85 results on '"Bernardini, M."'
Search Results
2. Strategic Debriefing for Advanced Simulation
- Author
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Capogna, G., Ingrassia, P. L., Capogna, E., Bernardini, M., Pietrabissa, Giada, Valteroni, E., and Nardone, G.
- Subjects
Debriefing ,Strategic Dialog ,Settore M-PSI/08 - PSICOLOGIA CLINICA - Published
- 2022
3. Turbulent Drag Reduction Using Spanwise Forcing in Compressible Regime
- Author
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Gattere, F., Chiarini, A., Zanolini, M., Gatti, D., Bernardini, M., and Quadrio, M.
- Published
- 2022
4. Swift/Uvot Follow-Up Of Gravitational Wave Alerts In The O3 Era
- Author
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Oates, S. R., Marshall, F. E., Breeveld, A. A., Kuin, N. P. M., Brown, P. J., De Pasquale, M., Evans, P. A., Fenney, A. J., Gronwall, C., Kennea, J. A., Klingler, N. J., Page, M. J., Siegel, M. H., Tohuvavohu, A., Ambrosi, E., Barthelmy, S. D., Beardmore, A. P., Bernardini, M. G., Campana, S., and Caputo, R.
- Abstract
In this paper, we report on the observational performance of the Swift Ultra-violet/Optical Telescope (UVOT) in response to the gravitational wave (GW) 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 GW 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 (AGNs)/quasars, three cataclysmic variables (CVs), nine supernovae, 11 unidentified sources that had archival photometry, and six 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.
- Published
- 2021
5. Swift Multiwavelength Follow-Up Of Lvc S200224Ca And The Implications For Binary Black Hole Mergers
- Author
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Klingler, N. J., Lien, A., Oates, S. R., Kennea, J. A., Evans, P. A., Tohuvavohu, A., Zhang, B., Page, K. L., Cenko, S. B., Barthelmy, S. D., Beardmore, A. P., Bernardini, M. G., Breeveld, A. A., Brown, P. J., Burrows, D. N., Campana, S., Cusumano, G., D'Ai, A., D'Avanzo, P., and D'Elia, V.
- Abstract
On 2020 February 24, during their third observing run ("O3"), the Laser Interferometer Gravitational-wave Observatory and Virgo Collaboration detected S200224ca: a candidate gravitational wave (GW) event produced by a binary black hole (BBH) merger. This event was one of the best-localized compact binary coalescences detected in O3 (with 50%/ 90% error regions of 13/72 deg(2)), and so the Neil Gehrels Swift Observatory performed rapid near-UV/X-ray followup observations. Swift-XRT and UVOT covered approximately 79.2% and 62.4% (respectively) of the GWerror region, making S200224ca the BBH event most thoroughly followed-up in near-UV (u-band) and X-ray to date. No likely EM counterparts to the GW event were found by the Swift BAT, XRT, or UVOT, nor by other observatories. Here, we report on the results of our searches for an EM counterpart, both in the BAT data near the time of the merger, and in follow-up UVOT/XRT observations. We also discuss the upper limits we can place on EM radiation from S200224ca, as well as the implications these limits have on the physics of BBH mergers. Namely, we place a shallow upper limit on the dimensionless BH charge, (q) over cap < 1.4 x 10(-4), and an upper limit on the isotropic-equivalent energy of a blast wave E< 4.1x10(51) erg (assuming typical GRB parameters).
- Published
- 2021
6. Observation of inverse Compton emission from a long $��$-ray burst
- Author
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Acciari, V. A., Ansoldi, S., Antonelli, L. A., Engels, A. Arbet, Baack, D., Babi��, A., Banerjee, B., de Almeida, U. Barres, Barrio, J. A., Gonz��lez, J. Becerra, Bednarek, W., Bellizzi, L., Bernardini, E., Berti, A., Besenrieder, J., Bhattacharyya, W., Bigongiari, C., Biland, A., Blanch, O., Bonnoli, G., Bo��njak, ��., Busetto, G., Carosi, R., Ceribella, G., Chai, Y., Chilingaryan, A., Cikota, S., Colak, S. M., Colin, U., Colombo, E., Contreras, J. L., Cortina, J., Covino, S., D'Elia, V., Da Vela, P., Dazzi, F., De Angelis, A., De Lotto, B., Delfino, M., Delgado, J., Depaoli, D., Di Pierro, F., Di Venere, L., Espi��eira, E. Do Souto, Prester, D. Dominis, Donini, A., Dorner, D., Doro, M., Elsaesser, D., Ramazani, V. Fallah, Fattorini, A., Ferrara, G., Fidalgo, D., Foffano, L., Fonseca, M. V., Font, L., Fruck, C., Fukami, S., L��pez, R. J. Garc��a, Garczarczyk, M., Gasparyan, S., Gaug, M., Giglietto, N., Giordano, F., Godinovi��, N., Green, D., Guberman, D., Hadasch, D., Hahn, A., Herrera, J., Hoang, J., Hrupec, D., H��tten, M., Inada, T., Inoue, S., Ishio, K., Iwamura, Y., Jouvin, L., Kerszberg, D., Kubo, H., Kushida, J., Lamastra, A., Lelas, D., Leone, F., Lindfors, E., Lombardi, S., Longo, F., L��pez, M., L��pez-Coto, R., L��pez-Oramas, A., Loporchio, S., Fraga, B. Machado de Oliveira, Maggio, C., Majumdar, P., Makariev, M., Mallamaci, M., Maneva, G., Manganaro, M., Mannheim, K., Maraschi, L., Mariotti, M., Mart��nez, M., Mazin, D., Mi��anovi��, S., Miceli, D., Minev, M., Miranda, J. M., Mirzoyan, R., Molina, E., Moralejo, A., Morcuende, D., Moreno, V., Moretti, E., Munar-Adrover, P., Neustroev, V., Nigro, C., Nilsson, K., Ninci, D., Nishijima, K., Noda, K., Nogu��s, L., Nozaki, S., Paiano, S., Palatiello, M., Paneque, D., Paoletti, R., Paredes, J. M., Pe��il, P., Peresano, M., Persic, M., Moroni, P. G. Prada, Prandini, E., Puljak, I., Rhode, W., Rib��, M., Rico, J., Righi, C., Rugliancich, A., Saha, L., Sahakyan, N., Saito, T., Sakurai, S., Satalecka, K., Schmidt, K., Schweizer, T., Sitarek, J., ��nidari��, I., Sobczynska, D., Somero, A., Stamerra, A., Strom, D., Strzys, M., Suda, Y., Suri��, T., Takahashi, M., Tavecchio, F., Temnikov, P., Terzi��, T., Teshima, M., Torres-Alb��, N., Tosti, L., Vagelli, V., van Scherpenberg, J., Vanzo, G., Acosta, M. Vazquez, Vigorito, C. F., Vitale, V., Vovk, I., Will, M., Zari��, D., Nava, L., Veres, P., Bhat, P. N., Briggs, M. S., Cleveland, W. H., Hamburg, R., Hui, C. M., Mailyan, B., Preece, R. D., Roberts, O., von Kienlin, A., Wilson-Hodge, C. A., Kocevski, D., Arimoto, M., Tak, D., Asano, K., Axelsson, M., Barbiellini, G., Bissaldi, E., Dirirsa, F. Fana, Gill, R., Granot, J., McEnery, J., Razzaque, S., Piron, F., Racusin, J. L., Thompson, D. J., Campana, S., Bernardini, M. G., Kuin, N. P. M., Siegel, M. H., Cenko, S. Bradley, O'Brien, P., Capalbi, M., D'A��, A., De Pasquale, M., Gropp, J., Klingler, N., Osborne, J. P., Perri, M., Starling, R., Tagliaferri, G., Tohuvavohu, A., Ursi, A., Tavani, M., Cardillo, M., Casentini, C., Piano, G., Evangelista, Y., Verrecchia, F., Pittori, C., Lucarelli, F., Bulgarelli, A., Parmiggiani, N., Anderson, G. E., Anderson, J. P., Bernardi, G., Bolmer, J., Caballero-Garc��a, M. D., Carrasco, I. M., Castell��n, A., Segura, N. Castro, Castro-Tirado, A. J., Cherukuri, S. V., Cockeram, A. M., D'Avanzo, P., Di Dato, A., Diretse, R., Fender, R. P., Fern��ndez-Garc��a, E., Fynbo, J. P. U., Fruchter, A. S., Greiner, J., Gromadzki, M., Heintz, K. E., Heywood, I., van der Horst, A. J., Hu, Y. -D., Inserra, C., Izzo, L., Jaiswal, V., Jakobsson, P., Japelj, J., Kankare, E., Kann, D. A., Kouveliotou, C., Klose, S., Levan, A. J., Li, X. Y., Lotti, S., Maguire, K., Malesani, D. B., Manulis, I., Marongiu, M., Martin, S., Melandri, A., Micha��owski, M., Miller-Jones, J. C. A., Misra, K., Moin, A., Mooley, K. P., Nasri, S., Nicholl, M., Noschese, A., Novara, G., Pandey, S. B., Peretti, E., del Pulgar, C. J. P��rez, P��rez-Torres, M. A., Perley, D. A., Piro, L., Ragosta, F., Resmi, L., Ricci, R., Rossi, A., S��nchez-Ram��rez, R., Selsing, J., Schulze, S., Smartt, S. J., Smith, I. A., Sokolov, V. V., Stevens, J., Tanvir, N. R., Th��ne, C. C., Tiengo, A., Tremou, E., Troja, E., Postigo, A. de Ugarte, Vergani, S. D., Wieringa, M., Woudt, P. A., Xu, D., Yaron, O., and Young, D. R.
- Subjects
High Energy Astrophysical Phenomena (astro-ph.HE) ,Astrophysics::High Energy Astrophysical Phenomena ,FOS: Physical sciences ,Astrophysics::Cosmology and Extragalactic Astrophysics ,Astrophysics::Galaxy Astrophysics - Abstract
Long-duration gamma-ray bursts (GRBs) originate from ultra-relativistic jets launched from the collapsing cores of dying massive stars. They are characterised by an initial phase of bright and highly variable radiation in the keV-MeV band that is likely produced within the jet and lasts from milliseconds to minutes, known as the prompt emission. Subsequently, the interaction of the jet with the external medium generates external shock waves, responsible for the afterglow emission, which lasts from days to months, and occurs over a broad energy range, from the radio to the GeV bands. The afterglow emission is generally well explained as synchrotron radiation by electrons accelerated at the external shock. Recently, an intense, long-lasting emission between 0.2 and 1 TeV was observed from the GRB 190114C. Here we present the results of our multi-frequency observational campaign of GRB~190114C, and study the evolution in time of the GRB emission across 17 orders of magnitude in energy, from $5\times10^{-6}$ up to $10^{12}$\,eV. We find that the broadband spectral energy distribution is double-peaked, with the TeV emission constituting a distinct spectral component that has power comparable to the synchrotron component. This component is associated with the afterglow, and is satisfactorily explained by inverse Compton upscattering of synchrotron photons by high-energy electrons. We find that the conditions required to account for the observed TeV component are not atypical, supporting the possibility that inverse Compton emission is commonly produced in GRBs.
- Published
- 2020
- Full Text
- View/download PDF
7. Experimental Observation of Proton Bunch Modulation in a Plasma at Varying Plasma Densities
- Author
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Adli, E, Ahuja, A, Apsimon, O, Apsimon, R, Bachmann, A-M, Barrientos, D, Barros, MM, Batkiewicz, J, Batsch, F, Bauche, J, Olsen, VK Berglyd, Bernardini, M, Biskup, B, Boccardi, A, Bogey, T, Bohl, T, Bracco, C, Braunmueller, F, Burger, S, Burt, G, Bustamante, S, Buttenschoen, B, Caldwell, A, Cascella, M, Chappell, J, Chevallay, E, Chung, M, Cooke, D, Damerau, H, Deacon, L, Deubner, LH, Dexter, A, Doebert, S, Farmer, J, Fedosseev, VN, Fior, G, Fiorito, R, Fonseca, RA, Friebel, F, Garolfi, L, Gessner, S, Gorgisyan, I, Gorn, AA, Granados, E, Grulke, O, Gschwendtner, E, Guerrero, A, Hansen, J, Helm, A, Henderson, JR, Hessler, C, Hofle, W, Huether, M, Ibison, M, Jensen, L, Jolly, S, Keeble, F, Kim, S-Y, Kraus, F, Lefevre, T, LeGodec, G, Li, Y, Liu, S, Lopes, N, Lotov, KV, Brun, L Maricalva, Martyanov, M, Mazzoni, S, Godoy, D Medina, Minakov, VA, Mitchell, J, Molendijk, JC, Mompo, R, Moody, JT, Moreira, M, Muggli, P, Mutin, C, Oez, E, Ozturk, E, Pasquino, C, Pardons, A, Asmus, F Pena, Pepitone, K, Perera, A, Petrenko, A, Pitman, S, Plyushchev, G, Pukhov, A, Rey, S, Rieger, K, Ruhl, H, Schmidt, JS, Shalimova, IA, Shaposhnikova, E, Sherwood, P, Silva, LO, Soby, L, Sosedkin, AP, Speroni, R, Spitsyn, RI, Tuev, PV, Turner, M, Velotti, F, Verra, L, Verzilov, VA, Vieira, J, Vincke, H, Welsch, CP, Williamson, B, Wing, M, Woolley, B, Xia, G, and Collaboration, AWAKE
- Subjects
Accelerator Physics (physics.acc-ph) ,Proton ,Other Fields of Physics ,General Physics and Astronomy ,FOS: Physical sciences ,Plasma oscillation ,Ciências Naturais::Ciências Físicas [Domínio/Área Científica] ,01 natural sciences ,law.invention ,law ,Physics::Plasma Physics ,Ionization ,physics.plasm-ph ,0103 physical sciences ,010306 general physics ,physics.acc-ph ,Physics ,Plasma ,Laser ,Accelerators and Storage Rings ,Physics - Plasma Physics ,Pulse (physics) ,ddc ,Plasma Physics (physics.plasm-ph) ,Modulation ,Physics::Space Physics ,Physics::Accelerator Physics ,Physics - Accelerator Physics ,Atomic physics ,Frequency modulation - Abstract
We give direct experimental evidence for the observation of the full transverse self-modulation of a relativistic proton bunch propagating through a dense plasma. The bunch exits the plasma with a density modulation resulting from radial wakefield effects with a period reciprocal to the plasma frequency. We show that the modulation is seeded by using an intense laser pulse co-propagating with the proton bunch which creates a relativistic ionization front within the bunch. We show by varying the plasma density over one order of magnitude that the modulation period scales with the expected dependence on the plasma density., Comment: 4 figures, AWAKE collaboration paper, Submitted to PRL
- Published
- 2018
8. Letter
- Author
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The AWAKE Collaboration, Adli, E., Ahuja, A., Apsimon, O., Apsimon, R., Bachmann, A. -M., Barrientos, D., Batsch, F., Bauche, J., Olsen, V. K. Berglyd, Bernardini, M., Bohl, T., Bracco, C., Braunmueller, F., Burt, G., Buttenschoen, B., Caldwell, A., Cascella, M., Chappell, J., Chevallay, E., Chung, M., Cooke, D., Damerau, H., Deacon, L., Deubner, L. H., Dexter, A., Doebert, S., Farmer, J., Fedosseev, V. N., Fiorito, R., Fonseca, R. A., Friebel, F., Garolfi, L., Gessner, S., Gorgisyan, I., Gorn, A. A., Granados, E., Grulke, O., Gschwendtner, E., Hansen, J., Helm, A., Henderson, J. R., Huether, M., Ibison, M., Jensen, L., Jolly, S., Keeble, F., Kim, S. -Y., Kraus, F., Li, Y., Liu, S., Lopes, N., Lotov, K. V., Brun, L. Maricalva, Martyanov, M., Mazzoni, S., Godoy, D. Medina, Minakov, V. A., Mitchell, J., Molendijk, J. C., Moody, J. T., Moreira, M., Muggli, P., Oez, E., Pasquino, C., Pardons, A., Asmus, F. Pena, Pepitone, K., Perera, A., Petrenko, A., Pitman, S., Pukhov, A., Rey, S., Rieger, K., Ruhl, H., Schmidt, J. S., Shalimova, I. A., Sherwood, P., Silva, L. O., Soby, L., Sosedkin, A. P., Speroni, R., Spitsyn, R. I., Tuev, P. V., Turner, M., Velotti, F., Verra, L., Verzilov, V. A., Vieira, J., Welsch, C. P., Williamson, B., Wing, M., Woolley, B., and Xia, G.
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Accelerator Physics (physics.acc-ph) ,Letter ,High energy particle ,Proton ,General Science & Technology ,FOS: Physical sciences ,Electron ,7. Clean energy ,01 natural sciences ,High Energy Physics - Experiment ,010305 fluids & plasmas ,Nuclear physics ,High Energy Physics - Experiment (hep-ex) ,Acceleration ,Affordable and Clean Energy ,Physics::Plasma Physics ,0103 physical sciences ,010306 general physics ,physics.acc-ph ,Physics ,Multidisciplinary ,Large Hadron Collider ,Plasma ,Plasma acceleration ,Accelerators and Storage Rings ,Physics - Plasma Physics ,Ciências Naturais::Outras Ciências Naturais [Domínio/Área Científica] ,Plasma Physics (physics.plasm-ph) ,Bunches ,Physics::Accelerator Physics ,Physics - Accelerator Physics ,Experimental particle physics ,Plasma-based accelerators - Abstract
High-energy particle accelerators have been crucial in providing a deeper understanding of fundamental particles and the forces that govern their interactions. To increase the energy of the particles or to reduce the size of the accelerator, new acceleration schemes need to be developed. Plasma wakefield acceleration1–5, in which the electrons in a plasma are excited, leading to strong electric fields (so called ‘wakefields’), is one such promising acceleration technique. Experiments have shown that an intense laser pulse6–9 or electron bunch10,11 traversing a plasma can drive electric fields of tens of gigavolts per metre and above—well beyond those achieved in conventional radio-frequency accelerators (about 0.1 gigavolt per metre). However, the low stored energy of laser pulses and electron bunches means that multiple acceleration stages are needed to reach very high particle energies5,12. The use of proton bunches is compelling because they have the potential to drive wakefields and to accelerate electrons to high energy in a single acceleration stage13. Long, thin proton bunches can be used because they undergo a process called self-modulation14–16, a particle–plasma interaction that splits the bunch longitudinally into a series of high-density microbunches, which then act resonantly to create large wakefields. The Advanced Wakefield (AWAKE) experiment at CERN17–19 uses high-intensity proton bunches—in which each proton has an energy of 400 gigaelectronvolts, resulting in a total bunch energy of 19 kilojoules—to drive a wakefield in a ten-metre-long plasma. Electron bunches are then injected into this wakefield. Here we present measurements of electrons accelerated up to two gigaelectronvolts at the AWAKE experiment, in a demonstration of proton-driven plasma wakefield acceleration. Measurements were conducted under various plasma conditions and the acceleration was found to be consistent and reliable. The potential for this scheme to produce very high-energy electron bunches in a single accelerating stage20 means that our results are an important step towards the development of future high-energy particle accelerators21,22., Electron acceleration to very high energies is achieved in a single step by injecting electrons into a ‘wake’ of charge created in a 10-metre-long plasma by speeding long proton bunches.
- Published
- 2018
9. Target of Opportunity Observations of Gravitational Wave Events with LSST
- Author
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Margutti, R., Cowperthwaite, P., Doctor, Z., Mortensen, K., Pankow, C. P., Salafia, O., Villar, V. A., Alexander, K., Annis, J., Andreoni, I., Baldeschi, A., Balmaverde, B., Berger, E., Bernardini, M. G., Berry, C. P. L., Bianco, F., Blanchard, P. K., Brocato, E., Carnerero, M. I., Cartier, R., Cenko, S. B., Chornock, R., Chomiuk, L., Copperwheat, C. M., Coughlin, M. W., Coppejans, D. L., Corsi, A., D'Ammando, F., Datrier, L., D'Avanzo, P., Dimitriadis, G., Drout, M. R., Foley, R. J., Fong, W., Fox, O., Ghirlanda, G., Goldstein, D., Grindlay, J., Guidorzi, C., Haiman, Z., Hendry, M., Holz, D., Hung, T., Inserra, C., Jones, D. O., Kalogera, V., Kilpatrick, C. D., Lamb, G., Laskar, T., Levan, A., Mason, E., Maguire, K., Melandri, A., Milisavljevic, D., Miller, A., Narayan, G., Nielsen, E., Nicholl, M., Nissanke, S., Nugent, P., Pan, Y. -C., Pasham, D., Paterson, K., Piranomonte, S., Racusin, J., Rest, A., Righi, C., Sand, D., Seaman, R., Scolnic, D., Siellez, K., Singer, L., Szkody, P., Smith, M., Steeghs, D., Sullivan, M., Tanvir, N., Terreran, G., Trimble, V., Valenti, S., Transient, with the support of the LSST, and Collaboration, Variable Stars
- Subjects
High Energy Astrophysical Phenomena (astro-ph.HE) ,FOS: Physical sciences ,Astrophysics::Cosmology and Extragalactic Astrophysics ,Astrophysics - High Energy Astrophysical Phenomena ,Astrophysics - Instrumentation and Methods for Astrophysics ,Instrumentation and Methods for Astrophysics (astro-ph.IM) ,Astrophysics::Galaxy Astrophysics - Abstract
The discovery of the electromagnetic counterparts to the binary neutron star merger GW170817 has opened the era of GW+EM multi-messenger astronomy. Exploiting this breakthrough requires increasing samples to explore the diversity of kilonova behaviour and provide more stringent constraints on the Hubble constant, and tests of fundamental physics. LSST can play a key role in this field in the 2020s, when the gravitational wave detector network is expected to detect higher rates of merger events involving neutron stars ($\sim$10s per year) out to distances of several hundred Mpc. Here we propose comprehensive target-of-opportunity (ToOs) strategies for follow-up of gravitational-wave sources that will make LSST the premiere machine for discovery and early characterization for neutron star mergers and other gravitational-wave sources., Comment: White paper for LSST cadence optimization- ToOs
- Published
- 2018
- Full Text
- View/download PDF
10. Analyses of germline variants associated with ovarian cancer survival identify functional candidates at the 1q22 and 19p12 outcome loci
- Author
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Glubb, DM, Johnatty, SE, Quinn, MCJ, O'Mara, TA, Tyrer, JP, Gao, B, Fasching, PA, Beckmann, MW, Lambrechts, D, Vergote, I, Edwards, DRV, Beeghly-Fadiel, A, Benitez, J, Garcia, MJ, Goodman, MT, Thompson, PJ, Doerk, T, Duerst, M, Modungo, F, Moysich, K, Heitz, F, du Bois, A, Pfisterer, J, Hillemanns, P, Karlan, BY, Lester, J, Goode, EL, Cunningham, JM, Winham, SJ, Larson, MC, McCauley, BM, Kjaer, SK, Jensen, A, Schildkraut, JM, Berchuck, A, Cramer, DW, Terry, KL, Salvesen, HB, Bjorge, L, Webb, PM, Grant, P, Pejovic, T, Moffitt, M, Hogdall, CK, Hogdall, E, Paul, J, Glasspool, R, Bernardini, M, Tone, A, Huntsman, D, Woo, M, deFazio, A, Kennedy, CJ, Pharoah, PDP, MacGregor, S, Chenevix-Trench, G, Grp, AGOS, Grp, AOCS, Tyrer, Jonathan [0000-0003-3724-4757], Pharoah, Paul [0000-0001-8494-732X], and Apollo - University of Cambridge Repository
- Subjects
meta-analysis ,genetic association ,Oncology and Carcinogenesis ,AGO Study Group ,ovarian cancer outcome ,gene regulation ,health care economics and organizations - Abstract
We previously identified associations with ovarian cancer outcome at five genetic loci. To identify putatively causal genetic variants and target genes, we prioritized two ovarian outcome loci (1q22 and 19p12) for further study. Bioinformatic and functional genetic analyses indicated that MEF2D and ZNF100 are targets of candidate outcome variants at 1q22 and 19p12, respectively. At 19p12, the chromatin interaction of a putative regulatory element with the ZNF100 promoter region correlated with candidate outcome variants. At 1q22, putative regulatory elements enhanced MEF2D promoter activity and haplotypes containing candidate outcome variants modulated these effects. In a public dataset, MEF2D and ZNF100 expression were both associated with ovarian cancer progression-free or overall survival time. In an extended set of 6,162 epithelial ovarian cancer patients, we found that functional candidates at the 1q22 and 19p12 loci, as well as other regional variants, were nominally associated with patient outcome; however, no associations reached our threshold for statistical significance (p
- Published
- 2017
11. AWAKE readiness for the study of the seeded self-modulation of a 400\,GeV proton bunch
- Author
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Muggli, P., Adli, E., Apsimon, R., Asmus, F., Baartman, R., Bachmann, A.-M., Barros Marin, M., Batsch, F., Bauche, J., Berglyd Olsen, V. K., Bernardini, M., Turner, M., Verzilov, V., Vieira, J., Vincke, H., Welsch, C. P., Williamson, B., Wing, M., Xia, G. X., Zhang, H., The AWAKE collaboration, Biskup, B., Blanco Vinuela, E., Boccardi, A., Bogey, T., Bohl, T., Bracco, C., Braunmuller, F., Burger, S., Burt, G., Bustamante, S., Buttenschön, B., Butterworth, A., Caldwell, A., Cascella, M., Chevallay, E., Chung, M., Damerau, H., Deacon, L., Dexter, A., Dirksen, P., Doebert, S., Farmer, J., Fedosseev, V., Feniet, T., Fior, G., Fiorito, R., Fonseca, R. A., Friebel, F., Gander, P., Gessner, S., Gorgisyan, I., Gorn, A. A., Grulke, O., Gschwendtner, E., Guerrero, A., Hansen, J., Hessler, C., Hofle, W., Holloway, J., Hüther, M., Ibison, M., Islam, M. R., Jensen, L., Jolly, S. W., Kasim, M., Keeble, F., Kim, S.-Y., Krausz, F., Lasheen, A., Lefevre, T., LeGodec, G., Li, Y., Liu, S., Lopes, N. C., Lotov, K., Martyanov, M., Mazzoni, S., Medina Godoy, D., Mete, O., Minakov, V. A., Mompo, R., Moody, J. T., Moreira, M. T., Mitchell, J., Mutin, C., Norreys, P., Öz, E., Ozturk, E., Pauw, W., Pardons, A., Pasquino, C., Pepitone, K., Petrenko, A., Pitmann, S., Plyushchev, G., Pukhov, A., Rieger, K., Ruhl, H., Schmidt, J., Shalimova, I. A., Shaposhnikova, E., Sherwood, P., Silva, L., Sosedkin, A. P., Speroni, R., Spitsyn, R. I., Szczurek, K., Thomas, J., Tuev, P. V., and AWAKE Collaboration
- Subjects
Accelerator Physics (physics.acc-ph) ,Proton ,Particle acceleration ,Other Fields of Physics ,chemistry.chemical_element ,FOS: Physical sciences ,01 natural sciences ,Ciências Naturais::Ciências Físicas [Domínio/Área Científica] ,010305 fluids & plasmas ,law.invention ,Rubidium ,law ,Physics::Plasma Physics ,Seeded self-modulation ,Ionization ,physics.plasm-ph ,Plasma wakefields driven by protons ,0103 physical sciences ,Physics::Atomic Physics ,010306 general physics ,Nuclear Experiment ,physics.acc-ph ,Physics ,Plasma ,Plasma-based accelerator ,Condensed Matter Physics ,Plasma acceleration ,Laser ,Accelerators and Storage Rings ,Physics - Plasma Physics ,Pulse (physics) ,Plasma Physics (physics.plasm-ph) ,Nuclear Energy and Engineering ,chemistry ,Physics::Accelerator Physics ,Seeding ,Physics - Accelerator Physics ,Plasma wakefields seeding ,Atomic physics - Abstract
AWAKE is a proton-driven plasma wakefield acceleration experiment. % We show that the experimental setup briefly described here is ready for systematic study of the seeded self-modulation of the 400\,GeV proton bunch in the 10\,m-long rubidium plasma with density adjustable from 1 to 10$\times10^{14}$\,cm$^{-3}$. % We show that the short laser pulse used for ionization of the rubidium vapor propagates all the way along the column, suggesting full ionization of the vapor. % We show that ionization occurs along the proton bunch, at the laser time and that the plasma that follows affects the proton bunch. %, Comment: Presented as an invited talk at the EPS=Plasma Physics Conference 2017
- Published
- 2017
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12. Multi-messenger Observations of a Binary Neutron Star Merger
- Author
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Abbott, B. P., Abbott, R., Abbott, T. D., Acernese, F., Ackley, K., Adams, C., Adams, T., Addesso, P., Adhikari, R. X., Adya, V. B., Affeldt, C., Afrough, M., Agarwal, B., Agathos, M., Agatsuma, K., Aggarwal, N., Aguiar, O. D., Aiello, L., Ain, A., Ajith, P., Allen, B., Allen, G., Allocca, A., Altin, P. A., Amato, A., Ananyeva, A., Anderson, S. B., Anderson, W. G., Angelova, S. V., Antier, S., Appert, S., Arai, K., Araya, M. C., Areeda, J. S., Arnaud, N., Arun, K. G., Ascenzi, S., Ashton, G., Ast, M., Aston, S. M., Astone, P., Atallah, D. V., Aufmuth, P., Aulbert, C., AultONeal, K., Austin, C., Avila-Alvarez, A., Babak, S., Bacon, P., Bader, M. K. M., Bae, S., Baker, P. T., Baldaccini, F., Ballardin, G., Ballmer, S. W., Banagiri, S., Barayoga, J. C., Barclay, S. E., Barish, B. C., Barker, D., Barkett, K., Barone, F., Barr, B., Barsotti, L., Barsuglia, M., Barta, D., Barthelmy, S. D., Bartlett, J., Bartos, I., Bassiri, R., Basti, A., Batch, J. C., Bawaj, M., Bayley, J. C., Bazzan, M., Bécsy, B., Beer, C., Bejger, M., Belahcene, I., Bell, A. S., Berger, B. K., Bergmann, G., Bero, J. J., Berry, C. P. L., Bersanetti, D., Bertolini, A., Betzwieser, J., Bhagwat, S., Bhandare, R., Bilenko, I. A., Billingsley, G., Billman, C. R., Birch, J., Birney, R., Birnholtz, O., Biscans, S., Biscoveanu, S., Bisht, A., Bitossi, M., Biwer, C., Bizouard, M. A., Blackburn, J. K., Blackman, J., Blair, C. D., Blair, D. G., Blair, R. M., Bloemen, S., Bock, O., Bode, N., Boer, M., Bogaert, G., Bohe, A., Bondu, F., Bonilla, E., Bonnand, R., Boom, B. A., Bork, R., Boschi, V., Bose, S., Bossie, K., Bouffanais, Y., Bozzi, A., Bradaschia, C., Brady, P. R., Branchesi, M., Brau, J. E., Briant, T., Brillet, A., Brinkmann, M., Brisson, V., Brockill, P., Broida, J. E., Brooks, A. F., Brown, D. A., Brown, D. D., Brunett, S., Buchanan, C. C., Buikema, A., Bulik, T., Bulten, H. J., Buonanno, A., Buskulic, D., Buy, C., Byer, R. 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H., Niculescu-Oglinzanu, M., Niechciol, M., Niemietz, L., Niggemann, T., Nitz, D., Nosek, D., Novotny, V., Nožka, L., Núñez, L. A., Oikonomou, F., Olinto, A., Palatka, M., Pallotta, J., Papenbreer, P., Parente, G., Parra, A., Paul, T., Pech, M., Pedreira, F., Pȩkala, J., Peña-Rodriguez, J., Pereira, L. A. S., Perlin, M., Perrone, L., Peters, C., Petrera, S., Phuntsok, J., Pierog, T., Pimenta, M., Pirronello, V., Platino, M., Plum, M., Poh, J., Porowski, C., Prado, R. R., Privitera, P., Prouza, M., Quel, E. J., Querchfeld, S., Quinn, S., Ramos-Pollan, R., Rautenberg, J., Ravignani, D., Ridky, J., Riehn, F., Risse, M., Ristori, P., Rizi, V., Rodrigues de Carvalho, W., Rodriguez Fernandez, G., Rodriguez Rojo, J., Roncoroni, M. J., Roth, M., Roulet, E., Rovero, A. C., Ruehl, P., Saffi, S. J., Saftoiu, A., Salamida, F., Saleh, A., Salina, G., Sánchez, F., Sanchez-Lucas, P., Santos, E. M., Santos, E., Sarazin, F., Sarmento, R., Sarmiento-Cano, C., Sato, R., Schauer, M., Scherini, V., Schieler, H., Schimp, M., Schmidt, D., Scholten, O., Schovánek, P., Schröder, F. G., Schröder, S., Schumacher, J., Sciutto, S. J., Segreto, A., Shadkam, A., Shellard, R. C., Sigl, G., Silli, G., Šmída, R., Snow, G. R., Sommers, P., Sonntag, S., Soriano, J. F., Squartini, R., Stanca, D., Stanič, S., Stasielak, J., Stassi, P., Stolpovskiy, M., Strafella, F., Streich, A., Suarez, F., Suarez-Durán, M., Sudholz, T., Suomijärvi, T., Supanitsky, A. D., Šupík, J., Swain, J., Szadkowski, Z., Taboada, A., Taborda, O. A., Timmermans, C., Todero Peixoto, C. J., Tomankova, L., Tomé, B., Torralba Elipe, G., Travnicek, P., Trini, M., Tueros, M., Ulrich, R., Unger, M., Urban, M., Valdés Galicia, J. F., Valiño, I., Valore, L., Aar, G. van, Bodegom, P. van, van den Berg, A. M., Vliet, A. van, Varela, E., Cárdenas, B. Vargas, Vázquez, R. A., Veberič, D., Ventura, C., Vergara Quispe, I. D., Verzi, V., Vicha, J., Villaseñor, L., Vorobiov, S., Wahlberg, H., Wainberg, O., Walz, D., Watson, A. A., Weber, M., Weindl, A., Wiedeński, M., Wiencke, L., Wilczyński, H., Wirtz, M., Wittkowski, D., Wundheiler, B., Yushkov, A., Zas, E., Zavrtanik, D., Zavrtanik, M., Zepeda, A., Zimmermann, B., Ziolkowski, M., Zong, Z., Zuccarello, F., Kim, S., Schulze, S., Corral-Santana, J. M., de Gregorio-Monsalvo, I., González-López, J., Hartmann, D. H., Ishwara-Chandra, C. H., Martín, S., Mehner, A., Misra, K., Michałowski, M. J., Resmi, L., Paragi, Z., Agudo, I., An, T., Beswick, R., Casadio, C., Frey, S., Jonker, P., Kettenis, M., Marcote, B., Moldon, J., Szomoru, A., van Langevelde, H. J., Cwiek, A., Cwiok, M., Czyrkowski, H., Dabrowski, R., Kasprowicz, G., Mankiewicz, L., Nawrocki, K., Opiela, R., Piotrowski, L. W., Wrochna, G., Zaremba, M., Żarnecki, A. F., Haggard, D., Nynka, M., Ruan, J. J., Bland, P. A., Booler, T., Devillepoix, H. A. R., Gois, J. S. de, Hancock, P. J., Howie, R. M., Paxman, J., Sansom, E. K., Towner, M. C., Tonry, J., Coughlin, M., Stubbs, C. W., Denneau, L., Heinze, A., Stalder, B., Weiland, H., Eatough, R. P., Kramer, M., Kraus, A., Piro, L., González, J. Becerra, Butler, N. R., Khandrika, H. G., Kutyrev, A., Lee, W. H., Ricci, R., Ryan Jr., R. E., Sánchez-Ramírez, R., Veilleux, S., Watson, A. M., Wieringa, M. H., Burgess, J. M., Eerten, H. van, Fontes, C. J., Korobkin, O., Wollaeger, R. T., Camilo, F., Foley, A. R., Goedhart, S., Makhathini, S., Oozeer, N., Smirnov, O. M., and Woudt, P. A.
- Subjects
ddc - Published
- 2016
13. Diversity of GRB energetics vs. SN homogeneity: supernova 2013cq associated with the gamma-ray burst 130427A
- Author
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Melandri, A., Pian, E., D'Elia, V., D'Avanzo, P., Della Valle, M., Mazzali, P. A., Tagliaferri, G., Cano, Z., Levan, A. J., Møller, P., Amati, L., Bernardini, M. G., Bersier, D., Bufano, F., Campana, S., Castro-Tirado, A. J., Covino, S., Ghirlanda, G., Hurley, K., Malesani, D., Masetti, N., Palazzi, E., Piranomonte, S., Rossi, A., Salvaterra, R., Starling, R. L. C., Tanaka, M., Tanvir, N. R., and Vergani, S. D.
- Subjects
High Energy Astrophysical Phenomena (astro-ph.HE) ,Cosmology and Nongalactic Astrophysics (astro-ph.CO) ,FOS: Physical sciences ,Astrophysics - High Energy Astrophysical Phenomena ,Astrophysics - Cosmology and Nongalactic Astrophysics - Abstract
Long-duration gamma-ray bursts (GRBs) have been found to be associated with broad-lined type-Ic supernovae (SNe), but only a handful of cases have been studied in detail. Prompted by the discovery of the exceptionally bright, nearby GRB130427A (redshift z=0.3399), we aim at characterising the properties of its associated SN2013cq. This is the first opportunity to test directly the progenitors of high-luminosity GRBs. We monitored the field of the Swift long duration GRB130427A using the 3.6-m TNG and the 8.2-m VLT during the time interval between 3.6 and 51.6 days after the burst. Photometric and spectroscopic observations revealed the presence of the type Ic SN2013cq. Spectroscopic analysis suggests that SN2013cq resembles two previous GRB-SNe, SN1998bw and SN2010bh associated with GRB980425 and XRF100316D, respectively. The bolometric light curve of SN2013cq, which is significantly affected by the host galaxy contribution, is systematically more luminous than that of SN2010bh ($\sim$ 2 mag at peak), but is consistent with SN1998bw. The comparison with the light curve model of another GRB-connected SN2003dh, indicates that SN2013cq is consistent with the model when brightened by 20%. This suggests a synthesised radioactive $^{56}$Ni mass of $\sim 0.4 M_\odot$. GRB130427A/SN2013cq is the first case of low-z GRB-SN connection where the GRB energetics are extreme ($E_{\rm \gamma, iso} \sim 10^{54}$ erg). We show that the maximum luminosities attained by SNe associated with GRBs span a very narrow range, but those associated with XRFs are significantly less luminous. On the other hand the isotropic energies of the accompanying GRBs span 6 orders of magnitude (10$^{48}$ erg $< E_{\rm \gamma, iso}, Comment: To appear in Astronomy and Astrophysics: 10 pages, 5 figures
- Published
- 2014
- Full Text
- View/download PDF
14. Astrophysical sources of gravitational waves
- Author
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Caron, B., Dominjon, A., Drezen, C., Flaminio, R., Grave, X., Marion, F., Massonnet, L., Mehmel, C., Morand, R., Mours, B., Yvert, M., Babusci, D., Giordano, G., Matone, G., Mackowski, J. M., Napolitano, M., Pinard, L., Dognin, L., Barone, Fabrizio, Calloni, E., Di Fiore, L., Flagiello, M., Grado, A., Longo, Maurizio, Lops, M., Marano, Stefano, Milano, L., Russo, G., Solimeno, S., Acker, Y., Brillet, A., Bondu, F., Brisson, V., Cavalier, F., Davier, M., Heitmann, H., Hello, P., Jacquemet, M., Latrach, L., Le Diberder, F., Man, C. N., Manh, P. T., Taubmann, M., Vinet, J. Y., Boccara, C., Gleyzes, P. h., Roger, J. P., Loriette, V., Cagnoli, G., Gammaitoni, L., Kovalik, J., Marchesoni, F., Punturo, M., Barsuglia, M., Bernardini, M., Braccini, S., Bradaschia, C., Del Fabbro, R., De Salvo, R., Di Virgilio, A., Ferrante, I., Fidecaro, F., Giassi, A., Giazotto, A., Gorini, G., Holloway, L., Lami, S., Lapenna, P., Losurdo, G., Mancini, S., Morganti, M., Palla, F., Pan, H. B., Passuello, D., Poggiani, R., Torelli, G., Zhang, Z., Majorana, E., Puppo, P., Rapagnani, P., and Ricci, F.
- Subjects
Physics ,Nuclear and High Energy Physics ,Gravitational-wave observatory ,Gravitational wave ,Astrophysics::High Energy Astrophysical Phenomena ,Astrophysics::Instrumentation and Methods for Astrophysics ,Astronomy ,Astrophysics::Cosmology and Extragalactic Astrophysics ,Astrophysics ,Gravitational-wave astronomy ,Atomic and Molecular Physics, and Optics ,LIGO ,Gravitational energy ,General Relativity and Quantum Cosmology ,Neutron star ,Gravitational collapse ,Astrophysics::Galaxy Astrophysics ,Gravitational redshift - Abstract
The interferometric detectors of gravitational waves (GW) (such as VIRGO and LIGO) will search for events in a frequency band within a few Hz and a few kHz, where several sources are expected to emit. In this talk we outline briefly the current theoretical knowledge on the emission of GW in events such as the coalescence of compact binaries, the gravitational collapse, the spinning of a neutron stars. Expected amplitudes are compared with the target sensitivity of the VIRGO/LIGO interferometric detectors.
- Published
- 2000
15. Virgo and interferometer for gravitational wave detection
- Author
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Caron, B., Dominjon, A., Drezen, C., Flaminio, R., Grave, X., Marion, F., Massonnet, L., Mehmel, C., Morand, R., Mours, B., Yvert, M., Babusci, D., Giordano, G., Matone, G., Mackowski, J. M., Napolitano, M., Pinard, L., Dognin, L., Barone, Fabrizio, Calloni, E., Di Fiore, L., Flagiello, M., Grado, A., Longo, Maurizio, Lops, M., Marano, Stefano, Milano, L., Russo, G., Solimeno, S., Acker, Y., Brillet, A., Bondu, F., Brisson, V., Cavalier, F., Davier, M., Heitmann, H., Hello, P., Jacquemet, M., Latrach, L., Le Diberder, F., Man, C. N., Manh, P. T., Taubmann, M., Vinet, J. Y., Boccara, C., Gleyzes, P. h., Roger, J. P., Loriette, V., Cagnoli, G., Gammaitoni, L., Kovalik, J., Marchesoni, F., Punturo, M., Barsuglia, M., Bernardini, M., Braccini, S., Bradaschia, C., Del Fabbro, R., De Salvo, R., Di Virgilio, A., Ferrante, I., Fidecaro, F., Giassi, A., Giazotto, A., Gorini, G., Holloway, L., Lami, S., Lapenna, P., Losurdo, G., Mancini, S., Morganti, M., Palla, F., Pan, H. B., Passuello, D., Poggiani, R., Torelli, G., Zhang, Z., Majorana, E., Puppo, P., Rapagnani, P., and Ricci, F.
- Subjects
Physics ,Nuclear and High Energy Physics ,Gravitational wave ,Detector ,Astrophysics::Instrumentation and Methods for Astrophysics ,Physics::Optics ,Astronomy ,Michelson interferometer ,Astrophysics::Cosmology and Extragalactic Astrophysics ,Astrophysics ,Atomic and Molecular Physics, and Optics ,law.invention ,General Relativity and Quantum Cosmology ,Interferometry ,law ,Astrophysics::Galaxy Astrophysics ,Noise (radio) - Abstract
Gravitational waves propagating from rapidly accelerating star masses can be detected by means of interferometric techniques. The Virgo detector is a Michelson interferometer, with two 3 km long Fabry-Perot cavities, that is going to be built in the countryside of Pisa (Italy). Principles of interferometric gravitational wave detection, and the main noise sources in the Virgo apparatus are treated. The Virgo optical scheme and its main components are also described. Finally, an overview on the status of works at the Virgo site is presented.
- Published
- 2000
16. Dust extinction for an unbiased sample of GRB afterglows
- Author
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Covino, S., Melandri, A., Salvaterra, R., Campana, S., Vergani, S. D., Bernardini, M. G., D'Avanzo, P., D'Elia, V., Fugazza, D., Ghirlanda, G., Ghisellini, G., Gomboc, A., Jin, Z. P., Kruehler, T., Malesani, D., Nava, L., Sbarufatti, B., and Tagliaferri, G.
- Subjects
High Energy Astrophysical Phenomena (astro-ph.HE) ,Astrophysics::High Energy Astrophysical Phenomena ,FOS: Physical sciences ,Astrophysics::Cosmology and Extragalactic Astrophysics ,Astrophysics - High Energy Astrophysical Phenomena ,Astrophysics::Galaxy Astrophysics - Abstract
In this paper we compute rest-frame extinctions for the afterglows of a sample of gamma-ray bursts complete in redshift. The selection criteria of the sample are based on observational high-energy parameters of the prompt emission and therefore our sample should not be biased against dusty sight-lines. It is therefore expected that our inferences hold for the general population of gamma-ray bursts. Our main result is that the optical/near-infrared extinction of gamma-ray burst afterglows in our sample does not follow a single distribution. 87% of the events are absorbed by less than 2 mag, and 50% suffer from less than 0.3-0.4 mag extinction. The remaining 13% of the afterglows are highly absorbed. The true percentage of gamma-ray burst afterglows showing high absorption could be even higher since a fair fraction of the events without reliable redshift measurement are probably part of this class. These events may be due to highly dusty molecular clouds/star forming regions associated with the gamma-ray burst progenitor or along the afterglow line of sight, and/or to massive dusty host galaxies. No clear evolution in the dust extinction properties is evident within the redshift range of our sample, although the largest extinctions are at z~1.5-2, close to the expected peak of the star formation rate. Those events classified as dark are characterized, on average, by a higher extinction than typical events in the sample. A correlation between optical/near-infrared extinction and hydrogen-equivalent column density based on X-ray studies is shown although the observed NH appears to be well in excess compared to those observed in the Local Group. Dust extinction does not seem to correlate with GRB energetics or luminosity., Comment: 18 pages, 7 figures, 10 tables, MNRAS, in press
- Published
- 2013
- Full Text
- View/download PDF
17. A comparative study of turbulent boundary layer wall pressure fluctuations obtained from high-speed tomographic PIV and DNS
- Author
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Probsting, S., fulvio scarano, Bernardini, M., and Pirozzoli, S.
- Published
- 2012
18. A comprehensive statistical analysis of Swift X-ray light-curves: the prompt-afterglow connection in Gamma-Ray Bursts
- Author
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Margutti, Raffaella, Zaninoni, E., Bernardini, M. G., and Chincarini, G.
- Subjects
High Energy Astrophysical Phenomena (astro-ph.HE) ,Astrophysics::High Energy Astrophysical Phenomena ,Astrophysics::Instrumentation and Methods for Astrophysics ,FOS: Physical sciences ,Astrophysics - High Energy Astrophysical Phenomena - Abstract
We present a comprehensive statistical analysis of Swift X-ray light-curves of Gamma-Ray Bursts (GRBs), with more than 650 GRBs. Two questions drive this effort: (1) Does the X-ray emission retain any kind of memory of the prompt phase? (2) Where is the dividing line between long and short GRBs? We show that short GRBs decay faster, are less luminous and less energetic than long GRBs, but are interestingly characterized by very similar intrinsic absorption. Our analysis reveal the existence of a number of relations that link the X-ray to prompt parameters in long GRBs; short GRBs are outliers of the majority of these 2-parameter relations. Here we concentrate on a 3-parameter (E_pk-Egamma,iso-E_X,iso) scaling that is shared by the GRB class as a whole (short GRBs, long GRBs and X-ray Flashes -XRFs): interpreted in terms of emission efficiency, this scaling may imply that GRBs with high $E_{\rm{pk}}$ are more efficient during their prompt emission., Comment: Proceedings of Science, "Gamma-Ray Bursts 2012" conference (Munich)
- Published
- 2012
- Full Text
- View/download PDF
19. Analysis of GRB 050509b
- Author
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DE BARROS, Gustavo, Bernardini, M. G., Bianco, Carlo Luciano, Caito, Letizia, Guida, R., and Ruffini, Remo
- Published
- 2011
20. GRB 060614: another example of 'fake' short burst from a merging binary system
- Author
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Caito, Letizia, Bernardini, M. G., Bianco, Carlo Luciano, Dainotti, M. G., Guida, R., and Ruffini, Remo
- Published
- 2011
21. Equations of motion of the 'fireshell'
- Author
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Bianco, Carlo Luciano, Bernardini, M. G., Caito, Letizia, Dainotti, M. G., Guida, R., Ruffini, Remo, Vereshchagin, G. V., and Xue, S. S.
- Published
- 2011
22. The GRB classification within the 'fireshell' model: short, long and 'fake' short GRBs
- Author
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Bernardini, M. G., Bianco, Carlo Luciano, Caito, Letizia, Dainotti, M. G., Guida, R., and Ruffini, Remo
- Published
- 2011
23. GRB 090423 in the fireshell scenario
- Author
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Izzo, L., Bernardini, M. G., Bianco, C. L., Caito, L., Patricelli, B., and Ruffini, Remo
- Published
- 2010
24. The end of the prompt emission within the fireshell model
- Author
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Bernardini, M. G., Bianco, C. L., Caito, L., Izzo, L., Patricelli, B., and Ruffini, Remo
- Published
- 2010
25. The fireshell model for Gamma-Ray Bursts
- Author
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Aksenov, A. G., Bernardini, M. G., Bianco, C. L., Caito, L., Cherubini, C, DE BARROS, G., Geralico, A., Izzo, L., Massucci, F. A., Patricelli, B, Rotondo, M., RUEDA HERNANDEZ, J. A., Ruffini, Remo, Vereshchagin, G, and Xue, S. S.
- Published
- 2010
26. Fattori di rischio, precursori, prodromi e caratteristiche cliniche delle psicosi giovanili
- Author
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Pollice, R, Di Mauro, S, Bernardini, M, Di Fabio, P, Santini, I, Ussorio, D, Di Giovambattista, E, De Simone, M, Roncone, Rita, and Casacchia, M.
- Published
- 2008
27. Population Dynamics of Natural Yeasts During Storage of Moscato and Prosecco Grape Pomace for Production of Grappa
- Author
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Bovo, Barbara, Andrighetto, C., Bernardini, M., Carlot, M., Filippini, Rachele, Lombardi, A., Giacomini, Alessio, and Corich, Viviana
- Published
- 2006
28. GRB 970228 and Its Associated Supernova within the EMBH Model
- Author
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Ruffini, Remo, Bernardini, M. G., Bianco, C. L., Corsi, A, Xue, S. S., and Chardonnet, P. AND FRASCHETTI F.
- Published
- 2006
29. General Features of GRB 030329 in the EMBH Model
- Author
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Bernardini, M. G., Bianco, C. L., Ruffini, Remo, Xue, S. S., and Chardonnet, P. AND FRASCHETTI F.
- Published
- 2006
30. Membro Comitato scientifico XVI Congresso Nazionale di Agopuntura dell'AIAM e XI incontro della Commissione Interuniversitaria di ricerca in agopuntura, 1 Marzo, Roma (relazione S. Ricci: Introduzione scientifica ai lavori)
- Author
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Bangrazi Petti, F., Spitali, R., Liguori, A., Pontieri, G. M., Osborn, J., Ippoliti, F., Ricci, Serafino, D. Camaioni, Z. Chong, and Bernardini, M.
- Published
- 2003
31. The intragastric infection of mice as a novel model of shigellosis
- Author
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Martino, C., Rossi, Giacomo, Martini, I., Citro, G., Phalipon, A., Sansonetti, P. J., Chiavolini, D., Pozzi, G., and Bernardini, M. L.
- Published
- 2002
32. The creep problem in the VIRGO suspensions: a possible solution using Maraging steel RID B-5375-2009 RID A-1920-2008
- Author
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Beccaria, M, Bernardini, M, Braccini, S, Bradaschia, C, Cagnoli, G, Casciano, C, Cella, G, Cuoco, E, Dattilo, V, De Carolis, G, De Salvo, R, Di Virgilio, A, Feng, Gt, Ferrante, Isidoro, Fidecaro, Francesco, Frasconi, F, Gaddi, A, Gammaitoni, L, Gennai, A, Giazotto, A, Holloway, L, Kovalik, J, La Penna, P, Losurdo, G, Malik, S, Mancini, S, Marchesoni, F, Nicolas, J, Palla, F, Pan, Hb, Paoletti, F, Pasqualetti, A, Passuello, D, Poggiani, Rosa, Popolizio, P, Punturo, M, Raffaelli, F, Rubino, V, Valentini, Renzo, Vicere, A, Waharte, F, and Zhang, Z.
- Published
- 1998
33. SEVERE INTRAUTERINE GROWTH RETARDATION (IUGR), MICROCEPHALY AND SENSORINEURAL DEAFNESS ASSOCIATED WITH INCREASED IGF-1 CONCENTRATIONS
- Author
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Ghirri, Paolo, Coccoli, L, Bernardini, M, Cuttano, A, Vuerich, M, Saggese, Giuseppe, Bottone, U, and Boldrini, Antonio
- Published
- 1998
34. The VIRGO interferometer for gravitational wave detection RID C-9235-2011 RID B-5375-2009 RID A-1920-2008
- Author
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Caron, B, Dominjon, A, Drezen, C, Flaminio, R, Grave, X, Marion, F, Massonnet, L, Mehmel, C, Morand, R, Mours, B, Sannibale, V, Yvert, M, Babusci, D, Bellucci, S, Candusso, S, Giordano, G, Matone, G, Mackowski, Jm, Pinard, L, Barone, F, Calloni, E, Difiore, L, Flagiello, M, Garuti, F, Grado, A, Longo, M, Lops, M, Marano, S, Milano, L, Solimeno, S, Brisson, V, Cavalier, F, Davier, M, Hello, P, Heusse, P, Mann, P, Acker, Y, Barsuglia, M, Bhawal, B, Bondu, F, Brillet, A, Heitmann, H, Innocent, Jm, Latrach, L, Man, Cn, Phamtu, M, Tournier, E, Taubmann, M, Vinet, Jy, Boccara, C, Gleyzes, P, Loriette, V, Roger, Jp, Cagnoli, G, Gammaitoni, L, Kovalik, J, Marchesoni, F, Punturo, M, Beccaria, M, Bernardini, M, Bougleux, E, Braccini, S, Bradaschia, C, Cella, G, Ciampa, A, Cuoco, E, Curci, G, Delfabbro, R, Desalvo, R, Divirgilio, A, Enard, D, Ferrante, Isidoro, Fidecaro, Francesco, Giassi, A, Giazotto, A, Holloway, L, Lapenna, P, Losurdo, G, Mancini, S, Mazzoni, M, Palla, F, Pan, Hb, Passuello, D, Pelfer, P, Poggiani, Rosa, Stanga, R, Vicere, A, Zhang, Z, Ferrari, V, Majorana, E, Puppo, P, Rapagnani, P, and Ricci, F.
- Published
- 1997
35. Status of the VIRGO experiment RID B-5375-2009 RID A-1920-2008
- Author
-
Caron, B, Dominjon, A, Drezen, C, Flaminio, R, Grave, X, Marion, F, Massonnet, L, Mehmel, C, Morand, R, Mours, B, Yvert, M, Babusci, D, Giordano, G, Matone, G, Mackowski, Jm, Napolitano, M, Pinard, L, Dognin, L, Barone, F, Calloni, E, Difiore, L, Flagiello, M, Grado, A, Longo, M, Lops, M, Marano, S, Milano, L, Russo, G, Solimeno, S, Acker, Y, Brillet, A, Bondu, F, Brisson, V, Cavalier, F, Davier, M, Heitmann, H, Hello, P, Jacquemet, M, Latrach, L, Lediberder, F, Man, Cn, Manh, Pt, Taubmann, M, Vinet, Jy, Boccara, C, Gleyzes, P, Roger, Jp, Loriette, V, Cagnoli, G, Gammaitoni, L, Kovalik, J, Marchesoni, F, Punturo, M, Barsuglia, M, Bernardini, M, Braccini, S, Bradaschia, C, Delfabbro, R, Desalvo, R, Divirgilio, A, Ferrante, Isidoro, Fidecaro, Francesco, Giassi, A, Giazotto, A, Gorini, G, Holloway, L, Lami, S, Lapenna, P, Losurdo, G, Mancini, S, Morganti, M, Palla, F, Pan, Hb, Passuello, D, Poggiani, Rosa, Torelli, G, Zhang, Z, Majorana, E, Puppo, P, Rapagnani, P, and Ricci, F.
- Published
- 1996
36. Suspension of detection masses for the virgo interferometer
- Author
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Caron, B., Dominjon, A., Drezen, C., Flaminio, R., Grave, X., Marion, F., Massonnet, L., Mehmel, C., Morand, R., Mours, B., Yvert, M., Babusci, D., Giordano, G., Matone, G., Mackowski, J. M., Napolitano, M., Pinard, L., Dognin, L., Barone, Fabrizio, Calloni, E., Di Fiore, L., Flagiello, M., Grado, A., Longo, Maurizio, Lops, M., Marano, Stefano, Milano, L., Russo, G., Solimeno, S., Acker, Y., Brillet, A., Bondu, F., Brisson, V., Cavalier, F., Heitmann, M. Davier H., Hello, P., Jacquemet, M., Latrach, L., Le Diberder, F., Man, C. N., Manh, P. T., Taubmann, M., Vinet, J. Y., Boccara, C., Gleyzes, P. h., Roger, J. P., Loriette, V., Cagnoli, G., Gammaitoni, L., Kovalik, J., Marchesoni, F., Punturo, M., Barsuglia, M., Bernardini, M., Braccini, S., Bradaschia, C., Del Fabbro, R., De Salvo, R., Di Virgilio, A., Ferrante, I., Fidecaro, F., Giassi, A., Giazotto, A., Gorini, G., Holloway, L., Lami, S., Lapenna, P., Losurdo, G., Mancini, S., Morganti, M., Palla, F., Pan, H. B., Passuello, D., Poggiani, R., Torelli, G., Zhang, Z., Majorana, E., Puppo, P., Rapagnani, P., and Ricc, F.
- Subjects
Physics ,Nuclear and High Energy Physics ,Interferometry ,Optics ,business.industry ,Gravitational wave ,Astrophysics::Instrumentation and Methods for Astrophysics ,Virgo interferometer ,Sensitivity (control systems) ,Seismic noise ,Suspension (vehicle) ,business ,Atomic and Molecular Physics, and Optics - Abstract
The masses used by the Virgo interferometer to detect gravitational waves need adequate isolation from seismic noise. A multistage suspension system has been designed to extend the interferometer sensitivity down around 4 Hz. Motivations for this choice and an outline of the solutions adopted are given.
- Published
- 1996
37. Antibiotic resistance transposons on a virulence plasmid from Salmonella wien
- Author
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Colonna, B., Bernardini, M., Gioacchino Micheli, Maimone, F., Nicoletti, M., Casalino, M., Colonna, B, Bernardini, M, Micheli, G, Maimone, F, Nicoletti, M, and Casalino, Maria Assunta
- Subjects
Virulence ,Salmonella ,Drug Resistance, Bacterial ,DNA Transposable Elements ,Microbial Sensitivity Tests ,Anti-Bacterial Agents - Published
- 1989
38. Science with the Cherenkov Telescope Array
- Author
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Cascone, E., Valore, L., Vallania, P., Valentino, M., Vagnetti, F., Vagelli, V., Umana, G., Tsujimoto, S., Pujadas, I., Trifoglio, M., Trichard, C., Travnicek, P., Tovmassian, G., Tothill, N., Tosti, G., Torresi, E., Torres, D., Tornikoski, M., Tonev, D., Tomastik, J., Tokanai, F., Peixoto, C., Tluczykont, M., Tibaldo, L., Tian, W., Thoudam, S., Testa, V., Teshima, M., Terzic, T., Terrier, R., Terada, Y., Temnikov, P., Tejedor, L., Tayabaly, K., Tavernet, J., Tavecchio, F., Tavani, M., Tajima, H., Tagliaferri, G., Supanitsky, A., Suomijarvi, T., Straumann, U., Stratta, G., Stolarczyk, T., Stephan, M., Stefanik, S., Stawarz, Ł., Starling, R., Stanič, S., Stamerra, A., Sol, H., Slowikowska, A., Sliusar, V., Sitarek, J., Sironi, G., Sillanpää, A., Siejkowski, H., Sidoli, L., Shellard, R., Shalchi, A., Servillat, M., Sergijenko, O., Semikoz, D., Seitenzahl, I., Scuderi, S., Sciacca, E., Schwanke, U., Schussler, F., Schulz, A., Schovanek, P., Schoorlemmer, H., Schneider, M., Schlenstedt, S., Schioppa, E., Saturni, F., Satalecka, K., Sarkar, S., Santander, M., Sano, H., Sanguillon, M., Sangiorgi, P., Sandoval, A., Sandaker, H., Sánchez-Conde, M., Salina, G., Sakurai, S., Sakaki, N., Saito, T., Safi-Harb, S., Sadeh, I., Rulten, C., Rugliancich, A., Rudak, B., Rowell, G., Rovero, A., Rosado, J., Romeo, G., Romano, P., Rojas, G., Vázquez, J., Fernandez, G., Rodriguez, J., Rizi, V., Rivoire, S., Riquelme, M., Rieger, F., Rico, J., Richtler, T., Ribó, M., Ribeiro, D., Rhode, W., Rezaeian, A., Renaud, M., Reisenegger, A., Reimer, A., Reimer, O., Razzaque, S., Rainò, S., Quirrenbach, A., Queiroz, F., Pürckhauer, S., Punch, M., Pühlhofer, G., Prouza, M., Prokoph, H., Prokhorov, D., Principe, G., Prast, J., Prandini, E., Pozo, D., Polo, M., Pohl, M., Pita, S., Pisarski, A., Piano, G., Pfeifer, M., Peyaud, B., Petruk, O., Petrucci, P., Petrashyk, A., Persic, M., Perri, M., Pedaletti, G., Pech, M., PeEr, A., Parsons, R., Pareschi, G., Paredes, J., Naito, T., Nagayoshi, T., Nagataki, S., Nagai, A., Murase, K., Muraishi, H., Murach, T., Mundell, C., Mukherjee, R., Moulin, E., Morselli, A., Morris, P., Morlino, G., Mori, K., Morcuende-Parrilla, D., Moralejo, A., Montaruli, T., Mohrmann, L., Mohammed, M., Moderski, R., Mizuno, T., Mitchell, A., Mirzoyan, R., Mirabal, N., Minaya, I., Meyer, M., Mereghetti, S., Melandri, A., Medina, C., Mazin, D., Maxted, N., Maurin, G., Masuda, S., Masetti, N., Martínez, G., Martínez, M., Martin, P., Martí, J., Markoff, S., Marín, J., Marcowith, A., Mangano, S., Manganaro, M., Maneva, G., Mandat, D., Malaguti, G., Majumdar, P., Maier, G., Maccarone, M., Lyard, E., Luque-Escamilla, P., Lucarelli, F., Lu, C., López-Coto, R., López, M., Longo, F., Lombardi, S., Lohse, T., Lindfors, E., Limon, M., Lico, R., Lenain, J., De Oliveira, M., Lefaucheur, J., Lees, J., Leach, S., Blanc, O., Lapington, J., Lang, R., Lamanna, G., La Palombara, N., Kushida, J., Kuroda, H., Mezek, G., Kubo, H., Krauß, F., Krause, M., Kraus, M., Kosack, K., Komin, N., Kohri, K., Koch, B., Knödlseder, J., Knapp, J., Kisaka, S., Kimura, S., Kimeswenger, S., Kieda, D., Khélifi, B., Kazanas, D., Kawanaka, N., Katz, U., Katagiri, H., Karkar, S., Kaaret, P., Jurysek, J., Jung-Richardt, I., Jean, P., Jankowsky, D., Janecek, P., Jamrozy, M., Iwamura, Y., Ishio, K., Iori, M., Ioka, K., Iocco, F., Inoue, Y., Inoue, T., Inoue, S., Inome, Y., Inada, T., Iarlori, M., Hütten, M., Humensky, T., Hrupec, D., Hrabovsky, M., Hovatta, T., Horvath, P., Horns, D., Hörandel, J., Horan, D., Holder, J., Hofmann, W., Hnatyk, B., Hinton, J., Hermann, G., Helo, J., Heller, M., Hayashida, M., Hayashi, K., Hassan, T., Hardcastle, M., Hara, S., Hadasch, D., Gunji, S., Griffiths, S., Greenshaw, T., Green, A., Granot, J., Grandi, P., Graham, J., Götz, D., González, J., González, M., Gómez-Vargas, G., Goldoni, P., Godinovic, N., Gnatyk, R., Glicenstein, J., Giuliani, A., Giroletti, M., Giro, E., Giordano, F., Giommi, P., Giglietto, N., Giavitto, G., Gerard, L., Gaug, M., Gasparetto, T., Gaskins, J., Garczarczyk, M., López, R., Garcia, B., Gallant, Y., Gadola, A., Gabici, S., Füßling, M., Funk, S., Fukazawa, Y., Fujita, Y., Fruck, C., Coromina, L., Fortson, L., Fornasa, M., Fontaine, G., Fioretti, V., Filipovic, M., Fesquet, M., Ferrand, G., Fernández-Barral, A., Fernandez-Alonso, M., Fegan, S., Fedorova, E., Fasola, G., Farnier, C., Falcone, A., Falceta-Goncalves, D., Fairbairn, M., Evoli, C., Espinoza, C., Ernenwein, J., Elsässer, D., Ekoume, T., Einecke, S., Egberts, K., Eckner, C., Ebr, J., Dwarkadas, V., Dubus, G., Dravins, D., Drass, H., Doro, M., Dorner, D., Prester, D., Domínguez, A., Djannati-Ataï, A., Diebold, S., Dib, C., Díaz, C., Di Venere, L., Di Pierro, F., Di Girolamo, T., Della Volpe, D., Delgado, C., Del Santo, M., Deil, C., Covino, S., Cotter, G., Costantini, H., Costa, A., Cortina, J., Contreras, J., Conrad, J., Connaughton, V., Conforti, V., Colin, P., Colafrancesco, S., Coco, V., Cieślar, M., Chudoba, J., Christov, A., Chikawa, M., Chernyakova, M., Chen, X., Chen, A., Chaty, S., Chadwick, P., Cerruti, M., Cauz, D., Catalano, O., Catalani, F., Casanova, S., Carr, J., Carquín, E., Carosi, R., Carlile, C., Cárdenas, V., Caraveo, P., Caproni, A., Capitanio, F., Capalbi, M., Canestrari, R., Busetto, G., Burtovoi, A., Burton, M., Bulik, T., Bulgarelli, A., Bühler, R., Bugaev, V., Buckley, J., Buanes, T., Brunetti, G., Brun, P., Brill, A., Bregeon, J., Braiding, C., Böttcher, M., Bosnjak, Z., Bonnoli, G., Bonavolontà, C., Bonardi, A., Bonanno, G., Bolmont, J., Boisson, C., Blazek, J., Blanch, O., Biteau, J., Bissaldi, E., Biland, A., Bigongiari, C., Biasuzzi, B., Bertucci, B., Bernlöhr, K., Bernardos, M., Bernardini, E., Berge, D., Benbow, W., Belfiore, A., Becherini, Y., Bastieri, D., Barkov, M., Bamba, A., Ballet, J., Ballester, O., Balbo, M., Balazs, C., Backes, M., Ashley, M., Paoletti, R., Palatka, M., Palatiello, M., Paizis, A., Padovani, M., Oya, I., Otte, N., Ostrowski, M., Osborne, J., Orito, R., Orienti, M., Ong, R., Okumura, A., Okazaki, N., Ohm, S., Ohishi, M., Ohira, Y., Oakes, L., OBrien, P., Nozaki, S., Novosyadlyj, B., Nosek, D., Noda, K., Nishijima, K., Nikołajuk, M., Nieto, D., Niemiec, J., Nakamura, Y., Nakamori, T., Asano, K., Arrabito, L., Arqueros, F., Armstrong, T., Araya, M., Aramo, C., Antolini, E., Ambrosi, G., Amato, E., Alispach, C., Alfaro, J., Alfaro, R., Agudo, I., Zhdanov, V.I., Zdziarski, A.A., Williams, D.A., Watson, J.J., Ward, J.E., Wagner, S.J., Vettolani, G.P., Varner, G.S., Torres, D.F., Todero Peixoto, C.J., Tejedor, L.A., Tavernet, J.-P., Supanitsky, A.D., Shellard, R.C., Rovero, A.C., Vázquez, J.J., Rezaeian, A.H., Parsons, R.D., Paredes, J.M., Osborne, J.P., Ong, R.A., De Souza, V., De Persio, F., De Palma, F., Wilhelmi, E., De Naurois, M., De Lucia, M., De Luca, A., De Lotto, B., Lopez, R., De La Calle, I., Pino, E., De Franco, A., De Cesare, G., Anjos, R., De Angelis, A., Dazzi, F., Dawson, B., Davids, I., Daniel, M., DUrso, D., DAvanzo, P., DAmmando, F., DAì, A., Cumani, P., Cuevas, O., Cuadra, J., Crocker, R., Minaya, I.A., Maccarone, M.C., Luque-Escamilla, P.L., Lenain, J.-P., De Oliveira M.A., Leigui, Lees, J.-P., Lang, R.G., Kukec Mezek, G., Kieda, D.B., Humensky, T.B., De Los Reyes Lopez, R., De Gouveia Dal Pino, E.M., Contreras, J.L., Chaves, R.C., Brown, A.M., Schioppa, E.J., Saturni, F.G., Bernardini, M.G., Barrio, J.A., Barres De Almeida, U., Antonelli, L.A., Amans, J.-P., Alves Batista, R., Al Samarai, I., Acharya, B.S., Helo, J.C., Hardcastle, M.J., Green, A.J., González, J.M., González, M.M., Glicenstein, J.-F., Ernenwein, J.-P., Ekoume, T.R., Dwarkadas, V.V., Dominis Prester, D., Chaves, R., Brown, A., Bernardini, M., Barrio, J., De Almeida, U., Antonelli, L., Amans, J., Batista, R., Samarai, I., Acharya, B., Consortium, The Cherenkov, Zorn, J., Ziegler, A., Zhdanov, V., Zechlin, H., Zech, A., Zdziarski, A., Zavrtanik, D., Zavrtanik, M., Zanin, R., Zandanel, F., Zampieri, L., Zaharijas, G., Zacharias, M., Yoshikoshi, T., Yoshiike, S., Yoshida, T., Yang, L., Yanagita, S., Yamazaki, R., Yamamoto, T., Wood, M., Wischnewski, R., Williams, D., Will, M., Wilcox, P., Wierzcholska, A., White, R., White, M., Werner, F., Watson, J., Warren, D., Ward, J., Walter, R., Wagner, R., Wagner, S., Vuillaume, T., Vrastil, M., Vorobiov, S., Vollhardt, A., Voelk, H., Villanueva, J., Vigorito, C., Viana, A., Vettolani, G., Verzi, V., Vergani, S., Veres, P., Vercellone, S., Vega, A., Vecchi, M., Acosta, M., Vassiliev, V., Vasileiadis, G., Varner, G., Vandenbroucke, J., Van Eldik, C., Cherenkov Telescope Array Consortium, The, Acharya, B. S., Agudo, I., Al Samarai, I., Alfaro, R., Alfaro, J., Alispach, C., Alves Batista, R., Amans, J. -P., Amato, E., Ambrosi, G., Antolini, E., Antonelli, L. A., Aramo, C., Araya, M., Armstrong, T., Arqueros, F., Arrabito, L., Asano, K., Ashley, M., Backes, M., Balazs, C., Balbo, M., Ballester, O., Ballet, J., Bamba, A., Barkov, M., Barres de Almeida, U., Barrio, J. A., Bastieri, D., Becherini, Y., Belfiore, A., Benbow, W., Berge, D., Bernardini, E., Bernardini, M. G., Bernardos, M., Bernlöhr, K., Bertucci, B., Biasuzzi, B., Bigongiari, C., Biland, A., Bissaldi, E., Biteau, J., Blanch, O., Blazek, J., Boisson, C., Bolmont, J., Bonanno, G., Bonardi, A., Bonavolontà, C., Bonnoli, G., Bosnjak, Z., Böttcher, M., Braiding, C., Bregeon, J., Brill, A., Brown, A. M., Brun, P., Brunetti, G., Buanes, T., Buckley, J., Bugaev, V., Bühler, R., Bulgarelli, A., Bulik, T., Burton, M., Burtovoi, A., Busetto, G., Canestrari, R., Capalbi, M., Capitanio, F., Caproni, A., Caraveo, P., Cárdenas, V., Carlile, C., Carosi, R., Carquín, E., Carr, J., Casanova, S., Cascone, E., Catalani, F., Catalano, O., Cauz, D., Cerruti, M., Chadwick, P., Chaty, S., Chaves, R. C. G., Chen, A., Chen, X., Chernyakova, M., Chikawa, M., Christov, A., Chudoba, J., Cieślar, M., Coco, V., Colafrancesco, S., Colin, P., Conforti, V., Connaughton, V., Conrad, J., Contreras, J. L., Cortina, J., Costa, A., Costantini, H., Cotter, G., Covino, S., Crocker, R., Cuadra, J., Cuevas, O., Cumani, P., D'Aì, A., D'Ammando, F., D'Avanzo, P., D'Urso, D., Daniel, M., Davids, I., Dawson, B., Dazzi, F., De Angelis, A., de Cássia dos Anjos, R., De Cesare, G., De Franco, A., de Gouveia Dal Pino, E. M., de la Calle, I., de los Reyes Lopez, R., De Lotto, B., De Luca, A., De Lucia, M., de Naurois, M., de Oña Wilhelmi, E., De Palma, F., De Persio, F., de Souza, V., Deil, C., Del Santo, M., Delgado, C., della Volpe, D., Di Girolamo, T., Di Pierro, F., Di Venere, L., Díaz, C., Dib, C., Diebold, S., Djannati-Ataï, A., Domínguez, A., Dominis Prester, D., Dorner, D., Doro, M., Drass, H., Dravins, D., Dubus, G., Dwarkadas, V. V., Ebr, J., Eckner, C., Egberts, K., Einecke, S., Ekoume, T. R. N., Elsässer, D., Ernenwein, J. -P., Espinoza, C., Evoli, C., Fairbairn, M., Falceta-Goncalves, D., Falcone, A., Farnier, C., Fasola, G., Fedorova, E., Fegan, S., Fernandez-Alonso, M., Fernández-Barral, A., Ferrand, G., Fesquet, M., Filipovic, M., Fioretti, V., Fontaine, G., Fornasa, M., Fortson, L., Freixas Coromina, L., Fruck, C., Fujita, Y., Fukazawa, Y., Funk, S., Füßling, M., Gabici, S., Gadola, A., Gallant, Y., Garcia, B., Garcia López, R., Garczarczyk, M., Gaskins, J., Gasparetto, T., Gaug, M., Gerard, L., Giavitto, G., Giglietto, N., Giommi, P., Giordano, F., Giro, E., Giroletti, M., Giuliani, A., Glicenstein, J. -F., Gnatyk, R., Godinovic, N., Goldoni, P., Gómez-Vargas, G., González, M. M., González, J. M., Götz, D., Graham, J., Grandi, P., Granot, J., Green, A. J., Greenshaw, T., Griffiths, S., Gunji, S., Hadasch, D., Hara, S., Hardcastle, M. J., Hassan, T., Hayashi, K., Hayashida, M., Heller, M., Helo, J. C., Hermann, G., Hinton, J., Hnatyk, B., Hofmann, W., Holder, J., Horan, D., Hörandel, J., Horns, D., Horvath, P., Hovatta, T., Hrabovsky, M., Hrupec, D., Humensky, T. B., Hütten, M., Iarlori, M., Inada, T., Inome, Y., Inoue, S., Inoue, T., Inoue, Y., Iocco, F., Ioka, K., Iori, M., Ishio, K., Iwamura, Y., Jamrozy, M., Janecek, P., Jankowsky, D., Jean, P., Jung-Richardt, I., Jurysek, J., Kaaret, P., Karkar, S., Katagiri, H., Katz, U., Kawanaka, N., Kazanas, D., Khélifi, B., Kieda, D. B., Kimeswenger, S., Kimura, S., Kisaka, S., Knapp, J., Knödlseder, J., Koch, B., Kohri, K., Komin, N., Kosack, K., Kraus, M., Krause, M., Krauß, F., Kubo, H., Kukec Mezek, G., Kuroda, H., Kushida, J., La Palombara, N., Lamanna, G., Lang, R. G., Lapington, J., Le Blanc, O., Leach, S., Lees, J. -P., Lefaucheur, J., Leigui de Oliveira, M. A., Lenain, J. -P., Lico, R., Limon, M., Lindfors, E., Lohse, T., Lombardi, S., Longo, F., López, M., López-Coto, R., Lu, C. -C., Lucarelli, F., Luque-Escamilla, P. L., Lyard, E., Maccarone, M. C., Maier, G., Majumdar, P., Malaguti, G., Mandat, D., Maneva, G., Manganaro, M., Mangano, S., Marcowith, A., Marín, J., Markoff, S., Martí, J., Martin, P., Martínez, M., Martínez, G., Masetti, N., Masuda, S., Maurin, G., Maxted, N., Mazin, D., Medina, C., Melandri, A., Mereghetti, S., Meyer, M., Minaya, I. A., Mirabal, N., Mirzoyan, R., Mitchell, A., Mizuno, T., Moderski, R., Mohammed, M., Mohrmann, L., Montaruli, T., Moralejo, A., Morcuende-Parrilla, D., Mori, K., Morlino, G., Morris, P., Morselli, A., Moulin, E., Mukherjee, R., Mundell, C., Murach, T., Muraishi, H., Murase, K., Nagai, A., Nagataki, S., Nagayoshi, T., Naito, T., Nakamori, T., Nakamura, Y., Niemiec, J., Nieto, D., Nikołajuk, M., Nishijima, K., Noda, K., Nosek, D., Novosyadlyj, B., Nozaki, S., O'Brien, P., Oakes, L., Ohira, Y., Ohishi, M., Ohm, S., Okazaki, N., Okumura, A., Ong, R. A., Orienti, M., Orito, R., Osborne, J. P., Ostrowski, M., Otte, N., Oya, I., Padovani, M., Paizis, A., Palatiello, M., Palatka, M., Paoletti, R., Paredes, J. M., Pareschi, G., Parsons, R. D., Pe'Er, A., Pech, M., Pedaletti, G., Perri, M., Persic, M., Petrashyk, A., Petrucci, P., Petruk, O., Peyaud, B., Pfeifer, M., Piano, G., Pisarski, A., Pita, S., Pohl, M., Polo, M., Pozo, D., Prandini, E., Prast, J., Principe, G., Prokhorov, D., Prokoph, H., Prouza, M., Pühlhofer, G., Punch, M., Pürckhauer, S., Queiroz, F., Quirrenbach, A., Rainò, S., Razzaque, S., Reimer, O., Reimer, A., Reisenegger, A., Renaud, M., Rezaeian, A. H., Rhode, W., Ribeiro, D., Ribó, M., Richtler, T., Rico, J., Rieger, F., Riquelme, M., Rivoire, S., Rizi, V., Rodriguez, J., Rodriguez Fernandez, G., Rodríguez Vázquez, J. J., Rojas, G., Romano, P., Romeo, G., Rosado, J., Rovero, A. C., Rowell, G., Rudak, B., Rugliancich, A., Rulten, C., Sadeh, I., Safi-Harb, S., Saito, T., Sakaki, N., Sakurai, S., Salina, G., Sánchez-Conde, M., Sandaker, H., Sandoval, A., Sangiorgi, P., Sanguillon, M., Sano, H., Santander, M., Sarkar, S., Satalecka, K., Saturni, F. G., Schioppa, E. J., Schlenstedt, S., Schneider, M., Schoorlemmer, H., Schovanek, P., Schulz, A., Schussler, F., Schwanke, U., Sciacca, E., Scuderi, S., Seitenzahl, I., Semikoz, D., Sergijenko, O., Servillat, M., Shalchi, A., Shellard, R. C., Sidoli, L., Siejkowski, H., Sillanpää, A., Sironi, G., Sitarek, J., Sliusar, V., Slowikowska, A., Sol, H., Stamerra, A., Stanič, S., Starling, R., Stawarz, Ł., Stefanik, S., Stephan, M., Stolarczyk, T., Stratta, G., Straumann, U., Suomijarvi, T., Supanitsky, A. D., Tagliaferri, G., Tajima, H., Tavani, M., Tavecchio, F., Tavernet, J. -P., Tayabaly, K., Tejedor, L. A., Temnikov, P., Terada, Y., Terrier, R., Terzic, T., Teshima, M., Testa, V., Thoudam, S., Tian, W., Tibaldo, L., Tluczykont, M., Todero Peixoto, C. J., Tokanai, F., Tomastik, J., Tonev, D., Tornikoski, M., Torres, D. F., Torresi, E., Tosti, G., Tothill, N., Tovmassian, G., Travnicek, P., Trichard, C., Trifoglio, M., Troyano Pujadas, I., Tsujimoto, S., Umana, G., Vagelli, V., Vagnetti, F., Valentino, M., Vallania, P., Valore, L., van Eldik, C., Vandenbroucke, J., Varner, G. S., Vasileiadis, G., Vassiliev, V., Vázquez Acosta, M., Vecchi, M., Vega, A., Vercellone, S., Veres, P., Vergani, S., Verzi, V., Vettolani, G. P., Viana, A., Vigorito, C., Villanueva, J., Voelk, H., Vollhardt, A., Vorobiov, S., Vrastil, M., Vuillaume, T., Wagner, S. J., Wagner, R., Walter, R., Ward, J. E., Warren, D., Watson, J. J., Werner, F., White, M., White, R., Wierzcholska, A., Wilcox, P., Will, M., Williams, D. A., Wischnewski, R., Wood, M., Yamamoto, T., Yamazaki, R., Yanagita, S., Yang, L., Yoshida, T., Yoshiike, S., Yoshikoshi, T., Zacharias, M., Zaharijas, G., Zampieri, L., Zandanel, F., Zanin, R., Zavrtanik, M., Zavrtanik, D., Zdziarski, A. A., Zech, A., Zechlin, H., Zhdanov, V. I., Ziegler, A., Zorn, J., 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 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), Département d'Astrophysique (ex SAP) (DAP), Institut de Recherches sur les lois Fondamentales de l'Univers (IRFU), 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, Institut de Physique Nucléaire d'Orsay (IPNO), Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Paris-Sud - Paris 11 (UP11), Laboratoire de Physique Nucléaire et de Hautes Énergies (LPNHE), Centre National de la Recherche Scientifique (CNRS)-Université Paris Diderot - Paris 7 (UPD7)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Pierre et Marie Curie - Paris 6 (UPMC), 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 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), AstroParticule et Cosmologie (APC (UMR_7164)), Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-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 de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3), Laboratoire de Physique Subatomique et de Cosmologie (LPSC), Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP )-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes [2016-2019] (UGA [2016-2019]), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay, Département de Physique des Particules (ex SPP) (DPP), 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), 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), CTA Consortium, Galaxies, Etoiles, Physique, Instrumentation (GEPI), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS), INAF - Osservatorio Astrofisico di Arcetri (OAA), Istituto Nazionale di Astrofisica (INAF), Istituto Nazionale di Fisica Nucleare, Sezione di Perugia (INFN, Sezione di Perugia), Istituto Nazionale di Fisica Nucleare (INFN), Departamento de Física Atómica, Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université de Montpellier (UM)-Centre National de la Recherche Scientifique (CNRS), College of Science and Engineering, Aoyama Gakuin University (AGU), Université Paris-Sud - Paris 11 (UP11)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Instituto de Fisica Corpuscular (IFIC), Consejo Superior de Investigaciones Científicas [Madrid] (CSIC)-Universitat de València (UV), 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), Laboratoire de Physique Nucléaire et de Hautes Énergies (LPNHE (UMR_7585)), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Paris Diderot - Paris 7 (UPD7)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Istituto di Radioastronomia [Bologna] (IRA), University of Naples Federico II = Università degli studi di Napoli Federico II, Max-Planck-Institut für Kernphysik (MPIK), Max-Planck-Gesellschaft, INAF - Osservatorio Astronomico di Padova (OAPD), 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), ISDC Data Centre for Astrophysics, Université de Genève = University of Geneva (UNIGE), Département de Physique Nucléaire et Corpusculaire [Genève] (DPNC), Universities Space Research Association (USRA), Universidad Complutense de Madrid = Complutense University of Madrid [Madrid] (UCM), INAF - Osservatorio Astronomico di Brera (OAB), Istituto di Astrofisica Spaziale e Fisica cosmica - Roma (IASF-Roma), Institut d'astrophysique spatiale (IAS), Université Paris-Sud - Paris 11 (UP11)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Centre National d’Études Spatiales [Paris] (CNES), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-École polytechnique (X)-Centre National de la Recherche Scientifique (CNRS), Dipartimento di Fı'sica Generale dell'Università, Istituto Nazionale di Fisica Nucleare, sezione di Bari (INFN, sezione di Bari), 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, Institut für Theoretische Physik und Astrophysik [Würzburg], Julius-Maximilians-Universität Würzburg (JMU), Jodrell Bank Centre for Astrophysics (JBCA), University of Manchester [Manchester], Institut des sciences du végétal (ISV), Centre National de la Recherche Scientifique (CNRS), Institut de Física d’Altes Energies [Barcelone] (IFAE), Universitat Autònoma de Barcelona (UAB), Agenzia Spaziale Italiana (ASI), APC - Astrophysique des Hautes Energies (APC - AHE), 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)-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)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS)-Alma Mater Studiorum Università di Bologna [Bologna] (UNIBO), Texas A&M University System, Istituto di Astrofisica Spaziale e Fisica cosmica - Bologna (IASF-Bo), Department of Natural Sciences [Ra'anana}, Open University of Israël, University of Hertfordshire [Hatfield] (UH), Deutsches Elektronen-Synchrotron [Zeuthen] (DESY), Helmholtz-Gemeinschaft = Helmholtz Association, Solar-Terrestrial Environment Laboratory [Nagoya] (STEL), Nagoya University, Laboratoire de l'Accélérateur Linéaire (LAL), Radboud University [Nijmegen], Metsähovi Radio Observatory, Aalto University, Humboldt University Of Berlin, The University of Tokyo (UTokyo), 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), Department of Physics and Astronomy [Iowa City], University of Iowa [Iowa City], Erlangen Centre for Astroparticle Physics (ECAP), Friedrich-Alexander Universität Erlangen-Nürnberg (FAU), Max-Planck-Institut für Extraterrestrische Physik (MPE), INAF- Milano, Università degli Studi di Udine - University of Udine [Italie], Dipartimento di Fisica [Roma La Sapienza], Università degli Studi di Roma 'La Sapienza' = Sapienza University [Rome] (UNIROMA), Astronomical Institute Anton Pannekoek (AI PANNEKOEK), University of Amsterdam [Amsterdam] (UvA), Istituto di Astrofisica Spaziale e Fisica Cosmica - Milano (IASF-MI), NASA Goddard Space Flight Center (GSFC), Institute for Physical Research (IPR), National Academy of Sciences of the Republic of Armenia [Yerevan] (NAS RA), Dept. of Physics, University of Wisconsin-Madison, Infrared Processing and Analysis Center (IPAC), California Institute of Technology (CALTECH), KEK (High energy accelerator research organization), Department of Physics [Tokyo], Tokyo Institure of Technology, Istituto di Radioastronomia INAF, Department of Physics and Astronomy [Leicester], University of Leicester, Departament d'Astronomia i Meteorologia [Barcelona] (DAM), Universitat de Barcelona (UB), IEEC-CSIC, INAF - Osservatorio Astronomico di Trieste (OAT), DLR Institut für Physik der Atmosphäre (IPA), Deutsches Zentrum für Luft- und Raumfahrt [Oberpfaffenhofen-Wessling] (DLR), Istituto di Astrofisica e Planetologia Spaziali - INAF (IAPS), Centro de Ciencias de la Atmosfera [Mexico], Universidad Nacional Autónoma de México = National Autonomous University of Mexico (UNAM), Technische Universität Dortmund [Dortmund] (TU), Institut de Ciencies del Cosmos (ICCUB), International Agency for Cancer Research (IACR), School of Chemistry and Physics, University of Adelaide, Copernicus Astronomical Center of the Polish Academy of Sciences (CAMK), Polish Academy of Sciences (PAN), Centro de Ciencias Aplicadas y Desarrollo Tecnológico, University of Oxford, AGH University of Science and Technology [Krakow, PL] (AGH UST), Dipartimento di Fisica 'Giuseppe Occhialini' = Department of Physics 'Giuseppe Occhialini' [Milano-Bicocca], Università degli Studi di Milano-Bicocca = University of Milano-Bicocca (UNIMIB), Département d'Astrophysique, de physique des Particules, de physique Nucléaire et de l'Instrumentation Associée (DAPNIA), Commissariat à l'énergie atomique et aux énergies alternatives (CEA), Department of Plant Sciences [Univ California Davis] (Plant - UC Davis), University of California [Davis] (UC Davis), University of California (UC)-University of California (UC), Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Institute for Climate and Atmospheric Science [Leeds] (ICAS), School of Earth and Environment [Leeds] (SEE), University of Leeds-University of Leeds, Antarctic Research a European Network for Astrophysics (ARENA), Institute of Atmospheric Physics [Prague] (IAP), Czech Academy of Sciences [Prague] (CAS), University of California (UC), Laboratoire d'études en Géophysique et océanographie spatiales (LEGOS), Instituto Nacional de Técnica Aeroespacial (INTA), Lawrence Berkeley National Laboratory [Berkeley] (LBNL), Istituto Nazionale di Fisica Nucleare, Sezione di Trieste (INFN, Sezione di Trieste), Jozef Stefan Institute [Ljubljana] (IJS), Istituto di Astrofisica Spaziale e Fisica cosmica - Palermo (IASF-Pa), Centre National de la Recherche Scientifique (CNRS)-Université Paris Diderot - Paris 7 (UPD7)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Institut national des sciences de l'Univers (INSU - CNRS), National Institute for Nuclear Physics (INFN), Université de Montpellier (UM)-Université Montpellier 2 - Sciences et Techniques (UM2)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Consejo Superior de Investigaciones Científicas [Spain] (CSIC)-Universitat de València (UV), University of Naples Federico II, Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Aix Marseille Université (AMU), Astrophysique Interprétation Modélisation (AIM (UMR_7158 / UMR_E_9005 / UM_112)), University of Geneva [Switzerland], Université de Genève (UNIGE), Complutense University of Madrid (UCM), Université Paris-Sud - Paris 11 (UP11)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Bureau d'Économie Théorique et Appliquée (BETA), Institut National de la Recherche Agronomique (INRA)-Université de Strasbourg (UNISTRA)-Université de Lorraine (UL)-Centre National de la Recherche Scientifique (CNRS), 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), Institut für Theoretische Physik und Astrophysik [Wurzburg], Julius-Maximilians-Universität Würzburg [Wurtzbourg, Allemagne] (JMU), Jodrell Bank Centre for Astrophysics, Universitat Autònoma de Barcelona [Barcelona] (UAB), 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)-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)-Dipartimento di Astronomia, Universita degli Studi di Bologna, Università di Bologna [Bologna] (UNIBO)-Università di Bologna [Bologna] (UNIBO), Helmholtz-Gemeinschaft, Radboud university [Nijmegen], Humboldt Universität zu Berlin, The University of Tokyo, Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS), Laboratoire d'Annecy de Physique des Particules (LAPP/Laboratoire d'Annecy-le-Vieux de Physique des Particules), PSL Research University (PSL)-PSL Research University (PSL)-Centre National de la Recherche Scientifique (CNRS), Department of Physics [Roma La Sapienza], Università degli Studi di Roma 'La Sapienza' [Rome], National Academy of Sciences of Armenia, CALTECH, Ctr Infrared Proc & Anal, Pasadena, CA 91125 USA, CALTECH, Ctr Infrared Proc & Anal, Pasadena, High Energy Accelerator Research Organization (KEK), University of Tsukuba, Universidad Nacional Autónoma de México (UNAM), University of Oxford [Oxford], Dip. di Fisica 'Occhialini' - Università degli Studi di Milano-Bicocca Piazza della Scienza, Department of Plant Sciences [Davis, CA], University of California-University of California, INAF-OAB, Czech Academy of Sciences [Prague] (ASCR), University of California, Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Centre National d'Études Spatiales [Toulouse] (CNES)-Observatoire Midi-Pyrénées (OMP), Observatoire de Paris - Site de Meudon (OBSPM), Institut de Planétologie et d'Astrophysique de Grenoble (IPAG), Centre National d'Études Spatiales [Toulouse] (CNES)-Observatoire des Sciences de l'Univers de Grenoble (OSUG ), Institut national des sciences de l'Univers (INSU - CNRS)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Institut National de Recherche pour l’Agriculture, l’Alimentation et l’Environnement (INRAE)-Université Grenoble Alpes (UGA)-Météo-France -Institut national des sciences de l'Univers (INSU - CNRS)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Institut National de Recherche pour l’Agriculture, l’Alimentation et l’Environnement (INRAE)-Université Grenoble Alpes (UGA)-Météo-France, Département de Physique des Particules (ex SPP) (DPhP), PSL Research University (PSL)-PSL Research University (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)-Centre National de la Recherche Scientifique (CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7), Université Joseph Fourier - Grenoble 1 (UJF)-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Institut Polytechnique de Grenoble - Grenoble Institute of Technology-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes (UGA), 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), 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)-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 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)-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 de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Dipartimento di Astronomia, Universita degli Studi di Bologna, Alma Mater Studiorum Università di Bologna [Bologna] (UNIBO)-Alma Mater Studiorum Università di Bologna [Bologna] (UNIBO), Humboldt-Universität zu Berlin, Università degli Studi di Roma 'La Sapienza' = Sapienza University [Rome], Università degli Studi di Milano-Bicocca [Milano] (UNIMIB), Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire Midi-Pyrénées (OMP), PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)-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, PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Dipartimento di Astronomia, Universita degli Studi di Bologna, 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, and Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)
- Subjects
propagation [photon] ,photon: propagation ,Cherenkov Telescope Array ,magnetic field ,01 natural sciences ,thermal ,Observatory ,formation [star] ,HESS ,site ,cluster ,ddc:522.6862 ,media_common ,pulsar ,High Energy Astrophysical Phenomena (astro-ph.HE) ,[SDU.ASTR.HE]Sciences of the Universe [physics]/Astrophysics [astro-ph]/High Energy Astrophysical Phenomena [astro-ph.HE] ,Astrophysics::Instrumentation and Methods for Astrophysics ,star: formation ,relativistic [jet] ,CERN LHC Coll ,binary [gamma ray] ,cosmic radiation [electron] ,axion-like particles ,violation ,Astrophysics - Instrumentation and Methods for Astrophysics ,Astrophysics - High Energy Astrophysical Phenomena ,performance ,Astrophysics and Astronomy ,bepress|Physical Sciences and Mathematics|Physics ,media_common.quotation_subject ,Astrophysics::High Energy Astrophysical Phenomena ,burst [gamma ray] ,Higgs particle ,invariance: Lorentz ,X-ray ,ionization ,supernova ,cosmic radiation: UHE ,Lorentz [invariance] ,AGN ,Instrumentation and Methods for Astrophysics (astro-ph.IM) ,CTA ,010308 nuclear & particles physics ,Astronomy ,sensitivity ,Universe ,angular resolution ,gamma ray: VHE ,quantum gravity ,galaxy ,[PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph] ,HAWC ,Computer science ,VHE [gamma ray] ,feedback ,High Energy Physics - Experiment ,High Energy Physics - Experiment (hep-ex) ,ultraviolet ,black hole ,[PHYS.HEXP]Physics [physics]/High Energy Physics - Experiment [hep-ex] ,cloud ,acceleration [hadron] ,neutron star ,010303 astronomy & astrophysics ,astro-ph.HE ,radio wave ,COSMIC cancer database ,imaging ,observatory ,Supernova ,annihilation ,bepress|Physical Sciences and Mathematics|Physics|Elementary Particles and Fields and String Theory ,infrared ,Particle Physics - Experiment ,accelerator ,WIMP ,Ground-based gamma-ray astronomy ,Dark matter ,UHE [cosmic radiation] ,FOS: Physical sciences ,gamma ray: burst ,GLAST ,dark matter ,jet: relativistic ,blazar ,target ,hadron: acceleration ,0103 physical sciences ,522.6862 ,[PHYS.PHYS.PHYS-INS-DET]Physics [physics]/Physics [physics]/Instrumentation and Detectors [physics.ins-det] ,TeV gamma-ray astronomy ,hep-ex ,Gravitational wave ,background ,gravitational radiation ,electron: cosmic radiation ,gamma ray: binary ,redshift ,[SDU.ASTR.IM]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Instrumentation and Methods for Astrophysic [astro-ph.IM] ,monitoring ,Sky ,bepress|Physical Sciences and Mathematics|Astrophysics and Astronomy ,astro-ph.IM - Abstract
Singapur : WORLD SCIENTIFIC, Cherenkov Telescope Array (CTA) 211 pp. (2017). doi:10.1142/10986, The Cherenkov Telescope Array, CTA, will be the major global observatory for very high energy gamma-ray astronomy over the next decade and beyond. The scientific potential of CTA is extremely broad: from understanding the role of relativistic cosmic particles to the search for dark matter. CTA is an explorer of the extreme universe, probing environments from the immediate neighbourhood of black holes to cosmic voids on the largest scales. Covering a huge range in photon energy from 20 GeV to 300 TeV, CTA will improve on all aspects of performance with respect to current instruments. The observatory will operate arrays on sites in both hemispheres to provide full sky coverage and will hence maximize the potential for the rarest phenomena such as very nearby supernovae, gamma-ray bursts or gravitational wave transients. With 99 telescopes on the southern site and 19 telescopes on the northern site, flexible operation will be possible, with sub-arrays available for specific tasks. CTA will have important synergies with many of the new generation of major astronomical and astroparticle observatories. Multi-wavelength and multi-messenger approaches combining CTA data with those from other instruments will lead to a deeper understanding of the broad-band non-thermal properties of target sources. The CTA Observatory will be operated as an open, proposal-driven observatory, with all data available on a public archive after a pre-defined proprietary period. Scientists from institutions worldwide have combined together to form the CTA Consortium. This Consortium has prepared a proposal for a Core Programme of highly motivated observations. The programme, encompassing approximately 40% of the available observing time over the first ten years of CTA operation, is made up of individual Key Science Projects (KSPs), which are presented in this document., Published by WORLD SCIENTIFIC, Singapur
39. The Transient High Energy Sky and Early Universe Surveyor (THESEUS)
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Amati, L., O Brien, P., Goetz, D., Bozzo, E., Tenzer, C., Frontera, F., Ghirlanda, G., Labanti, C., Osborne, J. P., Stratta, G., Tanvir, N., Willingale, R., Attina, P., Campana, R., Castro-Tirado, A. J., Contini, C., Fuschino, F., Gomboc, A., Hudec, R., Orleanski, P., Renotte, E., Rodic, T., Bagoly, Z., Blain, A., Callanan, P., Covino, S., Ferrara, A., Le Floch, E., Marisaldi, M., Mereghetti, S., Rosati, P., Vacchi, A., D Avanzo, P., Giommi, P., Piranomonte, S., Piro, L., Reglero, V., Rossi, A., Santangelo, A., Salvaterra, R., Tagliaferri, G., Vergani, S., Vinciguerra, S., Briggs, M., Campolongo, E., Ciolfi, R., Connaughton, V., Cordier, B., Morelli, B., Orlandini, M., Adami, C., Argan, A., Atteia, J. -L, Auricchio, N., Balazs, L., Baldazzi, G., Basa, S., Basak, R., Bellutti, P., Bernardini, M. G., Bertuccio, G., Braga, J., Branchesi, M., Brandt, S., Brocato, E., Budtz-Jorgensen, C., Bulgarelli, A., Burderi, L., Camp, J., Capozziello, S., Caruana, J., Casella, P., Cenko, B., Chardonnet, P., Ciardi, B., Colafrancesco, S., Dainotti, M. G., D Elia, V., Martino, D., Pasquale, M., Del Monte, E., Della Valle, M., Drago, A., Evangelista, Y., Feroci, M., Finelli, F., Fiorini, M., Fynbo, J., Gal-Yam, A., Gendre, B., Ghisellini, G., Grado, A., Guidorzi, C., Hafizi, M., Hanlon, L., Hjorth, J., Izzo, L., Kiss, L., Kumar, P., Kuvvetli, I., Lavagna, M., Li, T., Longo, F., Lyutikov, M., Maio, U., Maiorano, E., Malcovati, P., Malesani, D., Margutti, R., Martin-Carrillo, A., Masetti, N., Mcbreen, S., Mignani, R., Morgante, G., Mundell, C., Nargaard-Nielsen, H. U., Nicastro, L., Palazzi, E., Paltani, S., Panessa, F., Pareschi, G., Pe Er, A., Penacchioni, A. V., Pian, E., Piedipalumbo, E., Piran, T., Rauw, G., Razzano, M., Read, A., Rezzolla, L., Romano, P., Ruffini, R., Savaglio, S., Sguera, V., Schady, P., Skidmore, W., Song, L., Stanway, E., Starling, R., Topinka, M., Troja, E., Putten, M., Vanzella, E., Vercellone, S., Wilson-Hodge, C., Yonetoku, D., Zampa, G., Zampa, N., Zhang, B., Zhang, B. B., Zhang, S., Zhang, S. -N, Antonelli, A., Bianco, F., Boci, S., Boer, M., Botticella, M. T., Boulade, O., Butler, C., Campana, S., Capitanio, F., Celotti, A., Chen, Y., Colpi, M., Comastri, A., Cuby, J. -G, Dadina, M., Andrea De Luca, Dong, Y. -W, Ettori, S., Gandhi, P., Geza, E., Greiner, J., Guiriec, S., Harms, J., Hernanz, M., Hornstrup, A., Hutchinson, I., Israel, G., Jonker, P., Kaneko, Y., Kawai, N., Wiersema, K., Korpela, S., Lebrun, V., Lu, F., Macfadyen, A., Malaguti, G., Maraschi, L., Melandri, A., Modjaz, M., Morris, D., Omodei, N., Paizis, A., Pata, P., Petrosian, V., Rachevski, A., Rhoads, J., Ryde, F., Sabau-Graziati, L., Shigehiro, N., Sims, M., Soomin, J., Szecsi, D., Urata, Y., Uslenghi, M., Valenziano, L., Vianello, G., Vojtech, S., Watson, D., Zicha, J., and L. Amati, P. O’Brien, D. Goetz, E. Bozzo, C. Tenzer, F. Frontera, G. Ghirlanda, C. Labanti, J. P. Osborne, G. Stratta, N. Tanvir, R. Willingale , P. Attina, R. Campana, A.J. Castro-Tirado, C. Contini, F. Fuschino, A. Gomboc, R. Hudec, P. Orleanski, E. Renotte, T. Rodic, Z. Bagoly, A. Blain, P. Callanan, S. Covino, A. Ferrara, E. Le Floch, M. Marisaldi, S. Mereghetti, P. Rosati, A. Vacchi, P. D’Avanzo, P. Giommi, A. Gomboc, S. Piranomonte, L. Piro, V. Reglero, A. Rossi, A. Santangelo, R. Salvaterra, G. Tagliaferri, S. Vergani, S. Vinciguerra, M. Briggs, E. Campolongo, R. Ciolfi, V. Connaughton, B. Cordier, B. Morelli, M. Orlandini, C. Adami, A. Argan, J.-L. Atteia, N. Auricchio, L. Balazs, G. Baldazzi, S. Basa, R. Basak, P. Bellutti, M. G. Bernardini, G. Bertuccio, J. Braga, M. Branchesi, S. Brandt, E. Brocato, C. Budtz-Jorgensen, A. Bulgarelli, L. Burderi, J. Camp, S. Capozziello, J. Caruana, P. Casella, B. Cenko, P. Chardonnet, B. Ciardi, S. Colafrancesco, M. G. Dainotti, V. D’Elia, D. De Martino, M. De Pasquale, E. Del Monte, M. Della Valle, A. Drago, Y. Evangelista, M. Feroci, F. Finelli, M. Fiorini, J. Fynbo, A. Gal-Yam, B. Gendre, G. Ghisellini, A. Grado, C. Guidorzi, M. Hafizi, L. Hanlon, J. Hjorth, L. Izzo, L. Kiss, P. Kumar, I. Kuvvetli, M. Lavagna, T. Li, F. Longo, M. Lyutikov, U. Maio, E. Maiorano, P. Malcovati, D. Malesani, R. Margutti, A. Martin-Carrillo, N. Masetti, S. McBreen, R. Mignani, G. Morgante, C. Mundell, H. U. Nargaard-Nielsen, L. Nicastro, E. Palazzi, S. Paltani, F. Panessa, G. Pareschi, A. Pe’er, A. V. Penacchioni, E. Pian, E. Piedipalumbo, T. Piran, G. Rauw, M. Razzano, A. Read, L. Rezzolla, P. Romano, R. Ruffini, S. Savaglio, V. Sguera, P. Schady, W. Skidmore, L. Song, E. Stanway, R. Starling, M. Topinka, E. Troja, M. van Putten, E. Vanzella, S. Vercellone, C. Wilson-Hodge, D. Yonetoku, G. Zampa, N. Zampa, B. Zhang, B. B. Zhang, S. Zhang, S.-N. Zhang, A. Antonelli, F. Bianco, S. Boci, M. Boer, M. T. Botticella, O. Boulade, C. Butler, S. Campana, F. Capitanio, A. Celotti, Y. Chen, M. Colpi, A. Comastri, J.-G. Cuby, M. Dadina, A. De Luca, Y.-W. Dong, S. Ettori, P. Gandhi, E. Geza, J. Greiner, S. Guiriec, J. Harms, M. Hernanz, A. Hornstrup, I. Hutchinson, G. Israel, P. Jonker, Y. Kaneko, N. Kawai, K. Wiersema, S. Korpela, V. Lebrun, F. Lu, A. MacFadyen, G. Malaguti, L. Maraschi, A. Melandri, M. Modjaz, D. Morris, N. Omodei, A. Paizis, P. P´ata, V. Petrosian, A. Rachevski, J. Rhoads, F. Ryde, L. Sabau-Graziati, N. Shigehiro, M. Sims, J. Soomin, D. Szecsi, Y. Urata, M. Uslenghi, L. Valenziano, G. Vianello, S. Vojtech, D. Watson, J. Zicha
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Astrophysics::High Energy Astrophysical Phenomena ,Astrophysics::Instrumentation and Methods for Astrophysics ,Astrophysics::Cosmology and Extragalactic Astrophysics ,Gamma-ray bursts, Cosmology: observations, dark ages, re-ionization, first stars ,Astrophysics::Galaxy Astrophysics - Abstract
THESEUS is a space mission concept aimed at exploiting Gamma-Ray Bursts for investigating the early Universe and at providing a substantial advancement of multi-messenger and time-domain astrophysics. These goals will be achieved through a unique combination of instruments allowing GRBs and X-ray transients detection over a broad FOV (more than 1sr) with 0.5-1 arcmin localization, an energy band extending from several MeVs down to 0.3 keV and high sensitivity to transient sources in the soft X-ray domain, as well as on-board prompt (few minutes) follow-up with a 0.7 m class IR telescope with both imaging and spectroscopic capabilities. THESEUS will be perfectly suited for addressing the main open issues in cosmology such as, e.g., star formation rate and metallicity evolution of the inter-stellar and intra-galactic medium up to redshift ∼10, signatures of Pop III stars, sources and physics of re-ionization, and the faint end of the galaxy luminosity function. In addition, it will provide unprecedented capability to monitor the X-ray variable sky, thus detecting, localizing, and identifying the electromagnetic counterparts to sources of gravitational radiation, which may be routinely detected in the late '20s / early '30s by next generation facilities like aLIGO/ aVirgo, eLISA, KAGRA, and Einstein Telescope. THESEUS will also provide powerful synergies with the next generation of multi-wavelength observatories (e.g., LSST, ELT, SKA, CTA, ATHENA).
40. The management of the elderly with COPD in Italy. The OLD-COPD study | L'approcio all BPCO nel malato geriatrico in Italia. L'esperienza OLD-COPD
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Antonelli Incalzi, R., Corsonello, A., Masoti, G., Franco Rengo, Grassi, V., Bellia, V., Airoldi, G., Albo, E., Allegra, G., Andriolli, A., Arzilli, F., Ascione, G., Attardo Parrinello, G., Baldacchino, A., Baldasseroni, L., Ballini, E., Barassi, V., Bazzoni, P., Benintende, A., Bergamo, O., Bernardi, R., Bernardini, M., Bertoni, P., Bibbò, P., Buizza, M., Beatrice, G., Cancian, M., Cannaò, G., Caputo, A., Catanese, S., Cavatorta, A., Cendron, R., Chiarenza, S., Cibarelli, P., Cicala, R., Corrà, L., Cotrona, G., Cotroneo, A., Cottino, A., D Angelo, C., Alfieri, W., Del Greco, P., Della Rocca, G., D Ercole, M., Di Biase, A., Di Donato, W. S., Di Gennaro, L., Dionisia, P., Fabbri, G., Favretto, P., Ferrari, L., Fichera, U., Fiorio, L., Fracassi, L., Fradà, G., Frapiccini, A., Frattale, P., Galassi, L., Galimberti, V., Gallo, S., Gatto, P., Ghetti, A., Giordanetti, S., Giovane Sem, R., Guerrini, M., Gagliucci, A., Guizzardi, G., Gunelli, M., Iacomino, S., Ioli, G., Iraldi, G., Leo, N., Leonardi, R., Magris, D., Marchetto, P. E., Maresca, G., Martone, P., Mele Salerno, P., Miconi, R., Mussardo, V., Nalin, P., Nardelli, A., Nieddu, A., Orfei, S., Paternosto, D., Pedemonte, P., Pedone, V., Pedrazzoli, R., Pendenza, E., Pennacchietti, L., Piermattei, G., Piovesana, V., Pittaluga Pietro, A., Pizzoli, C., Podestà, F., Poli, N., Previdi, B., and Radice, L. G.
41. Relevance of Newtonian seismic noise for the VIRGO interferometer sensitivity
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Beccaria, M., Bernardini, M., Braccini, S., Bradaschia, C., Bozzi, A., Casciano, C., Cella, G., Ciampa, A., Cuoco, E., Curci, G., D Ambrosio, E., Dattilo, V., Carolis, G., Salvo, R., Angela Dora Vittoria Di Virgilio, Frasconi, F., Gaddi, A., Gennai, A., Gennaro, G., Giazotto, A., La Penna, P., Losurdo, G., Maggiore, M., Mancini, S., Palla, F., Pan, H. B., Paoletti, F., Pasqualetti, A., Passaquieti, R., Passuello, D., Poggiani, R., Popolizio, P., Raffaelli, F., Rapisarda, S., Vicere, A., and Zhang, Z.
42. The Compact Linear Collider (CLIC) - 2018 Summary Report
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CLICdp collaborations, The CLIC, Charles, T. K., Giansiracusa, P. J., Lucas, T. G., Rassool, R. P., Volpi, M., Balazs, C., Afanaciev, K., Makarenko, V., Patapenka, A., Zhuk, I., Collette, C., Boland, M. J., Hoffman, A. C. Abusleme, Diaz, M. A., Garay, F., Chi, Y., He, X., Pei, G., Pei, S., Shu, G., Wang, X., Zhang, J., Zhao, F., Zhou, Z., Chen, H., Gao, Y., Huang, W., Kuang, Y. P., Li, B., Li, Y., Meng, X., Shao, J., Shi, J., Tang, C., Wang, P., Wu, X., Zha, H., Ma, L., Han, Y., Fang, W., Gu, Q., Huang, D., Huang, X., Tan, J., Wang, Z., Zhao, Z., Uggerhøj, U. I., Wistisen, T. N., Aabloo, A., Aare, R., Kuppart, K., Vigonski, S., Zadin, V., Aicheler, M., Baibuz, E., Brücken, E., Djurabekova, F., Eerola, P., Garcia, F., Haeggström, E., Huitu, K., Jansson, V., Kassamakov, I., Kimari, J., Kyritsakis, A., Lehti, S., Meriläinen, A., Montonen, R., Nordlund, K., Österberg, K., Saressalo, A., Väinölä, J., Veske, M., Farabolini, W., Mollard, A., Peauger, F., Plouin, J., Bambade, P., Chaikovska, I., Chehab, R., Delerue, N., Davier, M., Faus-Golfe, A., Irles, A., Kaabi, W., LeDiberder, F., Pöschl, R., Zerwas, D., Aimard, B., Balik, G., J. -J. Blaising, Brunetti, L., Chefdeville, M., Dominjon, A., Drancourt, C., Geoffroy, N., Jacquemier, J., Jeremie, A., Karyotakis, Y., Nappa, J. M., Serluca, M., Vilalte, S., Vouters, G., Bernhard, A., Bründermann, E., Casalbuoni, S., Hillenbrand, S., Gethmann, J., Grau, A., Huttel, E., Müller, A.-S., Peiffer, P., Perić, I., Jauregui, D. Saez de, Emberger, L., Graf, C., Simon, F., Szalay, M., Kolk, N. van der, Brass, S., Kilian, W., Alexopoulos, T., Apostolopoulos, T., Gazis, E. N., Gazis, N., Kostopoulos, V., Kourkoulis, S., Heilig, B., Lichtenberger, J., Shrivastava, P., Dayyani, M. K., Ghasem, H., Hajari, S. S., Shaker, H., Ashkenazy, Y., Popov, I., Engelberg, E., Yashar, A., Abramowicz, H., Benhammou, Y., Borysov, O., Borysova, M., Levy, A., Levy, I., Alesini, D., Bellaveglia, M., Buonomo, B., Cardelli, A., Diomede, M., Ferrario, M., Gallo, A., Ghigo, A., Giribono, A., Piersanti, L., Stella, A., Vaccarezza, C., Blas, J. de, Franceschini, R., D’Auria, G., Mitri, S. Di, Abe, T., Aryshev, A., Fukuda, M., Furukawa, K., Hayano, H., Higashi, Y., Higo, T., Kubo, K., Kuroda, S., Matsumoto, S., Michizono, S., Naito, T., Okugi, T., Shidara, T., Tauchi, T., Terunuma, N., Urakawa, J., Yamamoto, A., Raboanary, R., Luiten, O. J., Stragier, X. F. D., Hart, R., Graaf, H. van der, Eigen, G., Adli, E., Lindstrøm, C. A., Lillestøl, R., Malina, L., Pfingstner, J., Sjobak, K. N., Ahmad, A., Hoorani, H., Khan, W. A., Bugiel, S., Bugiel, R., Firlej, M., Fiutowski, T. A., Idzik, M., Moroń, J., Świentek, K. P., Renstrom, P. Brückman de, Krupa, B., Kucharczyk, M., Lesiak, T., Pawlik, B., Sopicki, P., Turbiarz, B., Wojtoń, T., Zawiejski, L. K., Kalinowski, J., Nowak, K., Żarnecki, A. F., Firu, E., Ghenescu, V., Neagu, A. T., Preda, T., Zgura, I. S., Aloev, A., Azaryan, N., Boyko, I., Budagov, J., Chizhov, M., Filippova, M., Glagolev, V., Gongadze, A., Grigoryan, S., Gudkov, D., Karjavine, V., Lyablin, M., Nefedov, Yu, Olyunin, A., Rymbekova, A., Samochkine, A., Sapronov, A., Shelkov, G., Shirkov, G., Soldatov, V., Solodko, E., Trubnikov, G., Tyapkin, I., Uzhinsky, V., Vorozhtov, A., Zhemchugov, A., Levichev, E., Mezentsev, N., Piminov, P., Shatilov, D., Vobly, P., Zolotarev, K., Jelisavčić, I. Božović, Kačarević, G., Dumbelović, G. Milutinović, Pandurović, M., Radulović, M., Stevanović, J., Vukasinović, N., D. -H. Lee, Ayala, N., Benedetti, G., Guenzel, T., Iriso, U., Marti, Z., Perez, F., Pont, M., Trenado, J., Ruiz-Jimeno, A., Vila, I., Calero, J., Dominguez, M., Garcia-Tabares, L., Gavela, D., Lopez, D., Toral, F., Gutierrez, C. Blanch, Boronat, M., Esperante, D., Fullana, E., Fuster, J., García, I., Gimeno, B., Lopez, P. Gomis, González, D., Perelló, M., Ros, E., Villarejo, M. A., Vnuchenko, A., Vos, M., Borgmann, Ch, Brenner, R., Ekelöf, T., Jacewicz, M., Olvegård, M., Ruber, R., Ziemann, V., Aguglia, D., Gonzalvo, J. Alabau, Leon, M. Alcaide, Tehrani, N. Alipour, Anastasopoulos, M., Andersson, A., Andrianala, F., Antoniou, F., Apyan, A., Arominski, D., Artoos, K., Assly, S., Atieh, S., Baccigalupi, C., Sune, R. Ballabriga, Caballero, D. Banon, Barnes, M. J., Garcia, J. Barranco, Bartalesi, A., Bauche, J., Bayar, C., Belver-Aguilar, C., Morell, A. Benot, Bernardini, M., Bett, D. R., Bettoni, S., Bettencourt, M., Bielawski, B., Garcia, O. Blanco, Kraljevic, N. Blaskovic, Bolzon, B., Bonnin, X. A., Bozzini, D., Branger, E., Brondolin, E., Brunner, O., Buckland, M., Bursali, H., Burkhardt, H., Caiazza, D., Calatroni, S., Campbell, M., Lasheras, N. Catalan, Cassany, B., Castro, E., Soares, R. H. Cavaleiro, Bastos, M. Cerqueira, Cherif, A., Chevallay, E., Cilento, V., Corsini, R., Costa, R., Cure, B., Curt, S., Gobbo, A. Dal, Dannheim, D., Daskalaki, E., Deacon, L., Degiovanni, A., Michele, G. De, Oliveira, L. De, Romano, V. Del Pozo, Delahaye, J. P., Delikaris, D., Almeida, P. G. Dias de, Dobers, T., Doebert, S., Doytchinov, I., Draper, M., Ramos, F. Duarte, Duquenne, M., Plaja, N. Egidos, Elsener, K., Esberg, J., Esposito, M., Evans, L., Fedosseev, V., Ferracin, P., Fiergolski, A., Foraz, K., Fowler, A., Friebel, F., Fuchs, J.-F., Gaddi, A., Gamba, D., Fajardo, L. Garcia, Morales, H. Garcia, Garion, C., Gasior, M., Gatignon, L., Gayde, J.-C., Gerbershagen, A., Gerwig, H., Giambelli, G., Gilardi, A., Goldblatt, A. N., Anton, S. Gonzalez, Grefe, C., Grudiev, A., Guerin, H., Guillot-Vignot, F. G., Gutt-Mostowy, M. L., Lutz, M. Hein, Hessler, C., Holma, J. K., Holzer, E. B., Hourican, M., Hynds, D., Ikarios, E., Levinsen, Y. Inntjore, Janssens, S., Jeff, A., Jensen, E., Jonker, M., Kamugasa, S. W., Kastriotou, M., Kemppinen, J. M. K., Khan, V., Kieffer, R. B., Klempt, W., Kokkinis, N., Kossyvakis, I., Kostka, Z., Korsback, A., Platia, E. Koukovini, Kovermann, J. W., Kozsar, C.-I., Kremastiotis, I., Kröger, J., Kulis, S., Latina, A., Leaux, F., Lebrun, P., Lefevre, T., Leogrande, E., Linssen, L., Liu, X., Cudie, X. Llopart, Magnoni, S., Maidana, C., Maier, A. A., Durand, H. Mainaud, Mallows, S., Manosperti, E., Marelli, C., Lacoma, E. Marin, Marsh, S., Martin, R., Martini, I., Martyanov, M., Mazzoni, S., Mcmonagle, G., Mether, L. M., Meynier, C., Modena, M., Moilanen, A., Mondello, R., Cabral, P. B. Moniz, Irazabal, N. Mouriz, Munker, M., Muranaka, T., Nadenau, J., Navarro, J. G., Quirante, J. L. Navarro, Busto, E. Nebo Del, Nikiforou, N., Ninin, P., Nonis, M., Nisbet, D., Nuiry, F. X., Nürnberg, A., Ögren, J., Osborne, J., Ouniche, A. C., Pan, R., Papadopoulou, S., Papaphilippou, Y., Paraskaki, G., Pastushenko, A., Passarelli, A., Patecki, M., Pazdera, L., Pellegrini, D., Pepitone, K., Codina, E. Perez, Fontenla, A. Perez, Persson, T. H. B., Petrič, M., Pitman, S., Pitters, F., Pittet, S., Plassard, F., Popescu, D., Quast, T., Rajamak, R., Redford, S., Remandet, L., Renier, Y., Rey, S. F., Orozco, O. Rey, Riddone, G., Castro, E. Rodriguez, Roloff, P., Rossi, C., Rossi, F., Rude, V., Ruehl, I., Rumolo, G., Sailer, A., Sandomierski, J., Santin, E., Sanz, C., Bedolla, J. Sauza, Schnoor, U., Schmickler, H., Schulte, D., Senes, E., Serpico, C., Severino, G., Shipman, N., Sicking, E., Simoniello, R., Skowronski, P. K., Mompean, P. Sobrino, Soby, L., Sollander, P., Solodko, A., Sosin, M. P., Spannagel, S., Sroka, S., Stapnes, S., Sterbini, G., Stern, G., Ström, R., Stuart, M. J., Syratchev, I., Szypula, K., Tecker, F., Thonet, P. A., Thrane, P., Timeo, L., Tiirakari, M., Garcia, R. Tomas, Tomoiaga, C. I., Valerio, P., Vaňát, T., Vamvakas, A. L., Hoorne, J. Van, Viazlo, O., Pinto, M. Vicente Barreto, Vitoratou, N., Vlachakis, V., Weber, M. A., Wegner, R., Wendt, M., Widorski, M., Williams, O. E., Williams, M., Woolley, B., Wuensch, W., Wulzer, A., Uythoven, J., Xydou, A., Yang, R., Zelios, A., Zhao, Y., Zisopoulos, P., Benoit, M., Sultan, D. M. S., Riva, F., Bopp, M., Braun, H. H., Craievich, P., Dehler, M., Garvey, T., Pedrozzi, M., Raguin, J. Y., Rivkin, L., Zennaro, R., Guillaume, S., Rothacher, M., Aksoy, A., Nergiz, Z., Yavas, Ö., Denizli, H., Keskin, U., Oyulmaz, K. Y., Senol, A., Ciftci, A. K., Baturin, V., Karpenko, O., Kholodov, R., Lebed, O., Lebedynskyi, S., Mordyk, S., Musienko, I., Profatilova, Ia, Storizhko, V., Bosley, R. R., Price, T., Watson, M. F., Watson, N. K., Winter, A. G., Goldstein, J., Green, S., Marshall, J. S., Thomson, M. A., Xu, B., You, T., Gillespie, W. A., Spannowsky, M., Beggan, C., Martin, V., Zhang, Y., Protopopescu, D., Robson, A., Apsimon, R. J., Bailey, I., Burt, G. C., Dexter, A. C., Edwards, A. V., Hill, V., Jamison, S., Millar, W. L., Papke, K., Casse, G., Vossebeld, J., Aumeyr, T., Bergamaschi, M., Bobb, L., Bosco, A., Boogert, S., Boorman, G., Cullinan, F., Gibson, S., Karataev, P., Kruchinin, K., Lekomtsev, K., Lyapin, A., Nevay, L., Shields, W., Snuverink, J., Towler, J., Yamakawa, E., Boisvert, V., West, S., Jones, R., Joshi, N., Bett, D., Bodenstein, R. M., Bromwich, T., Burrows, P. N., Christian, G. B., Gohil, C., Korysko, P., Paszkiewicz, J., Perry, C., Ramjiawan, R., Roberts, J., Coates, T., Salvatore, F., Bainbridge, A., Clarke, J. A., Krumpa, N., Shepherd, B. J. A., Walsh, D., Chekanov, S., Demarteau, M., Gai, W., Liu, W., Metcalfe, J., Power, J., Repond, J., Weerts, H., Xia, L., Zupan, J., Wells, J. D., Zhang, Z., Adolphsen, C., Barklow, T., Dolgashev, V., Franzi, M., Graf, N., Hewett, J., Kemp, M., Kononenko, O., Markiewicz, T., Moffeit, K., Neilson, J., Nosochkov, Y., Oriunno, M., Phinney, N., Rizzo, T., Tantawi, S., Wang, J., Weatherford, B., White, G., and Woodley, M.
- Subjects
Technology ,Physics::Accelerator Physics ,High Energy Physics::Experiment ,ddc:600 ,Accelerators and Storage Rings ,physics.acc-ph - Abstract
The Compact Linear Collider (CLIC) is a TeV-scale high-luminosity linear $e^+e^−$ collider under development at CERN. Following the CLIC conceptual design published in 2012, this report provides an overview of the CLIC project, its current status, and future developments. It presents the CLIC physics potential and reports on design, technology, and implementation aspects of the accelerator and the detector. For an optimal exploitation of its physics potential, CLIC is foreseen to be built and operated in stages, at centre-of-mass energies of 380 GeV, 1.5 TeV and 3 TeV, respectively, for a site length ranging from 11 km to 50 km. CLIC uses a two-beam acceleration scheme, in which normal-conducting high-gradient 12 GHz accelerating structures are powered via a high-current drive beam. For the first stage, an alternative with X-band klystron powering is also considered. CLIC accelerator optimisation, technical developments and system tests have resulted in significant progress in recent years. Moreover, this has led to an increased energy efficiency (power around 170 MW) for the 380 GeV stage, together with a reduced cost estimate at the level of 6 billion CHF. The detector concept, which matches the physics performance requirements and the CLIC experimental conditions, has been refined using improved software tools for simulation and reconstruction. Significant progress has been made on detector technology developments for the tracking and calorimetry systems. A wide range of CLIC physics studies has been conducted, both through full detector simulations with overlay of beam-induced backgrounds, and through parametric studies, together providing a broad overview of the CLIC physics potential. Each of the three energy stages adds cornerstones of the full CLIC physics programme, such as Higgs width and couplings, top-quark properties, Higgs self-coupling, direct searches, and many precision electroweak measurements. The interpretation of the combined results gives crucial and accurate insight into new physics, largely complementary to LHC and HL-LHC. The construction of the first CLIC energy stage could start by 2026. First beams would be available by 2035, marking the beginning of a broad CLIC physics programme spanning 25–30 years. The Compact Linear Collider (CLIC) is a TeV-scale high-luminosity linear $e^+e^−$ collider under development at CERN. Following the CLIC conceptual design published in 2012, this report provides an overview of the CLIC project, its current status, and future developments. It presents the CLIC physics potential and reports on design, technology, and implementation aspects of the accelerator and the detector. For an optimal exploitation of its physics potential, CLIC is foreseen to be built and operated in stages, at centre-of-mass energies of 380 GeV, 1.5 TeV and 3 TeV, respectively, for a site length ranging from 11 km to 50 km. CLIC uses a two-beam acceleration scheme, in which normal-conducting high-gradient 12 GHz accelerating structures are powered via a high-current drive beam. For the first stage, an alternative with X-band klystron powering is also considered. CLIC accelerator optimisation, technical developments and system tests have resulted in significant progress in recent years. Moreover, this has led to an increased energy efficiency (power around 170 MW) for the 380 GeV stage, together with a reduced cost estimate at the level of 6 billion CHF. The detector concept, which matches the physics performance requirements and the CLIC experimental conditions, has been refined using improved software tools for simulation and reconstruction. Significant progress has been made on detector technology developments for the tracking and calorimetry systems. A wide range of CLIC physics studies has been conducted, both through full detector simulations with overlay of beam-induced backgrounds, and through parametric studies, together providing a broad overview of the CLIC physics potential. Each of the three energy stages adds cornerstones of the full CLIC physics programme, such as Higgs width and couplings, top-quark properties, Higgs self-coupling, direct searches, and many precision electroweak measurements. The interpretation of the combined results gives crucial and accurate insight into new physics, largely complementary to LHC and HL-LHC. The construction of the first CLIC energy stage could start by 2026. First beams would be available by 2035, marking the beginning of a broad CLIC physics programme spanning 25–30 years. The Compact Linear Collider (CLIC) is a TeV-scale high-luminosity linear $e^+e^−$ collider under development at CERN. Following the CLIC conceptual design published in 2012, this report provides an overview of the CLIC project, its current status, and future developments. It presents the CLIC physics potential and reports on design, technology, and implementation aspects of the accelerator and the detector. For an optimal exploitation of its physics potential, CLIC is foreseen to be built and operated in stages, at centre-of-mass energies of 380 GeV, 1.5 TeV and 3 TeV, respectively, for a site length ranging from 11 km to 50 km. CLIC uses a two-beam acceleration scheme, in which normal-conducting high-gradient 12 GHz accelerating structures are powered via a high-current drive beam. For the first stage, an alternative with X-band klystron powering is also considered. CLIC accelerator optimisation, technical developments and system tests have resulted in significant progress in recent years. Moreover, this has led to an increased energy efficiency (power around 170 MW) for the 380 GeV stage, together with a reduced cost estimate at the level of 6 billion CHF. The detector concept, which matches the physics performance requirements and the CLIC experimental conditions, has been refined using improved software tools for simulation and reconstruction. Significant progress has been made on detector technology developments for the tracking and calorimetry systems. A wide range of CLIC physics studies has been conducted, both through full detector simulations with overlay of beam-induced backgrounds, and through parametric studies, together providing a broad overview of the CLIC physics potential. Each of the three energy stages adds cornerstones of the full CLIC physics programme, such as Higgs width and couplings, top-quark properties, Higgs self-coupling, direct searches, and many precision electroweak measurements. The interpretation of the combined results gives crucial and accurate insight into new physics, largely complementary to LHC and HL-LHC. The construction of the first CLIC energy stage could start by 2026. First beams would be available by 2035, marking the beginning of a broad CLIC physics programme spanning 25–30 years. The Compact Linear Collider (CLIC) is a TeV-scale high-luminosity linear $e^+e^−$ collider under development at CERN. Following the CLIC conceptual design published in 2012, this report provides an overview of the CLIC project, its current status, and future developments. It presents the CLIC physics potential and reports on design, technology, and implementation aspects of the accelerator and the detector. For an optimal exploitation of its physics potential, CLIC is foreseen to be built and operated in stages, at centre-of-mass energies of 380 GeV, 1.5 TeV and 3 TeV, respectively, for a site length ranging from 11 km to 50 km. CLIC uses a two-beam acceleration scheme, in which normal-conducting high-gradient 12 GHz accelerating structures are powered via a high-current drive beam. For the first stage, an alternative with X-band klystron powering is also considered. CLIC accelerator optimisation, technical developments and system tests have resulted in significant progress in recent years. Moreover, this has led to an increased energy efficiency (power around 170 MW) for the 380 GeV stage, together with a reduced cost estimate at the level of 6 billion CHF. The detector concept, which matches the physics performance requirements and the CLIC experimental conditions, has been refined using improved software tools for simulation and reconstruction. Significant progress has been made on detector technology developments for the tracking and calorimetry systems. A wide range of CLIC physics studies has been conducted, both through full detector simulations with overlay of beam-induced backgrounds, and through parametric studies, together providing a broad overview of the CLIC physics potential. Each of the three energy stages adds cornerstones of the full CLIC physics programme, such as Higgs width and couplings, top-quark properties, Higgs self-coupling, direct searches, and many precision electroweak measurements. The interpretation of the combined results gives crucial and accurate insight into new physics, largely complementary to LHC and HL-LHC. The construction of the first CLIC energy stage could start by 2026. First beams would be available by 2035, marking the beginning of a broad CLIC physics programme spanning 25–30 years. The Compact Linear Collider (CLIC) is a TeV-scale high-luminosity linear $e^+e^−$ collider under development at CERN. Following the CLIC conceptual design published in 2012, this report provides an overview of the CLIC project, its current status, and future developments. It presents the CLIC physics potential and reports on design, technology, and implementation aspects of the accelerator and the detector. For an optimal exploitation of its physics potential, CLIC is foreseen to be built and operated in stages, at centre-of-mass energies of 380 GeV, 1.5 TeV and 3 TeV, respectively, for a site length ranging from 11 km to 50 km. CLIC uses a two-beam acceleration scheme, in which normal-conducting high-gradient 12 GHz accelerating structures are powered via a high-current drive beam. For the first stage, an alternative with X-band klystron powering is also considered. CLIC accelerator optimisation, technical developments and system tests have resulted in significant progress in recent years. Moreover, this has led to an increased energy efficiency (power around 170 MW) for the 380 GeV stage, together with a reduced cost estimate at the level of 6 billion CHF. The detector concept, which matches the physics performance requirements and the CLIC experimental conditions, has been refined using improved software tools for simulation and reconstruction. Significant progress has been made on detector technology developments for the tracking and calorimetry systems. A wide range of CLIC physics studies has been conducted, both through full detector simulations with overlay of beam-induced backgrounds, and through parametric studies, together providing a broad overview of the CLIC physics potential. Each of the three energy stages adds cornerstones of the full CLIC physics programme, such as Higgs width and couplings, top-quark properties, Higgs self-coupling, direct searches, and many precision electroweak measurements. The interpretation of the combined results gives crucial and accurate insight into new physics, largely complementary to LHC and HL-LHC. The construction of the first CLIC energy stage could start by 2026. First beams would be available by 2035, marking the beginning of a broad CLIC physics programme spanning 25–30 years. The Compact Linear Collider (CLIC) is a TeV-scale high-luminosity linear $e^+e^−$ collider under development at CERN. Following the CLIC conceptual design published in 2012, this report provides an overview of the CLIC project, its current status, and future developments. It presents the CLIC physics potential and reports on design, technology, and implementation aspects of the accelerator and the detector. For an optimal exploitation of its physics potential, CLIC is foreseen to be built and operated in stages, at centre-of-mass energies of 380 GeV, 1.5 TeV and 3 TeV, respectively, for a site length ranging from 11 km to 50 km. CLIC uses a two-beam acceleration scheme, in which normal-conducting high-gradient 12 GHz accelerating structures are powered via a high-current drive beam. For the first stage, an alternative with X-band klystron powering is also considered. CLIC accelerator optimisation, technical developments and system tests have resulted in significant progress in recent years. Moreover, this has led to an increased energy efficiency (power around 170 MW) for the 380 GeV stage, together with a reduced cost estimate at the level of 6 billion CHF. The detector concept, which matches the physics performance requirements and the CLIC experimental conditions, has been refined using improved software tools for simulation and reconstruction. Significant progress has been made on detector technology developments for the tracking and calorimetry systems. A wide range of CLIC physics studies has been conducted, both through full detector simulations with overlay of beam-induced backgrounds, and through parametric studies, together providing a broad overview of the CLIC physics potential. Each of the three energy stages adds cornerstones of the full CLIC physics programme, such as Higgs width and couplings, top-quark properties, Higgs self-coupling, direct searches, and many precision electroweak measurements. The interpretation of the combined results gives crucial and accurate insight into new physics, largely complementary to LHC and HL-LHC. The construction of the first CLIC energy stage could start by 2026. First beams would be available by 2035, marking the beginning of a broad CLIC physics programme spanning 25–30 years. The Compact Linear Collider (CLIC) is a TeV-scale high-luminosity linear $e^+e^−$ collider under development at CERN. Following the CLIC conceptual design published in 2012, this report provides an overview of the CLIC project, its current status, and future developments. It presents the CLIC physics potential and reports on design, technology, and implementation aspects of the accelerator and the detector. For an optimal exploitation of its physics potential, CLIC is foreseen to be built and operated in stages, at centre-of-mass energies of 380 GeV, 1.5 TeV and 3 TeV, respectively, for a site length ranging from 11 km to 50 km. CLIC uses a two-beam acceleration scheme, in which normal-conducting high-gradient 12 GHz accelerating structures are powered via a high-current drive beam. For the first stage, an alternative with X-band klystron powering is also considered. CLIC accelerator optimisation, technical developments and system tests have resulted in significant progress in recent years. Moreover, this has led to an increased energy efficiency (power around 170 MW) for the 380 GeV stage, together with a reduced cost estimate at the level of 6 billion CHF. The detector concept, which matches the physics performance requirements and the CLIC experimental conditions, has been refined using improved software tools for simulation and reconstruction. Significant progress has been made on detector technology developments for the tracking and calorimetry systems. A wide range of CLIC physics studies has been conducted, both through full detector simulations with overlay of beam-induced backgrounds, and through parametric studies, together providing a broad overview of the CLIC physics potential. Each of the three energy stages adds cornerstones of the full CLIC physics programme, such as Higgs width and couplings, top-quark properties, Higgs self-coupling, direct searches, and many precision electroweak measurements. The interpretation of the combined results gives crucial and accurate insight into new physics, largely complementary to LHC and HL-LHC. The construction of the first CLIC energy stage could start by 2026. First beams would be available by 2035, marking the beginning of a broad CLIC physics programme spanning 25–30 years. The Compact Linear Collider (CLIC) is a TeV-scale high-luminosity linear $e^+e^−$ collider under development at CERN. Following the CLIC conceptual design published in 2012, this report provides an overview of the CLIC project, its current status, and future developments. It presents the CLIC physics potential and reports on design, technology, and implementation aspects of the accelerator and the detector. For an optimal exploitation of its physics potential, CLIC is foreseen to be built and operated in stages, at centre-of-mass energies of 380 GeV, 1.5 TeV and 3 TeV, respectively, for a site length ranging from 11 km to 50 km. CLIC uses a two-beam acceleration scheme, in which normal-conducting high-gradient 12 GHz accelerating structures are powered via a high-current drive beam. For the first stage, an alternative with X-band klystron powering is also considered. CLIC accelerator optimisation, technical developments and system tests have resulted in significant progress in recent years. Moreover, this has led to an increased energy efficiency (power around 170 MW) for the 380 GeV stage, together with a reduced cost estimate at the level of 6 billion CHF. The detector concept, which matches the physics performance requirements and the CLIC experimental conditions, has been refined using improved software tools for simulation and reconstruction. Significant progress has been made on detector technology developments for the tracking and calorimetry systems. A wide range of CLIC physics studies has been conducted, both through full detector simulations with overlay of beam-induced backgrounds, and through parametric studies, together providing a broad overview of the CLIC physics potential. Each of the three energy stages adds cornerstones of the full CLIC physics programme, such as Higgs width and couplings, top-quark properties, Higgs self-coupling, direct searches, and many precision electroweak measurements. The interpretation of the combined results gives crucial and accurate insight into new physics, largely complementary to LHC and HL-LHC. The construction of the first CLIC energy stage could start by 2026. First beams would be available by 2035, marking the beginning of a broad CLIC physics programme spanning 25–30 years. The Compact Linear Collider (CLIC) is a TeV-scale high-luminosity linear $e^+e^−$ collider under development at CERN. Following the CLIC conceptual design published in 2012, this report provides an overview of the CLIC project, its current status, and future developments. It presents the CLIC physics potential and reports on design, technology, and implementation aspects of the accelerator and the detector. For an optimal exploitation of its physics potential, CLIC is foreseen to be built and operated in stages, at centre-of-mass energies of 380 GeV, 1.5 TeV and 3 TeV, respectively, for a site length ranging from 11 km to 50 km. CLIC uses a two-beam acceleration scheme, in which normal-conducting high-gradient 12 GHz accelerating structures are powered via a high-current drive beam. For the first stage, an alternative with X-band klystron powering is also considered. CLIC accelerator optimisation, technical developments and system tests have resulted in significant progress in recent years. Moreover, this has led to an increased energy efficiency (power around 170 MW) for the 380 GeV stage, together with a reduced cost estimate at the level of 6 billion CHF. The detector concept, which matches the physics performance requirements and the CLIC experimental conditions, has been refined using improved software tools for simulation and reconstruction. Significant progress has been made on detector technology developments for the tracking and calorimetry systems. A wide range of CLIC physics studies has been conducted, both through full detector simulations with overlay of beam-induced backgrounds, and through parametric studies, together providing a broad overview of the CLIC physics potential. Each of the three energy stages adds cornerstones of the full CLIC physics programme, such as Higgs width and couplings, top-quark properties, Higgs self-coupling, direct searches, and many precision electroweak measurements. The interpretation of the combined results gives crucial and accurate insight into new physics, largely complementary to LHC and HL-LHC. The construction of the first CLIC energy stage could start by 2026. First beams would be available by 2035, marking the beginning of a broad CLIC physics programme spanning 25–30 years. The Compact Linear Collider (CLIC) is a TeV-scale high-luminosity linear $e^+e^−$ collider under development at CERN. Following the CLIC conceptual design published in 2012, this report provides an overview of the CLIC project, its current status, and future developments. It presents the CLIC physics potential and reports on design, technology, and implementation aspects of the accelerator and the detector. For an optimal exploitation of its physics potential, CLIC is foreseen to be built and operated in stages, at centre-of-mass energies of 380 GeV, 1.5 TeV and 3 TeV, respectively, for a site length ranging from 11 km to 50 km. CLIC uses a two-beam acceleration scheme, in which normal-conducting high-gradient 12 GHz accelerating structures are powered via a high-current drive beam. For the first stage, an alternative with X-band klystron powering is also considered. CLIC accelerator optimisation, technical developments and system tests have resulted in significant progress in recent years. Moreover, this has led to an increased energy efficiency (power around 170 MW) for the 380 GeV stage, together with a reduced cost estimate at the level of 6 billion CHF. The detector concept, which matches the physics performance requirements and the CLIC experimental conditions, has been refined using improv The Compact Linear Collider (CLIC) is a TeV-scale high-luminosity linear $e^+e^−$ collider under development at CERN. Following the CLIC conceptual design published in 2012, this report provides an overview of the CLIC project, its current status, and future developments. It presents the CLIC physics potential and reports on design, technology, and implementation aspects of the accelerator and the detector. For an optimal exploitation of its physics potential, CLIC is foreseen to be built and operated in stages, at centre-of-mass energies of 380 GeV, 1.5 TeV and 3 TeV, respectively, for a site length ranging from 11 km to 50 km. CLIC uses a two-beam acceleration scheme, in which normal-conducting high-gradient 12 GHz accelerating structures are powered via a high-current drive beam. For the first stage, an alternative with X-band klystron powering is also considered. CLIC accelerator optimisation, technical developments and system tests have resulted in significant progress in recent years. Moreover, this has led to an increased energy efficiency (power around 170 MW) for the 380 GeV stage, together with a reduced cost estimate at the level of 6 billion CHF. The detector concept, which matches the physics performance requirements and the CLIC experimental conditions, has been refined using improv The Compact Linear Collider (CLIC) is a TeV-scale high-luminosity linear $e^+e^−$ collider under development at CERN. Following the CLIC conceptual design published in 2012, this report provides an overview of the CLIC project, its current status, and future developments. It presents the CLIC physics potential and reports on design, technology, and implementation aspects of the accelerator and the detector. For an optimal exploitation of its physics potential, CLIC is foreseen to be built and operated in stages, at centre-of-mass energies of 380 GeV, 1.5 TeV and 3 TeV, respectively, for a site length ranging from 11 km to 50 km. CLIC uses a two-beam acceleration scheme, in which normal-conducting high-gradient 12 GHz accelerating structures are powered via a high-current drive beam. For the first stage, an alternative with X-band klystron powering is also considered. CLIC accelerator optimisation, technical developments and system tests have resulted in significant progress in recent years. Moreover, this has led to an increased energy efficiency (power around 170 MW) for the 380 GeV stage, together with a reduced cost estimate at the level of 6 billion CHF. The detector concept, which matches the physics performance requirements and the CLIC experimental conditions, has been refined using improv The Compact Linear Collider (CLIC) is a TeV-scale high-luminosity linear $e^+e^−$ collider under development at CERN. Following the CLIC conceptual design published in 2012, this report provides an overview of the CLIC project, its current status, and future developments. It presents the CLIC physics potential and reports on design, technology, and implementation aspects of the accelerator and the detector. For an optimal exploitation of its physics potential, CLIC is foreseen to be built and operated in stages, at centre-of-mass energies of 380 GeV, 1.5 TeV and 3 TeV, respectively, for a site length ranging from 11 km to 50 km. CLIC uses a two-beam acceleration scheme, in which normal-conducting high-gradient 12 GHz accelerating structures are powered via a high-current drive beam. For the first stage, an alternative with X-band klystron powering is also considered. CLIC accelerator optimisation, technical developments and system tests have resulted in significant progress in recent years. Moreover, this has led to an increased energy efficiency (power around 170 MW) for the 380 GeV stage, together with a reduced cost estimate at the level of 6 billion CHF. The detector concept, which matches the physics performance requirements and the CLIC experimental conditions, has been refined using improv The Compact Linear Collider (CLIC) is a TeV-scale high-luminosity linear $e^+e^−$ collider under development at CERN. Following the CLIC conceptual design published in 2012, this report provides an overview of the CLIC project, its current status, and future developments. It presents the CLIC physics potential and reports on design, technology, and implementation aspects of the accelerator and the detector. For an optimal exploitation of its physics potential, CLIC is foreseen to be built and operated in stages, at centre-of-mass energies of 380 GeV, 1.5 TeV and 3 TeV, respectively, for a site length ranging from 11 km to 50 km. CLIC uses a two-beam acceleration scheme, in which normal-conducting high-gradient 12 GHz accelerating structures are powered via a high-current drive beam. For the first stage, an alternative with X-band klystron powering is also considered. CLIC accelerator optimisation, technical developments and system tests have resulted in significant progress in recent years. Moreover, this has led to an increased energy efficiency (power around 170 MW) for the 380 GeV stage, together with a reduced cost estimate at the level of 6 billion CHF. The detector concept, which matches the physics performance requirements and the CLIC experimental conditions, has been refined using improv The Compact Linear Collider (CLIC) is a TeV-scale high-luminosity linear $e^+e^−$ collider under development at CERN. Following the CLIC conceptual design published in 2012, this report provides an overview of the CLIC project, its current status, and future developments. It presents the CLIC physics potential and reports on design, technology, and implementation aspects of the accelerator and the detector. For an optimal exploitation of its physics potential, CLIC is foreseen to be built and operated in stages, at centre-of-mass energies of 380 GeV, 1.5 TeV and 3 TeV, respectively, for a site length ranging from 11 km to 50 km. CLIC uses a two-beam acceleration scheme, in which normal-conducting high-gradient 12 GHz accelerating structures are powered via a high-current drive beam. For the first stage, an alternative with X-band klystron powering is also considered. CLIC accelerator optimisation, technical developments and system tests have resulted in significant progress in recent years. Moreover, this has led to an increased energy efficiency (power around 170 MW) for the 380 GeV stage, together with a reduced cost estimate at the level of 6 billion CHF. The detector concept, which matches the physics performance requirements and the CLIC experimental conditions, has been refined using improv The Compact Linear Collider (CLIC) is a TeV-scale high-luminosity linear $e^+e^−$ collider under development at CERN. Following the CLIC conceptual design published in 2012, this report provides an overview of the CLIC project, its current status, and future developments. It presents the CLIC physics potential and reports on design, technology, and implementation aspects of the accelerator and the detector. For an optimal exploitation of its physics potential, CLIC is foreseen to be built and operated in stages, at centre-of-mass energies of 380 GeV, 1.5 TeV and 3 TeV, respectively, for a site length ranging from 11 km to 50 km. CLIC uses a two-beam acceleration scheme, in which normal-conducting high-gradient 12 GHz accelerating structures are powered via a high-current drive beam. For the first stage, an alternative with X-band klystron powering is also considered. CLIC accelerator optimisation, technical developments and system tests have resulted in significant progress in recent years. Moreover, this has led to an increased energy efficiency (power around 170 MW) for the 380 GeV stage, together with a reduced cost estimate at the level of 6 billion CHF. The detector concept, which matches the physics performance requirements and the CLIC experimental conditions, has been refined using improved software tools for simulation and reconstruction. Significant progress has been made on detector technology developments for the tracking and calorimetry systems. A wide range of CLIC physics studies has been conducted, both through full detector simulations with overlay of beam-induced backgrounds, and through parametric studies, together providing a broad overview of the CLIC physics potential. Each of the three energy stages adds cornerstones of the full CLIC physics programme, such as Higgs width and couplings, top-quark properties, Higgs self-coupling, direct searches, and many precision electroweak measurements. The interpretation of the combined results gives crucial and accurate insight into new physics, largely complementary to LHC and HL-LHC. The construction of the first CLIC energy stage could start by 2026. First beams would be available by 2035, marking the beginning of a broad CLIC physics programme spanning 25–30 years. The Compact Linear Collider (CLIC) is a TeV-scale high-luminosity linear $e^+e^−$ collider under development at CERN. Following the CLIC conceptual design published in 2012, this report provides an overview of the CLIC project, its current status, and future developments. It presents the CLIC physics potential and reports on design, technology, and implementation aspects of the accelerator and the detector. For an optimal exploitation of its physics potential, CLIC is foreseen to be built and operated in stages, at centre-of-mass energies of 380 GeV, 1.5 TeV and 3 TeV, respectively, for a site length ranging from 11 km to 50 km. CLIC uses a two-beam acceleration scheme, in which normal-conducting high-gradient 12 GHz accelerating structures are powered via a high-current drive beam. For the first stage, an alternative with X-band klystron powering is also considered. CLIC accelerator optimisation, technical developments and system tests have resulted in significant progress in recent years. Moreover, this has led to an increased energy efficiency (power around 170 MW) for the 380 GeV stage, together with a reduced cost estimate at the level of 6 billion CHF. The detector concept, which matches the physics performance requirements and the CLIC experimental conditions, has been refined using improved software tools for simulation and reconstruction. Significant progress has been made on detector technology developments for the tracking and calorimetry systems. A wide range of CLIC physics studies has been conducted, both through full detector simulations with overlay of beam-induced backgrounds, and through parametric studies, together providing a broad overview of the CLIC physics potential. Each of the three energy stages adds cornerstones of the full CLIC physics programme, such as Higgs width and couplings, top-quark properties, Higgs self-coupling, direct searches, and many precision electroweak measurements. The interpretation of the combined results gives crucial and accurate insight into new physics, largely complementary to LHC and HL-LHC. The construction of the first CLIC energy stage could start by 2026. First beams would be available by 2035, marking the beginning of a broad CLIC physics programme spanning 25–30 years. The Compact Linear Collider (CLIC) is a TeV-scale high-luminosity linear $e^+e^−$ collider under development at CERN. Following the CLIC conceptual design published in 2012, this report provides an overview of the CLIC project, its current status, and future developments. It presents the CLIC physics potential and reports on design, technology, and implementation aspects of the accelerator and the detector. For an optimal exploitation of its physics potential, CLIC is foreseen to be built and operated in stages, at centre-of-mass energies of 380 GeV, 1.5 TeV and 3 TeV, respectively, for a site length ranging from 11 km to 50 km. CLIC uses a two-beam acceleration scheme, in which normal-conducting high-gradient 12 GHz accelerating structures are powered via a high-current drive beam. For the first stage, an alternative with X-band klystron powering is also considered. CLIC accelerator optimisation, technical developments and system tests have resulted in significant progress in recent years. Moreover, this has led to an increased energy efficiency (power around 170 MW) for the 380 GeV stage, together with a reduced cost estimate at the level of 6 billion CHF. The detector concept, which matches the physics performance requirements and the CLIC experimental conditions, has been refined using improved software tools for simulation and reconstruction. Significant progress has been made on detector technology developments for the tracking and calorimetry systems. A wide range of CLIC physics studies has been conducted, both through full detector simulations with overlay of beam-induced backgrounds, and through parametric studies, together providing a broad overview of the CLIC physics potential. Each of the three energy stages adds cornerstones of the full CLIC physics programme, such as Higgs width and couplings, top-quark properties, Higgs self-coupling, direct searches, and many precision electroweak measurements. The interpretation of the combined results gives crucial and accurate insight into new physics, largely complementary to LHC and HL-LHC. The construction of the first CLIC energy stage could start by 2026. First beams would be available by 2035, marking the beginning of a broad CLIC physics programme spanning 25–30 years. The Compact Linear Collider (CLIC) is a TeV-scale high-luminosity linear $e^+e^−$ collider under development at CERN. Following the CLIC conceptual design published in 2012, this report provides an overview of the CLIC project, its current status, and future developments. It presents the CLIC physics potential and reports on design, technology, and implementation aspects of the accelerator and the detector. For an optimal exploitation of its physics potential, CLIC is foreseen to be built and operated in stages, at centre-of-mass energies of 380 GeV, 1.5 TeV and 3 TeV, respectively, for a site length ranging from 11 km to 50 km. CLIC uses a two-beam acceleration scheme, in which normal-conducting high-gradient 12 GHz accelerating structures are powered via a high-current drive beam. For the first stage, an alternative with X-band klystron powering is also considered. CLIC accelerator optimisation, technical developments and system tests have resulted in significant progress in recent years. Moreover, this has led to an increased energy efficiency (power around 170 MW) for the 380 GeV stage, together with a reduced cost estimate at the level of 6 billion CHF. The detector concept, which matches the physics performance requirements and the CLIC experimental conditions, has been refined using improved software tools for simulation and reconstruction. Significant progress has been made on detector technology developments for the tracking and calorimetry systems. A wide range of CLIC physics studies has been conducted, both through full detector simulations with overlay of beam-induced backgrounds, and through parametric studies, together providing a broad overview of the CLIC physics potential. Each of the three energy stages adds cornerstones of the full CLIC physics programme, such as Higgs width and couplings, top-quark properties, Higgs self-coupling, direct searches, and many precision electroweak measurements. The interpretation of the combined results gives crucial and accurate insight into new physics, largely complementary to LHC and HL-LHC. The construction of the first CLIC energy stage could start by 2026. First beams would be available by 2035, marking the beginning of a broad CLIC physics programme spanning 25–30 years. The Compact Linear Collider (CLIC) is a TeV-scale high-luminosity linear $e^+e^−$ collider under development at CERN. Following the CLIC conceptual design published in 2012, this report provides an overview of the CLIC project, its current status, and future developments. It presents the CLIC physics potential and reports on design, technology, and implementation aspects of the accelerator and the detector. For an optimal exploitation of its physics potential, CLIC is foreseen to be built and operated in stages, at centre-of-mass energies of 380 GeV, 1.5 TeV and 3 TeV, respectively, for a site length ranging from 11 km to 50 km. CLIC uses a two-beam acceleration scheme, in which normal-conducting high-gradient 12 GHz accelerating structures are powered via a high-current drive beam. For the first stage, an alternative with X-band klystron powering is also considered. CLIC accelerator optimisation, technical developments and system tests have resulted in significant progress in recent years. Moreover, this has led to an increased energy efficiency (power around 170 MW) for the 380 GeV stage, together with a reduced cost estimate at the level of 6 billion CHF. The detector concept, which matches the physics performance requirements and the CLIC experimental conditions, has been refined using improved software tools for simulation and reconstruction. Significant progress has been made on detector technology developments for the tracking and calorimetry systems. A wide range of CLIC physics studies has been conducted, both through full detector simulations with overlay of beam-induced backgrounds, and through parametric studies, together providing a broad overview of the CLIC physics potential. Each of the three energy stages adds cornerstones of the full CLIC physics programme, such as Higgs width and couplings, top-quark properties, Higgs self-coupling, direct searches, and many precision electroweak measurements. The interpretation of the combined results gives crucial and accurate insight into new physics, largely complementary to LHC and HL-LHC. The construction of the first CLIC energy stage could start by 2026. First beams would be available by 2035, marking the beginning of a broad CLIC physics programme spanning 25–30 years. The Compact Linear Collider (CLIC) is a TeV-scale high-luminosity linear $e^+e^−$ collider under development at CERN. Following the CLIC conceptual design published in 2012, this report provides an overview of the CLIC project, its current status, and future developments. It presents the CLIC physics potential and reports on design, technology, and implementation aspects of the accelerator and the detector. For an optimal exploitation of its physics potential, CLIC is foreseen to be built and operated in stages, at centre-of-mass energies of 380 GeV, 1.5 TeV and 3 TeV, respectively, for a site length ranging from 11 km to 50 km. CLIC uses a two-beam acceleration scheme, in which normal-conducting high-gradient 12 GHz accelerating structures are powered via a high-current drive beam. For the first stage, an alternative with X-band klystron powering is also considered. CLIC accelerator optimisation, technical developments and system tests have resulted in significant progress in recent years. Moreover, this has led to an increased energy efficiency (power around 170 MW) for the 380 GeV stage, together with a reduced cost estimate at the level of 6 billion CHF. The detector concept, which matches the physics performance requirements and the CLIC experimental conditions, has been refined using improved software tools for simulation and reconstruction. Significant progress has been made on detector technology developments for the tracking and calorimetry systems. A wide range of CLIC physics studies has been conducted, both through full detector simulations with overlay of beam-induced backgrounds, and through parametric studies, together providing a broad overview of the CLIC physics potential. Each of the three energy stages adds cornerstones of the full CLIC physics programme, such as Higgs width and couplings, top-quark properties, Higgs self-coupling, direct searches, and many precision electroweak measurements. The interpretation of the combined results gives crucial and accurate insight into new physics, largely complementary to LHC and HL-LHC. The construction of the first CLIC energy stage could start by 2026. First beams would be available by 2035, marking the beginning of a broad CLIC physics programme spanning 25–30 years. The Compact Linear Collider (CLIC) is a TeV-scale high-luminosity linear $e^+e^−$ collider under development at CERN. Following the CLIC conceptual design published in 2012, this report provides an overview of the CLIC project, its current status, and future developments. It presents the CLIC physics potential and reports on design, technology, and implementation aspects of the accelerator and the detector. For an optimal exploitation of its physics potential, CLIC is foreseen to be built and operated in stages, at centre-of-mass energies of 380 GeV, 1.5 TeV and 3 TeV, respectively, for a site length ranging from 11 km to 50 km. CLIC uses a two-beam acceleration scheme, in which normal-conducting high-gradient 12 GHz accelerating structures are powered via a high-current drive beam. For the first stage, an alternative with X-band klystron powering is also considered. CLIC accelerator optimisation, technical developments and system tests have resulted in significant progress in recent years. Moreover, this has led to an increased energy efficiency (power around 170 MW) for the 380 GeV stage, together with a reduced cost estimate at the level of 6 billion CHF. The detector concept, which matches the physics performance requirements and the CLIC experimental conditions, has been refined using improved software tools for simulation and reconstruction. Significant progress has been made on detector technology developments for the tracking and calorimetry systems. A wide range of CLIC physics studies has been conducted, both through full detector simulations with overlay of beam-induced backgrounds, and through parametric studies, together providing a broad overview of the CLIC physics potential. Each of the three energy stages adds cornerstones of the full CLIC physics programme, such as Higgs width and couplings, top-quark properties, Higgs self-coupling, direct searches, and many precision electroweak measurements. The interpretation of the combined results gives crucial and accurate insight into new physics, largely complementary to LHC and HL-LHC. The construction of the first CLIC energy stage could start by 2026. First beams would be available by 2035, marking the beginning of a broad CLIC physics programme spanning 25–30 years. The Compact Linear Collider (CLIC) is a TeV-scale high-luminosity linear $e^+e^−$ collider under development at CERN. Following the CLIC conceptual design published in 2012, this report provides an overview of the CLIC project, its current status, and future developments. It presents the CLIC physics potential and reports on design, technology, and implementation aspects of the accelerator and the detector. For an optimal exploitation of its physics potential, CLIC is foreseen to be built and operated in stages, at centre-of-mass energies of 380 GeV, 1.5 TeV and 3 TeV, respectively, for a site length ranging from 11 km to 50 km. CLIC uses a two-beam acceleration scheme, in which normal-conducting high-gradient 12 GHz accelerating structures are powered via a high-current drive beam. For the first stage, an alternative with X-band klystron powering is also considered. CLIC accelerator optimisation, technical developments and system tests have resulted in significant progress in recent years. Moreover, this has led to an increased energy efficiency (power around 170 MW) for the 380 GeV stage, together with a reduced cost estimate at the level of 6 billion CHF. The detector concept, which matches the physics performance requirements and the CLIC experimental conditions, has been refined using improved software tools for simulation and reconstruction. Significant progress has been made on detector technology developments for the tracking and calorimetry systems. A wide range of CLIC physics studies has been conducted, both through full detector simulations with overlay of beam-induced backgrounds, and through parametric studies, together providing a broad overview of the CLIC physics potential. Each of the three energy stages adds cornerstones of the full CLIC physics programme, such as Higgs width and couplings, top-quark properties, Higgs self-coupling, direct searches, and many precision electroweak measurements. The interpretation of the combined results gives crucial and accurate insight into new physics, largely complementary to LHC and HL-LHC. The construction of the first CLIC energy stage could start by 2026. First beams would be available by 2035, marking the beginning of a broad CLIC physics programme spanning 25–30 years. The Compact Linear Collider (CLIC) is a TeV-scale high-luminosity linear $e^+e^−$ collider under development at CERN. Following the CLIC conceptual design published in 2012, this report provides an overview of the CLIC project, its current status, and future developments. It presents the CLIC physics potential and reports on design, technology, and implementation aspects of the accelerator and the detector. For an optimal exploitation of its physics potential, CLIC is foreseen to be built and operated in stages, at centre-of-mass energies of 380 GeV, 1.5 TeV and 3 TeV, respectively, for a site length ranging from 11 km to 50 km. CLIC uses a two-beam acceleration scheme, in which normal-conducting high-gradient 12 GHz accelerating structures are powered via a high-current drive beam. For the first stage, an alternative with X-band klystron powering is also considered. CLIC accelerator optimisation, technical developments and system tests have resulted in significant progress in recent years. Moreover, this has led to an increased energy efficiency (power around 170 MW) for the 380 GeV stage, together with a reduced cost estimate at the level of 6 billion CHF. The detector concept, which matches the physics performance requirements and the CLIC experimental conditions, has been refined using improved software tools for simulation and reconstruction. Significant progress has been made on detector technology developments for the tracking and calorimetry systems. A wide range of CLIC physics studies has been conducted, both through full detector simulations with overlay of beam-induced backgrounds, and through parametric studies, together providing a broad overview of the CLIC physics potential. Each of the three energy stages adds cornerstones of the full CLIC physics programme, such as Higgs width and couplings, top-quark properties, Higgs self-coupling, direct searches, and many precision electroweak measurements. The interpretation of the combined results gives crucial and accurate insight into new physics, largely complementary to LHC and HL-LHC. The construction of the first CLIC energy stage could start by 2026. First beams would be available by 2035, marking the beginning of a broad CLIC physics programme spanning 25–30 years. The Compact Linear Collider (CLIC) is a TeV-scale high-luminosity linear $e^+e^−$ collider under development at CERN. Following the CLIC conceptual design published in 2012, this report provides an overview of the CLIC project, its current status, and future developments. It presents the CLIC physics potential and reports on design, technology, and implementation aspects of the accelerator and the detector. For an optimal exploitation of its physics potential, CLIC is foreseen to be built and operated in stages, at centre-of-mass energies of 380 GeV, 1.5 TeV and 3 TeV, respectively, for a site length ranging from 11 km to 50 km. CLIC uses a two-beam acceleration scheme, in which normal-conducting high-gradient 12 GHz accelerating structures are powered via a high-current drive beam. For the first stage, an alternative with X-band klystron powering is also considered. CLIC accelerator optimisation, technical developments and system tests have resulted in significant progress in recent years. Moreover, this has led to an increased energy efficiency (power around 170 MW) for the 380 GeV stage, together with a reduced cost estimate at the level of 6 billion CHF. The detector concept, which matches the physics performance requirements and the CLIC experimental conditions, has been refined using improved software tools for simulation and reconstruction. Significant progress has been made on detector technology developments for the tracking and calorimetry systems. A wide range of CLIC physics studies has been conducted, both through full detector simulations with overlay of beam-induced backgrounds, and through parametric studies, together providing a broad overview of the CLIC physics potential. Each of the three energy stages adds cornerstones of the full CLIC physics programme, such as Higgs width and couplings, top-quark properties, Higgs self-coupling, direct searches, and many precision electroweak measurements. The interpretation of the combined results gives crucial and accurate insight into new physics, largely complementary to LHC and HL-LHC. The construction of the first CLIC energy stage could start by 2026. First beams would be available by 2035, marking the beginning of a broad CLIC physics programme spanning 25–30 years. The Compact Linear Collider (CLIC) is a TeV-scale high-luminosity linear $e^+e^−$ collider under development at CERN. Following the CLIC conceptual design published in 2012, this report provides an overview of the CLIC project, its current status, and future developments. It presents the CLIC physics potential and reports on design, technology, and implementation aspects of the accelerator and the detector. For an optimal exploitation of its physics potential, CLIC is foreseen to be built and operated in stages, at centre-of-mass energies of 380 GeV, 1.5 TeV and 3 TeV, respectively, for a site length ranging from 11 km to 50 km. CLIC uses a two-beam acceleration scheme, in which normal-conducting high-gradient 12 GHz accelerating structures are powered via a high-current drive beam. For the first stage, an alternative with X-band klystron powering is also considered. CLIC accelerator optimisation, technical developments and system tests have resulted in significant progress in recent years. Moreover, this has led to an increased energy efficiency (power around 170 MW) for the 380 GeV stage, together with a reduced cost estimate at the level of 6 billion CHF. The detector concept, which matches the physics performance requirements and the CLIC experimental conditions, has been refined using improved software tools for simulation and reconstruction. Significant progress has been made on detector technology developments for the tracking and calorimetry systems. A wide range of CLIC physics studies has been conducted, both through full detector simulations with overlay of beam-induced backgrounds, and through parametric studies, together providing a broad overview of the CLIC physics potential. Each of the three energy stages adds cornerstones of the full CLIC physics programme, such as Higgs width and couplings, top-quark properties, Higgs self-coupling, direct searches, and many precision electroweak measurements. The interpretation of the combined results gives crucial and accurate insight into new physics, largely complementary to LHC and HL-LHC. The construction of the first CLIC energy stage could start by 2026. First beams would be available by 2035, marking the beginning of a broad CLIC physics programme spanning 25–30 years. The Compact Linear Collider (CLIC) is a TeV-scale high-luminosity linear $e^+e^−$ collider under development at CERN. Following the CLIC conceptual design published in 2012, this report provides an overview of the CLIC project, its current status, and future developments. It presents the CLIC physics potential and reports on design, technology, and implementation aspects of the accelerator and the detector. For an optimal exploitation of its physics potential, CLIC is foreseen to be built and operated in stages, at centre-of-mass energies of 380 GeV, 1.5 TeV and 3 TeV, respectively, for a site length ranging from 11 km to 50 km. CLIC uses a two-beam acceleration scheme, in which normal-conducting high-gradient 12 GHz accelerating structures are powered via a high-current drive beam. For the first stage, an alternative with X-band klystron powering is also considered. CLIC accelerator optimisation, technical developments and system tests have resulted in significant progress in recent years. Moreover, this has led to an increased energy efficiency (power around 170 MW) for the 380 GeV stage, together with a reduced cost estimate at the level of 6 billion CHF. The detector concept, which matches the physics performance requirements and the CLIC experimental conditions, has been refined using improved software tools for simulation and reconstruction. Significant progress has been made on detector technology developments for the tracking and calorimetry systems. A wide range of CLIC physics studies has been conducted, both through full detector simulations with overlay of beam-induced backgrounds, and through parametric studies, together providing a broad overview of the CLIC physics potential. Each of the three energy stages adds cornerstones of the full CLIC physics programme, such as Higgs width and couplings, top-quark properties, Higgs self-coupling, direct searches, and many precision electroweak measurements. The interpretation of the combined results gives crucial and accurate insight into new physics, largely complementary to LHC and HL-LHC. The construction of the first CLIC energy stage could start by 2026. First beams would be available by 2035, marking the beginning of a broad CLIC physics programme spanning 25–30 years. The Compact Linear Collider (CLIC) is a TeV-scale high-luminosity linear $e^+e^−$ collider under development at CERN. Following the CLIC conceptual design published in 2012, this report provides an overview of the CLIC project, its current status, and future developments. It presents the CLIC physics potential and reports on design, technology, and implementation aspects of the accelerator and the detector. For an optimal exploitation of its physics potential, CLIC is foreseen to be built and operated in stages, at centre-of-mass energies of 380 GeV, 1.5 TeV and 3 TeV, respectively, for a site length ranging from 11 km to 50 km. CLIC uses a two-beam acceleration scheme, in which normal-conducting high-gradient 12 GHz accelerating structures are powered via a high-current drive beam. For the first stage, an alternative with X-band klystron powering is also considered. CLIC accelerator optimisation, technical developments and system tests have resulted in significant progress in recent years. Moreover, this has led to an increased energy efficiency (power around 170 MW) for the 380 GeV stage, together with a reduced cost estimate at the level of 6 billion CHF. The detector concept, which matches the physics performance requirements and the CLIC experimental conditions, has been refined using improved software tools for simulation and reconstruction. Significant progress has been made on detector technology developments for the tracking and calorimetry systems. A wide range of CLIC physics studies has been conducted, both through full detector simulations with overlay of beam-induced backgrounds, and through parametric studies, together providing a broad overview of the CLIC physics potential. Each of the three energy stages adds cornerstones of the full CLIC physics programme, such as Higgs width and couplings, top-quark properties, Higgs self-coupling, direct searches, and many precision electroweak measurements. The interpretation of the combined results gives crucial and accurate insight into new physics, largely complementary to LHC and HL-LHC. The construction of the first CLIC energy stage could start by 2026. First beams would be available by 2035, marking the beginning of a broad CLIC physics programme spanning 25–30 years. The Compact Linear Collider (CLIC) is a TeV-scale high-luminosity linear $e^+e^−$ collider under development at CERN. Following the CLIC conceptual design published in 2012, this report provides an overview of the CLIC project, its current status, and future developments. It presents the CLIC physics potential and reports on design, technology, and implementation aspects of the accelerator and the detector. For an optimal exploitation of its physics potential, CLIC is foreseen to be built and operated in stages, at centre-of-mass energies of 380 GeV, 1.5 TeV and 3 TeV, respectively, for a site length ranging from 11 km to 50 km. CLIC uses a two-beam acceleration scheme, in which normal-conducting high-gradient 12 GHz accelerating structures are powered via a high-current drive beam. For the first stage, an alternative with X-band klystron powering is also considered. CLIC accelerator optimisation, technical developments and system tests have resulted in significant progress in recent years. Moreover, this has led to an increased energy efficiency (power around 170 MW) for the 380 GeV stage, together with a reduced cost estimate at the level of 6 billion CHF. The detector concept, which matches the physics performance requirements and the CLIC experimental conditions, has been refined using improved software tools for simulation and reconstruction. Significant progress has been made on detector technology developments for the tracking and calorimetry systems. A wide range of CLIC physics studies has been conducted, both through full detector simulations with overlay of beam-induced backgrounds, and through parametric studies, together providing a broad overview of the CLIC physics potential. Each of the three energy stages adds cornerstones of the full CLIC physics programme, such as Higgs width and couplings, top-quark properties, Higgs self-coupling, direct searches, and many precision electroweak measurements. The interpretation of the combined results gives crucial and accurate insight into new physics, largely complementary to LHC and HL-LHC. The construction of the first CLIC energy stage could start by 2026. First beams would be available by 2035, marking the beginning of a broad CLIC physics programme spanning 25–30 years. The Compact Linear Collider (CLIC) is a TeV-scale high-luminosity linear $e^+e^−$ collider under development at CERN. Following the CLIC conceptual design published in 2012, this report provides an overview of the CLIC project, its current status, and future developments. It presents the CLIC physics potential and reports on design, technology, and implementation aspects of the accelerator and the detector. For an optimal exploitation of its physics potential, CLIC is foreseen to be built and operated in stages, at centre-of-mass energies of 380 GeV, 1.5 TeV and 3 TeV, respectively, for a site length ranging from 11 km to 50 km. CLIC uses a two-beam acceleration scheme, in which normal-conducting high-gradient 12 GHz accelerating structures are powered via a high-current drive beam. For the first stage, an alternative with X-band klystron powering is also considered. CLIC accelerator optimisation, technical developments and system tests have resulted in significant progress in recent years. Moreover, this has led to an increased energy efficiency (power around 170 MW) for the 380 GeV stage, together with a reduced cost estimate at the level of 6 billion CHF. The detector concept, which matches the physics performance requirements and the CLIC experimental conditions, has been refined using improved software tools for simulation and reconstruction. Significant progress has been made on detector technology developments for the tracking and calorimetry systems. A wide range of CLIC physics studies has been conducted, both through full detector simulations with overlay of beam-induced backgrounds, and through parametric studies, together providing a broad overview of the CLIC physics potential. Each of the three energy stages adds cornerstones of the full CLIC physics programme, such as Higgs width and couplings, top-quark properties, Higgs self-coupling, direct searches, and many precision electroweak measurements. The interpretation of the combined results gives crucial and accurate insight into new physics, largely complementary to LHC and HL-LHC. The construction of the first CLIC energy stage could start by 2026. First beams would be available by 2035, marking the beginning of a broad CLIC physics programme spanning 25–30 years. The Compact Linear Collider (CLIC) is a TeV-scale high-luminosity linear $e^+e^−$ collider under development at CERN. Following the CLIC conceptual design published in 2012, this report provides an overview of the CLIC project, its current status, and future developments. It presents the CLIC physics potential and reports on design, technology, and implementation aspects of the accelerator and the detector. For an optimal exploitation of its physics potential, CLIC is foreseen to be built and operated in stages, at centre-of-mass energies of 380 GeV, 1.5 TeV and 3 TeV, respectively, for a site length ranging from 11 km to 50 km. CLIC uses a two-beam acceleration scheme, in which normal-conducting high-gradient 12 GHz accelerating structures are powered via a high-current drive beam. For the first stage, an alternative with X-band klystron powering is also considered. CLIC accelerator optimisation, technical developments and system tests have resulted in significant progress in recent years. Moreover, this has led to an increased energy efficiency (power around 170 MW) for the 380 GeV stage, together with a reduced cost estimate at the level of 6 billion CHF. The detector concept, which matches the physics performance requirements and the CLIC experimental conditions, has been refined using improved software tools for simulation and reconstruction. Significant progress has been made on detector technology developments for the tracking and calorimetry systems. A wide range of CLIC physics studies has been conducted, both through full detector simulations with overlay of beam-induced backgrounds, and through parametric studies, together providing a broad overview of the CLIC physics potential. Each of the three energy stages adds cornerstones of the full CLIC physics programme, such as Higgs width and couplings, top-quark properties, Higgs self-coupling, direct searches, and many precision electroweak measurements. The interpretation of the combined results gives crucial and accurate insight into new physics, largely complementary to LHC and HL-LHC. The construction of the first CLIC energy stage could start by 2026. First beams would be available by 2035, marking the beginning of a broad CLIC physics programme spanning 25–30 years. The Compact Linear Collider (CLIC) is a TeV-scale high-luminosity linear $e^+e^−$ collider under development at CERN. Following the CLIC conceptual design published in 2012, this report provides an overview of the CLIC project, its current status, and future developments. It presents the CLIC physics potential and reports on design, technology, and implementation aspects of the accelerator and the detector. For an optimal exploitation of its physics potential, CLIC is foreseen to be built and operated in stages, at centre-of-mass energies of 380 GeV, 1.5 TeV and 3 TeV, respectively, for a site length ranging from 11 km to 50 km. CLIC uses a two-beam acceleration scheme, in which normal-conducting high-gradient 12 GHz accelerating structures are powered via a high-current drive beam. For the first stage, an alternative with X-band klystron powering is also considered. CLIC accelerator optimisation, technical developments and system tests have resulted in significant progress in recent years. Moreover, this has led to an increased energy efficiency (power around 170 MW) for the 380 GeV stage, together with a reduced cost estimate at the level of 6 billion CHF. The detector concept, which matches the physics performance requirements and the CLIC experimental conditions, has been refined using improved software tools for simulation and reconstruction. Significant progress has been made on detector technology developments for the tracking and calorimetry systems. A wide range of CLIC physics studies has been conducted, both through full detector simulations with overlay of beam-induced backgrounds, and through parametric studies, together providing a broad overview of the CLIC physics potential. Each of the three energy stages adds cornerstones of the full CLIC physics programme, such as Higgs width and couplings, top-quark properties, Higgs self-coupling, direct searches, and many precision electroweak measurements. The interpretation of the combined results gives crucial and accurate insight into new physics, largely complementary to LHC and HL-LHC. The construction of the first CLIC energy stage could start by 2026. First beams would be available by 2035, marking the beginning of a broad CLIC physics programme spanning 25–30 years. The Compact Linear Collider (CLIC) is a TeV-scale high-luminosity linear $e^+e^−$ collider under development at CERN. Following the CLIC conceptual design published in 2012, this report provides an overview of the CLIC project, its current status, and future developments. It presents the CLIC physics potential and reports on design, technology, and implementation aspects of the accelerator and the detector. For an optimal exploitation of its physics potential, CLIC is foreseen to be built and operated in stages, at centre-of-mass energies of 380 GeV, 1.5 TeV and 3 TeV, respectively, for a site length ranging from 11 km to 50 km. CLIC uses a two-beam acceleration scheme, in which normal-conducting high-gradient 12 GHz accelerating structures are powered via a high-current drive beam. For the first stage, an alternative with X-band klystron powering is also considered. CLIC accelerator optimisation, technical developments and system tests have resulted in significant progress in recent years. Moreover, this has led to an increased energy efficiency (power around 170 MW) for the 380 GeV stage, together with a reduced cost estimate at the level of 6 billion CHF. The detector concept, which matches the physics performance requirements and the CLIC experimental conditions, has been refined using improved software tools for simulation and reconstruction. Significant progress has been made on detector technology developments for the tracking and calorimetry systems. A wide range of CLIC physics studies has been conducted, both through full detector simulations with overlay of beam-induced backgrounds, and through parametric studies, together providing a broad overview of the CLIC physics potential. Each of the three energy stages adds cornerstones of the full CLIC physics programme, such as Higgs width and couplings, top-quark properties, Higgs self-coupling, direct searches, and many precision electroweak measurements. The interpretation of the combined results gives crucial and accurate insight into new physics, largely complementary to LHC and HL-LHC. The construction of the first CLIC energy stage could start by 2026. First beams would be available by 2035, marking the beginning of a broad CLIC physics programme spanning 25–30 years. The Compact Linear Collider (CLIC) is a TeV-scale high-luminosity linear $e^+e^−$ collider under development at CERN. Following the CLIC conceptual design published in 2012, this report provides an overview of the CLIC project, its current status, and future developments. It presents the CLIC physics potential and reports on design, technology, and implementation aspects of the accelerator and the detector. For an optimal exploitation of its physics potential, CLIC is foreseen to be built and operated in stages, at centre-of-mass energies of 380 GeV, 1.5 TeV and 3 TeV, respectively, for a site length ranging from 11 km to 50 km. CLIC uses a two-beam acceleration scheme, in which normal-conducting high-gradient 12 GHz accelerating structures are powered via a high-current drive beam. For the first stage, an alternative with X-band klystron powering is also considered. CLIC accelerator optimisation, technical developments and system tests have resulted in significant progress in recent years. Moreover, this has led to an increased energy efficiency (power around 170 MW) for the 380 GeV stage, together with a reduced cost estimate at the level of 6 billion CHF. The detector concept, which matches the physics performance requirements and the CLIC experimental conditions, has been refined using improved software tools for simulation and reconstruction. Significant progress has been made on detector technology developments for the tracking and calorimetry systems. A wide range of CLIC physics studies has been conducted, both through full detector simulations with overlay of beam-induced backgrounds, and through parametric studies, together providing a broad overview of the CLIC physics potential. Each of the three energy stages adds cornerstones of the full CLIC physics programme, such as Higgs width and couplings, top-quark properties, Higgs self-coupling, direct searches, and many precision electroweak measurements. The interpretation of the combined results gives crucial and accurate insight into new physics, largely complementary to LHC and HL-LHC. The construction of the first CLIC energy stage could start by 2026. First beams would be available by 2035, marking the beginning of a broad CLIC physics programme spanning 25–30 years. The Compact Linear Collider (CLIC) is a TeV-scale high-luminosity linear $e^+e^−$ collider under development at CERN. Following the CLIC conceptual design published in 2012, this report provides an overview of the CLIC project, its current status, and future developments. It presents the CLIC physics potential and reports on design, technology, and implementation aspects of the accelerator and the detector. For an optimal exploitation of its physics potential, CLIC is foreseen to be built and operated in stages, at centre-of-mass energies of 380 GeV, 1.5 TeV and 3 TeV, respectively, for a site length ranging from 11 km to 50 km. CLIC uses a two-beam acceleration scheme, in which normal-conducting high-gradient 12 GHz accelerating structures are powered via a high-current drive beam. For the first stage, an alternative with X-band klystron powering is also considered. CLIC accelerator optimisation, technical developments and system tests have resulted in significant progress in recent years. Moreover, this has led to an increased energy efficiency (power around 170 MW) for the 380 GeV stage, together with a reduced cost estimate at the level of 6 billion CHF. The detector concept, which matches the physics performance requirements and the CLIC experimental conditions, has been refined using improved software tools for simulation and reconstruction. Significant progress has been made on detector technology developments for the tracking and calorimetry systems. A wide range of CLIC physics studies has been conducted, both through full detector simulations with overlay of beam-induced backgrounds, and through parametric studies, together providing a broad overview of the CLIC physics potential. Each of the three energy stages adds cornerstones of the full CLIC physics programme, such as Higgs width and couplings, top-quark properties, Higgs self-coupling, direct searches, and many precision electroweak measurements. The interpretation of the combined results gives crucial and accurate insight into new physics, largely complementary to LHC and HL-LHC. The construction of the first CLIC energy stage could start by 2026. First beams would be available by 2035, marking the beginning of a broad CLIC physics programme spanning 25–30 years. The Compact Linear Collider (CLIC) is a TeV-scale high-luminosity linear $e^+e^−$ collider under development at CERN. Following the CLIC conceptual design published in 2012, this report provides an overview of the CLIC project, its current status, and future developments. It presents the CLIC physics potential and reports on design, technology, and implementation aspects of the accelerator and the detector. For an optimal exploitation of its physics potential, CLIC is foreseen to be built and operated in stages, at centre-of-mass energies of 380 GeV, 1.5 TeV and 3 TeV, respectively, for a site length ranging from 11 km to 50 km. CLIC uses a two-beam acceleration scheme, in which normal-conducting high-gradient 12 GHz accelerating structures are powered via a high-current drive beam. For the first stage, an alternative with X-band klystron powering is also considered. CLIC accelerator optimisation, technical developments and system tests have resulted in significant progress in recent years. Moreover, this has led to an increased energy efficiency (power around 170 MW) for the 380 GeV stage, together with a reduced cost estimate at the level of 6 billion CHF. The detector concept, which matches the physics performance requirements and the CLIC experimental conditions, has been refined using improved software tools for simulation and reconstruction. Significant progress has been made on detector technology developments for the tracking and calorimetry systems. A wide range of CLIC physics studies has been conducted, both through full detector simulations with overlay of beam-induced backgrounds, and through parametric studies, together providing a broad overview of the CLIC physics potential. Each of the three energy stages adds cornerstones of the full CLIC physics programme, such as Higgs width and couplings, top-quark properties, Higgs self-coupling, direct searches, and many precision electroweak measurements. The interpretation of the combined results gives crucial and accurate insight into new physics, largely complementary to LHC and HL-LHC. The construction of the first CLIC energy stage could start by 2026. First beams would be available by 2035, marking the beginning of a broad CLIC physics programme spanning 25–30 years. The Compact Linear Collider (CLIC) is a TeV-scale high-luminosity linear $e^+e^−$ collider under development at CERN. Following the CLIC conceptual design published in 2012, this report provides an overview of the CLIC project, its current status, and future developments. It presents the CLIC physics potential and reports on design, technology, and implementation aspects of the accelerator and the detector. For an optimal exploitation of its physics potential, CLIC is foreseen to be built and operated in stages, at centre-of-mass energies of 380 GeV, 1.5 TeV and 3 TeV, respectively, for a site length ranging from 11 km to 50 km. CLIC uses a two-beam acceleration scheme, in which normal-conducting high-gradient 12 GHz accelerating structures are powered via a high-current drive beam. For the first stage, an alternative with X-band klystron powering is also considered. CLIC accelerator optimisation, technical developments and system tests have resulted in significant progress in recent years. Moreover, this has led to an increased energy efficiency (power around 170 MW) for the 380 GeV stage, together with a reduced cost estimate at the level of 6 billion CHF. The detector concept, which matches the physics performance requirements and the CLIC experimental conditions, has been refined using improved software tools for simulation and reconstruction. Significant progress has been made on detector technology developments for the tracking and calorimetry systems. A wide range of CLIC physics studies has been conducted, both through full detector simulations with overlay of beam-induced backgrounds, and through parametric studies, together providing a broad overview of the CLIC physics potential. Each of the three energy stages adds cornerstones of the full CLIC physics programme, such as Higgs width and couplings, top-quark properties, Higgs self-coupling, direct searches, and many precision electroweak measurements. The interpretation of the combined results gives crucial and accurate insight into new physics, largely complementary to LHC and HL-LHC. The construction of the first CLIC energy stage could start by 2026. First beams would be available by 2035, marking the beginning of a broad CLIC physics programme spanning 25–30 years. The Compact Linear Collider (CLIC) is a TeV-scale high-luminosity linear $e^+e^-$ collider under development at CERN. Following the CLIC conceptual design published in 2012, this report provides an overview of the CLIC project, its current status, and future developments. It presents the CLIC physics potential and reports on design, technology, and implementation aspects of the accelerator and the detector. CLIC is foreseen to be built and operated in stages, at centre-of-mass energies of 380 GeV, 1.5 TeV and 3 TeV, respectively. CLIC uses a two-beam acceleration scheme, in which 12 GHz accelerating structures are powered via a high-current drive beam. For the first stage, an alternative with X-band klystron powering is also considered. CLIC accelerator optimisation, technical developments and system tests have resulted in an increased energy efficiency (power around 170 MW) for the 380 GeV stage, together with a reduced cost estimate at the level of 6 billion CHF. The detector concept has been refined using improved software tools. Significant progress has been made on detector technology developments for the tracking and calorimetry systems. A wide range of CLIC physics studies has been conducted, both through full detector simulations and parametric studies, together providing a broad overview of the CLIC physics potential. Each of the three energy stages adds cornerstones of the full CLIC physics programme, such as Higgs width and couplings, top-quark properties, Higgs self-coupling, direct searches, and many precision electroweak measurements. The interpretation of the combined results gives crucial and accurate insight into new physics, largely complementary to LHC and HL-LHC. The construction of the first CLIC energy stage could start by 2026. First beams would be available by 2035, marking the beginning of a broad CLIC physics programme spanning 25-30 years.
43. Un modello di comunicazione per la prevenzione del rischio biologico in ambienti di lavoro non sanitari
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Calamusa, A., MARCO VERANI, Giuntini, A., Bernardini, M., and annalaura carducci
44. Weber-Christian disease: Report of a case
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Offidani, A., D Angelo, G., Bernardini, M. L., Marco Marigliano, Pierani, P., Giangiacomi, M., and Coppa, G. V.
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children ,weber-christian ,adipose tissue
45. Benign lymphocytic infiltration of Jessner-Kanof: A case report,Infiltrato linfocitario benigno di Jessner-Kanof: Descrizione di un caso
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Oriana SIMONETTI, Laghi, L., Cingolani, C., Verdolini, R., Bernardini, M. L., and Offidani, A.
46. The class of 'disguised' short GRBs and its implications for the Amati relation
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Bianco, C. L., Lorenzo Amati, Bernardini, M. G., Caito, L., Barros, G., Izzo, L., Patricelli, B., and Ruffni, R.
47. Status and noise limit of the VIRGO antenna
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Babusci, D., Fang, H., Giordano, G., Iannarelli, M., Matone, G., Turri, E., Mazzoni, M., Stanga, R., Calloni, E., Cavaliere, S., Di Fiore, L., Evangelista, G., Garifi, F., Grado, A., Milano, L., Solimeno, S., Cagnoli, G., Cattuto, C., Kovalik, J., Marchesoni, F., Punturo, M., Bernardini, M., Bozzi, A., Braccini, S., Bradaschia, C., Casciano, C., Cella, G., Ciampa, A., Cuoco, E., Curci, G., D Ambrosio, E., Dattilo, V., Carolis, G., Salvo, R., Angela Dora Vittoria Di Virgilio, Enard, D., Errico, A., Feng, G., Ferrante, I., Fidecaro, F., Frasconi, F., Gaddi, A., Gennai, A., Gennaro, G., Giazotto, A., La Penna, P., Losurdo, G., Maggiore, M., Mancini, S., Palla, F., Pan, H. B., Paoletti, F., Pasqualetti, A., Passaquieti, R., Passuello, D., Poggiani, R., Popolizio, P., Raffaelli, F., Rapisarda, S., Taddei, R., Vicere, A., Zhang, Z., Astone, P., Bronzini, F., Frasca, S., Majorana, E., Palomba, C., Perciballi, M., Puppo, P., Rapagnani, P., Ricci, F., Boccara, C., Daban, J. B., Leliboux, M., Loriette, V., Nahoum, R., Roger, J. P., Ganau, P., Lagrange, B., Mackowski, J. M., Michel, C., Morgago, N., Pinard, L., Remillieux, A., Arnault, C., Barrand, C., Beney, J. L., Bilhaut, R., Brisson, V., Cavalier, F., Chiche, R., Coulon, J. P., Cuzon, S., Davier, M., Dehamme, M., Dialinas, M., Eder, C., Gaspard, M., Hello, P., Heusse, P., Hrisoho, A., Jules, E., Marrucho, J. C., Mencik, M., Marin, P., Matone, L., Reboux, A., Roudier, P., Taurigna, M., Bellachia, F., Bermond, M., Boget, D., Caron, B., Carron, T., Castellazzi, D., Chollet, F., Daguin, G., David, P. Y., Derome, L., Drezen, C., Dufournaud, D., Flamino, R., Giacobone, L., Girard, C., Grave, X., Hermel, R., Lacotte, J. C., Le Marec, J. C., Lieunard, B., Marion, F., Massonnet, L., Mehmel, C., Morand, R., Mours, B., Mugnier, P., Sannibale, V., Sottile, R., Verkindt, D., Yvert, M., Acker, Y., Barillet, R., Barsuglia, M., Berthet, J. P., Brillet, A., Cachenaut, J., Cleva, F., Heitmann, H., Innocent, J. M., Lucenay, J. C., Man, N. C., Manh, P. T., Marck, J. A., Pelat, D., Reita, V., and Vinet, J. Y.
48. Linee guida flebo-linfologiche SIF-SICVE 2016 della Società Italiana di Flebologia e della Società Italiana di Chirurgia Vascolare ed Endovascolare
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Ebner, H., Stillo, F., Lanza, G., Mangialardi, N., Agus, G. B., Apperti, M., Bernardini, E., Bernardini, M., Bernardo, B., Bianchini, G., Bisacci, R., Camparini, S., Chiulli, N., Corda, D., Crespi, A., Fiores, A., Roberto Di Mitri, Dorigo, W., Ebner, J. A., Emanuelli, G., Ferrara, F., Genovese, G., Giacomelli, E., Giannasio, B., Gossetti, B., Guerra, M., Mattaliano, V., Musiani, A., Pieroni, O., Piccioli, R., Pisacreta, M., Pratesi, C., Ronchey, S., Quarto, G., Sellitti, A., Spinelli, G. M., Strati, E., Tori, A., Viani, M., Zolesio, P., Ebner, Heinrich, Stillo, Francesco, Lanza, Gaetano, Mangialardi, Nicola, Agus, Giovanni B, Apperti, Marco, Bernardini, Eugenio, Bernardini, Marcello, Bernardo, Benedetto, Bianchini, Giuseppe, Bisacci, Roberto, Camparini, Stefano, Chiulli, Nicola, Corda, Domenico, Crespi, Aldo, De Fiores, Antonio, Di Mitri, Roberto, Dorigo, Walter, Ebner, Juliane A, Emanuelli, Guglielmo, Ferrara, Francesco, Genovese, Giuseppe, Giacomelli, Elena, Giannasio, Benedetta, Gossetti, Bruno, Guerra, Mirko, Mattaliano, Vincenzo, Musiani, Antonello, Pieroni, Olindo, Piccioli, Riccardo, Pisacreta, Massimo, Pratesi, Carlo, Ronchey, Sonia, Quarto, Gennaro, Sellitti, Antonio, Spinelli, Giovanni M, Strati, Enzo, Tori, Antonio, Viani, Marco, and Zolesio, Pierluigi
- Abstract
Phlebology is not a specialty for its own in Italy. Phlebological patients are treated by vascular and general surgeons, dermatologists, phlebologists, angiologists, internists and even general practitioners. Even tough guidelines present a series of recommendations based on evidence-based medicine, guidelines may also be a tool to unify the diagnostic and therapeutic approach in a vast medical field like phlebology. Since vascular surgeons and phlebologists are particularly involved in phlebology-related pathologies the scientific societies of the Italian Society of Phlebology (SIF) and the Italian Society for Vascular and Endovascular Surgery (SICVE) decided to cooperate for the preparation of phlebo-lymphological guidelines. These guidelines comprehend also an important chapter dealing with the lymphology of the lower extremities; phlebological active physicians are often faced with lymphatic pathologies and a good differential diagnosis can be sometimes very helpful. Sclerotherapy and Surgery as the major therapeutical alternatives are extensively analyzed, but also the compression therapy, the medical and physical therapy are presented under the critical view of evidence based analyses. Separate chapters deal with the treatment alternatives for superficial and deep venous thromboses and the recommendations for the treatment of venous ulcers. The current scientific evidences were confronted with the experiences of Italian specialists and the particular practice and reality in Italy. They represent therefore the actual valid positions and recommendations in Italy which shall be updated regularly.
49. The transpedicular approach for the study of intervertebral disc regeneration strategies: In vivo characterization
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Vadalà, G., Russo, F., Strobel, F., Bernardini, M., Eglin, D., Grad, S., Alini, M., and Vincenzo Denaro
50. Changes of flow mediated dilation in pregnant patients with systemic autoimmune diseases
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Tani C, Rm, Bruno, Strigini F, Carli L, Bernardini M, Talarico R, CHIARA BALDINI, Ghiadoni L, and Mosca M
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