazionale di Fisica Nucleare (INFN), MIUR, Istituto Nazionale di Astrofisica (INAF-OABRERA) Grant Fondazione Cariplo/Regione Lombardia ID 2014-1980/RST_ERC, Italy; ICRR, University of Tokyo, JSPS, MEXT, Japan; Netherlands Research School for Astronomy (NOVA), Netherlands Organization for Scientific Research (NWO), Netherlands; University of Oslo, Norway; Ministry of Science and Higher Education, DIR/WK/2017/12, the National Centre for Research and Development and the National Science Centre, UMO-2016/22/M/ST9/00583, Poland; Slovenian Research Agency, grants P1-0031, P1-0385, I0-0033, J1-9146, J1-1700, N1-0111, and the Young Researcher program, Slovenia; South African Department of Science and Technology and National Research Foundation through the South African Gamma-Ray Astronomy Programme, South Africa; The Spanish groups acknowledge the Spanish Ministry of Science and Innovation and the Spanish Research State Agency (AEI) through grants AYA2016-79724-C4-1-P, AYA2016-80889-P, AYA2016-76012-C3-1-P, BES-2016-076342, FPA2017-82729-C6-1-R, FPA2017-82729-C6-2-R, FPA2017-82729-C6-3-R, FPA2017-82729-C6-4-R, FPA2017-82729-C6-5-R, FPA2017-82729-C6-6-R, PGC2018-095161-B-I00, PGC2018-095512-B-I00, PID2019-107988GB-C22; the “Centro de Excelencia Severo Ochoa” program through grants no. SEV-2016-0597, SEV-2016-0588, SEV-2017-0709, CEX2019-000920-S; the “Unidad de Excelencia María de Maeztu” program through grant no. MDM-2015-0509; the “Ramón y Cajal” programme through grants RYC-2013-14511, RYC-2017-22665; and the MultiDark Consolider Network FPA2017-90566-REDC. They also acknowledge the Atracción de Talento contract no. 2016-T1/TIC-1542 granted by the Comunidad de Madrid; the “Postdoctoral Junior Leader Fellowship” programme from La Caixa Bank ing Foundation, grants no. LCF/BQ/LI18/11630014 and LCF/BQ/PI18/11630012; the “Programa Operativo” FEDER 2014-2020, Consejería de Economía y Conocimiento de la Junta de Andalucía (Ref. 1257737), PAIDI 2020 (Ref. P18-FR-1580) and Universidad de Jaén; “Programa Operativo de Crecimiento Inteligente” FEDER 2014-2020 (Ref. ESFRI-2017-IAC-12), Ministerio de Ciencia e Innovación, 15% co-financed by Consejería de Economía, Industria, Comercio y Conocimiento del Gobierno de Canarias; the Spanish AEI EQC2018-005094-P FEDER 2014-2020; the European Union’s “Horizon 2020” research and innovation programme under Marie Skłodowska-Curie grant agreement no. 665919; and the ESCAPE project with grant no. GA:824064; Swedish Research Council, Royal Physiographic Society of Lund, Royal Swedish Academy of Sciences, The Swedish National Infrastructure for Computing (SNIC) at Lunarc (Lund), Sweden; State Secretariat for Education, Research and Innovation (SERI) and Swiss National Science Foundation (SNSF), Switzerland; Durham University, Leverhulme Trust, Liverpool University, University of Leicester, University of Oxford, Royal Soci ety, Science and Technology Facilities Council, UK; U.S. National Science Foundation, U.S. Department of Energy, Argonne National Laboratory, Barnard College, University of California, University of Chicago, Columbia University, Georgia Institute of Technology, Institute for Nuclear and Particle Astrophysics (INPAC-MRPI program), Iowa State University, the Smithsonian Institution, Washington University McDonnell Center for the Space Sciences, The University of Wisconsin and the Wisconsin Alumni Research Foundation, USA. The research leading to these results has received funding from the European Union’s Seventh Framework Programme (FP7/2007-2013) under grant agreements No 262053 and No 317446. This project is receiving funding from the European Union’s Horizon 2020 research and innovation programs under agreement No 676134. The research leading to these results has received funding from the European Union’s Horizon 2020 research and innovation program under the Marie Skłodowska-Curie grant agreement GammaRayCascades No 843800. The Fermi LAT Collaboration acknowledges generous ongoing support from a number of agencies and institutes that have supported both the development and the operation of the LAT as well as scientific data analysis. These include the National Aeronautics and Space Administration and the Department of Energy in the United States, the Commissariat à l’Energie Atomique and the Centre National de la Recherche Scientifique / Institut National de Physique Nucléaire et de Physique des Particules in France, the Agenzia Spaziale Italiana and the Istituto Nazionale di Fisica Nucleare in Italy, the Ministry of Education, Culture, Sports, Science and Technology (MEXT), High Energy Accelerator Research Organization (KEK) and Japan Aerospace Exploration Agency (JAXA) in Japan, and the K. A. Wallenberg Foundation, the Swedish Research Council and the Swedish National Space Board in Sweden. Additional support for science analysis during the operations phase is gratefully acknowledged from the Istituto Nazionale di Astrofisica in Italy and the Centre National d’Études Spatiales in France. This work performed in part under DOE Contract DE-AC02-76SF00515.

Published
2021

30. Swift/UVOT follow-up of Gravitational Wave Alerts in the O3 era

Author

J. P. Osborne, A. Tohuvavohu, A. P. Beardmore, Joshua E. Schlieder, Caryl Gronwall, J. A. Kennea, Scott Barthelmy, E. Ambrosi, Regina Caputo, David Palmer, E. Troja, F. E. Marshall, A. J. Fenney, B. Sbarufatti, M. G. Bernardini, M. de Pasquale, Phil Evans, Sergio Campana, A. Melandri, Valerio D'Elia, S. R. Oates, Peter J. Brown, T. Sakamoto, Paolo Giommi, Hans A. Krimm, Dieter H. Hartmann, M. J. Page, S. Laha, Giancarlo Cusumano, C. Pagani, Antonino D'Ai, N. J. Klingler, G. Tagliaferri, M. Perri, D. Malesani, A. A. Breeveld, J. A. Nousek, S. B. Cenko, P. T. O'Brien, J. L. Racusin, N. P. M. Kuin, K. L. Page, M. H. Siegel, and P. D'Avanzo

Subjects
Swift, Physics, High Energy Astrophysical Phenomena (astro-ph.HE), Gravitational-wave observatory, Active galactic nucleus, Gravitational wave, Astrophysics::High Energy Astrophysical Phenomena, Astrophysics::Instrumentation and Methods for Astrophysics, Astronomy, FOS: Physical sciences, Astronomy and Astrophysics, Quasar, Astrophysics::Cosmology and Extragalactic Astrophysics, Light curve, Photometry (astronomy), gravitational waves, ultraviolet: general, Space and Planetary Science, Gamma-ray burst, Astrophysics - High Energy Astrophysical Phenomena, computer, Astrophysics::Galaxy Astrophysics, computer.programming_language
Abstract

In this paper, we report on the observational performance of the Swift Ultra-violet/Optical Telescope (UVOT) in response to the Gravitational Wave alerts announced by the Advanced Laser Interferometer Gravitational Wave Observatory and the Advanced Virgo detector during the O3 period. We provide the observational strategy for follow-up of GW alerts and provide an overview of the processing and analysis of candidate optical/UV sources. For the O3 period, we also provide a statistical overview and report on serendipitous sources discovered by Swift/UVOT. Swift followed 18 gravitational-wave candidate alerts, with UVOT observing a total of 424 deg^2. We found 27 sources that changed in magnitude at the 3 sigma level compared with archival u or g-band catalogued values. Swift/UVOT also followed up a further 13 sources reported by other facilities during the O3 period. Using catalogue information, we divided these 40 sources into five initial classifications: 11 candidate active galactic nuclei (AGN)/quasars, 3 Cataclysmic Variables (CVs), 9 supernovae, 11 unidentified sources that had archival photometry and 6 uncatalogued sources for which no archival photometry was available. We have no strong evidence to identify any of these transients as counterparts to the GW events. The 17 unclassified sources are likely a mix of AGN and a class of fast-evolving transient, and one source may be a CV., 25 pages, 6 figures and 5 tables. Submitted to MNRAS. Supplementary contains 23 pages with 8 figures and 1 table

Published
2021

31. Multi-messenger astrophysics with THESEUS in the 2030s

Author

Marica Branchesi, Lijing Shao, A. Gomboc, Stefanie Komossa, Luca Izzo, Gor Oganesyan, Bruce Gendre, Antonio Martin-Carrillo, Silvia Celli, Lorenzo Amati, Diego Götz, Nial R. Tanvir, S. Vinciguerra, J. P. Osborne, Antonio Capone, Irene Di Palma, Giancarlo Ghirlanda, S. Ronchini, Gavin P. Lamb, Roberto Mignani, Bing Zhang, René Hudec, Francesco Longo, Albert K. H. Kong, Michela Fasano, Dafne Guetta, Lorraine Hanlon, Antonios Nathanail, Andrea Rossi, Simone Dall'Osso, Emeric Le Floc'h, Riccardo Ciolfi, Enrico Bozzo, G. Stratta, Piero Rosati, S. Ascenzi, Luciano Rezzolla, Silvia Piranomonte, S. Turriziani, F. Schüssler, P. D'Avanzo, Eric Howell, Silvia Zane, Paolo Fermani, Ayden McCann, Sandro Mereghetti, Sylvain Chaty, Hüsne Dereli-Bégué, Eliana Palazzi, István T. Horváth, Jan Harms, Om Sharan Salafia, Sandra Savaglio, Stéphane Paltani, Lána Salmon, Asaf Pe'er, A. Zegarelli, Andrew Blain, S. D. Vergani, Liang Li, Stefan Grimm, Olga Sergijenko, fnmMassimiliano De Pasquale, Maurice H. P. M. van Putten, Yuji Urata, P. T. O'Brien, Astrophysique Interprétation Modélisation (AIM (UMR7158 / UMR_E_9005 / UM_112)), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), 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 Paris Cité (UPCité), Institut de Recherches sur les lois Fondamentales de l'Univers (IRFU), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay, Galaxies, Etoiles, Physique, Instrumentation (GEPI), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), 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), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Université de Paris (UP), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris Diderot - Paris 7 (UPD7)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL), Ciolfi, Riccardo, Stratta, Giulia, Branchesi, Marica, Gendre, Bruce, Grimm, Stefan, Harms, Jan, Paul Lamb, Gavin, Martin-Carrillo, Antonio, Mccann, Ayden, Oganesyan, Gor, Palazzi, Eliana, Ronchini, Samuele, Rossi, Andrea, Sharan Salafia, Om, Salmon, Lana, Ascenzi, Stefano, Capone, Antonio, Celli, Silvia, Dall???osso, Simone, Di Palma, Irene, Fasano, Michela, Fermani, Paolo, Guetta, Dafne, Hanlon, Lorraine, Howell, Eric, Paltani, Stephane, Rezzolla, Luciano, Vinciguerra, Serena, Zegarelli, Angela, Amati, Lorenzo, Blain, Andrew, Bozzo, Enrico, Chaty, Sylvain, D???avanzo, Paolo, De Pasquale, Fnmmassimiliano, Dereli-B??gu??, H??sne, Ghirlanda, Giancarlo, Gomboc, Andreja, G??tz, Diego, Horvath, Istvan, Hudec, Rene, Izzo, Luca, Le Floch, Emeric, Li, Liang, Longo, Francesco, Komossa, S., Kong, Albert K. H., Mereghetti, Sandro, Mignani, Roberto, Nathanail, Antonio, O???brien, Paul T., Osborne, Julian P., Pe???er, Asaf, Piranomonte, Silvia, Rosati, Piero, Savaglio, Sandra, Sch??ssler, Fabian, Sergijenko, Olga, Shao, Lijing, Tanvir, Nial, Turriziani, Sara, Urata, Yuji, van Putten, Maurice, Vergani, Susanna, Zane, Silvia, and Zhang, Bing

Subjects
HIGH-ENERGY NEUTRINOS, cosmological model, neutron star: binary, ELECTROMAGNETIC COUNTERPARTS, Compact binary merger, EXTENDED EMISSION, Astrophysics, 01 natural sciences, GRAVITATIONAL-WAVES, Cosmology, MAGNETAR, NEUTRON-STAR, 010303 astronomy & astrophysics, High Energy Astrophysical Phenomena (astro-ph.HE), GAMMA-RAY BURSTS, Physics, Hubble constant, Multi-messenger astrophysics, Gamma-ray burst, Kilonova, X-ray sources, Neutrino sources, Detection rate, Neutrino, Astrophysics - Instrumentation and Methods for Astrophysics, Astrophysics - High Energy Astrophysical Phenomena, Multi-messenger astrophysics, Gamma-ray burst, Compact binary merger, Kilonova, X-ray sources, Neutrino source, FOS: Physical sciences, Context (language use), gamma ray: burst, NO, electromagnetic field: production, X-ray source, neutrino: production, binary: coalescence, 0103 physical sciences, gamma ray: detector, X-ray: emission, [PHYS.PHYS.PHYS-INS-DET]Physics [physics]/Physics [physics]/Instrumentation and Detectors [physics.ins-det], Instrumentation and Methods for Astrophysics (astro-ph.IM), Neutrino source, LIGHT CURVES, 010308 nuclear & particles physics, Gravitational wave, Astronomy and Astrophysics, Multi-messenger astrophysic, neutrino: particle source, magnetar, redshift, binary: compact, gravitational radiation detector, detector: sensitivity, black hole: binary, Space and Planetary Science, gravitational radiation: emission, BLACK-HOLE, Fundamental physics, gravitational radiation: localization, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], astro-ph.IM, astro-ph.HE, X-ray: detector
Abstract

Multi-messenger astrophysics is becoming a major avenue to explore the Universe, with the potential to span a vast range of redshifts. The growing synergies between different probes is opening new frontiers, which promise profound insights into several aspects of fundamental physics and cosmology. In this context, THESEUS will play a central role during the 2030s in detecting and localizing the electromagnetic counterparts of gravitational wave and neutrino sources that the unprecedented sensitivity of next generation detectors will discover at much higher rates than the present. Here, we review the most important target signals from multi-messenger sources that THESEUS will be able to detect and characterize, discussing detection rate expectations and scientific impact., Submitted to Experimental Astronomy

Published
2021
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33. The super-soft source phase of the recurrent nova V3890 Sgr

Author

Marina Orio, P. Bezak, K. L. Page, Ciro Pinto, B. Vander Meulen, A. Dobrotka, S. G. Starrfield, J. P. Osborne, J. U. Ness, K. P. Singh, J. J. Drake, and A. P. Beardmore

Subjects
High Energy Astrophysical Phenomena (astro-ph.HE), Physics, Space and Planetary Science, Phase (waves), FOS: Physical sciences, Astronomy and Astrophysics, Nova (laser), Astrophysics, Astrophysics - High Energy Astrophysical Phenomena
Abstract

The 30-year recurrent symbiotic nova V3890 Sgr exploded 2019 August 28 and was observed with multiple X-ray telescopes. An XMM-Newton observation during the SSS phase captured a high degree of X-ray variability including a deep dip in the middle of the observation, an initial rise of similar depth and shape and, after the deep dip, smaller dips of 10% amplitude, which might be periodic over 18.1-minutes. An eclipse model of the dips yields clump sizes and orbital radii of 0.5-8 and 5-150 white dwarf radii, respectively. The simultaneous UV light curve shows no significant variations beyond slow fading. The RGS spectrum contains both residual shock emission at short wavelengths and the SSS emission at longer wavelengths. The shock temperature has clearly decreased compared to an earlier Chandra observation (day 6). The dip spectrum is dominated by emission lines like in U Sco. The intensity of underlying blackbody-like emission is much lower with the blackbody normalisation yielding a similar radius as during the brighter phases, while the lower bolometric luminosity is ascribed to lower T_eff. This would be inconsistent with clump occultations unless Compton scattering of the continuum emission reduces the photon energies to mimic a lower effective temperature. However, systematic uncertainties are high. The absorption lines in the bright SSS spectrum are blue-shifted by 870+/-10 km/s before the dip and 900+/-10 km/s, after the dip. The reproduction of the observed spectrum is astonishing, especially that only a single absorbing layer is necessary while three such layers are needed to reproduce the RGS spectrum of V2491 Cyg. The ejecta of V3890 Sgr are thus more homogeneous than many other SSS spectra indicate. Abundance determination is in principle possible but highly uncertain. Generally, solar abundances are found except for N and possibly O higher by an order of magnitude., Accepted for A&A

Published
2022

34. The 2016 January eruption of recurrent Nova LMC 1968

Author

P. Mróz, Robert D. Gehrz, Radosław Poleski, A. P. Beardmore, Nidia Morrell, F. M. Walter, Andrzej Udalski, U. Munari, Michał K. Szymański, Rodolfo Angeloni, A. Evans, Martin Henze, M. J. Darnley, S. G. Starrfield, Greg J. Schwarz, Steven Williams, J. P. Osborne, A. A. Breeveld, Igor Soszyński, Jan Skowron, S. N. Shore, N. P. M. Kuin, Terry Bohlsen, F. Di Mille, V. A. R. M. Ribeiro, K. L. Page, National Science Centre (Poland), Foundation for Polish Science, Ministerio de Economía y Competitividad (España), National Aeronautics and Space Administration (US), National Science Foundation (US), and Fundação para a Ciência e a Tecnologia (Portugal)

Subjects
Binaries: eclipsing, Astrophysics, 01 natural sciences, Luminosity, symbols.namesake, X-rays: binaries, QB460, 0103 physical sciences, Roche lobe, Large Magellanic Cloud, Ejecta, 010303 astronomy & astrophysics, Novae, QB600, QC, QB, Physics, Cataclysmic variables, GE, Stars: individual: (Nova LMC 1968), 010308 nuclear & particles physics, eclipsing [Binaries], White dwarf, Astronomy and Astrophysics, Light curve, Supernova, Ultraviolet: stars, 13. Climate action, Space and Planetary Science, Eddington luminosity, symbols, binaries [X-rays], individual: (Nova LMC 1968) [Stars], stars [Ultraviolet], QB799
Abstract

We present a comprehensive review of all observations of the eclipsing recurrent Nova LMC 1968 in the Large Magellanic Cloud which was previously observed in eruption in 1968, 1990, 2002, 2010, and most recently in 2016. We derive a probable recurrence time of 6.2 ± 1.2 yr and provide the ephemerides of the eclipse. In the ultraviolet-optical-IR photometry the light curve shows high variability right from the first observation around 2 d after eruption. Therefore no colour changes can be substantiated. Outburst spectra from 2016 and 1990 are very similar and are dominated by H and He lines longward of 2000 Å. Interstellar reddening is found to be E(B − V) = 0.07 ± 0.01. The super soft X-ray luminosity is lower than the Eddington luminosity and the X-ray spectra suggest the mass of the white dwarf (WD) is larger than 1.3 M☉. Eclipses in the light curve suggest that the system is at high orbital inclination. On day 4 after the eruption a recombination wave was observed in Fe II ultraviolet absorption lines. Narrow-line components are seen after day 6 and explained as being due to reionization of ejecta from a previous eruption. The UV spectrum varies with orbital phase, in particular a component of the He II 1640 Å emission line, which leads us to propose that early-on the inner WD Roche lobe might be filled with a bound opaque medium prior to the re-formation of an accretion disc. Both this medium and the ejecta can cause the delay in the appearance of the soft X-ray source., The OGLE project received funding by the National Science Center, Poland, under grant MAESTRO 2014/14/A/ST9/00121 to AU. PM acknowledges support from the Foundation for Polish Science (Program START). NPMK, KLP, AAB, APB, and JPO acknowledge support from the U.K. Space Agency. MH acknowledges the support of the Spanish Ministry of Economy and Competitiveness (MINECO) under the grant FDPI-2013-16933. SS acknowledges partial support from NASA, HST, and NSF grants to ASU. Research in Novae at Stony Brook University is supported in part by NSF grant AST 1614113, with additional research support provided by the Stony Brook University. RDG was supported by NASA and the United States Air Force. VARMR acknowledges financial support from the Fundação para a Ciência e a Tecnologia (FCT) in the form of an exploratory project of reference IF/00498/2015, from the Center for Research & Development in Mathematics and Applications (CIDMA) strategic project UID/MAT/04106/2019, and supported by Enabling Green E-science for the Square Kilometre Array Research Infrastructure (ENGAGE-SKA), POCI-01-0145-FEDER-022217, and PHOBOS, POCI-01-0145-FEDER-029932, funded by Programa Operacional Competitividade e Internacionalização (COMPETE 2020) and FCT, Portugal. RA acknowledges financial support from DIDULS Regular PR#17142 by Universidad de La Serena.

Published
2020

35. Impact of collection method on assessment of semen HIV RNA viral load.

Author

Brendan J W Osborne, Prameet M Sheth, Colin Kovacs, Tony Mazzulli, and Rupert Kaul

Subjects
Medicine, Science
Abstract

The blood HIV RNA viral load is the best-defined predictor of HIV transmission, in part due to ease of measurement and the correlation of blood and genital tract (semen or cervico-vaginal) viral load, although recent studies found semen HIV RNA concentration to be a stronger predictor of HIV transmission. There is currently no standardized method for semen collection when measuring HIV RNA concentration. Therefore, we compared two collection techniques in order to study of the impact of antiretroviral therapy on the semen viral load.Semen was collected by masturbation from HIV-infected, therapy-naïve men who have sex with men (MSM) either undiluted (Visit 1) or directly into transport medium (Visit 2). Seminal plasma was then isolated, and the HIV RNA concentration obtained with each collection technique was measured and corrected for dilution if necessary. Collection of semen directly into transport medium resulted in a median HIV RNA viral load that was 0.4 log10 higher than undiluted samples.The method of semen collection is an important consideration when quantifying the HIV RNA viral load in this compartment.

Published
2011
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36. Redbay Ambrosia Beetle-Laurel Wilt Pathogen: A Potential Major Problem for the Florida Avocado Industry

Author

Jonathan H. Crane, Jorge E. Peña, and J. L. Osborne

Subjects
HS379, Agriculture (General), S1-972, Plant culture, SB1-1110, Biology (General), QH301-705.5
Abstract

HS1136, a 7-page illustrated factsheet by Jonathan H. Crane, Jorge Peña, and J.L. Osborne, describes this insect-fungal pest attacking woody plants in the laurel family, including avocado. Includes descriptions, origin, detection and spread of the pest, plant hosts in the U.S., a map of counties with the beetle, plant host symptoms and damage, management strategies & restrictions, agencies working on the issue, research and extension efforts, and references. Published by the UF Department of Horticultural Sciences, February 2008. Revised December 2008.

Published
2008

37. Investigating the nature of the INTEGRAL gamma-ray bursts and sub-threshold triggers with Swift follow-up

Author

Antonia Rowlinson, J. P. Osborne, Sandro Mereghetti, D. Gotz, K. Wiersema, A. J. Bird, Thomas J. Maccarone, N. Gehrels, Nial R. Tanvir, P. T. O'Brien, R. L. C. Starling, A. B. Higgins, 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), 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), High Energy Astrophys. & Astropart. Phys (API, FNWI), Laboratoire AIM, Université Paris Diderot - Paris 7 ( UPD7 ) -Centre d'Etudes de Saclay, and Astrophysique Interprétation Modélisation (AIM (UMR7158 / UMR_E_9005 / UM_112))

Subjects
Swift, Active galactic nucleus, 010504 meteorology & atmospheric sciences, [ PHYS.ASTR ] Physics [physics]/Astrophysics [astro-ph], Astrophysics::High Energy Astrophysical Phenomena, Population, FOS: Physical sciences, Astrophysics, 01 natural sciences, Coincident, 0103 physical sciences, education, 010303 astronomy & astrophysics, Alert system, 0105 earth and related environmental sciences, computer.programming_language, High Energy Astrophysical Phenomena (astro-ph.HE), Physics, education.field_of_study, Low fluence, Astronomy and Astrophysics, Space and Planetary Science, Sub threshold, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Astrophysics - High Energy Astrophysical Phenomena, Gamma-ray burst, computer
Abstract

We explore the potential of INTEGRAL to improve our understanding of the low fluence regime for explosive transients, such as GRBs. We probe the nature of the so-called "WEAK" INTEGRAL triggers, when the gamma-ray instruments record intensity spikes that are below the usual STRONG significance thresholds. In a targeted Swift follow-up campaign, we observed 15 WEAK triggers. We find six of these can be classified as GRBs. This includes GRB150305A, a GRB discovered from our campaign alone. We also identified a source coincident with one trigger, IGRW151019, as a candidate AGN. We show that real events such as GRBs exist within the IBAS WEAK trigger population. A comparison of the fluence distributions of the full INTEGRAL IBAS and Swift BAT GRB samples showed that the two are similar. We also find correlations between the prompt gamma-ray and X-ray properties of the two samples, supporting previous investigations. We find that both satellites reach similar, low fluence levels regularly, although Swift is more sensitive to short, low fluence GRBs., 12 pages, 8 figures, accepted by MNRAS. Minor typos changed and a reference added

Published
2017

38. Neil Gehrels Swift Observatory studies of supersoft novae

Author

J. P. Osborne, K. L. Page, and A. P. Beardmore

Subjects
High Energy Astrophysical Phenomena (astro-ph.HE), Swift, Atmospheric Science, History, 010504 meteorology & atmospheric sciences, FOS: Physical sciences, Aerospace Engineering, Astronomy, Astronomy and Astrophysics, 01 natural sciences, Geophysics, Space and Planetary Science, Observatory, 0103 physical sciences, General Earth and Planetary Sciences, Astrophysics - High Energy Astrophysical Phenomena, 010303 astronomy & astrophysics, computer, Rapid response, 0105 earth and related environmental sciences, computer.programming_language
Abstract

The rapid response capabilities of the Neil Gehrels Swift Observatory, together with the daily planning of its observing schedule, make it an ideal mission for following novae in the X-ray and UV bands, particularly during their early phases of rapid evolution and throughout the supersoft source interval. Many novae, both classical and recurrent, have been extensively monitored by Swift throughout their supersoft phase and later decline. We collect here results from observations of novae with outbursts which occurred between the start of 2006 and the end of 2017., 54 pages, 33 figure panels, 2 tables. To be published in a Special Issue of Advances in Space Research, entitled "Nova Eruptions, Cataclysmic Variables and Related Systems: observational vs theoretical challenges in the 2020 era", following COSPAR 2018

Published
2019

39. X-ray properties of two transient ULX candidates in galaxy NGC 7090

Author

J. P. Osborne, P. T. O'Brien, Phil Evans, Zhu Liu, and K. L. Page

Subjects
High Energy Astrophysical Phenomena (astro-ph.HE), Physics, 010308 nuclear & particles physics, Star (game theory), Astrophysics::High Energy Astrophysical Phenomena, X-ray, FOS: Physical sciences, Flux, Astronomy and Astrophysics, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Compact star, 01 natural sciences, Spectral line, Galaxy, Luminosity, Space and Planetary Science, 0103 physical sciences, Astrophysics::Solar and Stellar Astrophysics, Astrophysics::Earth and Planetary Astrophysics, Astrophysics - High Energy Astrophysical Phenomena, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics
Abstract

We report the X-ray data analysis of two transient ultraluminous X-ray sources (ULXs, hereafter X1 and X2) located in the nearby galaxy NGC 7090. While they were not detected in the 2004 XMM-Newton and 2005 Chandra observations, their 0.3-10 keV X-ray luminosities reached $>3\times10^{39}\,\mathrm{erg\,s^{-1}}$ in later XMM-Newton or Swift observations, showing increases in flux by a factor of $>80$ and $>300$ for X1 and X2, respectively. X1 showed indications of spectral variability: at the highest luminosity, its X-ray spectra can be fitted with a powerlaw ($\Gamma=1.55\pm0.15$), or a multicolour disc model with $T_{\mathrm{in}}=2.07^{+0.30}_{-0.23}$ keV; the X-ray spectrum became softer ($\Gamma=2.67^{+0.69}_{-0.64}$), or cooler ($T_\mathrm{in}=0.64^{+0.28}_{-0.17}$ keV) at lower luminosity. No strong evidence for spectral variability was found for X2. Its X-ray spectra can be fitted with a simple powerlaw model ($\Gamma=1.61^{+0.55}_{-0.50}$), or a multicolour disc model ($1.69^{+1.17}_{-0.48}$ keV). A possible optical counterpart for X1 is revealed in HST imaging. No optical variability is found, indicating that the optical radiation may be dominated by the companion star. Future X-ray and optical observations are necessary to determine the true nature of the compact object., Comment: Accepted for publication in MNRAS, 7 pages, 3 figures

Published
2019

40. 2SXPS: An improved and expanded Swift X-ray telescope point source catalog

Author

K. L. Page, Gianpiero Tagliaferri, Phil Evans, S. B. Cenko, J. P. Osborne, David N. Burrows, Richard Willingale, J. A. Kennea, M. Perri, Milvia Capalbi, and A. P. Beardmore

Subjects
Point spread function, Physics, High Energy Astrophysical Phenomena (astro-ph.HE), 010308 nuclear & particles physics, Stray light, Point source, media_common.quotation_subject, FOS: Physical sciences, Astronomy and Astrophysics, X-ray telescope, Astrophysics, Light curve, 01 natural sciences, law.invention, Telescope, Space and Planetary Science, Observatory, law, Sky, 0103 physical sciences, Astrophysics - Instrumentation and Methods for Astrophysics, Astrophysics - High Energy Astrophysical Phenomena, 010303 astronomy & astrophysics, Instrumentation and Methods for Astrophysics (astro-ph.IM), media_common
Abstract

We present the 2SXPS (Swift-XRT Point Source) catalog, containing 206,335 point sources detected by the Swift X-ray Telescope (XRT) in the 0.3--10 keV energy range. This catalog represents a significant improvement over 1SXPS, with double the sky coverage (now 3,790 deg$^2$), and several significant developments in source detection and classification. In particular, we present for the first time techniques to model the effect of stray light -- significantly reducing the number of spurious sources detected. These techniques will be very important for future, large effective area X-ray mission such as the forthcoming Athena X-ray observatory. We also present a new model of the XRT point spread function, and a method for correctly localising and characterising piled up sources. We provide light curves -- in four energy bands, two hardness ratios and two binning timescales -- for every source, and from these deduce that over 80,000 of the sources in 2SXPS are variable in at least one band or hardness ratio. The catalog data can be queried or downloaded via a bespoke web interface at https://www.swift.ac.uk/2SXPS, via HEASARC, or in Vizier (IX/58)., Comment: Accepted for publication in ApJS, 20 pages, 7 figures, plus appendices of 18 pages, 3 figures

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

Author

Michael H. Siegel, Judith Racusin, J. A. Kennea, Hans A. Krimm, N. P. M. Kuin, David Palmer, B. Sbarufatti, Dieter H. Hartmann, A. Tohuvavohu, M. Perri, S. R. Oates, M. de Pasquale, A. A. Breeveld, N. J. Klingler, S. W. K. Emery, Gianpiero Tagliaferri, Frank Marshall, Sergio Campana, A. Y. Lien, Valerio D'Elia, Caryl Gronwall, Peter J. Brown, A. Melandri, D. B. Malesani, Phil Evans, Paolo Giommi, J. P. Osborne, A. P. Beardmore, Javier A. García, P. D'Avanzo, T. Sakamoto, K. L. Page, Antonino D'Ai, Scott Barthelmy, David N. Burrows, Eleonora Troja, Giancarlo Cusumano, J. A. Nousek, P. T. O'Brien, S. B. Cenko, ITA, USA, and GBR

Subjects
Active galactic nucleus, media_common.quotation_subject, Astrophysics::High Energy Astrophysical Phenomena, Population, FOS: Physical sciences, Astrophysics, Surveys, X-ray sources, 01 natural sciences, Gravitational waves, Observatory, 0103 physical sciences, Astronomy data analysis, Gamma-ray bursts, X-ray surveys, Catalogs, Gravitational wave sources, education, 010303 astronomy & astrophysics, media_common, High Energy Astrophysical Phenomena (astro-ph.HE), Physics, education.field_of_study, 010308 nuclear & particles physics, Gravitational wave, Astronomy and Astrophysics, LIGO, Neutron star, Space and Planetary Science, Sky, Astrophysics - High Energy Astrophysical Phenomena, Gamma-ray burst
Abstract

The Neil Gehrels Swift Observatory carried out prompt searches for gravitational wave (GW) events detected by the LIGO/Virgo Collaboration (LVC) during the second observing run ("O2"). Swift performed extensive tiling of eight LVC triggers, two of which had very low false-alarm rates (GW 170814 and the epochal GW 170817), indicating a high confidence of being astrophysical in origin; the latter was the first GW event to have an electromagnetic counterpart detected. In this paper we describe the follow-up performed during O2 and the results of our searches. No GW electromagnetic counterparts were detected; this result is expected, as GW 170817 remained the only astrophysical event containing at least one neutron star after LVC's later retraction of some events. A number of X-ray sources were detected, with the majority of identified sources being active galactic nuclei. We discuss the detection rate of transient X-ray sources and their implications in the O2 tiling searches. Finally, we describe the lessons learned during O2, and how these are being used to improve the \swift\ follow-up of GW events. In particular, we simulate a population of GRB afterglows to evaluate our source ranking system's ability to differentiate them from unrelated and uncatalogued X-ray sources. We find that $\approx$60-70% of afterglows whose jets are oriented towards Earth will be given high rank (i.e., "interesting" designation) by the completion of our second follow-up phase (assuming their location in the sky was observed), but that this fraction can be increased to nearly 100% by performing a third follow-up observation of sources exhibiting fading behavior., Comment: 18 pages, 4 figures, 2 tables, accepted for publication in ApJS

Published
2019

42. Optimization of the Swift X-ray follow-up of Advanced LIGO and Virgo gravitational wave triggers in 2015–16

Author

Nial R. Tanvir, J. A. Kennea, N. Gehrels, Judith Racusin, P. A. Evans, J. P. Osborne, David N. Burrows, S. B. Cenko, P. T. O'Brien, Sergio Campana, ITA, USA, and GBR

Subjects
High Energy Astrophysical Phenomena (astro-ph.HE), Physics, 010308 nuclear & particles physics, Gravitational wave, Astrophysics::High Energy Astrophysical Phenomena, FOS: Physical sciences, Astronomy, Astronomy and Astrophysics, X-ray telescope, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, 01 natural sciences, LIGO, Galaxy, Afterglow, Neutron star, Space and Planetary Science, 0103 physical sciences, Binary star, Astrophysics - High Energy Astrophysical Phenomena, Gamma-ray burst, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics
Abstract

One of the most exciting near-term prospects in physics is the potential discovery of gravitational waves by the advanced LIGO and Virgo detectors. To maximise both the confidence of the detection and the science return, it is essential to identify an electromagnetic counterpart. This is not trivial, as the events are expected to be poorly localised, particularly in the near-term, with error regions covering hundreds or even thousands of square degrees. In this paper we discuss the prospects for finding an X-ray counterpart to a gravitational wave trigger with the Swift X-ray Telescope, using the assumption that the trigger is caused by a binary neutron star merger which also produces a short gamma-ray burst. We show that it is beneficial to target galaxies within the GW error region, highlighting the need for substantially complete galaxy catalogues out to distances of 300 Mpc. We also show that nearby, on-axis short GRBs are either extremely rare, or are systematically less luminous than those detected to date. We consider the prospects for detecting afterglow emission from an an off-axis GRB which triggered the GW facilities, finding that the detectability, and the best time to look, are strongly dependent on the characteristics of the burst such as circumburst density and our viewing angle., Comment: 17 pages, 14 figures. Accepted for publication in MNRAS

Published
2015

43. Design and implementation of electron diverters for lobster eye space-based X-ray optics

Author

Dennis J. Chornay, Paul Houghton, Christopher Bicknell, James F. Pearson, K Keresztes, Richard Willingale, S S Sachdev, J. P. Osborne, Tony Crawford, Charlotte Feldman, Adrian Martindale, Steve Sembay, and V Aslanyan

Subjects
010302 applied physics, Physics, business.industry, Astrophysics::High Energy Astrophysical Phenomena, Detector, Astrophysics::Instrumentation and Methods for Astrophysics, Magnetosphere, X-ray optics, Electron, 01 natural sciences, 010305 fluids & plasmas, law.invention, Telescope, Solar wind, Optics, law, Magnet, Physics::Space Physics, 0103 physical sciences, Ionosphere, business, Instrumentation
Abstract

Micropore optics have recently been implemented in a lobster eye geometry as a compact X-ray telescope. Fields generated by rare-earth magnets are used to reduce the flux of energetic electrons incident upon the focal plane detector in such a setup. We present the design and implementation of the electron diverters for X-ray telescopes of two upcoming missions: the microchannel X-ray telescope onboard the space-based multiband astronomical variable objects monitor and the soft X-ray instrument onboard the solar wind magnetosphere ionosphere link explorer. Electron diverters must be configured to conform to stringent limits on their total magnetic dipole moment and be compensated for any net moment arising from manufacturing errors. The two missions have differing designs, which are presented and evaluated in terms of the fractions of electrons reaching the detector, as determined by relativistic calculations of electron trajectories. The differential flux of electrons to the detector is calculated, and the integrated electron background is determined for both designs.

Published
2019

44. THESEUS: A key space mission concept for Multi-Messenger Astrophysics

Author

F. Fuschino, Ruben Salvaterra, F. Frontera, M. Branchesi, Bruce Gendre, U. Maio, Stefano Covino, Tomaz Rodic, Giancarlo Ghirlanda, Serena Vinciguerra, D. Mereghetti, Andrea Rossi, Lorenzo Amati, Diego Götz, M. H. P. M. van Putten, Monica Colpi, Roberto Mignani, P. D'Avanzo, Riccardo Campana, Eliana Palazzi, Andrea Bulgarelli, M. G. Bernardini, Valerio D'Elia, Jochen Greiner, Elisabetta Maiorano, Enzo Brocato, Joseph Caruana, Piero Rosati, R. L. C. Starling, Nial Tanvir, Riccardo Ciolfi, G. Stratta, S. D. Vergani, S. Colafrancesco, Claudio Labanti, Bing Zhang, Dorottya Szécsi, M. Razzano, Enrico Bozzo, Antonio Stamerra, D. Malesani, René Hudec, Francesco Longo, Luciano Rezzolla, S. Piranomonte, M. de Pasquale, Richard Willingale, B. Patricelli, J. P. Osborne, P. T. O'Brien, Peter G. Jonker, Luciano Nicastro, C. Guidorzi, Aniello Grado, M. Boer, Alessandro Drago, Maria Giovanna Dainotti, Carole Mundell, Centre d'étude spatiale des rayonnements (CESR), Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire Midi-Pyrénées (OMP), Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS), Istituto di Astrofisica Spaziale e Fisica Cosmica - Milano (IASF-MI), Istituto Nazionale di Astrofisica (INAF), ISDC Data Centre for Astrophysics, University of Geneva [Switzerland], INAF - Osservatorio Astronomico di Brera (OAB), University of Ferrara [Ferrara], Institut de Recherches sur les lois Fondamentales de l'Univers (IRFU), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay, Department of Physics and Astronomy [Leicester], University of Leicester, Max-Planck-Institut für Extraterrestrische Physik (MPE), Mullard Space Science Laboratory (MSSL), University College of London [London] (UCL), INAF - Osservatorio Astronomico di Roma (OAR), INAF-IASF Milano, Observatoire de Haute-Provence (OHP), Institut Pythéas (OSU PYTHEAS), Institut de Recherche pour le Développement (IRD)-Aix Marseille Université (AMU)-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Aix Marseille Université (AMU)-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Centre National de la Recherche Scientifique (CNRS), ASI-Science Data Center, Rome, Laboratori Nazionali di Frascati (LNF), National Institute for Nuclear Physics (INFN), Laboratoire d'Astrophysique de Marseille (LAM), Aix Marseille Université (AMU)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS), Astronomical Institute of the Czech Academy of Sciences, Czech Academy of Sciences [Prague] (ASCR), Department of Astrophysics [Nijmegen], Institute for Mathematics, Astrophysics and Particle Physics (IMAPP), Radboud university [Nijmegen]-Radboud university [Nijmegen], Dark Cosmology Centre (DARK), Niels Bohr Institute [Copenhagen] (NBI), Faculty of Science [Copenhagen], University of Copenhagen = Københavns Universitet (KU)-University of Copenhagen = Københavns Universitet (KU)-Faculty of Science [Copenhagen], University of Copenhagen = Københavns Universitet (KU)-University of Copenhagen = Københavns Universitet (KU), CNR Institute of Atmospheric Sciences and Climate (ISAC), Consiglio Nazionale delle Ricerche (CNR), Observatoire de Paris - Site de Meudon (OBSPM), Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Centre National de la Recherche Scientifique (CNRS), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire Midi-Pyrénées (OMP), Institut de Recherche pour le Développement (IRD)-Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Institut de Recherche pour le Développement (IRD)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Centre National de la Recherche Scientifique (CNRS), Université de Genève = University of Geneva (UNIGE), Università degli Studi di Ferrara = University of Ferrara (UniFE), Istituto Nazionale di Fisica Nucleare (INFN), Astronomical Institute of the Czech Academy of Sciences (ASU / CAS), Czech Academy of Sciences [Prague] (CAS), Radboud University [Nijmegen]-Radboud University [Nijmegen], University of Copenhagen = Københavns Universitet (UCPH)-University of Copenhagen = Københavns Universitet (UCPH)-Faculty of Science [Copenhagen], University of Copenhagen = Københavns Universitet (UCPH)-University of Copenhagen = Københavns Universitet (UCPH), National Research Council of Italy | Consiglio Nazionale delle Ricerche (CNR), Galaxies, Etoiles, Physique, Instrumentation (GEPI), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Département d'Astrophysique (ex SAP) (DAP), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay, Astrophysique Relativiste Théories Expériences Métrologie Instrumentation Signaux (ARTEMIS), Université Nice Sophia Antipolis (... - 2019) (UNS), COMUE Université Côte d'Azur (2015 - 2019) (COMUE UCA)-COMUE Université Côte d'Azur (2015 - 2019) (COMUE UCA)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de la Côte d'Azur, Université Côte d'Azur (UCA)-COMUE Université Côte d'Azur (2015 - 2019) (COMUE UCA)-Université Côte d'Azur (UCA)-Centre National de la Recherche Scientifique (CNRS), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS), Laboratoire Univers et Particules de Montpellier (LUPM), Université Montpellier 2 - Sciences et Techniques (UM2)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université de Montpellier (UM)-Centre National de la Recherche Scientifique (CNRS), THESEUS, Stratta, G., Ciolfi, R., Amati, L., Bozzo, E., Ghirlanda, G., Maiorano, E., Nicastro, L., Rossi, A., Vinciguerra, S., Frontera, F., Götz, D., Guidorzi, C., O'Brien, P., Osborne, J. P., Tanvir, N., Branchesi, M., Brocato, E., Dainotti, M. G., De Pasquale, M., Grado, A., Greiner, J., Longo, F., Maio, U., Mereghetti, D., Mignani, R., Piranomonte, S., Rezzolla, L., Salvaterra, R., Starling, R., Willingale, R., Böer, M., Bulgarelli, A., Caruana, J., Colafrancesco, S., Colpi, M., Covino, S., D'Avanzo, P., D'Elia, V., Drago, A., Fuschino, F., Gendre, B., Hudec, R., Jonker, P., Labanti, C., Malesani, D., Mundell, C. G., Palazzi, E., Patricelli, B., Razzano, M., Campana, R., Rosati, P., Rodic, T., Szécsi, D., Stamerra, A., van Putten, M., Vergani, S., Zhang, B., Bernardini, M., Observatoire Midi-Pyrénées (OMP), Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées, Università degli Studi di Ferrara (UniFE), Aix Marseille Université (AMU)-Centre National de la Recherche Scientifique (CNRS)-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Institut de Recherche pour le Développement (IRD)-Aix Marseille Université (AMU)-Centre National de la Recherche Scientifique (CNRS)-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Institut de Recherche pour le Développement (IRD), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris Diderot - Paris 7 (UPD7)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL), Stratta, G, Ciolfi, R, Amati, L, Bozzo, E, Ghirlanda, G, Maiorano, E, Nicastro, L, Rossi, A, Vinciguerra, S, Frontera, F, Götz, D, Guidorzi, C, O'Brien, P, Osborne, J, Tanvir, N, Branchesi, M, Brocato, E, Dainotti, M, De Pasquale, M, Grado, A, Greiner, J, Longo, F, Maio, U, Mereghetti, D, Mignani, R, Piranomonte, S, Rezzolla, L, Salvaterra, R, Starling, R, Willingale, R, Böer, M, Bulgarelli, A, Caruana, J, Colafrancesco, S, Colpi, M, Covino, S, D'Avanzo, P, D'Elia, V, Drago, A, Fuschino, F, Gendre, B, Hudec, R, Jonker, P, Labanti, C, Malesani, D, Mundell, C, Palazzi, E, Patricelli, B, Razzano, M, Campana, R, Rosati, P, Rodic, T, Szécsi, D, Stamerra, A, van Putten, M, Vergani, S, Zhang, B, and Bernardini, M

Subjects
Atmospheric Science, Computer science, Astronomy, Astronomical and space-research instrumentation, Gamma-ray bursts, Gamma-ray sources, X-ray bursts, X-ray sources, Aerospace Engineering, Space and Planetary Science, Astrophysics, 01 natural sciences, Economica, astronomical and space-research instrumentation, 010303 astronomy & astrophysics, ComputingMilieux_MISCELLANEOUS, media_common, High Energy Astrophysical Phenomena (astro-ph.HE), [PHYS]Physics [physics], energy: high, gamma-ray bursts, Gamma-ray source, neutrino: detector, Geophysics, Upgrade, Neutrino detector, upgrade, Neutrino, Astrophysics - High Energy Astrophysical Phenomena, Cosmic Vision, media_common.quotation_subject, FOS: Physical sciences, Context (language use), frequency: high, X-ray source, 0103 physical sciences, gravitational radiation: frequency, Gamma-ray burst, X-ray burst, gamma-ray sources, 010308 nuclear & particles physics, Gravitational wave, family: 3, Astronomy and Astrophysics, gravitational radiation detector, Universe, messenger, electromagnetic, General Earth and Planetary Sciences, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph]
Abstract

The recent discovery of the electromagnetic counterpart of the gravitational wave source GW170817, has demonstrated the huge informative power of multi-messenger observations. During the next decade the nascent field of multi-messenger astronomy will mature significantly. Around 2030, third generation gravitational wave detectors will be roughly ten times more sensitive than the current ones. At the same time, neutrino detectors currently upgrading to multi km^3 telescopes, will include a 10 km^3 facility in the Southern hemisphere that is expected to be operational around 2030. In this review, we describe the most promising high frequency gravitational wave and neutrino sources that will be detected in the next two decades. In this context, we show the important role of the Transient High Energy Sky and Early Universe Surveyor (THESEUS), a mission concept proposed to ESA by a large international collaboration in response to the call for the Cosmic Vision Programme M5 missions. THESEUS aims at providing a substantial advancement in early Universe science as well as playing a fundamental role in multi-messenger and time-domain astrophysics, operating in strong synergy with future gravitational wave and neutrino detectors as well as major ground- and space-based telescopes. This review is an extension of the THESEUS white paper (Amati et al. 2017), also in light of the discovery of GW170817/GRB170817A that was announced on October 16th, 2017., Comment: 25 pages, 13 figures, accepted to Advances in Space Research with minor revisions. Details on the THESEUS instrumentation, science case and expected performances can also be found in Amati et al. 2017 (arXiv:1710.04638) and in the presentations of the THESEUS Workshop 2017 (http://www.isdc.unige.ch/theseus/workshop2017-programme.html). v2 few typos corrected

Published
2018

45. Constraints on Minute-Scale Transient Astrophysical Neutrino Sources

Author

M. G. Aartsen, M. Ackermann, J. Adams, J. A. Aguilar, M. Ahlers, M. Ahrens, I. Al Samarai, D. Altmann, K. Andeen, T. Anderson, I. Ansseau, G. Anton, C. Argüelles, J. Auffenberg, S. Axani, P. Backes, H. Bagherpour, X. Bai, A. Barbano, J. P. Barron, S. W. Barwick, V. Baum, R. Bay, J. J. Beatty, J. Becker Tjus, K.-H. Becker, S. BenZvi, D. Berley, E. Bernardini, D. Z. Besson, G. Binder, D. Bindig, E. Blaufuss, S. Blot, C. Bohm, M. Börner, F. Bos, S. Böser, O. Botner, E. Bourbeau, J. Bourbeau, F. Bradascio, J. Braun, M. Brenzke, H.-P. Bretz, S. Bron, J. Brostean-Kaiser, A. Burgman, R. S. Busse, T. Carver, E. Cheung, D. Chirkin, A. Christov, K. Clark, L. Classen, G. H. Collin, J. M. Conrad, P. Coppin, P. Correa, D. F. Cowen, R. Cross, P. Dave, M. Day, J. P. A. M. de André, C. De Clercq, J. J. DeLaunay, H. Dembinski, K. Deoskar, S. De Ridder, P. Desiati, K. D. de Vries, G. de Wasseige, M. de With, T. DeYoung, J. C. Díaz-Vélez, V. di Lorenzo, H. Dujmovic, J. P. Dumm, M. Dunkman, E. Dvorak, B. Eberhardt, T. Ehrhardt, B. Eichmann, P. Eller, P. A. Evans, P. A. Evenson, S. Fahey, A. R. Fazely, J. Felde, K. Filimonov, C. Finley, A. Franckowiak, E. Friedman, A. Fritz, T. K. Gaisser, J. Gallagher, E. Ganster, L. Gerhardt, K. Ghorbani, W. Giang, T. Glauch, T. Glüsenkamp, A. Goldschmidt, J. G. Gonzalez, D. Grant, Z. Griffith, C. Haack, A. Hallgren, L. Halve, F. Halzen, K. Hanson, D. Hebecker, D. Heereman, K. Helbing, R. Hellauer, S. Hickford, J. Hignight, G. C. Hill, K. D. Hoffman, R. Hoffmann, T. Hoinka, B. Hokanson-Fasig, K. Hoshina, F. Huang, M. Huber, K. Hultqvist, M. Hünnefeld, R. Hussain, S. In, N. Iovine, A. Ishihara, E. Jacobi, G. S. Japaridze, M. Jeong, K. Jero, B. J. P. Jones, P. Kalaczynski, W. Kang, A. Kappes, D. Kappesser, T. Karg, A. Karle, U. Katz, M. Kauer, A. Keivani, J. L. Kelley, A. Kheirandish, J. Kim, T. Kintscher, J. Kiryluk, T. Kittler, S. R. Klein, R. Koirala, H. Kolanoski, L. Köpke, C. Kopper, S. Kopper, J. P. Koschinsky, D. J. Koskinen, M. Kowalski, K. Krings, M. Kroll, G. Krückl, S. Kunwar, N. Kurahashi, A. Kyriacou, M. Labare, J. L. Lanfranchi, M. J. Larson, F. Lauber, K. Leonard, M. Leuermann, Q. R. Liu, E. Lohfink, C. J. Lozano Mariscal, L. Lu, J. Lünemann, W. Luszczak, J. Madsen, G. Maggi, K. B. M. Mahn, Y. Makino, S. Mancina, I. C. Mariş, R. Maruyama, K. Mase, R. Maunu, K. Meagher, M. Medici, M. Meier, T. Menne, G. Merino, T. Meures, S. Miarecki, J. Micallef, G. Momenté, T. Montaruli, R. W. Moore, M. Moulai, R. Nagai, R. Nahnhauer, P. Nakarmi, U. Naumann, G. Neer, H. Niederhausen, S. C. Nowicki, D. R. Nygren, A. Obertacke Pollmann, A. Olivas, A. O’Murchadha, J. P. Osborne, E. O’Sullivan, T. Palczewski, H. Pandya, D. V. Pankova, P. Peiffer, J. A. Pepper, C. Pérez de los Heros, D. Pieloth, E. Pinat, A. Pizzuto, M. Plum, P. B. Price, G. T. Przybylski, C. Raab, M. Rameez, L. Rauch, K. Rawlins, I. C. Rea, R. Reimann, B. Relethford, G. Renzi, E. Resconi, W. Rhode, M. Richman, S. Robertson, M. Rongen, C. Rott, T. Ruhe, D. Ryckbosch, D. Rysewyk, I. Safa, S. E. Sanchez Herrera, A. Sandrock, J. Sandroos, M. Santander, S. Sarkar, K. Satalecka, M. Schaufel, P. Schlunder, T. Schmidt, A. Schneider, J. Schneider, S. Schöneberg, L. Schumacher, S. Sclafani, D. Seckel, S. Seunarine, J. Soedingrekso, D. Soldin, M. Song, G. M. Spiczak, C. Spiering, J. Stachurska, M. Stamatikos, T. Stanev, A. Stasik, R. Stein, J. Stettner, A. Steuer, T. Stezelberger, R. G. Stokstad, A. Stößl, N. L. Strotjohann, T. Stuttard, G. W. Sullivan, M. Sutherland, I. Taboada, F. Tenholt, S. Ter-Antonyan, A. Terliuk, S. Tilav, P. A. Toale, M. N. Tobin, C. Tönnis, S. Toscano, D. Tosi, M. Tselengidou, C. F. Tung, A. Turcati, C. F. Turley, B. Ty, E. Unger, M. A. Unland Elorrieta, M. Usner, J. Vandenbroucke, W. Van Driessche, D. van Eijk, N. van Eijndhoven, S. Vanheule, J. van Santen, M. Vraeghe, C. Walck, A. Wallace, M. Wallraff, F. D. Wandler, N. Wandkowsky, T. B. Watson, A. Waza, C. Weaver, M. J. Weiss, C. Wendt, J. Werthebach, S. Westerhoff, B. J. Whelan, N. Whitehorn, K. Wiebe, C. H. Wiebusch, L. Wille, D. R. Williams, L. Wills, M. Wolf, J. Wood, T. R. Wood, E. Woolsey, K. Woschnagg, G. Wrede, D. L. Xu, X. W. Xu, Y. Xu, J. P. Yanez, G. Yodh, S. Yoshida, T. Yuan, Physics, Faculty of Sciences and Bioengineering Sciences, Vriendenkring VUB, and Elementary Particle Physics

Subjects
HIGH-ENERGY NEUTRINOS, Astrophysics::High Energy Astrophysical Phenomena, Population, General Physics and Astronomy, FOS: Physical sciences, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, 7. Clean energy, 0103 physical sciences, Muon neutrino, ddc:530, education, 010303 astronomy & astrophysics, Physics, GAMMA-RAY BURSTS, High Energy Astrophysical Phenomena (astro-ph.HE), education.field_of_study, Muon, 010308 nuclear & particles physics, Supernova, Neutron star, Physics and Astronomy, 13. Climate action, Physique des particules élémentaires, High Energy Physics::Experiment, Neutrino, Gamma-ray burst, Astrophysics - High Energy Astrophysical Phenomena, Energy (signal processing)
Abstract

High-energy neutrino emission has been predicted for several short-lived astrophysical transients including gamma-ray bursts (GRBs), core-collapse supernovae with choked jets, and neutron star mergers. IceCube's optical and x-ray follow-up program searches for such transient sources by looking for two or more muon neutrino candidates in directional coincidence and arriving within 100 s. The measured rate of neutrino alerts is consistent with the expected rate of chance coincidences of atmospheric background events and no likely electromagnetic counterparts have been identified in Swift follow-up observations. Here, we calculate generic bounds on the neutrino flux of short-lived transient sources. Assuming an E-2.5 neutrino spectrum, we find that the neutrino flux of rare sources, like long gamma-ray bursts, is constrained to, 0, SCOPUS: ar.j, info:eu-repo/semantics/published

Published
2018
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46. A Multimessenger Picture of the Flaring Blazar TXS 0506+056: implications for High-Energy Neutrino Emission and Cosmic Ray Acceleration

Author

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

47. MXT instrument on-board the French-Chinese SVOM mission

Author

A. Meuris, Diego Götz, Vadim Burwitz, F. Gonzalez, Albert Gomes, Charlotte Feldman, Laurent Perraud, Richard Willingale, F. Pinsard, James F. Pearson, Narjiss Boufracha, Paul Drumm, P. T. O'Brien, Norbert Meidinger, Pierre Pasqier, Martin Boutelier, Estelle Raynal, J. P. Osborne, Jean Michel Le Duigou, K. Mercier, and Marie Claire Charmeau

Subjects
On board, Computer science, Payload, Real-time computing, X-ray telescope, Gamma-ray burst
Abstract

The SVOM (Space-based multi-band astronomical Variable Objects Monitor) French-Chinese mission is dedicated to the detection, localization and study of Gamma Ray Bursts (GRBs) and other high-energy transient phenomena. We first present the general description of the French payload composed of the ECLAIRs instrument, dedicated to GRB detection and localization and the MXT instrument, dedicated to GRB follow-up observation in soft X-ray band. Then the paper describes more in detail the design and the performances of the MXT instrument, finally a status of MXT development will be given.

Published
2018

48. Superhumps linked to X-ray emission. The superoutbursts of SSS J122221.7-311525 and GW Lib

Author

Vitaly Neustroev, Erik Kuulkers, J. P. Osborne, Sergey Zharikov, Christian Knigge, Tom Marsh, A. P. Beardmore, Valery F. Suleimanov, and K. L. Page

Subjects
High Energy Astrophysical Phenomena (astro-ph.HE), Physics, 010504 meteorology & atmospheric sciences, Accretion (meteorology), FOS: Physical sciences, Flux, White dwarf, Astronomy and Astrophysics, Context (language use), Astrophysics, Light curve, 01 natural sciences, SSS, Space and Planetary Science, U Geminorum, 0103 physical sciences, Astrophysics - High Energy Astrophysical Phenomena, 010303 astronomy & astrophysics, Dwarf nova, 0105 earth and related environmental sciences
Abstract

[Abridged] We present more than 4 years of Swift X-ray observations of the 2013 superoutburst, subsequent decline and quiescence of the WZ Sge-type dwarf nova SSS J122221.7-311525 (SSS122222) from 6 days after discovery. Only a handful of WZ Sge-type dwarf novae have been observed in X-rays, and until recently GW Lib was the only binary of this type with complete coverage of an X-ray light curve throughout a superoutburst. We collected extensive X-ray data of a second such system to understand the extent to which the unexpected properties of GW Lib are common to the WZ Sge class. We analysed the X-ray light curve and compared it with the behaviour of superhumps which were detected in the optical light curve. We also performed spectral analysis of the data. The results were compared with the properties of GW Lib, for which new X-ray observations were also obtained. SSS122222 was variable and around five times brighter in 0.3-10 keV X-rays during the superoutburst than in quiescence, mainly because of a significant strengthening of a high-energy component of the X-ray spectrum. The post-outburst decline of the X-ray flux lasted at least 500 d. The data show no evidence of the expected optically thick boundary layer in the system during the outburst. SSS122222 also exhibited a sudden X-ray flux change in the middle of the superoutburst, which occurred exactly at the time of the superhump stage transition. A similar X-ray behaviour was also detected in GW Lib. This result demonstrates a relationship between the outer disc and the white dwarf boundary layer for the first time, and suggests that models for accretion discs in high mass ratio accreting binaries are currently incomplete. The very long decline to X-ray quiescence is also in strong contrast to the expectation of low viscosity in the disc after outburst., 12 pages, 6 figures. Accepted for publication in A&A (abstract abridged). This paper is a sequel to arXiv:1701.03134

Published
2018

49. GRB171205A/SN2017iuk: A local low-luminosity gamma-ray burst

Author

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

Published
2018
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50. What we learn from the X-Ray grating spectra of Nova SMC 2016

Author

Gloria Sala, Stefano Ciroi, E. Aydi, Robert E. Williams, J. P. Osborne, K. L. Page, David A. H. Buckley, Marina Orio, Ehud Behar, Polina Zemko, Charles E. Woodward, Thomas Rauch, A. Dobrotka, Sumner Starrfield, M. Della Valle, Margarita Hernanz, Martin Henze, N. Ospina, Efrain Gatuzz, Jan-Uwe Ness, Universitat Politècnica de Catalunya. Departament de Física, and Universitat Politècnica de Catalunya. GAA - Grup d'Astronomia i Astrofísica

Subjects
Astrofísica, stars: abundances, 010504 meteorology & atmospheric sciences, education, stars: individual (N SMC 2016a), chemistry.chemical_element, FOS: Physical sciences, X-rays: stars, Astrophysics, 01 natural sciences, Spectral line, 0103 physical sciences, 010303 astronomy & astrophysics, novae, cataclysmic variables, stars: dwarf novae, 0105 earth and related environmental sciences, stars [X-rays], Physics, High Energy Astrophysical Phenomena (astro-ph.HE), novae, cataclysmic variables, Argon, Atmospheric models, White dwarf, Astronomy and Astrophysics, Effective temperature, Light curve, Interstellar medium, abundances [stars], individual (N SMC 2016a) [stars], chemistry, Space and Planetary Science, Física::Astronomia i astrofísica [Àrees temàtiques de la UPC], dwarf novae [stars], Small Magellanic Cloud, Astrophysics - High Energy Astrophysical Phenomena
Abstract

Nova SMC 2016 has been the most luminous nova known in the direction of the Magellanic Clouds. It turned into a very luminous supersoft X-ray source between day 16 and 28 after the optical maximum. We observed it with Chandra, the HRC-S camera and the Low Energy Transmission Grating (LETG) on 2016 November and 2017 January (days 39 and 88 after optical maximum), and with XMM-Newton on 2016 December (day 75). We detected the compact white dwarf (WD) spectrum as a luminous supersoft X-ray continuum with deep absorption features of carbon, nitrogen, magnesium, calcium, probably argon and sulfur on day 39, and oxygen, nitrogen and carbon on days 75 and 88. The spectral features attributed to the WD atmosphere are all blue-shifted, by about 1800 km/s on day 39 and up to 2100 km/s in the following observations. Spectral lines attributed to low ionization potential transitions in the interstellar medium are also observed. Assuming the distance of the Small Magellanic Cloud, the bolometric luminosity exceeded Eddington level for at least three months. A preliminary analysis with atmospheric models indicates effective temperature around 700,000 K on day 39, peaking at the later dates in the 850,000-900,000 K range, as expected for a 1.25 m(sol) WD. We suggest a possible classification as an oxygen-neon WD, but more precise modeling is needed to accurately determine the abundances. The X-ray light curves show large, aperiodic ux variability, not associated with spectral variability. We detected red noise, but did not find periodic or quasi-periodic modulations., Accepted for publication in the Astrophysical Journal, pending final editorial review after "minor changes"

Published
2018
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