17,384 results on '"Furlan A"'
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2. Opioid Utilization and Management in the Setting of Stewardship During Inpatient Rehab Care
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Murphy L, Leblanc K, Badr S, Ching E, Mao L, Steenhof N, Hamandi B, Rubin B, Seto A, and Furlan AD
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opioid ,pain management ,medication reconciliation ,pharmacy practice ,medication safety ,discharge prescription. ,Medicine (General) ,R5-920 - Abstract
Laura Murphy,1– 3 Kori Leblanc,1,2,4 Souzi Badr,1,2 Emily Ching,1 Lynda Mao,1,2 Naomi Steenhof,1,2 Bassem Hamandi,1,2,4 Bonita Rubin,1,2 Ada Seto,1 Andrea D Furlan3,5,6 1Department of Pharmacy, University Health Network, Toronto, ON, Canada; 2Leslie Dan Faculty of Pharmacy, University of Toronto, Toronto, ON, Canada; 3KITE Research Institute, University Health Network, Toronto, ON, Canada; 4Toronto General Hospital Research Institute, University Health Network, Toronto, ON, Canada; 5Department of Medicine, University of Toronto, Toronto, ON, Canada; 6Institute for Work & Health, Toronto, ON, CanadaCorrespondence: Laura Murphy, Department of Pharmacy, University Health Network, 550 University Ave, Toronto, ON, M5G 2A2, Canada, Tel +1 416-597-3422 x 3657, Fax +1 416-260-2658, Email laura.murphy@uhn.caBackground: Opioid utilization and management in an inpatient rehabilitation setting have not been widely described, despite the unique opportunities that exist in this setting to support opioid stewardship across transitions in care. We aimed to characterize opioid utilization and management by interprofessional teams across a large, inpatient rehabilitation setting after incorporation of opioid stewardship principles by pharmacists as part of their daily practice.Patients and methods: This was a retrospective chart review at Toronto Rehab, University Health Network, Toronto, Canada. Patients with admission orders for any opioid from November 2017 to February 2018 were included. Complex continuing care and palliative care patients were excluded. Descriptive statistics were primarily used to describe the data as well as univariate linear regression to compare associations with milligram morphine equivalent (MME) reduction.Results: A total of 448 patients were included. A reduction in total daily MME was seen in 49% (n=219) of the patients during their inpatient stay, with 73% (n=159) of these patients having a reduction of ≥ 50%. Sixty-nine percent (n=311) of the patients received an opioid prescription at discharge, with most scheduled (90%, n=98) with a supply of less than 30 days. Rehabilitation length of stay was correlated with a MME decrease during rehab (p< 0.01), suggesting that longer lengths of stay contributed to a greater reduction in MME. Patients with chronic opioid use prior to acute care admission (p=0.01), and those who started extended-release opioids during acute care (p=0.02) were significantly less likely to discontinue opioids during rehab stay.Conclusion: Opioid utilization and management in the setting of opioid stewardship across inpatient rehab and transitions of care were characterized. Opportunities exist for further quality improvement initiatives within inpatient rehabilitation and acute care settings to identify and support patients with complex pain management needs.Keywords: opioid, pain management, medication reconciliation, pharmacy practice, medication safety, discharge prescription
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- 2022
3. TOI-3568 b: a super-Neptune in the sub-Jovian desert
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Martioli, E., Petrucci, R. P., Jofre, E., Hebrard, G., Ghezzi, L., Chew, Y. Gomez Maqueo, Diaz, R. F., Perottoni, H. D., Garcia, L. H., Rapetti, D., Etangs, A. Lecavelier des, de Almeida, L., Arnold, L., Artigau, E., Basant, R., Bean, J. L., Bieryla, A., Boisse, I., Bonfils, X., Brady, M., Cadieux, C., Carmona, A., Cook, N. J., Delfosse, X., Donati, J. -F., Doyon, R., Furlan, E., Howell, S. B., Jenkins, J. M., Kasper, D., Kiefer, F., Latham, D. W., Levine, A. M., Lorenzo-Oliveira, D., Luque, R., McLeod, K., Melendez, J., Moutou, C., Netto, Y., Pritchard, T. A., Rowden, P., Seifahrt, A., Stefansson, G., Sturmer, J., and Twicken, D. J
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Astrophysics - Earth and Planetary Astrophysics ,Astrophysics - Solar and Stellar Astrophysics - Abstract
The sub-Jovian desert is a region in the mass-period and radius-period parameter space, typically encompassing short-period ranges between super-Earths and hot Jupiters, that exhibits an intrinsic dearth of planets. This scarcity is likely shaped by photoevaporation caused by the stellar irradiation received by giant planets that have migrated inward. We report the detection and characterization of TOI-3568 b, a transiting super-Neptune with a mass of $26.4\pm1.0$ M$_\oplus$, a radius of $5.30\pm0.27$ R$_\oplus$, a bulk density of $0.98\pm0.15$ g cm$^{-3}$, and an orbital period of 4.417965(5) d situated in the vicinity of the sub-Jovian desert. This planet orbiting a K dwarf star with solar metallicity, was identified photometrically by TESS. It was characterized as a planet by our high-precision radial velocity monitoring program using MAROON-X at Gemini North, supplemented by additional observations from the SPICE large program with SPIRou at CFHT. We performed a Bayesian MCMC joint analysis of the TESS and ground-based photometry, MAROON-X and SPIRou radial velocities, to measure the orbit, radius, and mass of the planet, as well as a detailed analysis of the high-resolution flux and polarimetric spectra to determine the physical parameters and elemental abundances of the host star. Our results reveal TOI-3568 b as a hot super-Neptune, rich in hydrogen and helium with a core of heavier elements with a mass between 10 and 25 M$_\oplus$. We analyzed the photoevaporation status of TOI-3568 b and found that it experiences one of the highest EUV luminosities among planets with a mass M$_{\rm p}$ $<2$ M$_{\rm Nep}$, yet it has an evaporation lifetime exceeding 5 Gyr. Positioned in the transition between two significant populations of exoplanets on the mass-period and energy diagrams, this planet presents an opportunity to test theories concerning the origin of the sub-Jovian desert., Comment: Accepted for publication in A&A on September 4, 2024
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- 2024
4. Aircrew rostering workload patterns and associated fatigue and sleepiness scores in short/medium haul flights under RBAC 117 rules in Brazil
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Rodrigues, Tulio E., Furlan, Eduardo, Helene, André F., Helene, Otaviano, Pessini, Eduardo, Simões, Alexandre, Pontes, Maurício, and Fischer, Frida M.
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Physics - Physics and Society - Abstract
The relationships between workload and fatigue or sleepiness are investigated through the analysis of rosters and responses to questionnaires from Brazilian aircrews, taken from Fadig\^ometro database. The approach includes temporal markers - coinciding with Samn-Perelli (SP) and Karolinska Sleepiness Scale (KSS) responses - where SAFTE-FAST model outcomes are calculated. The model results follow the increase of fatigue and sleepiness perceptions during the dawn (0h00 to 05h59), but underestimate the self-rated scores during the evening (18h00 to 23h59). On the other hand, the KSS scores fit the relative risk of pilot errors, representing a reasonable proxy for risk assessment. Linear relationships obtained between workload metrics, computed within 168-hours prior to the responses, and self-rated SP and KSS scores provide a consistent method to estimate accumulated fatigue and sleepiness. Considering 7149 rosters of 2023, the duty time ($DT$), the number of flight sectors ($N_{CREW}$) and the sum of flight sectors with sit periods longer than one hour ($N_{CREW}+N_{SIT}$) are associated with 70.1%/60.6% of the highest predicted scores of SP/KSS. Applying the mitigations $DT\leq44h$, $N_{CREW}\leq15$ and $N_{CREW}+N_{SIT}\leq19$ for every 168-hour interval yields a significant decrease in the higher values of SP/KSS with minimal impact on aircrew productivity., Comment: 16 pages and 5 figures
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- 2024
5. GJ 238 b: A 0.57 Earth Radius Planet Orbiting an M2.5 Dwarf Star at 15.2 pc
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Tey, Evan, Shporer, Avi, Lin, Zifan, Stassun, Keivan G., Lissauer, Jack J., Hellier, Coel, Collins, Karen A., Collins, Kevin I., Wingham, Geof, Relles, Howard M., Mallia, Franco, Isopi, Giovanni, Kielkopf, John F., Conti, Dennis M., Schwarz, Richard P., Zapparata, Aldo, Giacalone, Steven, Furlan, Elise, Hartman, Zachary D., Howell, Steve B., Scott, Nicholas J., Ziegler, Carl, Briceno, Cesar, Law, Nicholas, Mann, Andrew W., Charbonneau, David, Essack, Zahra, Striegel, Stephanie, Ricker, George R., Vanderspek, Roland, Seager, Sara, Winn, Joshua N., and Jenkins, Jon M.
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Astrophysics - Earth and Planetary Astrophysics - Abstract
We report the discovery of the transiting planet GJ 238 b, with a radius of $0.566\pm0.014$ R$_{\oplus}$ ($1.064\pm0.026$ times the radius of Mars) and an orbital period of 1.74 day. The transit signal was detected by the TESS mission and designated TOI-486.01. The star's position close to the Southern ecliptic pole allows for almost continuous observations by TESS when it is observing the Southern sky. The host star is an M2.5 dwarf with $V=11.57\pm0.02$ mag, $K=7.030\pm0.023$ mag, a distance of $15.2156\pm0.0030$ pc, a mass of $0.4193_{-0.0098}^{+0.0095}$ M$_{\odot}$, a radius of $0.4314_{-0.0071}^{+0.0075}$ R$_{\odot}$, and an effective temperature of $3{,}485\pm140$ K. We validate the planet candidate by ruling out or rendering highly unlikely each of the false positive scenarios, based on archival data and ground-based follow-up observations. Validation was facilitated by the host star's small size and high proper motion, of $892.633\pm0.025$ mas yr$^{-1}$., Comment: Published in AJ
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- 2024
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6. TOI 762 A b and TIC 46432937 b: Two Giant Planets Transiting M Dwarf Stars
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Hartman, Joel D., Bayliss, Daniel, Brahm, Rafael, Bryant, Edward M., Jordán, Andrés, Bakos, Gáspár Á., Hobson, Melissa J., Sedaghati, Elyar, Bonfils, Xavier, Cointepas, Marion, Almenara, Jose Manuel, Barkaoui, Khalid, Timmermans, Mathilde, Dransfield, George, Ducrot, Elsa, Zúñiga-Fernández, Sebastián, Hooton, Matthew J., Pedersen, Peter Pihlmann, Pozuelos, Francisco J., Triaud, Amaury H. M. J., Gillon, Michaël, Jehin, Emmanuel, Waalkes, William C., Berta-Thompson, Zachory K., Howell, Steve B., Furlan, Elise, Ricker, George R., Vanderspek, Roland, Seager, Sara, Winn, Joshua N., Jenkins, Jon M., Rapetti, David, Collins, Karen A., Charbonneau, David, Burke, Christopher J., and Rodriguez, David R.
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Astrophysics - Earth and Planetary Astrophysics - Abstract
We present the discovery of TOI 762 A b and TIC 46432937 b, two giant planets transiting M dwarf stars. Transits of both systems were first detected from observations by the NASA TESS mission, and the transiting objects are confirmed as planets through high-precision radial velocity (RV) observations carried out with VLT/ESPRESSO. TOI 762 A b is a warm sub-Saturn with a mass of 0.251 +- 0.042 M_J, a radius of 0.744 +- 0.017 R_J, and an orbital period of 3.4717 d. It transits a mid-M dwarf star with a mass of 0.442 +- 0.025 M_S and a radius of 0.4250 +- 0.0091 R_S. The star TOI 762 A has a resolved binary star companion TOI 762 B that is separated from TOI 762 A by 3.2" (~ 319 AU) and has an estimated mass of 0.227 +- 0.010 M_S. The planet TIC 46432937 b is a warm Super-Jupiter with a mass of 3.20 +- 0.11 M_J and radius of 1.188 +- 0.030 R_J. The planet's orbital period is P = 1.4404 d, and it undergoes grazing transits of its early M dwarf host star, which has a mass of 0.563 +- 0.029 M_S and a radius of 0.5299 +- 0.0091 R_S. TIC 46432937 b is one of the highest mass planets found to date transiting an M dwarf star. TIC 46432937 b is also a promising target for atmospheric observations, having the highest Transmission Spectroscopy Metric or Emission Spectroscopy Metric value of any known warm Super-Jupiter (mass greater than 3.0 M_J, equilibrium temperature below 1000 K)., Comment: 29 pages, 7 figures, 8 tables, accepted for publication in AAS Journals
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- 2024
7. Timing irregularities and glitches from the pulsar monitoring campaign at IAR
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Zubieta, E., Garcia, F., del Palacio, S., Furlan, S. B. Araujo, Gancio, G., Lousto, C. O., Combi, J. A., and Espinoza, C. M.
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Astrophysics - High Energy Astrophysical Phenomena ,High Energy Physics - Phenomenology - Abstract
Context. Pulsars have a very stable rotation. However, sudden increases in their rotation frequency known as glitches, perturb their evolution. While large glitches are commonly detected, small glitches are harder to detect because of the lack of daily-cadence observations over long periods of time. Aims. We aim to explore the timing behaviour of young pulsars at daily timescales looking for small glitches and other irregularities. This will further our comprehension of the distribution of glitch sizes, which has also consequences for the theoretical modeling of the glitch mechanism. Methods. We observed six pulsars with up to daily cadence during 5 years with the antennas of the Argentine Institute of Radio Astronomy (IAR). We used standard pulsar timing tools to characterise the rotation of pulsars and developed an algorithm to look for small timing events in the data and calculate the changes in $\nu$ and $\dot\nu$ at those epochs. Results. We found that the rotation of pulsars in this dataset is affected by small step changes in $\nu$ and $\dot\nu$. We found three glitches that had not been reported before: two in PSR J1048-5832 with relative sizes $\Delta\nu / \nu= 9.1(4) \times 10^{-10}$ and $\Delta\nu / \nu = 4.5(1) \times 10^{-10}$, and one in the Vela pulsar with a size $\Delta\nu / \nu = 2.0(2) \times 10^{-10}$. We also report new decay terms on the 2021 Vela giant glitch, and on the 2022 giant glitches in PSR J0742-2822 and PSR J1740-3015 respectively. Besides, we found that the red noise contribution significantly diminished in PSR J0742-2822 after its giant glitch in 2022. Conclusions. Our results highlight the importance of high-cadence monitoring with an exhaustive analysis of the residuals to better characterize the distribution of glitch sizes and to deepen our understanding of the mechanisms behind glitches, red noise and timing irregularities.
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- 2024
8. The PLATO Mission
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Rauer, Heike, Aerts, Conny, Cabrera, Juan, Deleuil, Magali, Erikson, Anders, Gizon, Laurent, Goupil, Mariejo, Heras, Ana, Lorenzo-Alvarez, Jose, Marliani, Filippo, Martin-Garcia, Cesar, Mas-Hesse, J. Miguel, O'Rourke, Laurence, Osborn, Hugh, Pagano, Isabella, Piotto, Giampaolo, Pollacco, Don, Ragazzoni, Roberto, Ramsay, Gavin, Udry, Stéphane, Appourchaux, Thierry, Benz, Willy, Brandeker, Alexis, Güdel, Manuel, Janot-Pacheco, Eduardo, Kabath, Petr, Kjeldsen, Hans, Min, Michiel, Santos, Nuno, Smith, Alan, Suarez, Juan-Carlos, Werner, Stephanie C., Aboudan, Alessio, Abreu, Manuel, Acuña, Lorena, Adams, Moritz, Adibekyan, Vardan, Affer, Laura, Agneray, François, Agnor, Craig, Børsen-Koch, Victor Aguirre, Ahmed, Saad, Aigrain, Suzanne, Al-Bahlawan, Ashraf, Gil, M de los Angeles Alcacera, Alei, Eleonora, Alencar, Silvia, Alexander, Richard, Alfonso-Garzón, Julia, Alibert, Yann, Prieto, Carlos Allende, Almeida, Leonardo, Sobrino, Roi Alonso, Altavilla, Giuseppe, Althaus, Christian, Trujillo, Luis Alonso Alvarez, Amarsi, Anish, Eiff, Matthias Ammler-von, Amôres, Eduardo, Andrade, Laerte, Antoniadis-Karnavas, Alexandros, António, Carlos, del Moral, Beatriz Aparicio, Appolloni, Matteo, Arena, Claudio, Armstrong, David, Aliaga, Jose Aroca, Asplund, Martin, Audenaert, Jeroen, Auricchio, Natalia, Avelino, Pedro, Baeke, Ann, Baillié, Kevin, Balado, Ana, Balestra, Andrea, Ball, Warrick, Ballans, Herve, Ballot, Jerome, Barban, Caroline, Barbary, Gaële, Barbieri, Mauro, Forteza, Sebastià Barceló, Barker, Adrian, Barklem, Paul, Barnes, Sydney, Navascues, David Barrado, Barragan, Oscar, Baruteau, Clément, Basu, Sarbani, Baudin, Frederic, Baumeister, Philipp, Bayliss, Daniel, Bazot, Michael, Beck, Paul G., Bedding, Tim, Belkacem, Kevin, Bellinger, Earl, Benatti, Serena, Benomar, Othman, Bérard, Diane, Bergemann, Maria, Bergomi, Maria, Bernardo, Pierre, Biazzo, Katia, Bignamini, Andrea, Bigot, Lionel, Billot, Nicolas, Binet, Martin, Biondi, David, Biondi, Federico, Birch, Aaron C., Bitsch, Bertram, Ceballos, Paz Victoria Bluhm, Bódi, Attila, Bognár, Zsófia, Boisse, Isabelle, Bolmont, Emeline, Bonanno, Alfio, Bonavita, Mariangela, Bonfanti, Andrea, Bonfils, Xavier, Bonito, Rosaria, Bonomo, Aldo Stefano, Börner, Anko, Saikia, Sudeshna Boro, Martín, Elisa Borreguero, Borsa, Francesco, Borsato, Luca, Bossini, Diego, Bouchy, Francois, Boué, Gwenaël, Boufleur, Rodrigo, Boumier, Patrick, Bourrier, Vincent, Bowman, Dominic M., Bozzo, Enrico, Bradley, Louisa, Bray, John, Bressan, Alessandro, Breton, Sylvain, Brienza, Daniele, Brito, Ana, Brogi, Matteo, Brown, Beverly, Brown, David, Brun, Allan Sacha, Bruno, Giovanni, Bruns, Michael, Buchhave, Lars A., Bugnet, Lisa, Buldgen, Gaël, Burgess, Patrick, Busatta, Andrea, Busso, Giorgia, Buzasi, Derek, Caballero, José A., Cabral, Alexandre, Calderone, Flavia, Cameron, Robert, Cameron, Andrew, Campante, Tiago, Martins, Bruno Leonardo Canto, Cara, Christophe, Carone, Ludmila, Carrasco, Josep Manel, Casagrande, Luca, Casewell, Sarah L., Cassisi, Santi, Castellani, Marco, Castro, Matthieu, Catala, Claude, Fernández, Irene Catalán, Catelan, Márcio, Cegla, Heather, Cerruti, Chiara, Cessa, Virginie, Chadid, Merieme, Chaplin, William, Charpinet, Stephane, Chiappini, Cristina, Chiarucci, Simone, Chiavassa, Andrea, Chinellato, Simonetta, Chirulli, Giovanni, Christensen-Dalsgaard, Jorgen, Church, Ross, Claret, Antonio, Clarke, Cathie, Claudi, Riccardo, Clermont, Lionel, Coelho, Hugo, Coelho, Joao, Cogato, Fabrizio, Colomé, Josep, Condamin, Mathieu, Conseil, Simon, Corbard, Thierry, Correia, Alexandre C. M., Corsaro, Enrico, Cosentino, Rosario, Costes, Jean, Cottinelli, Andrea, Covone, Giovanni, Creevey, Orlagh L., Crida, Aurelien, Csizmadia, Szilard, Cunha, Margarida, Curry, Patrick, da Costa, Jefferson, da Silva, Francys, Dalal, Shweta, Damasso, Mario, Damiani, Cilia, Damiani, Francesco, Chagas, Maria Liduina das, Davies, Melvyn, Davies, Guy, Davies, Ben, Davison, Gary, de Almeida, Leandro, de Angeli, Francesca, de Barros, Susana Cristina Cabral, Leão, Izan de Castro, de Freitas, Daniel Brito, de Freitas, Marcia Cristina, De Martino, Domitilla, de Medeiros, José Renan, de Paula, Luiz Alberto, de Plaa, Jelle, De Ridder, Joris, Deal, Morgan, Decin, Leen, Deeg, Hans, Degl'Innocenti, Scilla, Deheuvels, Sebastien, del Burgo, Carlos, Del Sordo, Fabio, Delgado-Mena, Elisa, Demangeon, Olivier, Denk, Tilmann, Derekas, Aliz, Desidera, Silvano, Dexet, Marc, Di Criscienzo, Marcella, Di Giorgio, Anna Maria, Di Mauro, Maria Pia, Rial, Federico Jose Diaz, Díaz-García, José-Javier, Dima, Marco, Dinuzzi, Giacomo, Dionatos, Odysseas, Distefano, Elisa, Nascimento Jr., Jose-Dias do, Domingo, Albert, D'Orazi, Valentina, Dorn, Caroline, Doyle, Lauren, Duarte, Elena, Ducellier, Florent, Dumaye, Luc, Dumusque, Xavier, Dupret, Marc-Antoine, Eggenberger, Patrick, Ehrenreich, David, Eigmüller, Philipp, Eising, Johannes, Emilio, Marcelo, Eriksson, Kjell, Ermocida, Marco, Giribaldi, Riano Isidoro Escate, Eschen, Yoshi, Estrela, Inês, Evans, Dafydd Wyn, Fabbian, Damian, Fabrizio, Michele, Faria, João Pedro, Farina, Maria, Farinato, Jacopo, Feliz, Dax, Feltzing, Sofia, Fenouillet, Thomas, Ferrari, Lorenza, Ferraz-Mello, Sylvio, Fialho, Fabio, Fienga, Agnes, Figueira, Pedro, Fiori, Laura, Flaccomio, Ettore, Focardi, Mauro, Foley, Steve, Fontignie, Jean, Ford, Dominic, Fornazier, Karin, Forveille, Thierry, Fossati, Luca, Franca, Rodrigo de Marca, da Silva, Lucas Franco, Frasca, Antonio, Fridlund, Malcolm, Furlan, Marco, Gabler, Sarah-Maria, Gaido, Marco, Gallagher, Andrew, Galli, Emanuele, Garcia, Rafael A., Hernández, Antonio García, Munoz, Antonio Garcia, García-Vázquez, Hugo, Haba, Rafael Garrido, Gaulme, Patrick, Gauthier, Nicolas, Gehan, Charlotte, Gent, Matthew, Georgieva, Iskra, Ghigo, Mauro, Giana, Edoardo, Gill, Samuel, Girardi, Leo, Winter, Silvia Giuliatti, Giusi, Giovanni, da Silva, João Gomes, Zazo, Luis Jorge Gómez, Gomez-Lopez, Juan Manuel, Hernández, Jonay Isai González, Murillo, Kevin Gonzalez, Gorius, Nicolas, Gouel, Pierre-Vincent, Goulty, Duncan, Granata, Valentina, Grenfell, John Lee, Grießbach, Denis, Grolleau, Emmanuel, Grouffal, Salomé, Grziwa, Sascha, Guarcello, Mario Giuseppe, Gueguen, Loïc, Guenther, Eike Wolf, Guilhem, Terrasa, Guillerot, Lucas, Guiot, Pierre, Guterman, Pascal, Gutiérrez, Antonio, Gutiérrez-Canales, Fernando, Hagelberg, Janis, Haldemann, Jonas, Hall, Cassandra, Handberg, Rasmus, Harrison, Ian, Harrison, Diana L., Hasiba, Johann, Haswell, Carole A., Hatalova, Petra, Hatzes, Artie, Haywood, Raphaelle, Hébrard, Guillaume, Heckes, Frank, Heiter, Ulrike, Hekker, Saskia, Heller, René, Helling, Christiane, Helminiak, Krzysztof, Hemsley, Simon, Heng, Kevin, Hermans, Aline, Hermes, JJ, Torres, Nadia Hidalgo, Hinkel, Natalie, Hobbs, David, Hodgkin, Simon, Hofmann, Karl, Hojjatpanah, Saeed, Houdek, Günter, Huber, Daniel, Huesler, Joseph, Hui-Bon-Hoa, Alain, Huygen, Rik, Huynh, Duc-Dat, Iro, Nicolas, Irwin, Jonathan, Irwin, Mike, Izidoro, André, Jacquinod, Sophie, Jannsen, Nicholas Emborg, Janson, Markus, Jeszenszky, Harald, Jiang, Chen, Mancebo, Antonio José Jimenez, Jofre, Paula, Johansen, Anders, Johnston, Cole, Jones, Geraint, Kallinger, Thomas, Kálmán, Szilárd, Kanitz, Thomas, Karjalainen, Marie, Karjalainen, Raine, Karoff, Christoffer, Kawaler, Steven, Kawata, Daisuke, Keereman, Arnoud, Keiderling, David, Kennedy, Tom, Kenworthy, Matthew, Kerschbaum, Franz, Kidger, Mark, Kiefer, Flavien, Kintziger, Christian, Kislyakova, Kristina, Kiss, László, Klagyivik, Peter, Klahr, Hubert, Klevas, Jonas, Kochukhov, Oleg, Köhler, Ulrich, Kolb, Ulrich, Koncz, Alexander, Korth, Judith, Kostogryz, Nadiia, Kovács, Gábor, Kovács, József, Kozhura, Oleg, Krivova, Natalie, Kučinskas, Arunas, Kuhlemann, Ilyas, Kupka, Friedrich, Laauwen, Wouter, Labiano, Alvaro, Lagarde, Nadege, Laget, Philippe, Laky, Gunter, Lam, Kristine Wai Fun, Lambrechts, Michiel, Lammer, Helmut, Lanza, Antonino Francesco, Lanzafame, Alessandro, Martiz, Mariel Lares, Laskar, Jacques, Latter, Henrik, Lavanant, Tony, Lawrenson, Alastair, Lazzoni, Cecilia, Lebre, Agnes, Lebreton, Yveline, Etangs, Alain Lecavelier des, Leinhardt, Zoe, Leleu, Adrien, Lendl, Monika, Leto, Giuseppe, Levillain, Yves, Libert, Anne-Sophie, Lichtenberg, Tim, Ligi, Roxanne, Lignieres, Francois, Lillo-Box, Jorge, Linsky, Jeffrey, Liu, John Scige, Loidolt, Dominik, Longval, Yuying, Lopes, Ilídio, Lorenzani, Andrea, Ludwig, Hans-Guenter, Lund, Mikkel, Lundkvist, Mia Sloth, Luri, Xavier, Maceroni, Carla, Madden, Sean, Madhusudhan, Nikku, Maggio, Antonio, Magliano, Christian, Magrin, Demetrio, Mahy, Laurent, Maibaum, Olaf, Malac-Allain, LeeRoy, Malapert, Jean-Christophe, Malavolta, Luca, Maldonado, Jesus, Mamonova, Elena, Manchon, Louis, Mann, Andrew, Mantovan, Giacomo, Marafatto, Luca, Marconi, Marcella, Mardling, Rosemary, Marigo, Paola, Marinoni, Silvia, Marques, Érico, Marques, Joao Pedro, Marrese, Paola Maria, Marshall, Douglas, Perales, Silvia Martínez, Mary, David, Marzari, Francesco, Masana, Eduard, Mascher, Andrina, Mathis, Stéphane, Mathur, Savita, Figueiredo, Ana Carolina Mattiuci, Maxted, Pierre F. L., Mazeh, Tsevi, Mazevet, Stephane, Mazzei, Francesco, McCormac, James, McMillan, Paul, Menou, Lucas, Merle, Thibault, Meru, Farzana, Mesa, Dino, Messina, Sergio, Mészáros, Szabolcs, Meunier, Nadége, Meunier, Jean-Charles, Micela, Giuseppina, Michaelis, Harald, Michel, Eric, Michielsen, Mathias, Michtchenko, Tatiana, Miglio, Andrea, Miguel, Yamila, Milligan, David, Mirouh, Giovanni, Mitchell, Morgan, Moedas, Nuno, Molendini, Francesca, Molnár, László, Mombarg, Joey, Montalban, Josefina, Montalto, Marco, Monteiro, Mário J. P. F. G., Morales, Juan Carlos, Morales-Calderon, Maria, Morbidelli, Alessandro, Mordasini, Christoph, Moreau, Chrystel, Morel, Thierry, Morello, Guiseppe, Morin, Julien, Mortier, Annelies, Mosser, Benoît, Mourard, Denis, Mousis, Olivier, Moutou, Claire, Mowlavi, Nami, Moya, Andrés, Muehlmann, Prisca, Muirhead, Philip, Munari, Matteo, Musella, Ilaria, Mustill, Alexander James, Nardetto, Nicolas, Nardiello, Domenico, Narita, Norio, Nascimbeni, Valerio, Nash, Anna, Neiner, Coralie, Nelson, Richard P., Nettelmann, Nadine, Nicolini, Gianalfredo, Nielsen, Martin, Niemi, Sami-Matias, Noack, Lena, Noels-Grotsch, Arlette, Noll, Anthony, Norazman, Azib, Norton, Andrew J., Nsamba, Benard, Ofir, Aviv, Ogilvie, Gordon, Olander, Terese, Olivetto, Christian, Olofsson, Göran, Ong, Joel, Ortolani, Sergio, Oshagh, Mahmoudreza, Ottacher, Harald, Ottensamer, Roland, Ouazzani, Rhita-Maria, Paardekooper, Sijme-Jan, Pace, Emanuele, Pajas, Miriam, Palacios, Ana, Palandri, Gaelle, Palle, Enric, Paproth, Carsten, Parro, Vanderlei, Parviainen, Hannu, Granado, Javier Pascual, Passegger, Vera Maria, Pastor-Morales, Carmen, Pätzold, Martin, Pedersen, May Gade, Hidalgo, David Pena, Pepe, Francesco, Pereira, Filipe, Persson, Carina M., Pertenais, Martin, Peter, Gisbert, Petit, Antoine C., Petit, Pascal, Pezzuto, Stefano, Pichierri, Gabriele, Pietrinferni, Adriano, Pinheiro, Fernando, Pinsonneault, Marc, Plachy, Emese, Plasson, Philippe, Plez, Bertrand, Poppenhaeger, Katja, Poretti, Ennio, Portaluri, Elisa, Portell, Jordi, de Mello, Gustavo Frederico Porto, Poyatos, Julien, Pozuelos, Francisco J., Moroni, Pier Giorgio Prada, Pricopi, Dumitru, Prisinzano, Loredana, Quade, Matthias, Quirrenbach160, ndreas, Reina6, Julio Arturo Rabanal, Soares, Maria Cristina Rabello, Raimondo, Gabriella, Rainer, Monica, Rodón, Jose Ramón, Ramón-Ballesta, Alejandro, Zapata, Gonzalo Ramos, Rätz, Stefanie, Rauterberg, Christoph, Redman, Bob, Redmer, Ronald, Reese, Daniel, Regibo, Sara, Reiners, Ansgar, Reinhold, Timo, Renie, Christian, Ribas, Ignasi, Ribeiro, Sergio, Ricciardi, Thiago Pereira, Rice, Ken, Richard, Olivier, Riello, Marco, Rieutord, Michel, Ripepi, Vincenzo, Rixon, Guy, Rockstein, Steve, Rodríguez, María Teresa Rodrigo, Díaz, Luisa Fernanda Rodríguez, Garcia, Juan Pablo Rodriguez, Rodriguez-Gomez, Julio, Roehlly, Yannick, Roig, Fernando, Rojas-Ayala, Bárbara, Rolf, Tobias, Rørsted, Jakob Lysgaard, Rosado, Hugo, Rosotti, Giovanni, Roth, Olivier, Roth, Markus, Rousseau, Alex, Roxburgh, Ian, Roy, Fabrice, Royer, Pierre, Ruane, Kirk, Mastropasqua, Sergio Rufini, de Galarreta, Claudia Ruiz, Russi, Andrea, Saar, Steven, Saillenfest, Melaine, Salaris, Maurizio, Salmon, Sebastien, Saltas, Ippocratis, Samadi, Réza, Samadi, Aunia, Samra, Dominic, da Silva, Tiago Sanches, Carrasco, Miguel Andrés Sánchez, Santerne, Alexandre, Santoli, Francesco, Santos, Ângela R. G., Mesa, Rosario Sanz, Sarro, Luis Manuel, Scandariato, Gaetano, Schäfer, Martin, Schlafly, Edward, Schmider, François-Xavier, Schneider, Jean, Schou, Jesper, Schunker, Hannah, Schwarzkopf, Gabriel Jörg, Serenelli, Aldo, Seynaeve, Dries, Shan, Yutong, Shapiro, Alexander, Shipman, Russel, Sicilia, Daniela, Sanmartin, Maria Angeles Sierra, Sigot, Axelle, Silliman, Kyle, Silvotti, Roberto, Simon, Attila E., Napoli, Ricardo Simoyama, Skarka, Marek, Smalley, Barry, Smiljanic, Rodolfo, Smit, Samuel, Smith, Alexis, Smith, Leigh, Snellen, Ignas, Sódor, Ádám, Sohl, Frank, Solanki, Sami K., Sortino, Francesca, Sousa, Sérgio, Southworth, John, Souto, Diogo, Sozzetti, Alessandro, Stamatellos, Dimitris, Stassun, Keivan, Steller, Manfred, Stello, Dennis, Stelzer, Beate, Stiebeler, Ulrike, Stokholm, Amalie, Storelvmo, Trude, Strassmeier, Klaus, Strøm, Paul Anthony, Strugarek, Antoine, Sulis, Sophia, Švanda, Michal, Szabados, László, Szabó, Róbert, Szabó, Gyula M., Szuszkiewicz, Ewa, Talens, Geert Jan, Teti, Daniele, Theisen, Tom, Thévenin, Frédéric, Thoul, Anne, Tiphene, Didier, Titz-Weider, Ruth, Tkachenko, Andrew, Tomecki, Daniel, Tonfat, Jorge, Tosi, Nicola, Trampedach, Regner, Traven, Gregor, Triaud, Amaury, Trønnes, Reidar, Tsantaki, Maria, Tschentscher, Matthias, Turin, Arnaud, Tvaruzka, Adam, Ulmer, Bernd, Ulmer-Moll, Solène, Ulusoy, Ceren, Umbriaco, Gabriele, Valencia, Diana, Valentini, Marica, Valio, Adriana, Guijarro, Ángel Luis Valverde, Van Eylen, Vincent, Van Grootel, Valerie, van Kempen, Tim A., Van Reeth, Timothy, Van Zelst, Iris, Vandenbussche, Bart, Vasiliou, Konstantinos, Vasilyev, Valeriy, de Mascarenhas, David Vaz, Vazan, Allona, Nunez, Marina Vela, Velloso, Eduardo Nunes, Ventura, Rita, Ventura, Paolo, Venturini, Julia, Trallero, Isabel Vera, Veras, Dimitri, Verdugo, Eva, Verma, Kuldeep, Vibert, Didier, Martinez, Tobias Vicanek, Vida, Krisztián, Vigan, Arthur, Villacorta, Antonio, Villaver, Eva, Aparicio, Marcos Villaverde, Viotto, Valentina, Vorobyov, Eduard, Vorontsov, Sergey, Wagner, Frank W., Walloschek, Thomas, Walton, Nicholas, Walton, Dave, Wang, Haiyang, Waters, Rens, Watson, Christopher, Wedemeyer, Sven, Weeks, Angharad, Weingril, Jörg, Weiss, Annita, Wendler, Belinda, West, Richard, Westerdorff, Karsten, Westphal, Pierre-Amaury, Wheatley, Peter, White, Tim, Whittaker, Amadou, Wickhusen, Kai, Wilson, Thomas, Windsor, James, Winter, Othon, Winther, Mark Lykke, Winton, Alistair, Witteck, Ulrike, Witzke, Veronika, Woitke, Peter, Wolter, David, Wuchterl, Günther, Wyatt, Mark, Yang, Dan, Yu, Jie, Sanchez, Ricardo Zanmar, Osorio, María Rosa Zapatero, Zechmeister, Mathias, Zhou, Yixiao, Ziemke, Claas, and Zwintz, Konstanze
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Astrophysics - Instrumentation and Methods for Astrophysics ,Astrophysics - Earth and Planetary Astrophysics ,Astrophysics - Solar and Stellar Astrophysics - Abstract
PLATO (PLAnetary Transits and Oscillations of stars) is ESA's M3 mission designed to detect and characterise extrasolar planets and perform asteroseismic monitoring of a large number of stars. PLATO will detect small planets (down to <2 R_(Earth)) around bright stars (<11 mag), including terrestrial planets in the habitable zone of solar-like stars. With the complement of radial velocity observations from the ground, planets will be characterised for their radius, mass, and age with high accuracy (5 %, 10 %, 10 % for an Earth-Sun combination respectively). PLATO will provide us with a large-scale catalogue of well-characterised small planets up to intermediate orbital periods, relevant for a meaningful comparison to planet formation theories and to better understand planet evolution. It will make possible comparative exoplanetology to place our Solar System planets in a broader context. In parallel, PLATO will study (host) stars using asteroseismology, allowing us to determine the stellar properties with high accuracy, substantially enhancing our knowledge of stellar structure and evolution. The payload instrument consists of 26 cameras with 12cm aperture each. For at least four years, the mission will perform high-precision photometric measurements. Here we review the science objectives, present PLATO's target samples and fields, provide an overview of expected core science performance as well as a description of the instrument and the mission profile at the beginning of the serial production of the flight cameras. PLATO is scheduled for a launch date end 2026. This overview therefore provides a summary of the mission to the community in preparation of the upcoming operational phases.
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- 2024
9. The TESS-Keck Survey XX: 15 New TESS Planets and a Uniform RV Analysis of all Survey Targets
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Polanski, Alex S., Lubin, Jack, beard, Corey, Murphy, Jospeh M. Akana, Rubenzahl, Ryan, Hill, Michelle L., Crossfield, Ian J. M., Chontos, Ashley, Robertson, Paul, Isaacson, Howard, Kane, Stephen R., Ciardi, David R., Batalha, Natalie M., Dressing, Courtney, Fulton, Benjamin, Howard, Andrew W., Huber, Daniel, Petigura, Erik A., Weiss, Lauren M., Angelo, Isabel, Behmard, Aida, Blunt, Sarah, Brinkman, Casey L., Dai, Fei, Dalba, Paul A., Fetherolf, Tara, Giacalone, Steven, Hirsch, Lea A., Holcomb, Rae, Kosiarek, Molly R., Mayo, Andrew W., MacDougall, Mason G., Močnik, Teo, Pidhorodetska, Daria, Rice, Malena, Rosenthal, Lee J., Scarsdale, Nicholas, Turtelboom, Emma V., Tyler, Dakotah, Van Zandt, Judah, Yee, Samuel W., Coria, David R., Dulz, Shannon D., Hartman, Joel D., Householder, Aaron, Lange, Sarah, Langford, Andrew, Louden, Emma M., Gilbert, Emily A., Gonzales, Erica J., Schlieder, Joshua E., Boyle, Andrew W., Christiansen, Jessie L., Clark, Catherine A., Fernandes, Rachel B., Lund, Michael B., Savel, Arjun B., Gill, Holden, Beichman, Charles, Matson, Rachel, Matthews, Elisabeth C., Furlan, E., Howell, Steve B., Scott, Nicholas J., Everett, Mark E., Livingston, John H., Ershova, Irina O., Cheryasov, Dmitry V., Safonov, Boris, Lillo-Box, Jorge, Barrado, David, and Morales-Calderón, María
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Astrophysics - Earth and Planetary Astrophysics - Abstract
The Transiting Exoplanet Survey Satellite (TESS) has discovered hundreds of new worlds, with TESS planet candidates now outnumbering the total number of confirmed planets from $\textit{Kepler}$. Owing to differences in survey design, TESS continues to provide planets that are better suited for subsequent follow-up studies, including mass measurement through radial velocity (RV) observations, compared to Kepler targets. In this work, we present the TESS-Keck Survey's (TKS) Mass Catalog: a uniform analysis of all TKS RV survey data which has resulted in mass constraints for 126 planets and candidate signals. This includes 58 mass measurements that have reached $\geq5\sigma$ precision. We confirm or validate 32 new planets from the TESS mission either by significant mass measurement (15) or statistical validation (17), and we find no evidence of likely false positives among our entire sample. This work also serves as a data release for all previously unpublished TKS survey data, including 9,204 RV measurements and associated activity indicators over our three year survey. We took the opportunity to assess the performance of our survey, and found that we achieved many of our goals including measuring the mass of 38 small ($<4R_{\oplus}$) planets, nearly achieving the TESS mission's basic science requirement. In addition, we evaluated the performance of the Automated Planet Finder (APF) as survey support and observed meaningful constraints on system parameters due to its more uniform phase coverage. Finally, we compared our measured masses to those predicted by commonly used mass-radius relations and investigated evidence of systematic bias., Comment: 51 pages (22 of text), 24 figures
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- 2024
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10. The Discovery and Follow-up of Four Transiting Short-period Sub-Neptunes Orbiting M dwarfs
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Hori, Y., Fukui, A., Hirano, T., Narita, N., de Leon, J. P., Ishikawa, H. T., Hartman, J. D., Morello, G., García, N. Abreu, Hernández, L. Álvarez, Béjar, V. J. S., Calatayud-Borras, Y., Carleo, I., Enoc, G., Esparza-Borges, E., Fukuda, I., Galán, D., Geraldía-González, S., Hayashi, Y., Ikoma, M., Ikuta, K., Isogai, K., Kagetani, T., Kawai, Y., Kawauchi, K., Kimura, T., Kodama, T., Korth, J., Kusakabe, N., Laza-Ramos, A., Livingston, J. H., Luque, R., Miyakawa, K., Mori, M., Torres, S. Muñoz, Murgas, F., Orell-Miquel, J., Palle, E., Parviainen, H., Peláez-Torres, A., Puig-Subirá, M., Sánchez-Benavente, M., Sosa-Guillén, P., Stangret, M., Terada, Y., Watanabe, N., Bakos, G. Á., Barkaoui, K., Beichman, C., Benkhaldoun, Z., Boyle, A. W., Ciardi, D. R., Clark, C. A., Collins, K. A., Collins, K. I., Conti, D. M., Crossfield, I. J. M., Everett, M. E., Furlan, E., Ghachoui, M., Gillon, M., Gonzales, E. J., Higuera, J., Horne, K., Howell, S. B., Jehin, E., Lester, K. V., Lund, M. B., Matson, R., Matthews, E. C., Pozuelos, F. J., Safonov, B. S., Schlieder, J. E., Schwarz, R. P., Sefako, R., Srdoc, G., Strakhov, I. A., Waalkes, W. C., Ziegler, C., Charbonneau, D., Essack, Z., Timmermans, M., Guerrero, N. M., Harakawa, H., Hedges, C., Ishizuka, M., Jenkins, J. M., Konishi, M., Kotani, T., Kudo, T., Kurokawa, T., Kuzuhara, M., Nishikawa, J., Omiya, M., Ricker, G. R., Seager, S., Serizawa, T., Striegel, S., Tamura, M., Ueda, A., Vanderspek, R., Vievard, S., and Winn, J. N.
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Astrophysics - Earth and Planetary Astrophysics - Abstract
Sub-Neptunes with $2-3R_\oplus$ are intermediate in size between rocky planets and Neptune-sized planets. The orbital properties and bulk compositions of transiting sub-Neptunes provide clues to the formation and evolution of close-in small planets. In this paper, we present the discovery and follow-up of four sub-Neptunes orbiting M dwarfs (TOI-782, TOI-1448, TOI-2120, and TOI-2406), three of which were newly validated by ground-based follow-up observations and statistical analyses. TOI-782 b, TOI-1448 b, TOI-2120 b, and TOI-2406 b have radii of $R_\mathrm{p} = 2.740^{+0.082}_{-0.079}\,R_\oplus$, $2.769^{+0.073}_{-0.068}\,R_\oplus$, $2.120\pm0.067\,R_\oplus$, and $2.830^{+0.068}_{-0.066}\,R_\oplus$ and orbital periods of $P = 8.02$, $8.11$, $5.80$, and $3.08$\,days, respectively. Doppler monitoring with Subaru/InfraRed Doppler instrument led to 2$\sigma$ upper limits on the masses of $<19.1\ M_\oplus$, $<19.5\ M_\oplus$, $<6.8\ M_\oplus$, and $<15.6\ M_\oplus$ for TOI-782 b, TOI-1448 b, TOI-2120 b, and TOI-2406 b, respectively. The mass-radius relationship of these four sub-Neptunes testifies to the existence of volatile material in their interiors. These four sub-Neptunes, which are located above the so-called ``radius valley'', are likely to retain a significant atmosphere and/or an icy mantle on the core, such as a water world. We find that at least three of the four sub-Neptunes (TOI-782 b, TOI-2120 b, and TOI-2406 b) orbiting M dwarfs older than 1 Gyr, are likely to have eccentricities of $e \sim 0.2-0.3$. The fact that tidal circularization of their orbits is not achieved over 1 Gyr suggests inefficient tidal dissipation in their interiors., Comment: Accepted for publication in AJ, 32 pages, 17 figures, 6 tables
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- 2024
11. LI-RADS: a conceptual and historical review from its beginning to its recent integration into AASLD clinical practice guidance
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Elsayes KM, Kielar AZ, Chernyak V, Morshid A, Furlan A, Masch WR, Marks RM, Kamaya A, Do RKG, Kono Y, Fowler KJ, Tang A, Bashir MR, Hecht EM, Jambhekar K, Lyshchik A, Rodgers SK, Heiken JP, Kohli M, Fetzer DT, Wilson SR, Kassam Z, Mendiratta-Lala M, Singal AG, Lim CS, Cruite I, Lee J, Ash R, Mitchell DG, McInnes MDF, and Sirlin CB
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Liver imaging ,LI-RADS ,reporting ,cirrhosis ,HCC ,CT ,MRI ,US ,Neoplasms. Tumors. Oncology. Including cancer and carcinogens ,RC254-282 - Abstract
Khaled M Elsayes,1 Ania Z Kielar,2 Victoria Chernyak,3 Ali Morshid,1 Alessandro Furlan,4 William R Masch,5 Robert M Marks,6 Aya Kamaya,7 Richard KG Do,8 Yuko Kono,9 Kathryn J Fowler,9 An Tang,10 Mustafa R Bashir,11 Elizabeth M Hecht,12 Kedar Jambhekar,13 Andrej Lyshchik,14 Shuchi K Rodgers,14 Jay P Heiken,15 Marc Kohli,16 David T Fetzer,17 Stephanie R Wilson,18 Zahra Kassam,19 Mishal Mendiratta-Lala,5 Amit G Singal,17 Christopher S Lim,20 Irene Cruite,21 James Lee,22 Ryan Ash,23 Donald G Mitchell,14 Matthew DF McInnes,24 Claude B Sirlin9 1Department of Diagnostic Radiology, The University of Texas MD Anderson Cancer Center, Houston, TX, USA; 2Department of Radiology, University of Toronto, ON, Canada; 3Department of Radiology, Montefiore Medical Center, Bronx, NY, USA; 4Department of Radiology, University of Pittsburgh, Pittsburgh, PA, USA; 5Department of Radiology, University of Michigan, Ann Arbor, MI, USA; 6Department of Radiology, Naval Medical Center San Diego, Uniformed Services University of the Health Sciences, Bethesda, MD, USA; 7Department of Radiology, Stanford University Medical Center, Stanford, CA, USA; 8Department of Radiology, Memorial Sloan Kettering Cancer Center, New York, NY, USA; 9Department of Radiology, University of California San Diego, CA, USA; 10Department of Radiology, Centre Hospitalier de l’Université de Montréal (CHUM), Montreal, QC, Canada; 11Department of Radiology, Center for Advanced Magnetic Resonance Development, and Division of Gastroenterology, Department of Medicine, Duke University Medical Center, Durham, NC, USA; 12Department of Radiology, Columbia University Medical Center, New York, NY, USA; 13Department of Radiology, University of Arkansas for Medical Sciences, Little Rock, AR, USA; 14Department of Radiology, Einstein Medical Center, Philadelphia, PA, USA; 15Department of Radiology, Mayo Clinic, Rochester, MN, USA; 16Department of Radiology, University of California San Francisco, CA, USA; 17Division of Digestive and Liver Diseases, UT Southwestern Medical Center, Dallas, TX, USA; 18Department of Radiology, University of Calgary, Calgary, AB, Canada; 19Department of Diagnostic Imaging, Schulich School of Medicine, London, ON, Canada; 20Department of Medical Imaging, Sunnybrook Health Sciences Centre, University of Toronto, ON, Canada; 21Department of Radiology, Inland Imaging, Spokane, WA, USA; 22Department of Radiology, University of Kentucky, Lexington, KY, USA; 23Department of Radiology, University of Kansas, Kansas City, KS, USA; 24Department of Radiology, University of Ottawa, ON, Canada Abstract: The Liver Imaging Reporting and Data System (LI-RADS®) is a comprehensive system for standardizing the terminology, technique, interpretation, reporting, and data collection of liver observations in individuals at high risk for hepatocellular carcinoma (HCC). LI-RADS is supported and endorsed by the American College of Radiology (ACR). Upon its initial release in 2011, LI-RADS applied only to liver observations identified at CT or MRI. It has since been refined and expanded over multiple updates to now also address ultrasound-based surveillance, contrast-enhanced ultrasound for HCC diagnosis, and CT/MRI for assessing treatment response after locoregional therapy. The LI-RADS 2018 version was integrated into the HCC diagnosis, staging, and management practice guidance of the American Association for the Study of Liver Diseases (AASLD). This article reviews the major LI-RADS updates since its 2011 inception and provides an overview of the currently published LI-RADS algorithms. Keywords: LI-RADS, v2018, CT, MRI, CEUS, US, HCC, liver imaging, reporting, cirrhosis
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- 2019
12. On finite group global and gauged $q$-form symmetries in TQFT
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Furlan, Manuel and Putrov, Pavel
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Mathematical Physics ,Condensed Matter - Strongly Correlated Electrons ,High Energy Physics - Theory ,Mathematics - Algebraic Topology ,Mathematics - Geometric Topology - Abstract
We describe a method to implement finite group global and gauged $q$-form symmetries into the axiomatic structure of $d$-dimensional Topological Quantum Field Theory (TQFT) in terms of bordisms decorated by cohomology classes. Namely, on a manifold with a boundary, the gauge field is considered as a class in an appropriate relative cohomology group. It is defined in a way that allows self-consistent cutting and gluing of the manifolds and involves a choice of a $(d-q-2)$-skeleton in the boundary. The method, in a sense, generalizes to arbitrary $d$ and $q$ a method that has been considered in the literature in the case of $d=3,\;q=0,1$., Comment: 21 pages, 6 figures
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- 2024
13. JWST observations of $^{13}$CO$_{2}$ ice: Tracing the chemical environment and thermal history of ices in protostellar envelopes
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Brunken, Nashanty G. C., Rocha, Will R. M., van Dishoeck, Ewine F., Gutermuth, Robert, Tyagi, Himanshu, Slavicinska, Katerina, Nazari, Pooneh, Megeath, S. Thomas, Evans II, Neal J., Narang, Mayank, Manoj, P., Rubinstein, Adam E., Watson, Dan M., Looney, Leslie W., Linnartz, Harold, Garatti, Alessio Caratti o, Beuther, Henrik, Linz, Hendrik, Klaassen, Pamela, Poteet, Charles A., Federman, Samuel, Anglada, Guillem, Atnagulov, Prabhani, Bourke, Tyler L., Fischer, William J., Furlan, Elise, Green, Joel, Habel, Nolan, Hartmann, Lee, Karnath, Nicole, Osorio, Mayra, Page, James Muzerolle, Pokhrel, Riwaj, Rahatgaonkar, Rohan, Sheehan, Patrick, Stanke, Thomas, Stutz, Amelia M., Tobin, John J., Tychoniec, Lukasz, Wolk, Scott, and Yang, Yao-Lun
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Astrophysics - Astrophysics of Galaxies ,Astrophysics - Solar and Stellar Astrophysics - Abstract
The structure and composition of simple ices can be modified during stellar evolution by protostellar heating. Key to understanding the involved processes are thermal and chemical tracers that can diagnose the history and environment of the ice. The 15.2 $\mu$m bending mode of $^{12}$CO$_2$ has proven to be a valuable tracer of ice heating events but suffers from grain shape and size effects. A viable alternative tracer is the weaker $^{13}$CO$_2$ isotopologue band at 4.39 $\mu$m which has now become accessible at high S/N with the $\textit{James Webb}$ Space Telescope (JWST). We present JWST NIRSpec observations of $^{13}$CO$_2$ ice in five deeply embedded Class 0 sources spanning a wide range in luminosities (0.2 - 10$^4$ L$_{\odot}$ ) taken as part of the Investigating Protostellar Accretion Across the Mass Spectrum (IPA) program. The band profiles vary significantly, with the most luminous sources showing a distinct narrow peak at 4.38 $\mu$m. We first apply a phenomenological approach and show that a minimum of 3-4 Gaussian profiles are needed to fit the $^{13}$CO$_2$ absorption feature. We then combine these findings with laboratory data and show that a 15.2 $\mu$m $^{12}$CO$_2$ band inspired five-component decomposition can be applied for the isotopologue band where each component is representative of CO$_2$ ice in a specific molecular environment. The final solution consists of cold mixtures of CO$_2$ with CH$_3$OH, H$_2$O and CO as well as segregated heated pure CO$_2$ ice. Our results are in agreement with previous studies of the $^{12}$CO$_2$ ice band, further confirming that $^{13}$CO$_{2}$ is a useful alternative tracer of protostellar heating events. We also propose an alternative solution consisting only of heated CO$_2$:CH$_3$OH and CO$_2$:H$_2$O ices and warm pure CO$_2$ ice for decomposing the ice profiles of the two most luminous sources in our sample.
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- 2024
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14. Revised Architecture and Two New Super-Earths in the HD 134606 Planetary System
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Li, Zhexing, Kane, Stephen R., Brandt, Timothy D., Fetherolf, Tara, Robertson, Paul, Zhao, Jinglin, Dalba, Paul A., Wittenmyer, Robert A., Butler, R. Paul, Diaz, Matias R., Howell, Steve B., Bailey, Jeremy, Carter, Brad, Furlan, Elise, Gnilka, Crystal L., Jones, Hugh R. A., O'Toole, Simon, and Tinney, Chris
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Astrophysics - Earth and Planetary Astrophysics - Abstract
Multi-planet systems exhibit a diversity of architectures that diverge from the solar system and contribute to the topic of exoplanet demographics. Radial velocity (RV) surveys form a crucial component of exoplanet surveys, as their long observational baselines allow searches for more distant planetary orbits. This work provides a significantly revised architecture for the multi-planet system HD 134606 using both HARPS and UCLES RVs. We confirm the presence of previously reported planets b, c, and d with periods $12.0897^{+0.0019}_{-0.0018}$, $58.947^{+0.056}_{-0.054}$, and $958.7^{+6.3}_{-5.9}$ days, and masses $9.14^{+0.65}_{-0.63}$, $11.0\pm1$, and $44.5\pm2.9$ Earth masses respectively, with the planet d orbit significantly revised to over double that originally reported. We report two newly detected super-Earths, e and f, with periods $4.31943^{+0.00075}_{-0.00068}$ and $26.9^{+0.019}_{-0.017}$ days, and masses $2.31^{+0.36}_{-0.35}$ and $5.52^{+0.74}_{-0.73}$ Earth masses, respectively. In addition, we identify a linear trend in the RV time series, and the cause of this acceleration is deemed to be a newly detected sub-stellar companion at large separation. HD 134606 now displays four low mass planets in a compact region near the star, one gas giant further out in the Habitable Zone, an additional massive companion in the outer regime, and a low mass M dwarf stellar companion at large separation, making it an intriguing target for system formation/evolution studies. The location of planet d in the Habitable Zone proves to be an exciting candidate for future space-based direct imaging missions, whereas continued RV observations of this system are recommended for understanding the nature of the massive, long period companion., Comment: 23 pages, 10 figures, 4 tables, accepted for publication in the Astronomical Journal
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- 2024
15. Revisiting the warm sub-Saturn TOI-1710b
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Orell-Miquel, J., Carleo, I., Murgas, F., Nowak, G., Palle, E., Luque, R., Masseron, T., Sanz-Forcada, J., Dragomir, D., Dalba, P. A., Tronsgaard, R., Wittrock, J., Kim, K., Stibbards, C., Collins, K. I., Plavchan, P., Howell, S. B., Furlan, E., Buchhave, L. A., Gnilka, C. L., Gupta, A. F., Henning, Th., Lester, K. V., Rodriguez, J. E., Scott, N. J., Osborn, H. P., Villanueva Jr., S., Seager, S., Winn, J. N., Jenkins, J. M., Vanderspek, R., Latham, D. W., Rowden, P., Watanabe, D., Torres, G., Burke, C. J., Daylan, T., Barclay, T., Twicken, J. D., and Ricker, G. R.
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Astrophysics - Earth and Planetary Astrophysics - Abstract
The Transiting Exoplanet Survey Satellite (TESS) provides a continuous suite of new planet candidates that need confirmation and precise mass determination from ground-based observatories. This is the case for the G-type star TOI-1710, which is known to host a transiting sub-Saturn planet ($\mathrm{M_p}=$28.3$\pm$4.7$\mathrm{M}_\oplus$) in a long-period orbit (P=24.28\,d). Here we combine archival SOPHIE and new and archival HARPS-N radial velocity data with newly available TESS data to refine the planetary parameters of the system and derive a new mass measurement for the transiting planet, taking into account the impact of the stellar activity on the mass measurement. We report for TOI-1710b a radius of $\mathrm{R_p}$$=$5.15$\pm$0.12$\mathrm{R}_\oplus$, a mass of $\mathrm{M_p}$$=$18.4$\pm$4.5$\mathrm{M}_\oplus$, and a mean bulk density of $\rho_{\rm p}$$=$0.73$\pm$0.18$\mathrm{g \, cm^{-3}}$, which are consistent at 1.2$\sigma$, 1.5$\sigma$, and 0.7$\sigma$, respectively, with previous measurements. Although there is not a significant difference in the final mass measurement, we needed to add a Gaussian process component to successfully fit the radial velocity dataset. This work illustrates that adding more measurements does not necessarily imply a better mass determination in terms of precision, even though they contribute to increasing our full understanding of the system. Furthermore, TOI-1710b joins an intriguing class of planets with radii in the range 4-8 $\mathrm{R}_\oplus$ that have no counterparts in the Solar System. A large gaseous envelope and a bright host star make TOI-1710b a very suitable candidate for follow-up atmospheric characterization., Comment: Accepted for publication in A&A. 21 pages, 14 figures
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- 2024
16. A macro-level circular economy index: theoretical proposal and application in European Union countries
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de Oliveira Frascareli, Fernanda Cortegoso, Furlan, Marcelo, Mariano, Enzo Barberio, and Jugend, Daniel
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- 2024
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17. Prospects for Detecting Fast Transients with the Radio Telescopes of the Argentine Institute of Radio Astronomy
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Furlan, Susana Beatriz Araujo, Zubieta, Ezequiel, Gancio, Guillermo, Romero, Gustavo Esteban, del Palacio, Santiago, García, Federico, Lousto, Carlos Oscar, and Combi, Jorge Ariel
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Astrophysics - High Energy Astrophysical Phenomena - Abstract
Currently, 6 out of 30 known magnetars had pulsed radio emission detected. In this work, we evaluated the possibility of detecting radio transient events from magnetars with the telescopes of the Instituto Argentino de Radioastronom\'ia (IAR). To this aim, we made daily observations of the magnetar XTE~J1810$-$197 from 02-Sep-22 to 30-Nov-22. We analysed the observations by applying ephemeris folding and single pulse searches. We fitted a timing model to our observations and were able to detect the magnetar on 6 of the 36 observing sessions with signal-to-noise ratios at the limit of detectability, $3.3\leq \mathrm{S/N} \leq4.1$. We searched for individual pulses in one of these 6 days and found 7 individual pulses with $8.5\leq \mathrm{S/N} \leq18.8$. The dispersion measure changed slightly between pulses within a range of $178 \leq \textrm{DM} \,[\mathrm{pc\, cm^{-3}}] \leq 182$. The pulse with $\mathrm{S/N}=18.8$ has an associated $\textrm{DM}$ of $180\,\mathrm{pc\, cm^{-3}}$. We confirmed that we can detect pulsed radio emission in the band of $1400-1456\, \mathrm{MHz}$ from magnetars with a time resolution of $146\,\mu s$, being able to detect both integrated pulse profiles and individual pulses., Comment: 6 pages, 3 figures
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- 2023
18. High-Resolution Imaging of a TESS Control Sample: Verifying a Deficit of Close-In Stellar Companions to Exoplanet Host Stars
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Littlefield, Colin, Howell, Steve B., Ciardi, David R., Lester, Kathryn V., Everett, Mark E., Furlan, Elise, Matson, Rachel A., Fajardo-Acosta, Sergio B., and Gnilka, Crystal L.
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Astrophysics - Solar and Stellar Astrophysics ,Astrophysics - Earth and Planetary Astrophysics - Abstract
The large number of exoplanets discovered with the Transiting Exoplanet Survey Satellite (TESS) means that any observational biases from TESS could influence the derived stellar multiplicity statistics of exoplanet host stars. To investigate this problem, we obtained speckle interferometry of 207 control stars whose properties in the TESS Input Catalog (TIC) closely match those of an exoplanetary host star in the TESS Object of Interest (TOI) catalog, with the objective of measuring the fraction of these stars that have companions within $\sim1.2"$. Our main result is the identification of a bias in the creation of the control sample that prevents the selection of binaries with $0.1" \lesssim \rho \lesssim 1.2"$ and $\Delta$mag $\lesssim3$. This bias is the result of large astrometric residuals that cause binaries with these parameters to fail the quality checks used to create the TIC, which in turn causes them to have incomplete stellar parameters (and uncertainties) in the TIC. Any stellar multiplicity study that relies exclusively upon TIC stellar parameters to identify its targets will struggle to select unresolved binaries in this parameter space. Left uncorrected, this selection bias disproportionately excludes high-mass-ratio binaries, causing the mass-ratio distribution of the companions to deviate significantly from the uniform distribution expected of FGK-type field binaries. After accounting for this bias, the companion rate of the FGK control stars is consistent with the canonical $46\pm2\%$ rate from Raghavan et al. 2010, and the mass-ratio distribution agrees with that of binary TOI host stars. There is marginal evidence that the control-star companions have smaller projected orbital separations than TOI host stars from previous studies., Comment: AJ accepted for publication
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- 2023
19. Updates on the glitching pulsar monitoring campaign performed from IAR
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Zubieta, Ezequiel, del Palacio, Santiago, García, Federico, Furlan, Susana Beatriz Araujo, Gancio, Guillermo, Lousto, Carlos Oscar, and Combi, Jorge Ariel
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Astrophysics - High Energy Astrophysical Phenomena ,High Energy Physics - Phenomenology - Abstract
Pulsars are known for their exceptionally stable rotation. However, this stability can be disrupted by glitches, sudden increases in rotation frequency whose cause is poorly understood. In this study, we present some preliminary results from the pulsar monitoring campaign conducted at the IAR since 2019. We present measurements from timing solution fits of the parameters of five glitches: one glitch in the Vela pulsar, one in PSR J0742-2822, one in PSR J1740-3015, and two mini-glitches in PSR J1048-5832. Finally, we applied the vortex creep model to characterize the inter-glitch period of Vela. However, the preliminary results yielded highly degenerate and loosely constrained parameters.
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- 2023
20. Multi-trap optical tweezers based on Kinoform Silver Mean lenses
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Muñoz-Pérez, Francisco M., Garmendía-Martínez, Adrián, Ferrando, Vicente, Castro-Palacio, Juan C., Furlan, Walter D., and Monsoriu, Juan A.
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Physics - Optics - Abstract
In this paper, we present the design and implementation of multi-trap optical tweezers based on new quadrifocal kinoform lenses. The phase distribution of these diffractive lenses is characterized by the Silver Mean sequence. The focusing properties of the resulting aperiodic DOEs coined Kinoform Silver Mean Lenses (KSMLs) are numerically examined. It is shown that, under monochromatic illumination, a KSML drives most of the incoming light into four single foci whose focal lengths are related to the Silver ratio. In this way, a KSML improves the diffraction efficiency of binary Fresnel Silver Mean Zone Plates. Through experimental results, the simultaneous trapping of particles in the four focal planes and their three-dimensional manipulation is demonstrated.
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- 2023
21. TOI-1736 and TOI-2141: two systems including sub-Neptunes around solar analogs revealed by TESS and SOPHIE
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Martioli, E., Hébrard, G., de Almeida, L., Heidari, N., Lorenzo-Oliveira, D., Kiefer, F., Almenara, J. M., Bieryla, A., Boisse, I., Bonfils, X., Briceño, C., Collins, K. A., Cortés-Zuleta, P., Dalal, S., Deleuil, M., Delfosse, X., Demangeon, O., Eastman, J. D., Furlan, T. ForveilleE., Howell, S. B., Hoyer, S., Jenkins, J. M., Latham, D. W., Law, N., Mann, A. W., Moutou, C., Santos, N. C., Sousa, S. G., Stassun, K. G., Stockdale, C., Torres, G., Twicken, J. D., Winn, J. N., and Ziegler, C.
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Astrophysics - Earth and Planetary Astrophysics - Abstract
Planetary systems around solar analogs inform us about how planets form and evolve in Solar System-like environments. We report the detection and characterization of two planetary systems around the solar analogs TOI-1736 and TOI-2141 using TESS photometry data and spectroscopic data obtained with the SOPHIE instrument on the 1.93 m telescope at the Observatoire de Haute-Provence (OHP). We performed a detailed spectroscopic analysis of these systems to obtain the precise radial velocities (RV) and physical properties of their host stars. TOI-1736 and TOI-2141 each host a transiting sub-Neptune with radii of $2.44\pm0.18$ R$_{\oplus}$ and $3.05\pm0.23$ R$_{\oplus}$, orbital periods of $7.073088(7)$ d and $18.26157(6)$ d, and masses of $12.8\pm1.8$ M$_{\oplus}$ and $24\pm4$ M$_{\oplus}$, respectively. TOI-1736 shows long-term RV variations that are consistent with a two-planet solution plus a linear trend of $-0.177$ ms$^{-1}$d$^{-1}$. We measured an RV semi-amplitude of $201.1\pm0.7$ ms$^{-1}$ for the outer companion, TOI-1736 c, implying a projected mass of $m_{c}\sin{i}=8.09\pm0.20$ M$_{\rm Jup}$. From the GAIA DR3 astrometric excess noise, we constrained the mass of TOI-1736 c at $8.7^{+1.5}_{-0.6}$ M$_{\rm Jup}$. This planet is in an orbit of $570.2\pm0.6$ d with an eccentricity of $0.362\pm0.003$ and a semi-major axis of $1.381\pm0.017$ au, where it receives a flux of $0.71\pm0.08$ times the bolometric flux incident on Earth, making it an interesting case of a supergiant planet that has settled into an eccentric orbit in the habitable zone of a solar analog. Our analysis of the mass-radius relation for the transiting sub-Neptunes shows that both TOI-1736 b and TOI-2141 b likely have an Earth-like dense rocky core and a water-rich envelope., Comment: Accepted for publication in A&A on October 6, 2023
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- 2023
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22. Discovery of a collimated jet from the low luminosity protostar IRAS 16253$-$2429 in a quiescent accretion phase with the JWST
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Narang, Mayank, P., Manoj, Tyagi, Himanshu, Watson, Dan M., Megeath, S. Thomas, Federman, Samuel, Rubinstein, Adam E., Gutermuth, Robert, Garatti, Alessio Caratti o, Beuther, Henrik, Bourke, Tyler L., Van Dishoeck, Ewine F., Evans II, Neal J., Anglada, Guillem, Osorio, Mayra, Stanke, Thomas, Muzerolle, James, Looney, Leslie W., Yang, Yao-Lun, Tobin, John J., Klaassen, Pamela, Karnath, Nicole, Atnagulov, Prabhani, Brunken, Nashanty, Fischer, William J., Furlan, Elise, Green, Joel, Habel, Nolan, Hartmann, Lee, Linz, Hendrik, Nazari, Pooneh, Pokhrel, Riwaj, Rahatgaonkar, Rohan, Rocha, Will R. M., Sheehan, Patrick, Slavicinska, Katerina, Stutz, Amelia, Tychoniec, Lukasz, and Wolk, Scott
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Astrophysics - Solar and Stellar Astrophysics ,Astrophysics - Astrophysics of Galaxies - Abstract
Investigating Protostellar Accretion (IPA) is a JWST Cycle~1 GO program that uses NIRSpec IFU and MIRI MRS to obtain 2.9--28~$\mu$m spectral cubes of young, deeply embedded protostars with luminosities of 0.2 to 10,000~L$_{\odot}$ and central masses of 0.15 to 12~M$_{\odot}$. In this Letter, we report the discovery of a highly collimated atomic jet from the Class~0 protostar IRAS~16253$-$2429, the lowest luminosity source ($L_\mathrm{bol}$ = 0.2 $L_\odot$) in the IPA program. The collimated jet is detected in multiple [Fe~II] lines, [Ne~II], [Ni~II], and H~I lines, but not in molecular emission. The atomic jet has a velocity of about 169~$\pm$~15~km\,s$^{-1}$, after correcting for inclination. The width of the jet increases with distance from the central protostar from 23 to~60 au, corresponding to an opening angle of 2.6~$\pm$~0.5\arcdeg. By comparing the measured flux ratios of various fine structure lines to those predicted by simple shock models, we derive a shock {speed} of 54~km\,s$^{-1}$ and a preshock density of 2.0$\times10^{3}$~cm$^{-3}$ at the base of the jet. {From these quantities and using a suite of jet models and extinction laws we compute a mass loss rate between $0.4 -1.1\times10^{-10}~M_{\odot}$~yr~$^{-1}$.} The low mass loss rate is consistent with simultaneous measurements of low mass accretion rate ($2.4~\pm~0.8~\times~10^{-9}~M_{\odot}$~yr$^{-1}$) for IRAS~16253$-$2429 from JWST observations (Watson et al. in prep), indicating that the protostar is in a quiescent accretion phase. Our results demonstrate that very low-mass protostars can drive highly collimated, atomic jets, even during the quiescent phase., Comment: Accepted to ApJL. Comments and feedback welcome
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- 2023
23. Confirmation of a Sub-Saturn-size transiting exoplanet orbiting a G dwarf: TOI-1194 b and a very low mass companion star: TOI-1251 B from TESS
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Wang, Jia-Qi, Jiang, Xiao-Jun, Zheng, Jie, Kellermann, Hanna, Riffeser, Arno, Wang, Liang, Collins, Karen A., Bieryla, Allyson, Buchhave, Lars A., Howell, Steve B., Furlan, Elise, Girardin, Eric, Gregorio, Joao, Jensen, Eric, Murgas, Felipe, Yilmaz, Mesut, Quinn, Sam, Gao, Xing, Zhou, Ruo-Yu, Grupp, Frank, and Wang, Hui-Juan
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Astrophysics - Earth and Planetary Astrophysics ,Astrophysics - Solar and Stellar Astrophysics - Abstract
We report the confirmation of a sub-Saturn-size exoplanet, TOI-1194 b with a mass about $0.456_{-0.051}^{+0.055}$ $M_{J}$, and a very low mass companion star with a mass of about $96.5\pm1.5$ $M_J$, TOI-1251 B. Exoplanet candidates provided by the Transiting Exoplanet Survey Satellite (TESS) are suitable for further follow-up observations by ground-based telescopes with small and medium apertures. The analysis is performed based on data from several telescopes worldwide, including telescopes in the Sino-German multiband photometric campaign, which aimed at confirming TESS Objects of Interest (TOIs) using ground-based small-aperture and medium-aperture telescopes, especially for long-period targets. TOI-1194 b is confirmed based on the consistent periodic transits depths from the multiband photometric data. We measure an orbital period of $2.310644\pm0.000001$ d, and radius is $0.767_{-0.041}^{+0.045}$ $R_J$, and amplitude of RV curve is $69.4_{-7.3}^{+7.9}$ m/s. TOI-1251 B is confirmed based on the multiband photometric and high-resolution spectroscopic data, whose orbiting period is $5.963054_{-0.000001}^{+0.000002}$ d, the radius is $0.947_{-0.033}^{+0.035}$ $R_J$, and amplitude of RV curve is $9849_{-40}^{+42}$ m/s., Comment: 28 pages, 8 figures, Accepted by RAA on Oct. 18th, 2023
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- 2023
24. TOI-1801 b: A temperate mini-Neptune around a young M0.5 dwarf
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Mallorquín, M., Goffo, E., Pallé, E., Lodieu, N., Béjar, V. J. S., Isaacson, H., Osorio, M. R. Zapatero, Dreizler, S., Stock, S., Luque, R., Murgas, F., Peña, L., Sanz-Forcada, J., Morello, G., Ciardi, D. R., Furlan, E., Collins, K. A., Herrero, E., Vanaverbeke, S., Plavchan, P., Narita, N., Schweitzer, A., Pérez-Torres, M., Quirrenbach, A., Kemmer, J., Hatzes, A. P., Howard, A., Schlecker, M., Reffert, S., Nagel, E., Morales, J. C., Orell-Miquel, J., Duque-Arribas, C., Carleo, I., Cifuentes, C., Nowak, G., Ribas, I., Reiners, A., Amado, P. J., Caballero, J. A., Henning, Th., Pinter, V., Murphy, J. M. Akana, Beard, C., Blunt, S., Brinkman, C. L., Cale, B., Chontos, A., Collins, K. I., Crossfield, I. J. M., Dai, F., Dalba, P. A., Dufoer, S., Mufti, M. El, Espinoza, N., Fetherolf, T., Fukui, A., Giacalone, S., Gnilka, C., Gonzales, E., Grunblatt, S. K., Howell, S., Huber, D., Kane, S. R., de León, J. P., Lubin, J., MacDougall, M. G., Massey, B., Montes, D., Mori, M., Parviainen, H., Passegger, V. M., Polanski, A. S., Robertson, P., Schwarz, R. P., Srdoc, G., Tabernero, H. M., Tanner, A., Turtelboom, E., Van Zandt, J., Weiss, L., and Zechmeister, M.
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Astrophysics - Earth and Planetary Astrophysics - Abstract
We report the discovery, mass, and radius determination of TOI-1801 b, a temperate mini-Neptune around a young M dwarf. TOI-1801 b was observed in TESS sectors 22 and 49, and the alert that this was a TESS planet candidate with a period of 21.3 days went out in April 2020. However, ground-based follow-up observations, including seeing-limited photometry in and outside transit together with precise radial velocity (RV) measurements with CARMENES and HIRES revealed that the true period of the planet is 10.6 days. These observations also allowed us to retrieve a mass of 5.74 $\pm$ 1.46 $M_\oplus$, which together with a radius of 2.08 $\pm$ 0.12 $R_\oplus$, means that TOI-1801 b is most probably composed of water and rock, with an upper limit of 2\% by mass of H$_{2}$ in its atmosphere. The stellar rotation period of 16 days is readily detectable in our RV time series and in the ground-based photometry. We derived a likely age of 600--800 Myr for the parent star TOI-1801, which means that TOI-1801 b is the least massive young mini-Neptune with precise mass and radius determinations. Our results suggest that if TOI-1801 b had a larger atmosphere in the past, it must have been removed by some evolutionary mechanism on timescales shorter than 1 Gyr., Comment: Accepted in A&A. 29 pages, 21 figures
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- 2023
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25. Cheap Talking Algorithms
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Condorelli, Daniele and Furlan, Massimiliano
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Economics - Theoretical Economics ,Computer Science - Artificial Intelligence - Abstract
We simulate behaviour of two independent reinforcement learning algorithms playing the Crawford and Sobel (1982) game of strategic information transmission. We adopt memoryless algorithms to capture learning in a static game where a large population interacts anonymously. We show that sender and receiver converge to Nash equilibrium play. The level of informativeness of the sender's cheap talk decreases as the bias increases and, at intermediate level of the bias, it matches the level predicted by the Pareto optimal equilibrium or by the second best one. Conclusions are robust to alternative specifications of the learning hyperparameters and of the game.
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- 2023
26. Investigating Protostellar Accretion-Driven Outflows Across the Mass Spectrum: JWST NIRSpec IFU 3-5~$\mu$m Spectral Mapping of Five Young Protostars
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Federman, Samuel, Megeath, S. Thomas, Rubinstein, Adam E., Gutermuth, Robert, Narang, Mayank, Tyagi, Himanshu, Manoj, P., Anglada, Guillem, Atnagulov, Prabhani, Beuther, Henrik, Bourke, Tyler L., Brunken, Nashanty, Garatti, Alessio Caratti o, Evans II, Neal J., Fischer, William J., Furlan, Elise, Green, Joel, Habel, Nolan, Hartmann, Lee, Karnath, Nicole, Klaassen, Pamela, Linz, Hendrik, Looney, Leslie W., Osorio, Mayra, Page, James Muzerolle, Pokhrel, Riwaj, Rahatgaonkar, Rohan, Rocha, Will R. M., Sheehan, Patrick, Slavicinska, Katerina, Stanke, Thomas, Stutz, Amelia M., Tobin, John J., Tychoniec, Lukasz, Van Dishoeck, Ewine F., Watson, Dan M., Wolk, Scott, and Yang, Yao-Lun
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Astrophysics - Solar and Stellar Astrophysics ,Astrophysics - Astrophysics of Galaxies - Abstract
Investigating Protostellar Accretion is a Cycle 1 JWST program using the NIRSpec+MIRI integral field units to obtain 2.9--28 $\mu$m spectral cubes of five young protostars with luminosities of 0.2-10,000 L$_{\odot}$ in their primary accretion phase. This paper introduces the NIRSpec 2.9--5.3 $\mu$m data of the inner 840-9000 au with spatial resolutions from 28-300 au. The spectra show rising continuum emission; deep ice absorption; emission from H$_{2}$, H~I, and [Fe~II]; and the CO fundamental series in emission and absorption. Maps of the continuum emission show scattered light cavities for all five protostars. In the cavities, collimated jets are detected in [Fe~II] for the four $< 320$~L$_{\odot}$ protostars, two of which are additionally traced in Br-$\alpha$. Knots of [Fe~II] emission are detected toward the most luminous protostar, and knots of [FeII] emission with dynamical times of $< 30$~yrs are found in the jets of the others. While only one jet is traced in H$_2$, knots of H$_2$ and CO are detected in the jets of four protostars. H$_2$ is seen extending through the cavities, showing that they are filled by warm molecular gas. Bright H$_2$ emission is seen along the walls of a single cavity, while in three cavities narrow shells of H$_2$ emission are found, one of which has an [Fe~II] knot at its apex. These data show cavities containing collimated jets traced in atomic/ionic gas surrounded by warm molecular gas in a wide-angle wind and/or gas accelerated by bow shocks in the jets., Comment: 26 pages, 12 figures
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- 2023
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27. Uncommon Salmonella Infantis Variants with Incomplete Antigenic Formula in the Poultry Food Chain, Italy
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Petrin, Sara, Tiengo, Alessia, Longo, Alessandra, Furlan, Maddalena, Marafin, Elisa, Zavagnin, Paola, Orsini, Massimiliano, Losasso, Carmen, and Barco, Lisa
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Tetracycline -- Contamination ,Genomics ,Drug resistance in microorganisms ,Poultry industry ,Antigens ,Epidemiology ,Tetracyclines -- Contamination ,Salmonella ,Health ,European Union. European Food Safety Authority - Abstract
The emergence of variants posing threats to human health and animal production characterizes the epidemiology of Salmonella (1) and also S. enterica serovar Infantis (antigenic formula 6,7:r:1,5). Over the past [...]
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- 2024
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28. Towards a knowledge-hub destination: analysis and recommendation for implementing TOD for Qatar national library metro station
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Valdeolmillos, Nur Alah Abdelzayed, Furlan, Raffaello, Tadi, Massimo, Sinclair, Brian R., and Awwaad, Reem
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- 2024
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29. Visual Orbits & Alignments of Planet Hosting Binary Systems
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Lester, Kathryn, Howell, Steve, Matson, Rachel, Furlan, Elise, Gnilka, Crystal, Littlefield, Colin, Ciardi, David, Everett, Mark, Fajardo-Acosta, Sergio, and Clark, Catherine
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Astrophysics - Solar and Stellar Astrophysics ,Astrophysics - Earth and Planetary Astrophysics - Abstract
Roughly half of Solar-type planet hosts have stellar companions, so understanding how these binary companions affect the formation and evolution of planets is an important component to understanding planetary systems overall. Measuring the dynamical properties of planet host binaries enables a valuable test of planet formation in multi-star systems and requires knowledge of the binary orbital parameters. Using high resolution imaging, we have measured the relative astrometry and visual orbits of 13 binary systems where one of the stars is known to host a transiting exoplanet. Our results indicate that the mutual inclination between the orbits of the binary hosts and the transiting planets are well aligned. Our results for close binary systems (a<100 AU) complement past work for wide planet host binaries from Gaia., Comment: Accepted for publication in AJ
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- 2023
30. Fast near-infrared photodetectors based on nontoxic and solution-processable AgBiS2
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Huang, Yi-Teng, Nodari, Davide, Furlan, Francesco, Zhang, Youcheng, Rusu, Marin, Dai, Linjie, Andaji-Garmaroudi, Zahra, Stranks, Samuel D., Sirringhaus, Henning, Rao, Akshay, Gasparini, Nicola, and Hoye, Robert L. Z.
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Condensed Matter - Materials Science - Abstract
Solution-processable near-infrared (NIR) photodetectors are urgently needed for a wide range of next-generation electronics, including sensors, optical communications and bioimaging. However, there is currently a compromise between low toxicity and slow (<300 kHz cut-off frequency) organic materials versus faster detectors (>300 kHz cut-off frequency) based on compounds containing toxic lead or cadmium. Herein, we circumvent this trade-off by developing solution-processed AgBiS2 photodetectors with high cut-off frequencies under both white light (>1 MHz) and NIR (approaching 500 kHz) illumination. These high cut-off frequencies are due to the short transit distances of charge-carriers in the AgBiS2 photodetectors, which arise from the strong light absorption of these materials, such that film thicknesses well below 120 nm are adequate to absorb >65% of near-infrared to visible light. By finely controlling the thickness of the photoactive layer, we can modulate the charge-collection efficiency, achieve low dark current densities, and minimize the effects of ion migration to realize fast photodetectors that are stable in air. These outstanding characteristics enable real-time heartbeat sensors based on NIR AgBiS2 photodetectors. # equal contribution, * corresponding authors, Comment: 29 pages, 4 figures, 1 table
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- 2023
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31. Identification of the Top TESS Objects of Interest for Atmospheric Characterization of Transiting Exoplanets with JWST
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Hord, Benjamin J., Kempton, Eliza M. -R., Mikal-Evans, Thomas, Latham, David W., Ciardi, David R., Dragomir, Diana, Colón, Knicole D., Ross, Gabrielle, Vanderburg, Andrew, de Beurs, Zoe L., Collins, Karen A., Watkins, Cristilyn N., Bean, Jacob, Cowan, Nicolas B., Daylan, Tansu, Morley, Caroline V., Ih, Jegug, Baker, David, Barkaoui, Khalid, Batalha, Natalie M., Behmard, Aida, Belinski, Alexander, Benkhaldoun, Zouhair, Benni, Paul, Bernacki, Krzysztof, Bieryla, Allyson, Binnenfeld, Avraham, Bosch-Cabot, Pau, Bouchy, François, Bozza, Valerio, Brahm, Rafael, Buchhave, Lars A., Calkins, Michael, Chontos, Ashley, Clark, Catherine A., Cloutier, Ryan, Cointepas, Marion, Collins, Kevin I., Conti, Dennis M., Crossfield, Ian J. M., Dai, Fei, de Leon, Jerome P., Dransfield, Georgina, Dressing, Courtney, Dustor, Adam, Esquerdo, Gilbert, Evans, Phil, Fajardo-Acosta, Sergio B., Fiołka, Jerzy, Forés-Toribio, Raquel, Frasca, Antonio, Fukui, Akihiko, Fulton, Benjamin, Furlan, Elise, Gan, Tianjun, Gandolfi, Davide, Ghachoui, Mourad, Giacalone, Steven, Gilbert, Emily A., Gillon, Michaël, Girardin, Eric, Gonzales, Erica, Horta, Ferran Grau, Gregorio, Joao, Greklek-McKeon, Michael, Guerra, Pere, Hartman, J. D., Hellier, Coel, Hełminiak, Krzysztof G., Henning, Thomas, Hill, Michelle L., Horne, Keith, Howard, Andrew W., Howell, Steve B., Huber, Daniel, Isaacson, Howard, Isopi, Giovanni, Jehin, Emmanuel, Jenkins, Jon M., Jensen, Eric L. N., Johnson, Marshall C., Jordán, Andrés, Kane, Stephen R., Kielkopf, John F., Krushinsky, Vadim, Lasota, Sławomir, Lee, Elena, Lewin, Pablo, Livingston, John H., Lubin, Jack, Lund, Michael B., Mallia, Franco, Mann, Christopher R., Marino, Giuseppe, Maslennikova, Nataliia, Massey, Bob, Matson, Rachel, Matthews, Elisabeth, Mayo, Andrew W., Mazeh, Tsevi, McLeod, Kim K., Michaels, Edward J., Močnik, Teo, Mori, Mayuko, Mraz, Georgia, Muñoz, Jose A., Narita, Norio, Nielsen, Louise Dyregaard, Osborn, Hugh, Palle, Enric, Panahi, Aviad, Papini, Riccardo, Polanski, Alex S., Popowicz, Adam, Pozuelos, Francisco J., Quinn, Samuel N., Radford, Don J., Reed, Phillip A., Relles, Howard M., Rice, Malena, Robertson, Paul, Rodriguez, Joseph E., Rosenthal, Lee J., Rubenzahl, Ryan A., Schanche, Nicole, Schlieder, Joshua, Schwarz, Richard P., Sefako, Ramotholo, Shporer, Avi, Sozzetti, Alessandro, Srdoc, Gregor, Stockdale, Chris, Tarasenkov, Alexander, Tan, Thiam-Guan, Timmermans, Mathilde, Ting, Eric B., Van Zandt, Judah, Vignes, JP, Waite, Ian, Watanabe, Noriharu, Weiss, Lauren M., Wittrock, Justin, Zhou, George, Ziegler, Carl, and Zucker, Shay
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Astrophysics - Earth and Planetary Astrophysics - Abstract
JWST has ushered in an era of unprecedented ability to characterize exoplanetary atmospheres. While there are over 5,000 confirmed planets, more than 4,000 TESS planet candidates are still unconfirmed and many of the best planets for atmospheric characterization may remain to be identified. We present a sample of TESS planets and planet candidates that we identify as "best-in-class" for transmission and emission spectroscopy with JWST. These targets are sorted into bins across equilibrium temperature $T_{\mathrm{eq}}$ and planetary radius $R{_\mathrm{p}}$ and are ranked by transmission and emission spectroscopy metric (TSM and ESM, respectively) within each bin. In forming our target sample, we perform cuts for expected signal size and stellar brightness, to remove sub-optimal targets for JWST. Of the 194 targets in the resulting sample, 103 are unconfirmed TESS planet candidates, also known as TESS Objects of Interest (TOIs). We perform vetting and statistical validation analyses on these 103 targets to determine which are likely planets and which are likely false positives, incorporating ground-based follow-up from the TESS Follow-up Observation Program (TFOP) to aid the vetting and validation process. We statistically validate 23 TOIs, marginally validate 33 TOIs to varying levels of confidence, deem 29 TOIs likely false positives, and leave the dispositions for 4 TOIs as inconclusive. 14 of the 103 TOIs were confirmed independently over the course of our analysis. We provide our final best-in-class sample as a community resource for future JWST proposals and observations. We intend for this work to motivate formal confirmation and mass measurements of each validated planet and encourage more detailed analysis of individual targets by the community., Comment: Submitted to AJ. Machine-readable versions of Tables 2 and 3 are included. 40 pages, 7 figures, 3 tables
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- 2023
32. Speckle Imaging of Gamma2 Velorum: The Inner Wind Possibly Resolved
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Shara, Michael M., Howell, Steve B., Furlan, Elise, Garland, James T., Moffat, Anthony F. J., and Zurek, David
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Astrophysics - Solar and Stellar Astrophysics - Abstract
Accurately quantifying the rates dM/dt at which massive stars lose mass is essential to any understanding of their evolution. All dM/dt estimates to date assume wind clumping factors; not allowing for clumping leads to overestimates of dM/dt and underestimates of lifetimes and masses when these stars explode as supernovae. Mid-IR spectroscopy suggested that the wind of the nearest Wolf-Rayet star, Gamma2 Vel, is resolved with a Full Width at 10 per cent intensity of 0.5 arcsec, or 171 AU at the 342 pc distance of the star. As the Zorro speckle imager on Gemini-South is capable of 0.02 arcsec resolution, we have used it to image Gamma2 Vel at two orbital phases (0.30 and 0.44) with two narrowband and two intermediate-band filters in an attempt to resolve its wind. Our observations demonstrate that the wind of Gamma2 Vel may be resolved as a 0.07 arcsec westward elongation through an 832 nm filter at orbital phase 0.3 . If confirmed, this is the smallest scale (24 AU) at which a WR star wind asymmetry has been directly imaged. Similar imaging at multiple phases is needed to determine if the asymmetry is due to stochastic wind clumping, co-rotating interaction regions or colliding-wind, cone-shaped shocks., Comment: 7 pages, 4 Figures, in press in MNRAS
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- 2023
33. A massive hot Jupiter orbiting a metal-rich early-M star discovered in the TESS full frame images
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Gan, Tianjun, Cadieux, Charles, Jahandar, Farbod, Vazan, Allona, Wang, Sharon X., Mao, Shude, Alvarado-Montes, Jaime A., Lin, D. N. C., Artigau, Étienne, Cook, Neil J., Doyon, René, Mann, Andrew W., Stassun, Keivan G., Burgasser, Adam J., Rackham, Benjamin V., Howell, Steve B., Collins, Karen A., Barkaoui, Khalid, Shporer, Avi, de Leon, Jerome, Arnold, Luc, Ricker, George R., Vanderspek, Roland, Latham, David W., Seager, Sara, Winn, Joshua N., Jenkins, Jon M., Burdanov, Artem, Charbonneau, David, Dransfield, Georgina, Fukui, Akihiko, Furlan, Elise, Gillon, Michaël, Hooton, Matthew J., Lewis, Hannah M., Littlefield, Colin, Mireles, Ismael, Narita, Norio, Ormel, Chris W., Quinn, Samuel N., Sefako, Ramotholo, Timmermans, Mathilde, Vezie, Michael, and de Wit, Julien
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Astrophysics - Earth and Planetary Astrophysics ,Astrophysics - Solar and Stellar Astrophysics - Abstract
Observations and statistical studies have shown that giant planets are rare around M dwarfs compared with Sun-like stars. The formation mechanism of these extreme systems remains under debate for decades. With the help of the TESS mission and ground based follow-up observations, we report the discovery of TOI-4201b, the most massive and densest hot Jupiter around an M dwarf known so far with a radius of $1.22\pm 0.04\ R_J$ and a mass of $2.48\pm0.09\ M_J$, about 5 times heavier than most other giant planets around M dwarfs. It also has the highest planet-to-star mass ratio ($q\sim 4\times 10^{-3}$) among such systems. The host star is an early-M dwarf with a mass of $0.61\pm0.02\ M_{\odot}$ and a radius of $0.63\pm0.02\ R_{\odot}$. It has significant super-solar iron abundance ([Fe/H]=$0.52\pm 0.08$ dex). However, interior structure modeling suggests that its planet TOI-4201b is metal-poor, which challenges the classical core-accretion correlation of stellar-planet metallicity, unless the planet is inflated by additional energy sources. Building on the detection of this planet, we compare the stellar metallicity distribution of four planetary groups: hot/warm Jupiters around G/M dwarfs. We find that hot/warm Jupiters show a similar metallicity dependence around G-type stars. For M dwarf host stars, the occurrence of hot Jupiters shows a much stronger correlation with iron abundance, while warm Jupiters display a weaker preference, indicating possible different formation histories., Comment: 24 pages, 14 figures, 4 tables, accepted to AJ
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- 2023
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34. TOI 4201 b and TOI 5344 b: Discovery of Two Transiting Giant Planets Around M Dwarf Stars and Revised Parameters for Three Others
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Hartman, J. D., Bakos, G. Á., Csubry, Z., Howard, A. W., Isaacson, H., Giacalone, S., Chontos, A., Narita, N., Fukui, A., de Leon, J. P., Watanabe, N., Mori, M., Kagetani, T., Fukuda, I., Kawai, Y., Ikoma, M., Palle, E., Murgas, F., Esparza-Borges, E., Parviainen, H., Bouma, L. G., Cointepas, M., Bonfils, X., Almenara, J. M., Collins, Karen A., Collins, Kevin I., Relles, Howard M., Barkaoui, Khalid, Schwarz, Richard P., Mourad, Ghachoui, Timmermans, Mathilde, Dransfield, Georgina, Burdanov, Artem, de Wit, Julien, Jehin, Emmanuël, Triaud, Amaury H. M. J., Gillon, Michaël, Benkhaldoun, Zouhair, Horne, Keith, Sefako, Ramotholo, Jordán, A., Brahm, R., Suc, V., Howell, Steve B., Furlan, E., Schlieder, J. E., Ciardi, D., Barclay, T., Gonzales, E. J., Crossfield, I., Dressing, C. D., Goliguzova, M., Tatarnikov, A., Ricker, George R., Vanderspek, Roland, Latham, David W., Seager, S., Winn, Joshua N., Jenkins, Jon M., Striegel, Stephanie, Shporer, Avi, Vanderburg, Andrew, Levine, Alan M., Kostov, Veselin B., and Watanabe, David
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Astrophysics - Earth and Planetary Astrophysics - Abstract
We present the discovery from the TESS mission of two giant planets transiting M dwarf stars: TOI 4201 b and TOI 5344 b. We also provide precise radial velocity measurements and updated system parameters for three other M dwarfs with transiting giant planets: TOI 519, TOI 3629 and TOI 3714. We measure planetary masses of 0.525 +- 0.064 M_J, 0.243 +- 0.020 M_J, 0.689 +- 0.030 M_J, 2.57 +- 0.15 M_J, and 0.412 +- 0.040 M_J for TOI 519 b, TOI 3629 b, TOI 3714 b, TOI 4201 b, and TOI 5344 b, respectively. The corresponding stellar masses are 0.372 +- 0.018 M_s, 0.635 +- 0.032 M_s, 0.522 +- 0.028 M_s, 0.625 +- 0.033 M_s and 0.612 +- 0.034 M_s. All five hosts have super-solar metallicities, providing further support for recent findings that, like for solar-type stars, close-in giant planets are preferentially found around metal-rich M dwarf host stars. Finally, we describe a procedure for accounting for systematic errors in stellar evolution models when those models are included directly in fitting a transiting planet system., Comment: 32 pages, 9 figures, 10 tables, submitted to AAS Journals; revised to add co-author
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- 2023
35. Evidence library of meta-analytical literature assessing the sustainability of agriculture – a dataset
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Andrea Schievano, Marta Pérez-Soba, Simona Bosco, Ana Montero-Castaño, Rui Catarino, Mathilde Chen, Giovanni Tamburini, Beatrice Landoni, Otho Mantegazza, Irene Guerrero, Maria Bielza, Michael Assouline, Renate Koeble, Frank Dentener, Marijn Van der Velde, Carlo Rega, Andrea Furlan, Maria Luisa Paracchini, Franz Weiss, Vincenzo Angileri, Jean-Michel Terres, and David Makowski
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Science - Abstract
Abstract In the last two decades, an exponentially growing number of meta-analyses (MAs) synthesize thousands of peer-reviewed studies on the environmental impacts of farming practices (FPs). This paper describes the iMAP-FP evidence library, a comprehensive dataset on the effects of 34 categories of FPs (such as agronomic practices, cropping and livestock systems, land management options and mitigation techniques) on 34 impacts including climate mitigation, soil health, environmental pollution, water use, nutrients cycling, biodiversity, and agricultural productivity. Through systematic screening, 570 MAs published since 2000 were selected and categorized according to the type of FP. We assessed their impacts, the geographic regions covered, and their quality. We extracted 3,811 effects and their statistical significance associated with sustainable FPs (intervention) compared to a control (typically conventional agriculture) across 223 different intervention-control pairs. Our dataset is accompanied with an online free-access library, which includes a catalogue of synthetic reports summarizing the available evidence on each evaluated FP.
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- 2024
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36. Nanodynamo quantifies subcellular RNA dynamics revealing extensive coupling between steps of the RNA life cycle
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Lucia Coscujuela Tarrero, Valeria Famà, Giacomo D’Andrea, Simone Maestri, Anna de Polo, Stefano Biffo, Mattia Furlan, and Mattia Pelizzola
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Science - Abstract
Abstract The coordinated action of transcriptional and post-transcriptional machineries shapes gene expression programs at steady state and determines their concerted response to perturbations. We have developed Nanodynamo, an experimental and computational workflow for quantifying the kinetic rates of nuclear and cytoplasmic steps of the RNA life cycle. Nanodynamo is based on mathematical modelling following sequencing of native RNA from cellular fractions and polysomes. We have applied this workflow to triple-negative breast cancer cells, revealing widespread post-transcriptional RNA processing that is mutually exclusive with its co-transcriptional counterpart. We used Nanodynamo to unravel the coupling between transcription, processing, export, decay and translation machineries. We have identified a number of coupling interactions within and between the nucleus and cytoplasm that largely contribute to coordinating how cells respond to perturbations that affect gene expression programs. Nanodynamo will be instrumental in unravelling the determinants and regulatory processes involved in the coordination of gene expression responses.
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- 2024
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37. Inflammatory signature in amyotrophic lateral sclerosis predicting disease progression
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Cinzia Femiano, Antonio Bruno, Luana Gilio, Fabio Buttari, Ettore Dolcetti, Giovanni Galifi, Federica Azzolini, Angela Borrelli, Roberto Furlan, Annamaria Finardi, Alessandra Musella, Georgia Mandolesi, Marianna Storto, Diego Centonze, and Mario Stampanoni Bassi
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Amyotrophic lateral sclerosis (ALS) ,Neuroinflammation ,Disease progression ,Cerebrospinal fluid (CSF) ,Cytokines ,Neutrophil-to-lymphocytes ratio (NLR) ,Medicine ,Science - Abstract
Abstract Experimental studies identified a role of neuroinflammation in the pathogenesis of neurodegenerative diseases, including amyotrophic lateral sclerosis (ALS). However, the role of inflammatory molecules as diagnostic and prognostic biomarkers in patients with ALS is unclear. In this cross-sectional study, the cerebrospinal fluid (CSF) levels of a set of inflammatory cytokines and chemokines were analyzed in 56 newly diagnosed ALS patients and in 47 age- and sex-matched control patients without inflammatory or degenerative neurological disorders. The molecules analyzed included: interleukin (IL)-1β, IL-2, IL-4, IL-5, IL-6, IL-7, IL-8, IL-9, IL-10, IL-12, IL-13, IL-17, granulocyte colony stimulating factor (GCSF), macrophage inflammatory protein (MIP)-1a, MIP-1b, tumor necrosis factors (TNF), eotaxin. Principal component analysis (PCA) was used to explore possible associations between CSF molecules and ALS diagnosis. In addition, we analyzed the association between CSF cytokine profiles and clinical characteristics, including the disease progression rate score, and peripheral inflammation assessed using the Neutrophil-to-lymphocyte ratio (NLR). PCA identified six principal components (PCs) explaining 70.67% of the total variance in the CSF cytokine set. The principal component (PC1) explained 26.8% of variance and showed a positive load with CSF levels of IL-9, IL-4, GCSF, IL-7, IL-17, IL-13, IL-6, IL-1β, TNF, and IL-2. Logistic regression showed a significant association between PC1 and ALS diagnosis. In addition, in ALS patients, the same component was significantly associated with higher disease progression rate score and positively correlated with NLR. CSF inflammatory activation in present in ALS at the time of diagnosis and may characterize patients at higher risk for disease progression.
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- 2024
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38. Notes on the relationship between Agroecology and rural schools in the during the COVID-19 pandemic
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Gabriela Furlan Carcaioli, Marilia Carla de Mello Gaia, and Roberto Antônio Finatto
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agroecology ,rural school ,rural education ,covid-19 pandemic. ,Education - Abstract
This article aims to organize some thoughts on the materiality of water courses and forests for rural individuals in different Brazilian territories and the relationship between rural schools and Agroecology during the COVID-19 pandemic. The analysis, based on data from 2020 and 2021, investigates how schools and their embeddedness contributed or could contribute to the construction of another agri-food system based on the principles of Agroecology. The methodological framework centered on surveying methods, literature review, and interviews with teachers from rural schools. The data point to the importance of schools in guaranteeing the food security of many families, in collective solidarity actions development, and in the production of pedagogical alternatives based on the critical understanding of the students' reality, which also are central elements for Agroecology practices.
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- 2024
39. Approach to the pharmacological management of chronic pain in patients with an alcohol use disorder
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Murphy L, Ng KWK, Su VCH, Woodworth-Giroux S, Levy TS, Sproule BA, and Furlan AD
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Medicine (General) ,R5-920 - Abstract
Laura Murphy,1,2 Karen WK Ng,1 Victoria CH Su,3 Sarah Woodworth-Giroux,4 Todd S Levy,1 Beth A Sproule,2,5 Andrea D Furlan1,6 1University Health Network, Toronto, ON, Canada; 2Leslie Dan Faculty of Pharmacy, University of Toronto, Toronto, ON, Canada; 3St Paul's Hospital, Lower Mainland Pharmacy Services, Vancouver, BC, Canada; 4Windsor Regional Hospital, Windsor, ON, Canada; 5Centre for Addiction and Mental Health (CAMH), Toronto, ON, Canada; 6Institute for Work and Health, Toronto, ON, Canada Abstract: This paper provides an overview of research, guidelines, and clinical considerations for the use of medications for chronic pain in the management of patients with an alcohol use disorder. A review of the literature identified randomized controlled trials, epidemiological cohort studies, consensus guidelines, and one systematic review and meta-analysis. Where gaps in the literature existed, clinical experience of the authors is included. Use of nonopioid medications should be given priority and may offer a more favorable risk profile as well as benefits beyond pain management, such as improvement in anxiety, depression, or insomnia. Pregabalin and gabapentin have additional benefits to decrease alcohol cravings or time to relapse after a period of abstinence from alcohol. Drug interactions between selected analgesics and alcohol, disulfiram, or naltrexone require careful consideration. Keywords: chronic pain, alcohol use disorder, opioids
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- 2015
40. TOI-2084 b and TOI-4184 b: two new sub-Neptunes around M dwarf stars
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Barkaoui, K., Timmermans, M., Soubkiou, A., Rackham, B. V., Burgasser, A. J., Chouqar, J., Pozuelos, F. J., Collins, K. A., Howell, S. B., Simcoe, R., Melis, C., Stassun, K. G., Tregloan-Reed, J., Cointepas, M., Gillon, M., Bonfils, X., Furlan, E., Gnilka, C. L., Almenara, J. M., Alonso, R., Benkhaldoun, Z., Bonavita, M., Bouchy, F., Burdanov, A., Chinchilla, P., Davoudi, F., Delrez, L., Demangeon, O., Dominik, M., Demory, B. -O., de Wit, J., Dransfield, G., Ducrot, E., Fukui, A., Hinse, T. C., Hooton, M. J., Jehin, E., Jenkins, J. M., Jørgensen, U. G., Latham, D. W., Garcia, L., Carrazco-Gaxiola, S., Ghachoui, M., Chew, Y. Gómez Maqueo, Günther, M. N., McCormac, J., Murgas, F., Murray, C. A., Narita, N., Niraula, P., Pedersen, P. P., Queloz, D., Rebolo-López, R., Ricker, G., Sabin, L., Sajadian, S., Schanche, N., Schwarz, R. P., Seager, S., Sebastian, D., Sefako, R., Sohy, S., Southworth, J., Srdoc, G., Thompson, S. J., Triaud, A. H. M. J., Vanderspek, R., Wells, R. D., Winn, J. N., and Zúñiga-Fernández, S.
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Astrophysics - Earth and Planetary Astrophysics - Abstract
We present the discovery and validation of two TESS exoplanets orbiting nearby M dwarfs: TOI-2084b, and TOI-4184b. We characterized the host stars by combining spectra from Shane/Kast and Magellan/FIRE, SED (Spectral Energy Distribution) analysis, and stellar evolutionary models. In addition, we used Gemini-South/Zorro & -North/Alopeke high-resolution imaging, archival science images, and statistical validation packages to support the planetary interpretation. We performed a global analysis of multi-colour photometric data from TESS and ground-based facilities in order to derive the stellar and planetary physical parameters for each system. We find that TOI-2084b and TOI-4184b are sub-Neptune-sized planets with radii of Rp = 2.47 +/- 0.13R_Earth and Rp = 2.43 +/- 0.21R_Earth, respectively. TOI-2084b completes an orbit around its host star every 6.08 days, has an equilibrium temperature of T_eq = 527 +/- 8K and an irradiation of S_p = 12.8 +/- 0.8 S_Earth. Its host star is a dwarf of spectral M2.0 +/- 0.5 at a distance of 114pc with an effective temperature of T_eff = 3550 +/- 50 K, and has a wide, co-moving M8 companion at a projected separation of 1400 au. TOI-4184b orbits around an M5.0 +/- 0.5 type dwarf star (Kmag = 11.87) each 4.9 days, and has an equilibrium temperature of T_eq = 412 +/- 8 K and an irradiation of S_p = 4.8 +/- 0.4 S_Earth. TOI-4184 is a metal poor star ([Fe/H] = -0.27 +/- 0.09 dex) at a distance of 69 pc with an effective temperature of T_eff = 3225 +/- 75 K. Both planets are located at the edge of the sub-Jovian desert in the radius-period plane. The combination of the small size and the large infrared brightness of their host stars make these new planets promising targets for future atmospheric exploration with JWST., Comment: Accepted for publication in A&A
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- 2023
41. TESS and CHEOPS Discover Two Warm Sub-Neptunes Transiting the Bright K-dwarf HD 15906
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Tuson, Amy, Queloz, Didier, Osborn, Hugh P., Wilson, Thomas G., Hooton, Matthew J., Beck, Mathias, Lendl, Monika, Olofsson, Göran, Fortier, Andrea, Bonfanti, Andrea, Brandeker, Alexis, Buchhave, Lars A., Cameron, Andrew Collier, Ciardi, David R., Collins, Karen A., Gandolfi, Davide, Garai, Zoltan, Giacalone, Steven, da Silva, João Gomes, Howell, Steve B., Patel, Jayshil A., Persson, Carina M., Serrano, Luisa M., Sousa, Sérgio G., Ulmer-Moll, Solène, Vanderburg, Andrew, Ziegler, Carl, Alibert, Yann, Alonso, Roi, Anglada, Guillem, Bárczy, Tamas, Navascues, David Barrado, Barros, Susana C. C., Baumjohann, Wolfgang, Beck, Thomas, Benz, Willy, Billot, Nicolas, Bonfils, Xavier, Borsato, Luca, Broeg, Christopher, Cabrera, Juan, Charnoz, Sébastien, Conti, Dennis M., Csizmadia, Szilard, Cubillos, Patricio E., Davies, Melvyn B., Deleuil, Magali, Delrez, Laetitia, Demangeon, Olivier D. S., Demory, Brice-Olivier, Dragomir, Diana, Dressing, Courtney D., Ehrenreich, David, Erikson, Anders, Essack, Zahra, Farinato, Jacopo, Fossati, Luca, Fridlund, Malcolm, Furlan, Elise, Gill, Holden, Gillon, Michaël, Gnilka, Crystal L., Gonzales, Erica, Güdel, Manuel, Günther, Maximilian N., Hoyer, Sergio, Isaak, Kate G., Jenkins, Jon M., Kiss, Laszlo L., Laskar, Jacques, Latham, David W., Law, Nicholas, Etangs, Alain Lecavelier des, Curto, Gaspare Lo, Lovis, Christophe, Luque, Rafael, Magrin, Demetrio, Mann, Andrew W., Maxted, Pierre F. L., Mayor, Michel, McDermott, Scott, Mecina, Marko, Mordasini, Christoph, Mortier, Annelies, Nascimbeni, Valerio, Ottensamer, Roland, Pagano, Isabella, Pallé, Enric, Peter, Gisbert, Piotto, Giampaolo, Pollacco, Don, Pritchard, Tyler, Ragazzoni, Roberto, Rando, Nicola, Ratti, Francesco, Rauer, Heike, Ribas, Ignasi, Ricker, George R., Rieder, Martin, Santos, Nuno C., Savel, Arjun B., Scandariato, Gaetano, Schwarz, Richard P., Seager, Sara, Ségransan, Damien, Shporer, Avi, Simon, Attila E., Smith, Alexis M. S., Steller, Manfred, Stockdale, Chris, Szabó, Gyula M., Thomas, Nicolas, Torres, Guillermo, Tronsgaard, René, Udry, Stéphane, Ulmer, Bernd, Van Grootel, Valérie, Vanderspek, Roland, Venturini, Julia, Walton, Nicholas A., Winn, Joshua N., and Wohler, Bill
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Astrophysics - Earth and Planetary Astrophysics - Abstract
We report the discovery of two warm sub-Neptunes transiting the bright (G = 9.5 mag) K-dwarf HD 15906 (TOI 461, TIC 4646810). This star was observed by the Transiting Exoplanet Survey Satellite (TESS) in sectors 4 and 31, revealing two small transiting planets. The inner planet, HD 15906 b, was detected with an unambiguous period but the outer planet, HD 15906 c, showed only two transits separated by $\sim$ 734 days, leading to 36 possible values of its period. We performed follow-up observations with the CHaracterising ExOPlanet Satellite (CHEOPS) to confirm the true period of HD 15906 c and improve the radius precision of the two planets. From TESS, CHEOPS and additional ground-based photometry, we find that HD 15906 b has a radius of 2.24 $\pm$ 0.08 R$_\oplus$ and a period of 10.924709 $\pm$ 0.000032 days, whilst HD 15906 c has a radius of 2.93$^{+0.07}_{-0.06}$ R$_\oplus$ and a period of 21.583298$^{+0.000052}_{-0.000055}$ days. Assuming zero bond albedo and full day-night heat redistribution, the inner and outer planet have equilibrium temperatures of 668 $\pm$ 13 K and 532 $\pm$ 10 K, respectively. The HD 15906 system has become one of only six multiplanet systems with two warm ($\lesssim$ 700 K) sub-Neptune sized planets transiting a bright star (G $\leq$ 10 mag). It is an excellent target for detailed characterisation studies to constrain the composition of sub-Neptune planets and test theories of planet formation and evolution., Comment: 30 pages, 20 figures, 11 tables (including appendix). Published in MNRAS
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- 2023
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42. Pulsar Observations at low latitudes and low frequencies
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Lousto, Carlos O., Missel, R., Zubieta, E., del Palacio, S., Garcia, F., Gancio, G., Wang, L., Furlan, S. B. Araujo, and Combi, J. A.
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Astrophysics - Instrumentation and Methods for Astrophysics ,Astrophysics - High Energy Astrophysical Phenomena - Abstract
The Pulsar Monitoring in Argentina (PuMA) is a collaboration between the Argentine Institute for Radioastronomy (IAR) and the Rochester Institute of Technology (RIT) that since 2017 has been observing southern sky pulsars with high cadence using the two restored IAR antennas in the L-Band (1400MHz). We briefly review the first set of results of this program to study transient phenomena, such as magnetars and glitching pulsars, as well as to perform precise timing of millisecond pulsars. Access to lower frequency bands, where most of the pulsars are brighter, would allow us to reach additional pulsars, currently buried into the background noise. We identify two dozen additional glitching pulsars that could be observable in the 400MHz band by the IAR's projected Multipurpose Interferometer Array (MIA). We also discuss the relevance and challenges of single-pulse pulsar timing at low frequencies and the search for Fast Radio Burst (FRB) in the collected data since 2017 using machine learning techniques., Comment: 11 pages, 10 figures, 5 tables. arXiv admin note: text overlap with arXiv:2108.13462
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- 2023
43. Time to treatment with bridging intravenous alteplase before endovascular treatment:subanalysis of the randomized controlled SWIFT-DIRECT trial.
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Meinel, Thomas, Kaesmacher, Johannes, Buetikofer, Lukas, Strbian, Daniel, Eker, Omer, Cognard, Christophe, Mordasini, Pasquale, Deppeler, Sandro, Mendes Pereira, Vitor, Albucher, Jean, Darcourt, Jean, Bourcier, Romain, Guillon, Benoit, Papagiannaki, Chrysanthi, Costentin, Guillaume, Sibolt, Gerli, Räty, Silja, Gory, Benjamin, Richard, Sébastien, Liman, Jan, Ernst, Marielle, Boulanger, Marion, Barbier, Charlotte, Mechtouff, Laura, Zhang, Liqun, Marnat, Gaultier, Sibon, Igor, Nikoubashman, Omid, Reich, Arno, Consoli, Arturo, Weisenburger, David, Requena, Manuel, Garcia-Tornel, Alvaro, Saleme, Suzana, Moulin, Solène, Pagano, Paolo, Saliou, Guillaume, Carrera, Emmanuel, Janot, Kevin, Boix, Marti, Pop, Raoul, Della Schiava, Lucie, Luft, Andreas, Piotin, Michel, Gentric, Jean, Pikula, Aleksandra, Pfeilschifter, Waltraud, Arnold, Marcel, Siddiqui, Adnan, Froehler, Michael, Furlan, Anthony, Chapot, René, Wiesmann, Martin, Machi, Paolo, Diener, Hans-Christoph, Kulcsar, Zsolt, Bonati, Leo, Bassetti, Claudio, Escalard, Simon, Liebeskind, David, Saver, Jeffrey, Fischer, Urs, and Gralla, Jan
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Thrombectomy ,Thrombolysis ,Humans ,Female ,Aged ,Male ,Tissue Plasminogen Activator ,Stroke ,Time-to-Treatment ,Thrombolytic Therapy ,Thrombectomy ,Brain Ischemia ,Treatment Outcome ,Fibrinolytic Agents - Abstract
BACKGROUND: We hypothesized that treatment delays might be an effect modifier regarding risks and benefits of intravenous thrombolysis (IVT) before mechanical thrombectomy (MT). METHODS: We used the dataset of the SWIFT-DIRECT trial, which randomized 408 patients to IVT+MT or MT alone. Potential interactions between assignment to IVT+MT and expected time from onset-to-needle (OTN) as well as expected time from door-to-needle (DTN) were included in regression models. The primary outcome was functional independence (modified Rankin Scale (mRS) 0-2) at 3 months. Secondary outcomes included mRS shift, mortality, recanalization rates, and (symptomatic) intracranial hemorrhage at 24 hours. RESULTS: We included 408 patients (IVT+MT 207, MT 201, median age 72 years (IQR 64-81), 209 (51.2%) female). The expected median OTN and DTN were 142 min and 54 min in the IVT+MT group and 129 min and 51 min in the MT alone group. Overall, there was no significant interaction between OTN and bridging IVT assignment regarding either the functional (adjusted OR (aOR) 0.76, 95% CI 0.45 to 1.30) and safety outcomes or the recanalization rates. Analysis of in-hospital delays showed no significant interaction between DTN and bridging IVT assignment regarding the dichotomized functional outcome (aOR 0.48, 95% CI 0.14 to 1.62), but the shift and mortality analyses suggested a greater benefit of IVT when in-hospital delays were short. CONCLUSIONS: We found no evidence that the effect of bridging IVT on functional independence is modified by overall or in-hospital treatment delays. Considering its low power, this subgroup analysis could have missed a clinically important effect, and exploratory analysis of secondary clinical outcomes indicated a potentially favorable effect of IVT with shorter in-hospital delays. Heterogeneity of the IVT effect size before MT should be further analyzed in individual patient meta-analysis of comparable trials. TRIAL REGISTRATION NUMBER: URL: https://www. CLINICALTRIALS: gov ; Unique identifier: NCT03192332.
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- 2023
44. Prognostic performance of blood neurofilament light chain protein in hospitalized COVID-19 patients without major central nervous system manifestations: an individual participant data meta-analysis
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Abdelhak, Ahmed, Barba, Lorenzo, Romoli, Michele, Benkert, Pascal, Conversi, Francesco, D’Anna, Lucio, Masvekar, Ruturaj R, Bielekova, Bibiana, Prudencio, Mercedes, Petrucelli, Leonard, Meschia, James F, Erben, Young, Furlan, Roberto, De Lorenzo, Rebecca, Mandelli, Alessandra, Sutter, Raoul, Hert, Lisa, Epple, Varenka, Marastoni, Damiano, Sellner, Johann, Steinacker, Petra, Aamodt, Anne Hege, Heggelund, Lars, Dyrhol-Riise, Anne Margarita, Virhammar, Johan, Fällmar, David, Rostami, Elham, Kumlien, Eva, Blennow, Kaj, Zetterberg, Henrik, Tumani, Hayrettin, Sacco, Simona, Green, Ari J, Otto, Markus, Kuhle, Jens, Ornello, Raffaele, Foschi, Matteo, and Abu-Rumeileh, Samir
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Biomedical and Clinical Sciences ,Clinical Sciences ,Clinical Research ,Good Health and Well Being ,Adult ,Male ,Humans ,Middle Aged ,Aged ,Aged ,80 and over ,Female ,Prognosis ,COVID-19 ,Biomarkers ,Intermediate Filaments ,Central Nervous System ,Neurofilament Proteins ,Biomarker ,NfL ,Neurosciences ,Neurology & Neurosurgery ,Clinical sciences - Abstract
Background and aimsTo investigate the prognostic value of blood neurofilament light chain protein (NfL) levels in the acute phase of coronavirus disease 2019 (COVID-19).MethodsWe conducted an individual participant data (IPD) meta-analysis after screening on MEDLINE and Scopus to May 23rd 2022. We included studies with hospitalized adult COVID-19 patients without major COVID-19-associated central nervous system (CNS) manifestations and with a measurement of blood NfL in the acute phase as well as data regarding at least one clinical outcome including intensive care unit (ICU) admission, need of mechanical ventilation (MV) and death. We derived the age-adjusted measures NfL Z scores and conducted mixed-effects modelling to test associations between NfL Z scores and other variables, encompassing clinical outcomes. Summary receiver operating characteristic curves (SROCs) were used to calculate the area under the curve (AUC) for blood NfL.ResultsWe identified 382 records, of which 7 studies were included with a total of 669 hospitalized COVID-19 cases (mean age 66.2 ± 15.0 years, 68.1% males). Median NfL Z score at admission was elevated compared to the age-corrected reference population (2.37, IQR: 1.13-3.06, referring to 99th percentile in healthy controls). NfL Z scores were significantly associated with disease duration and severity. Higher NfL Z scores were associated with a higher likelihood of ICU admission, need of MV, and death. SROCs revealed AUCs of 0.74, 0.80 and 0.71 for mortality, need of MV and ICU admission, respectively.ConclusionsBlood NfL levels were elevated in the acute phase of COVID-19 patients without major CNS manifestations and associated with clinical severity and poor outcome. The marker might ameliorate the performance of prognostic multivariable algorithms in COVID-19.
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- 2023
45. Identification of plasmid-mediated mcr-1 and chromosomal blaCTX−M-2 in Escherichia coli from fresh vegetables
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João Pedro Rueda Furlan, Ralf Lopes, Micaela Santana Ramos, Rafael da Silva Rosa, Lucas David Rodrigues dos Santos, and Eliana Guedes Stehling
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Microbiology ,QR1-502 - Published
- 2024
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46. Evidence library of meta-analytical literature assessing the sustainability of agriculture – a dataset
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Schievano, Andrea, Pérez-Soba, Marta, Bosco, Simona, Montero-Castaño, Ana, Catarino, Rui, Chen, Mathilde, Tamburini, Giovanni, Landoni, Beatrice, Mantegazza, Otho, Guerrero, Irene, Bielza, Maria, Assouline, Michael, Koeble, Renate, Dentener, Frank, Van der Velde, Marijn, Rega, Carlo, Furlan, Andrea, Paracchini, Maria Luisa, Weiss, Franz, Angileri, Vincenzo, Terres, Jean-Michel, and Makowski, David
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- 2024
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47. Nanodynamo quantifies subcellular RNA dynamics revealing extensive coupling between steps of the RNA life cycle
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Coscujuela Tarrero, Lucia, Famà, Valeria, D’Andrea, Giacomo, Maestri, Simone, de Polo, Anna, Biffo, Stefano, Furlan, Mattia, and Pelizzola, Mattia
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- 2024
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48. Inflammatory signature in amyotrophic lateral sclerosis predicting disease progression
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Femiano, Cinzia, Bruno, Antonio, Gilio, Luana, Buttari, Fabio, Dolcetti, Ettore, Galifi, Giovanni, Azzolini, Federica, Borrelli, Angela, Furlan, Roberto, Finardi, Annamaria, Musella, Alessandra, Mandolesi, Georgia, Storto, Marianna, Centonze, Diego, and Stampanoni Bassi, Mario
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- 2024
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49. Anesthetic gases environmental impact, anesthesiologists’ awareness, and improvement opportunities: a monocentric observational study
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Furlan, Ludovico, Di Francesco, Pietro, Del Marco, Patrick, Fumagalli, Jacopo, Abbruzzese, Chiara, and Grasselli, Giacomo
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- 2024
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50. Multi-scale structural characterization of ceramic-based photonic glasses for structural colors
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Häntsch, Yen, Diaz, Ana, Holler, Mirko, Krekeler, Tobias, Ritter, Martin, Rosenfeldt, Sabine, Retsch, Markus, and Furlan, Kaline P.
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- 2024
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