49 research outputs found
No Gas All Local: Developing a renewable-based and decentralised energy system for the historic centre of Amsterdam
No full textUrban energy systems are the key elements of combating the climate crisis as the energy transition is crucial to curb greenhouse gas emissions in urban areas, one of the main drivers of climate change. As such, there is a great effort in Amsterdam to phase out natural gas use by 2040, and to become carbon neutral by 2050. It is a great challenge since the existing centralised energy systems are specifically built on the transportation and use of large amounts of fossil fuels while renewable energy has many limitations due to the volatility of its sources, lack of capacity for energy load and storage. Yet, since renewable energy sources are locally available everywhere, the establishment of decentralised renewable energy infrastructures based on local sources can help overcome these limitations. On this basis, this research explores the possibility of developing such systems through a case study in the historic centre of Amsterdam where many local challenges like urban monumentality pose risks for the energy transition. The research is structured around the use of Smart Urban Isle approach as a methodological tool to reveal local potentials for energy reduction, reuse and production, and to design energy concepts based on these potentials to reduce the reliance on external energy input. The results of the case study show that it is possible to cover the heat and cold demand with local sources and to cut almost half of the external energy input into the site without bringing any significant pressure onto the power grid. This outcome is highly promising as it proves that such local interventions can make great contributions to the energy transition process by significantly reducing the tension on the regional and national energy systems for the replacement of fossil fuels. As for the field of architecture and urban planning, the results implicate that the bioclimatic design principles, mixed-use of buildings and urban spaces, and small-scale and decentralised urban infrastructures based on the circular economy and self-sufficiency principles are crucial to achieve higher energy efficiencies and more local energy inputs.Metropolitan Analysis, Design and Engineering (MADE
Summer in the city: Sun, Swimming - and Sleepless Nights?: Understanding nuisance problems in relation to citizen reporting on nuisance experiences and interventions in the context of urban summer recreation in green-blue open spaces in Amsterdam-east
No full textOver the last decade, summer recreation in urban green-blue open spaces has become increasingly popular in Amsterdam, but so has the amount of reported nuisance because of summer recreation. In this thesis, the nuisance that has been reported by citizens during the summer recreation season from 2020 has been analysed by coding the reports in Atlas.TI, and using a survey from the Muncipality of Amsterdam as a verification. There are two locations where large amounts of nuisance reports have been filed, the Bogortuin and Park Somerlust, and several smaller locations with quay walls in the Oostelijk Havengebied and on the Amstel river. The content on the individual nuisance experience in the reports has been separated in observations, providing the nuisance causes, and evaluations, providing the nuisance impact. Recreation in it self is not problematic per se, but the presence of large groups of youngsters and recreation during the evening hours and at night is. This impacts local residents because of noise nuisance, especially at night, and pollution of waste and public urination. The character of summer recreation nuisance can be classified as both physical and social nuisance that is experienced during the evening hours, on weekend days and when it’s dry and warm. Implemented interventions have been evaluated and together with proposed interventions been analysed with the prevention pyramid. The measures that deal with the physical nuisance, temporary public toilets and an increase of waste capacity are in general reviewed positively. One successful intervention on social nuisance is the anchoring ban with a buoy line in the water to prevent noise nuisance from boats. None of the measures has been designed in an integrated way, using all the levels of the pyramid. Metropolitan Analysis, Design and Engineering (MADE
Correction: MHCII reduction is insufficient to protect mice from alpha-synuclein-induced degeneration and the Parkinson’s HLA locus exhibits epigenetic regulation
No full textCorrection to: Scientific Reports 10.1038/s41598-025-95679-3, published online 21 April 2025
Fredric P. Manfredsson was omitted from the author list in the original version of this Article.
Consequently, in the Author contributions section,
“E.M.K. and M.G.T. conceived the study. E.M.K. designed the study and supervised the technical staff involved in the study. E.M.K., J.J., C.D.S., J.M., S.L.H., M.K.H., R.L.W., S.D.K., J.C., K.B.M., V.J. performed the various surgeries and assays. N.R.M. provided human samples in accordance with IRB. J.M.B. and M.G.T. obtained funding support. J.M.B. and C.D.S. provided guidance and interpretation on ATAC-seq and MHCII gene expression. E.M.K., J.J., M.G.T. and V.J. wrote and edited the paper. E.M.K., J.J. and V.J. were responsible for all prepared figures. All authors reviewed and approved the final version of the manuscript.”
now reads:
“E.M.K. and M.G.T. conceived the study. E.M.K. designed the study and supervised the technical staff involved in the study. E.M.K., J.J., C.D.S., J.M., S.L.H., M.K.H., R.L.W., S.D.K., J.C., K.B.M., F.P.M., and V.J. performed the various surgeries and assays. N.R.M. provided human samples in accordance with IRB. J.M.B. and M.G.T. obtained funding support. J.M.B. and C.D.S. provided guidance and interpretation on ATAC-seq and MHCII gene expression. E.M.K., J.J., M.G.T. and V.J. wrote and edited the paper. E.M.K., J.J. and V.J. were responsible for all prepared figures. All authors reviewed and approved the final version of the manuscript.”
Furthermore, the Acknowledgements section has been updated. It now reads:
“We thank the Emory Flow Cytometry Core for their assistance with the use of the LSRII, as well as the Emory Genomics Core for completing library preparations and sequencing. We thank Haydeh Payami and the Tansey lab for thoughtful discussions. Partial funding from this work came from a pilot grant from Emory PD-CERC (MGT and JMB), a pilot grant from NIH/NINDS 1P50NS071669 Emory’s Udall Parkinson’s Disease Center/UL1RR025008 Atlanta Clinical and Translational Science Institute (ACTSI) (JMB and MGT), NIH RO1AI153102 (JMB), NIH/NINDS RF1NS128800 (MGT) and NIH/NINDS 5R01NS092122 (MGT and JMB). Support was also provided by Michael J Fox foundation MJFF-023296 (VJ and MGT), 1FL ADRC Alzstars P30AG066506 (VJ) and Alzheimer’s Association AARG-22-927012 (VJ). Figure 1 was created in BioRender. Jernigan, J. (2025) https://BioRender.com/r71q005.”
In addition, the affiliation “Department of Physiology, Emory University School of Medicine, Atlanta, GA, USA” was omitted for authors Elizabeth M. Kline, Mary K. Herrick, Sean D. Kelly, Jianjun Chang, Malú Gámez Tansey, and Valerie Joers
Complement activation and protein adsorption by carbon nanotubes
No full textAs a first step to validate the use of carbon nanotubes as novel vaccine or drug delivery devices, their interaction with a part of the human immune system, complement, has been explored. Haemolytic assays were conducted to investigate the activation of the human serum complement system via the classical and alternative pathways. Western blot and sodium dodecyl sulphate-polyacrylamide gel electrophoresis (SDS-PAGE) techniques were used to elucidate the mechanism of activation of complement via the classical pathway, and to analyse the interaction of complement and other plasma proteins with carbon nanotubes. We report for the first time that carbon nanotubes activate human complement via both classical and alternative pathways. We conclude that complement activation by nanotubes is consistent with reported adjuvant effects, and might also in various circumstances promote damaging effects of excessive complement activation, such as inflammation and granuloma formation. C1q binds directly to carbon nanotubes. Protein binding to carbon nanotubes is highly selective, since out of the many different proteins in plasma, very few bind to the carbon nanotubes. Fibrinogen and apolipoproteins (AI, AIV and CIII) were the proteins that bound to carbon nanotubes in greatest quantit
Multi-messenger observations of a binary neutron star merger
No full text3614siopenOn 2017 August 17 a binary neutron star coalescence candidate (later designated GW170817) with merger time 12:41:04 UTC was observed through gravitational waves by the Advanced LIGO and Advanced Virgo detectors. The Fermi Gamma-ray Burst Monitor independently detected a gamma-ray burst (GRB 170817A) with a time delay of ~1.7 s with respect to the merger time. From the gravitational-wave signal, the source was initially localized to a sky region of 31 deg2 at a luminosity distance of 40 8 8-+ Mpc and with component masses consistent with neutron stars. The component masses were later measured to be in the range 0.86 to 2.26 M. An extensive observing campaign was launched across the electromagnetic spectrum leading to the discovery of a bright optical transient (SSS17a, now with the IAU identification of AT 2017gfo) in NGC 4993 (at ~40 Mpc) less than 11 hours after the merger by the One-Meter, Two Hemisphere (1M2H) team using the 1 m Swope Telescope. The optical transient was independently detected by multiple teams within an hour. Subsequent observations targeted the object and its environment. Early ultraviolet observations revealed a blue transient that faded within 48 hours. Optical and infrared observations showed a redward evolution over ~10 days. Following early non-detections, X-ray and radio emission were discovered at the transient's position ~9 and ~16 days, respectively, after the merger. Both the X-ray and radio emission likely arise from a physical process that is distinct from the one that generates the UV/optical/near-infrared emission. No ultra-high-energy gamma-rays and no neutrino candidates consistent with the source were found in follow-up searches. These observations support the hypothesis that GW170817 was produced by the merger of two neutron stars in NGC4993 followed by a short gamma-ray burst (GRB 170817A) and a kilonova/macronova powered by the radioactive decay of r-process nuclei synthesized in the ejecta.openAbbott, 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.L.; Cabero, M.; Cadonati, L.; Cagnoli, G.; Cahillane, C.; Calderón Bustillo, J.; Callister, T.A.; Calloni, E.; Camp, J.B.; Canepa, M.; Canizares, P.; Cannon, K.C.; Cao, H.; Cao, J.; Capano, C.D.; Capocasa, E.; Carbognani, F.; Caride, S.; Carney, M.F.; Casanueva Diaz, J.; Casentini, C.; Caudill, S.; Cavaglià, M.; Cavalier, F.; Cavalieri, R.; Cella, G.; Cepeda, C.B.; Cerdá-Durán, P.; Cerretani, G.; Cesarini, E.; Chamberlin, S.J.; Chan, M.; Chao, S.; Charlton, P.; Chase, E.; Chassande-Mottin, E.; Chatterjee, D.; Chatziioannou, K.; Cheeseboro, B.D.; Chen, H.Y.; Chen, X.; Chen, Y.; Cheng, H.-P.; Chia, H.; Chincarini, A.; Chiummo, A.; Chmiel, T.; Cho, H.S.; Cho, M.; Chow, J.H.; Christensen, N.; Chu, Q.; Chua, A.J.K.; Chua, S.; Chung, A.K.W.; Chung, S.; Ciani, G.; Ciolfi, R.; Cirelli, C.E.; Cirone, A.; Clara, F.; Clark, J.A.; Clearwater, P.; Cleva, F.; Cocchieri, C.; Coccia, E.; Cohadon, P.-F.; Cohen, D.; Colla, A.; Collette, C.G.; Cominsky, L.R.; Constancio, M.; Conti, L.; Cooper, S.J.; Corban, P.; Corbitt, T.R.; Cordero-Carrión, I.; Corley, K.R.; Cornish, N.; Corsi, A.; Cortese, S.; Costa, C.A.; Coughlin, M.W.; Coughlin, S.B.; Coulon, J.-P.; Countryman, S.T.; Couvares, P.; Covas, P.B.; Cowan, E.E.; Coward, D.M.; Cowart, M.J.; Coyne, D.C.; Coyne, R.; Creighton, J.D.E.; Creighton, T.D.; Cripe, J.; Crowder, S.G.; Cullen, T.J.; Cumming, A.; Cunningham, L.; Cuoco, E.; Dal Canton, T.; Dálya, G.; Danilishin, S.L.; D'Antonio, S.; Danzmann, K.; Dasgupta, A.; Da Silva Costa, C.F.; Dattilo, V.; Dave, I.; Davier, M.; Davis, D.; Daw, E.J.; Day, B.; De, S.; DeBra, D.; Degallaix, J.; De Laurentis, M.; Deléglise, S.; Del Pozzo, W.; Demos, N.; Denker, T.; Dent, T.; De Pietri, R.; Dergachev, V.; De Rosa, R.; DeRosa, R.T.; De Rossi, C.; DeSalvo, R.; De Varona, O.; Devenson, J.; Dhurandhar, S.; Díaz, M.C.; Di Fiore, L.; Di Giovanni, M.; Di Girolamo, T.; Di Lieto, A.; Di Pace, S.; Di Palma, I.; Di Renzo, F.; Doctor, Z.; Dolique, V.; Donovan, F.; Dooley, K.L.; Doravari, S.; Dorrington, I.; Douglas, R.; Dovale Álvarez, M.; Downes, T.P.; Drago, M.; Dreissigacker, C.; Driggers, J.C.; Du, Z.; Ducrot, M.; Dupej, P.; Dwyer, S.E.; Edo, T.B.; Edwards, M.C.; Effler, A.; Eggenstein, H.-B.; Ehrens, P.; Eichholz, J.; Eikenberry, S.S.; Eisenstein, R.A.; Essick, R.C.; Estevez, D.; Etienne, Z.B.; Etzel, T.; Evans, M.; Evans, T.M.; Factourovich, M.; Fafone, V.; Fair, H.; Fairhurst, S.; Fan, X.; Farinon, S.; Farr, B.; Farr, W.M.; Fauchon-Jones, E.J.; Favata, M.; Fays, M.; Fee, C.; Fehrmann, H.; Feicht, J.; Fejer, M.M.; Fernandez-Galiana, A.; Ferrante, I.; Ferreira, E.C.; Ferrini, F.; Fidecaro, F.; Finstad, D.; Fiori, I.; Fiorucci, D.; Fishbach, M.; Fisher, R.P.; Fitz-Axen, M.; Flaminio, R.; Fletcher, M.; Fong, H.; Font, J.A.; Forsyth, P.W.F.; Forsyth, S.S.; Fournier, J.-D.; Frasca, S.; Frasconi, F.; Frei, Z.; Freise, A.; Frey, R.; Frey, V.; Fries, E.M.; Fritschel, P.; Frolov, V.V.; Fulda, P.; Fyffe, M.; Gabbard, H.; Gadre, B.U.; Gaebel, S.M.; Gair, J.R.; Gammaitoni, L.; Ganija, M.R.; Gaonkar, S.G.; Garcia-Quiros, C.; Garufi, F.; Gateley, B.; Gaudio, S.; Gaur, G.; Gayathri, V.; Gehrels, N.; Gemme, G.; Genin, E.; Gennai, A.; George, D.; George, J.; Gergely, L.; Germain, V.; Ghonge, S.; Ghosh, Abhirup; Ghosh, Archisman; Ghosh, S.; Giaime, J.A.; Giardina, K.D.; Giazotto, A.; Gill, K.; Glover, L.; Goetz, E.; Goetz, R.; Gomes, S.; Goncharov, B.; González, G.; Gonzalez Castro, J.M.; Gopakumar, A.; Gorodetsky, M.L.; Gossan, S.E.; Gosselin, M.; Gouaty, R.; Grado, A.; Graef, C.; Granata, M.; Grant, A.; Gras, S.; Gray, C.; Greco, G.; Green, A.C.; Gretarsson, E.M.; Griswold, B.; Groot, P.; Grote, H.; Grunewald, S.; Gruning, P.; Guidi, G.M.; Guo, X.; Gupta, A.; Gupta, M.K.; Gushwa, K.E.; Gustafson, E.K.; Gustafson, R.; Halim, O.; Hall, B.R.; Hall, E.D.; Hamilton, E.Z.; Hammond, G.; Haney, M.; Hanke, M.M.; Hanks, J.; Hanna, C.; Hannam, M.D.; Hannuksela, O.A.; Hanson, J.; Hardwick, T.; Harms, J.; Harry, G.M.; Harry, I.W.; Hart, M.J.; Haster, C.-J.; Haughian, K.; Healy, J.; Heidmann, A.; Heintze, M.C.; Heitmann, H.; Hello, P.; Hemming, G.; Hendry, M.; Heng, I.S.; Hennig, J.; Heptonstall, A.W.; Heurs, M.; Hild, S.; Hinderer, T.; Hoak, D.; Hofman, D.; Holt, K.; Holz, D.E.; Hopkins, P.; Horst, C.; Hough, J.; Houston, E.A.; Howell, E.J.; Hreibi, A.; Hu, Y.M.; Huerta, E.A.; Huet, D.; Hughey, B.; Husa, S.; Huttner, S.H.; Huynh-Dinh, T.; Indik, N.; Inta, R.; Intini, G.; Isa, H.N.; Isac, J.-M.; Isi, M.; Iyer, B.R.; Izumi, K.; Jacqmin, T.; Jani, K.; Jaranowski, P.; Jawahar, S.; Jiménez-Forteza, F.; Johnson, W.W.; Jones, D.I.; Jones, R.; Jonker, R.J.G.; Ju, L.; Junker, J.; Kalaghatgi, C.V.; Kalogera, V.; Kamai, B.; Kandhasamy, S.; Kang, G.; Kanner, J.B.; Kapadia, S.J.; Karki, S.; Karvinen, K.S.; Kasprzack, M.; Katolik, M.; Katsavounidis, E.; Katzman, W.; Kaufer, S.; Kawabe, K.; Kéfélian, F.; Keitel, D.; Kemball, A.J.; Kennedy, R.; Kent, C.; Key, J.S.; Khalili, F.Y.; Khan, I.; Khan, S.; Khan, Z.; Khazanov, E.A.; Kijbunchoo, N.; Kim, Chunglee; Kim, J.C.; Kim, K.; Kim, W.; Kim, W.S.; Kim, Y.-M.; Kimbrell, S.J.; King, E.J.; King, P.J.; Kinley-Hanlon, M.; Kirchhoff, R.; Kissel, J.S.; Kleybolte, L.; Klimenko, S.; Knowles, T.D.; Koch, P.; Koehlenbeck, S.M.; Koley, S.; Kondrashov, V.; Kontos, A.; Korobko, M.; Korth, W.Z.; Kowalska, I.; Kozak, D.B.; Krämer, C.; Kringel, V.; Krishnan, B.; Królak, A.; Kuehn, G.; Kumar, P.; Kumar, R.; Kumar, S.; Kuo, L.; Kutynia, A.; Kwang, S.; Lackey, B.D.; Lai, K.H.; Landry, M.; Lang, R.N.; Lange, J.; Lantz, B.; Lanza, R.K.; Larson, S.L.; Lartaux-Vollard, A.; Lasky, P.D.; Laxen, M.; Lazzarini, A.; Lazzaro, C.; Leaci, P.; Leavey, S.; Lee, C.H.; Lee, H.K.; Lee, H.M.; Lee, H.W.; Lee, K.; Lehmann, J.; Lenon, A.; Leonardi, M.; Leroy, N.; Letendre, N.; Levin, Y.; Li, T.G.F.; Linker, S.D.; Littenberg, T.B.; Liu, J.; Lo, R.K.L.; Lockerbie, N.A.; London, L.T.; Lord, J.E.; Lorenzini, M.; Loriette, V.; Lormand, M.; Losurdo, G.; Lough, J.D.; Lousto, C.O.; Lovelace, G.; Lück, H.; Lumaca, D.; Lundgren, A.P.; Lynch, R.; Ma, Y.; Macas, R.; Macfoy, S.; Machenschalk, B.; MacInnis, M.; Macleod, D.M.; Magaña Hernandez, I.; Magaña-Sandoval, F.; Magaña Zertuche, L.; Magee, R.M.; Majorana, E.; Maksimovic, I.; Man, N.; Mandic, V.; Mangano, V.; Mansell, G.L.; Manske, M.; Mantovani, M.; Marchesoni, F.; Marion, F.; Márka, S.; Márka, Z.; Markakis, C.; Markosyan, A.S.; Markowitz, A.; Maros, E.; Marquina, A.; Marsh, P.; Martelli, F.; Martellini, L.; Martin, I.W.; Martin, R.M.; Martynov, D.V.; Mason, K.; Massera, E.; Masserot, A.; Massinger, T.J.; Masso-Reid, M.; Mastrogiovanni, S.; Matas, A.; Matichard, F.; Matone, L.; Mavalvala, N.; Mazumder, N.; McCarthy, R.; McClelland, D.E.; McCormick, S.; McCuller, L.; McGuire, S.C.; McIntyre, G.; McIver, J.; McManus, D.J.; McNeill, L.; McRae, T.; McWilliams, S.T.; Meacher, D.; Meadors, G.D.; Mehmet, M.; Meidam, J.; Mejuto-Villa, E.; Melatos, A.; Mendell, G.; Mercer, R.A.; Merilh, E.L.; Merzougui, M.; Meshkov, S.; Messenger, C.; Messick, C.; Metzdorff, R.; Meyers, P.M.; Miao, H.; Michel, C.; Middleton, H.; Mikhailov, E.E.; Milano, L.; Miller, A.L.; Miller, B.B.; Miller, J.; Millhouse, M.; Milovich-Goff, M.C.; Minazzoli, O.; Minenkov, Y.; Ming, J.; Mishra, C.; Mitra, S.; Mitrofanov, V.P.; Mitselmakher, G.; Mittleman, R.; Moffa, D.; Moggi, A.; Mogushi, K.; Mohan, M.; Mohapatra, S.R.P.; Montani, M.; Moore, C.J.; Moraru, D.; Moreno, G.; Morriss, S.R.; Mours, B.; Mow-Lowry, C.M.; Mueller, G.; Muir, A.W.; Mukherjee, Arunava; Mukherjee, D.; Mukherjee, S.; Mukund, N.; Mullavey, A.; Munch, J.; Muñiz, E.A.; Muratore, M.; Murray, P.G.; Napier, K.; Nardecchia, I.; Naticchioni, L.; Nayak, R.K.; Neilson, J.; Nelemans, G.; Nelson, T.J.N.; Nery, M.; Neunzert, A.; Nevin, L.; Newport, J.M.; Newton, G.; Ng, K.K.Y.; Nguyen, P.; Nguyen, T.T.; Nichols, D.; Nielsen, A.B.; Nissanke, S.; Nitz, A.; Noack, A.; Nocera, F.; Nolting, D.; North, C.; Nuttall, L.K.; Oberling, J.; O'Dea, G.D.; Ogin, G.H.; Oh, J.J.; Oh, S.H.; Ohme, F.; Okada, M.A.; 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Puncken, O.; Punturo, M.; Puppo, P.; Pürrer, M.; Qi, H.; Quetschke, V.; Quintero, E.A.; Quitzow-James, R.; Raab, F.J.; Rabeling, D.S.; Radkins, H.; Raffai, P.; Raja, S.; Rajan, C.; Rajbhandari, B.; Rakhmanov, M.; Ramirez, K.E.; Ramos-Buades, A.; Rapagnani, P.; Raymond, V.; Razzano, M.; Read, J.; Regimbau, T.; Rei, L.; Reid, S.; Reitze, D.H.; Ren, W.; Reyes, S.D.; Ricci, F.; Ricker, P.M.; Rieger, S.; Riles, K.; Rizzo, M.; Robertson, N.A.; Robie, R.; Robinet, F.; Rocchi, A.; Rolland, L.; Rollins, J.G.; Roma, V.J.; Romano, R.; Romel, C.L.; Romie, J.H.; Rosinska, D.; Ross, M.P.; Rowan, S.; Rüdiger, A.; Ruggi, P.; Rutins, G.; Ryan, K.; Sachdev, S.; Sadecki, T.; Sadeghian, L.; Sakellariadou, M.; Salconi, L.; Saleem, M.; Salemi, F.; Samajdar, A.; Sammut, L.; Sampson, L.M.; Sanchez, E.J.; Sanchez, L.E.; Sanchis-Gual, N.; Sandberg, V.; Sanders, J.R.; Sassolas, B.; Sathyaprakash, B.S.; Saulson, P.R.; Sauter, O.; Savage, R.L.; Sawadsky, A.; Schale, P.; Scheel, M.; Scheuer, J.; Schmidt, J.; Schmidt, P.; 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Multi-messenger observations of a binary neutron star merger
No full text3614sinoneOn 2017 August 17 a binary neutron star coalescence candidate (later designated GW170817) with merger time 12:41:04 UTC was observed through gravitational waves by the Advanced LIGO and Advanced Virgo detectors. The Fermi Gamma-ray Burst Monitor independently detected a gamma-ray burst (GRB 170817A) with a time delay of ~1.7 s with respect to the merger time. From the gravitational-wave signal, the source was initially localized to a sky region of 31 deg2 at a luminosity distance of 40 8 8-+ Mpc and with component masses consistent with neutron stars. The component masses were later measured to be in the range 0.86 to 2.26 M. An extensive observing campaign was launched across the electromagnetic spectrum leading to the discovery of a bright optical transient (SSS17a, now with the IAU identification of AT 2017gfo) in NGC 4993 (at ~40 Mpc) less than 11 hours after the merger by the One-Meter, Two Hemisphere (1M2H) team using the 1 m Swope Telescope. The optical transient was independently detected by multiple teams within an hour. Subsequent observations targeted the object and its environment. Early ultraviolet observations revealed a blue transient that faded within 48 hours. Optical and infrared observations showed a redward evolution over ~10 days. Following early non-detections, X-ray and radio emission were discovered at the transient's position ~9 and ~16 days, respectively, after the merger. Both the X-ray and radio emission likely arise from a physical process that is distinct from the one that generates the UV/optical/near-infrared emission. No ultra-high-energy gamma-rays and no neutrino candidates consistent with the source were found in follow-up searches. These observations support the hypothesis that GW170817 was produced by the merger of two neutron stars in NGC4993 followed by a short gamma-ray burst (GRB 170817A) and a kilonova/macronova powered by the radioactive decay of r-process nuclei synthesized in the ejecta.openAbbott, 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.; 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Multi-messenger observations of a binary neutron star merger
No full text3614siOn 2017 August 17 a binary neutron star coalescence candidate (later designated GW170817) with merger time 12:41:04 UTC was observed through gravitational waves by the Advanced LIGO and Advanced Virgo detectors. The Fermi Gamma-ray Burst Monitor independently detected a gamma-ray burst (GRB 170817A) with a time delay of ∼ 1.7 {{s}} with respect to the merger time. From the gravitational-wave signal, the source was initially localized to a sky region of 31 deg2 at a luminosity distance of {40}-8+8 Mpc and with component masses consistent with neutron stars. The component masses were later measured to be in the range 0.86 to 2.26 {M}ȯ . An extensive observing campaign was launched across the electromagnetic spectrum leading to the discovery of a bright optical transient (SSS17a, now with the IAU identification of AT 2017gfo) in NGC 4993 (at ∼ 40 {{Mpc}}) less than 11 hours after the merger by the One-Meter, Two Hemisphere (1M2H) team using the 1 m Swope Telescope. The optical transient was independently detected by multiple teams within an hour. Subsequent observations targeted the object and its environment. Early ultraviolet observations revealed a blue transient that faded within 48 hours. Optical and infrared observations showed a redward evolution over ∼10 days. Following early non-detections, X-ray and radio emission were discovered at the transient's position ∼ 9 and ∼ 16 days, respectively, after the merger. Both the X-ray and radio emission likely arise from a physical process that is distinct from the one that generates the UV/optical/near-infrared emission. No ultra-high-energy gamma-rays and no neutrino candidates consistent with the source were found in follow-up searches. These observations support the hypothesis that GW170817 was produced by the merger of two neutron stars in NGC 4993 followed by a short gamma-ray burst (GRB 170817A) and a kilonova/macronova powered by the radioactive decay of r-process nuclei synthesized in the ejecta.openopenAbbott, 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.; 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Hadron Physics Opportunities at FAIR
No full textInternational audienceThis White Paper outlines a coordinated, decade-spanning programme of hadron and QCD studies anchored at the GSI/FAIR accelerator complex. Profiting from intense deuteron, proton and pion beams coupled with high-rate capable detectors and an international theory effort, the initiative addresses fundamental questions related to the strong interaction featuring confinement and dynamical mass generation. This includes our understanding of hadron-hadron interactions and the composition of hadrons through mapping the baryon and meson spectra, including exotic states, and quantifying hadron structure. This interdisciplinary research connects topics in the fields of nuclear, heavy-ion, and (nuclear) astro (particle) physics, linking, for example, terrestrial data to constraints on neutron star structure. A phased roadmap with SIS100 accelerator start-up and envisaged detector upgrades will yield precision cross sections, transition form factors, in-medium spectral functions, and validated theory inputs. Synergies with external programmes at international accelerator facilities worldwide are anticipated. The programme is expected to deliver decisive advances in our understanding of non-perturbative (strong) QCD and astrophysics, and high-rate detector and data-science technology
Hadron Physics Opportunities at FAIR
No full textInternational audienceThis White Paper outlines a coordinated, decade-spanning programme of hadron and QCD studies anchored at the GSI/FAIR accelerator complex. Profiting from intense deuteron, proton and pion beams coupled with high-rate capable detectors and an international theory effort, the initiative addresses fundamental questions related to the strong interaction featuring confinement and dynamical mass generation. This includes our understanding of hadron-hadron interactions and the composition of hadrons through mapping the baryon and meson spectra, including exotic states, and quantifying hadron structure. This interdisciplinary research connects topics in the fields of nuclear, heavy-ion, and (nuclear) astro (particle) physics, linking, for example, terrestrial data to constraints on neutron star structure. A phased roadmap with SIS100 accelerator start-up and envisaged detector upgrades will yield precision cross sections, transition form factors, in-medium spectral functions, and validated theory inputs. Synergies with external programmes at international accelerator facilities worldwide are anticipated. The programme is expected to deliver decisive advances in our understanding of non-perturbative (strong) QCD and astrophysics, and high-rate detector and data-science technology
Hadron Physics Opportunities at FAIR
No full textInternational audienceThis White Paper outlines a coordinated, decade-spanning programme of hadron and QCD studies anchored at the GSI/FAIR accelerator complex. Profiting from intense deuteron, proton and pion beams coupled with high-rate capable detectors and an international theory effort, the initiative addresses fundamental questions related to the strong interaction featuring confinement and dynamical mass generation. This includes our understanding of hadron-hadron interactions and the composition of hadrons through mapping the baryon and meson spectra, including exotic states, and quantifying hadron structure. This interdisciplinary research connects topics in the fields of nuclear, heavy-ion, and (nuclear) astro (particle) physics, linking, for example, terrestrial data to constraints on neutron star structure. A phased roadmap with SIS100 accelerator start-up and envisaged detector upgrades will yield precision cross sections, transition form factors, in-medium spectral functions, and validated theory inputs. Synergies with external programmes at international accelerator facilities worldwide are anticipated. The programme is expected to deliver decisive advances in our understanding of non-perturbative (strong) QCD and astrophysics, and high-rate detector and data-science technology
