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1. The Athena X-ray Integral Field Unit

Author

Barret, Didier, Trong, Thien Lam, Herder, Jan-Willem den, Piro, Luigi, Cappi, Massimo, Huovelin, Juhani, Kelley, Richard, Mas-Hesse, J. Miguel, Mitsuda, Kazuhisa, Paltani, Stéphane, Rauw, Gregor, Rozanska, Agata, Wilms, Joern, Bandler, Simon, Barbera, Marco, Barcons, Xavier, Bozzo, Enrico, Ceballos, Maria Teresa, Charles, Ivan, Costantini, Elisa, Decourchelle, Anne, Hartog, Roland den, Duband, Lionel, Duval, Jean-Marc, Fiore, Fabrizio, Gatti, Flavio, Goldwurm, Andrea, Jackson, Brian, Jonker, Peter, Kilbourne, Caroline, Macculi, Claudio, Mendez, Mariano, Molendi, Silvano, Orleanski, Piotr, Pajot, François, Pointecouteau, Etienne, Porter, Frederick, Pratt, Gabriel W., Prêle, Damien, Ravera, Laurent, Sato, Kosuke, Schaye, Joop, Shinozaki, Keisuke, Thibert, Tanguy, Valenziano, Luca, Valette, Veronique, Vink, Jacco, Webb, Natalie, Wise, Michael, Yamasaki, Noriko, Delcelier-Douchin, Françoise, Mesnager, Jean-Michel, Pontet, Bernard, Pradines, Alice, Branduardi-Raymont, Graziella, Bulbul, Esra, Dadina, Mauro, Ettori, Stefano, Finoguenov, Alexis, Fukazawa, Yasushi, Janiuk, Agnieszka, Kaastra, Jelle, Mazzotta, Pasquale, Miller, Jon, Miniutti, Giovanni, Nazé, Yaël, Nicastro, Fabrizio, Sciortino, Salvatore, Simionescu, Aurora, Torrejon, Jose Miguel, Frezouls, Benoît, Geoffray, Hervé, Peille, Philippe, Aicardi, Corinne, André, Jérôme, Clénet, Antoine, Daniel, Christophe, Etcheverry, Christophe, Gloaguen, Emilie, Hervet, Gilles, Jolly, Antoine, Ledot, Aurélien, Maussang, Irwin, Paillet, Alexis, Schmisser, Roseline, Vella, Bruno, Damery, Jean-Charles, Boyce, Kevin, DiPirro, Michael, Lotti, Simone, Schwander, Denis, Smith, Stephen, van Leeuwen, Bert-Joost, van Weers, Henk, Clerc, Nicolas, Cobo, Beatriz, Dauser, Thomas, de Plaa, Jelle, Kirsch, Christian, Cucchetti, Edoardo, Eckart, Megan, Ferrando, Philippe, and Natalucci, Lorenzo

Subjects
Astrophysics - Instrumentation and Methods for Astrophysics, Astrophysics - Cosmology and Nongalactic Astrophysics, Astrophysics - Astrophysics of Galaxies, Astrophysics - High Energy Astrophysical Phenomena
Abstract

The X-ray Integral Field Unit (X-IFU) is the high resolution X-ray spectrometer of the ESA Athena X-ray observatory. Over a field of view of 5' equivalent diameter, it will deliver X-ray spectra from 0.2 to 12 keV with a spectral resolution of 2.5 eV up to 7 keV on ~5 arcsecond pixels. The X-IFU is based on a large format array of super-conducting molybdenum-gold Transition Edge Sensors cooled at about 90 mK, each coupled with an absorber made of gold and bismuth with a pitch of 249 microns. A cryogenic anti-coincidence detector located underneath the prime TES array enables the non X-ray background to be reduced. A bath temperature of about 50 mK is obtained by a series of mechanical coolers combining 15K Pulse Tubes, 4K and 2K Joule-Thomson coolers which pre-cool a sub Kelvin cooler made of a 3He sorption cooler coupled with an Adiabatic Demagnetization Refrigerator. Frequency domain multiplexing enables to read out 40 pixels in one single channel. A photon interacting with an absorber leads to a current pulse, amplified by the readout electronics and whose shape is reconstructed on board to recover its energy with high accuracy. The defocusing capability offered by the Athena movable mirror assembly enables the X-IFU to observe the brightest X-ray sources of the sky (up to Crab-like intensities) by spreading the telescope point spread function over hundreds of pixels. Thus the X-IFU delivers low pile-up, high throughput (>50%), and typically 10 eV spectral resolution at 1 Crab intensities, i.e. a factor of 10 or more better than Silicon based X-ray detectors. In this paper, the current X-IFU baseline is presented, together with an assessment of its anticipated performance in terms of spectral resolution, background, and count rate capability. The X-IFU baseline configuration will be subject to a preliminary requirement review that is scheduled at the end of 2018., Comment: 15 pages, 5 figures, to appear in Proc. SPIE Astronomical Telescopes and Instrumentation, Austin 2018

Published
2018

2. The Athena X-ray Integral Field Unit (X-IFU)

Author

Barret, Didier, Trong, Thien Lam, Herder, Jan-Willem den, Piro, Luigi, Barcons, Xavier, Huovelin, Juhani, Kelley, Richard, Mas-Hesse, J. Miguel, Mitsuda, Kazuhisa, Paltani, Stéphane, Rauw, Gregor, Rożanska, Agata, Wilms, Joern, Barbera, Marco, Bozzo, Enrico, Ceballos, Maria Teresa, Charles, Ivan, Decourchelle, Anne, Hartog, Roland den, Duval, Jean-Marc, Fiore, Fabrizio, Gatti, Flavio, Goldwurm, Andrea, Jackson, Brian, Jonker, Peter, Kilbourne, Caroline, Macculi, Claudio, Mendez, Mariano, Molendi, Silvano, Orleanski, Piotr, Pajot, François, Pointecouteau, Etienne, Porter, Frederick, Pratt, Gabriel W., Prêle, Damien, Ravera, Laurent, Renotte, Etienne, Schaye, Joop, Shinozaki, Keisuke, Valenziano, Luca, Vink, Jacco, Webb, Natalie, Yamasaki, Noriko, Delcelier-Douchin, Françoise, Du, Michel Le, Mesnager, Jean-Michel, Pradines, Alice, Branduardi-Raymont, Graziella, Dadina, Mauro, Finoguenov, Alexis, Fukazawa, Yasushi, Janiuk, Agnieszka, Miller, Jon, Nazé, Yaël, Nicastro, Fabrizio, Sciortino, Salvatore, Torrejon, Jose Miguel, Geoffray, Hervé, Hernandez, Isabelle, Luno, Laure, Peille, Philippe, André, Jérôme, Daniel, Christophe, Etcheverry, Christophe, Gloaguen, Emilie, Hassin, Jérémie, Hervet, Gilles, Maussang, Irwin, Moueza, Jérôme, Paillet, Alexis, Vella, Bruno, Garrido, Gonzalo Campos, Damery, Jean-Charles, Panem, Chantal, Panh, Johan, Bandler, Simon, Biffi, Jean-Marc, Boyce, Kevin, Clénet, Antoine, DiPirro, Michael, Jamotton, Pierre, Lotti, Simone, Schwander, Denis, Smith, Stephen, van Leeuwen, Bert-Joost, van Weers, Henk, Brand, Thorsten, Cobo, Beatriz, Dauser, Thomas, de Plaa, Jelle, and Cucchetti, Edoardo

Subjects
Astrophysics - Instrumentation and Methods for Astrophysics, Astrophysics - Cosmology and Nongalactic Astrophysics, Astrophysics - Astrophysics of Galaxies, Astrophysics - High Energy Astrophysical Phenomena
Abstract

The X-ray Integral Field Unit (X-IFU) on board the Advanced Telescope for High-ENergy Astrophysics (Athena) will provide spatially resolved high-resolution X-ray spectroscopy from 0.2 to 12 keV, with 5 arc second pixels over a field of view of 5 arc minute equivalent diameter and a spectral resolution of 2.5 eV up to 7 keV. In this paper, we first review the core scientific objectives of Athena, driving the main performance parameters of the X-IFU, namely the spectral resolution, the field of view, the effective area, the count rate capabilities, the instrumental background. We also illustrate the breakthrough potential of the X-IFU for some observatory science goals. Then we briefly describe the X-IFU design as defined at the time of the mission consolidation review concluded in May 2016, and report on its predicted performance. Finally, we discuss some options to improve the instrument performance while not increasing its complexity and resource demands (e.g. count rate capability, spectral resolution). The X-IFU will be provided by an international consortium led by France, The Netherlands and Italy, with further ESA member state contributions from Belgium, Finland, Germany, Poland, Spain, Switzerland and two international partners from the United States and Japan., Comment: 41 pages, 18 Figures

Published
2016
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3. The ATHENA X-ray Integral Field Unit (X-IFU)

Author

Barret, Didier, Thien Lam Trong, den Herder, Jan-Willem, Piro, Luigi, Cappi, Massimo, Huovelin, Juhani, Kelley, Richard, Mas-Hesse, J. Miguel, Mitsuda, Kazuhisa, Paltani, Stephane, Rauw, Gregor, Rozanska, Agata, Wilms, Joern, Bandler, Simon, Barbera, Marco, Barcons, Xavier, Bozzo, Enrico, Ceballos, Maria Teresa, Charles, Ivan, Costantini, Elisa, Decourchelle, Anne, den Hartog, Roland, Duband, Lionel, Duval, Jean-Marc, Fiore, Fabrizio, Gatti, Flavio, Goldwurm, Andrea, Jackson, Brian, Jonker, Peter, Kilbourne, Caroline, Macculi, Claudio, Mendez, Mariano, Molendi, Silvano, Orleanski, Piotr, Pajot, Francois, Pointecouteau, Etienne, Porter, Frederick, Pratt, Gabriel W., Prele, Damien, Ravera, Laurent, Sato, Kosuke, Schaye, Joop, Shinozaki, Keisuke, Thibert, Tanguy, Valenziano, Luca, Valette, Veronique, Vink, Jacco, Webb, Natalie, Wise, Michael, Yamasaki, Noriko, Delcelier-Douchin, Francoise, Mesnager, Jean-Michel, Pontet, Bernard, Pradines, Alice, Branduardi-Raymont, Graziella, Bulbul, Esra, Dadina, Mauro, Ettori, Stefano, Finoguenov, Alexis, Fukazawa, Yasushi, Janiuk, Agnieszka, Kaastra, Jelle, Mazzotta, Pasquale, Miller, Jon, Miniutti, Giovanni, Naze, Yael, Nicastro, Fabrizio, Sciortino, Salvatore, Simionescu, Aurora, Torrejon, Jose Miguel, Geoffray, Herve, Peille, Philippe, Aicardi, Corinne, Andre, Jerome, Garrido, Gonzalo Campos, Clenet, Antoine, Daniel, Christophe, Etcheverry, Christophe, Frezouls, Benot, Gloaguen, Emilie, Hervet, Gilles, Jolly, Antoine, Ledot, Aurelien, Maussang, Irwin, Paillet, Alexis, Schmisser, Roseline, Travert, Jean-Michel, Vella, Bruno, Damery, Jean-Charles, Boyce, Kevin, DiPirro, Michael, Lotti, Simone, Schwander, Denis, Smith, Stephen, van Leeuwen, Bert-Joost, van Weers, Henk, Clerc, Nicolas, Cobo, Beatriz, Dauser, Thomas, de Plaa, Jelle, Kirsch, Christian, Cucchetti, Edoardo, Eckart, Megan, Ferrando, Philippe, Natalucci, Lorenzo, European Commission, Ministerio de Economía y Competitividad (España), Fonds de la Recherche Scientifique (Fédération Wallonie-Bruxelles), High Energy Astrophys. & Astropart. Phys (API, FNWI), DenHerder, JWA, Nikzad, S, Nakazawa, K, Department of Physics, Barret, Didier, Lam Trong, Thien, den Herder, Jan-Willem, Piro, Luigi, Cappi, Massimo, Houvelin, Juhani, Kelley, Richard, Mas-Hesse, J. Miguel, Mitsuda, Kazuhisa, Paltani, Stéphane, Rauw, Gregor, Rozanska, Agata, Wilms, Joern, Bandler, Simon, Barbera, Marco, Barcons, Xavier, Bozzo, Enrico, Ceballos, Maria Teresa, Charles, Ivan, Costantini, Elisa, Decourchelle, Anne, den Hartog, Roland, Duband, Lionel, Duval, Jean-Marc, Fiore, Fabrizio, Gatti, Flavio, Goldwurm, Andrea, Jackson, Brian, Jonker, Peter, Kilbourne, Caroline, Macculi, Claudio, Mendez, Mariano, Molendi, Silvano, Orleanski, Piotr, Pajot, Françoi, Pointecouteau, Etienne, Porter, Frederick, Pratt, Gabriel W., Prêle, Damien, Ravera, Laurent, Sato, Kosuke, Schaye, Joop, Shinozaki, Keisuke, Thibert, Tanguy, Valenziano, Luca, Valette, Véronique, Vink, Jacco, Webb, Natalie, Wise, Michael, Yamasaki, Noriko, Douchin, Françoise, Mesnager, Jean-Michel, Pontet, Bernard, Pradines, Alice, Branduardi-Raymont, Graziella, Bulbul, Esra, Dadina, Mauro, Ettori, Stefano, Finoguenov, Alexi, Fukazawa, Yasushi, Janiuk, Agnieszka, Kaastra, Jelle, Mazzotta, Pasquale, Miller, Jon, Miniutti, Giovanni, Naze, Yael, Nicastro, Fabrizio, Scioritino, Salavtore, Simonescu, Aurora, Torrejon, Jose Miguel, Frezouls, Benoit, Geoffray, Hervé, Peille, Philippe, Aicardi, Corinne, André, Jérôme, Daniel, Christophe, Clénet, Antoine, Etcheverry, Christophe, Gloaguen, Emilie, Hervet, Gille, Jolly, Antoine, Ledot, Aurélien, Paillet, Irwin, Schmisser, Roseline, Vella, Bruno, Damery, Jean-Charle, Boyce, Kevin, Dipirro, Mike, Lotti, Simone, Schwander, Deni, Smith, Stephen, Van Leeuwen, Bert-Joost, van Weers, Henk, Clerc, Nicola, Cobo, Beatriz, Dauser, Thoma, Kirsch, Christian, Cucchetti, Edoardo, Eckart, Megan, Ferrando, Philippe, Natalucci, Lorenzo, and Fonds de la Recherche Scientifique (Belgique)

Subjects
Point spread function, Photon, Astrophysics::High Energy Astrophysical Phenomena, Field of view, Athena, Instrumentation, Space telescopes, X-ray Integral Field Unit, X-ray spectroscopy, Electronic, Optical and Magnetic Materials, Condensed Matter Physics, Computer Science Applications1707 Computer Vision and Pattern Recognition, Applied Mathematics, Electrical and Electronic Engineering, Condensed Matter Physic, Large format, 01 natural sciences, 7. Clean energy, law.invention, Telescope, Physics::Popular Physics, Settore FIS/05 - Astronomia E Astrofisica, Optics, law, Physics::Plasma Physics, 0103 physical sciences, Electronic, Optical and Magnetic Materials, Spectral resolution, 010306 general physics, 010303 astronomy & astrophysics, Physics, Spectrometer, business.industry, Electronic, Optical and Magnetic Material, Detector, Astrophysics::Instrumentation and Methods for Astrophysics, 115 Astronomy, Space science, Physics::History of Physics, Applied Mathematic, Space telescope, business
Abstract

Event: SPIE Astronomical Telescopes + Instrumentation, 2018, Austin, Texas, United States., The X-IFU will be provided by an international consortium led by France, The Netherlands and Italy, with further ESA member state contributions from Belgium, Finland, Germany, Poland, Spain, Switzerland and two international partners from the United States and Japan: et al., The X-ray Integral Field Unit (X-IFU) is the high resolution X-ray spectrometer of the ESA Athena X-ray observatory. Over a field of view of 5’ equivalent diameter, it will deliver X-ray spectra from 0.2 to 12 keV with a spectral resolution of 2.5 eV up to 7 keV on ∼ 5” pixels. The X-IFU is based on a large format array of super-conducting molybdenum-gold Transition Edge Sensors cooled at ∼ 90 mK, each coupled with an absorber made of gold and bismuth with a pitch of 249 μm. A cryogenic anti-coincidence detector located underneath the prime TES array enables the non X-ray background to be reduced. A bath temperature of ∼ 50 mK is obtained by a series of mechanical coolers combining 15K Pulse Tubes, 4K and 2K Joule-Thomson coolers which pre-cool a sub Kelvin cooler made of a 3He sorption cooler coupled with an Adiabatic Demagnetization Refrigerator. Frequency domain multiplexing enables to read out 40 pixels in one single channel. A photon interacting with an absorber leads to a current pulse, amplified by the readout electronics and whose shape is reconstructed on board to recover its energy with high accuracy. The defocusing capability offered by the Athena movable mirror assembly enables the X-IFU to observe the brightest X-ray sources of the sky (up to Crab-like intensities) by spreading the telescope point spread function over hundreds of pixels. Thus the X-IFU delivers low pile-up, high throughput (< 50%), and typically 10 eV spectral resolution at 1 Crab intensities, i.e. a factor of 10 or more better than Silicon based X-ray detectors. In this paper, the current X-IFU baseline is presented, together with an assessment of its anticipated performance in terms of spectral resolution, background, and count rate capability. The X-IFU baseline configuration will be subject to a preliminary requirement review that is scheduled at the end of 2018., We acknowledge support from the Athena Science Study Team, the Athena Working Group Chairs, the Athena Topical Panel Chairs and the Topical Panel members in strengthening the X-IFU top level performance requirements. Particular thanks go to: E. Rasia, V. Biffi, S. Borgani and K. Dolag for providing cosmological hydrodynamic simulations of a cluster used to produce simulation of X-IFU observation presented in Fig. 2; P.T. O'Brien for assistance with Sect. 2.2.1, A.C. Fabian and C. Pinto for providing inputs for Figure 1. We also thank the ESA project team, and in particular Mark Ayre and Ivo Ferreira, for their work on the assessment of the ToO efficiency requirement. The Italian contribution to X-IFU is supported through the ASI contractn. 2015-046-R.0. XB, MTC and BC acknowledge nancial support by MINECO through grant ESP2014-53672-C3-1-P. A.R., P.O, and A.J. were supported by Polish NSC grants: 2015/17/B/ST9/03422 and 2015/18/M/ST9/00541. GR, ER, YN, and PJ acknowledges support by FNRS and Prodex (Belspo). This work was supported by the French Space Agency (CNES).

Published
2018

5. Adapted ECC ozonesonde for long-duration flights aboard boundary-layer pressurised balloons

Author

Gheusi, François, primary, Durand, Pierre, additional, Verdier, Nicolas, additional, Dulac, François, additional, Attié, Jean-Luc, additional, Commun, Philippe, additional, Barret, Brice, additional, Basdevant, Claude, additional, Clenet, Antoine, additional, Derrien, Solène, additional, Doerenbecher, Alexis, additional, El Amraoui, Laaziz, additional, Fontaine, Alain, additional, Hache, Emeric, additional, Jambert, Corinne, additional, Jaumouillé, Elodie, additional, Meyerfeld, Yves, additional, Roblou, Laurent, additional, and Tocquer, Flore, additional

Published
2016
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6. Préparation de la mission spatiale SPICA : développement d'une chaîne de contrôle et de lecture pour matrice de bolomètres supraconducteurs multiplexés en fréquence

Author

Clenet, Antoine and Clenet, Antoine

Abstract

Après le succès des missions spatiales infrarouge de l'ESA Planck et Herschel (2009), le développement de détecteurs submillimétriques à très haute sensibilité en matrices de plusieurs milliers d'éléments est l'un des grands défis auxquels il faut apporter des solutions pour répondre aux besoins des missions scientifiques de l'astrophysique spatiale du futur comme le satellite SPICA (JAXA/ESA lancement potentiel pour 2026). Ce dernier permettra de nombreuses avancées spectaculaires dans la connaissance de l'Univers lointain. Il permettra, en particulier, d'observer l'émission infra-rouge des premières galaxies de l'Univers et des trous noirs qu'elles abritent en leur centre, de caractériser leur contenu en molécules complexes, et ainsi de mieux comprendre les mécanismes physiques de leur formation et de leur évolution. Il permettra également de découvrir et caractériser de nouvelles exoplanètes. Dans le cadre du projet SPICA, l'IRAP est en charge du développement de l'unité de contrôle et de lecture (Detector Control Unit - DCU) de l'instrument européen SAFARI. Ce sous-système assure le contrôle et la lecture de 3500 détecteurs supraconducteurs TES (Transition Edge Sensors). Pour cela il assure le multiplexage en fréquence des détecteurs et linéarise la chaîne de détection. Le DCU traite les signaux, pour une partie de manière analogique (filtrage et amplification), mais surtout de manière numérique (filtrage numérique, contrôle d'asservissement, ...) pour extraire le signal scientifique des bolomètres. La première partie de mon travail de thèse a été de développer un modèle de co-simulation analogique et numérique de l'ensemble de la chaîne de détection de SAFARI pour valider l'architecture de l'électronique conçue à l'IRAP. En effet, la chaîne de détection de SAFARI est développée dans plusieurs laboratoires européens et de ce fait l'IRAP ne dispose pas d'un plan focal représentatif qui permettrait de valider le concept ainsi que les fonctionnalités du DCU. L'impl, After the success of ESA's infrared space mission, Planck and Herschel (2009), it is mandatory to develop new generation ultra-sensitive detector arrays to meet the science requirements of the future space missions such as SPICA (JAXA/ESA due to be launched in 2026). SPICA will allow many breakthroughs in our knowledge of the far Universe by observing the first galaxies and characterizing their chemical composition. Thus, it will provide a better understanding of the physical mechanisms that contributed to their formation and their evolution. In addition to that, it will allow the discovery and characterization of new exoplanets. In the context of SPICA, IRAP is developing the digital control unit (DCU) of the European instrument SAFARI to drive the frequency domain multiplexed readout of the kilo-pixel bolometer arrays. It consists in a digital electronics performing a massively parallel signal processing to manage the data of the 3500 bolometers. My first objective was to develop a co-simulation model of the entire SAFARI detection chain in order to validate the DCU concept developed at IRAP. The instrument is a complex and expensive instrument developed by a European consortium; IRAP does not have a representative focal plane to be used with the DCU. My model mimics the DCU. This part has been used as a functional reference during the development of the DCU firmware. It also includes a realistic model of the focal plane array. This has been used to validate the readout concept of SAFARI. My second objective was to optimize the digital readout and control electronics in order to reduce its power consumption. With the DCU team at IRAP I developed an optimized digital architecture to process the bolometers data. Thanks to this, we managed to reduce the dynamic power consumption of the circuit by a factor of 10, saving at the same time about 1/3 of the digital resources. My third objective was to define the calibration protocol for the readout chain. Indeed, the oper

Published
2014

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