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98 results on '"De Horta, A."'

1. Photometric and Spectroscopic Study of Two Low Mass Ratio Contact Binary Systems: CRTS J225828.7-121122 and CRTS J030053.5+230139

Author: Wadhwa, Surjit S., Petrovic, Jelena, Tothill, Nick F. H., De Horta, Ain Y., Filipovic, Miroslav D., and Djuraševic, Gojko
Subjects: Astrophysics - Solar and Stellar Astrophysics
Abstract: The study reports photometric and spectroscopic observations of two recently recognised contact binary systems. Both systems show total eclipses and analysis of the light curves indicate both have a very low mass ratios of less than 0.3. We derive absolute parameters from colour and distance based calibrations and show that although both have low mass ratios they are likely to be in a stable orbit and unlikely to merge. In other respects both systems have characteristics similar to other contact binaries with the secondary larger and brighter than main sequence counterparts and we also find that the secondary is considerably denser than the primary in both systems., Comment: 10 pages. 3 Figures. 1 Table Accepted - Research in Astronomy and Astrophysics (RAA)
Published: 2023
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2. Metodología para la evaluación técnica de proyectos de agua y saneamiento en Cuba

Author: Córdova De Horta, Daniela
Published: 2024

3. Metodología para la evaluación técnica de proyectos de agua y saneamiento en Cuba

Author: Daniela Córdova de Horta
Subjects: abasto de agua, evaluaciones, metodología, proyectos, saneamiento, Hydraulic engineering, TC1-978, Environmental engineering, TA170-171
Abstract: El abasto de agua en Cuba se ve afectado por limitaciones económicas y financieras, además de los efectos del cambio climático, que han incrementado la sequía, afectando los servicios básicos a la población. Los sistemas de saneamiento resultan ineficientes debido a su insuficiencia. Para enfrentar estos desafíos, el gobierno cubano, con apoyo del Fondo de Cooperación para Agua y Saneamiento (FCAS), implementó el proyecto “Mejora y Ampliación de los Sistemas de Agua Potable y Saneamiento de Pequeñas Ciudades Cubanas” (2010), que incluyó la construcción y rehabilitación de plantas potabilizadoras, redes, metrocontadores y plantas de tratamiento. Se diseñó una metodología para evaluar los impactos sociales y técnicos del proyecto, permitiendo corregir deficiencias y lograr los objetivos planteados.
Published: 2024

4. New 20-cm Radio-Continuum Study of the Small Magellanic Cloud: Part I - Images

Author: Payne J. L., Galvin, T., Wong, G. F., Draskovic, D., De Horta, A. Y., Crawford, E. J., and Filipovic, M. D.
Subjects: Magellanic Clouds, Radio Continuum: galaxies, Astronomy, QB1-991
Abstract: We present and discuss new high-sensitivity and resolution radio-continuum images of the Small Magellanic Cloud (SMC) at $lambda$=20~cm($u$=1.4~GHz). The new images were created by merging 20-cm radio-continuum archival data, from the Australian Telescope Compact Array and the Parkes radio-telescope. Our images span from $sim$10arcsec to $sim$150arcsec in resolution and sensitivity of r.m.s.$geq$0.5~mJy/beam. These images will be used in future studies of the SMC's intrinsic sources and its overall extended structure.
Published: 2011

5. Multifrequency Radio Observations of a SNR in the LMC. The Case of SNR J0527-6549 (DEM L204)

Author: Bozzetto, L. M., Filipovic, M. D., Crawford, E. J., Bojicic, I. S., Payne, J. L., Medik, A., Wardlaw, B., and De Horta, A. Y.
Subjects: ISM: supernova remnants, Magellanic Clouds, Radio Continuum: ISM, Polarization, ISM: individual objects: SNR J0527-6549, Astronomy, QB1-991
Abstract: We present a detailed study and results of new Australia Telescope Compact Array (ATCA) observations of supernova remnant SNR J0527-6549. This Large Magellanic Cloud (LMC) object follows a typical supernova remnant (SNR) horseshoe morphology with a diameter of D=(66$imes$58)$pm$1~pc which is among the largest SNRs in the LMC. Its relatively large size indicates older age while a steeper than expected radio spectral index of $alpha$=-0.92$pm$0.11 is more typical of younger and energetic SNRs. Also, we report detections of regions with a high order of polarization at a peak value of $sim$ 54 per cent $pm$ 17 per cent at 6~cm.
Published: 2010

6. The 100 Strongest Radio Point Sources in the Field of the Large Magellanic Cloud at 1.4 GHz

Author: Payne, J. L., Tauber, L. A., Filipović, M. D., Crawford, E. J., and De Horta, A. Y.
Subjects: Radio Continuum: galaxies, Magellanic Clouds, Catalogs, Astronomy, QB1-991
Abstract: We present the 100 strongest 1.4~GHz point sources from a new mosaicimage in the direction of the Large Magellanic Cloud (LMC). The observationsmaking up the mosaic were made using Australia Telescope Compact Array (ATCA)over a ten year period and were combined with Parkes single dish data at 1.4 GHz to complete the image for short spacing. An initial list of co-identifications within 10arcsec at 0.843, 4.8 and 8.6 GHz consisted of 2682 sources. Elimination of extended objects and artifact noise allowed the creation of a refined list containing 1988 point sources. Most of these are presumed to be background objects seen through the LMC; a small portion may represent compact HII regions, young SNRs and radio planetary nebulae. For the 1988 point sources we find a preliminary average spectral index ($alpha$) of -0.53 and present a 1.4 GHz image showing source locationin the direction of the LMC.
Published: 2009

7. Optical Spectra of Radio Planetary Nebulae in the Large Magellanic Cloud

Author: Payne, J. L., Filipović, M. D., Millar, W. C., Crawford, E. J., De Horta, A. Y., Stootman, F. H., and Urošević, D.
Subjects: Planetary nebulae: individual: SMP L8, SMP L25, SMP L33, SMP L39, SMP L47, SMP L62, SMP L74, SMP L75, SMP L83, SMP L84, SMP L89, Astronomy, QB1-991
Abstract: We present 11 spectra from 12 candidate radio sources co-identified with known planetary nebulae (PNe) in the Large Magellanic Cloud (LMC). Originally found in Australia Telescope Compact Array (ATCA) LMC surveys at 1.4, 4.8 and 8.64~GHz and confirmed by new high resolution ATCA images at 6 and 3~cm (4arcsec/2arcsec), these complement data recently presented for candidate radio PNe in the Small Magellanic Cloud (SMC). Their spectra were obtained using the Radcliffe 1.9-meter telescope in Sutherland (South Africa). All of the optical PNe and radio candidates are within 2arcsec and may represent a population of selected radio bright sample only. Nebular ionized masses of these objects are estimated to be as high as 1.8~$M_odot$, supporting the idea that massive PNe progenitor central stars lose much of their mass in the asymptotic giant branch (AGB) phase or prior. We also identify a sub-population (33\%) of radio PNe candidates with prominent ionized iron emission lines.
Published: 2008

8. Radio-Continuum Study of the Supernova Remnants in the Large Magellanic Cloud - An SNR with a Highly Polarised Breakout Region - SNR J0455-6838

Author: Crawford, E. J., Filipović, M. D., De Horta, A. Y., Stootman, F. H., and Payne, J. L.
Subjects: ISM: supernova remnants, Magellanic Clouds, Radio Continuum: ISM, Polarization, ISM: individual objects: SNR J0455-6838, Astronomy, QB1-991
Abstract: We present the results of new moderate resolution ATCA observations of SNR. We found that this SNR exhibits a mostly typical appearance with rather steep and curved $alpha$=--0.81$pm$0.18 and D=43$imes$31$pm$1~pc. Regions of high polarisation were detected, including unusually strong ($sim$70\%) region corresponding to the northern breakout. Such a strong polarisation in breakout regions has not been observed in any other SNR.
Published: 2008

9. Optical Spectra of Radio Planetary Nebulae in the Small Magellanic Cloud

Author: Payne, J. L., Filipović, M. D., Crawford, E. J., De Horta, A. Y., White, G. L., and Stootman, F. H.
Subjects: Planetary nebulae: individual: N9, SMP11, N61, N68, Astronomy, QB1-991
Abstract: We present preliminary results from spectral observations of four (4) candidate radio sources co-identified with known planetary nebulae (PNe) in the Small Magellanic Cloud (SMC). These were made using the Radcliffe 1.9-meter telescope in Sutherland, South Africa. These radio PNe were originally found in Australia Telescope Compact Array (ATCA) surveys of the SMC at 1.42 and 2.37~GHz, and were further confirmed by new high resolution ATCA images at 6 and 3 cm (4arcsec/2arcsec). Optical PNe and radio candidates are within 2arcsec and may represent a sub-population of selected radio bright objects. Nebular ionized masses of these objects may be 2.6~$M_odot$ or greater, supporting the existence of PNe progenitor central stars with masses up to 8 $M_odot$.
Published: 2008

10. Patterns of oral anticoagulant use and outcomes in Asian patients with atrial fibrillation: a post-hoc analysis from the GLORIA-AF Registry

Author: Abban, Dzifa Wosornu, Abdul, Nasser, Abud, Atilio Marcelo, Adams, Fran, Addala, Srinivas, Adragão, Pedro, Ageno, Walter, Aggarwal, Rajesh, Agosti, Sergio, Agostoni, Piergiuseppe, Aguilar, Francisco, Linares, Julio Aguilar, Aguinaga, Luis, Ahmed, Jameel, Aiello, Allessandro, Ainsworth, Paul, Aiub, Jorge Roberto, Al-Dallow, Raed, Alderson, Lisa, Aldrete Velasco, Jorge Antonio, Alexopoulos, Dimitrios, Manterola, Fernando Alfonso, Aliyar, Pareed, Alonso, David, Alves da Costa, Fernando Augusto, Amado, José, Amara, Walid, Amelot, Mathieu, Amjadi, Nima, Ammirati, Fabrizio, Andrade, Marianna, Andrawis, Nabil, Annoni, Giorgio, Ansalone, Gerardo, Ariani, M.Kevin, Arias, Juan Carlos, Armero, Sébastien, Arora, Chander, Aslam, Muhammad Shakil, Asselman, M., Audouin, Philippe, Augenbraun, Charles, Aydin, S., Ayryanova, Ivaneta, Aziz, Emad, Backes, Luciano Marcelo, Badings, E., Bagni, Ermentina, Baker, Seth H., Bala, Richard, Baldi, Antonio, Bando, Shigenobu, Banerjee, Subhash, Bank, Alan, Esquivias, Gonzalo Barón, Barr, Craig, Bartlett, Maria, Kes, Vanja Basic, Baula, Giovanni, Behrens, Steffen, Bell, Alan, Benedetti, Raffaella, Mazuecos, Juan Benezet, Benhalima, Bouziane, Bergler-Klein, Jutta, Berneau, Jean-Baptiste, Bernstein, Richard A., Berrospi, Percy, Berti, Sergio, Berz, Andrea, Best, Elizabeth, Bettencourt, Paulo, Betzu, Robert, Bhagwat, Ravi, Bhatta, Luna, Biscione, Francesco, Bisignani, Giovanni, Black, Toby, Bloch, Michael J., Bloom, Stephen, Blumberg, Edwin, Bo, Mario, Bøhmer, Ellen, Bollmann, Andreas, Bongiorni, Maria Grazia, Boriani, Giuseppe, Boswijk, D.J., Bott, Jochen, Bottacchi, Edo, Kalan, Marica Bracic, Bradman, Drew, Brautigam, Donald, Breton, Nicolas, Brouwers, P.J.A.M., Browne, Kevin, Cortada, Jordi Bruguera, Bruni, A., Brunschwig, Claude, Buathier, Hervé, Buhl, Aurélie, Bullinga, John, Cabrera, Jose Walter, Caccavo, Alberto, Cai, Shanglang, Caine, Sarah, Calò, Leonardo, Calvi, Valeria, Sánchez, Mauricio Camarillo, Candeias, Rui, Capuano, Vincenzo, Capucci, Alessandro, Caputo, Ronald, Rizo, Tatiana Cárdenas, Cardona, Francisco, Carlos da Costa Darrieux, Francisco, Duarte Vera, Yan Carlos, Carolei, Antonio, Carreño, Susana, Carvalho, Paula, Cary, Susanna, Casu, Gavino, Cavallini, Claudio, Cayla, Guillaume, Celentano, Aldo, Cha, Tae-Joon, Cha, Kwang Soo, Chae, Jei Keon, Chalamidas, Kathrine, Challappa, Krishnan, Chand, Sunil Prakash, Chandrashekar, Harinath, Chartier, Ludovic, Chatterjee, Kausik, Chavez Ayala, Carlos Antero, Cheema, Aamir, Cheema, Amjad, Chen, Lin, Chen, Shih-Ann, Chen, Jyh Hong, Chiang, Fu-Tien, Chiarella, Francesco, Chih-Chan, Lin, Cho, Yong Keun, Choi, Jong-Il, Choi, Dong Ju, Chouinard, Guy, Hoi-Fan Chow, Danny, Chrysos, Dimitrios, Chumakova, Galina, José Roberto, Eduardo Julián, Valenzuela, Chuquiure, Nica, Nicoleta Cindea, Cislowski, David J., Clay, Anthony, Clifford, Piers, Cohen, Andrew, Cohen, Michael, Cohen, Serge, Colivicchi, Furio, Collins, Ronan, Colonna, Paolo, Compton, Steve, Connolly, Derek, Conti, Alberto, Buenostro, Gabriel Contreras, Coodley, Gregg, Cooper, Martin, Coronel, Julian, Corso, Giovanni, Sales, Juan Cosín, Cottin, Yves, Covalesky, John, Cracan, Aurel, Crea, Filippo, Crean, Peter, Crenshaw, James, Cullen, Tina, Darius, Harald, Dary, Patrick, Dascotte, Olivier, Dauber, Ira, Davalos, Vicente, Davies, Ruth, Davis, Gershan, Davy, Jean-Marc, Dayer, Mark, De Biasio, Marzia, De Bonis, Silvana, De Caterina, Raffaele, De Franceschi, Teresiano, de Groot, J.R., De Horta, José, De La Briolle, Axel, Topete, Gilberto de la Pena, Vicenzo de Paola, Angelo Amato, de Souza, Weimar, de Veer, A., De Wolf, Luc, Decoulx, Eric, Deepak, Sasalu, Defaye, Pascal, Del-Carpio Munoz, Freddy, Brkljacic, Diana Delic, Deumite, N. Joseph, Di Legge, Silvia, Diemberger, Igor, Dietz, Denise, Dionísio, Pedro, Dong, Qiang, Rossi dos Santos, Fabio, Dotcheva, Elena, Doukky, Rami, D'Souza, Anthony, Dubrey, Simon, Ducrocq, Xavier, Dupljakov, Dmitry, Duque, Mauricio, Dutta, Dipankar, Duvilla, Nathalie, Duygun, A., Dziewas, Rainer, Eaton, Charles B., Eaves, William, Ebels-Tuinbeek; Clifford Ehrlich, L.A., Eichinger-Hasenauer, Sabine, Eisenberg, Steven J., El Jabali, Adnan, El Shahawy, Mahfouz, Hernandes, Mauro Esteves, Izal, Ana Etxeberria, Evonich, Rudolph, III, Evseeva, Oksana, Ezhov, Andrey, Fahmy, Raed, Fang, Quan, Farsad, Ramin, Fauchier, Laurent, Favale, Stefano, Fayard, Maxime, Fedele, Jose Luis, Fedele, Francesco, Fedorishina, Olga, Fera, Steven R., Gomes Ferreira, Luis Gustavo, Ferreira, Jorge, Ferri, Claudio, Ferrier, Anna, Ferro, Hugo, Finsen, Alexandra, First, Brian, Fischer, Stuart, Fonseca, Catarina, Almeida, Luísa Fonseca, Forman, Steven, Frandsen, Brad, French, William, Friedman, Keith, Friese, Athena, Fruntelata, Ana Gabriela, Fujii, Shigeru, Fumagalli, Stefano, Fundamenski, Marta, Furukawa, Yutaka, Gabelmann, Matthias, Gabra, Nashwa, Gadsbøll, Niels, Galinier, Michel, Gammelgaard, Anders, Ganeshkumar, Priya, Gans, Christopher, Quintana, Antonio Garcia, Gartenlaub, Olivier, Gaspardone, Achille, Genz, Conrad, Georger, Frédéric, Georges, Jean-Louis, Georgeson, Steven, Giedrimas, Evaldas, Gierba, Mariusz, Ortega, Ignacio Gil, Gillespie, Eve, Giniger, Alberto, Giudici, Michael C., Gkotsis, Alexandros, Glotzer, Taya V., Gmehling, Joachim, Gniot, Jacek, Goethals, Peter, Goldbarg, Seth, Goldberg, Ronald, Goldmann, Britta, Golitsyn, Sergey, Gómez, Silvia, Mesa, Juan Gomez, Gonzalez, Vicente Bertomeu, Gonzalez Hermosillo, Jesus Antonio, González López, Víctor Manuel, Gorka, Hervé, Gornick, Charles, Gorog, Diana, Gottipaty, Venkat, Goube, Pascal, Goudevenos, Ioannis, Graham, Brett, Greer, G. Stephen, Gremmler, Uwe, Grena, Paul G., Grond, Martin, Gronda, Edoardo, Grönefeld, Gerian, Gu, Xiang, Torres Torres, Ivett Guadalupe, Guardigli, Gabriele, Guevara, Carolina, Guignier, Alexandre, Gulizia, Michele, Gumbley, Michael, Günther, Albrecht, Ha, Andrew, Hahalis, Georgios, Hakas, Joseph, Hall, Christian, Han, Bing, Han, Seongwook, Hargrove, Joe, Hargroves, David, Harris, Kenneth B., Haruna, Tetsuya, Hayek, Emil, Healey, Jeff, Hearne, Steven, Heffernan, Michael, Heggelund, Geir, Heijmeriks, J.A., Hemels, Maarten, Hendriks, I., Henein, Sam, Her, Sung-Ho, Hermany, Paul, Hernández Del Río, Jorge Eduardo, Higashino, Yorihiko, Hill, Michael, Hisadome, Tetsuo, Hishida, Eiji, Hoffer, Etienne, Hoghton, Matthew, Hong, Kui, Hong, Suk keun, Horbach, Stevie, Horiuchi, Masataka, Hou, Yinglong, Hsing, Jeff, Huang, Chi-Hung, Huckins, David, Hughes, kathy, Huizinga, A., Hulsman, E.L., Hung, Kuo-Chun, Hwang, Gyo-Seung, Ikpoh, Margaret, Imberti, Davide, Ince, Hüseyin, Indolfi, Ciro, Inoue, Shujiro, Irles, Didier, Iseki, Harukazu, Israel, C. Noah, Iteld, Bruce, Iyer, Venkat, Jackson-Voyzey, Ewart, Jaffrani, Naseem, Jäger, Frank, James, Martin, Jang, Sung-Won, Jaramillo, Nicolas, Jarmukli, Nabil, Jeanfreau, Robert J., Jenkins, Ronald D., Sánchez, Carlos Jerjes, Jimenez, Javier, Jobe, Robert, Joen-Jakobsen, Tomas, Jones, Nicholas, Moura Jorge, Jose Carlos, Jouve, Bernard, Jung, Byung Chun, Jung, Kyung Tae, Jung, Werner, Kachkovskiy, Mikhail, Kafkala, Krystallenia, Kalinina, Larisa, Kallmünzer, Bernd, Kamali, Farzan, Kamo, Takehiro, Kampus, Priit, Kashou, Hisham, Kastrup, Andreas, Katsivas, Apostolos, Kaufman, Elizabeth, Kawai, Kazuya, Kawajiri, Kenji, Kazmierski, John F., Keeling, P., Kerr Saraiva, José Francisco, Ketova, Galina, Khaira, Ajit Singh, Khripun, Aleksey, Kim, Doo-Il, Kim, Young Hoon, Kim, Nam Ho, Kim, Dae Kyeong, Kim, Jeong Su, Kim, June Soo, Kim, Ki Seok, Kim, Jin bae, Kinova, Elena, Klein, Alexander, Kmetzo, James J., Kneller, G. Larsen, Knezevic, Aleksandar, Angela Koh, Su Mei, Koide, Shunichi, Kollias, Anastasios, Kooistra, J.A., Koons, Jay, Koschutnik, Martin, Kostis, William J., Kovacic, Dragan, Kowalczyk, Jacek, Koziolova, Natalya, Kraft, Peter, Kragten, Johannes A., Krantz, Mori, Krause, Lars, Krenning, B.J., Krikke, F., Kromhout, Z., Krysiak, Waldemar, Kumar, Priya, Kümler, Thomas, Kuniss, Malte, Kuo, Jen-Yuan, Küppers, Achim, Karla Kurrelmeyer, Kwak, Choong Hwan, Laboulle, Bénédicte, Labovitz, Arthur, Lai, Wen Ter, Lam, Andy, Lam, Yat Yin, Zanetti, Fernando Lanas, Landau, Charles, Landini, Giancarlo, Figueiredo, Estêvão Lanna, Larsen, Torben, Lavandier, Karine, LeBlanc, Jessica, Lee, Moon Hyoung, Lee, Chang-Hoon, Lehman, John, Leitão, Ana, Lellouche, Nicolas, Lelonek, Malgorzata, Lenarczyk, Radoslaw, Lenderink, T., González, Salvador León, Leong-Sit, Peter, Leschke, Matthias, Ley, Nicolas, Li, Zhanquan, Li, Xiaodong, Li, Weihua, Li, Xiaoming, Lichy, Christhoh, Lieber, Ira, Limon Rodriguez, Ramon Horacio, Lin, Hailong, Lip, Gregory Y.H., Liu, Feng, Liu, Hengliang, Esperon, Guillermo Llamas, Navarro, Nassip Llerena, Lo, Eric, Lokshyn, Sergiy, López, Amador, López-Sendón, José Luís, Lorga Filho, Adalberto Menezes, Lorraine, Richard S., Luengas, Carlos Alberto, Luke, Robert, Luo, Ming, Lupovitch, Steven, Lyrer, Philippe, Ma, Changsheng, Ma, Genshan, Madariaga, Irene, Maeno, Koji, Magnin, Dominique, Maid, Gustavo, Mainigi, Sumeet K., Makaritsis, Konstantinos, Malhotra, Rohit, Manning, Rickey, Manolis, Athanasios, Manrique Hurtado, Helard Andres, Mantas, Ioannis, Jattin, Fernando Manzur, Maqueda, Vicky, Marchionni, Niccolo, Ortuno, Francisco Marin, Santana, Antonio Martín, Martinez, Jorge, Maskova, Petra, Hernandez, Norberto Matadamas, Matsuda, Katsuhiro, Maurer, Tillmann, Mauro, Ciro, May, Erik, Mayer, Nolan, McClure, John, McCormack, Terry, McGarity, William, McIntyre, Hugh, McLaurin, Brent, Medina Palomino, Feliz Alvaro, Melandri, Francesco, Meno, Hiroshi, Menzies, Dhananjai, Mercader, Marco, Meyer, Christian, Meyer, Beat J., Miarka, Jacek, Mibach, Frank, Michalski, Dominik, Michel, Patrik, Chreih, Rami Mihail, Mikdadi, Ghiath, Mikus, Milan, Milicic, Davor, Militaru, Constantin, Minaie, Sedi, Minescu, Bogdan, Mintale, Iveta, Mirault, Tristan, Mirro, Michael J., Mistry, Dinesh, Miu, Nicoleta Violeta, Miyamoto, Naomasa, Moccetti, Tiziano, Mohammed, Akber, Nor, Azlisham Mohd, Mollerus, Michael, Molon, Giulio, Mondillo, Sergio, Moniz, Patrícia, Mont, Lluis, Montagud, Vicente, Montaña, Oscar, Monti, Cristina, Moretti, Luciano, Mori, Kiyoo, Moriarty, Andrew, Morka, Jacek, Moschini, Luigi, Moschos, Nikitas, Mügge, Andreas, Mulhearn, Thomas J., Muresan, Carmen, Muriago, Michela, Musial, Wlodzimierz, Musser, Carl W., Musumeci, Francesco, Nageh, Thuraia, Nakagawa, Hidemitsu, Nakamura, Yuichiro, Nakayama, Toru, Nam, Gi-Byoung, Nanna, Michele, Natarajan, Indira, Nayak, Hemal M., Naydenov, Stefan, Nazlić, Jurica, Cristian Nechita, Alexandru, Nechvatal, Libor, Negron, Sandra Adela, Neiman, James, Neuenschwander, Fernando Carvalho, Neves, David, Neykova, Anna, Miguel, Ricardo Nicolás, Nijmeh, George, Nizov, Alexey, Campos, Rodrigo Noronha, Nossan, Janko, Novikova, Tatiana, Nowalany-Kozielska, Ewa, Nsah, Emmanuel, Nunez Fragoso, Juan Carlos, Nurgalieva, Svetlana, Nuyens, Dieter, Nyvad, Ole, Odin de Los Rios Ibarra, Manuel, O'Donnell, Philip, O'Donnell, Martin, Oh, Seil, Oh, Yong Seog, Oh, Dongjin, O'Hara, Gilles, Oikonomou, Kostas, Olivares, Claudia, Oliver, Richard, Ruiz, Rafael Olvera, Olympios, Christoforos, omaszuk-Kazberuk, Anna, Asensi, Joaquín Osca, Jose, eena Padayattil, Padilla Padilla, Francisco Gerardo, Rios, Victoria Padilla, Pajes, Giuseppe, Pandey, Shekhar, Paparella, Gaetano, Paris, F., Park, Hyung Wook, Park, Jong Sung, Parthenakis, Fragkiskos, Passamonti, Enrico, Patel, Rajesh J., Patel, Jaydutt, Patel, Mehool, Patrick, Janice, Jimenez, Ricardo Pavón, Paz, Analía, Pengo, Vittorio, Pentz, William, Pérez, Beatriz, Pérez Ríos, Alma Minerva, Pérez-Cabezas, Alejandro, Perlman, Richard, Persic, Viktor, Perticone, Francesco, Peters, Terri K., Petkar, Sanjiv, Pezo, Luis Felipe, Pflücke, Christian, Pham, David N., Phillips, Roland T., Phlaum, Stephen, Pieters, Denis, Pineau, Julien, Pinter, Arnold, Pinto, Fausto, Pisters, R., Pivac, Nediljko, Pocanic, Darko, Podoleanu, Cristian, Politano, Alessandro, Poljakovic, Zdravka, Pollock, Stewart, Garcéa, Jose Polo, Poppert, Holger, Porcu, Maurizio, Reino, Antonio Pose, Prasad, Neeraj, Précoma, Dalton Bertolim, Prelle, Alessandro, Prodafikas, John, Protasov, Konstantin, Pye, Maurice, Qiu, Zhaohui, Quedillac, Jean-Michel, Raev, Dimitar, Raffo Grado, Carlos Antonio, Rahimi, Sidiqullah, Raisaro, Arturo, Rama, Bhola, Ramos, Ricardo, Ranieri, Maria, Raposo, Nuno, Rashba, Eric, Rauch-Kroehnert, Ursula, Reddy, Ramakota, Renda, Giulia, Reza, Shabbir, Ria, Luigi, Richter, Dimitrios, Rickli, Hans, Rieker, Werner, Vera, Tomas Ripolil, Ritt, Luiz Eduardo, Roberts, Douglas, Briones, Ignacio Rodriguez, Rodriguez Escudero, Aldo Edwin, Pascual, Carlos Rodríguez, Roman, Mark, Romeo, Francesco, Ronner, E., Roux, Jean-Francois, Rozkova, Nadezda, Rubacek, Miroslav, Rubalcava, Frank, Russo, Andrea M., Rutgers, Matthieu Pierre, Rybak, Karin, Said, Samir, Sakamoto, Tamotsu, Salacata, Abraham, Salem, Adrien, Bodes, Rafael Salguero, Saltzman, Marco A., Salvioni, Alessandro, Vallejo, Gregorio Sanchez, Fernández, Marcelo Sanmartín, Saporito, Wladmir Faustino, Sarikonda, Kesari, Sasaoka, Taishi, Sati, Hamdi, Savelieva, Irina, Scala, Pierre-Jean, Schellinger, Peter, Scherr, Carlos, Schmitz, Lisa, Schmitz, Karl-Heinz, Schmitz, Bettina, Schnabel, Teresa, Schnupp, Steffen, Schoeniger, Peter, Schön, Norbert, Schwimmbeck, Peter, Seamark, Clare, Searles, Greg, Seidl, Karl-Heinz, Seidman, Barry, Sek, Jaroslaw, Sekaran, Lakshmanan, Serrati, Carlo, Shah, Neerav, Shah, Vinay, Shah, Anil, Shah, Shujahat, Sharma, Vijay Kumar, Shaw, Louise, Sheikh, Khalid H., Shimizu, Naruhito, Shimomura, Hideki, Shin, Dong-Gu, Shin, Eun-Seok, Shite, Junya, Sibilio, Gerolamo, Silver, Frank, Sime, Iveta, Simmers, Tim A., Singh, Narendra, Siostrzonek, Peter, Smadja, Didier, Smith, David W., Snitman, Marcelo, Filho, Dario Sobral, Soda, Hassan, Sofley, Carl, Sokal, Adam, Oi Yan, Yannie Soo, Sotolongo, Rodolfo, Ferreira de Souza, Olga, Sparby, Jon Arne, Spinar, Jindrich, Sprigings, David, Spyropoulos, Alex C., Stakos, Dimitrios, Steinwender, Clemens, Stergiou, Georgios, Stiell, Ian, Stoddard, Marcus, Stoikov, Anastas, Streb, Witold, Styliadis, Ioannis, Su, Guohai, Su, Xi, Sudnik, Wanda, Sukles, Kai, Sun, Xiaofei, Swart, H., Szavits-Nossan, Janko, Taggeselle, Jens, Takagi, Yuichiro, Singh Takhar, Amrit Pal, Tamm, Angelika, Tanaka, Katsumi, Tanawuttiwat, Tanyanan, Tang, Sherman, Tang, Aylmer, Tarsi, Giovanni, Tassinari, Tiziana, Tayal, Ashis, Tayebjee, Muzahir, Berg, J.M. ten, Tesloianu, Dan, The, Salem H.K., Thomas, Dierk, Timsit, Serge, Tobaru, Tetsuya, Tomasik, Andrzej R., Torosoff, Mikhail, Touze, Emmanuel, Trendafilova, Elina, Tsai, W. Kevin, Tse, Hung Fat, Tsutsui, Hiroshi, Tu, Tian Ming, Tuininga, Ype, Turakhia, Minang, Turk, Samir, Turner, Wayne, Tveit, Arnljot, Tytus, Richard, Valadão, C., van Bergen, P.F.M.M., van de Borne, Philippe, van den Berg, B.J., van der Zwaan, C., Van Eck, M., Vanacker, Peter, Vasilev, Dimo, Vasilikos, Vasileios, Vasilyev, Maxim, Veerareddy, Srikar, Miño; Asok Venkataraman, Mario Vega, Verdecchia, Paolo, Versaci, Francesco, Vester, Ernst Günter, Vial, Hubert, Victory, Jason, Villamil, Alejandro, Vincent, Marc, Vlastaris, Anthony, Dahl, Jürgen vom, Vora, Kishor, Vranian, Robert B., Wakefield, Paul, Wang, Ningfu, Wang, Mingsheng, Wang, Xinhua, Wang, Feng, Wang, Tian, Warner, Alberta L., Watanabe, Kouki, Wei, Jeanne, Weimar, Christian, Weiner, Stanislav, Weinrich, Renate, Wen, Ming-Shien, Wiemer, Marcus, Wiggers, Preben, Wilke, Andreas, Williams, David, Williams, Marcus L., Witzenbichler, Bernhard, Wong, Brian, Lawrence Wong, Ka Sing, Wozakowska-Kaplon, Beata, Wu, Shulin, Wu, Richard C., Wunderlich, Silke, Wyatt, Nell, Wylie, John (Jack), Xu, Yong, Xu, Xiangdong, Yamanoue, Hiroki, Yamashita, Takeshi, Bryan Yan, Ping Yen, Yang, Tianlun, Yao, Jing, Yeh, Kuo-Ho, Yin, Wei Hsian, Yotov, Yoto, Zahn, Ralf, Zarich, Stuart, Zenin, Sergei, Zeuthen, Elisabeth Louise, Zhang, Huanyi, Zhang, Donghui, Zhang, Xingwei, Zhang, Ping, Zhang, Jun, Zhao, Shui Ping, Zhao, Yujie, Zhao, Zhichen, Zheng, Yang, Zhou, Jing, Zimmermann, Sergio, Zini, Andrea, Zizzo, Steven, Zong, Wenxia, Zukerman, L. Steven, Romiti, Giulio Francesco, Corica, Bernadette, Proietti, Marco, Mei, Davide Antonio, Frydenlund, Juliane, Bisson, Arnaud, Olshansky, Brian, Chan, Yi-Hsin, Huisman, Menno V., and Chao, Tze-Fan
Published: 2023
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11. Effective temperature and the light curve solution of contact binary systems

Author: Wadhwa S., Tothill N.F.H., Filipović M.D., and de Horta A.Y.
Subjects: techniques: photometric, stars: binaries: eclipsing, stars: low-mass, Astronomy, QB1-991
Abstract: With an increasing number of contact binary discoveries and the recognition that luminous red novae are the result of contact binary merger events, there has been a significant increase in the number of light curve solutions appearing in the literature. One key element of such solutions is assigning and fixing the effective temperature of the primary component (T1). Sometimes the expectation that the assigned temperature will significantly alter light curve solution is exaggerated even though theoretical considerations suggest that the absolute value of T1 has little influence on the geometric elements of the light curve solution. In this study, we show that assigning T1 over a range of 1000 K has no significant influence on the light curve solutions of two extreme low mass ratio contact binary systems. In addition, we explore the use of photometric spectral energy distribution as a potential standard for assigning T1 in the absence of spectroscopic observations.
Published: 2023
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12. Analysis of dual band and survey photometry of two low mass ratio contact binary systems

Author: WADHWA, SURJIT S., DE HORTA, AIN Y., FILIPOVIĆ, MIROSLAV D., and TOTOHILL, F. H. NICK
Published: 2022
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13. Simplified method for the identification of low mass ratio contact binary systems that are potential red nova progenitors

Author: Wadhwa, Surjit S., De Horta, Ain Y., Filipović, Miroslav D., Tothill, Nick F. H., Arbutina, Bojan, Petrović, Jelena, and Djurašević, Gojko
Published: 2022
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14. Polarimetric detection of non-radial oscillation modes in the β Cephei star β Crucis

Author: Cotton, Daniel V., Buzasi, Derek L., Aerts, Conny, Bailey, Jeremy, Burssens, Siemen, Pedersen, May G., Stello, Dennis, Kedziora-Chudczer, Lucyna, De Horta, Ain, De Cat, Peter, Lewis, Fiona, Malla, Sai Prathyusha, Wright, Duncan J., and Bott, Kimberly
Published: 2022
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15. Simulación numérica de la red de drenaje pluvial de la cuenca Gancedo. La Habana

Author: de Horta Brito, Patricia Ruth and Pino Plans, Luis Manuel
Published: 2021

16. Simulación numérica del drenaje pluvial de la CUJAE. Soluciones propuestas

Author: de Horta Brito, Patricia Ruth and Córdova López, Luis Fermín
Published: 2021

17. Anticoagulant selection in relation to the SAMe-TT2R2 score in patients with atrial fibrillation: The GLORIA-AF registry

Author: George Ntaios, Menno V. Huisman, Hans-Christoph Diener, Jonathan L. Halperin, Christine Teutsch, Sabrina Marler, Venkatesh K. Gurusamy, Milla Thompson, Gregory Y.H. Lip, Brian Olshansky, Dzifa Wosornu Abban, Nasser Abdul, Atilio Marcelo Abud, Fran Adams, Srinivas Addala, Pedro Adragão, Walter Ageno, Rajesh Aggarwal, Sergio Agosti, Piergiuseppe Agostoni, Francisco Aguilar, Julio Aguilar Linares, Luis Aguinaga, Jameel Ahmed, Allessandro Aiello, Paul Ainsworth, Jorge Roberto Aiub, Raed Al-Dallow, Lisa Alderson, Jorge Antonio Aldrete Velasco, Dimitrios Alexopoulos, Fernando Alfonso Manterola, Pareed Aliyar, David Alonso, Fernando Augusto Alves da Costa, José Amado, Walid Amara, Mathieu Amelot, Nima Amjadi, Fabrizio Ammirati, Marianna Andrade, Nabil Andrawis, Giorgio Annoni, Gerardo Ansalone, M.Kevin Ariani, Juan Carlos Arias, Sébastien Armero, Chander Arora, Muhammad Shakil Aslam, M. Asselman, Philippe Audouin, Charles Augenbraun, S. Aydin, Ivaneta Ayryanova, Emad Aziz, Luciano Marcelo Backes, E. Badings, Ermentina Bagni, Seth H. Baker, Richard Bala, Antonio Baldi, Shigenobu Bando, Subhash Banerjee, Alan Bank, Gonzalo Barón Esquivias, Craig Barr, Maria Bartlett, Vanja Basic Kes, Giovanni Baula, Steffen Behrens, Alan Bell, Raffaella Benedetti, Juan Benezet Mazuecos, Bouziane Benhalima, Jutta Bergler-Klein, Jean-Baptiste Berneau, Richard A. Bernstein, Percy Berrospi, Sergio Berti, Andrea Berz, Elizabeth Best, Paulo Bettencourt, Robert Betzu, Ravi Bhagwat, Luna Bhatta, Francesco Biscione, Giovanni BISIGNANI, Toby Black, Michael J. Bloch, Stephen Bloom, Edwin Blumberg, Mario Bo, Ellen Bøhmer, Andreas Bollmann, Maria Grazia Bongiorni, Giuseppe Boriani, D.J. Boswijk, Jochen Bott, Edo Bottacchi, Marica Bracic Kalan, Drew Bradman, Donald Brautigam, Nicolas Breton, P.J.A.M. Brouwers, Kevin Browne, Jordi Bruguera Cortada, A. Bruni, Claude Brunschwig, Hervé Buathier, Aurélie Buhl, John Bullinga, Jose Walter Cabrera, Alberto Caccavo, Shanglang Cai, Sarah Caine, Leonardo Calò, Valeria Calvi, Mauricio Camarillo Sánchez, Rui Candeias, Vincenzo Capuano, Alessandro Capucci, Ronald Caputo, Tatiana Cárdenas Rizo, Francisco Cardona, Francisco Carlos da Costa Darrieux, Yan Carlos Duarte Vera, Antonio Carolei, Susana Carreño, Paula Carvalho, Susanna Cary, Gavino Casu, Claudio Cavallini, Guillaume Cayla, Aldo Celentano, Tae-Joon Cha, Kwang Soo Cha, Jei Keon Chae, Kathrine Chalamidas, Krishnan Challappa, Sunil Prakash Chand, Harinath Chandrashekar, Ludovic Chartier, Kausik Chatterjee, Carlos Antero Chavez Ayala, Aamir Cheema, Amjad Cheema, Lin Chen, Shih-Ann Chen, Jyh Hong Chen, Fu-Tien Chiang, Francesco Chiarella, Lin Chih-Chan, Yong Keun Cho, Jong-Il Choi, Dong Ju Choi, Guy Chouinard, Danny Hoi-Fan Chow, Dimitrios Chrysos, Galina Chumakova, Eduardo Julián José Roberto Chuquiure Valenzuela, Nicoleta Cindea Nica, David J. Cislowski, Anthony Clay, Piers Clifford, Andrew Cohen, Michael Cohen, Serge Cohen, Furio Colivicchi, Ronan Collins, Paolo Colonna, Steve Compton, Derek Connolly, Alberto Conti, Gabriel Contreras Buenostro, Gregg Coodley, Martin Cooper, Julian Coronel, Giovanni Corso, Juan Cosín Sales, Yves Cottin, John Covalesky, Aurel Cracan, Filippo Crea, Peter Crean, James Crenshaw, Tina Cullen, Harald Darius, Patrick Dary, Olivier Dascotte, Ira Dauber, Vicente Davalos, Ruth Davies, Gershan Davis, Jean-Marc Davy, Mark Dayer, Marzia De Biasio, Silvana De Bonis, Raffaele De Caterina, Teresiano De Franceschi, J.R. de Groot, José De Horta, Axel De La Briolle, Gilberto de la Pena Topete, Angelo Amato Vicenzo de Paola, Weimar de Souza, A. de Veer, Luc De Wolf, Eric Decoulx, Sasalu Deepak, Pascal Defaye, Freddy Del-Carpio Munoz, Diana Delic Brkljacic, N. Joseph Deumite, Silvia Di Legge, Igor Diemberger, Denise Dietz, Pedro Dionísio, Qiang Dong, Fabio Rossi dos Santos, Elena Dotcheva, Rami Doukky, Anthony D'Souza, Simon Dubrey, Xavier Ducrocq, Dmitry Dupljakov, Mauricio Duque, Dipankar Dutta, Nathalie Duvilla, A. Duygun, Rainer Dziewas, Charles B. Eaton, William Eaves, L.A. Ebels-Tuinbeek, Clifford Ehrlich, Sabine Eichinger-Hasenauer, Steven J. Eisenberg, Adnan El Jabali, Mahfouz El Shahawy, Mauro Esteves Hernandes, Ana Etxeberria Izal, Rudolph Evonich, III, Oksana Evseeva, Andrey Ezhov, Raed Fahmy, Quan Fang, Ramin Farsad, Laurent Fauchier, Stefano Favale, Maxime Fayard, Jose Luis Fedele, Francesco Fedele, Olga Fedorishina, Steven R. Fera, Luis Gustavo Gomes Ferreira, Jorge Ferreira, Claudio Ferri, Anna Ferrier, Hugo Ferro, Alexandra Finsen, Brian First, Stuart Fischer, Catarina Fonseca, Luísa Fonseca Almeida, Steven Forman, Brad Frandsen, William French, Keith Friedman, Athena Friese, Ana Gabriela Fruntelata, Shigeru Fujii, Stefano Fumagalli, Marta Fundamenski, Yutaka Furukawa, Matthias Gabelmann, Nashwa Gabra, Niels Gadsbøll, Michel Galinier, Anders Gammelgaard, Priya Ganeshkumar, Christopher Gans, Antonio Garcia Quintana, Olivier Gartenlaub, Achille Gaspardone, Conrad Genz, Frédéric Georger, Jean-Louis Georges, Steven Georgeson, Evaldas Giedrimas, Mariusz Gierba, Ignacio Gil Ortega, Eve Gillespie, Alberto Giniger, Michael C. Giudici, Alexandros Gkotsis, Taya V. Glotzer, Joachim Gmehling, Jacek Gniot, Peter Goethals, Seth Goldbarg, Ronald Goldberg, Britta Goldmann, Sergey Golitsyn, Silvia Gómez, Juan Gomez Mesa, Vicente Bertomeu Gonzalez, Jesus Antonio Gonzalez Hermosillo, Víctor Manuel González López, Hervé Gorka, Charles Gornick, Diana Gorog, Venkat Gottipaty, Pascal Goube, Ioannis Goudevenos, Brett Graham, G. Stephen Greer, Uwe Gremmler, Paul G. Grena, Martin Grond, Edoardo Gronda, Gerian Grönefeld, Xiang Gu, Ivett Guadalupe Torres Torres, Gabriele Guardigli, Carolina Guevara, Alexandre Guignier, Michele Gulizia, Michael Gumbley, Albrecht Günther, Andrew Ha, Georgios Hahalis, Joseph Hakas, Christian Hall, Bing Han, Seongwook Han, Joe Hargrove, David Hargroves, Kenneth B. Harris, Tetsuya Haruna, Emil Hayek, Jeff Healey, Steven Hearne, Michael Heffernan, Geir Heggelund, J.A. Heijmeriks, Maarten Hemels, I. Hendriks, Sam Henein, Sung-Ho Her, Paul Hermany, Jorge Eduardo Hernández Del Río, Yorihiko Higashino, Michael Hill, Tetsuo Hisadome, Eiji Hishida, Etienne Hoffer, Matthew Hoghton, Kui Hong, Suk keun Hong, Stevie Horbach, Masataka Horiuchi, Yinglong Hou, Jeff Hsing, Chi-Hung Huang, David Huckins, kathy Hughes, A. Huizinga, E.L. Hulsman, Kuo-Chun Hung, Gyo-Seung Hwang, Margaret Ikpoh, Davide Imberti, Hüseyin Ince, Ciro Indolfi, Shujiro Inoue, Didier Irles, Harukazu Iseki, C. Noah Israel, Bruce Iteld, Venkat Iyer, Ewart Jackson-Voyzey, Naseem Jaffrani, Frank Jäger, Martin James, Sung-Won Jang, Nicolas Jaramillo, Nabil Jarmukli, Robert J. Jeanfreau, Ronald D. Jenkins, Carlos Jerjes Sánchez, Javier Jimenez, Robert Jobe, Tomas Joen-Jakobsen, Nicholas Jones, Jose Carlos Moura Jorge, Bernard Jouve, Byung Chun Jung, Kyung Tae Jung, Werner Jung, Mikhail Kachkovskiy, Krystallenia Kafkala, Larisa Kalinina, Bernd Kallmünzer, Farzan Kamali, Takehiro Kamo, Priit Kampus, Hisham Kashou, Andreas Kastrup, Apostolos Katsivas, Elizabeth Kaufman, Kazuya Kawai, Kenji Kawajiri, John F. Kazmierski, P. Keeling, José Francisco Kerr Saraiva, Galina Ketova, AJIT Singh Khaira, Aleksey Khripun, Doo-Il Kim, Young Hoon Kim, Nam Ho Kim, Dae Kyeong Kim, Jeong Su Kim, June Soo Kim, Ki Seok Kim, Jin bae Kim, Elena Kinova, Alexander Klein, James J. Kmetzo, G. Larsen Kneller, Aleksandar Knezevic, Su Mei Angela Koh, Shunichi Koide, Anastasios Kollias, J.A. Kooistra, Jay Koons, Martin Koschutnik, William J. Kostis, Dragan Kovacic, Jacek Kowalczyk, Natalya Koziolova, Peter Kraft, Johannes A. Kragten, Mori Krantz, Lars Krause, B.J. Krenning, F. Krikke, Z. Kromhout, Waldemar Krysiak, Priya Kumar, Thomas Kümler, Malte Kuniss, Jen-Yuan Kuo, Achim Küppers, Karla Kurrelmeyer, Choong Hwan Kwak, Bénédicte Laboulle, Arthur Labovitz, Wen Ter Lai, Andy Lam, Yat Yin Lam, Fernando Lanas Zanetti, Charles Landau, Giancarlo Landini, Estêvão Lanna Figueiredo, Torben Larsen, Karine Lavandier, Jessica LeBlanc, Moon Hyoung Lee, Chang-Hoon Lee, John Lehman, Ana Leitão, Nicolas Lellouche, Malgorzata Lelonek, Radoslaw Lenarczyk, T. Lenderink, Salvador León González, Peter Leong-Sit, Matthias Leschke, Nicolas Ley, Zhanquan Li, Xiaodong Li, Weihua Li, Xiaoming Li, Christhoh Lichy, Ira Lieber, Ramon Horacio Limon Rodriguez, Hailong Lin, Feng Liu, Hengliang Liu, Guillermo Llamas Esperon, Nassip Llerena Navarro, Eric Lo, Sergiy Lokshyn, Amador López, José Luís López-Sendón, Adalberto Menezes Lorga Filho, Richard S. Lorraine, Carlos Alberto Luengas, Robert Luke, Ming Luo, Steven Lupovitch, Philippe Lyrer, Changsheng Ma, Genshan Ma, Irene Madariaga, Koji Maeno, Dominique Magnin, Gustavo Maid, Sumeet K. Mainigi, Konstantinos Makaritsis, Rohit Malhotra, Rickey Manning, Athanasios Manolis, Helard Andres Manrique Hurtado, Ioannis Mantas, Fernando Manzur Jattin, Vicky Maqueda, Niccolo Marchionni, Francisco Marin Ortuno, Antonio Martín Santana, Jorge Martinez, Petra Maskova, Norberto Matadamas Hernandez, Katsuhiro Matsuda, Tillmann Maurer, Ciro Mauro, Erik May, Nolan Mayer, John McClure, Terry McCormack, William McGarity, Hugh McIntyre, Brent McLaurin, Feliz Alvaro Medina Palomino, Francesco Melandri, Hiroshi Meno, Dhananjai Menzies, Marco Mercader, Christian Meyer, Beat j. Meyer, Jacek Miarka, Frank Mibach, Dominik Michalski, Patrik Michel, Rami Mihail Chreih, Ghiath Mikdadi, Milan Mikus, Davor Milicic, Constantin Militaru, Sedi Minaie, Bogdan Minescu, Iveta Mintale, Tristan Mirault, Michael J. Mirro, Dinesh Mistry, Nicoleta Violeta Miu, Naomasa Miyamoto, Tiziano Moccetti, Akber Mohammed, Azlisham Mohd Nor, Michael Mollerus, Giulio Molon, Sergio Mondillo, Patrícia Moniz, Lluis Mont, Vicente Montagud, Oscar Montaña, Cristina Monti, Luciano Moretti, Kiyoo Mori, Andrew Moriarty, Jacek Morka, Luigi Moschini, Nikitas Moschos, Andreas Mügge, Thomas J. Mulhearn, Carmen Muresan, Michela Muriago, Wlodzimierz Musial, Carl W. Musser, Francesco Musumeci, Thuraia Nageh, Hidemitsu Nakagawa, Yuichiro Nakamura, Toru Nakayama, Gi-Byoung Nam, Michele Nanna, Indira Natarajan, Hemal M. Nayak, Stefan Naydenov, Jurica Nazli, Alexandru Cristian Nechita, Libor Nechvatal, Sandra Adela Negron, James Neiman, Fernando Carvalho Neuenschwander, David Neves, Anna Neykova, Ricardo Nicolás Miguel, George Nijmeh, Alexey Nizov, Rodrigo Noronha Campos, Janko Nossan, Tatiana Novikova, Ewa Nowalany-Kozielska, Emmanuel Nsah, Juan Carlos Nunez Fragoso, Svetlana Nurgalieva, Dieter Nuyens, Ole Nyvad, Manuel Odin de Los Rios Ibarra, Philip O'Donnell, Martin O'Donnell, Seil Oh, Yong Seog Oh, Dongjin Oh, Gilles O'Hara, Kostas Oikonomou, Claudia Olivares, Richard Oliver, Rafael Olvera Ruiz, Christoforos Olympios, Anna omaszuk-Kazberuk, Joaquín Osca Asensi, eena Padayattil jose, Francisco Gerardo Padilla Padilla, Victoria Padilla Rios, Giuseppe Pajes, A. Shekhar Pandey, Gaetano Paparella, F. Paris, Hyung Wook Park, Jong Sung Park, Fragkiskos Parthenakis, Enrico Passamonti, Rajesh J. Patel, Jaydutt Patel, Mehool Patel, Janice Patrick, Ricardo Pavón Jimenez, Analía Paz, Vittorio Pengo, William Pentz, Beatriz Pérez, Alma Minerva Pérez Ríos, Alejandro Pérez-Cabezas, Richard Perlman, Viktor Persic, Francesco Perticone, Terri K. Peters, Sanjiv Petkar, Luis Felipe Pezo, Christian Pflücke, David N. Pham, Roland T. Phillips, Stephen Phlaum, Denis Pieters, Julien Pineau, Arnold Pinter, Fausto Pinto, R. Pisters, Nediljko Pivac, Darko Pocanic, Cristian Podoleanu, Alessandro Politano, Zdravka Poljakovic, Stewart Pollock, Jose Polo Garcéa, Holger Poppert, Maurizio Porcu, Antonio Pose Reino, Neeraj Prasad, Dalton Bertolim Précoma, Alessandro Prelle, John Prodafikas, Konstantin Protasov, Maurice Pye, Zhaohui Qiu, Jean-Michel Quedillac, Dimitar Raev, Carlos Antonio Raffo Grado, Sidiqullah Rahimi, Arturo Raisaro, Bhola Rama, Ricardo Ramos, Maria Ranieri, Nuno Raposo, Eric Rashba, Ursula Rauch-Kroehnert, Ramakota Reddy, Giulia Renda, Shabbir Reza, Luigi Ria, Dimitrios Richter, Hans Rickli, Werner Rieker, Tomas Ripolil Vera, Luiz Eduardo Ritt, Douglas Roberts, Ignacio Rodriguez Briones, Aldo Edwin Rodriguez Escudero, Carlos Rodríguez Pascual, Mark Roman, Francesco Romeo, E. Ronner, Jean-Francois Roux, Nadezda Rozkova, Miroslav Rubacek, Frank Rubalcava, Andrea M. Russo, Matthieu Pierre Rutgers, Karin Rybak, Samir Said, Tamotsu Sakamoto, Abraham Salacata, Adrien Salem, Rafael Salguero Bodes, Marco A. Saltzman, Alessandro Salvioni, Gregorio Sanchez Vallejo, Marcelo Sanmartín Fernández, Wladmir Faustino Saporito, Kesari Sarikonda, Taishi Sasaoka, Hamdi Sati, Irina Savelieva, Pierre-Jean Scala, Peter Schellinger, Carlos Scherr, Lisa Schmitz, Karl-Heinz Schmitz, Bettina Schmitz, Teresa Schnabel, Steffen Schnupp, Peter Schoeniger, Norbert Schön, Peter Schwimmbeck, Clare Seamark, Greg Searles, Karl-Heinz Seidl, Barry Seidman, Jaroslaw Sek, Lakshmanan Sekaran, Carlo SERRATI, Neerav Shah, Vinay Shah, Anil Shah, Shujahat Shah, Vijay Kumar Sharma, Louise Shaw, Khalid H. Sheikh, Naruhito Shimizu, Hideki Shimomura, Dong-Gu Shin, Eun-Seok Shin, Junya Shite, Gerolamo Sibilio, Frank Silver, Iveta Sime, Tim A. Simmers, Narendra Singh, Peter Siostrzonek, Didier Smadja, David W. Smith, Marcelo Snitman, Dario Sobral Filho, Hassan Soda, Carl Sofley, Adam Sokal, Yannie Soo Oi Yan, Rodolfo Sotolongo, Olga Ferreira de Souza, Jon Arne Sparby, Jindrich Spinar, David Sprigings, Alex C. Spyropoulos, Dimitrios Stakos, Clemens Steinwender, George Stergiou, Ian Stiell, Marcus Stoddard, Anastas Stoikov, Witold Streb, Ioannis Styliadis, Guohai Su, Xi Su, Wanda Sudnik, Kai Sukles, Xiaofei Sun, H. Swart, Janko Szavits-Nossan, Jens Taggeselle, Yuichiro Takagi, Amrit Pal Singh Takhar, Angelika Tamm, Katsumi Tanaka, Tanyanan Tanawuttiwat, Sherman Tang, Aylmer Tang, Giovanni Tarsi, Tiziana Tassinari, Ashis Tayal, Muzahir Tayebjee, J.M. ten Berg, Dan Tesloianu, Salem H.K. The, Dierk Thomas, Serge Timsit, Tetsuya Tobaru, Andrzej R. Tomasik, Mikhail Torosoff, Emmanuel Touze, Elina Trendafilova, W. Kevin Tsai, Hung Fat Tse, Hiroshi Tsutsui, Tian Ming Tu, Ype Tuininga, Minang Turakhia, Samir Turk, Wayne Tcurner, Arnljot Tveit, Richard Tytus, C. Valadão, P.F.M.M. van Bergen, Philippe van de Borne, B.J. van den Berg, C. van der Zwaan, M. Van Eck, Peter Vanacker, Dimo Vasilev, Vasileios Vasilikos, Maxim Vasilyev, Srikar Veerareddy, Mario Vega Miño, Asok Venkataraman, Paolo Verdecchia, Francesco Versaci, Ernst Günter Vester, Hubert Vial, Jason Victory, Alejandro Villamil, Marc Vincent, Anthony Vlastaris, Jürgen vom Dahl, Kishor Vora, Robert B. Vranian, Paul Wakefield, Ningfu Wang, Mingsheng Wang, Xinhua Wang, Feng Wang, Tian Wang, Alberta L. Warner, Kouki Watanabe, Jeanne Wei, Christian Weimar, Stanislav Weiner, Renate Weinrich, Ming-Shien Wen, Marcus Wiemer, Preben Wiggers, Andreas Wilke, David Williams, Marcus L. Williams, Bernhard Witzenbichler, Brian Wong, Ka Sing Lawrence Wong, Beata Wozakowska-Kaplon, Shulin Wu, Richard C. Wu, Silke Wunderlich, Nell Wyatt, John (Jack) Wylie, Yong Xu, Xiangdong Xu, Hiroki Yamanoue, Takeshi Yamashita, Ping Yen Bryan Yan, Tianlun Yang, Jing Yao, Kuo-Ho Yeh, Wei Hsian Yin, Yoto Yotov, Ralf Zahn, Stuart Zarich, Sergei Zenin, Elisabeth Louise Zeuthen, Huanyi Zhang, Donghui Zhang, Xingwei Zhang, Ping Zhang, Jun Zhang, Shui Ping Zhao, Yujie Zhao, Zhichen Zhao, Yang Zheng, Jing Zhou, Sergio Zimmermann, Andrea Zini, Steven Zizzo, Wenxia Zong, and L Steven Zukerman
Subjects: SAMe-TT2R2, atrial fibrillation, non-vitamin-K antagonist oral anticoagulants, vitamin-K-antagonist oral anticoagulants, Diseases of the circulatory (Cardiovascular) system, RC666-701
Abstract: Aim: The SAMe-TT2R2 score helps identify patients with atrial fibrillation (AF) likely to have poor anticoagulation control during anticoagulation with vitamin K antagonists (VKA) and those with scores >2 might be better managed with a target-specific oral anticoagulant (NOAC). We hypothesized that in clinical practice, VKAs may be prescribed less frequently to patients with AF and SAMe-TT2R2 scores >2 than to patients with lower scores. Methods and results: We analyzed the Phase III dataset of the Global Registry on Long-Term Oral Antithrombotic Treatment in Patients with Atrial Fibrillation (GLORIA-AF), a large, global, prospective global registry of patients with newly diagnosed AF and ≥1 stroke risk factor. We compared baseline clinical characteristics and antithrombotic prescriptions to determine the probability of the VKA prescription among anticoagulated patients with the baseline SAMe-TT2R2 score >2 and ≤ 2. Among 17,465 anticoagulated patients with AF, 4,828 (27.6%) patients were prescribed VKA and 12,637 (72.4%) patients an NOAC: 11,884 (68.0%) patients had SAMe-TT2R2 scores 0-2 and 5,581 (32.0%) patients had scores >2. The proportion of patients prescribed VKA was 28.0% among patients with SAMe-TT2R2 scores >2 and 27.5% in those with scores ≤2. Conclusions: The lack of a clear association between the SAMe-TT2R2 score and anticoagulant selection may be attributed to the relative efficacy and safety profiles between NOACs and VKAs as well as to the absence of trial evidence that an SAMe-TT2R2-guided strategy for the selection of the type of anticoagulation in NVAF patients has an impact on clinical outcomes of efficacy and safety. The latter hypothesis is currently being tested in a randomized controlled trial. Clinical trial registration: URL: https://www.clinicaltrials.gov//Unique identifier: NCT01937377, NCT01468701, and NCT01671007.
Published: 2021
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18. Simulacion de la inundacion costera en la zona del Malecon Tradicional, huracan Wilma 2005

Author: Córdova de Horta, Daniela and Córdova López, Luis F.
Published: 2021

19. Simulación numérica de la red de drenaje pluvial de la cuenca Gancedo. La Habana

Author: Patricia Ruth de Horta Brito and Luis Manuel Pino Plans
Subjects: Hydraulic engineering, TC1-978, Environmental engineering, TA170-171
Abstract: Las inundaciones ocasionadas por lluvias son una amenaza continua que afecta a muchas zonas urbanas en todo el mundo, la cuenca Gancedo, ubicada en la zona central de La Habana, comprende los municipios de Habana Vieja, Diez de Octubre y Cerro, y presenta este problema con relativa frecuencia. A partir de la situación existente en la cuenca se realiza el estudio del funcionamiento hidráulico de las redes mediante el uso del software de modelación matemática EPA-SWMM. Se simula para tres variantes de lluvia, resultando 9 áreas de inundación, esto evidencia el mal estado de la red de drenaje pluvial de la cuenca, se presentan varias soluciones ingenieras para lograr su adecuado funcionamiento.
Published: 2021

20. Simulación numérica del drenaje pluvial de la CUJAE. Soluciones propuestas.

Author: Patricia Ruth de Horta Brito and Luis Fermín Córdova López
Subjects: Hydraulic engineering, TC1-978, Environmental engineering, TA170-171
Abstract: La Universidad Tecnológica de La Habana José Antonio Echeverría (CUJAE) presenta serios problemas de inundaciones causadas por lluvias, afectando con relativa frecuencia tanto la zona docente como la residencia estudiantil (beca). Debido a estos problemas se presenta un estudio del comportamiento hidráulico de la residencia estudiantil mediante el uso de modelos numéricos. La simulación de ambas redes dio paso a la propuesta de varias soluciones, luego de haber sido analizados los resultados para así minimizar los problemas existentes en las zonas críticas.
Published: 2021

21. Multi-frequency study of supernova remnants in the Large Magellanic Cloud. Confirmation of the supernova remnant status of DEM L205

Author: Maggi, P., Haberl, F., Bozzetto, L. M., Filipović, M. D., Points, S. D., Chu, Y. -H., Sasaki, M., Pietsch, W., Gruendl, R. A., Dickel, J., Smith, R. C., Sturm, R., Crawford, E. J., and De Horta, A. Y.
Subjects: Astrophysics - High Energy Astrophysical Phenomena, Astrophysics - Galaxy Astrophysics
Abstract: We present new X-ray and radio data of the LMC SNR candidate DEM L205, obtained by XMM-Newton and ATCA, along with archival optical and infrared observations. We use data at various wavelengths to study this object and its complex neighbourhood, in particular in the context of the star formation activity, past and present, around the source. We analyse the X-ray spectrum to derive some remnant's properties, such as age and explosion energy. Supernova remnant features are detected at all observed wavelengths: soft and extended X-ray emission is observed, arising from a thermal plasma with a temperature kT between 0.2 keV and 0.3 keV. Optical line emission is characterised by an enhanced [SII]/Halpha ratio and a shell-like morphology, correlating with the X-ray emission. The source is not or only tentatively detected at near-infrared wavelengths (< 10 microns), but there is a detection of arc-like emission at mid and far-infrared wavelengths (24 and 70 micron) that can be unambiguously associated with the remnant. We suggest that thermal emission from dust heated by stellar radiation and shock waves is the main contributor to the infrared emission. Finally, an extended and faint non-thermal radio emission correlates with the remnant at other wavelengths and we find a radio spectral index between -0.7 and -0.9, within the range for SNRs. The size of the remnant is ~79x64 pc and we estimate a dynamical age of about 35000 years. We definitely confirm DEM L205 as a new SNR. This object ranks amongst the largest remnants known in the LMC. The numerous massive stars and the recent outburst in star formation around the source strongly suggest that a core-collapse supernova is the progenitor of this remnant. (abridged), Comment: 11 pages, 6 figures, accepted for publication in A&A
Published: 2012
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22. Radio Planetary Nebulae in the Magellanic Clouds

Author: Filipović, M. D., Cohen, M., Reid, W. A., Payne, J. L., Parker, Q. A., Crawford, E. J., Bojičić, I. S., De Horta, A. Y., Hughes, A., Dickel, J., and Stootman, F.
Subjects: Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: We report the extragalactic radio-continuum detection of 15 planetary nebulae (PNe) in the Magellanic Clouds (MCs) from recent Australia Telescope Compact Array+Parkes mosaic surveys. These detections were supplemented by new and high resolution radio, optical and IR observations which helped to resolve the true nature of the objects. Four of the PNe are located in the Small Magellanic Cloud (SMC) and 11 are located in the Large Magellanic Cloud (LMC). Based on Galactic PNe the expected radio flux densities at the distance of the LMC/SMC are up to ~2.5 mJy and ~2.0 mJy at 1.4 GHz, respectively. We find that one of our new radio PNe in the SMC has a flux density of 5.1 mJy at 1.4 GHz, several times higher than expected. We suggest that the most luminous radio PN in the SMC (N S68) may represent the upper limit to radio peak luminosity because it is ~3 times more luminous than NGC 7027, the most luminous known Galactic PN. We note that the optical diameters of these 15 MCs PNe vary from very small (~0.08 pc or 0.32"; SMP L47) to very large (~1 pc or 4"; SMP L83). Their flux densities peak at different frequencies, suggesting that they may be in different stages of evolution. We briefly discuss mechanisms that may explain their unusually high radio-continuum flux densities. We argue that these detections may help solve the "missing mass problem" in PNe whose central stars were originally 1-8 Msun. We explore the possible link between ionised halos ejected by the central stars in their late evolution and extended radio emission. Because of their higher than expected flux densities we tentatively call this PNe (sub)sample - "Super PNe"., Comment: 10 pages, 6 figures, 1 table accepted by mnras
Published: 2009
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23. Rapid polarization variations in the O4 supergiant ζ Puppis.

Author: Bailey, Jeremy, Howarth, Ian D, Cotton, Daniel V, Kedziora-Chudczer, Lucyna, De Horta, Ain, Martell, Sarah L, Eldridge, Colin, and Luckas, Paul
Subjects: LIGHT curves, STELLAR winds, PHOTOMETRY, SUPERGIANT stars
Abstract: We present time-series linear-polarization observations of the bright O4 supergiant ζ Puppis. The star is found to show polarization variation on time-scales of around an hour and longer. Many of the observations were obtained contemporaneously with Transiting Exoplanet Survey Satellite (TESS) photometry. We find that the polarization varies on similar time-scales to those seen in the TESS light curve. The previously reported 1.78-d photometric periodicity is seen in both the TESS and polarization data. The amplitude ratio of photometry to polarization is ∼9 for the periodic component and the polarization variation is oriented along position angle ∼70°–160°. Higher frequency stochastic variability is also seen in both data sets with an amplitude ratio of ∼19 and no preferred direction. We model the polarization expected for a rotating star with bright photospheric spots and find that models that fit the photometric variation produce too little polarization variation to explain the observations. We suggest that the variable polarization is more likely the result of scattering from the wind, with corotating interaction regions producing the periodic variation and a clumpy outflow producing the stochastic component. The Hα emission line strength was seen to increase by 10 per cent in 2021 with subsequent observations showing a return to the pre-2018 level. [ABSTRACT FROM AUTHOR]
Published: 2024
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24. Simulación de la inundación costera en la zona del Malecón Tradicional, huracán Wilma 2005

Author: Daniela Córdova de Horta and Luis Fermín Córdova López
Subjects: huracán, inundaciones costeras, modelo iber, oleaje, Hydraulic engineering, TC1-978, Environmental engineering, TA170-171
Abstract: El 23 de octubre de 2005 el Huracán Wilma se alejaba de Cuba, a pesar de estar a más de 200 km en el Golfo de México dejó sus huellas en La Habana. La necesidad de proteger el Malecón habanero de los embates del mar conduce al estudio del comportamiento de las inundaciones costeras en el tramo del Malecón tradicional. En este trabajo se presentan las ecuaciones para el cálculo del rebase promedio. Se definen las características del oleaje mediante el establecimiento de un tren de modelos numéricos que permiten obtener los hidrogramas para alimentar el modelo hidrodinámico Iber, y se realiza la simulación de la inundación en la zona de estudio, lo que permite definir los puntos de mayor calado en la zona estudiada.
Published: 2021

25. Polarized reflected light from the Spica binary system

Author: Bailey, Jeremy, Cotton, Daniel V., Kedziora-Chudczer, Lucyna, De Horta, Ain, and Maybour, Darren
Published: 2019
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26. Effects of metallicity on the instability mass ratio of low-mass contact binary systems.

Author: Wadhwa, Surjit S, Landin, Natália R, Kostić, Petar, Vince, Oliver, Arbutina, Bojan, De Horta, Ain Y, Filipović, Miroslav D, Tothill, Nicholas F H, Petrović, Jelena, and Djurašević, Gojko
Subjects: MERGERS & acquisitions, ECLIPSING binaries, DEPENDENT variables
Abstract: The orbital stability of contact binary systems has been receiving considerable attention recently. Theoretical studies indicate that merger is likely to occur at very low-mass ratios, but the actual mass ratio at which merger may take place is likely to be variable and dependent on the mass of the primary. We consider the effects of metal content on the orbital stability of contact binary systems by modelling the gyration radius of a rotating and tidally distorted primary component at various values of |$\rm [Fe/H]$| in the range −1.25 to +0.5. We determine the instability mass ratio range for contact binary systems with a low-mass primary 0.6 M⊙ ≤ M 1 ≤ 1.4 M⊙ at various metallicity levels and show that systems with low metallicity have an instability mass ratio lower than those with higher metal content and therefore are likely to be more stable. We illustrate the effect through light-curve analysis of two otherwise very similar contact binary systems, except for different metallicity. While both would be considered unstable if metallicity was not taken into consideration, only one remains in that category after appropriate adjustments based on metallicity have been made. [ABSTRACT FROM AUTHOR]
Published: 2024
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27. Photometric and Spectroscopic Study of Two Low Mass Ratio Contact Binary Systems: CRTS J225828.7-121122 and CRTSJ030053.5+230139.

Author: Wadhwa, Surjit S., Petrović, Jelena, Tothill, Nick F. H., De Horta, Ain Y., Filipović, Miroslav D., and Djurašević, Gojko
Published: 2023
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28. A Study of Twelve Potential Merger Candidate Contact Binary Systems.

Author: Wadhwa, Surjit S., Arbutina, Bojan, Tothill, Nick F. H., Filipović, Miroslav D., De Horta, Ain Y., Petrović, Jelena, and Djurašević, Gojko
Subjects: BINARY stars
Abstract: Photometric observations and analysis of twelve previously poorly studied contact binary systems is presented. All show total eclipses and have extremely low mass ratios ranging from 0.072 to 0.15. Also, all show characteristics of orbital instability with mass ratios within the theoretical orbital instability range. Although none demonstrate a significant O'Connell effect at least nine of the systems have other indicators of increased chromospheric and magnetic activity. [ABSTRACT FROM AUTHOR]
Published: 2023
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29. PICSARR: high-precision polarimetry using CMOS image sensors.

Author: Bailey, Jeremy, Cotton, Daniel V, De Horta, Ain, Kedziora-Chudczer, Lucyna, and Shastri, Om
Subjects: CMOS image sensors, POLARIMETRY, SCIENTIFIC apparatus & instruments, POLARISCOPE, QUANTUM efficiency, IMAGE converters, MEASURING instruments
Abstract: We have built and tested a compact, low-cost, but very high performance astronomical polarimeter based on a continuously rotating half-wave plate and a high-speed imaging detector. The polarimeter is suitable for small telescopes up to ∼1 m in aperture. The optical system provides very high transmission over a wide wavelength range from the atmospheric ultraviolet cut-off to ∼1000 nm. The high quantum efficiency, low noise, and high speed of the detectors enable bright stars to be observed with high precision as well as polarization imaging of extended sources. We have measured the performance of the instrument on 20 and 60 cm aperture telescopes. We show some examples of the type of science possible with this instrument. The polarimeter is particularly suited to studies of the wavelength dependence and time variability of the polarization of stars and planets. [ABSTRACT FROM AUTHOR]
Published: 2023
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30. Radio-continuum study of the nearby Sculptor group Galaxies. Part 2: NGC 55 at λ=20, 13, 6 and 3 cm

Author: O’Brien, Andrew N., Filipović, Miroslav D., Crawford, Evan J., Tothill, Nicholas F. H., Collier, Jordan D., De Horta, Ain Y., Wong, Graeme F., Drašković, Danica, Payne, Jeff L., Pannuti, Thomas G., Napier, Jared P., Griffith, Stephen A., Staggs, Wayne D., and Kotuš, Srdjan
Published: 2013
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31. Radio-continuum study of the Nearby sculptor group galaxies. Part 1: NGC 300 at λ=20 cm

Author: Galvin, Timothy J., Filipović, Miroslav D., Crawford, Evan J., Wong, Graeme, Payne, Jeff L., De Horta, Ain, White, Graeme L., Tothill, Nick, Drašković, Danica, Pannuti, Thomas G., Grimes, Caleb K., Cahall, Benjamin J., Millar, William C., and Laine, Seppo
Published: 2012
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32. ZZ Piscis Austrinus (ZZ PsA): a bright red nova progenitor and the instability mass ratio of contact binary stars.

Author: Wadhwa, Surjit S, De Horta, Ain, Filipović, Miroslav D, Tothill, N F H, Arbutina, Bojan, Petrović, Jelena, and Djurašević, Gojko
Subjects: *BINARY stars, *ECLIPSING binaries
Abstract: ZZ Piscis Austrinus (ZZ PsA) is a neglected bright southern contact binary system with maximum V magnitude of 9.26. We present the first multiband photometric analysis and find the system to be in deep contact (>95 per cent) with an extremely low mass ratio of 0.078. The primary has a mass of 1.213 M⊙ in keeping with its reported spectral class of F6. In order to determine if ZZ PsA is a merger candidate, we outline the current status regarding the instability mass ratio and develop new relationship linking the mass of the primary to the instability mass ratio of the system and the degree of contact. We find that ZZ PsA along with two other examples from the literature to be merger candidates while an additional three require further observations to be confirmed as potential merger candidates. [ABSTRACT FROM AUTHOR]
Published: 2021
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33. Radio observations of supernova remnant G1.9+0.3.

Author: Luken, Kieran J, Filipović, Miroslav D, Maxted, Nigel I, Kothes, Roland, Norris, Ray P, Allison, James R, Blackwell, Rebecca, Braiding, Catherine, Brose, Robert, Burton, Michael, De Horta, Ain Y, Galvin, Tim J, Harvey-Smith, Lisa, Hurley-Walker, Natasha, Leahy, Denis, Ralph, Nicholas O, Roper, Quentin, Rowell, Gavin, Sushch, Iurii, and Urošević, Dejan
Subjects: SUPERNOVA remnants, HOLOCENE Epoch, RADIOS, ACTINIC flux
Abstract: We present 1–10 GHz radio continuum flux density, spectral index, polarization, and rotation measure (RM) images of the youngest known Galactic supernova remnant (SNR) G1.9+0.3, using observations from the Australia Telescope Compact Array. We have conducted an expansion study spanning eight epochs between 1984 and 2017, yielding results consistent with previous expansion studies of G1.9+0.3. We find a mean radio continuum expansion rate of (0.78 ± 0.09) per cent yr−1 (or ∼8900 km s−1 at an assumed distance of 8.5 kpc), although the expansion rate varies across the SNR perimetre. In the case of the most recent epoch between 2016 and 2017, we observe faster-than-expected expansion of the northern region. We find a global spectral index for G1.9+0.3 of −0.81 ± 0.02 (76 MHz–10 GHz). Towards the northern region, however, the radio spectrum is observed to steepen significantly (∼−1). Towards the two so-called (east and west) 'ears' of G1.9+0.3, we find very different RM values of 400–600 and 100–200 rad m2, respectively. The fractional polarization of the radio continuum emission reaches (19 ± 2) per cent, consistent with other, slightly older, SNRs such as Cas A. [ABSTRACT FROM AUTHOR]
Published: 2020
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34. The first observed stellar occultations by the irregular satellite Phoebe (Saturn IX) and improved rotational period.

Author: Gomes-Júnior, A R, Assafin, M, Braga-Ribas, F, Benedetti-Rossi, G, Morgado, B E, Camargo, J I B, Vieira-Martins, R, Desmars, J, Sicardy, B, Barry, T, Campbell-White, J, Fernández-Lajús, E, Giles, D, Hanna, W, Hayamizu, T, Hirose, T, De Horta, A, Horvat, R, Hosoi, K, and Jehin, E
Subjects: OCCULTATIONS (Astronomy), NATURAL satellites, LIGHT curves, LONGITUDE, ROTATIONAL motion
Abstract: We report six stellar occultations by Phoebe (Saturn IX), an irregular satellite of Saturn, obtained between mid-2017 and mid-2019. The 2017 July 6 event was the first stellar occultation by an irregular satellite ever observed. The occultation chords were compared to a 3D shape model of the satellite obtained from Cassini observations. The rotation period available in the literature led to a sub-observer point at the moment of the observed occultations where the chords could not fit the 3D model. A procedure was developed to identify the correct sub-observer longitude. It allowed us to obtain the rotation period with improved precision compared to the currently known value from literature. We show that the difference between the observed and the predicted sub-observer longitude suggests two possible solutions for the rotation period. By comparing these values with recently observed rotational light curves and single-chord stellar occultations, we can identify the best solution for Phoebe's rotational period as 9.27365 ± 0.00002 h. From the stellar occultations, we also obtained six geocentric astrometric positions in the ICRS as realized by the Gaia DR2 with uncertainties at the 1-mas level. [ABSTRACT FROM AUTHOR]
Published: 2020
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35. Tobacco and end stage renal disease: a multicenter, cross-sectional study in Argentinian Northern Patagonia.

Author: Alba, Maria M., Citarelli, Alicia N., Menni, Fernanda, Agricola, Maria, Braicovich, Alejandra, De Horta, Eduardo, De Rosa, Fernando, Filanino, Graciela, Gaggiotti, Raul, Junqueras, Nelson, Martinelli, Sandra, Milan, Adriana, Morales, Mabel E., Setti, Silvia, and Villalba, Daniel O.
Abstract: Copyright of Tobacco Induced Diseases is the property of EU European Publishing and its content may not be copied or emailed to multiple sites or posted to a listserv without the copyright holder's express written permission. However, users may print, download, or email articles for individual use. This abstract may be abridged. No warranty is given about the accuracy of the copy. Users should refer to the original published version of the material for the full abstract. (Copyright applies to all Abstracts.)
Published: 2015
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36. RADIO-CONTINUUM EMISSION FROM THE YOUNG GALACTIC SUPERNOVA REMNANT G1.9+0.3.

Author: De Horta, A. Y., Filipović, M. D., Crawford, E. J., Stootman, F. H., Pannuti, T. G., Bozzetto, L. M., Collier, J. D., Sommer, E. R., and Kosakowski, A. R.
Subjects: *GALACTIC dynamics, *SOLAR radio emission, *SUPERNOVA remnants, *INTERSTELLAR medium, *VERY large array telescopes
Abstract: We present an analysis of a new Australia Telescope Compact Array (ATCA) radio-continuum observation of supernova remnant (SNR) G1.9+0.3, which at an age of ~181±25 years is the youngest known in the Galaxy. We analysed all available radio-continuum observations at 6-cm from the ATCA and Very Large Array. Using this data we estimate an expansion rate for G1.9+0.3 of 0.563%±0.078% per year between 1984 and 2009. We note that in the 1980's G1.9+0.3 expanded somewhat slower (0.484% per year) than more recently (0.641% per year). We estimate that the average spectral index between 20-cm and 6-cm, across the entire SNR is α=0.72±0.26 which is typical for younger SNRs. At 6-cm, we detect an average of 6% fractionally polarised radio emission with a peak of 17%±3%. The polarised emission follows the contours of the strongest of X-ray emission. Using the new equipartition formula we estimate a magnetic field strength of B≈273 µG, which to date, is one of the highest magnetic field strength found for any SNR and consistent with G1.9+0.3 being a very young remnant. [ABSTRACT FROM AUTHOR]
Published: 2014
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37. THE PUZZLING JET AND PULSAR WIND NEBULA OF IGR J11014-6103.

Author: PAVAN, LUCIA, BORDAS, POL, PÜHLHOFER, GERD, FILIPOVIC, MIROSLAV D., DE HORTA, AIN, O' BRIEN, ANDREW, CRAWFORD, EVAN, BALBO, MATTEO, WALTER, ROLAND, BOZZO, ENRICO, FERRIGNO, CARLO, and STELLA, LUIGI
Published: 2014
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38. The long helical jet of the Lighthouse nebula, IGR J11014-6103.

Author: Pavan, L., Bordas, P., Pühlhofer, G., Filipović, M. D., De Horta, A., O' Brien, A., Balbo, M., Walter, R., Bozzo, E., Ferrigno, C., Crawford, E., and Stella, L.
Subjects: X-ray binaries, NEBULAE, NEUTRON stars, SUPERNOVAE, JETS (Nuclear physics), BIPOLAR outflows (Astrophysics), SUPERNOVA remnants, CIRCUMSTELLAR matter
Abstract: Context. Jets from rotation-powered pulsars so far have only been observed in systems moving subsonically through their ambient medium and/or embedded in their progenitor supernova remnant (SNR). Supersonic runaway pulsars are also expected to produce jets, but they have not been confirmed to so far. Aims. We investigated the nature of the jet-like structure associated with the INTEGRAL source IGR J11014-6103 (the "Lighthouse nebula"). The source is a neutron star escaping its parent SNR MSH 11-61A supersonically at a velocity exceeding 1000 km s-1. Methods. We observed the Lighthouse nebula and its jet-like X-ray structure through dedicated high spatial resolution observations in X-rays (with Chandra) and in the radio band (with ATCA). Results. Our results show that the feature is a true pulsar's jet. It extends highly collimated over ≳11pc, displays a clear precession like modulation, and propagates nearly perpendicular to the system direction of motion, implying that the neutron star's spin axis in IGR J11014-6103 is almost perpendicular to the direction of the kick received during the supernova explosion. Conclusions. Our findings suggest that jets are common to rotation-powered pulsars, and demonstrate that supernovae can impart high kick velocities to misaligned spinning neutron stars, possibly through distinct, exotic, core-collapse mechanisms. [ABSTRACT FROM AUTHOR]
Published: 2014
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39. Active galactic nuclei behind the SMC selected from radio and X-ray surveys.

Author: Sturm, R., Drašković, D., Filipović, M. D., Haberl, F., Collier, J., Crawford, E. J., Ehle, M., De Horta, A., Pietsch, W., Tothill, N. F.H., and Wong, G.
Subjects: ACTIVE galactic nuclei, SMALL magellanic cloud, RADIO astronomy, X-ray astronomy, GALACTIC X-ray sources, X-ray emission spectroscopy
Abstract: Context. The XMM-Newton survey of the Small Magellanic Cloud (SMC) revealed 3053 X-ray sources with the majority expected to be active galactic nuclei (AGN) behind the SMC. However, the high stellar density in this field often does not allow assigning unique optical counterparts and hinders source classification. On the other hand, the association of X-ray point sources with radio emission can be used to select background AGN with high confidence, and to constrain other object classes like pulsar wind nebula. Aims. To classify X-ray and radio sources, we use clear correlations of X-ray sources found in the XMM-Newton survey with radiocontinuum sources detected with ATCA and MOST. Methods. Deep radio-continuum images were searched for correlations with X-ray sources of the XMM-Newton SMC-survey pointsource catalogue as well as galaxy clusters seen with extended X-ray emission. Results. Eighty eight discrete radio sources were found in common with the X-ray point-source catalogue in addition to six correlations with extended X-ray sources. One source is identified as a Galactic star and eight as galaxies. Eight radio sources likely originate in AGN that are associated with clusters of galaxies seen in X-rays. One source is a pulsar wind nebula candidate. We obtain 43 new candidates for background sources located behind the SMC. A total of 24 X-ray sources show jet-like radio structures. [ABSTRACT FROM AUTHOR]
Published: 2013
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40. Multi-frequency observations of SNR J0453-6829 in the LMC. A composite supernova remnant with a pulsar wind nebula.

Author: Haberl, F., Filipović, M. D., Bozzetto, L. M., Crawford, E. J., Points, S. D., Pietsch, W., De Horta, A. Y., Tothill, N., Payne, J. L., and Sasaki, M.
Subjects: NEBULAE, SUPERNOVA remnants, X-ray diffraction, PULSAR detection, SPECTRUM analysis, MAGELLANIC clouds
Abstract: Context. The Large Magellanic Cloud (LMC) is rich in supernova remnants (SNRs), which can be investigated in detail with radio, optical, and X-ray observations. SNR-J0453-6829 is an X-ray and radio-bright remnant in the LMC, within which previous studies revealed the presence of a pulsar wind nebula (PWN), making it one of the most interesting SNRs in the Local Group of galaxies. Aims. We study the emission of SNR-J0453-6829 to improve our understanding of its morphology, spectrum, and thus the emission mechanisms in the shell and the PWN of the remnant. Methods. We obtained new radio data with the Australia Telescope Compact Array and analysed archival XMM-Newton observations of SNR-J0453-6829. We studied the morphology of SNR-J0453-6829 from radio, optical, and X-ray images and investigated the energy spectra in the different parts of the remnant. Results. Our radio results confirm that this LMC SNR hosts a typical PWN. The prominent central core of the PWN exhibits a radio spectral index αCore of −0.04 ± 0.04, while in the rest of the SNR shell the spectral slope is somewhat steeper with αShell = −0.43- ± -0.01. We detect regions with a mean polarisation of P ≅ (12 ± 4)% at 6 cm and (9 ± 2)% at 3 cm. The full remnant is of roughly circular shape with dimensions of (31 ± 1) pc- × (29 ± 1) pc. The spectral analysis of the XMM-Newton EPIC and RGS spectra allowed us to derive physical parameters for the SNR. Somewhat depending on the spectral model, we obtain for the remnant a shock temperature of around 0.2 keV and estimate the dynamical age to 12-000-15-000 years. Using a Sedov model we further derive an electron density in the X-ray emitting material of 1.56-cm-3, typical for LMC remnants, a large swept-up mass of 830 M⊙, and an explosion energy of 7.6 × 1050 erg. These parameters indicate a well evolved SNR with an X-ray spectrum dominated by emission from the swept-up material. [ABSTRACT FROM AUTHOR]
Published: 2012
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41. Multi-frequency observations of SNRJ0453-6829 in the LMC A composite supernova remnant with a pulsar wind nebula.

Author: Haberl, F., Filipović, M.D., Bozzetto, L.M., Crawford, E.J., Points, S. D., Pietsch, W., De Horta, A.Y., Tothill, N., Payne, J. L., and Sasaki, M.
Subjects: NEBULAE, X-rays, TELESCOPES, SPECTRUM analysis
Abstract: Context. The Large Magellanic Cloud (LMC) is rich in supernova remnants (SNRs), which can be investigated in detail with radio, optical, and X-ray observations. SNRJ0453-6829 is an X-ray and radio-bright remnant in the LMC, within which previous studies revealed the presence of a pulsar wind nebula (PWN), making it one of the most interesting SNRs in the Local Group of galaxies. Aims. We study the emission of SNRJ0453-6829 to improve our understanding of its morphology, spectrum, and thus the emission mechanisms in the shell and the PWN of the remnant. Methods. We obtained new radio data with the Australia Telescope Compact Array and analysed archival XMM-Newton observations of SNRJ0453-6829. We studied the morphology of SNRJ0453-6829 from radio, optical, and X-ray images and investigated the energy spectra in the different parts of the remnant. Results. Our radio results confirm that this LMC SNR hosts a typical PWN. The prominent central core of the PWN exhibits a radio spectral index αCore of -0.04 ± 0.04, while in the rest of the SNR shell the spectral slope is somewhat steeper with αShell = -0.43 ± 0.01. We detect regions with a mean polarisation of P (12 ± 4)% at 6 cm and (9 ± 2)% at 3 cm. The full remnant is of roughly circular shape with dimensions of (31±1) pc × (29±1) pc. The spectral analysis of the XMM-Newton EPIC and RGS spectra allowed us to derive physical parameters for the SNR. Somewhat depending on the spectral model, we obtain for the remnant a shock temperature of around 0.2 keV and estimate the dynamical age to 12 000-15 000 years. Using a Sedov model we further derive an electron density in the X-ray emitting material of 1.56 cm-3, typical for LMC remnants, a large swept-up mass of 830 M☉, and an explosion energy of 7.6 × 1050 erg. These parameters indicate a well evolved SNR with an X-ray spectrum dominated by emission from the swept-up material. [ABSTRACT FROM AUTHOR]
Published: 2012
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42. Multifrequency study of the Large Magellanic Cloud supernova remnant J0529−6653 near pulsar B0529-66.

Author: Bozzetto, L. M., Filipović, M. D., Crawford, E. J., Haberl, F., Sasaki, M., Urošević, D., Pietsch, W., Payne, J. L., De Horta, A. Y., Stupar, M., Tothill, N. F. H., Dickel, J., Chu, Y.-H., and Gruendl, R.
Subjects: SUPERNOVA remnants, TELESCOPES, RADIO frequency, X-rays, ASTROPHYSICS, DATA analysis, MAGELLANIC clouds
Abstract: ABSTRACT We report the Australia Telescope Compact Array (ATCA) and ROSAT detection of supernova remnant (SNR) J0529−6653 in the Large Magellanic Cloud (LMC) which is positioned in the projected vicinity of the known radio pulsar PSR B0529−66. In the radio continuum frequencies, this LMC object follows a typical SNR structure of a shell morphology with brightened regions in the south-west. It exhibits an almost circular shape of D= 33 × 31 pc (1-pc uncertainty in each direction) and radio spectral index of α=−0.68 ± 0.03 - typical for mid-age SNRs. We also report detection of polarized regions with a peak value of ∼17 ± 7 per cent at 6 cm. An investigation of ROSAT images produced from merged Position Sensitive Proportional Counter (PSPC) data reveals the presence of extended X-ray emission coincident with the radio emission of the SNR. In X-rays, the brightest part is in the north-east. We discuss various scenarios with regard to the SNR-pulsar association with emphasis on the large age difference, lack of a pulsar trail and no prominent point-like radio or X-ray source. [ABSTRACT FROM AUTHOR]
Published: 2012
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43. Electrocardiographic Identification of Mid-Septal Accessory Pathways in Close Proximity to the Atrioventricular Conduction System.

Author: Lorga, Adalberto, Sosa, Eduardo, Scanavacca, Mauricio, d'Avila, André, Kuniyoshi, Ricardo, de Horta, José, Fenelon, Guilherme, and Brugada, Pedro
Subjects: ELECTROCARDIOGRAPHY, HEART septum, ATRIOVENTRICULAR node, CATHETER ablation, ELECTROSURGERY, PATIENTS
Abstract: System. In order to identify ECG characteristics of overt mid-septal accessory pathways (APs) predictive of dose proximity to the AV conduction system we analyzed data from patients who underwent successful RF catheter ablation of a mid-septa! AP. Mean patient age was 31 ± 16 years, and 13 were male. The 40° right anterior oblique view was used to divide the mid-septal area into 3 zones: 1 (anterior portion); 2 (intermediate); and 3 (posterior portion). The 12-lead ECG was analyzed with regard to delta wave polarity and R/S transition in the precordial leads. The findings from patients ablated at zone 3 were compared to those at zones 1 and 2. All patients had a positive delta wave in the leads I, II, aVL, and negative delta wave in the leads III and aVR. The R/S transition occurred in lead V2 in 80% of patients. The delta wave in lead aVF was the only ECG characteristic that correlated with the AP ablation zone. Six of 8 patients ablated at zone 3 had a negative delta wave in lead aVF while 6 out of 7 patients ablated at zone 1 or 2 had a positive or isoelectric delta wave in lead aVF (P = 0.03). A positive or isoelectric delta wave in lead aVF identifies mid-septal AP in close proximity to the AV conduction system. [ABSTRACT FROM AUTHOR]
Published: 1996
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44. Radio planetary nebulae in the Magellanic Clouds.

Author: Crawford, Evan J., Filipović, Miroslav D., Bojičić, Ivan S., Cohen, Martin, Payne, Jeff L., De Horta, Ain Y., and Reid, Warren
Abstract: We present preliminary results of our deep Australia Telescope Compact Array (ATCA) radio-continuum survey of the Magellanic Clouds Planetary Nebulae. [ABSTRACT FROM PUBLISHER]
Published: 2011
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45. NEW 6 AND 3-cm RADIO-CONTINUUM MAPS OF THE SMALL MAGELLANIC CLOUD. PART I - THE MAPS.

Author: Crawford, E. J., Filipović, M. D., De Horta, A. Y., Wong, G. F., Tothill, N. F. H., Drašković, D., Collier, J. D., and Galvin, T. J.
Subjects: *RADIO sources (Astronomy), *DECONVOLUTION (Mathematics), *GALAXIES, *RADIO astronomy, *MAPS, *OPTICAL resolution, *MAGELLANIC clouds
Abstract: We present new 6 and 3-cm radio-continuum maps of the Small Magellanic Cloud (SMC), created with the "peeling" technique and a joint deconvolution. The maps have resolutions of 30" and 20" and r.m.s., noise of 0.7 and 0.8 mJy/beam at 6 and 3 cm, respectively. These maps will be used for future studies of the SMC's radio source population and overall extended structure. [ABSTRACT FROM AUTHOR]
Published: 2011
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46. New 20-cm radio-continuum study of the small Magellanic cloud - part III: Compact Hii regions

Author: Wong G.F., Filipović M.D., Crawford E.J., Tothill N.F.H., de Horta A.Y., and Galvin T.J.
Subjects: Magellanic Clouds, radio continuum: ISM, catalogs, Astronomy, QB1-991
Abstract: We present and discuss a new catalogue of 48 compact Hii regions in the Small Magellanic Cloud (SMC) and a newly created deep 1420 MHz (λ=20 cm) radio-continuum image of the N19 region located in the southwestern part of the SMC. The new images were created by merging 1420 MHz radiocontinuum archival data from the Australian Telescope Compact Array. The majority of these detected radio compact Hii regions have rather flat spectral indices which indicates, as expected, that the dominant emission mechanism is of thermal nature.
Published: 2012
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47. Multifrequency radio observations of SNR J0536-6735 (N 59B) with associated pulsar

Author: Bozzetto L.M., Filipović M.D., Crawford E.J., de Horta A.Y., and Stupar M.
Subjects: ISM: supernova remnants, Magellanic Clouds, radio continuum: ISM, ISM: individual objects: SNR J0536-6735, Astronomy, QB1-991
Abstract: We present a study of new Australian Telescope Compact Array (ATCA) observations of supernova remnant, SNR J0536-6735. This remnant appears to follow a shell morphology with a diameter of D=36x29 pc (with 1 pc uncertainty in each direction). There is an embedded HII region on the northern limb of the remnant which made various analysis and measurements (such as flux density, spectral index and polarisation) difficult. The radio-continuum emission followed the same structure as the optical emission, allowing for extent and flux density estimates at 20 cm. We estimate the surface brightness at 1 GHz of 2.55x10−21 Wm−2 Hz−1 sr−1 for the SNR. Also, we detect a distinctive radio-continuum point source which confirms the previous suggestion of this remnant being associated with pulsar wind nebula (PWN). The tail of this remnant is not seen in the radio-continuum images and is only seen in the optical and X-ray images.
Published: 2012
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48. 20cm VLA radio-continuum study of M31: Images and point source catalogues

Author: Galvin T.J., Filipović M.D., Crawford E.J., Tothill N.F.H., Wong G.F., and de Horta A.Y.
Subjects: techniques: image processing, radio continuum, catalogs, Astronomy, QB1-991
Abstract: We present a series of new high-sensitivity and high-resolution radio-continuum images of M31 at λ=20 cm (ν=1.4 GHz). These new images were produced by merging archived 20 cm radio-continuum observations from the Very Large Array (VLA) telescope. Images presented here are sensitive to rms=60 μJy and feature high angular resolution (
Published: 2012
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49. New 20-cm radio-continuum study of the small Magellanic cloud: Part I. Images

Author: Wong G.F., Filipović M.D., Crawford E.J., de Horta A., Galvin T., Drašković D., and Payne J.L.
Subjects: Magellanic Clouds, Radio Continuum: galaxies, Astronomy, QB1-991
Abstract: We present and discuss new high-sensitivity and resolution radiocontinuum images of the Small Magellanic Cloud (SMC) at λ=20 cm (ν=1.4 GHz). The new images were created by merging 20-cm radio-continuum archival data, from the Australian Telescope Compact Array and the Parkes radio-telescope. Our images span from ～10"to ～150" in resolution and sensitivity of r.m.s.≥0.5 mJy/beam. These images will be used in future studies of the SMC’s intrinsic sources and its overall extended structure.
Published: 2011
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50. New 20-cm radio-continuum study of the Small Magellanic Cloud, part II: Point sources

Author: Wong G.F., Filipović M.D., Crawford E.J., Tothill N.F.H., de Horta A.Y., Drašković D., Galvin T.J., Collier J.D., and Payne J.L.
Subjects: Magellanic Clouds, radio continuum: galaxies, catalogs, Astronomy, QB1-991
Abstract: We present a new catalogue of radio-continuum sources in the field of the Small Magellanic Cloud (SMC). This catalogue contains sources previously not found in 2370 MHz (λ=13 cm) with sources found at 1400 MHz (λ=20 cm) and 843 MHz (λ=36 cm). 45 sources have been detected at 13 cm, with 1560 sources at 20 cm created from new high sensitivity and resolution radio-continuum images of the SMC at 20 cm from paper I. We also created a 36 cm catalogue to which we listed 1689 radio-continuum sources.
Published: 2011
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