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- ItemWarm ionized gas in the blue compact galaxy Haro 14 viewed by MUSE(Les Ulis : EDP Sciences, 2022) Cairós, L. M.; González-Pérez, J.N.; Weilbacher, P.M.; Manso Sainz, R.We investigate the warm ionized gas in the blue compact galaxy (BCG) Haro 14 by means of integral field spectroscopic observations taken with the Multi Unit Spectroscopic Explorer (MUSE) at the Very Large Telescope. The large field of view of MUSE and its unprecedented sensitivity enable observations of the galaxy nebular emission up to large galactocentric distances, even in the important but very faint [O i] λ6300 diagnostic line. This allowed us to trace the ionized gas morphology and ionization structure of Haro 14 up to kiloparsec scales and, for the first time, to accurately investigate the excitation mechanism operating in the outskirts of a typical BCG. The intensity and diagnostic maps reveal at least two highly distinct components of ionized gas: the bright central regions, mostly made of individual clumps, and a faint component which extends up to kiloparsec scales and consists of widespread diffuse emission, well-delineated filamentary structures, and faint knots. Noteworthy are the two curvilinear filaments extending up to 2 and 2.3 kpc southwest, which likely trace the edges of supergiant expanding bubbles driven by galactic outflows. We find that while the central clumps in Haro 14 are Hii-region complexes, the morphology and line ratios of the whole low-surface-brightness component are not compatible with star formation photoionization. In the spatially resolved emission-line-ratio diagnostic diagrams, spaxels above the maximum starburst line form the majority (∼75% and ∼50% in the diagnostic diagrams involving [O i] and [S ii] respectively). Moreover, our findings suggest that more than one alternative mechanism is ionizing the outer galaxy regions. The properties of the diffiuse component are consistent with ionization by diluted radiation and the large filaments and shells are most probably shocked areas at the edge of bubbles. The mechanism responsible for the ionization of the faint individual clumps observed in the galaxy periphery is more difficult to assess. These clumps could be the shocked debris of fragmented shells or regions where star formation is proceeding under extreme conditions.
- ItemThe European Solar Telescope(Les Ulis : EDP Sciences, 2022) Quintero Noda, C.; Schlichenmaier, R.; Bellot Rubio, L.R.; Löfdahl, M.G.; Khomenko, E.; Jurčák, J.; Leenaarts, J.; Kuckein, C.; González Manrique, S.J.; Gunár, S.; Nelson, C.J.; Giovannelli, L.; González, F.; González, J.B.; González-Cava, J.M.; González García, M.; Gömöry, P.; Gracia, F.; Grauf, B.; Greco, V.; Grivel, C.; de la Cruz Rodríguez, J.; Guerreiro, N.; Guglielmino, S.L.; Hammerschlag, R.; Hanslmeier, A.; Hansteen, V.; Heinzel, P.; Hernández-Delgado, A.; Hernández Suárez, E.; Hidalgo, S.L.; Hill, F.; Tziotziou, K.; Hizberger, J.; Hofmeister, S.; Jägers, A.; Janett, G.; Jarolim, R.; Jess, D.; Jiménez Mejías, D.; Jolissaint, L.; Kamlah, R.; Kapitán, J.; Tsiropoula, G.; Kašparová, J.; Keller, C.U.; Kentischer, T.; Kiselman, D.; Kleint, L.; Klvana, M.; Kontogiannis, I.; Krishnappa, N.; Kučera, A.; Labrosse, N.; Aulanier, G.; Lagg, A.; Landi Degl’Innocenti, E.; Langlois, M.; Lafon, M.; Laforgue, D.; Le Men, C.; Lepori, B.; Lepreti, F.; Lindberg, B.; Lilje, P.B.; Aboudarham, J.; López Ariste, A.; López Fernández, V.A.; López Jiménez, A.C.; López López, R.; Manso Sainz, R.; Marassi, A.; Marco de la Rosa, J.; Marino, J.; Marrero, J.; Martín, A.; Allegri, D.; Martín Gálvez, A.; Martín Hernando, Y.; Masciadri, E.; Martínez González, M.; Matta-Gómez, A.; Mato, A.; Mathioudakis, M.; Matthews, S.; Mein, P.; Merlos García, F.; Alsina Ballester, E.; Moity, J.; Montilla, I.; Molinaro, M.; Molodij, G.; Montoya, L.M.; Munari, M.; Murabito, M.; Núñez Cagigal, M.; Oliviero, M.; Orozco Suárez, D.; Amans, J.P.; Ortiz, A.; Padilla-Hernández, C.; Paéz Mañá, E.; Paletou, F.; Pancorbo, J.; Pastor Cañedo, A.; Pastor Yabar, A.; Peat, A.W.; Pedichini, F.; Peixinho, N.; Asensio Ramos, A.; Peñate, J.; Pérez de Taoro, A.; Peter, H.; Petrovay, K.; Piazzesi, R.; Pietropaolo, E.; Pleier, O.; Poedts, S.; Pötzi, W.; Podladchikova, T.; Bailén, F.J.; Prieto, G.; Quintero Nehrkorn, J.; Ramelli, R.; Ramos Sapena, Y.; Rasilla, J.L.; Reardon, K.; Rebolo, R.; Regalado Olivares, S.; Reyes García-Talavera, M.; Riethmüller, T.L.; Balaguer, M.; Rimmele, T.; Rodríguez Delgado, H.; Rodríguez González, N.; Rodríguez-Losada, J.A.; Rodríguez Ramos, L.F.; Romano, P.; Roth, M.; Rouppe van der Voort, L.; Rudawy, P.; Ruiz de Galarreta, C.; Baldini, V.; Rybák, J.; Salvade, A.; Sánchez-Capuchino, J.; Sánchez Rodríguez, M.L.; Sangiorgi, M.; Sayède, F.; Scharmer, G.; Scheiffelen, T.; Schmidt, W.; Schmieder, B.; Balthasar, H.; Scirè, C.; Scuderi, S.; Siegel, B.; Sigwarth, M.; Simões, P.J.A.; Snik, F.; Sliepen, G.; Sobotka, M.; Socas-Navarro, H.; Sola La Serna, P.; Barata, T.; Solanki, S. K.; Soler Trujillo, M.; Soltau, D.; Sordini, A.; Sosa Méndez, A.; Stangalini, M.; Steiner, O.; Stenflo, J.O.; Štěpán, J.; Strassmeier, K.G.; Barczynski, K.; Sudar, D.; Suematsu, Y.; Sütterlin, P.; Tallon, M.; Temmer, M.; Tenegi, F.; Tritschler, A.; Trujillo Bueno, J.; Turchi, A.; Utz, D.; Barreto Cabrera, M.; van Harten, G.; van Noort, M.; van Werkhoven, T.; Vansintjan, R.; Vaz Cedillo, J.J.; Vega Reyes, N.; Verma, M.; Veronig, A.M.; Viavattene, G.; Vitas, N.; Baur, A.; Vögler, A.; von der Lühe, O.; Volkmer, R.; Waldmann, T.A.; Walton, D.; Wisniewska, A.; Zeman, J.; Zeuner, F.; Zhang, L.Q.; Zuccarello, F.; Béchet, C.; Collados, M.; Beck, C.; Belío-Asín, M.; Bello-González, N.; Belluzzi, L.; Bentley, R.D.; Berdyugina, S.V.; Berghmans, D.; Berlicki, A.; Berrilli, F.; Berkefeld, T.; Bettonvil, F.; Bianda, M.; Bienes Pérez, J.; Bonaque-González, S.; Brajša, R.; Bommier, V.; Bourdin, P.-A.; Burgos Martín, J.; Calchetti, D.; Calcines, A.; Calvo Tovar, J.; Campbell, R.J.; Carballo-Martín, Y.; Carbone, V.; Carlin, E.S.; Carlsson, M.; Castro López, J.; Cavaller, L.; Cavallini, F.; Cauzzi, G.; Cecconi, M.; Chulani, H.M.; Cirami, R.; Consolini, G.; Coretti, I.; Cosentino, R.; Cózar-Castellano, J.; Dalmasse, K.; Danilovic, S.; De Juan Ovelar, M.; Del Moro, D.; del Pino Alemán, T.; del Toro Iniesta, J. C.; Denker, C.; Dhara, S.K.; Di Marcantonio, P.; Díaz Baso, C.J.; Diercke, A.; Dineva, E.; Díaz-García, J.J.; Doerr, H.-P.; Doyle, G.; Erdelyi, R.; Ermolli, I.; Escobar Rodríguez, A.; Esteban Pozuelo, S.; Faurobert, M.; Felipe, T.; Feller, A.; Feijoo Amoedo, N.; Femenía Castellá, B.; Fernandes, J.; Ferro Rodríguez, I.; Figueroa, I.; Fletcher, L.; Franco Ordovas, A.; Gafeira, R.; Gardenghi, R.; Gelly, B.; Giorgi, F.; Gisler, D.The European Solar Telescope (EST) is a project aimed at studying the magnetic connectivity of the solar atmosphere, from the deep photosphere to the upper chromosphere. Its design combines the knowledge and expertise gathered by the European solar physics community during the construction and operation of state-of-the-art solar telescopes operating in visible and near-infrared wavelengths: the Swedish 1m Solar Telescope, the German Vacuum Tower Telescope and GREGOR, the French Télescope Héliographique pour l'Étude du Magnétisme et des Instabilités Solaires, and the Dutch Open Telescope. With its 4.2 m primary mirror and an open configuration, EST will become the most powerful European ground-based facility to study the Sun in the coming decades in the visible and near-infrared bands. EST uses the most innovative technological advances: the first adaptive secondary mirror ever used in a solar telescope, a complex multi-conjugate adaptive optics with deformable mirrors that form part of the optical design in a natural way, a polarimetrically compensated telescope design that eliminates the complex temporal variation and wavelength dependence of the telescope Mueller matrix, and an instrument suite containing several (etalon-based) tunable imaging spectropolarimeters and several integral field unit spectropolarimeters. This publication summarises some fundamental science questions that can be addressed with the telescope, together with a complete description of its major subsystems.