1,734 results on '"Gonçalves D"'
Search Results
52. Flash floods and landslides in the city of Recife, Northeast Brazil after heavy rain on May 25–28, 2022: Causes, impacts, and disaster preparedness
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Marengo, J.A., Alcantara, E., Cunha, A.P., Seluchi, M., Nobre, C.A., Dolif, G., Goncalves, D., Assis Dias, M., Cuartas, L.A., Bender, F., Ramos, A.M., Mantovani, J.R., Alvalá, R.C., and Moraes, O.L.
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- 2023
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53. Unifying interval maps and branching systems with applications to relative graph C*-algebras
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Correia Ramos, C., Gonçalves, D., Martins, Nuno, and Pinto, Paulo R.
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- 2023
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54. Initial experience with targeted axillary dissection after neoadjuvant therapy in breast cancer patients
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Pinto, C. S., Peleteiro, B., Pinto, C. A., Osório, F., Costa, S., Magalhães, A., Mora, H., Amaral, J., Gonçalves, D., and Fougo, J. L.
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- 2022
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55. The $R_\infty$--property for nilpotent quotients of Baumslag--Solitar groups
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Dekimpe, K. and Gonçalves, D. L.
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Mathematics - Group Theory ,Primary: 20E36, secondary: 20F14, 20F18 - Abstract
A group $G$ has the $R_{\infty}$--property if the number $R(\varphi)$ of twisted conjugacy classes is infinite for any automorphism $\varphi$ of $G$. For such a group $G$, the $R_{\infty}$--nilpotency index is the least integer $c$ such that $G/\gamma_{c+1}(G)$ still has the $R_\infty$--property. In this paper, we determine the $R_{\infty}$--nilpotency degree of all Baumslag--Solitar groups., Comment: 12 pg
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- 2018
56. Explicit solutions of certain orientable quadratic equations in free groups
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Gonçalves, D. L. and Nasybullov, T.
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Mathematics - Group Theory ,Mathematics - Geometric Topology - Abstract
For $g\geq1$ denote by $F_{2g}=\langle x_1, y_1,\dots,x_g,y_g\rangle$ the free group on $2g$ generators and by $B_g=[x_1,y_1]\dots[x_g,y_g]$. For $l,c\geq 1$ and elements $w_1,\dots,w_l\in F_{2g}$ we study orientable quadratic equations of the form $[u_1,v_1]\dots[u_h,v_h]=(B_g^{w_1})^c(B_g^{w_2})^c\dots(B_g^{w_l})^c$ with unknowns $u_1,v_1,\dots,u_h,v_h$ and provide explicit solutions for them for the minimal possible number $h$. In the particular case when $g=1$, $w_i=y_1^{i-1}$ for $i=1,\dots,l$ and $h$ the minimal number which satisfies $h \geq l(c-1)/2+1$ we provide two types of solutions depending on the image of the subgroup $H=\langle u_1,v_1,\dots,u_h,v_h\rangle$ generated by the solution under the natural homomorphism $p:F_2\to F_2/[F_2,F_2]$: the first solution, which is called a primitive solution, satisfies $p(H)=F_2/[F_2,F_2]$, the second solution satisfies $p(H) = \big\langle p(x_1),p(y_1^l)\big\rangle$. We also provide an explicit solution of the equation $[u_1,v_1]\dots[u_k, v_k] = \big(B_1\big)^{k+l} \big({B_1}^{y}\big)^{k-l}$ for $k>l\geq0$ in $F_2$, and prove that if $l\neq0$, then every solution of this equation is primitive. As a geometrical consequence, for every solution we obtain a map $f:S_h\to T$ from the orientable surface $S_h$ of genus $h$ to the torus $T=S_1$ which has the minimal number of roots among all maps from the homotopy class of $f$. Depending on the number $|p(F_2):p(H)|$ such maps have fundamentally different geometric properties: in some cases they satisfy the Wecken property and in other cases not.
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- 2018
57. The Borsuk-Ulam theorem for the Seifert manifolds having flat geometry
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Bauval, A., Gonçalves, D. L., and Hayat, C.
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Mathematics - Geometric Topology ,57M05 57M10 57M50 - Abstract
Let M be a Seifert manifold which belongs to the geometry Flat. In this work we determine all the free involutions {\tau} on M, and the Borsuk-Ulam indice of (M,{\tau}).
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- 2018
58. J-PLUS: measuring ${\rm H}\alpha$ emission line fluxes in the nearby universe
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Logroño-García, R., Vilella-Rojo, G., López-Sanjuan, C., Varela, J., Viironen, K., Muniesa, D. J., Cenarro, A. J., Cristóbal-Hornillos, D., Ederoclite, A., Marín-Franch, A., Moles, M., Ramió, H. Vázquez, Bonoli, S., Díaz-García, L. A., Orsi, A., Roman, I. San, Akras, S., Chies-Santos, A. L., Coelho, P. R. T., Daflon, S., Costa-Duarte, M. V., Dupke, R., Galbany, L., Delgado, R. M. González, Hernandez-Jimenez, J. A., de Oliveira, R. Lopes, de Oliveira, C. Mendes, Oteo, I., Gonçalves, D. R., Sánchez-Portal, M., Schmidtobreick, L., and Sodré Jr, L.
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Astrophysics - Astrophysics of Galaxies - Abstract
In the present paper we aim to validate a methodology designed to extract the Halpha emission line flux from J-PLUS photometric data. J-PLUS is a multi narrow-band filter survey carried out with the 2 deg2 field of view T80Cam camera, mounted on the JAST/T80 telescope in the OAJ, Teruel, Spain. The information of the twelve J-PLUS bands, including the J0660 narrow-band filter located at rest-frame Halpha, is used over 42 deg2 to extract de-reddened and [NII] decontaminated Halpha emission line fluxes of 46 star-forming regions with previous SDSS and/or CALIFA spectroscopic information. The agreement of the inferred J-PLUS photometric Halpha fluxes and those obtained with spectroscopic data is remarkable, with a median comparison ratio R = 1.05 +- 0.25. This demonstrates that it is possible to retrieve reliable Halpha emission line fluxes from J-PLUS photometric data. With an expected area of thousands of square degrees upon completion, the J-PLUS dataset will allow the study of several star formation science cases in the nearby universe, as the spatially resolved star formation rate of nearby galaxies at z < 0.015, and how it is influenced by the environment, morphology or nuclear activity. As an illustrative example, the close pair of interacting galaxies NGC3994 and NGC3995 is analyzed, finding an enhancement of the star formation rate not only in the center, but also in outer parts of the disk of NGC3994., Comment: 13 pages, 8 figures, 3 tables. Submitted to Astronomy and Astrophysics. Comments are welcome
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- 2018
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59. J-PLUS: The Javalambre Photometric Local Universe Survey
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Cenarro, A. J., Moles, M., Cristóbal-Hornillos, D., Marín-Franch, A., Ederoclite, A., Varela, J., López-Sanjuan, C., Hernández-Monteagudo, C., Angulo, R. E., Ramió, H. Vázquez, Viironen, K., Bonoli, S., Orsi, A. A., Hurier, G., Roman, I. San, Greisel, N., Vilella-Rojo, G., Díaz-García, L. A., Logroño-García, R., Gurung-López, S., Spinoso, D., Izquierdo-Villalba, D., Aguerri, J. A. L., Prieto, C. Allende, Bonatto, C., Carvano, J. M., Chies-Santos, A. L., Daflon, S., Dupke, R. A., Falcón-Barroso, J., Gonçalves, D. R., Jiménez-Teja, Y., Molino, A., Placco, V. M., Solano, E., Whitten, D. D., Abril, J., Antón, J. L., Bello, R., de Toledo, S. Bielsa, Castillo-Ramírez, J., Chueca, S., Civera, T., Díaz-Martín, M. C., Domínguez-Martínez, M., Garzarán-Calderaro, J., Hernández-Fuertes, J., Iglesias-Marzoa, R., Iñiguez, C., Ruiz, J. M. Jiménez, Kruuse, K., Lamadrid, J. L., Lasso-Cabrera, N., López-Alegre, G., López-Sainz, A., Maícas, N., Moreno-Signes, A., Muniesa, D. J., Rodríguez-Llano, S., Rueda-Teruel, F., Rueda-Teruel, S., Soriano-Laguía, I., Tilve, V., Valdivielso, L., Yanes-Díaz, A., Alcaniz, J. S., de Oliveira, C. Mendes, Sodré, L., Coelho, P., de Oliveira, R. Lopes, Tamm, A., Xavier, H. S., Abramo, L. R., Akras, S., Alfaro, E. J., Alvarez-Candal, A., Ascaso, B., Beasley, M. A., Beers, T. C., Fernandes, M. Borges, Bruzual, G. R., Buzzo, M. L., Carrasco, J. M., Cepa, J., Cortesi, A., Costa-Duarte, M. V., De Prá, M., Favole, G., Galarza, A., Galbany, L., Garcia, K., Delgado, R. M. González, González-Serrano, J. I., Gutiérrez-Soto, L. A., Hernandez-Jimenez, J. A., Kanaan, A., Kuncarayakti, H., Landim, R. C. G., Laur, J., Licandro, J., Neto, G. B. Lima, Lyman, J. D., Apellániz, J. Maíz, Miralda-Escudé, J., Morate, D., Nogueira-Cavalcante, J. P., Novais, P. M., Oncins, M., Oteo, I., Overzier, R. A., Pereira, C. B., Rebassa-Mansergas, A., Reis, R. R. R., Roig, F., Sako, M., Salvador-Rusiñol, N., Sampedro, L., Sánchez-Blázquez, P., Santos, W. A., Schmidtobreick, L., Siffert, B. B., and Telles, E.
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Astrophysics - Astrophysics of Galaxies ,Astrophysics - Cosmology and Nongalactic Astrophysics - Abstract
J-PLUS is an ongoing 12-band photometric optical survey, observing thousands of square degrees of the Northern hemisphere from the dedicated JAST/T80 telescope at the Observatorio Astrof\'isico de Javalambre. T80Cam is a 2 sq.deg field-of-view camera mounted on this 83cm-diameter telescope, and is equipped with a unique system of filters spanning the entire optical range. This filter system is a combination of broad, medium and narrow-band filters, optimally designed to extract the rest-frame spectral features (the 3700-4000\AA\ Balmer break region, H$\delta$, Ca H+K, the G-band, the Mgb and Ca triplets) that are key to both characterize stellar types and to deliver a low-resolution photo-spectrum for each pixel of the sky observed. With a typical depth of AB $\sim 21.25$ mag per band, this filter set thus allows for an indiscriminate and accurate characterization of the stellar population in our Galaxy, it provides an unprecedented 2D photo-spectral information for all resolved galaxies in the local universe, as well as accurate photo-z estimates ($\Delta\,z\sim 0.01-0.03$) for moderately bright (up to $r\sim 20$ mag) extragalactic sources. While some narrow band filters are designed for the study of particular emission features ([OII]/$\lambda$3727, H$\alpha$/$\lambda$6563) up to $z < 0.015$, they also provide well-defined windows for the analysis of other emission lines at higher redshifts. As a result, J-PLUS has the potential to contribute to a wide range of fields in Astrophysics, both in the nearby universe (Milky Way, 2D IFU-like studies, stellar populations of nearby and moderate redshift galaxies, clusters of galaxies) and at high redshifts (ELGs at $z\approx 0.77, 2.2$ and $4.4$, QSOs, etc). With this paper, we release $\sim 36$ sq.deg of J-PLUS data, containing about $1.5\times 10^5$ stars and $10^5$ galaxies at $r<21$ mag., Comment: Submitted to A&A
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- 2018
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60. DETERMINAÇÃO DO ESTÁGIO DE MATURAÇÃO DE FRUTOS
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Oliveira, V. C., primary, Costa, N. A., additional, Gonçalves, D. J. R., additional, Paiva, M. J. A., additional, and Vieira, É. N. R., additional
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- 2022
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61. Hyperelastic Behaviour of Adhesives and Its Effect on Bonded Joints: An Exploratory Study
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Sánchez-Arce, I. J., primary, Ramalho, L. D. C., additional, Gonçalves, D. C., additional, Campilho, R. D. S. G., additional, and Belinha, J., additional
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- 2022
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62. Complexity of some arc-partition problems for digraphs
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Bang-Jensen, J., Bessy, S., Gonçalves, D., and Picasarri-Arrieta, L.
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- 2022
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63. Casamento Feliz: desenvolvendo a arte de ser uma só carne
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GONÇALVES, D., primary and GONÇALVES, D. F., additional
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- 2022
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64. The ASTRI Mini-Array of Cherenkov telescopes at the Observatorio del Teide
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Scuderi, S., Giuliani, A., Pareschi, G., Tosti, G., Catalano, O., Amato, E., Antonelli, L.A., Becerra Gonzàles, J., Bellassai, G., Bigongiari, C., Biondo, B., Böttcher, M., Bonanno, G., Bonnoli, G., Bruno, P., Bulgarelli, A., Canestrari, R., Capalbi, M., Caraveo, P., Cardillo, M., Conforti, V., Contino, G., Corpora, M., Costa, A., Cusumano, G., D'Aì, A., de Gouveia Dal Pino, E., Della Ceca, R., Escribano Rodriguez, E., Falceta-Gonçalves, D., Fermino, C., Fiori, M., Fioretti, V., Fiorini, M., Gallozzi, S., Gargano, C., Garozzo, S., Germani, S., Ghedina, A., Gianotti, F., Giarrusso, S., Gimenes, R., Giordano, V., Grillo, A., Grivel Gelly, C., Impiombato, D., Incardona, F., Incorvaia, S., Iovenitti, S., La Barbera, A., La Palombara, N., La Parola, V., Lamastra, A., Lessio, L., Leto, G., Lo Gerfo, F., Lodi, M., Lombardi, S., Longo, F., Lucarelli, F., Maccarone, M.C., Marano, D., Martinetti, E., Mereghetti, S., Micciché, A., Millul, R., Mineo, T., Mollica, D., Morlino, G., Morselli, A., Naletto, G., Nicotra, G., Pagliaro, A., Parmiggiani, N., Piano, G., Pintore, F., Poretti, E., Olmi, B., Rodeghiero, G., Rodriguez Fernandez, G., Romano, P., Romeo, G., Russo, F., Sangiorgi, P., Saturni, F.G., Schwarz, J.H., Sciacca, E., Sironi, G., Sottile, G., Stamerra, A., Tagliaferri, G., Testa, V., Umana, G., Uslenghi, M., Vercellone, S., Zampieri, L., and Zanmar Sanchez, R.
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- 2022
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65. Some aspects of Reidemeister fixed point theory, equivariant fixed point theory and coincidence theory
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Borsari, L. D., Cardona, F., and Gonçalves, D. L.
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- 2022
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66. The Ogden model and the natural neighbour radial point interpolation method for hyperelastic analyses
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Sánchez-Arce, I. J., Gonçalves, D. C., Ramalho, L. D. C., Campilho, R. D. S. G., and Belinha, J.
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- 2023
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67. Observations of the first electromagnetic counterpart to a gravitational wave source by the TOROS collaboration
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Díaz, M. C., Macri, L. M., Lambas, D. Garcia, de Oliveira, C. Mendes, Castellón, J. L. Nilo, Ribeiro, T., Sánchez, B., Schoenell, W., Abramo, L. R., Akras, S., Alcaniz, J. S., Artola, R., Beroiz, M., Bonoli, S., Cabral, J., Camuccio, R., Castillo, M., Chavushyan, V., Coelho, P., Colazo, C., Costa-Duarte, M. V., Larenas, H. Cuevas, DePoy, D. L., Romero, M. Domínguez, Dultzin, D., Fernández, D., García, J., Girardini, C., Gonçalves, D. R., Gonçalves, T. S., Gurovich, S., Jiménez-Teja, Y., Kanaan, A., Lares, M., de Oliveira, R. Lopes, López-Cruz, O., Marshall, J. L., Melia, R., Molino, A., Padilla, N., Peñuela, T., Placco, V. M., Quiñones, C., Rivera, A. Ramírez, Renzi, V., Riguccini, L., Ríos-López, E., Rodriguez, H., Sampedro, L., Schneiter, M., Sodré, L., Starck, M., Torres-Flores, S., Tornatore, M., and Zadrożny, A.
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Astrophysics - High Energy Astrophysical Phenomena ,Astrophysics - Solar and Stellar Astrophysics - Abstract
We present the results of prompt optical follow-up of the electromagnetic counterpart of the gravitational-wave event GW170817 by the Transient Optical Robotic Observatory of the South Collaboration (TOROS). We detected highly significant dimming in the light curves of the counterpart (Delta g=0.17+-0.03 mag, Delta r=0.14+-0.02 mag, Delta i=0.10 +- 0.03 mag) over the course of only 80 minutes of observations obtained ~35 hr after the trigger with the T80-South telescope. A second epoch of observations, obtained ~59 hr after the event with the EABA 1.5m telescope, confirms the fast fading nature of the transient. The observed colors of the counterpart suggest that this event was a "blue kilonova" relatively free of lanthanides., Comment: Accepted for publication in The Astrophysical Journal Letters
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- 2017
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68. Science with the Cherenkov Telescope Array
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Consortium, The Cherenkov Telescope Array, Acharya, B. S., Agudo, I., Samarai, I. Al, Alfaro, R., Alfaro, J., Alispach, C., Batista, R. Alves, Amans, J. -P., Amato, E., Ambrosi, G., Antolini, E., Antonelli, L. A., Aramo, C., Araya, M., Armstrong, T., Arqueros, F., Arrabito, L., Asano, K., Ashley, M., Backes, M., Balazs, C., Balbo, M., Ballester, O., Ballet, J., Bamba, A., Barkov, M., de Almeida, U. Barres, Barrio, J. A., Bastieri, D., Becherini, Y., Belfiore, A., Benbow, W., Berge, D., Bernardini, E., Bernardini, M. G., Bernardos, M., Bernlöhr, K., Bertucci, B., Biasuzzi, B., Bigongiari, C., Biland, A., Bissaldi, E., Biteau, J., Blanch, O., Blazek, J., Boisson, C., Bolmont, J., Bonanno, G., Bonardi, A., Bonavolontà, C., Bonnoli, G., Bosnjak, Z., Böttcher, M., Braiding, C., Bregeon, J., Brill, A., Brown, A. M., Brun, P., Brunetti, G., Buanes, T., Buckley, J., Bugaev, V., Bühler, R., Bulgarelli, A., Bulik, T., Burton, M., Burtovoi, A., Busetto, G., Canestrari, R., Capalbi, M., Capitanio, F., Caproni, A., Caraveo, P., Cárdenas, V., Carlile, C., Carosi, R., Carquín, E., Carr, J., Casanova, S., Cascone, E., Catalani, F., Catalano, O., Cauz, D., Cerruti, M., Chadwick, P., Chaty, S., Chaves, R. C. G., Chen, A., Chen, X., Chernyakova, M., Chikawa, M., Christov, A., Chudoba, J., Cieślar, M., Coco, V., Colafrancesco, S., Colin, P., Conforti, V., Connaughton, V., Conrad, J., Contreras, J. L., Cortina, J., Costa, A., Costantini, H., Cotter, G., Covino, S., Crocker, R., Cuadra, J., Cuevas, O., Cumani, P., D'Aì, A., D'Ammando, F., D'Avanzo, P., D'Urso, D., Daniel, M., Davids, I., Dawson, B., Dazzi, F., De Angelis, A., Anjos, R. de Cássia dos, De Cesare, G., De Franco, A., Pino, E. M. de Gouveia Dal, de la Calle, I., Lopez, R. de los Reyes, De Lotto, B., De Luca, A., De Lucia, M., de Naurois, M., Wilhelmi, E. de Oña, De Palma, F., De Persio, F., de Souza, V., Deil, C., Del Santo, M., Delgado, C., della Volpe, D., Di Girolamo, T., Di Pierro, F., Di Venere, L., Díaz, C., Dib, C., Diebold, S., Djannati-Ataï, A., Domínguez, A., Prester, D. Dominis, Dorner, D., Doro, M., Drass, H., Dravins, D., Dubus, G., Dwarkadas, V. V., Ebr, J., Eckner, C., Egberts, K., Einecke, S., Ekoume, T. R. N., Elsässer, D., Ernenwein, J. -P., Espinoza, C., Evoli, C., Fairbairn, M., Falceta-Goncalves, D., Falcone, A., Farnier, C., Fasola, G., Fedorova, E., Fegan, S., Fernandez-Alonso, M., Fernández-Barral, A., Ferrand, G., Fesquet, M., Filipovic, M., Fioretti, V., Fontaine, G., Fornasa, M., Fortson, L., Coromina, L. Freixas, Fruck, C., Fujita, Y., Fukazawa, Y., Funk, S., Füßling, M., Gabici, S., Gadola, A., Gallant, Y., Garcia, B., López, R. Garcia, Garczarczyk, M., Gaskins, J., Gasparetto, T., Gaug, M., Gerard, L., Giavitto, G., Giglietto, N., Giommi, P., Giordano, F., Giro, E., Giroletti, M., Giuliani, A., Glicenstein, J. -F., Gnatyk, R., Godinovic, N., Goldoni, P., Gómez-Vargas, G., González, M. M., González, J. M., Götz, D., Graham, J., Grandi, P., Granot, J., Green, A. J., Greenshaw, T., Griffiths, S., Gunji, S., Hadasch, D., Hara, S., Hardcastle, M. J., Hassan, T., Hayashi, K., Hayashida, M., Heller, M., Helo, J. C., Hermann, G., Hinton, J., Hnatyk, B., Hofmann, W., Holder, J., Horan, D., Hörandel, J., Horns, D., Horvath, P., Hovatta, T., Hrabovsky, M., Hrupec, D., Humensky, T. B., Hütten, M., Iarlori, M., Inada, T., Inome, Y., Inoue, S., Inoue, T., Inoue, Y., Iocco, F., Ioka, K., Iori, M., Ishio, K., Iwamura, Y., Jamrozy, M., Janecek, P., Jankowsky, D., Jean, P., Jung-Richardt, I., Jurysek, J., Kaaret, P., Karkar, S., Katagiri, H., Katz, U., Kawanaka, N., Kazanas, D., Khélifi, B., Kieda, D. B., Kimeswenger, S., Kimura, S., Kisaka, S., Knapp, J., Knödlseder, J., Koch, B., Kohri, K., Komin, N., Kosack, K., Kraus, M., Krause, M., Krauß, F., Kubo, H., Mezek, G. Kukec, Kuroda, H., Kushida, J., La Palombara, N., Lamanna, G., Lang, R. G., Lapington, J., Blanc, O. Le, Leach, S., Lees, J. -P., Lefaucheur, J., de Oliveira, M. A. Leigui, Lenain, J. -P., Lico, R., Limon, M., Lindfors, E., Lohse, T., Lombardi, S., Longo, F., López, M., López-Coto, R., Lu, C. -C., Lucarelli, F., Luque-Escamilla, P. L., Lyard, E., Maccarone, M. C., Maier, G., Majumdar, P., Malaguti, G., Mandat, D., Maneva, G., Manganaro, M., Mangano, S., Marcowith, A., Marín, J., Markoff, S., Martí, J., Martin, P., Martínez, M., Martínez, G., Masetti, N., Masuda, S., Maurin, G., Maxted, N., Mazin, D., Medina, C., Melandri, A., Mereghetti, S., Meyer, M., Minaya, I. A., Mirabal, N., Mirzoyan, R., Mitchell, A., Mizuno, T., Moderski, R., Mohammed, M., Mohrmann, L., Montaruli, T., Moralejo, A., Morcuende-Parrilla, D., Mori, K., Morlino, G., Morris, P., Morselli, A., Moulin, E., Mukherjee, R., Mundell, C., Murach, T., Muraishi, H., Murase, K., Nagai, A., Nagataki, S., Nagayoshi, T., Naito, T., Nakamori, T., Nakamura, Y., Niemiec, J., Nieto, D., Nikołajuk, M., Nishijima, K., Noda, K., Nosek, D., Novosyadlyj, B., Nozaki, S., O'Brien, P., Oakes, L., Ohira, Y., Ohishi, M., Ohm, S., Okazaki, N., Okumura, A., Ong, R. A., Orienti, M., Orito, R., Osborne, J. P., Ostrowski, M., Otte, N., Oya, I., Padovani, M., Paizis, A., Palatiello, M., Palatka, M., Paoletti, R., Paredes, J. M., Pareschi, G., Parsons, R. D., Pe'er, A., Pech, M., Pedaletti, G., Perri, M., Persic, M., Petrashyk, A., Petrucci, P., Petruk, O., Peyaud, B., Pfeifer, M., Piano, G., Pisarski, A., Pita, S., Pohl, M., Polo, M., Pozo, D., Prandini, E., Prast, J., Principe, G., Prokhorov, D., Prokoph, H., Prouza, M., Pühlhofer, G., Punch, M., Pürckhauer, S., Queiroz, F., Quirrenbach, A., Rainò, S., Razzaque, S., Reimer, O., Reimer, A., Reisenegger, A., Renaud, M., Rezaeian, A. H., Rhode, W., Ribeiro, D., Ribó, M., Richtler, T., Rico, J., Rieger, F., Riquelme, M., Rivoire, S., Rizi, V., Rodriguez, J., Fernandez, G. Rodriguez, Vázquez, J. J. Rodríguez, Rojas, G., Romano, P., Romeo, G., Rosado, J., Rovero, A. C., Rowell, G., Rudak, B., Rugliancich, A., Rulten, C., Sadeh, I., Safi-Harb, S., Saito, T., Sakaki, N., Sakurai, S., Salina, G., Sánchez-Conde, M., Sandaker, H., Sandoval, A., Sangiorgi, P., Sanguillon, M., Sano, H., Santander, M., Sarkar, S., Satalecka, K., Saturni, F. G., Schioppa, E. 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Astrophysics - Instrumentation and Methods for Astrophysics ,Astrophysics - High Energy Astrophysical Phenomena ,High Energy Physics - Experiment - Abstract
The Cherenkov Telescope Array, CTA, will be the major global observatory for very high energy gamma-ray astronomy over the next decade and beyond. The scientific potential of CTA is extremely broad: from understanding the role of relativistic cosmic particles to the search for dark matter. CTA is an explorer of the extreme universe, probing environments from the immediate neighbourhood of black holes to cosmic voids on the largest scales. Covering a huge range in photon energy from 20 GeV to 300 TeV, CTA will improve on all aspects of performance with respect to current instruments. The observatory will operate arrays on sites in both hemispheres to provide full sky coverage and will hence maximize the potential for the rarest phenomena such as very nearby supernovae, gamma-ray bursts or gravitational wave transients. With 99 telescopes on the southern site and 19 telescopes on the northern site, flexible operation will be possible, with sub-arrays available for specific tasks. CTA will have important synergies with many of the new generation of major astronomical and astroparticle observatories. Multi-wavelength and multi-messenger approaches combining CTA data with those from other instruments will lead to a deeper understanding of the broad-band non-thermal properties of target sources. The CTA Observatory will be operated as an open, proposal-driven observatory, with all data available on a public archive after a pre-defined proprietary period. Scientists from institutions worldwide have combined together to form the CTA Consortium. This Consortium has prepared a proposal for a Core Programme of highly motivated observations. The programme, encompassing approximately 40% of the available observing time over the first ten years of CTA operation, is made up of individual Key Science Projects (KSPs), which are presented in this document., Comment: 213 pages, including references and glossary. Version 2: credits and references updated, some figures updated, and author list updated
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- 2017
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69. Cherenkov Telescope Array Contributions to the 35th International Cosmic Ray Conference (ICRC2017)
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Acero, F., Acharya, B. S., Portella, V. Acín, Adams, C., Agudo, I., Aharonian, F., Samarai, I. Al, Alberdi, A., Alcubierre, M., Alfaro, R., Alfaro, J., Alispach, C., Aloisio, R., Batista, R. Alves, Amans, J. -P., Amato, E., Ambrogi, L., Ambrosi, G., Ambrosio, M., Anderson, J., Anduze, M., Angüner, E. O., Antolini, E., Antonelli, L. A., Antonuccio, V., Antoranz, P., Aramo, C., Araya, M., Arcaro, C., Armstrong, T., Arqueros, F., Arrabito, L., Arrieta, M., Asano, K., Asano, A., Ashley, M., Aubert, P., Singh, C. B., Babic, A., Backes, M., Bajtlik, S., Balazs, C., Balbo, M., Ballester, O., Ballet, J., Ballo, L., Balzer, A., Bamba, A., Bandiera, R., Barai, P., Barbier, C., Barcelo, M., Barkov, M., de Almeida, U. Barres, Barrio, J. A., Bastieri, D., Bauer, C., Becciani, U., Becherini, Y., Tjus, J. Becker, Bednarek, W., Belfiore, A., Benbow, W., Benito, M., Berge, D., Bernardini, E., Bernardini, M. G., Bernardos, M., Bernhard, S., Bernlöhr, K., Salucci, C. 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J., Schlenstedt, S., Schmidt, T., Schmoll, J., Schneider, M., Schoorlemmer, H., Schovanek, P., Schulz, A., Schussler, F., Schwanke, U., Schwarz, J., Schweizer, T., Schwemmer, S., Sciacca, E., Scuderi, S., Seglar-Arroyo, M., Segreto, A., Seitenzahl, I., Semikoz, D., Sergijenko, O., Serre, N., Servillat, M., Seweryn, K., Shah, K., Shalchi, A., Sharma, M., Shellard, R. C., Shilon, I., Sidoli, L., Sidz, M., Siejkowski, H., Silk, J., Sillanpää, A., Simone, D., Singh, B. B., Sironi, G., Sitarek, J., Sizun, P., Sliusar, V., Slowikowska, A., Smith, A., Sobczyńska, D., Sokolenko, A., Sol, H., Sottile, G., Springer, W., Stahl, O., Stamerra, A., Stanič, S., Starling, R., Staszak, D., Stawarz, Ł., Steenkamp, R., Stefanik, S., Stegmann, C., Steiner, S., Stella, C., Stephan, M., Sternberger, R., Sterzel, M., Stevenson, B., Stodulska, M., Stodulski, M., Stolarczyk, T., Stratta, G., Straumann, U., Stuik, R., Suchenek, M., Suomijarvi, T., Supanitsky, A. D., Suric, T., Sushch, I., Sutcliffe, P., Sykes, J., Szanecki, M., Szepieniec, T., Tagliaferri, G., Tajima, H., Takahashi, K., Takahashi, H., Takahashi, M., Takalo, L., Takami, S., Takata, J., Takeda, J., Tam, T., Tanaka, M., Tanaka, T., Tanaka, Y., Tanaka, S., Tanci, C., Tavani, M., Tavecchio, F., Tavernet, J. -P., Tayabaly, K., Tejedor, L. A., Temme, F., Temnikov, P., Terada, Y., Terrazas, J. C., Terrier, R., Terront, D., Terzic, T., Tescaro, D., Teshima, M., Testa, V., Thoudam, S., Tian, W., Tibaldo, L., Tiengo, A., Tiziani, D., Tluczykont, M., Peixoto, C. J. Todero, Tokanai, F., Tokarz, M., Toma, K., Tomastik, J., Tonachini, A., Tonev, D., Tornikoski, M., Torres, D. F., Torresi, E., Tosti, G., Totani, T., Tothill, N., Toussenel, F., Tovmassian, G., Trakarnsirinont, N., Travnicek, P., Trichard, C., Trifoglio, M., Pujadas, I. Troyano, Tsirou, M., Tsujimoto, S., Tsuru, T., Uchiyama, Y., Umana, G., Uslenghi, M., Vagelli, V., Vagnetti, F., Valentino, M., Vallania, P., Valore, L., Berg, A. M. Van den, van Driel, W., van Eldik, C., van Soelen, B., Vandenbroucke, J., Vanderwalt, J., Varner, G. S., Vasileiadis, G., Vassiliev, V., Vázquez, J. R., Acosta, M. Vázquez, Vecchi, M., Vega, A., Veitch, P., Venault, P., Venter, C., Vercellone, S., Veres, P., Vergani, S., Verzi, V., Vettolani, G. P., Veyssiere, C., Viana, A., Vicha, J., Vigorito, C., Villanueva, J., Vincent, P., Vink, J., Visconti, F., Vittorini, V., Voelk, H., Voisin, V., Vollhardt, A., Vorobiov, S., Vovk, I., Vrastil, M., Vuillaume, T., Wagner, S. J., Wagner, R., Wagner, P., Wakely, S. P., Walstra, T., Walter, R., Ward, M., Ward, J. E., Warren, D., Watson, J. J., Webb, N., Wegner, P., Weiner, O., Weinstein, A., Weniger, C., Werner, F., Wetteskind, H., White, M., White, R., Wierzcholska, A., Wiesand, S., Wijers, R., Wilcox, P., Wilhelm, A., Wilkinson, M., Will, M., Williams, D. A., Winter, M., Wojcik, P., Wolf, D., Wood, M., Wörnlein, A., Wu, T., Yadav, K. K., Yaguna, C., Yamamoto, T., Yamamoto, H., Yamane, N., Yamazaki, R., Yanagita, S., Yang, L., Yelos, D., Yoshida, T., Yoshida, M., Yoshiike, S., Yoshikoshi, T., Yu, P., Zaborov, D., Zacharias, M., Zaharijas, G., Zajczyk, A., Zampieri, L., Zandanel, F., Zanin, R., Sanchez, R. Zanmar, Zaric, D., Zavrtanik, M., Zavrtanik, D., Zdziarski, A. A., Zech, A., Zechlin, H., Zhdanov, V. I., Ziegler, A., Ziemann, J., Ziętara, K., Zink, A., Ziółkowski, J., Zitelli, V., Zoli, A., and Zorn, J.
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Astrophysics - High Energy Astrophysical Phenomena - Abstract
List of contributions from the Cherenkov Telescope Array Consortium presented at the 35th International Cosmic Ray Conference, July 12-20 2017, Busan, Korea., Comment: Index of Cherenkov Telescope Array conference proceedings at the ICRC2017, Busan, Korea
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- 2017
70. Monte Carlo Performance Studies for the Site Selection of the Cherenkov Telescope Array
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Hassan, T., Arrabito, L., Bernlöhr, K., Bregeon, J., Cortina, J., Cumani, P., Di Pierro, F., Falceta-Goncalves, D., Lang, R. G., Hinton, J., Jogler, T., Maier, G., Moralejo, A., Morselli, A., Peixoto, C. J. Todero, and Wood, M.
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Astrophysics - Instrumentation and Methods for Astrophysics - Abstract
The Cherenkov Telescope Array (CTA) represents the next generation of ground-based instruments for very-high-energy (VHE) gamma-ray astronomy, aimed at improving on the sensitivity of current-generation experiments by an order of magnitude and providing coverage over four decades of energy. The current CTA design consists of two arrays of tens of imaging atmospheric Cherenkov telescopes, comprising Small, Medium and Large-Sized Telescopes, with one array located in each of the Northern and Southern Hemispheres. To study the effect of the site choice on the overall \gls{cta} performance and support the site evaluation process, detailed Monte Carlo simulations have been performed. These results show the impact of different site-related attributes such as altitude, night-sky background and local geomagnetic field on CTA performance for the observation of VHE gamma rays., Comment: 34 pages, 11 figures, Accepted for publication in APP
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- 2017
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71. Prospects for CTA observations of the young SNR RX J1713.7-3946
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Consortium, The CTA, Acero, F., Aloisio, R., Amans, J., Amato, E., Antonelli, L. A., Aramo, C., Armstrong, T., Arqueros, F., Asano, K., Ashley, M., Backes, M., Balazs, C., Balzer, A., Bamba, A., Barkov, M., Barrio, J. A., Benbow, W., Bernlöhr, K., Beshley, V., Bigongiari, C., Biland, A., Bilinsky, A., Bissaldi, E., Biteau, J., Blanch, O., Blasi, P., Blazek, J., Boisson, C., Bonanno, G., Bonardi, A., Bonavolontà, C., Bonnoli, G., Braiding, C., Brau-Nogué, S., Bregeon, J., Brown, A. M., Bugaev, V., Bulgarelli, A., Bulik, T., Burton, M., Burtovoi, A., Busetto, G., Böttcher, M., Cameron, R., Capalbi, M., Caproni, A., Caraveo, P., Carosi, R., Cascone, E., Cerruti, M., Chaty, S., Chen, A., Chen, X., Chernyakova, M., Chikawa, M., Chudoba, J., Cohen-Tanugi, J., Colafrancesco, S., Conforti, V., Contreras, J. L., Costa, A., Cotter, G., Covino, S., Covone, G., Cumani, P., Cusumano, G., D'Ammando, F., D'Urso, D., Daniel, M., Dazzi, F., De Angelis, A., De Cesare, G., De Franco, A., De Frondat, F., Pino, E. M. de Gouveia Dal, De Lisio, C., Lopez, R. de los Reyes, De Lotto, B., de Naurois, M., De Palma, F., Del Santo, M., Delgado, C., della Volpe, D., Di Girolamo, T., Di Giulio, C., Di Pierro, F., Di Venere, L., Doro, M., Dournaux, J., Dumas, D., Dwarkadas, V., Díaz, C., Ebr, J., Egberts, K., Einecke, S., Elsässer, D., Eschbach, S., Falceta-Goncalves, D., Fasola, G., Fedorova, E., Fernández-Barral, A., Ferrand, G., Fesquet, M., Fiandrini, E., Fiasson, A., Filipovíc, M. D., Fioretti, V., Font, L., Fontaine, G., Franco, F. J., Coromina, L. Freixas, Fujita, Y., Fukui, Y., Funk, S., Förster, A., Gadola, A., López, R. Garcia, Garczarczyk, M., Giglietto, N., Giordano, F., Giuliani, A., Glicenstein, J., Gnatyk, R., Goldoni, P., Grabarczyk, T., Graciani, R., Graham, J., Grandi, P., Granot, J., Green, A. J., Griffiths, S., Gunji, S., Hakobyan, H., Hara, S., Hassan, T., Hayashida, M., Heller, M., Helo, J. C., Hinton, J., Hnatyk, B., Huet, J., Huetten, M., Humensky, T. B., Hussein, M., Hörandel, J., Ikeno, Y., Inada, T., Inome, Y., Inoue, S., Inoue, T., Inoue, Y., Ioka, K., Iori, M., Jacquemier, J., Janecek, P., Jankowsky, D., Jung, I., Kaaret, P., Katagiri, H., Kimeswenger, S., Kimura, S., Knödlseder, J., Koch, B., Kocot, J., Kohri, K., Komin, N., Konno, Y., Kosack, K., Koyama, S., Kraus, M., Kubo, H., Mezek, G. Kukec, Kushida, J., La Palombara, N., Lalik, K., Lamanna, G., Landt, H., Lapington, J., Laporte, P., Lee, S., Lees, J., Lefaucheur, J., Lenain, J. -P., Leto, G., Lindfors, E., Lohse, T., Lombardi, S., Longo, F., Lopez, M., Lucarelli, F., Luque-Escamilla, P. L., López-Coto, R., Maccarone, M. C., Maier, G., Malaguti, G., Mandat, D., Maneva, G., Mangano, S., Marcowith, A., Martí, J., Martínez, M., Martínez, G., Masuda, S., Maurin, G., Maxted, N., Melioli, C., Mineo, T., Mirabal, N., Mizuno, T., Moderski, R., Mohammed, M., Montaruli, T., Moralejo, A., Mori, K., Morlino, G., Morselli, A., Moulin, E., Mukherjee, R., Mundell, C., Muraishi, H., Murase, K., Nagataki, S., Nagayoshi, T., Naito, T., Nakajima, D., Nakamori, T., Nemmen, R., Niemiec, J., Nieto, D., Nievas-Rosillo, M., Nikołajuk, M., Nishijima, K., Noda, K., Nogues, L., Nosek, D., Novosyadlyj, B., Nozaki, S., Ohira, Y., Ohishi, M., Ohm, S., Okumura, A., Ong, R. A., Orito, R., Orlati, A., Ostrowski, M., Oya, I., Padovani, M., Palacio, J., Palatka, M., Paredes, J. M., Pavy, S., Pe'er, A., Persic, M., Petrucci, P., Petruk, O., Pisarski, A., Pohl, M., Porcelli, A., Prandini, E., Prast, J., Principe, G., Prouza, M., Pueschel, E., Pühlhofer, G., Quirrenbach, A., Rameez, M., Reimer, O., Renaud, M., Ribó, M., Rico, J., Rizi, V., Rodriguez, J., Fernandez, G. Rodriguez, Vázquez, J. J. Rodríguez, Romano, P., Romeo, G., Rosado, J., Rousselle, J., Rowell, G., Rudak, B., Sadeh, I., Safi-Harb, S., Saito, T., Sakaki, N., Sanchez, D., Sangiorgi, P., Sano, H., Santander, M., Sarkar, S., Sawada, M., Schioppa, E. J., Schoorlemmer, H., Schovanek, P., Schussler, F., Sergijenko, O., Servillat, M., Shalchi, A., Shellard, R. C., Siejkowski, H., Sillanpää, A., Simone, D., Sliusar, V., Sol, H., Stanič, S., Starling, R., Stawarz, Ł., Stefanik, S., Stephan, M., Stolarczyk, T., Szanecki, M., Szepieniec, T., Tagliaferri, G., Tajima, H., Takahashi, M., Takeda, J., Tanaka, M., Tanaka, S., Tejedor, L. A., Telezhinsky, I., Temnikov, P., Terada, Y., Tescaro, D., Teshima, M., Testa, V., Thoudam, S., Tokanai, F., Torres, D. F., Torresi, E., Tosti, G., Townsley, C., Travnicek, P., Trichard, C., Trifoglio, M., Tsujimoto, S., Vagelli, V., Vallania, P., Valore, L., van Driel, W., van Eldik, C., Vandenbroucke, J., Vassiliev, V., Vecchi, M., Vercellone, S., Vergani, S., Vigorito, C., Vorobiov, S., Vrastil, M., Acosta, M. L. Vázquez, Wagner, S. J., Wagner, R., Wakely, S. P., Walter, R., Ward, J. E., Watson, J. J., Weinstein, A., White, M., White, R., Wierzcholska, A., Wilcox, P., Williams, D. A., Wischnewski, R., Wojcik, P., Yamamoto, T., Yamamoto, H., Yamazaki, R., Yanagita, S., Yang, L., Yoshida, T., Yoshida, M., Yoshiike, S., Yoshikoshi, T., Zacharias, M., Zampieri, L., Zanin, R., Zavrtanik, M., Zavrtanik, D., Zdziarski, A., Zech, A., Zechlin, H., Zhdanov, V., Ziegler, A., and Zorn, J.
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Astrophysics - High Energy Astrophysical Phenomena - Abstract
We perform simulations for future Cherenkov Telescope Array (CTA) observations of RX~J1713.7$-$3946, a young supernova remnant (SNR) and one of the brightest sources ever discovered in very-high-energy (VHE) gamma rays. Special attention is paid to explore possible spatial (anti-)correlations of gamma rays with emission at other wavelengths, in particular X-rays and CO/H{\sc i} emission. We present a series of simulated images of RX J1713.7$-$3946 for CTA based on a set of observationally motivated models for the gamma-ray emission. In these models, VHE gamma rays produced by high-energy electrons are assumed to trace the non-thermal X-ray emission observed by {\it XMM-Newton}, whereas those originating from relativistic protons delineate the local gas distributions. The local atomic and molecular gas distributions are deduced by the NANTEN team from CO and H{\sc i} observations. Our primary goal is to show how one can distinguish the emission mechanism(s) of the gamma rays (i.e., hadronic vs leptonic, or a mixture of the two) through information provided by their spatial distribution, spectra, and time variation. This work is the first attempt to quantitatively evaluate the capabilities of CTA to achieve various proposed scientific goals by observing this important cosmic particle accelerator., Comment: 19 pages, 5 figures. Accepted for publication in ApJ
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- 2017
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72. Analysis of the effects of free-length on bonded T-joints by an elastoplastic meshless analysis.
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Sousa, R. J. C., Sánchez-Arce, I. J., Dionísio, J. M. M., Ramalho, L. D. C., Gonçalves, D. C., Campilho, R.D.S.G., and Belinha, J.
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MESHFREE methods ,FINITE element method ,ALUMINUM alloys ,ALUMINUM alloying ,EPOXY compounds - Abstract
Various configurations of adhesive joints exist, each with unique characteristics. In the case of peel load solicitations, T-joints are the most common choice but are not sufficiently addressed in the literature, especially regarding the geometrical and material influence on their performance. Recently, meshless methods, like the Radial Point Interpolation Method (RPIM), have been used as alternatives to the Finite Element Method (FEM) for investigating joint behaviours. The present work aims to study the free length (FL) effect in T-joints, which is related to substrate stiffness. Three distinct FL dimensions were evaluated. At the same time, the effect of t
p2 and adhesive type were taken into account. Initially, joint strength (Pmax ) was predicted using two numerical approaches: FEM and RPIM, both employing elastic-plastic material models. Subsequently, the results were compared with the experimental data. Moreover, two yield criteria were considered to analyse the adhesive: von Mises and the Exponential Drucker-Prager criteria. The data resultant from this first phase was then used to select the correct yield criterion for evaluating the influence of FL in the adhesive joints. The methodology was validated, and then geometrical and material design recommendations were presented for the efficient use of T-joints in structural applications. [ABSTRACT FROM AUTHOR]- Published
- 2024
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73. Deaf Inclusion Through Brazilian Sign Language: A Computational Architecture Supporting Artifacts and Interactive Applications and Tools
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Garcia, L. S., Felipe, T. A., Guedes, A. P., Antunes, D. R., Iatskiu, C. E., Todt, E., Bueno, J., Trindade, D. de F. G., Gonçalves, D. A., Canteri, R., Canal, M. C., Ferreira, M. A. M., Silva, A. M. C., Galvão, L., Rodrigues, L., Goos, Gerhard, Founding Editor, Hartmanis, Juris, Founding Editor, Bertino, Elisa, Editorial Board Member, Gao, Wen, Editorial Board Member, Steffen, Bernhard, Editorial Board Member, Woeginger, Gerhard, Editorial Board Member, Yung, Moti, Editorial Board Member, Antona, Margherita, editor, and Stephanidis, Constantine, editor
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- 2021
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74. Selection for winners impacts the endocrine system in the Siamese fighting fish
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Ramos, A. and Gonçalves, D.
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- 2022
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75. Topology optimization of light structures using the natural neighbour radial point interpolation method
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Gonçalves, D. C., Lopes, J. D. F., Campilho, R. D. S. G., and Belinha, J.
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- 2022
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76. The ammonium excreting Azospirillum brasilense strain HM053 : a new alternative inoculant for maize
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Pedrosa, F. O., Oliveira, A. L. M., Guimarães, V. F., Etto, R. M., Souza, E. M., Furmam, F. G., Gonçalves, D. R. P., Santos, O. J. A. P., Gonçalves, L. S. A., Battistus, A. G., and Galvão, C. W.
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- 2020
77. Features of collisionless turbulence in the intracluster medium from simulated Faraday rotation maps II: the effects of instabilities feedback
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Santos-Lima, R., Pino, E. M. de Gouveia Dal, Falceta-Gonçalves, D. A., Nakwacki, M. S., and Kowal, G.
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Astrophysics - High Energy Astrophysical Phenomena ,Physics - Fluid Dynamics ,Physics - Plasma Physics - Abstract
Statistical analysis of Faraday Rotation Measure (RM) maps of the intracluster medium (ICM) of galaxy clusters provides a unique tool to evaluate some spatial features of the magnetic fields there. Its combination with numerical simulations of magnetohydrodynamic (MHD) turbulence allows the diagnosis of the ICM turbulence. Being the ICM plasma weakly collisional, the thermal velocity distribution of the particles naturally develops anisotropies as a consequence of the large scale motions and the conservation of the magnetic moment of the charged particles. A previous study (Paper I) analyzed the impact of large scale thermal anisotropy on the statistics of RM maps synthesized from simulations of turbulence; these simulations employed a collisionless MHD model which considered a tensor pressure with uniform anisotropy. In the present work, we extend that analysis to a collisionless MHD model in which the thermal anisotropy develops according to the conservation of the magnetic moment of the thermal particles. We also consider the effect of anisotropy relaxation caused by the micro-scale mirror and firehose instabilities. We show that if the relaxation rate is fast enough to keep the anisotropy limited by the threshold values of the instabilities, the dispersion and power spectrum of the RM maps are indistinguishable from those obtained from collisional MHD. Otherwise, there is a reduction in the dispersion and steepening of the power spectrum of the RM maps (compared to the collisional case). Considering the first scenario, the use of collisional MHD simulations for modeling the RM statistics in the ICM becomes better justified., Comment: 7 pages, 4 figures, accepted for publication on MNRAS
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- 2016
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78. Handbook of LHC Higgs Cross Sections: 4. Deciphering the Nature of the Higgs Sector
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de Florian, D., Grojean, C., Maltoni, F., Mariotti, C., Nikitenko, A., Pieri, M., Savard, P., Schumacher, M., Tanaka, R., Aggleton, R., Ahmad, M., Allanach, B., Anastasiou, C., Astill, W., Badger, S., Badziak, M., Baglio, J., Bagnaschi, E., Ballestrero, A., Banfi, A., Barducci, D., Beckingham, M., Becot, C., Bélanger, G., Bellm, J., Belyaev, N., Bernlochner, F. U., Beskidt, C., Biekötter, A., Bishara, F., Bizon, W., Bomark, N. E., Bonvini, M., Borowka, S., Bortolotto, V., Boselli, S., Botella, F. J., Boughezal, R., Branco, G. C., Brehmer, J., Brenner, L., Bressler, S., Brivio, I., Broggio, A., Brun, H., Buchalla, G., Burgard, C. D., Calandri, A., Caminada, L., Armadans, R. Caminal, Campanario, F., Campbell, J., Caola, F., Calame, C. M. Carloni, Carrazza, S., Carvalho, A., Casolino, M., Cata, O., Celis, A., Cerutti, F., Chanon, N., Chen, M., Chen, X., Nejad, B. Chokoufé, Christensen, N., Ciuchini, M., Contino, R., Corbett, T., Costa, R., Curtin, D., Dall'Osso, M., David, A., Dawson, S., de Blas, J., de Boer, W., Manzano, P. de Castro, Degrande, C., Delgado, R. L., Demartin, F., Denner, A., Di Micco, B., Di Nardo, R., Dittmaier, S., Dobado, A., Dorigo, T., Dreyer, F. A., Dührssen, M., Duhr, C., Dulat, F., Ecker, K., Ellis, K., Ellwanger, U., Englert, C., Espriu, D., Falkowski, A., Fayard, L., Feger, R., Ferrera, G., Ferroglia, A., Fidanza, N., Figy, T., Flechl, M., Fontes, D., Forte, S., Francavilla, P., Franco, E., Frederix, R., Freitas, A., Freitas, F. F., Frensch, F., Frixione, S., Fuks, B., Furlan, E., Gadatsch, S., Gao, J., Gao, Y., Garzelli, M. V., Gehrmann, T., Gerosa, R., Ghezzi, M., Ghosh, D., Gieseke, S., Gillberg, D., Giudice, G. F., Glover, E. W. N., Goertz, F., Gonçalves, D., Gonzalez-Fraile, J., Gorbahn, M., Gori, S., Gottardo, C. A., Gouzevitch, M., Govoni, P., Gray, D., Grazzini, M., Greiner, N., Greljo, A., Grigo, J., Gritsan, A. V., Gröber, R., Guindon, S., Haber, H. E., Han, C., Han, T., Harlander, R., Harrendorf, M. A., Hartanto, H. B., Hays, C., Heinemeyer, S., Heinrich, G., Herrero, M., Herzog, F., Hespel, B., Hirschi, V., Hoeche, S., Honeywell, S., Huber, S. J., Hugonie, C., Huston, J., Ilnicka, A., Isidori, G., Jäger, B., Jaquier, M., Jones, S. P., Juste, A., Kallweit, S., Kaluza, A., Kardos, A., Karlberg, A., Kassabov, Z., Kauer, N., Kazakov, D. I., Kerner, M., Kilian, W., Kling, F., Köneke, K., Kogler, R., Konoplich, R., Kortner, S., Kraml, S., Krause, C., Krauss, F., Krawczyk, M., Kulesza, A., Kuttimalai, S., Lane, R., Lazopoulos, A., Lee, G., Lenzi, P., Lewis, I. M., Li, Y., Liebler, S., Lindert, J., Liu, X., Liu, Z., Llanes-Estrada, F. J., Logan, H. E., Lopez-Val, D., Low, I., Luisoni, G., Maierhöfer, P., Maina, E., Mansoulié, B., Mantler, H., Mantoani, M., Marini, A. C., Outschoorn, V. I. Martinez, Marzani, S., Marzocca, D., Massironi, A., Mawatari, K., Mazzitelli, J., McCarn, A., Mellado, B., Melnikov, K., Menari, S. B., Merlo, L., Meyer, C., Milenovic, P., Mimasu, K., Mishima, S., Mistlberger, B., Moch, S. -O., Mohammadi, A., Monni, P. F., Montagna, G., Llácer, M. Moreno, Moretti, N., Moretti, S., Motyka, L., Mück, A., Mühlleitner, M., Munir, S., Musella, P., Nadolsky, P., Napoletano, D., Nebot, M., Neu, C., Neubert, M., Nevzorov, R., Nicrosini, O., Nielsen, J., Nikolopoulos, K., No, J. M., O'Brien, C., Ohl, T., Oleari, C., Orimoto, T., Pagani, D., Pandini, C. E., Papaefstathiou, A., Papanastasiou, A. S., Passarino, G., Pecjak, B. D., Pelliccioni, M., Perez, G., Perrozzi, L., Petriello, F., Petrucciani, G., Pianori, E., Piccinini, F., Pierini, M., Pilkington, A., Plätzer, S., Plehn, T., Podskubka, R., Potter, C. T., Pozzorini, S., Prokofiev, K., Pukhov, A., Puljak, I., Queitsch-Maitland, M., Quevillon, J., Rathlev, D., Rauch, M., Re, E., Rebelo, M. N., Rebuzzi, D., Reina, L., Reuschle, C., Reuter, J., Riembau, M., Riva, F., Rizzi, A., Robens, T., Röntsch, R., Rojo, J., Romão, J. C., Rompotis, N., Roskes, J., Roth, R., Salam, G. P., Salerno, R., Sampaio, M. O. P., Santos, R., Sanz, V., Sanz-Cillero, J. J., Sargsyan, H., Sarica, U., Schichtel, P., Schlenk, J., Schmidt, T., Schmitt, C., Schönherr, M., Schubert, U., Schulze, M., Sekula, S., Sekulla, M., Shabalina, E., Shao, H. S., Shelton, J., Shepherd-Themistocleous, C. H., Shim, S. Y., Siegert, F., Signer, A., Silva, J. P., Silvestrini, L., Sjodahl, M., Slavich, P., Slawinska, M., Soffi, L., Spannowsky, M., Speckner, C., Sperka, D. M., Spira, M., Stål, O., Staub, F., Stebel, T., Stefaniak, T., Steinhauser, M., Stewart, I. W., Strassler, M. J., Streicher, J., Strom, D. M., Su, S., Sun, X., Tackmann, F. J., Tackmann, K., Teixeira, A. M., de Lima, R. 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- Subjects
High Energy Physics - Phenomenology ,High Energy Physics - Experiment - Abstract
This Report summarizes the results of the activities of the LHC Higgs Cross Section Working Group in the period 2014-2016. The main goal of the working group was to present the state-of-the-art of Higgs physics at the LHC, integrating all new results that have appeared in the last few years. The first part compiles the most up-to-date predictions of Higgs boson production cross sections and decay branching ratios, parton distribution functions, and off-shell Higgs boson production and interference effects. The second part discusses the recent progress in Higgs effective field theory predictions, followed by the third part on pseudo-observables, simplified template cross section and fiducial cross section measurements, which give the baseline framework for Higgs boson property measurements. The fourth part deals with the beyond the Standard Model predictions of various benchmark scenarios of Minimal Supersymmetric Standard Model, extended scalar sector, Next-to-Minimal Supersymmetric Standard Model and exotic Higgs boson decays. This report follows three previous working-group reports: Handbook of LHC Higgs Cross Sections: 1. Inclusive Observables (CERN-2011-002), Handbook of LHC Higgs Cross Sections: 2. Differential Distributions (CERN-2012-002), and Handbook of LHC Higgs Cross Sections: 3. Higgs properties (CERN-2013-004). The current report serves as the baseline reference for Higgs physics in LHC Run 2 and beyond., Comment: 869 pages, 295 figures, 248 tables and 1645 citations. Working Group web page: https://twiki.cern.ch/twiki/bin/view/LHCPhysics/LHCHXSWG
- Published
- 2016
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79. Contributions of the Cherenkov Telescope Array (CTA) to the 6th International Symposium on High-Energy Gamma-Ray Astronomy (Gamma 2016)
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Consortium, The CTA, Abchiche, A., Abeysekara, U., Abril, Ó., Acero, F., Acharya, B. S., Adams, C., Agnetta, G., Aharonian, F., Akhperjanian, A., Albert, A., Alcubierre, M., Alfaro, J., Alfaro, R., Allafort, A. J., Aloisio, R., Amans, J. -P., Amato, E., Ambrogi, L., Ambrosi, G., Ambrosio, M., Anderson, J., Anduze, M., Angüner, E. O., Antolini, E., Antonelli, L. A., Antonucci, M., Antonuccio, V., Antoranz, P., Aramo, C., Aravantinos, A., Araya, M., Arcaro, C., Arezki, B., Argan, A., Armstrong, T., Arqueros, F., Arrabito, L., Arrieta, M., Asano, K., Ashley, M., Aubert, P., Singh, C. B., Babic, A., Backes, M., Bais, A., Bajtlik, S., Balazs, C., Balbo, M., Balis, D., Balkowski, C., Ballester, O., Ballet, J., Balzer, A., Bamba, A., Bandiera, R., Barber, A., Barbier, C., Barcelo, M., Barkov, M., Barnacka, A., de Almeida, U. Barres, Barrio, J. A., Basso, S., Bastieri, D., Bauer, C., Becciani, U., Becherini, Y., Tjus, J. Becker, Beckmann, V., Bednarek, W., Benbow, W., Ventura, D. 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C., Rataj, M., Ravel, T., Razzaque, S., Reardon, P., Reichardt, I., Reimann, O., Reimer, A., Reimer, O., Reisenegger, A., Renaud, M., Renner, S., Reposeur, T., Reville, B., Rezaeian, A., Rhode, W., Ribeiro, D., Prado, R. Ribeiro, Ribó, M., Richards, G., Richer, M. G., Richtler, T., Rico, J., Ridky, J., Rieger, F., Riquelme, M., Ristori, P. R., Rivoire, S., Rizi, V., Roache, E., Rodriguez, J., Fernandez, G. Rodriguez, Vázquez, J. J. Rodríguez, Rojas, G., Romano, P., Romeo, G., Roncadelli, M., Rosado, J., Rose, J., Rosen, S., Lees, S. Rosier, Ross, D., Rouaix, G., Rousselle, J., Rovero, A. C., Rowell, G., Roy, F., Royer, S., Rubini, A., Rudak, B., Rugliancich, A., Rujopakarn, W., Rulten, C., Rupiński, M., Russo, F., Rutkowski, K., Saavedra, O., Sabatini, S., Sacco, B., Sadeh, I., Saemann, E. O., Safi-Harb, S., Saggion, A., Sahakian, V., Saito, T., Sakaki, N., Sakurai, S., Salamon, A., Salega, M., Salek, D., Greus, F. Salesa, Salgado, J., Salina, G., Salinas, L., Salini, A., Sanchez, D., Sanchez-Conde, M., Sandaker, H., Sandoval, A., Sangiorgi, P., Sanguillon, M., Sano, H., Santander, M., Santangelo, A., Santos, E. M., Santos-Lima, R., Sanuy, A., Sapozhnikov, L., Sarkar, S., Satalecka, K., Sato, Y., Savalle, R., Sawada, M., Sayède, F., Schanne, S., Schanz, T., Schioppa, E. J., Schlenstedt, S., Schmid, J., Schmidt, T., Schmoll, J., Schneider, M., Schoorlemmer, H., Schovanek, P., Schubert, A., Schullian, E. -M., Schultze, J., Schulz, A., Schulz, S., Schure, K., Schussler, F., Schwab, T., Schwanke, U., Schwarz, J., Schweizer, T., Schwemmer, S., Schwendicke, U., Schwerdt, C., Sciacca, E., Scuderi, S., Segreto, A., Seiradakis, J. -H., Sembroski, G. H., Semikoz, D., Sergijenko, O., Serre, N., Servillat, M., Seweryn, K., Shafi, N., Shalchi, A., Sharma, M., Shayduk, M., Shellard, R. C., Shibata, T., Shigenaka, A., Shilon, I., Shum, E., Sidoli, L., Sidz, M., Sieiro, J., Siejkowski, H., Silk, J., Sillanpää, A., Simone, D., Simpson, H., Singh, B. B., Sinha, A., Sironi, G., Sitarek, J., Sizun, P., Sliusar, V., Smith, A., Sobczyńska, D., Sol, H., Sottile, G., Sowiński, M., Spanier, F., Spengler, G., Spiga, R., Stadler, R., Stahl, O., Stamerra, A., Stanič, S., Starling, R., Staszak, D., Stawarz, Ł., Steenkamp, R., Stefanik, S., Stegmann, C., Steiner, S., Stella, C., Stephan, M., Stergioulas, N., Sternberger, R., Sterzel, M., Stevenson, B., Stinzing, F., Stodulska, M., Stodulski, M., Stolarczyk, T., Stratta, G., Straumann, U., Stringhetti, L., Strzys, M., Stuik, R., Sulanke, K. -H., Suomijärvi, T., Supanitsky, A. D., Suric, T., Sushch, I., Sutcliffe, P., Sykes, J., Szanecki, M., Szepieniec, T., Szwarnog, P., Tacchini, A., Tachihara, K., Tagliaferri, G., Tajima, H., Takahashi, H., Takahashi, K., Takahashi, M., Takalo, L., Takami, S., Takata, J., Takeda, J., Talbot, G., Tam, T., Tanaka, M., Tanaka, S., Tanaka, T., Tanaka, Y., Tanci, C., Tanigawa, S., Tavani, M., Tavecchio, F., Tavernet, J. -P., Tayabaly, K., Taylor, A., Tejedor, L. A., Telezhinsky, I., Temme, F., Temnikov, P., Tenzer, C., Terada, Y., Terrazas, J. C., Terrier, R., Terront, D., Terzic, T., Tescaro, D., Teshima, M., Testa, V., Tezier, D., Thayer, J., Thornhill, J., Thoudam, S., Thuermann, D., Tibaldo, L., Tiengo, A., Timpanaro, M. C., Tiziani, D., Tluczykont, M., Peixoto, C. J. Todero, Tokanai, F., Tokarz, M., Toma, K., Tomastik, J., Tomono, Y., Tonachini, A., Tonev, D., Torii, K., Tornikoski, M., Torres, D. F., Torres, M., Torresi, E., Toso, G., Tosti, G., Totani, T., Tothill, N., Toussenel, F., Tovmassian, G., Toyama, T., Travnicek, P., Trichard, C., Trifoglio, M., Pujadas, I. Troyano, Trzeciak, M., Tsinganos, K., Tsujimoto, S., Tsuru, T., Uchiyama, Y., Umana, G., Umetsu, Y., Upadhya, S. S., Uslenghi, M., Vagelli, V., Vagnetti, F., Valdes-Galicia, J., Valentino, M., Vallania, P., Valore, L., van Driel, W., van Eldik, C., van Soelen, B., Vandenbroucke, J., Vanderwalt, J., Vasileiadis, G., Vassiliev, V., Vázquez, J. R., Acosta, M. L. Vázquez, Vecchi, M., Vega, A., Vegas, I., Veitch, P., Venault, P., Venema, L., Venter, C., Vercellone, S., Vergani, S., Verma, K., Verzi, V., Vettolani, G. P., Veyssiere, C., Viana, A., Viaux, N., Vicha, J., Vigorito, C., Vincent, P., Vincent, S., Vink, J., Vittorini, V., Vlahakis, N., Vlahos, L., Voelk, H., Voisin, V., Vollhardt, A., Volpicelli, A., von Brand, H., Vorobiov, S., Vovk, I., Vrastil, M., Vu, L. V., Vuillaume, T., Wagner, R., Wagner, S. J., Wakely, S. P., Walstra, T., Walter, R., Walther, T., Ward, J. E., Ward, M., Warda, K., Warren, D., Wassberg, S., Watson, J. J., Wawer, P., Wawrzaszek, R., Webb, N., Wegner, P., Weiner, O., Weinstein, A., Wells, R., Werner, F., Wetteskind, H., White, M., White, R., Więcek, M., Wierzcholska, A., Wiesand, S., Wijers, R., Wilcox, P., Wild, N., Wilhelm, A., Wilkinson, M., Will, M., Williams, D. A., Williams, J. T., Willingale, R., Wilson, N., Winde, M., Winiarski, K., Winkler, H., Winter, M., Wischnewski, R., Witt, E., Wojcik, P., Wolf, D., Wood, M., Wörnlein, A., Wu, E., Wu, T., Yadav, K. K., Yamamoto, H., Yamamoto, T., Yamane, N., Yamazaki, R., Yanagita, S., Yang, L., Yelos, D., Yoshida, A., Yoshida, M., Yoshida, T., Yoshiike, S., Yoshikoshi, T., Yu, P., Zabalza, V., Zaborov, D., Zacharias, M., Zaharijas, G., Zajczyk, A., Zampieri, L., Zandanel, F., Sanchez, R. Zanmar, Zaric, D., Zavrtanik, D., Zavrtanik, M., Zdziarski, A., Zech, A., Zechlin, H., Zhao, A., Zhdanov, V., Ziegler, A., Ziemann, J., Ziętara, K., Zink, A., Ziółkowski, J., Zitelli, V., Zoli, A., Zorn, J., and Żychowski, P.
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Astrophysics - High Energy Astrophysical Phenomena - Abstract
List of contributions from the Cherenkov Telescope Array (CTA) Consortium presented at the 6th International Symposium on High-Energy Gamma-Ray Astronomy (Gamma 2016), July 11-15, 2016, in Heidelberg, Germany., Comment: Index of CTA conference proceedings for the Gamma 2016, Heidelberg, Germany
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- 2016
80. Deciphering the bipolar planetary nebula Abell 14 with 3D ionization and morphological studies
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Akras, S., Clyne, N., Boumis, P., Monteiro, H., Gonçalves, D. R., Redman, M. P., and Williams, S.
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Astrophysics - Solar and Stellar Astrophysics ,Astrophysics - Astrophysics of Galaxies - Abstract
Abell 14 is a poorly studied object despite being considered a born again planetary nebula. We performed a detailed study of its 3D morphology and ionization structure using the SHAPE and MOCASSIN codes. We found that Abell 14 is a highly evolved, bipolar nebula with a kinematical age of $\sim$19,400 yr for a distance of 4 kpc. The high He abundance, and N/O ratio indicate a progenitor of 5 $M_{\odot}$ that has experienced the third dredge-up and hot bottom burning phases. The stellar parameters of the central source reveal a star at a highly evolved stage near to the white dwarf cooling track, being inconsistent with the born again scenario. The nebula shows unexpectedly strong [N I] $\lambda 5200$ and [O I] $\lambda 6300$ emission lines indicating possible shock interactions. Abell 14 appears to be a member of a small group of highly evolved, extreme Type-I PNe. The members of this group lie at the lower-left corner of the PNe regime on the [N II]/H$\alpha$ vs. [S II]/H$\alpha$ diagnostic diagram, where shock--excited regions/objects are also placed. The low luminosity of their central stars, in conjunction with the large physical size of the nebulae, result in a very low photo-ionization rate, which can make any contribution of shock interaction easily perceptible, even for small velocities., Comment: 12 pages, 9 figures and 4 tables, accepted for publication in MNRAS
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- 2016
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81. Phosphonium-based ionic liquids as additives in calcium/lithium greases
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García Tuero, A., Bartolomé, M., Gonçalves, D., Viesca, J.L., Fernández-González, A., Seabra, J.H.O., and Hernández Battez, A.
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- 2021
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82. Mobile Application for Aid in Identifying Fall Risk in Elderly: App Fisioberg
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Gonçalves, D. C., primary, Pinto, F. P., additional, and Magalhães, D. S. F., additional
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- 2022
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83. ANTECEDENTES DA COMPRA POR IMPULSO: UMA ANÁLISE COM CONSUMIDORES DA SHOPEE
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MELO, M. M., primary, GONÇALVES, D. A., additional, and VILAS BOAS, L. H. B., additional
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- 2022
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84. FILO DINOFLAGELLATA
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Pinheiro, J. V, primary, Soares, D. C, additional, Narciso, C. S, additional, Gonçalves, D. M, additional, and Da Silva, C. C, additional
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- 2022
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85. Greases additised with phosphonium-based ionic liquids - Part I: Rheology, lubricant film thickness and Stribeck curves
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Bartolomé, M., Gonçalves, D., Tuero, A. García, González, R., Battez, A. Hernández, and Seabra, J.H.O.
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- 2021
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86. Integrative phylogenetic, phylogeographic and morphological characterisation of the Unio crassus species complex reveals cryptic diversity with important conservation implications
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Lopes-Lima, M., Geist, J., Egg, S., Beran, L., Bikashvili, A., Van Bocxlaer, B., Bogan, A. E., Bolotov, I. N., Chelpanovskaya, O. A., Douda, K., Fernandes, V., Gomes-dos-Santos, A., Gonçalves, D. V., Gürlek, M. E., Johnson, N. A., Karaouzas, I., Kebapçı, Ü., Kondakov, A. V., Kuehn, R., Lajtner, J., Mumladze, L., Nagel, K. -O, Neubert, E., Österling, Martin, Pfeiffer, J., Prié, V., Riccardi, N., Sell, J., Schneider, LD., Shumka, S., Sîrbu, I., Skujienė, G., Smith, CH., Sousa, R., Stöckl, K., Taskinen, J., Teixeira, A., Todorov, M., Trichkova, T., Urbańska, M., Välilä, S., Varandas, S., Veríssimo, J., Vikhrev, I. V., Woschitz, G., Zając, K., Zając, T., Zanatta, D., Zieritz, A., Zogaris, S., Froufe, E., Lopes-Lima, M., Geist, J., Egg, S., Beran, L., Bikashvili, A., Van Bocxlaer, B., Bogan, A. E., Bolotov, I. N., Chelpanovskaya, O. A., Douda, K., Fernandes, V., Gomes-dos-Santos, A., Gonçalves, D. V., Gürlek, M. E., Johnson, N. A., Karaouzas, I., Kebapçı, Ü., Kondakov, A. V., Kuehn, R., Lajtner, J., Mumladze, L., Nagel, K. -O, Neubert, E., Österling, Martin, Pfeiffer, J., Prié, V., Riccardi, N., Sell, J., Schneider, LD., Shumka, S., Sîrbu, I., Skujienė, G., Smith, CH., Sousa, R., Stöckl, K., Taskinen, J., Teixeira, A., Todorov, M., Trichkova, T., Urbańska, M., Välilä, S., Varandas, S., Veríssimo, J., Vikhrev, I. V., Woschitz, G., Zając, K., Zając, T., Zanatta, D., Zieritz, A., Zogaris, S., and Froufe, E.
- Abstract
The global decline of freshwater mussels and their crucial ecological services highlight the need to understand their phylogeny, phylogeography and patterns of genetic diversity to guide conservation efforts. Such knowledge is urgently needed for Unio crassus, a highly imperilled species originally widespread throughout Europe and southwest Asia. Recent studies have resurrected several species from synonymy based on mitochondrial data, revealing U. crassus to be a complex of cryptic species. To address long-standing taxonomic uncertainties hindering effective conservation, we integrate morphometric, phylogenetic, and phylogeographic analyses to examine species diversity within the U. crassus complex across its entire range. Phylogenetic analyses were performed using cytochrome c oxidase subunit I (815 specimens from 182 populations) and, for selected specimens, whole mitogenome sequences and Anchored Hybrid Enrichment (AHE) data on ∼ 600 nuclear loci. Mito-nuclear discordance was detected, consistent with mitochondrial DNA gene flow between some species during the Pliocene and Pleistocene. Fossil-calibrated phylogenies based on AHE data support a Mediterranean origin for the U. crassus complex in the Early Miocene. The results of our integrative approach support 12 species in the group: the previously recognised Unio bruguierianus, Unio carneus, Unio crassus, Unio damascensis, Unio ionicus, Unio sesirmensis, and Unio tumidiformis, and the reinstatement of five nominal taxa: Unio desectus stat. rev., Unio gontierii stat. rev., Unio mardinensis stat. rev., Unio nanus stat. rev., and Unio vicarius stat. rev. Morphometric analyses of shell contours reveal important morphospace overlaps among these species, highlighting cryptic, but geographically structured, diversity. The distribution, taxonomy, phylogeography, and conservation of each species are succinctly described.
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- 2024
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87. Features of collisionless turbulence in the intracluster medium from simulated Faraday Rotation maps
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Nakwacki, M. S., Kowal, G., Santos-Lima, R., Pino, E. M. de Gouveia Dal, and Falceta-Gonçalves, D. A.
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Astrophysics - Cosmology and Nongalactic Astrophysics ,Astrophysics - Astrophysics of Galaxies - Abstract
Observations of the intracluster medium (ICM) in galaxy clusters suggest for the presence of turbulence and the magnetic fields existence has been proved through observations of Faraday Rotation and synchrotron emission. The ICM is also known to be filled by a rarefied weakly collisional plasma. In this work we study the possible signatures left on Faraday Rotation maps by collisionless instabilities. For this purpose we use a numerical approach to investigate the dynamics of the turbulence in collisionless plasmas based on an magnetohydrodynamical (MHD) formalism taking into account different levels of pressure anisotropy. We consider models covering the sub/super-Alfv\'enic and trans/supersonic regimes, one of them representing the fiducial conditions corresponding to the ICM. From the simulated models we compute Faraday Rotation maps and analyze several statistical indicators in order to characterize the magnetic field structure and compare the results obtained with the collisionless model to those obtained using standard collisional MHD framework. We find that important imprints of the pressure anisotropy prevails in the magnetic field and also manifest in the associated Faraday Rotation maps which evidence smaller correlation lengths in the collisionless MHD case. These points are remarkably noticeable for the case mimicking the conditions prevailing in ICM. Nevertheless, in this study we have neglected the decrease of pressure anisotropy due to the feedback of the instabilities that naturally arise in collisionless plasmas at small scales. This decrease may not affect the statistical imprint differences described above, but should be examined elsewhere., Comment: 24 pages, 15 figures, MNRAS accepted
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- 2015
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88. Magnetic fields, non-thermal radiation and particle acceleration in colliding winds of WR-O stars
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Falceta-Goncalves, D.
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Astrophysics - High Energy Astrophysical Phenomena ,Astrophysics - Solar and Stellar Astrophysics - Abstract
Non-thermal emission has been detected in WR-stars for many years at long wavelengths spectral range, in general attributed to synchrotron emission. Two key ingredients are needed to explain such emissions, namely magnetic fields and relativistic particles. Particles can be accelerated to relativistic speeds by Fermi processes at strong shocks. Therefore, strong synchrotron emission is usually attributed to WR binarity. The magnetic field may also be amplified at shocks, however the actual picture of the magnetic field geometry, intensity, and its role on the acceleration of particles at WR binary systems is still unclear. In this work we discuss the recent developments in MHD modelling of wind-wind collision regions by means of numerical simulations, and the coupled particle acceleration processes related., Comment: Proceedings of the International Workshop on Wolf-Rayet Stars, held in Potsdam/Germany, 1-5 June 2015. Universit\"atsverlag Potsdam. Editors W.-R. Hamann, A. Sander, and H. Todt
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- 2015
89. Evidence for a [WR] or WEL-type binary nucleus in the bipolar planetary nebula Vy 1-2
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Akras, S., Boumis, P., Meaburn, J., Alikakos, J., López, J. A., and Gonçalves, D. R.
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Astrophysics - Solar and Stellar Astrophysics - Abstract
We present high-dispersion spectroscopic data of the compact planetary nebula Vy 1-2, where high expansion velocities up to 100 km/s are found in the Ha, [N II] and [O III] emission lines. HST images reveal a bipolar structure. Vy 1-2 displays a bright ring-like structure with a size of 2.4"x3.2" and two faint bipolar lobes in the west-east direction. A faint pair of knots is also found, located almost symmetrically on opposite sides of the nebula at PA=305 degrees. Furthermore, deep low-dispersion spectra are also presented and several emission lines are detected for the first time in this nebula, such as the doublet [Cl III] 5517, 5537 A, [K IV] 6101 A, C II 6461 A, the doublet C IV 5801, 5812 A. By comparison with the solar abundances, we find enhanced N, depleted C and solar O. The central star must have experienced the hot bottom burning (CN-cycle) during the 2nd dredge-up phase, implying a progenitor star of higher than 3 solar masses. The very low C/O and N/O abundance ratios suggest a likely post-common envelope close binary system. A simple spherically symmetric geometry with either a blackbody or a H-deficient stellar atmosphere model is not able to reproduce the ionisation structure of Vy 1-2. The effective temperature and luminosity of its central star indicate a young nebula located at a distance of ~9.7 kpc with an age of ~3500 years. The detection of stellar emission lines, C II 6461 A, the doublet C IV {\lambda}{\lambda} 5801, 5812 A and O III 5592 A, emitted from a H-deficient star, indicates the presence of a late-type Wolf-Rayet or a WEL type central star., Comment: 20 pages, 18 figures, accepted for publication in MNRAS
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- 2015
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90. Fast magnetic field amplification in the early Universe: growth of collisionless plasma instabilities in turbulent media
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Falceta-Goncalves, D. and Kowal, G.
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Astrophysics - Cosmology and Nongalactic Astrophysics ,Astrophysics - High Energy Astrophysical Phenomena ,Physics - Fluid Dynamics - Abstract
In this work we report a numerical study of the cosmic magnetic field amplification due to collisionless plasma instabilities. The collisionless magnetohydrodynamic equations derived account for the pressure anisotropy that leads, in specific conditions, to the firehose and mirror instabilities. We study the time evolution of seed fields in turbulence under the influence of such instabilities. An approximate analytical time evolution of magnetic field is provided. The numerical simulations and the analytical predictions are compared. We found that i) amplification of magnetic field was efficient in firehose unstable turbulent regimes, but not in the mirror unstable models, ii) the growth rate of the magnetic energy density is much faster than the turbulent dynamo, iii) the efficient amplification occurs at small scales. The analytical prediction for the correlation between the growth timescales with pressure anisotropy ratio is confirmed by the numerical simulations. These results reinforce the idea that pressure anisotropies - driven naturally in a turbulent collisionless medium, e.g. the intergalactic medium -, could efficiently amplify the magnetic field in the early Universe (post-recombination era), previous to the collapse of the first large-scale gravitational structures. This mechanism, though fast for the small scale fields ($\sim$kpc scales), is however unable to provide relatively strong magnetic fields at large scales. Other mechanisms that were not accounted here (e.g., collisional turbulence once instabilities are quenched, velocity shear, or gravitationally induced inflows of gas into galaxies and clusters) could operate afterwards to build up large scale coherent field structures in the long time evolution., Comment: ApJ accepted
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- 2015
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91. The Staggered Quantum Walk Model
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Portugal, R., Santos, R. A. M., Fernandes, T. D., and Gonçalves, D. N.
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Quantum Physics - Abstract
There are at least three models of discrete-time quantum walks (QWs) on graphs currently under active development. In this work we focus on the equivalence of two of them, known as Szegedy's and staggered QWs. We give a formal definition of the staggered model and discuss generalized versions for searching marked vertices. Using this formal definition, we prove that any instance of Szegedy's model is equivalent to an instance of the staggered model. On the other hand, we show that there are instances of the staggered model that cannot be cast into Szegedy's framework. Our analysis also works when there are marked vertices. We show that Szegedy's spatial search algorithms can be converted into search algorithms in staggered QWs. We take advantage of the similarity of those models to define the quantum hitting time in the staggered model and to describe a method to calculate the eigenvalues and eigenvectors of the evolution operator of staggered QWs., Comment: 21 pages, 9 figures
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- 2015
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92. GHIGLS: HI mapping at intermediate Galactic latitude using the Green Bank Telescope
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Martin, P. G., Blagrave, K. P. M., Lockman, Felix J., Goncalves, D. Pinheiro, Boothroyd, A. I., Joncas, G., Miville-Deschenes, M. -A., and Stephan, G.
- Subjects
Astrophysics - Astrophysics of Galaxies - Abstract
This paper introduces the data cubes from GHIGLS, deep Green Bank Telescope surveys of the 21-cm line emission of HI in 37 targeted fields at intermediate Galactic latitude. The GHIGLS fields together cover over 1000 square degrees at 9.55' spatial resolution. The HI spectra have an effective velocity resolution about 1.0 km/s and cover at least -450 < v < +250 km/s. GHIGLS highlights that even at intermediate Galactic latitude the interstellar medium is very complex. Spatial structure of the HI is quantified through power spectra of maps of the column density, NHI. For our featured representative field, centered on the North Ecliptic Pole, the scaling exponents in power-law representations of the power spectra of NHI maps for low, intermediate, and high velocity gas components (LVC, IVC, and HVC) are -2.86 +/- 0.04, -2.69 +/- 0.04, and -2.59 +/- 0.07, respectively. After Gaussian decomposition of the line profiles, NHI maps were also made corresponding to the narrow-line and broad-line components in the LVC range; for the narrow-line map the exponent is -1.9 +/- 0.1, reflecting more small scale structure in the cold neutral medium (CNM). There is evidence that filamentary structure in the HI CNM is oriented parallel to the Galactic magnetic field. The power spectrum analysis also offers insight into the various contributions to uncertainty in the data. The effect of 21-cm line opacity on the GHIGLS NHI maps is estimated., Comment: Accepted for publication in The Astrophysical Journal, 2015 July 16. 32 pages, 21 figures (Fig. 10 new). Minor revisions from review, particularly Section 8 and Appendix C; results unchanged. Additional surveys added and made available; new Appendix B. Added descriptions of available FITS files and links to four illustrative movies on enhanced GHIGLS archive (www.cita.utoronto.ca/GHIGLS/)
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- 2015
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93. Planck intermediate results. XXXV. Probing the role of the magnetic field in the formation of structure in molecular clouds
- Author
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Planck Collaboration, Ade, P. A. R., Aghanim, N., Alves, M. I. R., Arnaud, M., Arzoumanian, D., Ashdown, M., Aumont, J., Baccigalupi, C., Banday, A. J., Barreiro, R. B., Bartolo, N., Battaner, E., Benabed, K., Benoît, A., Benoit-Lévy, A., Bernard, J. -P., Bersanelli, M., Bielewicz, P., Bock, J. J., Bonavera, L., Bond, J. R., Borrill, J., Bouchet, F. R., Boulanger, F., Bracco, A., Burigana, C., Calabrese, E., Cardoso, J. -F., Catalano, A., Chiang, H. C., Christensen, P. R., Colombo, L. P. L., Combet, C., Couchot, F., Crill, B. P., Curto, A., Cuttaia, F., Danese, L., Davies, R. D., Davis, R. J., de Bernardis, P., de Rosa, A., de Zotti, G., Delabrouille, J., Dickinson, C., Diego, J. M., Dole, H., Donzelli, S., Doré, O., Douspis, M., Ducout, A., Dupac, X., Efstathiou, G., Elsner, F., Enßlin, T. A., Eriksen, H. K., Falceta-Gonçalves, D., Falgarone, E., Ferrière, K., Finelli, F., Forni, O., Frailis, M., Fraisse, A. A., Franceschi, E., Frejsel, A., Galeotta, S., Galli, S., Ganga, K., Ghosh, T., Giard, M., Gjerløw, E., González-Nuevo, J., Górski, K. M., Gregorio, A., Gruppuso, A., Gudmundsson, J. E., Guillet, V., Harrison, D. L., Helou, G., Hennebelle, P., Henrot-Versillé, S., Hernández-Monteagudo, C., Herranz, D., Hildebrandt, S. R., Hivon, E., Holmes, W. A., Hornstrup, A., Huffenberger, K. M., Hurier, G., Jaffe, A. H., Jaffe, T. R., Jones, W. C., Juvela, M., Keihänen, E., Keskitalo, R., Kisner, T. S., Knoche, J., Kunz, M., Kurki-Suonio, H., Lagache, G., Lamarre, J. -M., Lasenby, A., Lattanzi, M., Lawrence, C. R., Leonardi, R., Levrier, F., Liguori, M., Lilje, P. B., Linden-Vørnle, M., López-Caniego, M., Lubin, P. M., Macías-Pérez, J. F., Maino, D., Mandolesi, N., Mangilli, A., Maris, M., Martin, P. G., Martínez-González, E., Masi, S., Matarrese, S., Melchiorri, A., Mendes, L., Mennella, A., Migliaccio, M., Miville-Deschênes, M. -A., Moneti, A., Montier, L., Morgante, G., Mortlock, D., Munshi, D., Murphy, J. A., Naselsky, P., Nati, F., Netterfield, C. B., Noviello, F., Novikov, D., Novikov, I., Oppermann, N., Oxborrow, C. A., Pagano, L., Pajot, F., Paladini, R., Paoletti, D., Pasian, F., Perotto, L., Pettorino, V., Piacentini, F., Piat, M., Pierpaoli, E., Pietrobon, D., Plaszczynski, S., Pointecouteau, E., Polenta, G., Ponthieu, N., Pratt, G. W., Prunet, S., Puget, J. -L., Rachen, J. P., Reinecke, M., Remazeilles, M., Renault, C., Renzi, A., Ristorcelli, I., Rocha, G., Rossetti, M., Roudier, G., Rubiño-Martín, J. A., Rusholme, B., Sandri, M., Santos, D., Savelainen, M., Savini, G., Scott, D., Soler, J. D., Stolyarov, V., Sudiwala, R., Sutton, D., Suur-Uski, A. -S., Sygnet, J. -F., Tauber, J. A., Terenzi, L., Toffolatti, L., Tomasi, M., Tristram, M., Tucci, M., Umana, G., Valenziano, L., Valiviita, J., Van Tent, B., Vielva, P., Villa, F., Wade, L. A., Wandelt, B. D., Wehus, I. K., Ysard, N., Yvon, D., and Zonca, A.
- Subjects
Astrophysics - Astrophysics of Galaxies - Abstract
Within ten nearby (d < 450 pc) Gould Belt molecular clouds we evaluate statistically the relative orientation between the magnetic field projected on the plane of sky, inferred from the polarized thermal emission of Galactic dust observed by Planck at 353 GHz, and the gas column density structures, quantified by the gradient of the column density, $N_H$. The selected regions, covering several degrees in size, are analyzed at an effective angular resolution of 10' FWHM, thus sampling physical scales from 0.4 to 40 pc in the nearest cloud. The column densities in the selected regions range from $N_H \approx 10^{21}$ to $10^{23}$ cm$^{-2}$, and hence they correspond to the bulk of the molecular clouds. The relative orientation is evaluated pixel by pixel and analyzed in bins of column density using the novel statistical tool called "Histogram of Relative Orientations". Throughout this study, we assume that the polarized emission observed by Planck at 353 GHz is representative of the projected morphology of the magnetic field in each region, i.e., we assume a constant dust grain alignment efficiency, independent of the local environment. Within most clouds we find that the relative orientation changes progressively with increasing $N_H$, from preferentially parallel or having no preferred orientation to preferentially perpendicular. In simulations of magnetohydrodynamic turbulence in molecular clouds this trend in relative orientation is a signature of Alfv\'enic or sub-Alfv\'enic turbulence, implying that the magnetic field is significant for the gas dynamics at the scales probed by Planck. We compare the deduced magnetic field strength with estimates we obtain from other methods and discuss the implications of the Planck observations for the general picture of molecular cloud formation and evolution., Comment: 28 pages, 20 figures. A&A accepted. Corresponding author: J.D. Soler
- Published
- 2015
- Full Text
- View/download PDF
94. Anti-fibrotic effect of a FGF ligands trap in pulmonary fibrosis
- Author
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Gonçalves, D., primary, Scribe, C., additional, Dellugat, P., additional, Rignol, G., additional, Ghilain, C., additional, Marsault, R., additional, Etasse, L., additional, Garcia-Pizarro, J., additional, Mari, B., additional, Czech, C., additional, and Herbert, C., additional
- Published
- 2024
- Full Text
- View/download PDF
95. Ciência e esoterismo: o elo perdido
- Author
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GONÇALVES, D., primary
- Published
- 2024
- Full Text
- View/download PDF
96. Planck intermediate results
- Author
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Ade, PAR, Aghanim, N, Alves, MIR, Arnaud, M, Arzoumanian, D, Ashdown, M, Aumont, J, Baccigalupi, C, Banday, AJ, Barreiro, RB, Bartolo, N, Battaner, E, Benabed, K, Benoît, A, Benoit-Lévy, A, Bernard, J-P, Bersanelli, M, Bielewicz, P, Bock, JJ, Bonavera, L, Bond, JR, Borrill, J, Bouchet, FR, Boulanger, F, Bracco, A, Burigana, C, Calabrese, E, Cardoso, J-F, Catalano, A, Chiang, HC, Christensen, PR, Colombo, LPL, Combet, C, Couchot, F, Crill, BP, Curto, A, Cuttaia, F, Danese, L, Davies, RD, Davis, RJ, de Bernardis, P, de Rosa, A, de Zotti, G, Delabrouille, J, Dickinson, C, Diego, JM, Dole, H, Donzelli, S, Doré, O, Douspis, M, Ducout, A, Dupac, X, Efstathiou, G, Elsner, F, Enßlin, TA, Eriksen, HK, Falceta-Gonçalves, D, Falgarone, E, Ferrière, K, Finelli, F, Forni, O, Frailis, M, Fraisse, AA, Franceschi, E, Frejsel, A, Galeotta, S, Galli, S, Ganga, K, Ghosh, T, Giard, M, Gjerløw, E, González-Nuevo, J, Górski, KM, Gregorio, A, Gruppuso, A, Gudmundsson, JE, Guillet, V, Harrison, DL, Helou, G, Hennebelle, P, Henrot-Versillé, S, Hernández-Monteagudo, C, Herranz, D, Hildebrandt, SR, Hivon, E, Holmes, WA, Hornstrup, A, Huffenberger, KM, Hurier, G, Jaffe, AH, Jaffe, TR, Jones, WC, Juvela, M, Keihänen, E, Keskitalo, R, Kisner, TS, Knoche, J, Kunz, M, Kurki-Suonio, H, and Lagache, G
- Subjects
Space Sciences ,Particle and High Energy Physics ,Astronomical Sciences ,Physical Sciences ,ISM: general ,ISM: magnetic fields ,ISM: clouds ,dust ,extinction ,submillimeter: ISM ,infrared: ISM ,astro-ph.GA ,Astronomical and Space Sciences ,Astronomy & Astrophysics ,Astronomical sciences ,Particle and high energy physics ,Space sciences - Abstract
Within ten nearby (d < 450 pc) Gould belt molecular clouds we evaluate statistically the relative orientation between the magnetic field projected on the plane of sky, inferred from the polarized thermal emission of Galactic dust observed by Planck at 353 GHz, and the gas column density structures, quantified by the gradient of the column density, NH. The selected regions, covering several degrees in size, are analysed at an effective angular resolution of 10′ FWHM, thus sampling physical scales from 0.4 to 40 pc in the nearest cloud. The column densities in the selected regions range from NH ≈ 1021 to 1023 cm-2, and hence they correspond to the bulk of the molecular clouds. The relative orientation is evaluated pixel by pixel and analysed in bins of column density using the novel statistical tool called "histogram of relative orientations". Throughout this study, we assume that the polarized emission observed by Planck at 353 GHz is representative of the projected morphology of the magnetic field in each region, i.e., we assume a constant dust grain alignment efficiency, independent of the local environment. Within most clouds we find that the relative orientation changes progressively with increasing NH, from mostly parallel or having no preferred orientation to mostly perpendicular. In simulations of magnetohydrodynamic turbulence in molecular clouds this trend in relative orientation is a signature of Alfvénic or sub-Alfvénic turbulence, implying that the magnetic field is significant for the gas dynamics at the scales probed by Planck. We compare the deduced magnetic field strength with estimates we obtain from other methods and discuss the implications of the Planck observations for the general picture of molecular cloud formation and evolution.
- Published
- 2016
97. Planck intermediate results: XXXV. Probing the role of the magnetic field in the formation of structure in molecular clouds
- Author
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Ade, PAR, Aghanim, N, Alves, MIR, Arnaud, M, Arzoumanian, D, Ashdown, M, Aumont, J, Baccigalupi, C, Banday, AJ, Barreiro, RB, Bartolo, N, Battaner, E, Benabed, K, Benoît, A, Benoit-Lévy, A, Bernard, JP, Bersanelli, M, Bielewicz, P, Bock, JJ, Bonavera, L, Bond, JR, Borrill, J, Bouchet, FR, Boulanger, F, Bracco, A, Burigana, C, Calabrese, E, Cardoso, JF, Catalano, A, Chiang, HC, Christensen, PR, Colombo, LPL, Combet, C, Couchot, F, Crill, BP, Curto, A, Cuttaia, F, Danese, L, Davies, RD, Davis, RJ, De Bernardis, P, De Rosa, A, De Zotti, G, Delabrouille, J, Dickinson, C, Diego, JM, Dole, H, Donzelli, S, Doré, O, Douspis, M, Ducout, A, Dupac, X, Efstathiou, G, Elsner, F, Enßlin, TA, Eriksen, HK, Falceta-Gonçalves, D, Falgarone, E, Ferrière, K, Finelli, F, Forni, O, Frailis, M, Fraisse, AA, Franceschi, E, Frejsel, A, Galeotta, S, Galli, S, Ganga, K, Ghosh, T, Giard, M, Gjerløw, E, González-Nuevo, J, Górski, KM, Gregorio, A, Gruppuso, A, Gudmundsson, JE, Guillet, V, Harrison, DL, Helou, G, Hennebelle, P, Henrot-Versillé, S, Hernández-Monteagudo, C, Herranz, D, Hildebrandt, SR, Hivon, E, Holmes, WA, Hornstrup, A, Huffenberger, KM, Hurier, G, Jaffe, AH, Jaffe, TR, Jones, WC, Juvela, M, Keihänen, E, Keskitalo, R, Kisner, TS, Knoche, J, Kunz, M, Kurki-Suonio, H, and Lagache, G
- Subjects
ISM: general ,ISM: magnetic fields ,ISM: clouds ,dust ,extinction ,submillimeter: ISM ,infrared: ISM ,astro-ph.GA ,Astronomy & Astrophysics ,Astronomical and Space Sciences - Abstract
Within ten nearby (d < 450 pc) Gould belt molecular clouds we evaluate statistically the relative orientation between the magnetic field projected on the plane of sky, inferred from the polarized thermal emission of Galactic dust observed by Planck at 353 GHz, and the gas column density structures, quantified by the gradient of the column density, NH. The selected regions, covering several degrees in size, are analysed at an effective angular resolution of 10′ FWHM, thus sampling physical scales from 0.4 to 40 pc in the nearest cloud. The column densities in the selected regions range from NH ≈ 1021 to 1023 cm-2, and hence they correspond to the bulk of the molecular clouds. The relative orientation is evaluated pixel by pixel and analysed in bins of column density using the novel statistical tool called "histogram of relative orientations". Throughout this study, we assume that the polarized emission observed by Planck at 353 GHz is representative of the projected morphology of the magnetic field in each region, i.e., we assume a constant dust grain alignment efficiency, independent of the local environment. Within most clouds we find that the relative orientation changes progressively with increasing NH, from mostly parallel or having no preferred orientation to mostly perpendicular. In simulations of magnetohydrodynamic turbulence in molecular clouds this trend in relative orientation is a signature of Alfvénic or sub-Alfvénic turbulence, implying that the magnetic field is significant for the gas dynamics at the scales probed by Planck. We compare the deduced magnetic field strength with estimates we obtain from other methods and discuss the implications of the Planck observations for the general picture of molecular cloud formation and evolution.
- Published
- 2016
98. Ambient magnetic field amplification in shock fronts of relativistic jets: an application to GRB afterglows
- Author
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da Silva, G. Rocha, Falceta-Goncalves, D., Kowal, G., and Pino, E. M. de Gouveia Dal
- Subjects
Astrophysics - High Energy Astrophysical Phenomena - Abstract
Strong downstream magnetic fields of order of $\sim 1$G, with large correlation lengths, are believed to cause the large synchrotron emission at the afterglow phase of gamma ray bursts (GRBs). Despite of the recent theoretical efforts, models have failed to fully explain the amplification of the magnetic field, particularly in a matter dominated scenario. We revisit the problem by considering the synchrotron emission to occur at the expanding shock front of a weakly magnetized relativistic jet over a magnetized surrounding medium. Analytical estimates and a number of high resolution 2D relativistic magneto-hydrodynamical (RMHD) simulations are provided. Jet opening angles of $\theta = 0^{\circ} - 20^{\circ}$, and ambient to jet density ratios of $10^{-4} - 10^2$ were considered. We found that most of the amplification is due to compression of the ambient magnetic field at the contact discontinuity between the reverse and forward shocks at the jet head, with substantial pile-up of the magnetic field lines as the jet propagates sweeping the ambient field lines. The pile-up is maximum for $\theta \rightarrow 0$, decreasing with $\theta$, but larger than in the spherical blast problem. Values obtained for certain models are able to explain the observed intensities. The maximum correlation lengths found for such strong fields is of $l_{\rm corr} \leq 10^{14}$ cm, $2 - 6$ orders of magnitude larger than the found in previous works., Comment: mnras accepted
- Published
- 2014
- Full Text
- View/download PDF
99. The onset of large scale turbulence in the interstellar medium of spiral galaxies
- Author
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Falceta-Goncalves, D., Bonnell, I., Kowal, G., Lepine, J., and Braga, C.
- Subjects
Astrophysics - Astrophysics of Galaxies - Abstract
Turbulence is ubiquitous in the interstellar medium (ISM) of the Milky Way and other spiral galaxies. The energy source for this turbulence has been much debated with many possible origins proposed. The universality of turbulence, its reported large-scale driving, and that it occurs also in starless molecular clouds, challenges models invoking any stellar source. A more general process is needed to explain the observations. In this work we study the role of galactic spiral arms. This is accomplished by means of three-dimensional hydrodynamical simulations which follow the dynamical evolution of interstellar diffuse clouds (100cm-3) interacting with the gravitational potential field of the spiral pattern. We find that the tidal effects of the arm's potential on the cloud result in internal vorticity, fragmentation and hydrodynamical instabilities. The triggered turbulence result in large-scale driving, on sizes of the ISM inhomogeneities, i.e. as large as 100pc, and efficiencies in converting potential energy into turbulence in the range 10 to 25 percent per arm crossing. This efficiency is much higher than those found in previous models. The statistics of the turbulence in our simulations are strikingly similar to the observed power spectrum and Larson scaling relations of molecular clouds and the general ISM. The dependency found from different models indicate that the ISM turbulence is mainly related to local spiral arm properties, such as its mass density and width. This correlation seems in agreement with recent high angular resolution observations of spiral galaxies, e.g. M51 and M33., Comment: MNRAS accepted
- Published
- 2014
- Full Text
- View/download PDF
100. Planetary nebulae: the universal mass-metallicity relation for Local Group dwarf galaxies and the chemistry of NGC 205
- Author
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Gonçalves, D. R., Magrini, Laura, Teodorescu, Ana M., and Carneiro, Carolina M.
- Subjects
Astrophysics - Astrophysics of Galaxies - Abstract
Here we study 16 planetary nebulae (PNe) in the dwarf irregular galaxy NGC 205 by using GMOS@Gemini spectra to derive their physical and chemical parameters. The chemical patterns and evolutionary tracks for 14 of our PNe suggest that there are no type I PNe among them. These PNe have an average oxygen abundance of 12+log(O/H)=8.08$\pm$0.28, progenitor masses of 2-2.5M$_{\odot}$ and thus were born ~1.0-1.7Gyr ago. Our results are in good agreement with previous PN studies in NGC 205. The present 12+log(O/H) is combined with our previous works and with the literature to study the PN metallicity trends of the Local Group (LG) dwarf galaxies, in an effort to establish the PN luminosity- and mass-metallicity relations (LZR and MZR) for the LG dwarf irregulars (dIrrs) and dwarf spheroidals (dSphs). Previous attempts to obtain such relations failed to provide correct conclusions because were based on limited samples (Richer & McCall 1995; Gon\c{c}calves et al. 2007). As far as we are able to compare stellar with nebular metallicities, our MZR is in very good agreement with the slope of the MZR recently obtained for LG dwarf galaxies using spectroscopic stellar metallicities (Kirby et al. 2013). Actually, we found that both dIrr and dSph galaxies follow the same MZR, at variance with the differences claimed in the past. Moreover our MZR is also consistent with the global MZR of star-forming galaxies, which span a wider stellar mass range ($\sim10^6$ - $\sim10^{11}$M$\odot$)., Comment: MNRAS in press
- Published
- 2014
- Full Text
- View/download PDF
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