Proyecto de Investigación: RTI2018-096686-B-C21
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RTI2018-096686-B-C21
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Mid-IR cosmological spectrophotometric surveys from space: Measuring AGN and star formation at the cosmic noon with a SPICA-like mission
(Cambridge University Press, 2021-04-23) Spignoglio, L.; Mordini, S.; Fernández Ontiveros, J. A.; Alonso Herrero, A.; Armus, L.; Bisigello, L.; Calura, F.; Carrera, F. J.; Cooray, A.; Dannerbauer, H.; Decarli, R.; Egami, E.; Elbaz, D.; Franceschini, A.; González Alfonso, E.; Graziani, L.; Gruppioni, C.; Hatziminaoglou, Evanthia; Kaneda, H.; Kohno, K.; Labiano, Á.; Magdis, Georgios E.; Malkan, M. A.; Matsuhara, H.; Nagao, T.; Naylor, D.; Pereira Santaella, M.; Pozzi, F.; Rodighiero, G.; Roelfsema, P.; Serjeant, S.; Vignali, C.; Wang, L.; Yamada, T.; Agenzia Spaziale Italiana (ASI); Agencia Estatal de Investigación (AEI); Comunidad de Madrid; Spignoglio, L. [0000-0001-8840-1551]; Fernández Ontiveros, J. A. [0000-0001-9490-899X]; Gruppioni, C. [0000-0002-5836-4056]; Graziani, L. [0000-0002-9231-1505]; Unidad de Excelencia Científica María de Maeztu Instituto de Astrofísica de Cantabria, MDM-2017-0765; Unidad de Excelencia Científica María de Maeztu Centro de Astrobiología del Instituto Nacional de Técnica Aeroespacial y CSIC, MDM-2017-0737
We use the SPace Infrared telescope for Cosmology and Astrophysics (SPICA) project as a template to demonstrate how deep spectrophotometric surveys covering large cosmological volumes over extended fields (1– ) with a mid-IR imaging spectrometer (17– ) in conjunction with deep photometry with a far-IR camera, at wavelengths which are not affected by dust extinction can answer the most crucial questions in current galaxy evolution studies. A SPICA-like mission will be able for the first time to provide an unobscured three-dimensional (3D, i.e. x, y, and redshift z) view of galaxy evolution back to an age of the universe of less than 2 Gyrs, in the mid-IR rest frame. This survey strategy will produce a full census of the Star Formation Rate (SFR) in the universe, using polycyclic aromatic hydrocarbons (PAH) bands and fine-structure ionic lines, reaching the characteristic knee of the galaxy luminosity function, where the bulk of the population is distributed, at any redshift up to . Deep follow-up pointed spectroscopic observations with grating spectrometers onboard the satellite, across the full IR spectral range (17– ), would simultaneously measure Black Hole Accretion Rate (BHAR), from high-ionisation fine-structure lines, and SFR, from PAH and low- to mid-ionisation lines in thousands of galaxies from solar to low metallicities, down to the knee of their luminosity functions. The analysis of the resulting atlas of IR spectra will reveal the physical processes at play in evolving galaxies across cosmic time, especially its heavily dust-embedded phase during the activity peak at the cosmic noon ( –3), through IR emission lines and features that are insensitive to the dust obscuration.
Multiphase feedback processes in the Sy2 galaxy NGC 5643
(EDP Sciences, 2021-01-12) García Bernete, I.; Alonso Herrero, A.; García Burillo, S.; Pereira Santaella, M.; García Lorenzo, B.; Carrera, F. J.; Rigopoulou, D.; Ramos Almeida, C.; Villar Martín, M.; González Martín, O.; Hicks, E. K. S.; Labiano, Á.; Ricci, C.; Mateos, S.; Ministerio de Economía y Competitividad (MINECO); Science and Technology Facilities Council (STFC); Agencia Estatal de Investigación (AEI); Comunidad de Madrid; Fondo Nacional de Desarrollo Científico y Tecnológico (FONDECYT); García Lorenzo, M. B. [0000-0002-7228-7173]; Ramos Almeida, C. [0000-0001-8353-649X]; Carrero, F. J. [0000-0003-2135-9023]; Unidad de Excelencia Científica María de Maeztu Centro de Astrobiología del Instituto Nacional de Técnica Aeroespacial y CSIC, MDM-2017-0737; Unidad de Excelencia Científica María de Maeztu AGENCIA ESTATAL CONSEJO SUPERIOR DE INVESTIGACIONES CIENTIFICAS (CSIC), MDM-2017-0765
We study the multiphase feedback processes in the central ∼3 kpc of the barred Seyfert 2 galaxy NGC 5643. We used observations of the cold molecular gas (ALMA CO(2−1) transition) and ionized gas (MUSE IFU optical emission lines). We studied different regions along the outflow zone, which extends out to ∼2.3 kpc in the same direction (east-west) as the radio jet, as well as nuclear and circumnuclear regions in the host galaxy disk. The CO(2−1) line profiles of regions in the outflow and spiral arms show two or more different velocity components: one associated with the host galaxy rotation, and the others with out- or inflowing material. In the outflow region, the [O III]λ5007 Å emission lines have two or more components: the narrow component traces rotation of the gas in the disk, and the others are related to the ionized outflow. The deprojected outflowing velocities of the cold molecular gas (median Vcentral ∼ 189 km s−1) are generally lower than those of the outflowing ionized gas, which reach deprojected velocities of up to 750 km s−1 close to the active galactic nucleus (AGN), and their spatial profiles follow those of the ionized phase. This suggests that the outflowing molecular gas in the galaxy disk is being entrained by the AGN wind. We derive molecular and ionized outflow masses of ∼5.2 × 107 M⊙ (αCOGalactic) and 8.5 × 104 M⊙ and molecular and ionized outflow mass rates of ∼51 M⊙ yr−1 (αCOGalactic) and 0.14 M⊙ yr−1, respectively. This means that the molecular phase dominates the outflow mass and outflow mass rate, while the kinetic power and momentum of the outflow are similar in both phases. However, the wind momentum loads (Ṗout/ṖAGN) for the molecular and ionized outflow phases are ∼27−5 (αCOGalactic and αCOULIRGs) and < 1, which suggests that the molecular phase is not momentum conserving, but the ionized phase most certainly is. The molecular gas content (Meast ∼ 1.5 × 107 M⊙; αCOGalactic) of the eastern spiral arm is approximately 50−70% of the content of the western one. We interpret this as destruction or clearing of the molecular gas produced by the AGN wind impacting in the eastern side of the host galaxy (negative feedback process). The increase in molecular phase momentum implies that part of the kinetic energy from the AGN wind is transmitted to the molecular outflow. This suggests that in Seyfert-like AGN such as NGC 5643, the radiative or quasar and the kinetic or radio AGN feedback modes coexist and may shape the host galaxies even at kiloparsec scales through both positive and (mild) negative feedback.
The athena x-ray integral field unit: a consolidated design for the system requirement review of the preliminary definition phase
(Springer Link, 2022-08-30) Barret, Didier; Albouys, Vincent; Herderm Jan-Willem den; Piro, Luigi; Cappi, Massimo; Huovelin, Juhani; Kelley, Richard; Mas-Hesse, J. Miguel; Paltani, Stéphane; Rauw, Gregor; Rozanska, Agata; Fiore, Fabrizio; Bonny, Patrick; Boorman, Peter; Boreux, Charles; Bounab, Ayoub; Cuttaia, Francesco; Gabici, Stefano; Boutelier, Martin; Boyce, Kevin; Molin, Alexeï; Etcheverry, Christophe; Brienza, Daniele; Bruijn, Marcel; Bandler, Simon; Puccio, Elena; Bulgarelli, Andrea; Calarco, Simona; Callanan, Paul; D'Ai, Antonino; Camus, Thierry; Canourgues, Florent; Branduardi-Raymont, Graziella; Cavazzuti, Elisabetta; Gant, Florent; Capobianco, Vito; Cardiel, Nicolás; Castellani, Florent; Cheatom, Oscar; Pascale, Ramon; Chervenak, James; D'anca, Fabio; Gastaldello, Fabio; Ettori, Stefano; Dadina, Mauro; Barbera, Marco; Daniel, Christophe; Peille, Philippe; Gloaguen, Emilie; DeNigris, Natalie; Dercksen, Johannes; DiPirro, Michael; Doumayrou, Eric; Dubbeldam, Luc; Finoguenov, Alexis; Bozzo , Enrico; Dupieux, Michel; Monestes, David; Genolet, Ludovic; Ghizzardi, Simona; Plaa, Jelle de; Alcacera Gil, María Ángeles; Dupourqué, Simon; Giovannini, Elisa; Durkin, Malcom; Grosso, Nicolas; Charles, Ivan; Godet, Olivier; Gómez Elvira, J.; Montinaro, Nicola; González, Manuel; González, Raoul; Gottardi, Luciano; Ardellier, Florence; Granat, Dolorès; Gros, Michel; Pinsard, Frederic; Rioland, Guillaume; Guignard, Nicolas; Hieltjes, Paul; Fioretti, Valentina; Mot, Baptiste; Hurtado, Adolfo Jesus; Costantini, Elisa; Irwin, Kent; Jacquey, Christian; Argan, Andrea; Van der Kuur, Jan; Janiuk, Agnieszka; Jaubert, Jean; Rodriguez, Louis; Jolly, Antoine; Smith, Stephen; Jourdan, Thierry; Julien, Sabine; Geoffray, Hervé; Kedziora, Bartosz; Kaastra, Jelle; Korb, Andrew; Van Leeuwen, Bert-Joost; Dauser, Thomas; Kreykenbohm, Ingo; König, Ole; Langer, Mathieu; Murat, David; Roig, Anton; Laudet, Philippe; Laurent, Philippe; Mazzotta, Pasquale; Laurenza, Monica; Lesrel, Jean; Jacques, Lionel; Bellouard, Elise; Ligori, Sebastiano; Lorenz, Maximilian; Luminari, Alfredo; Nagayoshi, Kenichiro; Decourchelle, Anne; Maffei, Bruno; Colonges, Stéphane; Rollet, Bertrand; Maisonnave, Océane; Marelli, Lorenzo; Massonet, Didier; Maussang, Irwin; Carron, Jérôme; Nazé, Yaël; Roudil, Gilles; Noguès, Loïc; Kirsch, Christian; Pailot, Damien; Chiarello, Fabio; Fossecave, Hervé; Duval, Jean-Marc; Panessa, Francesca; Parodi, Luigi; Petit, Pascal; Piconcelli, Enrico; Adams, Joseph; Pinto, Ciro; Miller, Jon; Rudnicki, Tomasz; Gatti, Flavio; Clerc, Nicolas; Sanisidro, Julien; Encinas Plaza, José Miguel; Sciortino, Luisa; Durand, Jean Louis; Hoogeveen, Ruud; Silva, Vitor; Sordet, Michael; Miniutti, Giovanni; Soto Aguilar, Javier; Spizzi, Pierre; Surace, Christian; Clerc, Laurent; Fernández Sánchez, Miguel; Taralli, Emanuele; Fiorini, Mauro; Goldwurm, Andrea; Hartog, Roland den; Eckert, Dominique; Nicastro, Fabrizio; Jackson, Brian; Svoboda, Jiri; Jonker, Peter; Kilbourne, Caroline; Cobo, Beatriz; Korpela, Seppo; Macculi, Claudio; Mendez, Mariano; Khosropanah, Pourya; Mitsuda, Kazuhisa; Finkbeiner, Fred; Molendi, Silvano; Pajot, François; Eiriz, Valvanera; Pointecouteau, Etienne; Porter, Frederick; Gao, Jian-Rong; Van der Hulst, Paul; Pratt, Gabriel W.; Prêle, Damien; Ravera, Laurent; Sciortino, Salvatore; Martin, Sylvain; Sato, Kosuke; Schaye, Joop; Shinozaki, Keisuke; Skup, Konrad; Ercolani, Eric; Coeur-Joly, Odile; Soucek, Jan; Thibert, Tanguy; Vink, Jacco; Yamaguchi, Hiroya; Kiviranta, Mikko; Webb, Natalie; Perry, James; Chaoul, Laurence; Raulin, Desi; Simionescu, Aurora; Torrejón, José Miguel; Coleiro, Alexis; Acero, Fabio; Beaumont, Sophie; Pradines, Alice; Cucchetti, Edoardo; D'Andrea, Matteo; Le Mer, Isabelle; Reina, M.; Ledot, Aurélien; Eckart, Megan; Ferrando, Philippe; Kammoun, Elias; Lotti, Simone; Fiocchi, Maria Teresa; Mesnager, Jean-Michel; Rigano, Manuela; Van Loon, Dennis; Michalski, Lea; Roelfsema, Peter; Natalucci, Lorenzo; Schwander, Denis; Poyatos Martínez, D.; Ceballos, Maria Teresa; Torrioli, Guido; Ullom, Joel; Medinaceli Villegas, Eduardo; Zuchniak, Monika; Millerioux, Jean-Pierre; Brachet, Frank; Lo Cicero, Ugo; Corcione, Leonardo; Lyautey, Bertrand; Parot, Yann; Prouvé, Thomas; Sakai, Kazuhiro; Doriese, William; Weers, Henk van; Wilms, Joern; Mineo, Teresa; Abdoelkariem, Shariefa; Adam, Thomas; Adami, Christophe; Coriat, Mickael; Aicardi, Corinne; Akamatsu, Hiroki; Merino Alonso, Pablo Eleazar; Ptak, Andy; Amato, Roberta; André, Jérôme; Roncarelli, Mauro; Franssen, Philippe; Angelinelli, Matteo; Añón Cancela, M.; Yamasaki, Noriko; Coynel, Alexandre; Anvar, Shebli; Atienza, R.; Attard, Anthony; Auricchio, Natalia; Puccetti, Simonetta; Duband, Lionel; Balado, A.; Bancel, Florian; Ferrari Barusso, Lorenzo; Frericks, Martin; Bernard, Vivian; Barcons, Xavier; Berrocal, A.; Blin, Sylvie; Audard, Marc; Bonino, Donata; Minervini, Gabriele; Bonnet, François; Jiménez, María; Gonzalo Melchor, Alejandro; VERA TRALLERO, ISABEL; Agencia Estatal de Investigación (AEI); Ministerio de Ciencia e Innovación (MICINN); Centre National D'Etudes Spatiales (CNES); Agenzia Spaziale Italiana (ASI); European Space Agency (ESA)
The Athena X-ray Integral Unit (X-IFU) is the high resolution X-ray spectrometer, studied since 2015 for flying in the mid-30s on the Athena space X-ray Observatory, a versatile observatory designed to address the Hot and Energetic Universe science theme, selected in November 2013 by the Survey Science Committee. Based on a large format array of Transition Edge Sensors (TES), it aims to provide spatially resolved X-ray spectroscopy, with a spectral resolution of 2.5 eV (up to 7 keV) over an hexagonal field of view of 5 arc minutes (equivalent diameter). The X-IFU entered its System Requirement Review (SRR) in June 2022, at about the same time when ESA called for an overall X-IFU redesign (including the X-IFU cryostat and the cooling chain), due to an unanticipated cost overrun of Athena. In this paper, after illustrating the breakthrough capabilities of the X-IFU, we describe the instrument as presented at its SRR, browsing through all the subsystems and associated requirements. We then show the instrument budgets, with a particular emphasis on the anticipated budgets of some of its key performance parameters. Finally we briefly discuss on the ongoing key technology demonstration activities, the calibration and the activities foreseen in the X-IFU Instrument Science Center, and touch on communication and outreach activities, the consortium organisation, and finally on the life cycle assessment of X-IFU aiming at minimising the environmental footprint, associated with the development of the instrument. Thanks to the studies conducted so far on X-IFU, it is expected that along the design-to-cost exercise requested by ESA, the X-IFU will maintain flagship capabilities in spatially resolved high resolution X-ray spectroscopy, enabling most of the original X-IFU related scientific objectives of the Athena mission to be retained.
