939 results on '"GREEN, DAVID"'
Search Results
2. A Scientific Approach to Addressing Social Issues Using Administrative Data
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Green, David, Simard-Duplain, Gaëlle, Sweetman, Arthur, and Warburton, William
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- 2023
3. A Reanalysis of "The Town with No Poverty: The Health Effects of a Canadian Guaranteed Annual Income Field Experiment"
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Green, David A.
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- 2023
4. “A vibrant life force”: A Review Essay on Black Queer Flesh: Rejecting Subjectivity in the African American Novel
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Green, David B.
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- 2023
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5. Getting a foot in the door
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Green, David
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- 2024
6. Manganese Oxide Minerals from Veins in the Leinster Granite
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Moreton, Stephen, Green, David I., and Tindle, Andrew G.
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- 2022
7. Sir Keith Holyoake: Towards a Political Biography ed. by Margaret Clark (review)
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Green, David
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- 2022
8. Ultrasoft state of microquasar Cygnus X-3: X-ray polarimetry reveals the geometry of astronomical puzzle
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Veledina, Alexandra, Poutanen, Juri, Bocharova, Anastasiia, Di Marco, Alessandro, Forsblom, Sofia V., La Monaca, Fabio, Podgorny, Jakub, Tsygankov, Sergey S., Zdziarski, Andrzej A., Ahlberg, Varpu, Green, David A., Muleri, Fabio, Rhodes, Lauren, Bianchi, Stefano, Costa, Enrico, Dovciak, Michal, Loktev, Vladislav, McCollough, Michael, Soffitta, Paolo, and Sunyaev, Rashid
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Astrophysics - High Energy Astrophysical Phenomena ,Astrophysics - Solar and Stellar Astrophysics - Abstract
Cygnus X-3 is an enigmatic X-ray binary, that is both an exceptional accreting system and a cornerstone for the population synthesis studies. Prominent X-ray and radio properties follow a well-defined pattern, yet the physical reasons for the state changes observed in this system are not known. Recently, the presence of an optically thick envelope around the central source in the hard state was revealed using the X-ray polarization data obtained with Imaging X-ray Polarimetry Explorer (IXPE). In this work, we analyse IXPE data obtained in the ultrasoft (radio quenched) state of the source. The average polarization degree (PD) of $11.9\pm0.5\%$ at a polarization angle (PA) of $94^{\circ}\pm1^{\circ}$ is inconsistent with the simple geometry of the accretion disc viewed at an intermediate inclination. The high PD, the blackbody-like spectrum, and the weakness of fluorescent iron line imply that the central source is hidden behind the optically thick outflow and its beamed radiation is scattered towards our line of sight. In this picture the observed PD is directly related to the source inclination, which we conservatively determine to lie in the range $26^{\circ}
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- 2024
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9. Geophysical Observations of the 24 September 2023 OSIRIS-REx Sample Return Capsule Re-Entry
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Silber, Elizabeth A., Bowman, Daniel C., Carr, Chris G., Eisenberg, David P., Elbing, Brian R., Fernando, Benjamin, Garcés, Milton A., Haaser, Robert, Krishnamoorthy, Siddharth, Langston, Charles A., Nishikawa, Yasuhiro, Webster, Jeremy, Anderson, Jacob F., Arrowsmith, Stephen, Bazargan, Sonia, Beardslee, Luke, Beck, Brant, Bishop, Jordan W., Blom, Philip, Bracht, Grant, Chichester, David L., Christe, Anthony, Cummins, Kenneth, Cutts, James, Danielson, Lisa, Donahue, Carly, Eack, Kenneth, Fleigle, Michael, Fox, Douglas, Goel, Ashish, Green, David, Hasumi, Yuta, Hayward, Chris, Hicks, Dan, Hix, Jay, Horton, Stephen, Hough, Emalee, Huber, David P., Hunt, Madeline A., Inman, Jennifer, Islam, S. M. Ariful, Izraelevitz, Jacob, Jacob, Jamey D., Clarke, Jacob, Johnson, James, KC, Real J., Komjathy, Attila, Lam, Eric, LaPierre, Justin, Lewis, Kevin, Lewis, Richard D., Liu, Patrick, Martire, Léo, McCleary, Meaghan, McGhee, Elisa A., Mitra, Ipsita, Nag, Amitabh, Giraldo, Luis Ocampo, Pearson, Karen, Plaisir, Mathieu, Popenhagen, Sarah K., Rassoul, Hamid, Giannone, Miro Ronac, Samnani, Mirza, Schmerr, Nicholas, Spillman, Kate, Srinivas, Girish, Takazawa, Samuel K., Tempert, Alex, Turley, Reagan, Van Beek, Cory, Viens, Loïc, Walsh, Owen A., Weinstein, Nathan, White, Robert, Williams, Brian, Wilson, Trevor C., Wyckoff, Shirin, Yamamoto, Masa-yuki, Yap, Zachary, Yoshiyama, Tyler, and Zeiler, Cleat
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Astrophysics - Earth and Planetary Astrophysics ,Astrophysics - Instrumentation and Methods for Astrophysics ,Physics - Geophysics - Abstract
Sample Return Capsules (SRCs) entering Earth's atmosphere at hypervelocity from interplanetary space are a valuable resource for studying meteor phenomena. The 24 September 2023 arrival of the OSIRIS-REx (Origins, Spectral Interpretation, Resource Identification, and Security-Regolith Explorer) SRC provided an unprecedented chance for geophysical observations of a well-characterized source with known parameters, including timing and trajectory. A collaborative effort involving researchers from 16 institutions executed a carefully planned geophysical observational campaign at strategically chosen locations, deploying over 400 ground-based sensors encompassing infrasound, seismic, distributed acoustic sensing (DAS), and GPS technologies. Additionally, balloons equipped with infrasound sensors were launched to capture signals at higher altitudes. This campaign (the largest of its kind so far) yielded a wealth of invaluable data anticipated to fuel scientific inquiry for years to come. The success of the observational campaign is evidenced by the near-universal detection of signals across instruments, both proximal and distal. This paper presents a comprehensive overview of the collective scientific effort, field deployment, and preliminary findings. The early findings have the potential to inform future space missions and terrestrial campaigns, contributing to our understanding of meteoroid interactions with planetary atmospheres. Furthermore, the dataset collected during this campaign will improve entry and propagation models as well as augment the study of atmospheric dynamics and shock phenomena generated by meteoroids and similar sources., Comment: 87 pages, 14 figures
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- 2024
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10. Emergence of a radio jet in the changing-look AGN 1ES 1927+654
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Meyer, Eileen T., Laha, Sibasish, Shuvo, Onic I., Roychowdhury, Agniva, Green, David A., Rhodes, Lauren, Hankla, Amelia M., Philippov, Alexander, Mbarek, Rostom, laor, Ari, Begelman, Mitchell C., Sadaula, Dev R., Ghosh, Ritesh, Bruni, Gabriele, Panessa, Francesca, Guainazzi, Matteo, Behar, Ehud, Masterson, Megan, Zhang, Haocheng, Yang, Xiaolong, Gurwell, Mark A., Keating, Garrett K., Williams-Baldwin, David, Bray, Justin D., Bempong-Manful, Emmanuel K., Wrigley, Nicholas, Bianchi, Stefano, Ricci, Federica, La Franca, Fabio, Kara, Erin, Georganopoulos, Markos, Oates, Samantha, Nicholl, Matt, Pal, Main, and Cenko, S. Bradley
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Astrophysics - High Energy Astrophysical Phenomena ,Astrophysics - Astrophysics of Galaxies - Abstract
We present multi-frequency (5-345 GHz) and multi-resolution radio observations of 1ES 1927+654, widely considered one of the most unusual and extreme changing-look active galactic nuclei (CL-AGN). The source was first designated a CL-AGN after an optical outburst in late 2017 and has since displayed considerable changes in X-ray emission, including the destruction and rebuilding of the X-ray corona in 2019-2020. Radio observations prior to 2023 show a faint and compact radio source not unusual for radio-quiet AGN. Starting in February 2023, 1ES 1927+654 began exhibiting a radio flare with a steep exponential rise, reaching a peak 60 times previous flux levels, and has maintained this higher level of radio emission for nearly a year. The 5-23 GHz spectrum is broadly similar to gigahertz-peaked radio sources, which are understood to be young radio jets less than ~1000 years old. Recent high-resolution VLBA observations at 23.5 GHz now show resolved extensions on either side of the core, with a separation of 0.14 pc, consistent with a new and mildly relativistic bipolar outflow. A steady increase in the soft X-ray band (0.3-2 keV) concurrent with the radio may be consistent with jet-driven shocked gas, though further observations are needed to test alternate scenarios. This source joins a growing number of CL-AGN and tidal disruption events which show late-time radio activity, years after the initial outburst., Comment: Submitted to ApJ Letters 24 June 2023. 15 pages, 4 figures, 1 table
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- 2024
11. An IXPE-Led X-ray Spectro-Polarimetric Campaign on the Soft State of Cygnus X-1: X-ray Polarimetric Evidence for Strong Gravitational Lensing
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Steiner, James F., Nathan, Edward, Hu, Kun, Krawczynski, Henric, Dovciak, Michal, Veledina, Alexandra, Muleri, Fabio, Svoboda, Jiri, Alabarta, Kevin, Parra, Maxime, Bhargava, Yash, Matt, Giorgio, Poutanen, Juri, Petrucci, Pierre-Olivier, Tennant, Allyn F., Baglio, M. Cristina, Baldini, Luca, Barnier, Samuel, Bhattacharyya, Sudip, Bianchi, Stefano, Brigitte, Maimouna, Cabezas, Mauricio, Cangemi, Floriane, Capitanio, Fiamma, Casey, Jacob, Cavero, Nicole Rodriguez, Castellano, Simone, Cavazzuti, Elisabetta, Chun, Sohee, Churazov, Eugene, Costa, Enrico, Di Lalla, Niccolo, Di Marco, Alessandro, Egron, Elise, Ewing, Melissa, Fabiani, Sergio, Garcia, Javier A., Green, David A., Grinberg, Victoria, Hadrava, Petr, Ingram, Adam, Kaaret, Philip, Kislat, Fabian, Kitaguchi, Takao, Kravtsov, Vadim, Kubatova, Brankica, La Monaca, Fabio, Latronico, Luca, Loktev, Vladislav, Malacaria, Christian, Marin, Frederic, Marinucci, Andrea, Maryeva, Olga, Mastroserio, Guglielmo, Mizuno, Tsunefumi, Negro, Michela, Omodei, Nicola, Podgorny, Jakub, Rankin, John, Ratheesh, Ajay, Rhodes, Lauren, Russell, David M., Slechta, Miroslav, Soffitta, Paolo, Spooner, Sean, Suleimanov, Valery, Tombesi, Francesco, Trushkin, Sergei A., Weisskopf, Martin C., Zane, Silvia, Zdziarski, Andrzej A., Zhang, Sixuan, Zhang, Wenda, Zhou, Menglei, Agudo, Ivan, Antonelli, Lucio A., Bachetti, Matteo, Baumgartner, Wayne H., Bellazzini, Ronaldo, Bongiorno, Stephen D., Bonino, Raffaella, Brez, Alessandro, Bucciantini, Niccolo, Chen, Chien-Ting, Ciprini, Stefano, De Rosa, Alessandra, Del Monte, Ettore, Di Gesu, Laura, Donnarumma, Immacolata, Doroshenko, Victor, Ehlert, Steven R., Enoto, Teruaki, Evangelista, Yuri, Ferrazzoli, Riccardo, Gunji, Shuichi, Hayashida, Kiyoshi, Heyl, Jeremy, Iwakiri, Wataru, Jorstad, Svetlana G., Karas, Vladimir, Kolodziejczak, Jeffery J., Liodakis, Ioannis, Maldera, Simone, Manfreda, Alberto, Marscher, Alan P., Marshall, Herman L., Massaro, Francesco, Mitsuishi, Ikuyuki, Ng, Chi-Yung, O'Dell, Stephen L., Oppedisano, Chiara, Papitto, Alessandro, Pavlov, George G., Peirson, Abel L., Perri, Matteo, Pesce-Rollins, Melissa, Pilia, Maura, Possenti, Andrea, Puccetti, Simonetta, Ramsey, Brian D., Roberts, Oliver J., Romani, Roger W., Sgro, Carmelo, Slane, Patrick, Spandre, Gloria, Swartz, Douglas A., Tamagawa, Toru, Tavecchio, Fabrizio, Taverna, Roberto, Tawara, Yuzuru, Thomas, Nicholas E., Trois, Alessio, Tsygankov, Sergey S., Turolla, Roberto, Vink, Jacco, Wu, Kinwah, and Xie, Fei
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Astrophysics - High Energy Astrophysical Phenomena - Abstract
We present the first X-ray spectropolarimetric results for Cygnus X-1 in its soft state from a campaign of five IXPE observations conducted during 2023 May-June. Companion multiwavelength data during the campaign are likewise shown. The 2-8 keV X-rays exhibit a net polarization degree PD=1.99%+/-0.13% (68% confidence). The polarization signal is found to increase with energy across IXPE's 2-8 keV bandpass. The polarized X-rays exhibit an energy-independent polarization angle of PA=-25.7+/-1.8 deg. East of North (68% confidence). This is consistent with being aligned to Cyg X-1's AU-scale compact radio jet and its pc-scale radio lobes. In comparison to earlier hard-state observations, the soft state exhibits a factor of 2 lower polarization degree, but a similar trend with energy and a similar (also energy-independent) position angle. When scaling by the natural unit of the disk temperature, we find the appearance of a consistent trendline in the polarization degree between soft and hard states. Our favored polarimetric model indicates Cyg X-1's spin is likely high (a* above ~0.96). The substantial X-ray polarization in Cyg X-1's soft state is most readily explained as resulting from a large portion of X-rays emitted from the disk returning and reflecting off the disk surface, generating a high polarization degree and a polarization direction parallel to the black hole spin axis and radio jet. In IXPE's bandpass, the polarization signal is dominated by the returning reflection emission. This constitutes polarimetric evidence for strong gravitational lensing of X-rays close to the black hole., Comment: 20 pages, accepted for publication in ApJL
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- 2024
12. Brightening and Fading in the Youngest Galactic Supernova Remnant G1.9+0.3: 13 years of monitoring with the Chandra X-ray Observatory
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Borkowski, Kazimierz J., Reynolds, Stephen P., Petre, Robert, and Green, David A.
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Astrophysics - High Energy Astrophysical Phenomena - Abstract
We report results from 13 years of Chandra monitoring of nonthermal X-ray emission from the youngest Galactic supernova remnant G1.9+0.3, the only remnant known to be increasing in brightness. We confirm the spatially-integrated flux increase rate of $(1.2 \pm 0.2)$% yr$^{-1}$ between 1 and 7 keV, but find large spatial variations, from decreases of $-3$% yr$^{-1}$ to increases of 7% yr$^{-1}$, over length scales as small as $10''$ or smaller. We observe relatively little change in spectral slope, though one region shows significant hardening (photon index $\Delta \Gamma \sim 0.4$) as it brightens by 1% yr$^{-1}$. Such rates of change can be accommodated by any of several explanations, including steady evolution of the blast wave, expansion or compression of discrete plasma blobs, strong magnetic turbulence, or variations in magnetic-field aspect angle. Our results do not constrain the mean magnetic-field strength, but a self-consistent picture of the spatially averaged rate of increase can be produced in which the maximum energies of accelerated particles are limited by the remnant age (applying both to electrons and to ions) to about 20 TeV, and the remnant-averaged magnetic field strength is about 30 $\mu$G. The deceleration parameter $m$ (average shock radius varying as $t^m$) is about 0.7, consistent with estimates from overall expansion dynamics, and confirming an explosion date of about 1900 CE. Shock-efficiency factors $\epsilon_e$ and $\epsilon_B$ (fractions of shock energy in relativistic electrons and magnetic field) are 0.003 and 0.0002 in this picture. However, the large range of rates of brightness change indicates that such a global model is oversimplified. Temporal variations of photon index, expected to be small but measurable with longer time baselines, can discriminate among possible models., Comment: 21 pages, 15 figures, submitted to ApJ
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- 2024
13. Sparse-grid Discontinuous Galerkin Methods for the Vlasov-Poisson-Lenard-Bernstein Model
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Schnake, Stefan, Kendrick, Coleman, Endeve, Eirik, Stoyanov, Miroslav, Hahn, Steven, Hauck, Cory D, Green, David L, Snyder, Phil, and Canik, John
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Mathematics - Numerical Analysis - Abstract
Sparse-grid methods have recently gained interest in reducing the computational cost of solving high-dimensional kinetic equations. In this paper, we construct adaptive and hybrid sparse-grid methods for the Vlasov-Poisson-Lenard-Bernstein (VPLB) model. This model has applications to plasma physics and is simulated in two reduced geometries: a 0x3v space homogeneous geometry and a 1x3v slab geometry. We use the discontinuous Galerkin (DG) method as a base discretization due to its high-order accuracy and ability to preserve important structural properties of partial differential equations. We utilize a multiwavelet basis expansion to determine the sparse-grid basis and the adaptive mesh criteria. We analyze the proposed sparse-grid methods on a suite of three test problems by computing the savings afforded by sparse-grids in comparison to standard solutions of the DG method. The results are obtained using the adaptive sparse-grid discretization library ASGarD.
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- 2024
14. Levin-Wen is a gauge theory: entanglement from topology
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Kawagoe, Kyle, Jones, Corey, Sanford, Sean, Green, David, and Penneys, David
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Condensed Matter - Strongly Correlated Electrons ,Mathematical Physics ,Mathematics - Category Theory ,Mathematics - Operator Algebras ,Mathematics - Quantum Algebra ,81V27, 18M30 (primary) 18M20, 46L60, 57R56, 81T05, 81T25 (secondary) - Abstract
We show that the Levin-Wen model of a unitary fusion category $\mathcal{C}$ is a gauge theory with gauge symmetry given by the tube algebra $\operatorname{Tube}(\mathcal{C})$. In particular, we define a model corresponding to a $\operatorname{Tube}(\mathcal{C})$ symmetry protected topological phase, and we provide a gauging procedure which results in the corresponding Levin-Wen model. In the case $\mathcal{C}=\mathsf{Hilb}(G,\omega)$, we show how our procedure reduces to the twisted gauging of a trivial $G$-SPT to produce the Twisted Quantum Double. We further provide an example which is outside the bounds of the current literature, the trivial Fibonacci SPT, whose gauge theory results in the doubled Fibonacci string-net. Our formalism has a natural topological interpretation with string diagrams living on a punctured sphere. We provide diagrams to supplement our mathematical proofs and to give the reader an intuitive understanding of the subject matter., Comment: 16 pages, 1 figure
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- 2024
15. Cygnus X-3 revealed as a Galactic ultraluminous X-ray source by IXPE
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Veledina, Alexandra, Muleri, Fabio, Poutanen, Juri, Podgorný, Jakub, Dovčiak, Michal, Capitanio, Fiamma, Churazov, Eugene, De Rosa, Alessandra, Di Marco, Alessandro, Forsblom, Sofia V., Kaaret, Philip, Krawczynski, Henric, La Monaca, Fabio, Loktev, Vladislav, Lutovinov, Alexander A., Molkov, Sergey V., Mushtukov, Alexander A., Ratheesh, Ajay, Rodriguez Cavero, Nicole, Steiner, James F., Sunyaev, Rashid A., Tsygankov, Sergey S., Weisskopf, Martin C., Zdziarski, Andrzej A., Bianchi, Stefano, Bright, Joe S., Bursov, Nikolaj, Costa, Enrico, Egron, Elise, Garcia, Javier A., Green, David A., Gurwell, Mark, Ingram, Adam, Kajava, Jari J. E., Kale, Ruta, Kraus, Alex, Malyshev, Denys, Marin, Frédéric, Matt, Giorgio, McCollough, Michael, Mereminskiy, Ilya A., Nizhelsky, Nikolaj, Piano, Giovanni, Pilia, Maura, Pittori, Carlotta, Rao, Ramprasad, Righini, Simona, Soffitta, Paolo, Shevchenko, Anton, Svoboda, Jiri, Tombesi, Francesco, Trushkin, Sergei A., Tsybulev, Peter, Ursini, Francesco, Wu, Kinwah, Agudo, Iván, Antonelli, Lucio A., Bachetti, Matteo, Baldini, Luca, Baumgartner, Wayne H., Bellazzini, Ronaldo, Bongiorno, Stephen D., Bonino, Raffaella, Brez, Alessandro, Bucciantini, Niccolò, Castellano, Simone, Cavazzuti, Elisabetta, Chen, Chien-Ting, Ciprini, Stefano, Del Monte, Ettore, Di Gesu, Laura, Di Lalla, Niccolò, Donnarumma, Immacolata, Doroshenko, Victor, Ehlert, Steven R., Enoto, Teruaki, Evangelista, Yuri, Fabiani, Sergio, Ferrazzoli, Riccardo, Gunji, Shuichi, Hayashida, Kiyoshi, Heyl, Jeremy, Iwakiri, Wataru, Jorstad, Svetlana G., Karas, Vladimir, Kislat, Fabian, Kitaguchi, Takao, Kolodziejczak, Jeffery J., Latronico, Luca, Liodakis, Ioannis, Maldera, Simone, Manfreda, Alberto, Marinucci, Andrea, Marscher, Alan P., Marshall, Herman L., Massaro, Francesco, Mitsuishi, Ikuyuki, Mizuno, Tsunefumi, Negro, Michela, Ng, Chi-Yung, O’Dell, Stephen L., Omodei, Nicola, Oppedisano, Chiara, Papitto, Alessandro, Pavlov, George G., Peirson, Abel L., Perri, Matteo, Pesce-Rollins, Melissa, Petrucci, Pierre-Olivier, Possenti, Andrea, Puccetti, Simonetta, Ramsey, Brian D., Rankin, John, Roberts, Oliver, Romani, Roger W., Sgrò, Carmelo, Slane, Patrick, Spandre, Gloria, Swartz, Doug, Tamagawa, Toru, Tavecchio, Fabrizio, Taverna, Roberto, Tawara, Yuzuru, Tennant, Allyn F., Thomas, Nicholas E., Trois, Alessio, Turolla, Roberto, Vink, Jacco, Xie, Fei, and Zane, Silvia
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- 2024
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16. Using computational approaches to enhance the interpretation of missense variants in the PAX6 gene
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Andhika, Nadya S., Biswas, Susmito, Hardcastle, Claire, Green, David J., Ramsden, Simon C., Birney, Ewan, Black, Graeme C., and Sergouniotis, Panagiotis I.
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- 2024
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17. Detection of the 2021 Outburst of RS Ophiuchi with the LST-1
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Kobayashi, Yukiho, Aguasca-Cabot, Arnau, Martín, María Isabel Bernardos, Green, David, and López-Coto, Rubén
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Astrophysics - High Energy Astrophysical Phenomena - Abstract
Novae are luminous explosions in close binaries which host a white dwarf and a companion donor star. They are triggered by a thermonuclear runaway when the white dwarf accretes a critical amount of matter from the secondary. Though novae are established as high-energy gamma-ray emitters through observations by the Fermi Large Area Telescope (LAT), the origin of the gamma-ray emission, whether it is hadronic or leptonic, had been under intense debate until very recently. RS Ophiuchi (RS Oph) is a well-known recurrent symbiotic nova with a recurrence time scale of 15 years. The most recent outburst of RS Oph in 2021 brought the first detection of very-high-energy (VHE) gamma rays from a nova ever. The first Large-Sized Telescope prototype (LST-1) of the Cherenkov Telescope Array observed this historic event along with H.E.S.S. and MAGIC. The LST-1 observations in the first days after the burst onset show a clear VHE gamma-ray signal from RS Oph. The low energy threshold of LST-1 allows us to reconstruct the RS Oph gamma-ray spectrum down to $\sim$30 GeV, providing the best connection of the VHE gamma-ray data to the Fermi LAT energy range. The results from the analysis of the LST-1 observations are consistent with those obtained with H.E.S.S. and MAGIC, and also support a hadronic origin for the observed gamma-ray fluxes. In this contribution, we will present the analysis results of the LST-1 observations of the 2021 outburst of RS Oph., Comment: Presented at the 38th International Cosmic Ray Conference (ICRC 2023), 2023 (arXiv:2309.08219)
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- 2023
18. Chasing Gravitational Waves with the Cherenkov Telescope Array
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Green, Jarred Gershon, Carosi, Alessandro, Nava, Lara, Patricelli, Barbara, Schüssler, Fabian, Seglar-Arroyo, Monica, Consortium, Cta, Abe, Kazuki, Abe, Shotaro, Acharyya, Atreya, Adam, Remi, Aguasca-Cabot, Arnau, Agudo, Ivan, Alfaro, Jorge, Alvarez-Crespo, Nuria, Batista, Rafael Alves, Amans, Jean-Philippe, Amato, Elena, Ambrosino, Filippo, Angüner, Ekrem Oguzhan, Antonelli, Lucio Angelo, Aramo, Carla, Arcaro, Cornelia, Arrabito, Luisa, Asano, Katsuaki, Aschersleben, Jann, Ashkar, Halim, Stuani, Luiz Augusto, Baack, Dominik, Backes, Michael, Balazs, Csaba, Balbo, Matteo, Larriva, Andres Baquero, Martins, Victor Barbosa, de Almeida, Ulisses Barres, Barrio, Juan Abel, Bastieri, Denis, Batista, Pedro Ivo, Batković, Ivana, Batzofin, Rowan William, Baxter, Joshua Ryo, Beck, Geoffrey, Tjus, Julia Becker, Beiske, Lukas, Belardinelli, Daniele, Benbow, Wystan, Bernardini, Elisa, Medrano, Juan Bernete, Bernlöhr, Konrad, Berti, Alessio, Beshley, Vasyl, Bhattacharjee, Pooja, Bhattacharyya, Saptashwa, Bi, Baiyang, Biederbeck, Noah, Biland, Adrian, Bissaldi, Elisabetta, Blanch, Oscar, Blazek, Jiri, Boisson, Catherine, Bolmont, Julien, Bonnoli, Giacomo, Bordas, Pol, Bošnjak, Željka, Bradascio, Federica, Braiding, Catherine, Bronzini, Ettore, Brose, Robert, Brown, Anthony M., Brun, Francois, Brunelli, Giulia, Bulgarelli, Andrea, Burelli, Irene, Burmistrov, Leonid, Burton, Michael, Bylund, Tomas, Calisse, Paolo Gherardo, Campoy-Ordaz, Anna, Cantlay, Brandon Khan, Capalbi, Milvia, Caproni, Anderson, Capuzzo-Dolcetta, Roberto, Carlile, Colin, Caroff, Sami, Carosi, Roberto, Carrasco, Marie-Sophie, Cascone, Enrico, Cassol, Franca, Castrejon, Noelia, Catalani, Fernando, Cerasole, Davide, Cerruti, Matteo, Chaty, Sylvain, Chen, Andrew W, Chernyakova, Maria, Chiavassa, Andrea, Chudoba, Jiří, Araujo, Carlos Henrique Coimbra, Conforti, Vito, Conte, Francesco, Contreras, Jose Luis, Cossou, Christophe, Costa, Alessandro, Costantini, Heide, Cristofari, Pierre, Cuevas, Omar, Curtis-Ginsberg, Zachary, D'Amico, Giacomo, D'Ammando, Filippo, Dadina, Mauro, Dalchenko, Mykhailo, David, Ludovic, Davids, Isak Delberth, Dazzi, Francesco, De Angelis, Alessandro, de Lavergne, Mathieu de Bony, De Caprio, Vincenzo, De Cesare, Giovanni, Pino, Elisabete M. de Gouveia Dal, De Lotto, Barbara, de Lucia, Mario, de Menezes, Raniere, de Naurois, Mathieu, Wilhelmi, Emma de Oña, De Simone, Nicola, de Souza, Vitor, Del Peral, Luis, del Valle, Maria Victoria, Delagnes, Eric, Giler, Andres Gabriel Delgado, Delgado, Carlos, Dell'aiera, Michael, Della Ceca, Roberto, Della Valle, Massimo, Della Volpe, Domenico, Depaoli, Davide, Dettlaff, Antonios, Di Girolamo, Tristano, Di Piano, Ambra, Di Pierro, Federico, Di Tria, Riccardo, Di Venere, Leonardo, Díaz-Bahamondes, Christian, Dib, Claudio, Diebold, Sebastian, Dima, Razvan, Dinesh, Adithiya, Djannati-Ataï, Arache, Djuvsland, Julia Isabel, Dominguez, Alberto, Dominik, Rune Michael, Donini, Alice, Dorner, Daniela, Dörner, Julien, Doro, Michele, Anjos, Rita de Cassia dos, Dournaux, Jean-Laurent, Dravins, Dainis, Duangchan, Chaimongkol, Dubos, Coline, Ducci, Lozenzo, Dwarkadas, Vikram V., Ebr, Jan, Eckner, Christopher, Egberts, Kathrin, Einecke, Sabrina, Elsässer, Dominik, Emery, Gabriel, Godoy, Miguel Escobar, Escudero, Juan, Esposito, Paolo, Falceta-Gonçalves, Diego, Ramazani, Vandad Fallah, Faure, Alice, Fedorova, Elena, Fegan, Stephen, Feijen, Kirsty, Feng, Qi, Ferrand, Gilles, Ferrarotto, Fabio, Fiandrini, Emanuele, Fiasson, Armand, Fioretti, Valentina, Foffano, Luca, Guiteras, Lluis Font, Fontaine, Gerard, Fröse, Stefan, Fukami, Satoshi, Fukui, Yasuo, Funk, Stefan, Gaggero, Daniele, Galanti, Giorgio, Galaz, Gaspar, Gallant, Yves A., Gallozzi, Stefano, Gammaldi, Viviana, Gasbarra, Claudio, Gaug, Markus, Ghalumyan, Arsen, Gianotti, Fulvio, Giarrusso, Marina, Giglietto, Nicola, Giordano, Francesco, Giuliani, Andrea, Glicenstein, Jean-Francois, Glombitza, Jonas, Goldoni, Paolo, González, José Mauricio, González, Maria Magdalena, Coelho, Jaziel Goulart, Granot, Jonathan, Grasso, Dario, Haro, Roger Grau, Green, David, Greenshaw, Tim, Grolleron, Guillaume, Grube, Jeff, Gueta, Orel, Gunji, Shuichi, Hadasch, Daniela, Hamal, Petr, Hanlon, William, Hara, Satoshi, Harvey, Violet M., Hashiyama, Kazuaki, Hassan, Tarek, Heller, Matthieu, Cadena, Sergio Hernández, Hie, Jonathan, Hiroshima, Nagisa, Hnatyk, Bohdan, Hnatyk, Roman, Hoffmann, Dirk, Hofmann, Werner, Holler, Markus, Horan, Deirdre, Horvath, Pavel, Hovatta, Talvikki, Hrupec, Dario, Hussain, Saqib, Iarlori, Marco, Inada, Tomohiro, Incardona, Federico, Inome, Yusuke, Inoue, Susumu, Iocco, Fabio, Ishio, Kazuma, Jamrozy, Marek, Janecek, Petr, Jankowsky, Felix, Jarnot, Christian, Jean, Pierre, Martínez, Irene Jiménez, Jin, Weidong, Jocou, Laurent, Juramy-Gilles, Claire, Jurysek, Jakub, KALEKIN, Oleg, Kantzas, Dimitrios, Karas, Vladimir, Kaufmann, Sarah, Kerszberg, Daniel, Khelifi, Bruno, Kieda, David B, Kleiner, Tobias Kai, Kluźniak, Włodzimierz, Kobayashi, Yukiho, Kohri, Kazunori, Komin, Nukri, Kornecki, Paula, Kosack, Karl, Kubo, Hidetoshi, Kushida, Junko, La Barbera, Antonino, La Palombara, Nicola, Lainez, Maria, Lamastra, Alessandra, Lapington, Jon S, Lazarevic, Sanja, Lazendic-Galloway, Jasmina, Leach, Steven, Lemoine-Goumard, Marianne, Lenain, Jean-Philippe, Leto, Giuseppe, Leuschner, Fabian, Lindfors, Elina, Linhoff, Maximilian, Liodakis, Ioannis, Loïc, Lozach, Lombardi, Saverio, Longo, Francesco, López-Coto, Rubén, López-Moya, Marcos, López-Oramas, Alicia, Loporchio, Serena, Bahilo, Julio Lozano, Luque-Escamilla, Pedro L., Macias, Oscar, Maier, Gernot, Majumdar, Pratik, Malyshev, Denys, Malyshev, Dmitry, Mandat, Dusan, Manicò, Giulio, Marinos, Peter David, Markoff, Sera, Márquez, Isabel, Marquez, Patricia, Marsella, Giovanni, Martí, Josep, Martin, Pierrick, Martínez, Gustavo Augusto, Martínez, Manel, Martinez, Oibar, Marty, Christophe, Mas-Aguilar, Alvaro, Mastropietro, Michele, Maurin, Gilles, Max-Moerbeck, Walter, Mazin, Daniel, Melkumyan, David, Menchiari, Stefano, Mestre, Enrique, Meunier, Jean-Luc, Meyer, Dominique M. -A., Miceli, Davide, Michailidis, Miltiadis, Michałowski, Jerzy, Miener, Tjark, Miranda, Jose Miguel, Mitchell, Alison, Mizote, Masaya, Mizuno, Tsunefumi, Moderski, Rafal, Mohrmann, Lars, Molero, Miguel, Molfese, Cesare, Molina, Edgar, Montaruli, Teresa, Moralejo, Abelardo, Morcuende, Daniel, Morik, Katharina, Morselli, Aldo, Moulin, Emmanuel, Zamanillo, Victor Moya, Mukherjee, Reshmi, Munari, Kevin, Muraczewski, Adam, Muraishi, Hiroshi, Nakamori, Takeshi, Nayak, Amrit, Nemmen, Rodrigo, Nickel, Lukas, Niemiec, Jacek, Nieto, Daniel, Rosillo, Mireia Nievas, Nikołajuk, Marek, Nishijima, Kyoshi, Noda, Koji, Nosek, Dalibor, Novosyadlyj, Bohdan, Novotný, Vladimír, Nozaki, Seiya, O'Brien, Paul, Ohishi, Michiko, Ohtani, Yoshiki, Okumura, Akira, Olive, Jean-François, Olmi, Barbara, Ong, Rene A., Orienti, Monica, Orito, Reiko, Orlandini, Mauro, Orlando, Elena, Ostrowski, Michal, Otte, Nepomuk, Oya, Igor, Pagano, Isabella, Pagliaro, Antonio, Palatiello, Michele, Panebianco, Gabriele, Paredes, Josep M., Parmiggiani, Nicolò, Patel, Sonal Ramesh, Pavlović, Dijana, Pe'er, Asaf, Pech, Miroslav, Pecimotika, Mario, Peresano, Michele, Pérez-Romero, Judit, Peron, Giada, Persic, Massimo, Petrucci, Pierre-Olivier, Petruk, Oleh, Pfeifle, Felix, Pintore, Fabio, Pirola, Giorgio, Pittori, Carlotta, Plard, Cyann, Podobnik, Franjo, Pohl, Martin, Pons, Estelle, Prandini, Elisa, Prast, Julie, Principe, Giacomo, Priyadarshi, Chaitanya, Produit, Nicolas, Prokhorov, Dmitry, Pueschel, Elisa, Pühlhofer, Gerd, Pumo, Maria Letizia, Punch, Michael, Quirrenbach, Andreas, Raino, Silvia, Randazzo, Nunzio, Rando, Riccardo, Ravel, Thierry, Razzaque, Soebur, Regeard, Maxime, Reichherzer, Patrick, Reimer, Anita, Reimer, Olaf, Reisenegger, Andreas, Reposeur, Thierry, Reville, Brian, Rhode, Wolfgang, Ribó, Marc, Richtler, Tom, Rieger, Frank, Roache, Emmet, Fernandez, Gonzalo Rodriguez, Frías, Maria Dolores Rodríguez, Rodríguez-Vázquez, Juan José, Romano, Patrizia, Romeo, Giuseppe, Rosado, Jaime, Rowell, Gavin P, Rudak, Bronislaw, Ruiter, Ashley J., Rulten, Cameron Boyd, Russo, Federico, Sadeh, Iftach, Saha, Lab, Saito, Takayuki, Sakurai, Shunsuke, Salzmann, Heiko, Sanchez, David, Sanchez-Conde, Miguel, Sangiorgi, Pierluca, Sano, Hidetoshi, Santander, Marcos, Santangelo, Andrea, Santos-Lima, Reinaldo, Sanuy, Andreu, Šarić, Toni, Sarkar, Arkadipta, Sarkar, Subir, Saturni, Francesco Gabriele, Savchenko, Volodymyr, Scherer, Andres, Schipani, Pietro, Schleicher, Bernd, Schovanek, Petr, Schubert, Jan Lukas, Schwanke, Ullrich, Schwefer, Georg, Scuderi, Salvatore, Arroyo, Monica Seglar, Seitenzahl, Ivo, Sergijenko, Olga, Sguera, Vito, Shang, Ruo-Yu, Sharma, Pooja, Sidibe, Guereguin Der Sylvestre, Sidoli, Lara, Siejkowski, Hubert, Siqueira, Clarissa, Sizun, Patrick, Sliusar, Vitalii, Slowikowska, Agnieszka, Sol, Helene, Specovius, Andreas, Spencer, Samuel Timothy, Spiga, Daniele, Stamerra, Antonio, Stanič, Samo, Starecki, Tomasz, Starling, Rhaana, Steppa, Constantin, Stolarczyk, Thierry, Strišković, Jelena, Strzys, Marcel C., Suda, Yusuke, Suomijarvi, Tiina, Tak, Donggeun, Takahashi, Mitsunari, Takeishi, Ryuji, Tam, Pak-Hin Thomas, Tanaka, Shuta J, Tanaka, Takaaki, Terauchi, Kenta, Testa, Vincenzo, Tibaldo, Luigi, Tibolla, Omar, Torradeflot, Francesc, Torres, Diego F., Torresi, Eleonora, Tothill, Nick, Toussenel, Francois, Touzard, Victoria, Tramacere, Andrea, Travnicek, Petr, Tripodo, Giovanni, Truzzi, Stefano, Tsiahina, Adellain, Tutone, Antonio, Vacula, Martin, Vallage, Bertrand, Vallania, Piero, Vallés, Ramon, van Eldik, Christopher, van Scherpenberg, Juliane, Vandenbroucke, Justin, Vassiliev, Vladimir, Venault, Philippe, Ventura, Sofia, Vercellone, Stefano, Verna, Gaia, Viana, Aion, Viaux, Nicolás, Vigliano, Alessandro, Vignatti, Jonatan, Vigorito, Carlo francesco, Vitale, Vincenzo, Vodeb, Veronika, Voisin, Vincent, Vorobiov, Serguei, Voutsinas, Georgios Gerasimos, Vovk, Ievgen, Waegebaert, Vincent, Wagner, Stefan Joachim, Walter, Roland, Ward, Martin, Wechakama, Maneenate, White, Richard, Wierzcholska, Alicja, Will, Martin, Williams, David A., Wohlleben, Frederik, Wolter, Anna, Yamamoto, Tokonatsu, Yamazaki, Ryo, Yang, Lili, Yoshida, Tatsuo, Yoshikoshi, Takanori, Zacharias, Michael, Sanchez, Ricardo Zanmar, Zavrtanik, Danilo, Zavrtanik, Marko, Zdziarski, Andrzej A., Zech, Andreas, Zhdanov, Valery I., Ziȩtara, Krzysztof, Živec, Miha, and Zuriaga-Puig, Jaume
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Astrophysics - High Energy Astrophysical Phenomena - Abstract
The detection of gravitational waves from a binary neutron star merger by Advanced LIGO and Advanced Virgo (GW170817), along with the discovery of the electromagnetic counterparts of this gravitational wave event, ushered in a new era of multimessenger astronomy, providing the first direct evidence that BNS mergers are progenitors of short gamma-ray bursts (GRBs). Such events may also produce very-high-energy (VHE, > 100GeV) photons which have yet to be detected in coincidence with a gravitational wave signal. The Cherenkov Telescope Array (CTA) is a next-generation VHE observatory which aims to be indispensable in this search, with an unparalleled sensitivity and ability to slew anywhere on the sky within a few tens of seconds. New observing modes and follow-up strategies are being developed for CTA to rapidly cover localization areas of gravitational wave events that are typically larger than the CTA field of view. This work will evaluate and provide estimations on the expected number of of gravitational wave events that will be observable with CTA, considering both on- and off-axis emission. In addition, we will present and discuss the prospects of potential follow-up strategies with CTA., Comment: Presented at the 38th International Cosmic Ray Conference (ICRC 2023), 2023 (arXiv:2309.08219)
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- 2023
19. Emissions from the Construction Sector in the United Kingdom
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Desouza, Carl, Marsh, Daniel, Beevers, Sean, Molden, Nick, and Green, David
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- 2024
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20. Low-dose azithromycin prophylaxis in patients with atrial fibrillation and chronic obstructive pulmonary disease
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Bucci, Tommaso, Wat, Dennis, Sibley, Sarah, Wootton, Dan, Green, David, Pignatelli, Pasquale, Lip, Gregory Y. H., and Frost, Freddy
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- 2024
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21. Tannaka-Krein reconstruction for fusion 2-categories
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Green, David
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Mathematics - Category Theory ,Mathematics - Quantum Algebra ,Mathematics - Representation Theory - Abstract
We reprove the classical Tannaka-Krein reconstruction theorem by finding a monoidal equivalence of categories between a 1-truncated sub-2-category of the slice 2-category ${\sf Mod}({\sf Vec})/{\sf Vec}$ and the category of algebras. We then immediately generalize this approach to find a monoidal equivalence of 2-categories between a 2-truncated sub-3-category of the slice 3-category ${\sf Mod}({\sf TwoVec})/{\sf TwoVec}$ and the category of algebras. As an immediate consequence, a finite semisimple 2-Hopf algebra $C$ can be recovered from its fusion 2-category of modules together with the monoidal fiber 2-functor to ${\sf TwoVec}$. Moreover, every fusion 2-category equipped with a monoidal functor to ${\sf TwoVec}$ is of this form., Comment: 35 pages, many figures. Comments welcome!
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- 2023
22. A Radio Flare in the Long-Lived Afterglow of the Distant Short GRB 210726A: Energy Injection or a Reverse Shock from Shell Collisions?
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Schroeder, Genevieve, Rhodes, Lauren, Laskar, Tanmoy, Nugent, Anya, Escorial, Alicia Rouco, Rastinejad, Jillian C., Fong, Wen-fai, van der Horst, Alexander J., Veres, Péter, Alexander, Kate D., Andersson, Alex, Berger, Edo, Blanchard, Peter K., Chastain, Sarah, Christensen, Lise, Fender, Rob, Green, David A., Groot, Paul, Heywood, Ian, Horesh, Assaf, Izzo, Luca, Kilpatrick, Charles D., Körding, Elmar, Lien, Amy, Malesani, Daniele B., McBride, Vanessa, Mooley, Kunal, Rowlinson, Antonia, Sears, Huei, Stappers, Ben, Tanvir, Nial, Vergani, Susanna D., Wijers, Ralph A. M. J., Williams-Baldwin, David, and Woudt, Patrick
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Astrophysics - High Energy Astrophysical Phenomena - Abstract
We present the discovery of the radio afterglow of the short $\gamma$-ray burst (GRB) 210726A, localized to a galaxy at a photometric redshift of $z\sim 2.4$. While radio observations commenced $\lesssim 1~$day after the burst, no radio emission was detected until $\sim11~$days. The radio afterglow subsequently brightened by a factor of $\sim 3$ in the span of a week, followed by a rapid decay (a "radio flare"). We find that a forward shock afterglow model cannot self-consistently describe the multi-wavelength X-ray and radio data, and underpredicts the flux of the radio flare by a factor of $\approx 5$. We find that the addition of substantial energy injection, which increases the isotropic kinetic energy of the burst by a factor of $\approx 4$, or a reverse shock from a shell collision are viable solutions to match the broad-band behavior. At $z\sim 2.4$, GRB 210726A is among the highest redshift short GRBs discovered to date as well as the most luminous in radio and X-rays. Combining and comparing all previous radio afterglow observations of short GRBs, we find that the majority of published radio searches conclude by $\lesssim 10~$days after the burst, potentially missing these late rising, luminous radio afterglows., Comment: 29 pages, 10 figures, accepted to ApJ
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- 2023
23. The Third Fermi Large Area Telescope Catalog of Gamma-ray Pulsars
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Smith, David A., Bruel, Philippe, Clark, Colin J., Guillemot, Lucas, Kerr, Matthew T., Ray, Paul, Abdollahi, Soheila, Ajello, Marco, Baldini, Luca, Ballet, Jean, Baring, Matthew, Bassa, Cees, Gonzalez, Josefa Becerra, Bellazzini, Ronaldo, Berretta, Alessandra, Bhattacharyya, Bhaswati, Bissaldi, Elisabetta, Bonino, Raffaella, Bottacini, Eugenio, Bregeon, Johan, Burgay, Marta, Burnett, Toby, Cameron, Rob, Camilo, Fernando, Caputo, Regina, Caraveo, Patrizia, Cavazzuti, Elisabetta, Chiaro, Graziano, Ciprini, Stefano, Cognard, Ismael, Orestano, Paolo Cristarella, Crnogorcevic, Milena, Cuoco, Alessandro, Cutini, Sara, D'Ammando, Filippo, de Angelis, Alessandro, De Gaetano, Salvatore, de Menezes, Raniere, de Palma, Francesco, DeCesar, Megan, Deneva, Julia, Di Lalla, Niccola, Di Venere, Leonardo, Dirirsa, Feraol Fana, Dominguez, Alberto, Dumora, Denis, Fegan, Stephen, Ferrara, Elizabeth, Fiori, Alessio, Fleischhack, Henrike, Flynn, Chris, Franckowiak, Anna, Freire, Paulo, Fukazawa, Yasushi, Fusco, Piergiorgio, Galanti, Giorgio, Gammaldi, Viviana, Gargano, Fabio, Gasparrini, Dario, Giacchino, Federica, Giglietto, Nico, Giordano, Francesco, Giroletti, Marcello, Green, David, Grenier, Isabelle, Guiriec, Sylvain, Gustafsson, Michael, Harding, Alice, Hays, Liz, Hewitt, John, Horan, Deirdre, Hou, Xian, Jankowski, Fabian, Johnson, Tyrel, Johnson, Robert, Johnston, Simon, Kataoka, Jun, Keith, Michael J., Kramer, Michael, Kuss, Michael, Latronico, Luca, Lee, Shiu-Hang, Li, Di, Li, Jian, Limyansky, Brent, Longo, Francesco, Loparco, Francesco, Lorusso, Leonarda, Lovellette, Michael, Lower, Marcus, Lubrano, Pasquale, Lyne, Andrew, Maldera, Simone, Manchester, Richard, Manfreda, Alberto, Marelli, Martino, Marta-Devesa, Guillem, Mazziotta, Mario Nicola, McEnery, Julie, Mereu, Isabella, Michelson, Peter, Mitthumsiri, Warit, Mizuno, Tsunefumi, Moiseev, Alex, Monzani, Maria Elena, Morselli, Aldo, Negro, Michela, Nemmen, Rodrigo, Nieder, Lars, Nuss, Eric, Omodei, Nicola, Orienti, Monica, Orlando, Elena, Ormes, Jonathan F., Palatiello, Michele, Paneque, David, Panzarini, Giuliana, Persic, Massimo, Pesce-Rollins, Melissa, Pillera, Roberta, Poon, Helen, Porter, Troy, Principe, Giacomo, Raino, Silvia, Rando, Riccardo, Ransom, Scott, Razzano, Massimiliano, Razzaque, Soebur, Reimer, Anita, Reimer, Olaf, Renault-Tinacci, Nicolas, Romani, Roger, Sanchez-Conde, Miguel A., Parkinson, Pablo Saz, Scotton, Lorenzo, Serini, Davide, Sgro, Carmelo, Shannon, Ryan, Sharma, Vidushi, Siskind, Eric J., Spandre, Gloria, Spinelli, Paolo, Stappers, Ben, Stephens, Tom, Suson, Dan, Tajima, Hiro, Tak, Dongguen, Theureau, Gilles, Thompson, David, Tibolla, Omar, Torres, Diego F., Valverde, Janeth, Venter, Christo, Wadiasingh, Zorawar, Wang, Nina, Wang, Pei, Weltevrede, Patrick, Wood, Kent, and Zaharijas, Gabrijela
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Astrophysics - High Energy Astrophysical Phenomena - Abstract
We present 294 pulsars found in GeV data from the Large Area Telescope (LAT) on the Fermi Gamma-ray Space Telescope. Another 33 millisecond pulsars (MSPs) discovered in deep radio searches of LAT sources will likely reveal pulsations once phase-connected rotation ephemerides are achieved. A further dozen optical and/or X-ray binary systems co-located with LAT sources also likely harbor gamma-ray MSPs. This catalog thus reports roughly 340 gamma-ray pulsars and candidates, 10% of all known pulsars, compared to $\leq 11$ known before Fermi. Half of the gamma-ray pulsars are young. Of these, the half that are undetected in radio have a broader Galactic latitude distribution than the young radio-loud pulsars. The others are MSPs, with 6 undetected in radio. Overall, >235 are bright enough above 50 MeV to fit the pulse profile, the energy spectrum, or both. For the common two-peaked profiles, the gamma-ray peak closest to the magnetic pole crossing generally has a softer spectrum. The spectral energy distributions tend to narrow as the spindown power $\dot E$ decreases to its observed minimum near $10^{33}$ erg s$^{-1}$, approaching the shape for synchrotron radiation from monoenergetic electrons. We calculate gamma-ray luminosities when distances are available. Our all-sky gamma-ray sensitivity map is useful for population syntheses. The electronic catalog version provides gamma-ray pulsar ephemerides, properties and fit results to guide and be compared with modeling results., Comment: 142 pages. Accepted by the Astrophysical Journal Supplement
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- 2023
24. Applied Bayesian Structural Health Monitoring: inclinometer data anomaly detection and forecasting
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Green, David K. E. and Jaspan, Adam
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Computer Science - Machine Learning ,Statistics - Machine Learning - Abstract
Inclinometer probes are devices that can be used to measure deformations within earthwork slopes. This paper demonstrates a novel application of Bayesian techniques to real-world inclinometer data, providing both anomaly detection and forecasting. Specifically, this paper details an analysis of data collected from inclinometer data across the entire UK rail network. Practitioners have effectively two goals when processing monitoring data. The first is to identify any anomalous or dangerous movements, and the second is to predict potential future adverse scenarios by forecasting. In this paper we apply Uncertainty Quantification (UQ) techniques by implementing a Bayesian approach to anomaly detection and forecasting for inclinometer data. Subsequently, both costs and risks may be minimised by quantifying and evaluating the appropriate uncertainties. This framework may then act as an enabler for enhanced decision making and risk analysis. We show that inclinometer data can be described by a latent autocorrelated Markov process derived from measurements. This can be used as the transition model of a non-linear Bayesian filter. This allows for the prediction of system states. This learnt latent model also allows for the detection of anomalies: observations that are far from their expected value may be considered to have `high surprisal', that is they have a high information content relative to the model encoding represented by the learnt latent model. We successfully apply the forecasting and anomaly detection techniques to a large real-world data set in a computationally efficient manner. Although this paper studies inclinometers in particular, the techniques are broadly applicable to all areas of engineering UQ and Structural Health Monitoring (SHM)., Comment: 6 Pages. Conference proceedings from GAMM23
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- 2023
25. Innovative products and applications
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Klug, David, primary, Kaneshiro, Jon, additional, Cubeta, Richard, additional, Green, David, additional, and Winterberg, Ralf, additional
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- 2024
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26. Enriched string-net models and their excitations
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Green, David, Huston, Peter, Kawagoe, Kyle, Penneys, David, Poudel, Anup, and Sanford, Sean
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Condensed Matter - Strongly Correlated Electrons ,Mathematical Physics ,Mathematics - Category Theory ,Mathematics - Quantum Algebra ,Quantum Physics ,18M20 (Primary) 81V27, 18M30, 57R56 (Secondary) - Abstract
Boundaries of Walker-Wang models have been used to construct commuting projector models which realize chiral unitary modular tensor categories (UMTCs) as boundary excitations. Given a UMTC $\mathcal{A}$ representing the Witt class of an anomaly, the article [arXiv:2208.14018] gave a commuting projector model associated to an $\mathcal{A}$-enriched unitary fusion category $\mathcal{X}$ on a 2D boundary of the 3D Walker-Wang model associated to $\mathcal{A}$. That article claimed that the boundary excitations were given by the enriched center/M\"uger centralizer $Z^\mathcal{A}(\mathcal{X})$ of $\mathcal{A}$ in $Z(\mathcal{X})$. In this article, we give a rigorous treatment of this 2D boundary model, and we verify this assertion using topological quantum field theory (TQFT) techniques, including skein modules and a certain semisimple algebra whose representation category describes boundary excitations. We also use TQFT techniques to show the 3D bulk point excitations of the Walker-Wang bulk are given by the M\"uger center $Z_2(\mathcal{A})$, and we construct bulk-to-boundary hopping operators $Z_2(\mathcal{A})\to Z^{\mathcal{A}}(\mathcal{X})$ reflecting how the UMTC of boundary excitations $Z^{\mathcal{A}}(\mathcal{X})$ is symmetric-braided enriched in $Z_2(\mathcal{A})$. This article also includes a self-contained comprehensive review of the Levin-Wen string net model from a unitary tensor category viewpoint, as opposed to the skeletal $6j$ symbol viewpoint., Comment: 43 pages; numerous figures
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- 2023
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27. AT 2021loi: A Bowen Fluorescence Flare with a Rebrightening Episode, Occurring in a Previously-Known AGN
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Makrygianni, Lydia, Trakhtenbrot, Benny, Arcavi, Iair, Ricci, Claudio, Lam, Marco C., Horesh, Assaf, Sfaradi, Itai, Bostroem, K. Azalee, Hosseinzadeh, Griffin, Howell, D. Andrew, Pellegrino, Craig, Fender, Rob, Green, David A., Williams, David R. A., and Bright, Joe
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Astrophysics - Astrophysics of Galaxies ,Astrophysics - High Energy Astrophysical Phenomena - Abstract
AT 2021loi is an optical-ultraviolet transient located at the center of its host galaxy. Its spectral features identify it as a member of the ``Bowen Fluorescence Flare'' (BFF) class. The first member of this class was considered to be related to a tidal disruption event, but enhanced accretion onto an already active supermassive black hole was suggested as an alternative explanation. AT 2021loi, having occurred in a previously-known unobscured AGN, strengthens the latter interpretation. Its light curve is similar to those of previous BFFs, showing a rebrightening approximately one year after the main peak (which was not explicitly identified, but might be the case, in all previous BFFs). An emission feature around 4680 A, seen in the pre-flare spectrum, strengthens by a factor of $\sim$2 around the optical peak of the flare, and is clearly seen as a double peaked feature then, suggesting a blend of NIII $\lambda 4640$ with HeII $\lambda4686$ as its origin. The appearance of OIII $\lambda$3133 and possible NIII $\lambda\lambda4097,4103$ (blended with H$\delta$) during the flare further support a Bowen Fluorescence classification. Here, we present ZTF, ATLAS, Keck, Las Cumbres Observatory, NEOWISE-R, $Swift$, AMI and VLA observations of AT 2021loi, making it one of the best observed BFFs to date. AT 2021loi thus provides some clarity on the nature of BFFs but also further demonstrates the diversity of nuclear transients., Comment: Submitted to ApJ. This version addresses comments from the referee
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- 2023
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28. Millihertz X-ray variability during the 2019 outburst of black hole candidate Swift~J1357.2$-$0933
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Beri, Aru, Gaur, Vishal, Charles, Phil, Williams, David R. A., Jahanvi, Paice, John A., Gandhi, Poshak, Altamirano, Diego, Fender, Rob, Green, David A., and Titterington, David
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Astrophysics - High Energy Astrophysical Phenomena - Abstract
Swift J1357.2$-$0933 is a black-hole candidate X-ray transient, which underwent its third outburst in 2019, during which several multi-wavelength observations were carried out.~Here, we report results from the \emph{Neil Gehrels Swift} and \emph{NICER} observatories and radio data from \emph{AMI}.~For the first time,~millihertz quasi-periodic X-ray oscillations with frequencies varying between ${\sim}$~1--5~$\rm{mHz}$ were found in \emph{NICER} observations and a similar feature was also detected in one \emph{Swift}--\textsc{XRT} dataset.~Our spectral analysis indicate that the maximum value of the measured X-ray flux is much lower compared to the peak values observed during the 2011 and 2017 outbursts.~This value is ${\sim}$~100 times lower than found with \emph{MAXI} on MJD~58558 much ($\sim$~68 days) earlier in the outburst, suggesting that the \emph{Swift} and \emph{NICER} fluxes belong to the declining phase of the 2019 outburst.~An additional soft component was detected in the \textsc{XRT} observation with the highest flux level, but at a relatively low $L_{\rm X}$~$\sim$~$3{\times}10^{34}~(d/{\rm 6~kpc)}^2\rm{erg}~\rm{s}^{-1}$, and which we fitted with a disc component at a temperature of $\sim 0.17$~keV.~The optical/UV magnitudes obtained from \emph{Swift}--\textsc{UVOT} showed a correlation with X-ray observations, indicating X-ray reprocessing to be the plausible origin of the optical and UV emission.~However, the source was not significantly detected in the radio band.~There are currently a number of models that could explain this millihertz-frequency X-ray variability; not least of which involves an X-ray component to the curious dips that, so far, have only been observed in the optical., Comment: 14 pages, Accepted for publication in MNRAS
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- 2023
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29. Evidence for a black hole spin--orbit misalignment in the X-ray binary Cyg X-1
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Zdziarski, Andrzej A., Veledina, Alexandra, Szanecki, Michal, Green, David A., Bright, Joe S., and Williams, David R. A.
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Astrophysics - High Energy Astrophysical Phenomena - Abstract
Recently, the accretion geometry of the black-hole X-ray binary Cyg X-1 was probed with the X-ray polarization. The position angle of the X-ray emitting flow was found to be aligned with the position angle of the radio jet in the plane of the sky. At the same time, the observed high polarization degree could be obtained only for a high inclination of the X-ray emitting flow, indicating a misalignment between the binary axis and the black hole spin. The jet, in turn, is believed to be directed by the spin axis, hence similar misalignment is expected between the jet and binary axes. We test this hypothesis using very long (up to about 26 years) multi-band radio observations. We find the misalignment of $20^\circ$--$30^\circ$. However, on the contrary to the earlier expectations, the jet and binary viewing angles are found to be similar, while the misalignment is seen between position angles of the jet and the binary axis on the plane of the sky. Furthermore, the presence of the misalignment questions our understanding of the evolution of this binary system., Comment: ApJL, in press
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- 2023
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30. A hierarchical modeling approach to predict the distribution and density of Sierra Nevada Red Fox (Vulpes vulpes necator).
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Green, David, Martin, Marie, Matthews, Sean, Akins, Jocelyn, Carlson, Jennifer, Figura, Pete, Hatfield, Brian, Perrine, John, Quinn, Cate, Stephenson, Thomas, Stock, Sarah, Tucker, Jody, and Sacks, Benjamin
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Royle–Nichols model ,Sierra Nevada Red Fox ,Vulpes vulpes necator ,hierarchical modeling ,occupancy modeling ,remote cameras ,species distribution model - Abstract
Carnivores play critical roles in ecosystems, yet many species are declining worldwide. The Sierra Nevada Red Fox (Vulpes vulpes necator; SNRF) is a rare and endangered subspecies of red fox limited to upper montane forests, subalpine, and alpine environments of California and Oregon, United States. Having experienced significant distribution contractions and population declines in the last century, the subspecies is listed as at-risk by relevant federal and state agencies. Updated information on its contemporary distribution and density is needed to guide and evaluate conservation and management actions. We combined 12 years (2009-2020) of detection and nondetection data collected throughout California and Oregon to model the potential distribution and density of SNRFs throughout their historical and contemporary ranges. We used an integrated species distribution and density modeling approach, which predicted SNRF density in sampled locations based on observed relationships between environmental covariates and detection frequencies, and then projected those predictions to unsampled locations based on the estimated correlations with environmental covariates. This approach provided predictions that serve as density estimates in sampled regions and projections in unsampled areas. Our model predicted a density of 1.06 (95% credible interval = 0.8-1.36) foxes per 100 km2 distributed throughout 22,926 km2 in three distinct regions of California and Oregon-Sierra Nevada, Lassen Peak, and Oregon Cascades. SNRFs were most likely to be found in areas with low minimum temperatures and high snow water equivalent. Our results provide a contemporary baseline to inform the development and evaluation of conservation and management actions, and guide future survey efforts.
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- 2023
31. Refugees by Another Name: Displaced Learners in Japanese Higher Education
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Green, David, Unangst, Lisa, Tomita, Eriko, Kim, Mikyoung, Series Editor, Momesso, Lara, editor, and Ivanova, Polina, editor
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- 2024
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32. Social Construction of Barriers or Challenges to Parenting: Black Jamaican Fathers’ and Mothers’ Perspectives
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Green, David S., Chuang, Susan S., and Goldstein, Abby L.
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- 2024
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33. Anticoagulant prescribing patterns in patients with primary central nervous system malignancies and secondary metastases
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Abdelmessih, Emily, Ahuja, Tania, Wo, Stephanie, Sango, Aaron, Papadopoulos, John, Green, David, and Xiang, Elaine
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- 2024
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34. Precise Measurements of Self-absorbed Rising Reverse Shock Emission from Gamma-ray Burst 221009A
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Bright, Joe S., Rhodes, Lauren, Farah, Wael, Fender, Rob, van der Horst, Alexander J., Leung, James K., Williams, David R. A., Anderson, Gemma E., Atri, Pikky, DeBoer, David R., Giarratana, Stefano, Green, David A., Heywood, Ian, Lenc, Emil, Murphy, Tara, Pollak, Alexander W., Premnath, Pranav H., Scott, Paul F., Sheikh, Sofia Z., Siemion, Andrew, and Titterington, David J.
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Astrophysics - High Energy Astrophysical Phenomena - Abstract
The deaths of massive stars are sometimes accompanied by the launch of highly relativistic and collimated jets. If the jet is pointed towards Earth, we observe a "prompt" gamma-ray burst due to internal shocks or magnetic reconnection events within the jet, followed by a long-lived broadband synchrotron afterglow as the jet interacts with the circum-burst material. While there is solid observational evidence that emission from multiple shocks contributes to the afterglow signature, detailed studies of the reverse shock, which travels back into the explosion ejecta, are hampered by a lack of early-time observations, particularly in the radio band. We present rapid follow-up radio observations of the exceptionally bright gamma-ray burst GRB 221009A which reveal an optically thick rising component from the reverse shock in unprecedented detail both temporally and in frequency space. From this, we are able to constrain the size, Lorentz factor, and internal energy of the outflow while providing accurate predictions for the location of the peak frequency of the reverse shock in the first few hours after the burst., Comment: 11 figures, 4 tables
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- 2023
35. Minor Flares on Cygnus X-3 -- VLBI Prospects
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Spencer, Ralph E., Bray, Justin D., Green, David A., and Garrett, Michael A.
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Astrophysics - High Energy Astrophysical Phenomena - Abstract
The cm-wavelength radio flares on Cygnus X-3 have been studied for many years. Our recent paper (Spencer et al., 2022) looked again at the minor flares (flux density S of a few 100 mJy) and compared their properties with those of a sample of major flares (S > 1 Jy). We find that the minor flares have rise times and duration of ~ 1 hour, as opposed to ~ days for the major flares. Minor flares show more rapid expansion of the synchrotron radiation emitting material than in the strong flares. They also appear closer to the binary, whereas the large flares form a more developed jet, i.e. the jets formed in minor flares are short and wide, those in major flares are long and thin. We used the results of Fender & Bright (2019) to calculate the magnetic field and expansion velocity as a fraction B of the speed of light under minimum energy conditions when the source is optically thick for samples of minor and major flares. The minimum power in the source was found using the rise time of the flares. The minor flares have lower minimum power but have larger velocities and energy densities than the major flares. Minor flares can occur while a major flare is in progress, suggesting an indirect coupling between them. The spectral evolution of the minor flares can be explained by either an expanding synchrotron source or a shock model. Further investigation requires high resolution VLBI observations at the 1 mas level if we wish to understand the development of the source. The problem is that Cygnus X-3 is strongly scattered by the interstellar medium so high frequencies in the several 10s of GHz are required for the resolution needed. The minor flares are rapid [...] and hence only short snapshot VLBI observations can capture the structure. Large numbers of telescopes are required which is a problem at the highest frequencies. We discuss the VLBI possibilities and trade-offs for this awkward object., Comment: Accepted to PoS (EVN2022): proceedings of 15th European VLBI Network Symposium
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- 2023
36. A lattice model for condensation in Levin-Wen systems
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Christian, Jessica, Green, David, Huston, Peter, and Penneys, David
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Condensed Matter - Strongly Correlated Electrons ,Mathematical Physics ,Mathematics - Category Theory ,Mathematics - Quantum Algebra ,Quantum Physics ,18M20 (Primary) 81V27, 18M30, 57R56 (Secondary) - Abstract
Levin-Wen string-net models provide a construction of (2+1)D topologically ordered phases of matter with anyonic localized excitations described by the {Drinfeld} center of a unitary fusion category. Anyon condensation is a mechanism for phase transitions between (2+1)D topologically ordered phases. We construct an extension of Levin-Wen models in which tuning a parameter implements anyon condensation. We also describe the classification of anyons in Levin-Wen models via representation theory of the tube algebra, and use a variant of the tube algebra to classify low-energy localized excitations in the condensed phase., Comment: 45 pages; numerous figures
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- 2023
37. Cygnus X-3 revealed as a Galactic ultraluminous X-ray source by IXPE
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Veledina, Alexandra, Muleri, Fabio, Poutanen, Juri, Podgorný, Jakub, Dovčiak, Michal, Capitanio, Fiamma, Churazov, Eugene, De Rosa, Alessandra, Di Marco, Alessandro, Forsblom, Sofia, Kaaret, Philip, Krawczynski, Henric, La Monaca, Fabio, Loktev, Vladislav, Lutovinov, Alexander A., Molkov, Sergey V., Mushtukov, Alexander A., Ratheesh, Ajay, Cavero, Nicole Rodriguez, Steiner, James F., Sunyaev, Rashid A., Tsygankov, Sergey S., Zdziarski, Andrzej A., Bianchi, Stefano, Bright, Joe S., Bursov, Nikolaj, Costa, Enrico, Egron, Elise, Garcia, Javier A., Green, David A., Gurwell, Mark, Ingram, Adam, Kajava, Jari J. E., Kale, Ruta, Kraus, Alex, Malyshev, Denys, Marin, Frédéric, Matt, Giorgio, McCollough, Michael, Mereminskiy, Ilia A., Nizhelsky, Nikolaj, Piano, Giovanni, Pilia, Maura, Pittori, Carlotta, Rao, Ramprasad, Righini, Simona, Soffitta, Paolo, Shevchenko, Anton, Svoboda, Jiri, Tombesi, Francesco, Trushkin, Sergei, Tsybulev, Peter, Ursini, Francesco, Weisskopf, Martin C., Wu, Kinwah, Agudo, Iván, Antonelli, Lucio A., Bachetti, Matteo, Baldini, Luca, Baumgartner, Wayne H., Bellazzini, Ronaldo, Bongiorno, Stephen D., Bonino, Raffaella, Brez, Alessandro, Bucciantini, Niccolò, Castellano, Simone, Cavazzuti, Elisabetta, Chen, Chien-Ting, Ciprini, Stefano, Del Monte, Ettore, Di Gesu, Laura, Di Lalla, Niccolò, Donnarumma, Immacolata, Doroshenko, Victor, Ehlert, Steven R., Enoto, Teruaki, Evangelista, Yuri, Fabiani, Sergio, Ferrazzoli, Riccardo, Gunji, Shuichi, Hayashida, Kiyoshi, Heyl, Jeremy, Iwakiri, Wataru, Jorstad, Svetlana G., Karas, Vladimir, Kislat, Fabian, Kitaguchi, Takao, Kolodziejczak, Jeffery J., Latronico, Luca, Liodakis, Ioannis, Maldera, Simone, Manfreda, Alberto, Marinucci, Andrea, Marscher, Alan P., Marshall, Herman L., Massaro, Francesco, Mitsuishi, Ikuyuki, Mizuno, Tsunefumi, Negro, Michela, Ng, Chi-Yung, O'Dell, Stephen L., Omodei, Nicola, Oppedisano, Chiara, Papitto, Alessandro, Pavlov, George G., Peirson, Abel L., Perri, Matteo, Pesce-Rollins, Melissa, Petrucci, Pierre-Olivier, Possenti, Andrea, Puccetti, Simonetta, Ramsey, Brian D., Rankin, John, Roberts, Oliver, Romani, Roger W., Sgrò, Carmelo, Slane, Patrick, Spandre, Gloria, Swartz, Doug, Tamagawa, Toru, Tavecchio, Fabrizio, Taverna, Roberto, Tawara, Yuzuru, Tennant, Allyn F., Thomas, Nicholas E., Trois, Alessio, Turolla, Roberto, Vink, Jacco, Xie, Fei, and Zane, Silvia
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Astrophysics - High Energy Astrophysical Phenomena ,Astrophysics - Solar and Stellar Astrophysics - Abstract
The accretion of matter by compact objects can be inhibited by radiation pressure if the luminosity exceeds the critical value, known as the Eddington limit. Discovery of ultraluminous X-ray sources has shown that accretion can proceed even when the apparent luminosity significantly exceeds this limit. High apparent luminosity might be produced thanks to geometric beaming of the radiation by an outflow. The outflow half-opening angle, which determines the amplification due to beaming, has never been robustly constrained. Using the Imaging X-ray Polarimetry Explorer, we made the measurement of X-ray polarization in the Galactic X-ray binary Cyg X-3. We find high, over 20%, nearly energy-independent linear polarization, orthogonal to the direction of the radio ejections. These properties unambiguously indicate the presence of a collimating outflow in the X-ray binary Cyg~X-3 and constrain its half-opening angle, <15 degrees. Thus, the source can be used as a laboratory for studying the super-critical accretion regime. This finding underscores the importance of X-ray polarimetry in advancing our understanding of accreting sources., Comment: 52 pages, 14 figures, 3 tables. Author version of the article published in Nature Astronomy
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- 2023
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38. Mandated Leave Policies in the Context of Student Mental Health Challenges at Canadian Universities: A Framework Analysis
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Green, David S., Goldstein, Abby L., Yousaf, Amina, and Ansari, Negin
- Abstract
Although there is increased attention to the mental health needs of university students, far less attention has been given to mental health-related university policies. Many Canadian public universities have mandated leave policies that specify the conditions under which a student may be required to take a leave of absence from university. The purpose of the current study was to conduct an in-depth analysis of current mandated leave policies in public Canadian English-speaking universities. Applied framework analysis methodology was used to examine the approaches to balancing the needs of students experiencing mental health challenges and providing a safe environment on campus. Three primary themes regarding mandated leave policies were identified, including (a) approaches for addressing mental health concerns, (b) balancing the needs of the student with the needs of the institution, and (c) guidelines, standards, and quality assurance. Implications for mandated leave policies and approaches to students experiencing mental health challenges are discussed.
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- 2022
39. Critiquing the Learning Design of a SENCERized Team-Based Activity
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Green, David
- Abstract
A team-based learning activity is presented that was created to support a university-level course with an integrative theme of environmental sustainability. Students in a General Education "Environmental Biology" course were asked to relate academic concepts to real-world scenarios by creating a hypothetical ecoresort on an island that had suffered severe habitat degradation. The Earth Charter helped guide student understanding of how to balance ecological, social, and economic needs. Furthermore, the SENCER approach to educational practice helped teach the science through complex social issues. Student-generated media (in the form of a webpage) helped learners integrate and showcase their gains in knowledge and skills. The "ecoresort activity" is critiqued against educational best practices, by aligning its design with Fink's Taxonomy of Significant Learning and Merrill's Principles for Instructional Design. Finally, practical recommendations (with an accompanying facilitator's guide) are provided that should help STEM educators calibrate interacting variables during technology-enhanced course designs: permeable learning spaces, assessment strategies, and social learning settings.
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- 2022
40. Landing Style Influences Peak ‘Ground’ Reaction Forces during Repeated Jumping Using a Supine Jump Sled in Microgravity
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Price, Phil DB, Kennett, John E, Scott, Jonathan PR, Green, David A, and Cleather, Daniel J
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- 2024
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41. Sub-kpc radio jets in the brightest central galaxy of the cool-core galaxy cluster RXJ1720.1+2638
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Perrott, Yvette C., SM, Gopika, Edge, Alastair C., Grainge, Keith J. B., Green, David A., and Saunders, Richard D. E.
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Astrophysics - Astrophysics of Galaxies - Abstract
The cool-core galaxy cluster RXJ1720.1+2638 hosts extended radio emission near the cluster core, known as a minihalo. The origin of this emission is still debated and one piece of the puzzle has been the question of whether the supermassive black hole in the brightest central galaxy is actively powering jets. Here we present high-resolution e-MERLIN observations clearly indicating the presence of sub-kpc jets; this may have implications for the proposed origin of the minihalo emission, providing an ongoing source of relativistic electrons rather than a single burst sometime in the past, as previously assumed in simulations attempting to reproduce observational characteristics of minihalo-hosting systems., Comment: 5 pages, 4 figures. Minor changes from v1, accepted to MNRAS
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- 2022
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42. The Fourth Catalog of Active Galactic Nuclei Detected by the Fermi Large Area Telescope -- Data Release 3
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collaboration, The Fermi-LAT, Ajello, Marco, Baldini, Luca, Ballet, Jean, Bastieri, Denis, Gonzalez, Josefa Becerra, Bellazzini, Ronaldo, Berretta, Alessandra, Bissaldi, Elisabetta, Bonino, Raffaella, Brill, Ari, Bruel, Philippe, Buson, Sara, Caputo, Regina, Caraveo, Patrizia, Cheung, Teddy, Chiaro, Graziano, Cibrario, Nicolo, Ciprini, Stefano, Crnogorcevic, Milena, Cutini, Sara, D'Ammando, Filippo, De Gaetano, Salvatore, Di Lalla, Niccolo, Di Venere, Leonardo, Dominguez, Alberto, Ramazani, Vandad Fallah, Ferrara, Elizabeth, Fiori, Alessio, Fukazawa, Yasushi, Funk, Stefan, Fusco, Piergiorgio, Gammaldi, Viviana, Gargano, Fabio, Garrappa, Simone, Gasparrini, Dario, Giglietto, Nico, Giordano, Francesco, Giroletti, Marcello, Green, David, Grenier, Isabelle, Guiriec, Sylvain, Horan, Deirdre, Hou, Xian, Kayanoki, Taishu, Kuss, Michael, Larsson, Stefan, Latronico, Luca, Lewis, Tiffany, Li, Jian, Liodakis, Ioannis, Longo, Francesco, Loparco, Francesco, Lott, Benoit, Lovellette, Michael, Lubrano, Pasquale, Madejski, Grzegorz, Maldera, Simone, Manfreda, Alberto, Marti-Devesa, Guillem, Mazziotta, Mario Nicola, Mereu, Isabella, Michelson, Peter, Mirabal, Nestor, Mitthumsiri, Warit, Mizuno, Tsunefumi, Monzani, Maria Elena, Morselli, Aldo, Moskalenko, Igor, Negro, Michela, Ojha, Roopesh, Orienti, Monica, Orlando, Elena, Ormes, Jonathan F., Pei, Zhiyuan, Pena-Herazo, Harold A., Persic, Massimo, Pesce-Rollins, Melissa, Petrosian, Vahe, Pillera, Roberta, Poon, Helen, Porter, Troy, Principe, Giacomo, Raino, Silvia, Rando, Riccardo, Rani, Bindu, Razzano, Massimiliano, Razzaque, Soebur, Reimer, Anita, Reimer, Olaf, Scargle, Jeff, Scotton, Lorenzo, Serini, Davide, Sgro, Carmelo, Siskind, Eric J., Spandre, Gloria, Spinelli, Paolo, Suson, Dan, Tajima, Hiro, Torres, Diego F., Valverde, Janeth, Yassin, Hend, and Zaharijas, Gabrijela
- Subjects
Astrophysics - High Energy Astrophysical Phenomena ,Astrophysics - Astrophysics of Galaxies - Abstract
An incremental version of the fourth catalog of active galactic nuclei (AGNs) detected by the Fermi-Large Area Telescope is presented. This version (4LAC-DR3) derives from the third data release of the 4FGL catalog based on 12 years of E>50 MeV gamma-ray data, where the spectral parameters, spectral energy distributions (SEDs), yearly light curves, and associations have been updated for all sources. The new reported AGNs include 587 blazar candidates and four radio galaxies. We describe the properties of the new sample and outline changes affecting the previously published one. We also introduce two new parameters in this release, namely the peak energy of the SED high-energy component and the corresponding flux. These parameters allow an assessment of the Compton dominance, the ratio of the Inverse-Compton to the synchrotron peak luminosities, without relying on X-ray data., Comment: 13 pages, 7 figures, accepted for publication in The Astrophysical Journal Supplement Series. Fits files are available at https://fermi.gsfc.nasa.gov/ssc/data/access/lat/4LACDR3/ or alternatively at https://www.ssdc.asi.it/fermi4lac-DR3/table-4LAC-DR3-h.fits and https://www.ssdc.asi.it/fermi4lac-DR3/table-4LAC-DR3-l.fits
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- 2022
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43. Fusion Energy Sciences Exascale Requirements Review. An Office of Science review sponsored jointly by Advanced Scientific Computing Research and Fusion Energy Sciences, January 27-29, 2016, Gaithersburg, Maryland
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Chang, Choong-Seock, Greenwald, Martin, Riley, Katherine, Antypas, Katie, Coffey, Richard, Dart, Eli, Dosanjh, Sudip, Gerber, Richard, Hack, James, Monga, Inder, Papka, Michael E, Rotman, Lauren, Straatsma, Tjerk, Wells, Jack, Andre, R, Bernholdt, David, Bhattacharjee, Amitava, Bonoli, Paul, Boyd, Iain, Bulanov, Stepan, Cary, John R, Chen, Yang, Curreli, Davide, Ernst, Darin R, Ethier, Stephane, Green, David, Hager, Robert, Hakim, Ammar, Hassanein, A, Hatch, David, Held, ED, Howard, Nathan, Izzo, Valerie A, Jardin, Steve, Jenkins, TG, Jenko, Frank, Kemp, Andreas, King, Jacob, Kritz, Arnold, Krstic, Predrag, Kruger, Scott E, Kurtz, Rick, Lin, Zhihong, Loring, Burlen, Nandipati, Giridhar, Pankin, AY, Parker, Scott, Perez, Danny, Pigarov, Alex Y, Poli, Francesca, Pueschel, MJ, Rafiq, Tariq, Rübel, Oliver, Setyawan, Wahyu, Sizyuk, Valeryi A, Smithe, DN, Sovinec, CR, Turner, Miles, Umansky, Maxim, Vay, Jean-Luc, Verboncoeur, John, Vincenti, Henri, Voter, Arthur, Wang, Weixing, Wirth, Brian, Wright, John, and Yuan, X
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- 2022
44. Major and Minor Flares on Cygnus X-3 Revisited
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Spencer, Ralph E., Garrett, Michael, Bray, Justin D., and Green, David A.
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Astrophysics - Solar and Stellar Astrophysics - Abstract
Intense flares at cm-wavelengths reaching levels of tens of Jy have been observed from Cygnus X-3 for many years. This active high mass X-ray binary also has periods of quenching before major outbursts, and has minor flares at levels of a few hundred mJy. In this paper we show that the minor flares have much shorter rise times and durations suggesting more rapid expansion of the synchrotron radiation emitting material than in the strong flares. They also appear closer to the binary, whereas the large flares form a more developed jet. Calculations of physical conditions show that the minor out-bursts have lower minimum power but have larger magnetic fields and energy densities than the major flares. Minor flares can occur while a major flare is in progress, suggesting an indirect coupling between them. The spectral evolution of the minor flares can be explained by either an expanding synchrotron source or a shock model. The possibility that there is a brightening zone as in SS433 is explored., Comment: Accepted for publication in MNRAS
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- 2022
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45. Incremental Fermi Large Area Telescope Fourth Source Catalog
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collaboration, Fermi-LAT, Abdollahi, Soheila, Acero, Fabio, Baldini, Luca, Ballet, Jean, Bastieri, Denis, Bellazzini, Ronaldo, Berenji, Bijan, Berretta, Alessandra, Bissaldi, Elisabetta, Blandford, Roger D., Bloom, Elliott, Bonino, Raffaella, Brill, Ari, Britto, Richard J., Bruel, Philippe, Burnett, Toby H., Buson, Sara, Cameron, Rob A., Caputo, Regina, Caraveo, Patrizia A., Castro, Daniel, Chaty, Sylvain, Cheung, Teddy C., Chiaro, Graziano, Cibrario, Nicolo, Ciprini, Stefano, Coronado-Blazquez, Javier, Crnogorcevic, Milena, Cutini, Sara, D'Ammando, Filippo, De Gaetano, Salvatore, Digel, Seth W., Di Lalla, Niccolo, Dirirsa, Feraol F., Di Venere, Leonardo, Dominguez, Alberto, Ramazani, Vandad Fallah, Fegan, Stephen J., Ferrara, Elizabeth C., Fiori, Alessio, Fleischhack, Henrike, Franckowiak, Anna, Fukazawa, Yasushi, Funk, Stefan, Fusco, Piergiorgio, Galanti, Giorgio, Gammaldi, Viviana, Gargano, Fabio, Garrappa, Simone, Gasparrini, Dario, Giacchino, Federica, Giglietto, Nico, Giordano, Francesco, Giroletti, Marcello, Glanzman, Thomas, Green, David, Grenier, Isabelle A., Grondin, Marie-Helene, Guillemot, Lucas, Guiriec, Sylvain, Gustafsson, Michael, Harding, Alice K., Hays, Liz, Hewitt, John W., Horan, Deirdre, Hou, Xian, Johannesson, Gudlaugur, Karwin, Christopher M., Kayanoki, Taishu, Kerr, Matthew T., Kuss, Michael, Landriu, David, Larsson, Stefan, Latronico, Luca, Lemoine-Goumard, Marianne, Li, Jian, Liodakis, Ioannis, Longo, Francesco, Loparco, Francesco, Lott, Benoit, Lubrano, Pasquale, Maldera, Simone, Malyshev, Dmitry, Manfreda, Alberto, Marti-Devesa, Guillem, Mazziotta, Mario N., Mereu, Isabella, Meyer, Manuel, Michelson, Peter F., Mirabal, Nestor, Mitthumsiri, Warit, Mizuno, Tsunefumi, Moiseev, Alex A., Monzani, Maria E., Morselli, Aldo, Moskalenko, Igor V., Negro, Michela, Nuss, Eric, Omodei, Nicola, Orienti, Monica, Orlando, Elena, Paneque, David, Pei, Zhiyuan, Perkins, Jeremy S., Persic, Massimo, Pesce-Rollins, Melissa, Petrosian, Vahe, Pillera, Roberta, Poon, Helen, Porter, Troy A., Principe, Giacomo, Raino, Silvia, Rando, Riccardo, Rani, Bindu, Razzano, Massimiliano, Razzaque, Soebur, Reimer, Anita, Reimer, Olaf, Reposeur, Thierry, Sanchez-Conde, Miguel A., Parkinson, Pablo M. Saz, Scotton, Lorenzo, Serini, Davide, Sgro, Carmelo, Siskind, Eric J., Smith, David A., Spandre, Gloria, Spinelli, Paolo, Sueoka, Kohei, Suson, Dan J., Tajima, Hiro, Tak, Dongguen, Thayer, Jana B., Thompson, David J., Torres, Diego F., Troja, Eleonora, Valverde, Janeth, Wood, Kent, and Zaharijas, Gabrijela
- Subjects
Astrophysics - High Energy Astrophysical Phenomena - Abstract
We present an incremental version (4FGL-DR3, for Data Release 3) of the fourth Fermi-LAT catalog of gamma-ray sources. Based on the first twelve years of science data in the energy range from 50 MeV to 1 TeV, it contains 6658 sources. The analysis improves on that used for the 4FGL catalog over eight years of data: more sources are fit with curved spectra, we introduce a more robust spectral parameterization for pulsars, and we extend the spectral points to 1 TeV. The spectral parameters, spectral energy distributions, and associations are updated for all sources. Light curves are rebuilt for all sources with 1 yr intervals (not 2 month intervals). Among the 5064 original 4FGL sources, 16 were deleted, 112 are formally below the detection threshold over 12 yr (but are kept in the list), while 74 are newly associated, 10 have an improved association, and seven associations were withdrawn. Pulsars are split explicitly between young and millisecond pulsars. Pulsars and binaries newly detected in LAT sources, as well as more than 100 newly classified blazars, are reported. We add three extended sources and 1607 new point sources, mostly just above the detection threshold, among which eight are considered identified, and 699 have a plausible counterpart at other wavelengths. We discuss degree-scale residuals to the global sky model and clusters of soft unassociated point sources close to the Galactic plane, which are possibly related to limitations of the interstellar emission model and missing extended sources., Comment: accepted in ApJS; follow-up paper to 1902.10045
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- 2022
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46. European Aerosol Phenomenology -- 8: Harmonised Source Apportionment of Organic Aerosol using 22 Year-long ACSM/AMS Datasets
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Chen, Gang, Canonaco, Francesco, Tobler, Anna, Aas, Wenche, Alastuey, Andres, Allan, James, Atabakhsh, Samira, Aurela, Minna, Baltensperger, Urs, Bougiatioti, Aikaterini, De Brito, Joel F., Ceburnis, Darius, Chazeau, Benjamin, Chebaicheb, Hasna, Daellenbach, Kaspar R., Ehn, Mikael, Haddad, Imad El, Eleftheriadis, Konstantinos, Favez, Olivier, Flentje, Harald, Font, Anna, Fossum, Kirsten, Freney, Evelyn, Gini, Maria, Green, David C, Heikkinen, Liine, Herrmann, Hartmut, Kalogridis, Athina-Cerise, Keernik, Hannes, Lhotka, Radek, Lin, Chunshui, Lunder, Chris, Maasikmets, Marek, Manousakas, Manousos I., Marchand, Nicolas, Marin, Cristina, Marmureanu, Luminita, Mihalopoulos, Nikolaos, Močnik, Griša, Nęcki, Jaroslaw, O'Dowd, Colin, Ovadnevaite, Jurgita, Peter, Thomas, Petit, Jean-Eudes, Pikridas, Michael, Platt, Stephen Matthew, Pokorná, Petra, Poulain, Laurent, Priestman, Max, Riffault, Véronique, Rinaldi, Matteo, Różański, Kazimierz, Schwarz, Jaroslav, Sciare, Jean, Simon, Leïla, Skiba, Alicja, Slowik, Jay G., Sosedova, Yulia, Stavroulas, Iasonas, Styszko, Katarzyna, Teinemaa, Erik, Timonen, Hilkka, Tremper, Anja, Vasilescu, Jeni, Via, Marta, Vodička, Petr, Wiedensohler, Alfred, Zografou, Olga, Minguillón, María Cruz, and Prévôt, André S. H.
- Subjects
Physics - Atmospheric and Oceanic Physics - Abstract
Organic aerosol (OA) is a key component to total submicron particulate matter (PM1), and comprehensive knowledge of OA sources across Europe is crucial to mitigate PM1 levels. Europe has a well-established air quality research infrastructure from which yearlong datasets using 21 aerosol chemical speciation monitors (ACSMs) and 1 aerosol mass spectrometer (AMS) were gathered during 2013-2019. It includes 9 non-urban and 13 urban sites. This study developed a state-of-the-art source apportionment protocol to analyse long-term OA mass spectrum data by applying the most advanced source apportionment strategies (i.e., rolling PMF, ME-2, and bootstrap). This harmonised protocol enables the quantifications of the most common OA components such as hydrocarbon-like OA (HOA), biomass burning OA (BBOA), cooking-like OA (COA), more oxidised-oxygenated OA (MO-OOA), and less oxidised-oxygenated OA (LO-OOA). Other components such as coal combustion OA (CCOA), solid fuel OA (SFOA: mainly mixture of coal and peat combustion), cigarette smoke OA (CSOA), sea salt (mostly inorganic but part of the OA mass spectrum), coffee OA, and ship industry OA could also be separated at a few specific sites. Oxygenated OA (OOA) components make up most of the submicron OA mass (average = 71.1%, a range of 43.7-100%). Solid fuel combustion-related OA components (i.e., BBOA, CCOA, and SFOA) are still considerable with in total 16.0% yearly contribution to the OA, yet mainly during winter months (21.4%). Overall, this comprehensive protocol works effectively across all sites governed by different sources and generates robust and consistent source apportionment results. Our work presents a comprehensive overview of OA sources in Europe with a unique combination of high time resolution and long-term data coverage (9-36 months), providing essential information to improve/validate air quality, health impact, and climate models.
- Published
- 2022
- Full Text
- View/download PDF
47. Indoor air quality in subway microenvironments: Pollutant characteristics, adverse health impacts, and population inequity
- Author
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Wang, Shunyao, Qin, Tianchen, Tu, Ran, Li, Tianyuan, Chen, Gang I., Green, David C., Zhang, Xin, Feng, Jialiang, Liu, Haobing, Hu, Ming, and Fu, Qingyan
- Published
- 2024
- Full Text
- View/download PDF
48. Transperineal Versus Transrectal Magnetic Resonance Imaging–targeted and Systematic Prostate Biopsy to Prevent Infectious Complications: The PREVENT Randomized Trial
- Author
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Hu, Jim C., Assel, Melissa, Allaf, Mohamad E., Ehdaie, Behfar, Vickers, Andrew J., Cohen, Andrew J., Ristau, Benjamin T., Green, David A., Han, Misop, Rezaee, Michael E., Pavlovich, Christian P., Montgomery, Jeffrey S., Kowalczyk, Keith J., Ross, Ashley E., Kundu, Shilajit D., Patel, Hiten D., Wang, Gerald J., Graham, John N., Shoag, Jonathan E., Ghazi, Ahmed, Singla, Nirmish, Gorin, Michael A., Schaeffer, Anthony J., and Schaeffer, Edward M.
- Published
- 2024
- Full Text
- View/download PDF
49. A Review of Road Traffic-Derived Non-Exhaust Particles: Emissions, Physicochemical Characteristics, Health Risks, and Mitigation Measures
- Author
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Fussell, Julia C, Franklin, Meredith, Green, David C, Gustafsson, Mats, Harrison, Roy M, Hicks, William, Kelly, Frank J, Kishta, Franceska, Miller, Mark R, Mudway, Ian S, Oroumiyeh, Farzan, Selley, Liza, Wang, Meng, and Zhu, Yifang
- Subjects
Engineering ,Environmental Sciences ,Pollution and Contamination ,Climate-Related Exposures and Conditions ,Good Health and Well Being ,Air Pollutants ,Dust ,Environmental Monitoring ,Particle Size ,Particulate Matter ,Vehicle Emissions ,exposure assessment ,health effects ,mitigation ,nonexhaust emissions ,road traffic ,toxicity - Abstract
Implementation of regulatory standards has reduced exhaust emissions of particulate matter from road traffic substantially in the developed world. However, nonexhaust particle emissions arising from the wear of brakes, tires, and the road surface, together with the resuspension of road dust, are unregulated and exceed exhaust emissions in many jurisdictions. While knowledge of the sources of nonexhaust particles is fairly good, source-specific measurements of airborne concentrations are few, and studies of the toxicology and epidemiology do not give a clear picture of the health risk posed. This paper reviews the current state of knowledge, with a strong focus on health-related research, highlighting areas where further research is an essential prerequisite for developing focused policy responses to nonexhaust particles.
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- 2022
50. Fusion Energy Sciences Network Requirements Review (Final Report)
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Wala, Fatema, Bonoli, Paul, Brown, Ben, Chang, CS, Churchill, Michael, Cook, Brandon, Curry, Doug, Dart, Eli, Diallo, Ahmed, Dorland, Bill, Fiuza, Frederico, Foster, Mark, Gerber, Richard, Green, David, Guok, Chin, Guttenfelder, Walter, Hicks, Susan, Hier-Majumder, Saswata, Hughes, Jerry, Kafader, James, Kampel, Scott, Kaye, Stan, King, Josh, Lau, Cornwell, Mandrekas, John, Meneghini, Orso, Miller, Bill, Miller, Ken, Monga, Inder, Nazikian, Raffi, Nguyen, Jeff, Poli, Francesca, Rapp, Jurgen, Riley, Katherine, Rotman, Lauren, Sabbagh, Steve, Savage, Brandon, Schissel, David, Schumacher, Douglass, Stephey, Laurie, Stillerman, Josh, Wiedlea, Andrew, Youchison, Dennis, and Zurawski, Jason
- Abstract
The Energy Sciences Network (ESnet) is the high-performance network user facility for the US Department of Energy (DOE) Office of Science (SC) and delivers highly reliable data transport capabilities optimized for the requirements of data-intensive science. In essence, ESnet is the circulatory system that enables the DOE science mission by connecting all of its laboratories and facilities in the US and abroad. ESnet is funded and stewarded by the Advanced Scientific Computing Research (ASCR) program and managed and operated by the Scientific Networking Division at Lawrence Berkeley National Laboratory (LBNL). ESnet is widely regarded as a global leader in the research and education networking community.Throughout 2021, ESnet and the Office of Fusion Energy Sciences (FES) of the DOE SC organized an ESnet requirements review of FES-supported activities. Preparation for these events included identification of key stakeholders: program and facility management, research groups, and technology providers. Each stakeholder group was asked to prepare formal case study documents about their relationship to the FES program to build a complete understanding of the current, near-term, and long-term status, expectations, and processes that will support the science going forward.
- Published
- 2022
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