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1. Microcalorimeter Absorber Optimization for ATHENA and LEM.

Author

Wassell, Edward, Adams, Joseph, Bandler, Simon, Chervenak, James, Cumbee, Renata, Finkbeiner, Fred, Fuhrman, Joshua, Hull, Samuel, Kelley, Richard, Kilbourne, Caroline, Mateo, Jennette, Muramatsu, Haruka, Porter, Frederick, Rani, Asha, Sakai, Kazuhiro, Smith, Stephen, Wakeham, Nicholas, and Yoon, Sang

Subjects
X-ray telescopes, SOFT X rays, QUANTUM efficiency, ENTHALPY, HEAT capacity, QUANTUM noise, ASTROPHYSICS, INFRARED radiation
Abstract

High quantum efficiency (QE) X-ray absorbers are needed for future X-ray astrophysics telescopes. The Advanced Telescope for High ENergy Astrophysics (ATHENA) mission requirements for the X-ray Integral Field Unit (X-IFU) instrument dictate, at their most stringent, that the absorber achieve vertical QE > 90.6% at 7 keV and low total heat capacity, 0.731 pJ/K. The absorber we have designed is 313 µm square composed of 1.05 μm Au and 5.51 μm electroplated Bi films (Barret et al. in Exp Astron 55:373–426, 2023). Overhanging the TES, the absorber is mechanically supported by 6 small legs whose 5 μm diameter is tuned to the target thermal conductance for the device. Further requirements for the absorber for X-IFU include a > 40% reflectance at wavelengths from 1 to 20 μm to reduce shot noise from infrared radiation from higher temperature stages in the cryostat. We meet this requirement by capping our absorbers with an evaporated Ti/Au thin film. Additionally, narrow gaps between absorbers are required for high fill fraction, as well as low levels of fine particulate remaining on the substrate and zero shorts between absorbers that may cause thermal crosstalk. The Light Element Mapper (LEM) is an X-ray probe concept optimized to explore the soft X-ray emission from 0.2 to 2.0 keV. These pixels for LEM require high residual resistance ratio (RRR) thin 0.5 µm Au absorbers to thermalize uniformly and narrow < 2 μm gaps between pixels for high areal fill fraction. This paper reports upon technology developments required to successfully yield arrays of pixels for both mission concepts and presents first testing results of devices with these new absorber recipes. [ABSTRACT FROM AUTHOR]

Published
2024
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2. The Athena X-ray Integral Field Unit: a consolidated design for the system requirement review of the preliminary definition phase

Author

Universidad de Alicante. Departamento de Física, Ingeniería de Sistemas y Teoría de la Señal, Universidad de Alicante. Instituto Universitario de Física Aplicada a las Ciencias y las Tecnologías, Barret, Didier, Albouys, Vincent, den Herder, Jan-Willem, Piro, Luigi, Cappi, Massimo, Huovelin, Juhani, Kelley, Richard, Mas-Hesse, J. Miguel, Paltani, Stéphane, Rauw, Gregor, Rozanska, Agata, Bernard, Vivian, Berrocal, Alicia, Audard, Marc, Blin, Sylvie, Bonino, Donata, Frericks, Martin, Bonnet, François, Bonny, Patrick, Boorman, Peter, Ptak, Andy, Chaoul, Laurence, Boreux, Charles, Bounab, Ayoub, Boutelier, Martin, Boyce, Kevin, Brienza, Daniele, Bandler, Simon, Bruijn, Marcel, Gabici, Stefano, Bulgarelli, Andrea, Calarco, Simona, Raulin, Desi, Gloaguen, Emilie, Callanan, Paul, Prada Campello, Alberto, Camus, Thierry, Canourgues, Florent, Capobianco, Vito, Cardiel, Nicolas, Castellani, Florent, Barbera, Marco, Gant, Florent, Simionescu, Aurora, Cheatom, Oscar, Doumayrou, Eric, Chervenak, James, Chiarello, Fabio, Clerc, Laurent, Clerc, Nicolas, Cobo, Beatriz, Coeur-Joly, Odile, Coleiro, Alexis, Colonges, Stéphane, Torrejon, Jose M., Corcione, Leonardo, Gao, Jian-Rong, Puccetti, Simonetta, Barcons, Xavier, Coriat, Mickael, Coynel, Alexandre, Cuttaia, Francesco, D’Ai, Antonino, D’anca, Fabio, Dadina, Mauro, Acero, Fabio, Daniel, Christophe, Dauner, Lea, DeNigris, Natalie, Puccio, Elena, Gastaldello, Fabio, Dercksen, Johannes, Bozzo, Enrico, DiPirro, Michael, Genolet, Ludovic, Durkin, Malcom, van Leeuwen, Bert-Joost, Charles, Ivan, Ghizzardi, Simona, Alcacera Gil, M. Angeles, Giovannini, Elisa, Ramon, Pascale, Godet, Olivier, Gomez-Elvira, Javier, Gonzalez, Raoul, Gonzalez, Manuel, Gottardi, Luciano, Branduardi-Raymont, Graziella, Granat, Dolorès, Fioretti, Valentina, Gros, Michel, Costantini, Elisa, Guignard, Nicolas, Reina, Manuel, Hieltjes, Paul, Hurtado, Adolfo Jesús, Irwin, Kent, Jacquey, Christian, Ettori, Stefano, Janiuk, Agnieszka, Jaubert, Jean, Jiménez, Maria, Geoffray, Hervé, Jolly, Antoine, Jourdan, Thierry, Rioland, Guillaume, Dauser, Thomas, Julien, Sabine, Kedziora, Bartosz, Finoguenov, Alexis, Korb, Andrew, Kreykenbohm, Ingo, König, Ole, Langer, Mathieu, Laudet, Philippe, Jacques, Lionel, Laurent, Philippe, Rodriguez, Louis, Laurenza, Monica, Lesrel, Jean, Etcheverry, Christophe, Decourchelle, Anne, Ligori, Sebastiano, Lorenz, Maximilian, Luminari, Alfredo, Maffei, Bruno, Maisonnave, Océane, Marelli, Lorenzo, Kirsch, Christian, Roig, Anton, Massonet, Didier, Petit, Pascal, Maussang, Irwin, Melchor, Alejandro Gonzalo, Le Mer, Isabelle, Duband, Lionel, San Millan, Francisco Javier, Millerioux, Jean-Pierre, Mineo, Teresa, Minervini, Gabriele, Molin, Alexeï, Gatti, Flavio, Grosso, Nicolas, Smith, Stephen, Monestes, David, Montinaro, Nicola, Mot, Baptiste, Murat, David, Nagayoshi, Kenichiro, Duval, Jean-Marc, Nazé, Yaël, Noguès, Loïc, Pailot, Damien, Kaastra, Jelle, Rollet, Bertrand, Panessa, Francesca, Adams, Joseph, Parodi, Luigi, Roncarelli, Mauro, Dubbeldam, Luc, Hoogeveen, Ruud, Roudil, Gilles, Rudnicki, Tomasz, Sanisidro, Julien, Mazzotta, Pasquale, Sciortino, Luisa, Silva, Vitor, Sordet, Michael, Soto-Aguilar, Javier, Spizzi, Pierre, Goldwurm, Andrea, Dupieux, Michel, Surace, Christian, Svoboda, Jiri, Fernández Sánchez, Miguel, Miller, Jon, Taralli, Emanuele, Terrasa, Guilhem, Terrier, Régis, Todaro, Michela, Ubertini, Pietro, Uslenghi, Michela, Vaate, Jan Geralt Bijd de, Dupourqué, Simon, Vaccaro, Davide, den Hartog, Roland, Miniutti, Giovanni, van der Hulst, Paul, Varisco, Salvatore, Varnière, Peggy, Vibert, Laurent, Vidriales, María, Villa, Fabrizio, Vodopivec, Boris Martin, Volpe, Angela, Durand, Jean Louis, Vries, Cor de, Nicastro, Fabrizio, Wakeham, Nicholas, Walmsley, Gavin, Kiviranta, Mikko, Jackson, Brian, Wise, Michael, Wit, Martin de, Woźniak, Grzegorz, Jonker, Peter, Kilbourne, Caroline, Eckert, Dominique, Sciortino, Salvatore, Korpela, Seppo, Macculi, Claudio, Mendez, Mariano, Mitsuda, Kazuhisa, van der Kuur, Jan, Molendi, Silvano, Pajot, François, Pointecouteau, Etienne, Porter, Frederick, Pratt, Gabriel W., van Loon, Dennis, Eiriz, Valvanera, Prêle, Damien, Ravera, Laurent, Sato, Kosuke, Schaye, Joop, Shinozaki, Keisuke, Ledot, Aurélien, Skup, Konrad, Soucek, Jan, Thibert, Tanguy, Yamaguchi, Hiroya, Vink, Jacco, Ercolani, Eric, Webb, Natalie, Beaumont, Sophie, Piconcelli, Enrico, Ceballos, Maria Teresa, Cucchetti, Edoardo, D’Andrea, Matteo, Eckart, Megan, Ferrando, Philippe, Kammoun, Elias, Lotti, Simone, Mesnager, Jean-Michel, Natalucci, Lorenzo, Lyautey, Bertrand, Pinto, Ciro, Peille, Philippe, Doriese, William, de Plaa, Jelle, Ardellier, Florence, Argan, Andrea, Bellouard, Elise, Carron, Jérôme, Cavazzuti, Elisabetta, Fiorini, Mauro, Khosropanah, Pourya, Encinas Plaza, Jose Miguel, Martin, Sylvain, Parot, Yann, Finkbeiner, Fred, Perry, James, Pinsard, Frederic, Pradines, Alice, Rigano, Manuela, Roelfsema, Peter, Schwander, Denis, Torrioli, Guido, Plaza, Borja, Ullom, Joel, Vera, Isabel, Medinaceli Villegas, Eduardo, Fiocchi, Mariateresa, Sakai, Kazuhiro, Zuchniak, Monika, Brachet, Frank, Lo Cicero, Ugo, van Weers, Henk, Wilms, Joern, Fiore, Fabrizio, Abdoelkariem, Shariefa, Adam, Thomas, Adami, Christophe, Aicardi, Corinne, Fossecave, Hervé, Akamatsu, Hiroki, Merino Alonso, Pablo Eleazar, Amato, Roberta, André, Jérôme, Angelinelli, Matteo, Poyatos, David, Anon-Cancela, Manuel, Yamasaki, Noriko, Anvar, Shebli, Atienza, Ricardo, Attard, Anthony, Franssen, Philippe, Auricchio, Natalia, Balado, Ana, Bancel, Florian, Barusso, Lorenzo Ferrari, Prouvé, Thomas, Bascuñan, Arturo, Universidad de Alicante. Departamento de Física, Ingeniería de Sistemas y Teoría de la Señal, Universidad de Alicante. Instituto Universitario de Física Aplicada a las Ciencias y las Tecnologías, Barret, Didier, Albouys, Vincent, den Herder, Jan-Willem, Piro, Luigi, Cappi, Massimo, Huovelin, Juhani, Kelley, Richard, Mas-Hesse, J. Miguel, Paltani, Stéphane, Rauw, Gregor, Rozanska, Agata, Bernard, Vivian, Berrocal, Alicia, Audard, Marc, Blin, Sylvie, Bonino, Donata, Frericks, Martin, Bonnet, François, Bonny, Patrick, Boorman, Peter, Ptak, Andy, Chaoul, Laurence, Boreux, Charles, Bounab, Ayoub, Boutelier, Martin, Boyce, Kevin, Brienza, Daniele, Bandler, Simon, Bruijn, Marcel, Gabici, Stefano, Bulgarelli, Andrea, Calarco, Simona, Raulin, Desi, Gloaguen, Emilie, Callanan, Paul, Prada Campello, Alberto, Camus, Thierry, Canourgues, Florent, Capobianco, Vito, Cardiel, Nicolas, Castellani, Florent, Barbera, Marco, Gant, Florent, Simionescu, Aurora, Cheatom, Oscar, Doumayrou, Eric, Chervenak, James, Chiarello, Fabio, Clerc, Laurent, Clerc, Nicolas, Cobo, Beatriz, Coeur-Joly, Odile, Coleiro, Alexis, Colonges, Stéphane, Torrejon, Jose M., Corcione, Leonardo, Gao, Jian-Rong, Puccetti, Simonetta, Barcons, Xavier, Coriat, Mickael, Coynel, Alexandre, Cuttaia, Francesco, D’Ai, Antonino, D’anca, Fabio, Dadina, Mauro, Acero, Fabio, Daniel, Christophe, Dauner, Lea, DeNigris, Natalie, Puccio, Elena, Gastaldello, Fabio, Dercksen, Johannes, Bozzo, Enrico, DiPirro, Michael, Genolet, Ludovic, Durkin, Malcom, van Leeuwen, Bert-Joost, Charles, Ivan, Ghizzardi, Simona, Alcacera Gil, M. Angeles, Giovannini, Elisa, Ramon, Pascale, Godet, Olivier, Gomez-Elvira, Javier, Gonzalez, Raoul, Gonzalez, Manuel, Gottardi, Luciano, Branduardi-Raymont, Graziella, Granat, Dolorès, Fioretti, Valentina, Gros, Michel, Costantini, Elisa, Guignard, Nicolas, Reina, Manuel, Hieltjes, Paul, Hurtado, Adolfo Jesús, Irwin, Kent, Jacquey, Christian, Ettori, Stefano, Janiuk, Agnieszka, Jaubert, Jean, Jiménez, Maria, Geoffray, Hervé, Jolly, Antoine, Jourdan, Thierry, Rioland, Guillaume, Dauser, Thomas, Julien, Sabine, Kedziora, Bartosz, Finoguenov, Alexis, Korb, Andrew, Kreykenbohm, Ingo, König, Ole, Langer, Mathieu, Laudet, Philippe, Jacques, Lionel, Laurent, Philippe, Rodriguez, Louis, Laurenza, Monica, Lesrel, Jean, Etcheverry, Christophe, Decourchelle, Anne, Ligori, Sebastiano, Lorenz, Maximilian, Luminari, Alfredo, Maffei, Bruno, Maisonnave, Océane, Marelli, Lorenzo, Kirsch, Christian, Roig, Anton, Massonet, Didier, Petit, Pascal, Maussang, Irwin, Melchor, Alejandro Gonzalo, Le Mer, Isabelle, Duband, Lionel, San Millan, Francisco Javier, Millerioux, Jean-Pierre, Mineo, Teresa, Minervini, Gabriele, Molin, Alexeï, Gatti, Flavio, Grosso, Nicolas, Smith, Stephen, Monestes, David, Montinaro, Nicola, Mot, Baptiste, Murat, David, Nagayoshi, Kenichiro, Duval, Jean-Marc, Nazé, Yaël, Noguès, Loïc, Pailot, Damien, Kaastra, Jelle, Rollet, Bertrand, Panessa, Francesca, Adams, Joseph, Parodi, Luigi, Roncarelli, Mauro, Dubbeldam, Luc, Hoogeveen, Ruud, Roudil, Gilles, Rudnicki, Tomasz, Sanisidro, Julien, Mazzotta, Pasquale, Sciortino, Luisa, Silva, Vitor, Sordet, Michael, Soto-Aguilar, Javier, Spizzi, Pierre, Goldwurm, Andrea, Dupieux, Michel, Surace, Christian, Svoboda, Jiri, Fernández Sánchez, Miguel, Miller, Jon, Taralli, Emanuele, Terrasa, Guilhem, Terrier, Régis, Todaro, Michela, Ubertini, Pietro, Uslenghi, Michela, Vaate, Jan Geralt Bijd de, Dupourqué, Simon, Vaccaro, Davide, den Hartog, Roland, Miniutti, Giovanni, van der Hulst, Paul, Varisco, Salvatore, Varnière, Peggy, Vibert, Laurent, Vidriales, María, Villa, Fabrizio, Vodopivec, Boris Martin, Volpe, Angela, Durand, Jean Louis, Vries, Cor de, Nicastro, Fabrizio, Wakeham, Nicholas, Walmsley, Gavin, Kiviranta, Mikko, Jackson, Brian, Wise, Michael, Wit, Martin de, Woźniak, Grzegorz, Jonker, Peter, Kilbourne, Caroline, Eckert, Dominique, Sciortino, Salvatore, Korpela, Seppo, Macculi, Claudio, Mendez, Mariano, Mitsuda, Kazuhisa, van der Kuur, Jan, Molendi, Silvano, Pajot, François, Pointecouteau, Etienne, Porter, Frederick, Pratt, Gabriel W., van Loon, Dennis, Eiriz, Valvanera, Prêle, Damien, Ravera, Laurent, Sato, Kosuke, Schaye, Joop, Shinozaki, Keisuke, Ledot, Aurélien, Skup, Konrad, Soucek, Jan, Thibert, Tanguy, Yamaguchi, Hiroya, Vink, Jacco, Ercolani, Eric, Webb, Natalie, Beaumont, Sophie, Piconcelli, Enrico, Ceballos, Maria Teresa, Cucchetti, Edoardo, D’Andrea, Matteo, Eckart, Megan, Ferrando, Philippe, Kammoun, Elias, Lotti, Simone, Mesnager, Jean-Michel, Natalucci, Lorenzo, Lyautey, Bertrand, Pinto, Ciro, Peille, Philippe, Doriese, William, de Plaa, Jelle, Ardellier, Florence, Argan, Andrea, Bellouard, Elise, Carron, Jérôme, Cavazzuti, Elisabetta, Fiorini, Mauro, Khosropanah, Pourya, Encinas Plaza, Jose Miguel, Martin, Sylvain, Parot, Yann, Finkbeiner, Fred, Perry, James, Pinsard, Frederic, Pradines, Alice, Rigano, Manuela, Roelfsema, Peter, Schwander, Denis, Torrioli, Guido, Plaza, Borja, Ullom, Joel, Vera, Isabel, Medinaceli Villegas, Eduardo, Fiocchi, Mariateresa, Sakai, Kazuhiro, Zuchniak, Monika, Brachet, Frank, Lo Cicero, Ugo, van Weers, Henk, Wilms, Joern, Fiore, Fabrizio, Abdoelkariem, Shariefa, Adam, Thomas, Adami, Christophe, Aicardi, Corinne, Fossecave, Hervé, Akamatsu, Hiroki, Merino Alonso, Pablo Eleazar, Amato, Roberta, André, Jérôme, Angelinelli, Matteo, Poyatos, David, Anon-Cancela, Manuel, Yamasaki, Noriko, Anvar, Shebli, Atienza, Ricardo, Attard, Anthony, Franssen, Philippe, Auricchio, Natalia, Balado, Ana, Bancel, Florian, Barusso, Lorenzo Ferrari, Prouvé, Thomas, and Bascuñan, Arturo

Abstract

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. Athena is a versatile observatory designed to address the Hot and Energetic Universe science theme, as selected in November 2013 by the Survey Science Committee. Based on a large format array of Transition Edge Sensors (TES), X-IFU aims to provide spatially resolved X-ray spectroscopy, with a spectral resolution of 2.5 eV (up to 7 keV) over a 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 (i.e. in the course of its preliminary definition phase, so-called B1), 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, such as the instrument efficiency, spectral resolution, energy scale knowledge, count rate capability, non X-ray background and target of opportunity efficiency. Finally, we briefly discuss the ongoing key technology demonstration activities, the calibration and the activities foreseen in the X-IFU Instrument Science Center, touch on communication and outreach activities, the consortium organisation and 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 th

Published
2023

3. Thermal Crosstalk Measurements and Simulations for an X-ray Microcalorimeter Array.

Author

Miniussi, Antoine R., Adams, Joseph S., Bandler, Simon R., Beaumont, Sophie, Chang, Meng P., Chervenak, James A., Finkbeiner, Fred M., Ha, Jong Y., Hummatov, Ruslan, Kelley, Richard L., Kilbourne, Caroline A., Porter, Frederick S., Sadleir, John E., Sakai, Kazuhiro, Smith, Stephen J., Wakeham, Nicholas A., and Wassell, Edward J.

Subjects
CROSSTALK, X-rays, CONFIGURATIONS (Geometry), HEAT, HEAT sinks
Abstract

Arrays of high-density microcalorimeters require careful heat sinking in order to minimize the thermal crosstalk between nearby pixels. For the array of microcalorimeters developed for the Athena X-ray Integral Field Unit instrument, which has more than 3000 pixels on a 275 µm pitch, it is essential to address this problem in order to meet the energy-resolution requirements. The instrument's energy-resolution budget requires that the impact of the thermal crosstalk on the energy resolution be a contribution that, added in quadrature to other energy-resolution contributions, is less than 0.2 eV. This value results in a derived requirement that the ratio between the amplitude of the crosstalk signal to an X-ray pulse (for example at 6 keV) is less than 1 × 10−3 (for the first neighbor), less than 4 × 10−4 (for the diagonal neighbor) and less than 8 × 10−5 (for the second nearest neighbor). We have measured the thermal crosstalk levels between pixels in various geometries and configurations. The results show a crosstalk ratio which is at least a factor of 4 lower than the derived requirement. We also developed a finite element (FEM) 2D thermal model to predict the thermal behavior of large-scale arrays. This model successfully simulates the measured data in terms of pulse amplitude and time constants. [ABSTRACT FROM AUTHOR]

Published
2020
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4. Thermal Impact of Cosmic Ray Interaction with an X-Ray Microcalorimeter Array.

Author

Miniussi, Antoine R., Adams, Joseph S., Bandler, Simon R., Beaumont, Sophie, Chang, Meng P., Chervenak, James A., Finkbeiner, Fred M., Ha, Jong Y., Hummatov, Ruslan, Kelley, Richard L., Kilbourne, Caroline A., Porter, Frederick S., Sadleir, John E., Sakai, Kazuhiro, Smith, Stephen J., Wakeham, Nicholas A., and Wassell, Edward J.

Subjects
X-ray astronomy, COSMIC rays, LAGRANGIAN points, RELATIVISTIC astrophysics, HEAT capacity, ASTROPHYSICS
Abstract

The X-ray Integral Field Unit (X-IFU) instrument on the Athena mission will be positioned at the Lagrangian point L2 and be subject to cosmic rays generated by astrophysics sources, primarily relativistic protons. Previous simulations have shown that particles of energy higher than 150 MeV will make it through the outer layers of the satellite. They will reach the detector wafer with a rate of 3 cts cm−2 s−1 and a most probable energy deposited in the Si frame supporting the array at 150 keV. These events can affect the energy resolution of the detectors through the thermal fluctuations that they produce. This study assesses this potential problem and discusses two suggested design approaches to decrease the impact of cosmic ray in order to limit their effect to their allocation of 0.2 eV within the Athena/X-IFU energy-resolution budget. The first is the addition of a coating layer of high heat capacity material (e.g., Pd) and the second is the splitting of this coating into two thermal regions near the TES array to keep the heat away from the array. Implementing these two features is predicted to cause a decrease in the number of events above 1 µK by more than a factor 10 to ~ 1.5 cps when compared to an equivalent design without these features. [ABSTRACT FROM AUTHOR]

Published
2020
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5. Design of Magnetic Shielding and Field Coils for a TES X-ray Microcalorimeter Test Platform.

Author

Miniussi, Antoine R., Adams, Joseph S., Bandler, Simon R., Chervenak, James A., Datesman, Aaron M., Doriese, William B., Eckart, Megan E., Finkbeiner, Fred M., Kelley, Richard L., Kilbourne, Caroline A., Porter, Frederick S., Sadleir, John E., Sakai, Kazuhiro, Smith, Stephen J., Wakeham, Nicholas A., Wassell, Edward J., van Weers, Henk J., and Yoon, Wonsik

Subjects
MAGNETIC shielding, MAGNETIC fields, CALORIMETERS, ELECTROMAGNETS, X-rays, MAGNETIC traps, CRYOGENICS
Abstract

The performance of transition-edge sensors (TES) and their SQUID multiplexed readouts is very sensitive to ambient magnetic field and its fluctuations. In order to run ground experiments on thousands of X-ray TES microcalorimeters with a small uniform ambient magnetic field (< 1 μT, with a uniformity < 0.1 μT), we need a very low ambient field to be trapped into the superconducting magnetic shields. We have designed a sub-Kelvin test platform to reach these specifications. For this purpose, we modeled a new design for the shielding consisting of a series of different mu-metal and superconducting shields, including a niobium shield at 50 mK, a cryoperm (A4K) shield at 3 K, and a mu-metal shield at 300 K. A magnetic field coil is used to vary the local perpendicular magnetic field over the TES array. To optimize this field, we have studied a number of different field-coil designs and the impact of the different shield geometries, in order to reach the required field uniformity. [ABSTRACT FROM AUTHOR]

Published
2019
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6. Performance of an X-ray Microcalorimeter with a 240 μm Absorber and a 50 μm TES Bilayer.

Author

Miniussi, Antoine R., Adams, Joseph S., Bandler, Simon R., Chervenak, James A., Datesman, Aaron M., Eckart, Megan E., Ewin, Audrey J., Finkbeiner, Fred M., Kelley, Richard L., Kilbourne, Caroline A., Porter, Frederick S., Sadleir, John E., Sakai, Kazuhiro, Smith, Stephen J., Wakeham, Nicholas A., Wassell, Edward J., and Yoon, Wonsik

Subjects
CALORIMETERS, ASTROPHYSICS, SILICON nitride, NITRIDES, THERMAL conductivity
Abstract

Superconducting transition-edge sensor (TES) microcalorimeters are being developed for a variety of potential astrophysics missions, including Athena. The X-ray integral field unit instrument on this mission requires close-packed pixels on a 0.25 mm pitch, and high quantum efficiency between 0.2 and 12 keV. In this work, we describe a new approach with 50 μm square TESs consisting of a Mo/Au bilayer, deposited on silicon nitride membranes to provide a weak thermal conductance to a ~ 50 mK heat bath. Larger TESs usually have additional normal metal stripes on top of the bilayer to reduce the noise. However, we have found that excellent spectral performance can be achieved without the need for any normal metal stripes on top of the TES. A spectral performance of 1.58 ± 0.12 eV at 5.9 keV has been achieved, the best resolution seen in any of our devices with this pixel size. [ABSTRACT FROM AUTHOR]

Published
2018
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7. The Magnetically-Tuned Transition-Edge Sensor.

Author

Sadleir, John E., Sang-Jun Lee, Smith, Stephen J., Busch, Sarah E., Bandler, Simon R., Adams, Joseph S., Eckart, Megan E., Chervenak, James A., Kelley, Richard L., Kilbourne, Caroline A., Porter, Frederick S., and Porst, Jan-Patrick

Subjects
PARTICLE detectors, CRYOGENICS, MAGNETIC fields, SUPERCONDUCTING junction devices, RESISTIVE force, PARAMETER estimation
Abstract

We present the first measurements on the proposed magnetically-tuned superconducting transition-edge sensor and compare the modified resistive transition with the theoretical prediction (Sadleir et al., IEEE Trans App Supercond 23:2101405, ). A TES's resistive transition is customarily characterized in terms of the unitless device parameters α and β corresponding to the resistive response to changes in temperature and current respectively. We present a new relationship between measured IV quantities (sensor current I and voltage V) and the parameters α and β and use these relations to confirm we have stably biased a TES with negative β parameter with magnetic tuning. Motivated by access to this new unexplored parameter space, we investigate the conditions for bias stability of a TES taking into account both self and externally applied magnetic fields. [ABSTRACT FROM AUTHOR]

Published
2014
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8. The High-Resolution X-Ray Microcalorimeter Spectrometer, SXS, on Astro-H.

Author

Mitsuda, Kazuhisa, Kelley, Richard, Boyce, Kevin, Brown, Gregory, Costantini, Elisa, DiPirro, Michael, Ezoe, Yuichiro, Fujimoto, Ryuichi, Gendreau, Keith, Herder, Jan-Willem, Hoshino, Akio, Ishisaki, Yoshitaka, Kilbourne, Caroline, Kitamoto, Shunji, McCammon, Dan, Murakami, Masahide, Murakami, Hiroshi, Ogawa, Mina, Ohashi, Takaya, and Okamoto, Atsushi

Subjects
CALORIMETERS, X-ray spectrometers, ASTROPHYSICS, X-ray telescopes, TURBULENCE, GALAXY clusters, FORCE & energy
Abstract

The science and an overview of the Soft X-ray Spectrometer onboard the STRO-H mission are presented. The SXS consists of X-ray focusing mirrors and a microcalorimeter array and is developed by international collaboration lead by JAXA and NASA with European participation. The detector is a 6×6 format microcalorimeter array operated at a cryogenic temperature of 50 mK and covers a 3′×3′ field of view of the X-ray telescope of 5.6 m focal length. We expect an energy resolution better than 7 eV (FWHM, requirement) with a goal of 4 eV. The effective area of the instrument will be 225 cm at 7 keV; by a factor of about two larger than that of the X-ray microcalorimeter on board Suzaku. One of the main scientific objectives of the SXS is to investigate turbulent and/or macroscopic motions of hot gas in clusters of galaxies. [ABSTRACT FROM AUTHOR]

Published
2012
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