Professor Rob Fender: Publications

An artist's impression of a relativistic jet propagating away from a black hole at close to the speed of light. Such jets are formed by the inner regions of the accretion flow: matter flowing inwards towards the black hole, via processes which are not yet fully understood. The accretion flow emits primarily in X-rays, the relativistic jet in the radio band: by combing observations in each band we can try and understand how such jets form and how much energy they carry away from the black hole.

High-energy gamma-ray observations of the accreting black hole V404 Cygni during its June 2015 outburst

(2016)

Authors:

A Loh, S Corbel, G Dubus, J Rodriguez, I Grenier, T Hovatta, T Pearson, A Readhead, R Fender, K Mooley

Localization and broadband follow-up of the gravitational-wave transient GW150914

Astrophysical Journal Letters American Astronomical Society 826:1 (2016) L13-L13

Authors:

BP Abbott, R Abbott, TD Abbott, F Acernese, K Ackley, C Adams, T Adams, P Addesso, RX Adhikari, VB Adya, C Affeldt, M Agathos, K Agatsuma, N Aggarwal, OD Aguiar, L Aiello, A Ain, P Ajith, B Allen, A Allocca, PA Altin, SB Anderson, WG Anderson, MC Araya

Abstract:

A gravitational-wave (GW) transient was identified in data recorded by the Advanced Laser Interferometer Gravitational-wave Observatory (LIGO) detectors on 2015 September 14. The event, initially designated G184098 and later given the name GW150914, is described in detail elsewhere. By prior arrangement, preliminary estimates of the time, significance, and sky location of the event were shared with 63 teams of observers covering radio, optical, near-infrared, X-ray, and gamma-ray wavelengths with ground- and space-based facilities. In this Letter we describe the low-latency analysis of the GW data and present the sky localization of the first observed compact binary merger. We summarize the follow-up observations reported by 25 teams via private Gamma-ray Coordinates Network circulars, giving an overview of the participating facilities, the GW sky localization coverage, the timeline, and depth of the observations. As this event turned out to be a binary black hole merger, there is little expectation of a detectable electromagnetic (EM) signature. Nevertheless, this first broadband campaign to search for a counterpart of an Advanced LIGO source represents a milestone and highlights the broad capabilities of the transient astronomy community and the observing strategies that have been developed to pursue neutron star binary merger events. Detailed investigations of the EM data and results of the EM follow-up campaign are being disseminated in papers by the individual teams.

Supplement: “Localization and broadband follow-up of the gravitational-wave transient GW150914” (2016, ApJL, 826, L13)

Astrophysical Journal Supplement Series American Astronomical Society 225:8 (2016) 1-15

Authors:

BP Abbott, R Abbott, TD Abbott, Ian Heywood

Abstract:

This Supplement provides 91̽��ing material for Abbott et al. (2016a). We briefly summarize past electromagnetic (EM) follow-up efforts as well as the organization and policy of the current EM follow-up program. We compare the four probability sky maps produced for the gravitational-wave transient GW150914, and provide additional details of the EM follow-up observations that were performed in the different bands.

XIPE: the x-ray imaging polarimetry explorer

Proceedings of SPIE--the International Society for Optical Engineering SPIE, the international society for optics and photonics (2016) 990515-990515-20

Authors:

Paolo Soffitta, Ronaldo Bellazzini, Enrico Bozzo, Vadim Burwitz, Alberto Castro Tirado, Enrico Costa, Thierry Courvoisier, Hua Feng, Szymon Gburek, Rene' Goosmann, Vladimir Karas, Giorgio Matt, Fabio Muleri, Kirpal Nandra, Mark Pearce, Juri Poutanen, Victor Reglero, Maria Dolores Graziati, Andrea Santangelo, Gianpiero Tagliaferri, Christopher Tenzer, Jacco Vink, Martin Weisskopf, Silvia Zane, I Agudo, A Antonelli, P Attina, L Baldini, A Bykov, R Carpentiero, E Cavazzuti, E Churazov, E Del Monte, D De Martino, I Donnarumma, V Doroshenko, Y Evangelista, I Ferreira, E Gallo, N Grosso, P Kaaret, E Kuulkers, J Laranaga, L Latronico, DH Lumb, J Macian, J Malzac, F Marin, E Massaro, M Minuti, C Mundell, JU Ness, T Oosterbroek, S Paltani, G Pareschi, R Perna, P-O Petrucci, HB Pinazo, M Pinchera, JP Rodriguez, M Roncadelli, A Santovincenzo, S Sazonov, C Sgro, D Spiga, J Svoboda, C Theobald, T Theodorou, R Turolla, E Wilhelmi de Ona, B Winter, AM Akbar, H Allan, R Aloisio, D Altamirano, L Amati, E Amato, E Angelakis, J Arezu, J-L Atteia, M Axelsson, M Bachetti, L Ballo, S Balman, R Bandiera, X Barcons, S Basso, A Baykal, W Becker, E Behar, B Beheshtipour, R Belmont, E Berger, F Bernardini, S Bianchi, G Bisnovatyi-Kogan, P Blasi, P Blay, A Bodaghee, M Boer, M Boettcher, S Bogdanov, I Bombaci, R Bonino, J Braga, W Brandt, A Brez, N Bucciantini, L Burderi, I Caiazzo, R Campana, S Campana, F Capitanio, M Cappi, M Cardillo, P Casella, O Catmabacak, B Cenko, P Cerda-Duran, C Cerruti, S Chaty, M Chauvin, Y Chen, J Chenevez, M Chernyakova, CCT Cheung, D Christodoulou, P Connell, R Corbet, F Coti Zelati, S Covino, W Cui, G Cusumano, A D’Ai, F D’Ammando, M Dadina, Z Dai, A De Rosa, L de Ruvo, N Degenaar, M Del Santo, L Del Zanna, G Dewangan, S Di Cosimo, N Di Lalla, G Di Persio, T Di Salvo, T Dias, C Done, M Dovciak, G Doyle, L Ducci, R Elsner, T Enoto, J Escada, P Esposito, C Eyles, S Fabiani, M Falanga, S Falocco, Y Fan, R Fender, M Feroci, C Ferrigno, W Forman, L Foschini, C Fragile, F Fuerst, Y Fujita, JL Gasent-Blesa, J Gelfand, B Gendre, G Ghirlanda, G Ghisellini, M Giroletti, D Goetz, E Gogus, J-L Gomez, D Gonzalez, R Gonzalez-Riestra, E Gotthelf, L Gou, P Grandi, V Grinberg, F Grise, C Guidorzi, N Gurlebeck, T Guver, D Haggard, M Hardcastle, D Hartmann, C Haswell, A Heger, M Hernanz, J Heyl, L Ho, J Hoormann, J Horak, J Huovelin, D Huppenkothen, R Iaria, C Inam Sitki, A Ingram, G Israel, L Izzo, M Burgess, M Jackson, L Ji, J Jiang, T Johannsen, C Jones, S Jorstad, JJE Kajava, M Kalamkar, E Kalemci, T Kallman, A Kamble, F Kislat, M Kiss, D Klochkov, E Koerding, M Kolehmainen, K Koljonen, S Komossa, A Kong, S Korpela, M Kowalinski, H Krawczynski, I Kreykenbohm, M Kuss, D Lai, M Lan, J Larsson, S Laycock, D Lazzati, D Leahy, H Li, J Li, L Li, T Li, Z Li, M Linares, M Lister, H Liu, G Lodato, A Lohfink, F Longo, G Luna, A Lutovinov, S Mahmoodifar, J Maia, V Mainieri, C Maitra, D Maitra, A Majczyna, S Maldera, D Malyshev, A Manfreda, A Manousakis, R Manuel, R Margutti, A Marinucci, S Markoff, A Marscher, H Marshall, F Massaro, M McLaughlin, G Medina-Tanco, M Mehdipour, M Middleton, R Mignani, P Mimica, T Mineo, B Mingo, G Miniutti, SM Mirac, G Morlino, AV Motlagh, S Motta, A Mushtukov, S Nagataki, F Nardini, J Nattila, GJ Navarro, B Negri, Matteo Negro, S Nenonen, V Neustroev, F Nicastro, A Norton, A Nucita, P O’Brien, S O’Dell, S Turriziani

Corrigendum: A large light-mass component of cosmic rays at 1017-1017.5 electronvolts from radio observations.

Nature Nature Publishing Group 537:7621 (2016) 572

Authors:

S Buitink, A Corstanje, H Falcke, T Huege, A Nelles, JP Rachen, L Rossetto, P Schellart, O Scholten, S Ter Veen, S Thoudam, TNG Trinh, J Anderson, A Asgekar, IM Avruch, ME Bell, MJ Bentum, G Bernardi, P Best, A Bonafede, F Breitling, JW Broderick, WN Brouw, M Brüggen, HR Butcher, D Carbone, B Ciardi, JE Conway, F de Gasperin, E de Geus, A Deller, R-J Dettmar, G van Diepen, S Duscha, J Eislöffel, D Engels, JE Enriquez, RA Fallows, Robert P Fender, C Ferrari, W Frieswijk, MA Garrett, JM Grießmeier, AW Gunst, van van Haarlem, TE Hassall, G Heald, JWT Hessels, M Hoeft

Abstract:

In this Letter, we omitted to cite preliminary results from the low-energy extension of the Pierre Auger Observatory, as presented at the International Cosmic Ray Conference 2015 (ref. 1). Figure 1 of this Corrigendum shows measurements of the average value of Xmax for the Low Frequency Array (LOFAR), and earlier experiments using different techniques, now including the data from the Pierre Auger Observatory1 , specifically the contribution of A. Porcelli. Our values are in agreement with those of ref. 1 within systematic uncertainties.

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