31 research outputs found
HexagDLy—Processing hexagonally sampled data with CNNs in PyTorch
No full textHexagDLy is a Python-library extending the PyTorch deep learning framework with convolution and pooling operations on hexagonal grids. It aims to ease the access to convolutional neural networks for applications that rely on hexagonally sampled data as, for example, commonly found in ground-based astroparticle physics experiments. Keywords: Convolutional neural networks, Hexagonal grid, PyTorch, Astroparticle physic
Proceedings of Patient Reported Outcome Measure’s (PROMs) Conference Sheffield 2016: advances in patient reported outcomes research
Get PDFTable of contents S1 Using computerized adaptive testing Tim Croudace S2 Well-being: what is it, how does it compare to health and what are the implications of using it to inform health policy John Brazier O1 “Am I going to get better?”—Using PROMs to inform patients about the likely benefit of surgery Nils Gutacker, Andrew Street O2 Identifying Patient Reported Outcome Measures for an electronic Personal Health Record Dan Robotham, Samantha Waterman, Diana Rose, Safarina Satkunanathan, Til Wykes O3 Examining the change process over time qualitatively: transformative learning and response shift Nasrin Nasr, Pamela Enderby O4 Developing a PROM to evaluate self-management in diabetes (HASMID): giving patients a voice Jill Carlton, Donna Rowen, Jackie Elliott, John Brazier, Katherine Stevens, Hasan Basarir, Alex Labeit O5 Development of the Primary Care Outcomes Questionnaire (PCOQ) Mairead Murphy, Sandra Hollinghurst, Chris Salisbury O6 Developing the PKEX score- a multimodal assessment tool for patients with shoulder problems Dominic Marley, James Wilson, Amy Barrat, Bibhas Roy O7 Applying multiple imputation to multi-item patient reported outcome measures: advantages and disadvantages of imputing at the item, sub-scale or score level Ines Rombach, Órlaith Burke, Crispin Jenkinson, Alastair Gray, Oliver Rivero-Arias O8 Integrating Patient Reported Outcome Measures (PROMs) into routine primary care for patients with multimorbidity: a feasibility study Ian Porter, Jaheeda Gangannagaripalli, Charlotte Bramwell, Jose M. Valderas O9 eRAPID: electronic self-report and management of adverse-events for pelvic radiotherapy (RT) patients Patricia Holch, Susan Davidson, Jacki Routledge, Ann Henry, Kevin Franks, Alex Gilbert, Kate Absolom & Galina Velikova O10 Patient reported outcomes (PROMs) based recommendation in clinical guidance for the management of chronic conditions in the United Kingdom Ian Porter, Jose M.Valderas O11 Cross-sectional and longitudinal parameter shifts in epidemiological data: measurement invariance and response shifts in cohort and survey data describing the UK’s Quality of Life Jan R. Boehnke O12 Patient-reported outcomes within health technology decision making: current status and implications for future policy Andrew Trigg, Ruth Howells O13 Can social care needs and well-being be explained by the EQ-5D? Analysis of Health Survey for England dataset Jeshika Singh, Subhash Pokhrel, Louise Longworth O14 Where patients and policy meet: exploring individual-level use of the Long-Term Conditions Questionnaire (LTCQ) Caroline Potter, Cheryl Hunter, Laura Kelly, Elizabeth Gibbons, Julian Forder, Angela Coulter, Ray Fitzpatrick, Michele Peter
Author Correction: Discovery of a radiation component from the Vela pulsar reaching 20 teraelectronvolts
No full textIn the version of the article initially published, R. Zanin, M. Kerr, S. Johnston, R. M. Shannon and D. A. Smith mistakenly appeared in the main author list but are now instead listed as members of The H.E.S.S. Collaboration et al. in the HTML and PDF versions of the article
Preliminary evidence on the uptake, use and benefits of the CONSORT-PRO extension.
Get PDFPURPOSE: This study assessed the uptake of the CONsolidated Standards of Reporting Trials (CONSORT)-Patient-Reported Outcomes (PRO) statement; determined if use of CONSORT-PRO was associated with more complete reporting of PRO endpoints in randomised controlled trials (RCTs) and identified the extent to which high-impact journals publishing RCTs with PRO endpoints endorse CONSORT-PRO. METHODS: CONSORT-PRO citations were identified by systematically searching Medline, EMBASE and Google from 2013 (year CONSORT-PRO released) to 17 December 2015. RCTs that cited CONSORT-PRO (cases) were compared to a comparable control sample of RCTs in terms of adherence to CONSORT-PRO using t tests. General linear models assessed the relationship between CONSORT-PRO score and key, pre-specified variables. The 100 highest-impact journals that published RCTs with PRO endpoints (2014-2015) were identified via a systematic Medline search. Instructions for authors were reviewed to determine whether journals endorsed CONSORT-PRO. RESULTS: Total CONSORT-PRO scores ranged from 47 to 100% for cases and 25-96% for controls. Cases had significantly higher total CONSORT-PRO scores compared to controls: t = 2.64, p = 0.01. 'Citing CONSORT-PRO', 'journal endorsing CONSORT-PRO' and 'dedicated PRO paper' were significant predictors of higher CONSORT-PRO adherence score: R (2) = 0.48, p < 0.001. 11/100 top-ranked journals endorsed CONSORT-PRO in their instructions to authors, seven of these journals published RCTs included as cases in this study. CONCLUSION: This study demonstrated improved PRO reporting associated with journal endorsement and author use of the CONSORT-PRO extension. Despite growing awareness, more work is needed to promote appropriate use of CONSORT-PRO to improve completeness of reporting; in particular, stronger journal endorsement of CONSORT-PRO
Broadband multi-wavelength properties of M87 during the 2018 EHT campaign including a very high energy flaring episode
No full textAlgaba, Juan-Carlos et al.-- Full list of authors: Algaba, J. C.; Baloković, M.; Chandra, S.; Cheong, W. -Y.; Cui, Y. -Z.; D'Ammando, F.; Falcone, A. D.; Ford, N. M.; Giroletti, M.; Goddi, C.; Gurwell, M. A.; Hada, K.; Haggard, D.; Jorstad, S.; Kaur, A.; Kawashima, T.; Kerby, S.; Kim, J. -Y.; Kino, M.; Kravchenko, E. V.; Lee, S. -S.; Lu, R. -S.; Markoff, S.; Michail, J.; Neilsen, J.; Nowak, M. A.; Principe, G.; Ramakrishnan, V.; Ripperda, B.; Sasada, M.; Savchenko, S. S.; Sheridan, C.; Akiyama, K.; Alberdi, A.; Alef, W.; Anantua, R.; Asada, K.; Azulay, R.; Bach, U.; Baczko, A. -K.; Ball, D.; Bandyopadhyay, B.; Barrett, J.; Bauböck, M.; Benson, B. A.; Bintley, D.; lackburn, L.; Blundell, R.; Bouman, K. L.; Bower, G. C.; Boyce, H.; Bremer, M.; Brissenden, R.; Britzen, S.; Broderick, A. E.; Broguiere, D.; Bronzwaer, T.; Bustamante, S.; Carlstrom, J. E.; Chael, A.; Chan, C. -k.; Chang, D. O.; Chatterjee, K.; Chatterjee, S.; Chen, M. -T.; Chen, Y.; Cheng, X.; Cho, I.; Christian, P.; Conroy, N. S.; Conway, J. E.; Crawford, T. M.; Crew, G. B.; Cruz-Osorio, A.; Dahale, R.; Davelaar, J.; De Laurentis, M.; Deane, R.; Dempsey, J.; Desvignes, G.; Dexter, J.; Dhruv, V.; Dihingia, I. K.; Doeleman, S. S.; Dzib, S. A.; Eatough, R. P.; Emami, R.; Falcke, H.; Farah, J.; Fish, V. L.; Fomalont, E.; Ford, H. A.; Foschi, M.; Fraga-Encinas, R.; Freeman, W. T.; Friberg, P.; Fromm, C. M.; Fuentes, A.; Galison, P.; Gammie, C. F.; García, R.; Gentaz, O.; Georgiev, B.; Gold, R.; Gómez-Ruiz, A. I.; Gómez, J. L.; Gu, M.; Hesper, R.; Heumann, D.; Ho, L. C.; Ho, P.; Honma, M.; Huang, C. -W. L.; Huang, L.; Hughes, D. H.; Ikeda, S.; Impellizzeri, C. M. V.; Inoue, M.; Issaoun, S.; James, D. J.; Jannuzi, B. T.; Janssen, M.; Jeter, B.; Jiang, W.; Jiménez-Rosales, A.; Johnson, M. D.; Jones, A. C.; Joshi, A. V.; Jung, T.; Karuppusamy, R.; Keating, G. K.; Kettenis, M.; Kim, D. -J.; Kim, J.; Kim, J.; Koay, J. Y.; Kocherlakota, P.; Kofuji, Y.; Koch, P. M.; Koyama, S.; Kramer, C.; Kramer, J. A.; Kramer, M.; Krichbaum, T. P.; Kuo, C. -Y.; La Bella, N.; Levis, A.; Li, Z.; Lico, R.; Lindahl, G.; Lindqvist, M.; Lisakov, M.; Liu, J.; Liu, K.; Liuzzo, E.; Lo, W. -P.; Lobanov, A. P.; Loinard, L.; Lonsdale, C. J.; Lowitz, A. E.; MacDonald, N. R.; Mao, J.; Marchili, N.; Marrone, D. P.; Marscher, A. P.; Martí-Vidal, I.; Matsushita, S.; Matthews, L. D.; Medeiros, L.; Menten, K. M.; Mizuno, I.; Mizuno, Y.; Montgomery, J.; Moran, J. M.; Moriyama, K.; Moscibrodzka, M.; Mulaudzi, W.; Müller, C.; Müller, H.; Mus, A.; Musoke, G.; Myserlis, I.; Nagai, H.; Nagar, N. M.; Nair, D. G.; Nakamura, M.; Narayanan, G.; Natarajan, I.; Nathanail, A.; Navarro Fuentes, S.; Ni, C.; Oh, J.; Okino, H.; Olivares, H.; Oyama, T.; Özel, F.; Palumbo, D. C. M.; Filippos Paraschos, G.; Park, J.; Parsons, H.; Patel, N.; Pen, U. -L.; Pesce, D. W.; Piétu, V.; PopStefanija, A.; Porth, O.; Prather, B.; Psaltis, D.; Pu, H. -Y.; Rao, R.; Rawlings, M. G.; Raymond, A. W.; Rezzolla, L.; Ricarte, A.; Roelofs, F.; Romero-Cañizales, C.; Ros, E.; Roshanineshat, A.; Rottmann, H.; Roy, A. L.; Ruiz, I.; Ruszczyk, C.; Rygl, K. L. J.; Sánchez, S.; Sánchez-Argüelles, D.; Sánchez-Portal, M.; Satapathy, K.; Savolainen, T.; Schloerb, F. P.; Schonfeld, J.; Schuster, K. -F.; Shao, L.; Shen, Z.; Small, D.; Sohn, B. W.; SooHoo, J.; Sosapanta Salas, L. D.; Souccar, K.; Stanway, J. S.; Sun, H.; Tazaki, F.; Tetarenko, A. J.; Tiede, P.; Tilanus, R. P. J.; Titus, M.; Toma, K.; Torne, P.; Toscano, T.; Traianou, E.; Trent, T.; Trippe, S.; Turk, M.; van Bemmel, I.; van Langevelde, H. J.; van Rossum, D. R.; Vos, J.; Wagner, J.; Ward-Thompson, D.; Wardle, J.; Washington, J. E.; Weintroub, J.; Wharton, R.; Wielgus, M.; Wiik, K.; Witzel, G.; Wondrak, M. F.; Wong, G. N.; Wu, Q.; Yadlapalli, N.; Yamaguchi, P.; Yfantis, A.; Yoon, D.; Young, A.; Younsi, Z.; Yu, W.; Yuan, F.; Yuan, Y. -F.; Zensus, J. A.; Zhang, S.; Zhao, G. -Y.; Zhao, S. -S.; Bellazzini, R.; Berenji, B.; Bissaldi, E.; Blandford, R. D.; Bonino, R.; Bruel, P.; Cameron, R. A.; Caraveo, P. A.; Cavazzuti, E.; Cheung, C. C.; Ciprini, S.; Cristarella Orestano, P.; Cutini, S.; Di Lalla, N.; Dinesh, A.; Di Venere, L.; Domínguez, A.; Fegan, S. J.; Franckowiak, A.; Fukazawa, Y.; Fusco, P.; Gargano, F.; Gasbarra, C.; Germani, S.; Giliberti, M.; Grenier, I. A.; Hays, E.; Horan, D.; Kuss, M.; Larsson, S.; Liodakis, I.; Longo, F.; Loparco, F.; Lovellette, M. N.; Maldera, S.; Mazziotta, M. N.; Mereu, I.; Michelson, P. F.; Mirabal, N.; Mizuno, T.; Monzani, M. E.; Morselli, A.; Negro, M.; Omodei, N.; Orlando, E.; Persic, M.; Rainò, S.; Rani, B.; Reimer, A.; Reimer, O.; Sánchez-Conde, M.; Saz Parkinson, P. M.; Sgrò, C.; Siskind, E. J.; Spinelli, P.; Suson, D. J.; Tajima, H.; Torres, D. F.; Zaharijas, G.; Aharonian, F.; Ait Benkhali, F.; Aschersleben, J.; Ashkar, H.; Backes, M.; Barbosa Martins, V.; Batzofin, R.; Becherini, Y.; Berge, D.; Böttcher, M.; Boisson, C.; Bolmont, J.; de Bony de Lavergne, M.; Borowska, J.; Bouyahiaoui, M.; Bradascio, F.; Brose, R.; Brown, A.; Bruno, B.; Bulik, T.; Burger-Scheidlin, C.; Casanova, S.; Cecil, R.; Celic, J.; Cerruti, M.; Chand, T.; Chen, A.; Chibueze, J.; Chibueze, O.; Cotter, G.; Damascene Mbarubucyeye, J.; Devin, J.; Djuvsland, J.; Dmytriiev, A.; Einecke, S.; Ernenwein, J. -P.; Feijen, K.; Fontaine, G.; Funk, S.; Gabici, S.; Glawion, D.; Glicenstein, J. F.; Goswami, P.; Grolleron, G.; Haerer, L.; Heß, B.; Holch, T. L.; Holler, M.; Horns, D.; Huang, Zhiqiu; Jamrozy, M.; Jankowsky, F.; Jung-Richardt, I.; Kasai, E.; Katarzyński, K.; Khatoon, R.; Khélifi, B.; Kluźniak, W.; Komin, Nu.; Kosack, K.; Kundu, A.; Lang, R. G.; Le Stum, S.; Leitl, F.; Lemière, A.; Lemoine-Goumard, M.; Lenain, J. -P.; Leuschner, F.; Luashvili, A.; Mackey, J.; Malyshev, D.; Martí-Devesa, G.; Marx, R.; Meyer, M.; Mitchell, A.; Moderski, R.; Moghadam, M. O.; Mohrmann, L.; Montanari, A.; Moulin, E.; de Naurois, M.; Niemiec, J.; O'Brien, P.; Ohm, S.; de Ona Wilhelmi, E.; Ostrowski, M.; Panny, S.; Panter, M.; Pensec, U.; Pita, S.; Pühlhofer, G.; Quirrenbach, A.; Ravikularaman, S.; Reimer, A.; Reimer, O.; Reville, B.; Reis, I.; Ren, H.; Rieger, F.; Roellinghoff, G.; Rudak, B.; Ruiz-Velasco, E.; Sabri, K.; Sahakian, V.; Salzmann, H.; Santangelo, A.; Sasaki, M.; Schäfer, J.; Schüssler, F.; Schutte, H. M.; Shapopi, J. N. S.; Sharma, A.; Sol, H.; Spencer, S.; Stawarz, Ł.; Steppa, C.; Streil, K.; Suzuki, H.; Takahashi, T.; Tanaka, T.; Taylor, A. M.; Terrier, R.; Tluczykont, M.; Tsirou, M.; van Eldik, C.; Vecchi, M.; Wach, T.; Wagner, S. J.; Wierzcholska, A.; Zacharias, M.; Zdziarski, A. A.; Zech, A.; Żywucka, N.; Abe, S.; Abhir, J.; Abhishek, A.; Acciari, V. A.; Aguasca-Cabot, A.; Agudo, I.; Aniello, T.; Ansoldi, S.; Antonelli, L. A.; Arbet Engels, A.; Arcaro, C.; Artero, M.; Asano, K.; Babić, A.; Barres de Almeida, U.; Barrio, J. A.; Batković, I.; Bautista, A.; Baxter, J.; Becerra González, J.; Bednarek, W.; Bernardini, E.; Bernete, J.; Berti, A.; Besenrieder, J.; Bigongiari, C.; Biland, A.; Blanch, O.; Bonnoli, G.; Bošnjak, Ž.; Bronzini, E.; Burelli, I.; Busetto, G.; Campoy-Ordaz, A.; Carosi, A.; Carosi, R.; Carretero-Castrillo, M.; Castro-Tirado, A. J.; Cerasole, D.; Ceribella, G.; Chai, Y.; Cifuentes, A.; Colombo, E.; Contreras, J. L.; Cortina, J.; Covino, S.; D'Amico, G.; D'Elia, V.; Da Vela, P.; Dazzi, F.; De Angelis, A.; De Lotto, B.; de Menezes, R.; Delfino, M.; Delgado, J.; Delgado Mendez, C.; Di Pierro, F.; Di Tria, R.; Di Venere, L.; Dominis Prester, D.; Donini, A.; Dorner, D.; Doro, M.; Elsaesser, D.; Escudero, J.; Fariña, L.; Fattorini, A.; Foffano, L.; Font, L.; Fröse, S.; Fukami, S.; Fukazawa, Y.; García López, R. J.; Garczarczyk, M.; Gasparyan, S.; Gaug, M.; Giesbrecht Paiva, J. G.; Giglietto, N.; Giordano, F.; Gliwny, P.; Godinović, N.; Gradetzke, T.; Grau, R.; Green, D.; Green, J. G.; Günther, P.; Hadasch, D.; Hahn, A.; Hassan, T.; Heckmann, L.; Herrera Llorente, J.; Hrupec, D.; Imazawa, R.; Ishio, K.; Jiménez Martínez, I.; Jormanainen, J.; Kayanoki, T.; Kerszberg, D.; Kluge, G. W.; Kobayashi, Y.; Kouch, P. M.; Kubo, H.; Kushida, J.; Láinez, M.; Lamastra, A.; Leone, F.; Lindfors, E.; Lombardi, S.; López-Coto, R.; López-Moya, M.; López-Oramas, A.; Loporchio, S.; Lorini, A.; Lyard, E.; Machado de Oliveira Fraga, B.; Majumdar, P.; Makariev, M.; Maneva, G.; Manganaro, M.; Mangano, S.; Mannheim, K.; Mariotti, M.; Martínez, M.; Martínez-Chicharro, M.; Mas-Aguilar, A.; Mazin, D.; Menchiari, S.; Mender, S.; Miceli, D.; Miener, T.; Miranda, J. M.; Mirzoyan, R.; Molero González, M.; Molina, E.; Mondal, H. A.; Moralejo, A.; Morcuende, D.; Nakamori, T.; Nanci, C.; Neustroev, V.; Nickel, L.; Nievas Rosillo, M.; Nigro, C.; Nikolić, L.; Nilsson, K.; Nishijima, K.; Njoh Ekoume, T.; Noda, K.; Nozaki, S.; Ohtani, Y.; Okumura, A.; Otero-Santos, J.; Paiano, S.; Paneque, D.; Paoletti, R.; Paredes, J. M.; Peresano, M.; Persic, M.; Pihet, M.; Pirola, G.; Podobnik, F.; Prada Moroni, P. G.; Prandini, E.; Priyadarshi, C.; Ribó, M.; Rico, J.; Righi, C.; Sahakyan, N.; Saito, T.; Saturni, F. G.; Schmidt, K.; Schmuckermaier, F.; Schubert, J. L.; Schweizer, T.; Sciaccaluga, A.; Silvestri, G.; Sitarek, J.; Sliusar, V.; Sobczynska, D.; Spolon, A.; Stamerra, A.; Strišković, J.; Strom, D.; Strzys, M.; Suda, Y.; Suutarinen, S.; Tajima, H.; Takahashi, M.; Takeishi, R.; Tavecchio, F.; Temnikov, P.; Terauchi, K.; Terzić, T.; Teshima, M.; Truzzi, S.; Tutone, A.; Ubach, S.; van Scherpenberg, J.; Vazquez Acosta, M.; Ventura, S.; Verna, G.; Viale, I.; Vigorito, C. F.; Vitale, V.; Vovk, I.; Walter, R.; Will, M.; Wunderlich, C.; Yamamoto, T.; Acharyya, A.; Adams, C. B.; Bangale, P.; Bartkoske, J. T.; Benbow, W.; Christiansen, J. L.; Duerr, A.; Errando, M.; Feng, Q.; Foote, J.; Fortson, L.; Furniss, A.; Hanlon, W.; Hervet, O.; Hinrichs, C. E.; Holder, J.; Humensky, T. B.; Jin, W.; Johnson, M. N.; Kaaret, P.; Kertzman, M.; Kieda, D.; Kleiner, T. K.; Korzoun, N.; Krennrich, F.; Kumar, S.; Lang, M. J.; Lundy, M.; Maier, G.; McGrath, C. E.; Millard, M. J.; Mooney, C. L.; Moriarty, P.; Mukherjee, R.; Ning, W.; O'Brien, S.; Ong, R. A.; Pohl, M.; Pueschel, E.; Quinn, J.; Ragan, K.; Reynolds, P. T.; Ribeiro, D.; Roache, E.; Ryan, J. L.; Sadeh, I.; Saha, L.; Santander, M.; Sembroski, G. H.; Shang, R.; Splettstoesser, M.; Talluri, A. K.; Tucci, J. V.; Valverde, J.; Vassiliev, V. V.; Williams, D. A.; Wong, S. L.; Chen, Z.; Cui, L.; Hirota, T.; Li, B.; Li, G.; Liu, Q.; Liu, X.; Liu, Z.; Ma, J.; Niinuma, K.; Ro, H.; Sakai, N.; Sawada-Satoh, S.; Wajima, K.; Wang, J.; Wang, N.; Xia, B.; Yan, H.; Yonekura, Y.; Zhang, H.; Zhao, R.; Zhong, W.Context. The nearby elliptical galaxy M87 contains one of only two supermassive black holes whose emission surrounding the event horizon has been imaged by the Event Horizon Telescope (EHT). In 2018, more than two dozen multi-wavelength (MWL) facilities (from radio to γ-ray energies) took part in the second M87 EHT campaign.Aims. The goal of this extensive MWL campaign was to better understand the physics of the accreting black hole M87*, the relationship between the inflow and inner jets, and the high-energy particle acceleration. Understanding the complex astrophysics is also a necessary first step towards performing further tests of general relativity.Methods. The MWL campaign took place in April 2018, overlapping with the EHT M87* observations. We present a new, contemporaneous spectral energy distribution (SED) ranging from radio to very high-energy (VHE) γ-rays as well as details of the individual observations and light curves. We also conducted phenomenological modelling to investigate the basic source properties.Results. We present the first VHE γ-ray flare from M87 detected since 2010. The flux above 350 GeV more than doubled within a period of ≈36 hours. We find that the X-ray flux is enhanced by about a factor of two compared to 2017, while the radio and millimetre core fluxes are consistent between 2017 and 2018. We detect evidence for a monotonically increasing jet position angle that corresponds to variations in the bright spot of the EHT image.Conclusions. Our results show the value of continued MWL monitoring together with precision imaging for addressing the origins of high-energy particle acceleration. While we cannot currently pinpoint the precise location where such acceleration takes place, the new VHE γ-ray flare already presents a challenge to simple one-zone leptonic emission model approaches, and it emphasises the need for combined image and spectral modelling. © The Authors 2024The Event Horizon Telescope Collaboration thanks the following organisations and programs: the Academia Sinica;
the Academy of Finland (projects 274477, 284495, 312496,
315721); the Agencia Nacional de Investigación y Desarrollo
(ANID), Chile via NCN19_058 (TITANs), Fondecyt 1221421
and BASAL FB210003; the Alexander von Humboldt Stiftung;
an Alfred P. Sloan Research Fellowship; Allegro, the European
ALMA Regional Centre node in the Netherlands, the NL astronomy research network NOVA and the astronomy institutes of
the University of Amsterdam, Leiden University, and Radboud
University; the ALMA North America Development Fund; the
Astrophysics and High Energy Physics programme by MCIN
(with funding from European Union NextGenerationEU, PRTRC17I1); the Black Hole Initiative, that is funded by grants from
the John Templeton Foundation (60477, 61497, 62286) and the
Gordon and Betty Moore Foundation (Grant GBMF-8273) -
although the opinions expressed in this work are those of the
author and do not necessarily reflect the views of these Foundations; the Brinson Foundation; “la Caixa” Foundation (ID
100010434) through fellowship codes LCF/BQ/DI22/11940027
and LCF/BQ/DI22/11940030; Chandra DD7-18089X and
TM6-17006X; the China Scholarship Council; the China
Postdoctoral Science Foundation fellowships (2020M671266,
2022M712084); Consejo Nacional de Humanidades, Ciencia
y Tecnología (CONAHCYT, Mexico, projects U0004-246083,
U0004-259839, F0003-272050, M0037-279006, F0003-
281692, 104497, 275201, 263356); the Colfuturo Scholarship;
the Consejería de Economía, Conocimiento, Empresas y
Universidad of the Junta de Andalucía (grant P18-FR-1769),
the Consejo Superior de Investigaciones Científicas (grant
2019AEP112); the Delaney Family via the Delaney Family
John A. Wheeler Chair at Perimeter Institute; Dirección General
de Asuntos del Personal Académico-Universidad Nacional
Autónoma de México (DGAPA-UNAM, projects IN112820
and IN108324); the Dutch Organization for Scientific Research
(NWO) for the VICI award (grant 639.043.513), the grant
OCENW.KLEIN.113, and the Dutch Black Hole Consortium
(with project No. NWA 1292.19.202) of the research programme
the National Science Agenda; the Dutch National Supercomputers, Cartesius and Snellius (NWO grant 2021.013); the EACOA
Fellowship awarded by the East Asia Core Observatories
Association, which consists of the Academia Sinica Institute
of Astronomy and Astrophysics, the National Astronomical
Observatory of Japan, Center for Astronomical Mega-Science,
Chinese Academy of Sciences, and the Korea Astronomy and
Space Science Institute; the European Research Council (ERC)
Synergy Grant “BlackHoleCam: Imaging the Event Horizon of
Black Holes" (grant 610058); the European Union Horizon 2020
research and innovation programme under grant agreements
RadioNet (No. 730562) and M2FINDERS (No. 101018682);
the European Research Council for advanced grant ‘JETSET:
Launching, propagation and emission of relativistic jets from
binary mergers and across mass scales’ (grant No. 884631); the
Horizon ERC Grants 2021 programme under grant agreement
No. 101040021; the FAPESP (Fundação de Amparo á Pesquisa
do Estado de São Paulo) under grant 2021/01183-8; the Fondo
CAS-ANID folio CAS220010; the Generalitat Valenciana
(grants APOSTD/2018/177 and ASFAE/2022/018) and GenT
Program (project CIDEGENT/2018/021); the Gordon and Betty
Moore Foundation (GBMF-3561, GBMF-5278, GBMF-10423);
the Institute for Advanced Study; the Istituto Nazionale di
Fisica Nucleare (INFN) sezione di Napoli, iniziative specifiche
TEONGRAV; the International Max Planck Research School
for Astronomy and Astrophysics at the Universities of Bonn
and Cologne; DFG research grant “Jet physics on horizon scales
and beyond” (grant No. 443220636); Joint Columbia/Flatiron
Postdoctoral Fellowship (research at the Flatiron Institute is
supported by the Simons Foundation); the Japan Ministry of
Education, Culture, Sports, Science and Technology (MEXT;
grant JPMXP1020200109); the Japan Society for the Promotion
of Science (JSPS) Grant-in-Aid for JSPS Research Fellowship
(JP17J08829); the Joint Institute for Computational Fundamental Science, Japan; the Key Research Program of Frontier
Sciences, Chinese Academy of Sciences (CAS, grants QYZDJSSW-SLH057, QYZDJSSW-SYS008, ZDBS-LY-SLH011);
the Leverhulme Trust Early Career Research Fellowship; the
Max-Planck-Gesellschaft (MPG); the Max Planck Partner
Group of the MPG and the CAS; the MEXT/JSPS KAKENHI
(grants 18KK0090, JP21H01137, JP18H03721, JP18K13594,
18K03709, JP19K14761, 18H01245, 25120007, 19H01943,
21H01137, 21H04488, 22H00157, 23K03453); the MICINN
Research Project PID2019-108995GB-C22; the MIT International Science and Technology Initiatives (MISTI) Funds;
the Ministry of Science and Technology (MOST) of Taiwan
(103-2119-M-001-010-MY2, 105-2112-M-001-025-MY3, 105-
2119-M-001-042, 106-2112-M-001-011, 106-2119-M-001-013,
106-2119-M-001-027, 106-2923-M-001-005, 107-2119-
M-001-017, 107-2119-M-001-020, 107-2119-M-001-041,
107-2119-M-110-005, 107-2923-M-001-009, 108-2112-M001-048, 108-2112-M-001-051, 108-2923-M-001-002, 109-
2112-M-001-025, 109-2124-M-001-005, 109-2923-M-001-001,
110-2112-M-001-033, 110-2124-M-001-007, 110-2923-M-001-
001, and 112-2112-M-003-010-MY3); the National Science and
Technology Council (NSTC) of Taiwan (111-2124-M-001-005,
112-2124-M-001-014); the Ministry of Education (MoE) of
Taiwan Yushan Young Scholar Program; the Physics Division, National Center for Theoretical Sciences of Taiwan; the
National Aeronautics and Space Administration (NASA, Fermi
Guest Investigator grant 80NSSC23K1508, NASA Astrophysics
Theory Program grant 80NSSC20K0527, NASA NuSTAR
award 80NSSC20K0645); NASA Hubble Fellowship grants
HST-HF2-51431.001-A, HST-HF2-51482.001-A awarded by
the Space Telescope Science Institute, which is operated by
the Association of Universities for Research in Astronomy,
Inc., for NASA, under contract NAS5-26555; the National
Institute of Natural Sciences (NINS) of Japan; the National
Key Research and Development Program of China (grant
2016YFA0400704, 2017YFA0402703, 2016YFA0400702); the
National Science and Technology Council (NSTC, grants NSTC
111-2112-M-001 -041, NSTC 111-2124-M-001-005, NSTC
112-2124-M-001-014); the US National Science Foundation
(NSF, grants AST-0096454, AST-0352953, AST-0521233,
AST-0705062, AST-0905844, AST-0922984, AST-1126433,
OIA-1126433, AST-1140030, DGE-1144085, AST-1207704,
AST-1207730, AST-1207752, MRI-1228509, OPP-1248097,
AST-1310896, AST-1440254, AST-1555365, AST-1614868,
AST-1615796, AST-1715061, AST-1716327, AST-1726637,
OISE-1743747, AST-1743747, AST-1816420, AST-1935980,
AST-1952099, AST-2034306, AST-2205908, AST-2307887);
NSF Astronomy and Astrophysics Postdoctoral Fellowship
(AST-1903847); the Natural Science Foundation of China
(grants 11650110427, 10625314, 11721303, 11725312,
11873028, 11933007, 11991052, 11991053, 12192220,
12192223, 12273022, 12325302); the Natural Sciences and
Engineering Research Council of Canada (NSERC, including
a Discovery Grant and the NSERC Alexander Graham Bell
Canada Graduate Scholarships-Doctoral Program); the National
Research Foundation of Korea (the Global PhD Fellowship
Grant: grants NRF-2015H1A2A1033752, the Korea Research
Fellowship Program: NRF-2015H1D3A1066561, Brain Pool
Program: 2019H1D3A1A01102564, Basic Research Support Grant 2019R1F1A1059721, 2021R1A6A3A01086420,
2022R1C1C1005255, 2022R1F1A1075115); Netherlands
Research School for Astronomy (NOVA) Virtual Institute of
Accretion (VIA) postdoctoral fellowships; NOIRLab, which
is managed by the Association of Universities for Research
in Astronomy (AURA) under a cooperative agreement with
the National Science Foundation; Onsala Space Observatory
(OSO) national infrastructure, for the provisioning of its
facilities/observational support (OSO receives funding through
the Swedish Research Council under grant 2017-00648);
the Perimeter Institute for Theoretical Physics (research at
Perimeter Institute is supported by the Government of Canada
through the Department of Innovation, Science and Economic
Development and by the Province of Ontario through the
Ministry of Research, Innovation and Science); the Princeton
Gravity Initiative; the Spanish Ministerio de Ciencia e Innovación (grants PGC2018-098915-B-C21, AYA2016-80889-P,
PID2019-108995GB-C21, PID2020-117404GB-C21); the
University of Pretoria for financial aid in the provision of
the new Cluster Server nodes and SuperMicro (USA) for a
SEEDING GRANT approved toward these nodes in 2020; the
Shanghai Municipality orientation program of basic research for
international scientists (grant no. 22JC1410600); the Shanghai
Pilot Program for Basic Research, Chinese Academy of Science,
Shanghai Branch (JCYJ-SHFY-2021-013); the State Agency
for Research of the Spanish MCIU through the “Center of
Excellence Severo Ochoa” award for the Instituto de Astrofísica
de Andalucía (SEV-2017- 0709); the Spanish Ministry for
Science and Innovation grant CEX2021-001131-S funded by
MCIN/AEI/10.13039/501100011033; the Spinoza Prize SPI
78-409; the South African Research Chairs Initiative, through
the South African Radio Astronomy Observatory (SARAO,
grant ID 77948), which
Broadband Multi-wavelength Properties of M87 during the 2017 Event Horizon Telescope Campaign
No full textIn 2017, the Event Horizon Telescope (EHT) Collaboration succeeded in capturing the first direct image of the center of the M87 galaxy. The asymmetric ring morphology and size are consistent with theoretical expectations for a weakly accreting supermassive black hole of mass ∼6.5 × 109 M o˙. The EHTC also partnered with several international facilities in space and on the ground, to arrange an extensive, quasi-simultaneous multi-wavelength campaign. This Letter presents the results and analysis of this campaign, as well as the multi-wavelength data as a legacy data repository. We captured M87 in a historically low state, and the core flux dominates over HST-1 at high energies, making it possible to combine core flux constraints with the more spatially precise very long baseline interferometry data. We present the most complete simultaneous multi-wavelength spectrum of the active nucleus to date, and discuss the complexity and caveats of combining data from different spatial scales into one broadband spectrum. We apply two heuristic, isotropic leptonic single-zone models to provide insight into the basic source properties, but conclude that a structured jet is necessary to explain M87's spectrum. We can exclude that the simultaneous γ-ray emission is produced via inverse Compton emission in the same region producing the EHT mm-band emission, and further conclude that the γ-rays can only be produced in the inner jets (inward of HST-1) if there are strongly particle-dominated regions. Direct synchrotron emission from accelerated protons and secondaries cannot yet be excluded. © 2021. The Author(s). Published by the American Astronomical Society.
The -ray spectrum of the core of Centaurus A as observed with H.E.S.S. and Fermi-LAT
Get PDFInternational audienceCentaurus A (Cen A) is the nearest radio galaxy discovered as a very-high-energy (VHE; 100 GeV–100 TeV) γ-ray source by the High Energy Stereoscopic System (H.E.S.S.). It is a faint VHE γ-ray emitter, though its VHE flux exceeds both the extrapolation from early Fermi-LAT observations as well as expectations from a (misaligned) single-zone synchrotron-self Compton (SSC) description. The latter satisfactorily reproduces the emission from Cen A at lower energies up to a few GeV. New observations with H.E.S.S., comparable in exposure time to those previously reported, were performed and eight years of Fermi-LAT data were accumulated to clarify the spectral characteristics of the γ-ray emission from the core of Cen A. The results allow us for the first time to achieve the goal of constructing a representative, contemporaneous γ-ray core spectrum of Cen A over almost five orders of magnitude in energy. Advanced analysis methods, including the template fitting method, allow detection in the VHE range of the core with a statistical significance of 12σ on the basis of 213 hours of total exposure time. The spectrum in the energy range of 250 GeV–6 TeV is compatible with a power-law function with a photon index Γ = 2.52 ± 0.13stat ± 0.20sys. An updated Fermi-LAT analysis provides evidence for spectral hardening by ΔΓ ≃ 0.4 ± 0.1 at γ-ray energies above 2.8+1.0−0.6 GeV at a level of 4.0σ. The fact that the spectrum hardens at GeV energies and extends into the VHE regime disfavour a single-zone SSC interpretation for the overall spectral energy distribution (SED) of the core and is suggestive of a new γ-ray emitting component connecting the high-energy emission above the break energy to the one observed at VHE energies. The absence of significant variability at both GeV and TeV energies does not yet allow disentanglement of the physical nature of this component, though a jet-related origin is possible and a simple two-zone SED model fit is provided to this end.Key words: gamma rays: galaxies / radiation mechanisms: non-thermal⋆ Corresponding author: H.E.S.S. and LAT Collaborations, e-mail: [email protected]; [email protected].† Funded by EU FP7 Marie Curie, grant agreement No. PIEF-GA-2012-332350
Revealing x-ray and gamma ray temporal and spectral similarities in the GRB 190829A afterglow
Get PDFInternational audienceGamma-ray bursts (GRBs), which are bright flashes of gamma rays from extragalactic sources followed by fading afterglow emission, are associated with stellar core collapse events. We report the detection of very-high-energy (VHE) gamma rays from the afterglow of GRB 190829A, between 4 and 56 hours after the trigger, using the High Energy Stereoscopic System (H.E.S.S.). The low luminosity and redshift of GRB 190829A reduce both internal and external absorption, allowing determination of its intrinsic energy spectrum. Between energies of 0.18 and 3.3 tera–electron volts, this spectrum is described by a power law with photon index of 2.07 ± 0.09, similar to the x-ray spectrum. The x-ray and VHE gamma-ray light curves also show similar decay profiles. These similar characteristics in the x-ray and gamma-ray bands challenge GRB afterglow emission scenarios.</p
Searches for gamma-ray lines and 'pure WIMP' spectra from Dark Matter annihilations in dwarf galaxies with H.E.S.S
Get PDFInternational audienceDwarf spheroidal galaxies are among the most promising targets for detecting signals of Dark Matter (DM) annihilations. The H.E.S.S. experiment has observed five of these systems for a total of about 130 hours. The data are re-analyzed here, and, in the absence of any detected signals, are interpreted in terms of limits on the DM annihilation cross section. Two scenarios are considered: i) DM annihilation into mono-energetic gamma-rays and ii) DM in the form of pure WIMP multiplets that, annihilating into all electroweak bosons, produce a distinctive gamma-ray spectral shape with a high-energy peak at the DM mass and a lower-energy continuum. For case i), upper limits at 95% confidence level of about σ v 3 × 10−25 cm3 s−1 are obtained in the mass range of 400 GeV to 1 TeV. For case ii), the full spectral shape of the models is used and several excluded regions are identified, but the thermal masses of the candidates are not robustly ruled out
H.E.S.S. follow-up observations of binary black hole coalescence events during the second and third gravitational-wave observing runs of advanced LIGO and advanced Virgo
Get PDFInternational audienceWe report on the observations of four well-localized binary black hole (BBH) mergers by the High Energy Stereoscopic System (H.E.S.S.) during the second and third observing runs of Advanced LIGO and Advanced Virgo, O2 and O3. H.E.S.S. can observe 20 deg of the sky at a time and follows up gravitational-wave (GW) events by “tiling” localization regions to maximize the covered localization probability. During O2 and O3, H.E.S.S. observed large portions of the localization regions, between 35% and 75%, for four BBH mergers (GW170814, GW190512_180714, GW190728_064510, and S200224ca). For these four GW events, we find no significant signal from a pointlike source in any of the observations, and we set upper limits on the very high energy (>100 GeV) γ-ray emission. The 1–10 TeV isotropic luminosity of these GW events is below 10 erg s at the times of the H.E.S.S. observations, around the level of the low-luminosity GRB 190829A. Assuming no changes are made to how follow-up observations are conducted, H.E.S.S. can expect to observe over 60 GW events per year in the fourth GW observing run, O4, of which eight would be observable with minimal latency
