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33 results on '"Kilbourne, Caroline"'

1. Circumgalactic Medium on the Largest Scales: Detecting X-ray Absorption Lines with Large-Area Microcalorimeters

Author: Bogdan, Akos, Khabibullin, Ildar, Kovacs, Orsolya, Schellenberger, Gerrit, ZuHone, John, Burchett, Joseph, Dolag, Klaus, Churazov, Eugene, Forman, William, Jones, Christine, Kilbourne, Caroline, Kraft, Ralph, Lau, Erwin, Markevitch, Maxim, McCammon, Dan, Nagai, Daisuke, Nelson, Dylan, Ogorzalek, Anna, Oppenheimer, Benjamin, Sarkar, Arnab, Su, Yuanyuan, Truong, Nhut, Veilleux, Sylvain, Vladutescu-Zopp, Stephan, and Zhuravleva, Irina
Subjects: High Energy Astrophysical Phenomena (astro-ph.HE), Astrophysics of Galaxies (astro-ph.GA), FOS: Physical sciences, Astrophysics - High Energy Astrophysical Phenomena, Astrophysics - Astrophysics of Galaxies
Abstract: The circumgalactic medium (CGM) plays a crucial role in galaxy evolution as it fuels star formation, retains metals ejected from the galaxies, and hosts gas flows in and out of galaxies. For Milky Way-type and more massive galaxies, the bulk of the CGM is in hot phases best accessible at X-ray wavelengths. However, our understanding of the CGM remains largely unconstrained due to its tenuous nature. A promising way to probe the CGM is via X-ray absorption studies. Traditional absorption studies utilize bright background quasars, but this method probes the CGM in a pencil beam, and, due to the rarity of bright quasars, the galaxy population available for study is limited. Large-area, high spectral resolution X-ray microcalorimeters offer a new approach to exploring the CGM in emission and absorption. Here, we demonstrate that the cumulative X-ray emission from cosmic X-ray background sources can probe the CGM in absorption. We construct column density maps of major X-ray ions from the Magneticum simulation and build realistic mock images of nine galaxies to explore the detectability of X-ray absorption lines arising from the large-scale CGM. We conclude that the OVII absorption line is detectable around individual massive galaxies at the $3\sigma-6\sigma$ confidence level. For Milky Way-type galaxies, the OVII and OVIII absorption lines are detectable at the $\sim\,6\sigma$ and $\sim\,3\sigma$ levels even beyond the virial radius when co-adding data from multiple galaxies. This approach complements emission studies, does not require additional exposures, and will allow probing of the baryon budget and the CGM at the largest scales., Comment: 16 pages, 8 figures, accepted for publication in ApJ
Published: 2023

2. Ground test results of the electromagnetic interference for the x-ray microcalorimeter onboard XRISM

Author: Kurihara, Miki, Tsujimoto, Masahiro, Eckart, Megan E., Kilbourne, Caroline A., Matsuda, Frederick T., McLaughlin, Brian, Oguri, Shugo, Porter, Frederick S., Takei, Yoh, and Kochibe, Yoichi
Subjects: FOS: Physical sciences, Astrophysics - Instrumentation and Methods for Astrophysics, Instrumentation and Methods for Astrophysics (astro-ph.IM)
Abstract: Electromagnetic interference (EMI) for low-temperature detectors is a serious concern in many missions. We investigate the EMI caused by the spacecraft components to the x-ray microcalorimeter of the Resolve instrument onboard the X-Ray Imaging and Spectroscopy Mission (XRISM), which is currently under development by an international collaboration and is planned to be launched in 2023. We focus on the EMI from (a) the low-frequency magnetic field generated by the magnetic torquers (MTQ) used for the spacecraft attitude control and (b) the radio-frequency (RF) electromagnetic field generated by the S and X band antennas used for communication between the spacecraft and the ground stations. We executed a series of ground tests both at the instrument and spacecraft levels using the flight-model hardware in 2021-2022 in a JAXA facility in Tsukuba. We also conducted electromagnetic simulations partially using the Fugaku high-performance computing facility. The MTQs were found to couple with the microcalorimeter, which we speculate through pick-ups of low-frequency magnetic field and further capacitive coupling. There is no evidence that the resultant energy resolution degradation is beyond the current allocation of noise budget. The RF communication system was found to leave no significant effect. We present the result of the tests and simulation in this article., JATIS in press
Published: 2023

3. Ground test results of the micro-vibration interference for the x-ray microcalorimeter onboard XRISM

Author: Hasebe, Takashi, Imamura, Ryuta, Tsujimoto, Masahiro, Awaki, Hisamitsu, Chiao, Meng P., Fujimoto, Ryuichi, Hartz, Leslie S., Kilbourne, Caroline A., Sneiderman, Gary A., Takei, Yoh, and Yasuda, Susumu
Subjects: FOS: Physical sciences, Astrophysics - Instrumentation and Methods for Astrophysics, Instrumentation and Methods for Astrophysics (astro-ph.IM)
Abstract: Resolve is a payload hosting an X-ray microcalorimeter detector operated at 50 mK in the X-Ray Imaging and Spectroscopy Mission (XRISM). It is currently under development as part of an international collaboration and is planned to be launched in 2023. A primary technical concern is the micro-vibration interference in the sensitive microcalorimeter detector caused by the spacecraft bus components. We conducted a series of verification tests in 2021-2022 on the ground, the results of which are reported here. We defined the micro-vibration interface between the spacecraft and the Resolve instrument. In the instrument-level test, the flight-model hardware was tested against the interface level by injecting it with micro-vibrations and evaluating the instrument response using the 50 mK stage temperature stability, ADR magnet current consumption rate, and detector noise spectra. We found strong responses when injecting micro-vibration at about 200, 380, and 610 Hz. In the former two cases, the beat between the injected frequency and cryocooler frequency harmonics were observed in the detector noise spectra. In the spacecraft-level test, the acceleration and instrument responses were measured with and without suspension of the entire spacecraft. The reaction wheels (RWs) and inertial reference units (IRUs), two major sources of micro-vibration among the bus components, were operated. In conclusion, the observed responses of Resolve are within the acceptable levels in the nominal operational range of the RWs and IRUs. There is no evidence that the resultant energy resolution degradation is beyond the current allocation of noise budget., Journal of Astronomical Telescopes, Instruments, and Systems, Vol. 9, Issue 1, 014003 (March 2023)
Published: 2023

4. Line Emission Mapper (LEM): Probing the physics of cosmic ecosystems

Author: Kraft, Ralph, Markevitch, Maxim, Kilbourne, Caroline, Adams, Joseph S., Akamatsu, Hiroki, Ayromlou, Mohammadreza, Bandler, Simon R., Barbera, Marco, Bennett, Douglas A., Bhardwaj, Anil, Biffi, Veronica, Bodewits, Dennis, Bogdan, Akos, Bonamente, Massimiliano, Borgani, Stefano, Branduardi-Raymont, Graziella, Bregman, Joel N., Burchett, Joseph N., Cann, Jenna, Carter, Jenny, Chakraborty, Priyanka, Churazov, Eugene, Crain, Robert A., Cumbee, Renata, Dave, Romeel, DiPirro, Michael, Dolag, Klaus, Doriese, W. Bertrand, Drake, Jeremy, Dunn, William, Eckart, Megan, Eckert, Dominique, Ettori, Stefano, Forman, William, Galeazzi, Massimiliano, Gall, Amy, Gatuzz, Efrain, Hell, Natalie, Hodges-Kluck, Edmund, Jackman, Caitriona, Jahromi, Amir, Jennings, Fred, Jones, Christine, Kaaret, Philip, Kavanagh, Patrick J., Kelley, Richard L., Khabibullin, Ildar, Kim, Chang-Goo, Koutroumpa, Dimitra, Kovacs, Orsolya, Kuntz, K. D., Lau, Erwin, Lee, Shiu-Hang, Leutenegger, Maurice, Lin, Sheng-Chieh, Lisse, Carey, Cicero, Ugo Lo, Lovisari, Lorenzo, McCammon, Dan, McEntee, Sean, Mernier, Francois, Miller, Eric D., Nagai, Daisuke, Negro, Michela, Nelson, Dylan, Ness, Jan-Uwe, Nulsen, Paul, Ogorzalek, Anna, Oppenheimer, Benjamin D., Oskinova, Lidia, Patnaude, Daniel, Pfeifle, Ryan W., Pillepich, Annalisa, Plucinsky, Paul, Pooley, David, Porter, Frederick S., Randall, Scott, Rasia, Elena, Raymond, John, Ruszkowski, Mateusz, Sakai, Kazuhiro, Sarkar, Arnab, Sasaki, Manami, Sato, Kosuke, Schellenberger, Gerrit, Schaye, Joop, Simionescu, Aurora, Smith, Stephen J., Steiner, James F., Stern, Jonathan, Su, Yuanyuan, Sun, Ming, Tremblay, Grant, Truong, Nhut, Tutt, James, Ursino, Eugenio, Veilleux, Sylvain, Vikhlinin, Alexey, Vladutescu-Zopp, Stephan, Vogelsberger, Mark, Walker, Stephen A., Weaver, Kimberly, Weigt, Dale M., Werk, Jessica, Werner, Norbert, Wolk, Scott J., Zhang, Congyao, Zhang, William W., Zhuravleva, Irina, and ZuHone, John
Subjects: High Energy Astrophysical Phenomena (astro-ph.HE), Astrophysics of Galaxies (astro-ph.GA), FOS: Physical sciences, Astrophysics - Instrumentation and Methods for Astrophysics, Astrophysics - High Energy Astrophysical Phenomena, Instrumentation and Methods for Astrophysics (astro-ph.IM), Astrophysics - Astrophysics of Galaxies
Abstract: The Line Emission Mapper (LEM) is an X-ray Probe for the 2030s that will answer the outstanding questions of the Universe's structure formation. It will also provide transformative new observing capabilities for every area of astrophysics, and to heliophysics and planetary physics as well. LEM's main goal is a comprehensive look at the physics of galaxy formation, including stellar and black-hole feedback and flows of baryonic matter into and out of galaxies. These processes are best studied in X-rays, and emission-line mapping is the pressing need in this area. LEM will use a large microcalorimeter array/IFU, covering a 30x30' field with 10" angular resolution, to map the soft X-ray line emission from objects that constitute galactic ecosystems. These include supernova remnants, star-forming regions, superbubbles, galactic outflows (such as the Fermi/eROSITA bubbles in the Milky Way and their analogs in other galaxies), the Circumgalactic Medium in the Milky Way and other galaxies, and the Intergalactic Medium at the outskirts and beyond the confines of galaxies and clusters. LEM's 1-2 eV spectral resolution in the 0.2-2 keV band will make it possible to disentangle the faintest emission lines in those objects from the bright Milky Way foreground, providing groundbreaking measurements of the physics of these plasmas, from temperatures, densities, chemical composition to gas dynamics. While LEM's main focus is on galaxy formation, it will provide transformative capability for all classes of astrophysical objects, from the Earth's magnetosphere, planets and comets to the interstellar medium and X-ray binaries in nearby galaxies, AGN, and cooling gas in galaxy clusters. In addition to pointed observations, LEM will perform a shallow all-sky survey that will dramatically expand the discovery space., 18 pages. White paper for a mission concept to be submitted for the 2023 NASA Astrophysics Probes opportunity. v2: All-sky survey figure expanded, references fixed. v3: Added energy resolution measurements for prototype detector array. v4: Author list and reference fixes
Published: 2022

5. First Flight Performance of the Micro-X Microcalorimeter X-Ray Sounding Rocket

Author: Adams, Joseph S., Baker, Robert, Bandler, Simon R., Bastidon, Noemie, Castro, Daniel, Danowksi, Meredith E., Doriese, William B., Eckart, Megan E., Figueroa-Feliciano, Enectali, Fuhrman, Joshua, Goldfinger, David C., Heine, Sarah N. T., Hilton, Gene, Hubbard, Antonia J. F., Jardin, Daniel, Kelley, Richard L., Kilbourne, Caroline A., Leman, Steven W., Manzagol-Harwood, Renee E., McCammon, Dan, Oakley, Philip H. H., Okajima, Takashi, Porter, Frederick Scott, Reintsema, Carl D., Rutherford, John, Saab, Tarek, Sato, Kosuke, Serlemitsos, Peter, Smith, Stephen J., Soong, Yang, and Wikus, Patrick
Subjects: FOS: Physical sciences, Astrophysics - Instrumentation and Methods for Astrophysics, Instrumentation and Methods for Astrophysics (astro-ph.IM)
Abstract: The flight of the Micro-X sounding rocket on July 22, 2018 marked the first operation of Transition-Edge Sensors and their SQUID readouts in space. The instrument combines the microcalorimeter array with an imaging mirror to take high-resolution spectra from extended X-ray sources. The first flight target was the Cassiopeia~A Supernova Remnant. While a rocket pointing malfunction led to no time on-target, data from the flight was used to evaluate the performance of the instrument and demonstrate the flight viability of the payload. The instrument successfully achieved a stable cryogenic environment, executed all flight operations, and observed X-rays from the on-board calibration source. The flight environment did not significantly affect the performance of the detectors compared to ground operation. The flight provided an invaluable test of the impact of external magnetic fields and the instrument configuration on detector performance. This flight provides a milestone in the flight readiness of these detector and readout technologies, both of which have been selected for future X-ray observatories.
Published: 2022
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6. X線分光撮像衛星(XRISM)搭載Resolveの開発状況

Author: KELLEY, Richard L., BIALAS, Thomas G., BROWN, Gregory V., CHAO, Meng P., COSTANTINI, Elisa, HERDER, Jan-Willem den, DIPIRRO, Michael J., EKART, Megan E., FERRIGNO, Carlo, GRAHAM, Steven M., GRIM, Martin, KILBOURNE, Caroline A., LEUTENEGGER, Maurice A., PALTANI, Stephane, PORTER, F. Scott, SHIRRON, PeterJ., SNEIDERMAN, Gary J., SOONG, Yang, SZYMKOWIAK, Andrew E., CorP., de Vries, ISHIZAKI, Yoshitaka, AKAMATSU, Hiroki, AWAKI, Hisamitsu, EZOE, Yuichiro, FUJIMOTO, Ryuichi, FURUZAWA, Akihiro, HAYASHI, Takayoshi, HORIUCHI, Takashi, HOSHINO, Akio, ICHINOHE, Yuto, IIZUKA, Ryo, ISHIDA, Manabu, ISHIKAWA, Kumi, KITAMOTO, Shunji, MITSUISHI, Ikuyuki, MIZUMOTO, Misaki, MORI, Hideyuki, OHASHI, Takaya, OKAJIMA, Takashi, SATO, Kosuke, SAWADA, Makoto, SETA, Hiromi, TAKEI, Yo, TAMAGAWA, Toru, TSUJIMOTO, Masahiro, UCHIDA, Yusuke, YAMADA, Shinya, YAMASAKI, Noriko, YASUDA, Susumu, and YOSHIOKA, Nasa
Abstract: 第21回宇宙科学シンポジウム (2021年1月6日-7日. オンライン開催), 21st Space Science Symposium (January 6-7, 2021. Online Meeting), 著者人数: 50名, 資料番号: SA6000163128, レポート番号: g21-1
Published: 2021

7. In-orbit Operation of the Soft X-ray Spectrometer onboard the Hitomi satellite

Author: Kelley, Richard L., den, Herder Jan-Willem, Bialas, Thomas G., Boyce, Kevin R., Chiao, Meng P., de, Vries Cor P., DiPirro, Michael J., Eckart, Megan E., Kilbourne, Caroline A., Leutenegger, Maurice A., Masters, Candace M., Porter, Frederick S., Savinell, Joseph C., Shirron, Peter J., Sneiderman, Gary A., Tsujimoto, Masahiro, Mitsuda, Kazuhisa, Ezoe, Yuichiro, Fujimoto, Ryuichi, Hoshino, Akio, Ishikawa, Kumi, Ishisaki, Yoshitaka, Koyama, Shu, Mitsuishi, Ikuyuki, Noda, Hirofumi, Okajima, Takashi, Okamoto, Atsushi, Porter, Frederic S., Sato, Kosuke, Sato, Yohichi, Sawada, Makoto, Seta, Hiromi, Takei, Yoh, Tamagawa, Toru, Tashiro, Makoto S., Watanabe, Tomomi, Yamada, Shinya, Yamasaki, Noriko Y., and Yatsu, Yoichi
Subjects: Physics, Soft x ray, x-ray microcalorimeter, Spectrometer, Mechanical Engineering, Space operations, Astronomy and Astrophysics, 02 engineering and technology, 021001 nanoscience & nanotechnology, 01 natural sciences, Electronic, Optical and Magnetic Materials, 010309 optics, soft x-ray spectrometer, Short lifetime, Hitomi, Space and Planetary Science, Control and Systems Engineering, 0103 physical sciences, Orbit (dynamics), Satellite, in-orbit operations, 0210 nano-technology, Instrumentation, Remote sensing
Abstract: 形態: カラー図版あり, Physical characteristics: Original contains color illustrations, Accepted: 2017-10-13, 資料番号: PA1810023000
Published: 2017

8. 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

9. X線分光撮像衛星 (XRISM) 搭載 Resolve の開発状況

Author: KELLEY, Richard L., BIALAS, Thomas G., BROWN, Gregory V., CHIAO, Meng P., CONSTANTINI, Elisa, DENHERDER, Jan-Willem, DIPIRRO, Michael J., ECKART, Megan E., FERRIGNO, Carlo, GRAHAM, Steven M., GRIM, Martin, KILBOURNE, Caroline A., LEUTENEGGER, Maurice A., MCCMMON, Dan, PALTANI, Stephane, PORTER, F. Scott, SHIRRON, Peter J., SNEIDERMAN, Gary A., SOONG, Yang, SZYMKOWIAK, Andrew E., VRIES, Cor P. de, ISHISAKI, Yoshitaka, AKAMATSU, Hiroki, AWAKI, HIisamitsu, COSTANTINI, Elisa, DEN, HERDER Jan-William, EZOE, Yuichiro, FUJIMOTO, Ryuichi, FURUZAWA, Akihiro, HAYASHI, Takayuki, HORIUCHI, Takafumi, HOSHINO, Akio, ICHINOHE, Yuto, IIZUKA, Ryo, ISHIBASHI, Kazunori, ISHIDA, Manabu, ISHIKAWA, Kumi, KITAMOTO, Shunji, MAEDA, Yoshitomo, MCCAMMON, Dan, MITSUISHI, Ikuyuki, MORI, Hideyuki, OHASHI, Takaya, OKAJIMA, Takashi, SATO, Kosuke, SAWADA, Makoto, SETA, Hiromi, SHIBANO, Yasuko, TAKEI, Yoh, TAMAGAWA, Toru, TSUJIMOTO, Masahiro, UCHIDA, Yuusuke, YAMADA, Shinya, YAMASAKI, Noriko Y., YASUDA, Susumu, and YOSHIOKA, Nasa
Abstract: 第19回宇宙科学シンポジウム (2019年1月9日-10日. 宇宙航空研究開発機構宇宙科学研究所(JAXA)(ISAS)相模原キャンパス), 相模原市, 神奈川県, 19th Space Science Symposium (January 9-10, 2019. Institute of Space and Astronautical Science, Japan Aerospace Exploration Agency(JAXA)(ISAS)Sagamihara Campus), Sagamihara, Kanagawa Japan, 著者人数: 53名, 資料番号: SA6000144056, レポート番号: P-020
Published: 2019

10. The Athena X-ray Integral Field Unit

Author: Barret, Didier, Trong, Thien Lam, Den Herder, Jan-Willem, Piro, Luigi, Cappi, Massimo, Huovelin, Juhani, Kelley, Richard, Miguel Mas-Hesse, J., 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, 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, Benot, 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, Natalucci, Lorenzo, Institut de recherche en astrophysique et planétologie (IRAP), Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Observatoire Midi-Pyrénées (OMP), Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS), Centre National d'Études Spatiales [Toulouse] (CNES), Institut Nanosciences et Cryogénie (INAC), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Grenoble Alpes (UGA), Astrophysique Interprétation Modélisation (AIM (UMR_7158 / UMR_E_9005 / UM_112)), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), AstroParticule et Cosmologie (APC (UMR_7164)), Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire Midi-Pyrénées (OMP), Institut de Recherche pour le Développement (IRD)-Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Institut de Recherche pour le Développement (IRD)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Centre National de la Recherche Scientifique (CNRS), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Grenoble Alpes [2016-2019] (UGA [2016-2019]), Astrophysique Interprétation Modélisation (AIM (UMR7158 / UMR_E_9005 / UM_112)), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris Diderot - Paris 7 (UPD7), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7), Institut national des sciences de l'Univers (INSU - CNRS)-Université Toulouse III - Paul Sabatier (UT3), Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Centre National de la Recherche Scientifique (CNRS), and Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Université de Paris (UP)
Subjects: High Energy Astrophysical Phenomena (astro-ph.HE), Cosmology and Nongalactic Astrophysics (astro-ph.CO), Astrophysics of Galaxies (astro-ph.GA), FOS: Physical sciences, [PHYS.PHYS.PHYS-INS-DET]Physics [physics]/Physics [physics]/Instrumentation and Detectors [physics.ins-det], Astrophysics - Instrumentation and Methods for Astrophysics, Astrophysics - High Energy Astrophysical Phenomena, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Astrophysics - Astrophysics of Galaxies, Instrumentation and Methods for Astrophysics (astro-ph.IM), Astrophysics - Cosmology and Nongalactic Astrophysics
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., 15 pages, 5 figures, to appear in Proc. SPIE Astronomical Telescopes and Instrumentation, Austin 2018
Published: 2018
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11. Design and on-orbit operation of the soft x-ray spectrometer adiabatic demagnetization refrigerator on the Hitomi observatory

Author: Shirron, Peter John, Kimball, Mark O., James, Bryan L., Muench, Theodore, Canavan, Edgar R., DiPirro, Michael J., Bialas, Thomas A., Sneiderman, Gary A., Boyce, Kevin R., Kilbourne, Caroline Anne, Porter, Frederick S., Fujimoto, Ryuichi, Takei, Yoh, Yoshida, Seiji, and Mitsuda, Kazuhisa
Subjects: Materials science, Nuclear engineering, Refrigerator car, chemistry.chemical_element, Cryogenics, Heat sink, microcalorimeter, 01 natural sciences, law.invention, 010309 optics, Operating temperature, law, 0103 physical sciences, 010306 general physics, Instrumentation, Helium, Spectrometer, Liquid helium, Mechanical Engineering, Astronomy and Astrophysics, Cryocooler, Electronic, Optical and Magnetic Materials, adiabatic demagnetization refrigerator, astronomy, chemistry, x-ray, Space and Planetary Science, Control and Systems Engineering
Abstract: 著者人数: 15名, Accepted: 2018-02-19, 資料番号: SA1180074000
Published: 2018

12. Cryogen-free operation of the Soft X-ray Spectrometer instrument

Author: Sneiderman, Gary A., Shirron, Peter J., Bialas, Thomas G., Boyce, Kevin R., Chiao, Meng P., DiPirro, Michael J., Eckart, Megan E., Hartz, Leslie, Kilbourne, Caroline A., Masters, Candace, McCammon, Dan, Porter, Frederick S., Szymkowiak, Andrew E., Fujimoto, Ryuichi, Ishisaki, Yoshitaka, Mitsuda, Kazuhisa, Noda, Hirofumi, Takei, Yoh, Tsujimoto, Mashiro, and Yoshida, Seiji
Subjects: Cryostat, Materials science, Nuclear engineering, chemistry.chemical_element, Cryogenics, Heat sink, magnetic refrigeration, law.invention, cooling system, law, Water cooling, cryocooler, cryogenic, Soft X-ray Spectrometer, cryogen free, Instrumentation, Helium, Spectrometer, Liquid helium, Mechanical Engineering, Astronomy and Astrophysics, Cryocooler, Astro-H, Electronic, Optical and Magnetic Materials, adiabatic demagnetization refrigerator, chemistry, Space and Planetary Science, Control and Systems Engineering
Abstract: 著者人数: 20名, Accepted: 2018-02-22, 資料番号: SA1180075000
Published: 2018

13. In-flight calibration of Hitomi Soft X-ray Spectrometer. (1) Background

Author: Kilbourne, Caroline A., Angellini, Lorella, Boyce, Kevin R., Eckart, Megan E., Kelley, Richard L., Koyama, Shu, Leutenegger, Maurice A., Loewenstein, Michael, MacCammon, Dan, Porter, Frederick S., Sawada, Makoto, Tsujimoto, Masahiro, Fujimoto, Ryuichi, Ishisaki, Yoshitaka, Mitsuda, Kazuhisa, Nakashima, Shinya, Seta, Hiromi, Takei, Yoh, Tashiro, Makoto S., Terada, Yukikatsu, Yamada, Shinya, and Yamasaki, Noriko Y.
Subjects: Physics, Soft x ray, Spectrometer, Astrophysics::High Energy Astrophysical Phenomena, Astronomy and Astrophysics, Astrophysics, 01 natural sciences, Spectral line, Calorimeter, 010309 optics, Background spectrum, Space and Planetary Science, 0103 physical sciences, Calibration, methods: observational, space vehicles: instruments, Spectral resolution, 010303 astronomy & astrophysics, instrumentation: spectrographs
Abstract: 著者人数: 22名, Accepted: 2017-11-01, 資料番号: SA1170315000
Published: 2018
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14. In-flight performance of the soft x-ray spectrometer detector system on Astro-H

Author: Porter, Frederick S., Boyce, Kevin R., Chiao, Meng P., Eckart, Megan E., Kilbourne, Caroline Anne, Leutenegger, Maurice A., McCammon, Daniel, Sneiderman, Gary A., Szymkowiak, Andrew E., Watanabe, Tomomi, Fujimoto, Ryuichi, Ishisaki, Yoshitaka, Mitsuda, Kazuhisa, Sato, Kosuke, Seta, Hiromi, Sawada, Makoto, Takei, Yoh, Tashiro, Makoto S., Tsujimoto, Masahiro, and Yamada, Shinya
Subjects: Physics::Instrumentation and Detectors, Astrophysics::High Energy Astrophysical Phenomena, X-ray detector, 02 engineering and technology, x-ray spectroscopy, 01 natural sciences, 010309 optics, Optics, Interference (communication), Observatory, 0103 physical sciences, Calibration, x-ray astrophysics, Instrumentation, Physics, Spacecraft, Spectrometer, business.industry, x-ray detectors, Mechanical Engineering, Detector, Astronomy and Astrophysics, 021001 nanoscience & nanotechnology, Electronic, Optical and Magnetic Materials, Calorimeter, Space and Planetary Science, Control and Systems Engineering, Astrophysics::Earth and Planetary Astrophysics, 0210 nano-technology, business
Abstract: 著者人数: 20名, Accepted: 2018-01-19, 資料番号: SA1170308000
Published: 2018

15. In-flight performance of pulse-processing system of the ASTRO-H/Hitomi soft x-ray spectrometer

Author: Kato, Yuka, Boyce, Kevin R., Chiao, Meng P., Watanabe, Tomomi, Leutenegger, Maurice A., Eckart, Megan E., Porter, Frederick Scott, Kilbourne, Caroline Anne, Ishisaki, Yoshitaka, Yamada, Shinya, Seta, Hiromi, Tashiro, Makoto S., Takeda, Sawako, Terada, Yukikatsu, Tsujimoto, Masahiro, Koyama, Shu, Mitsuda, Kazuhisa, and Sawada, Makoto
Subjects: Complex event processing, 02 engineering and technology, microcalorimeter, 01 natural sciences, SpaceWire, 010309 optics, 0103 physical sciences, Calibration, Instrumentation, Simulation, Physics, Signal processing, Spectrometer, Spacecraft, business.industry, Mechanical Engineering, Computer Science::Software Engineering, Astronomy and Astrophysics, 021001 nanoscience & nanotechnology, Electronic, Optical and Magnetic Materials, pulse processing, x-ray, Space and Planetary Science, Control and Systems Engineering, Orbit (dynamics), Central processing unit, 0210 nano-technology, business
Abstract: 著者人数: 18名, Accepted: 2018-01-19, 資料番号: SA1170307000
Published: 2018

16. Ground calibration of the Astro-H (Hitomi) soft x-ray spectrometer

Author: Eckart, Megan E., Adams, Joseph S., Boyce, Kevin R., Brown, Gregory V., Chiao, Meng P., Haas, Daniel A., den, Herder Jan-Willem A., Kilbourne, Caroline A., Leutenegger, Maurice A., McCammon, Daniel, Porter, F. Scott, Sneiderman, Gary A., Szymkowiak, Andrew E., de, Vries Cor P., Watanabe, Tomomi, Fujimoto, Ryuichi, Hoshino, Akio, Ishisaki, Yoshitaka, Kitamoto, Shunji, Mitsuda, Kazuhisa, Sato, Kosuke, Sawada, Makoto, Seta, Hiromi, Takei, Yoh, Tashiro, Makoto S., Tsujimoto, Masahiro, Yamada, Shinya, and Yamasaki, Noriko Y.
Subjects: Materials science, Physics::Instrumentation and Detectors, Astrophysics::High Energy Astrophysical Phenomena, x-ray spectroscopy, microcalorimeter, 01 natural sciences, law.invention, Telescope, detectors, calibration, Optics, law, 0103 physical sciences, Calibration, Spectral resolution, 010306 general physics, Optical filter, 010303 astronomy & astrophysics, Instrumentation, Spectrometer, business.industry, Mechanical Engineering, Thermistor, Detector, Astrophysics::Instrumentation and Methods for Astrophysics, Astronomy and Astrophysics, Synchrotron, Electronic, Optical and Magnetic Materials, Space and Planetary Science, Control and Systems Engineering, business
Abstract: 著者人数: 28名, Accepted: 2018-02-22, 資料番号: SA1170305000
Published: 2018

17. In-flight Calibration of Hitomi Soft X-ray Spectrometer (3) Effective Area

Author: Eckart, Megan E., Kelley, Richard L., Kilbourne, Caroline A., Leutenegger, Maurice A., Porter, Frederick S., Serlemitsos, Peter J., Szymkowiak, Andrew, Yaqoob, Tahir, Tsujimoto, Masahiro, Okajima, Takashi, Hayashi, Takayuki, Hoshino, Akio, Iizuka, Ryo, Maeda, Yoshitomo, Mori, Hideyuki, Sato, Kosuke, and Sato, Toshiki
Subjects: Physics, High Energy Astrophysical Phenomena (astro-ph.HE), Spectrometer, Astrophysics::High Energy Astrophysical Phenomena, Antenna aperture, Continuum (design consultancy), Flux, FOS: Physical sciences, Astronomy and Astrophysics, 01 natural sciences, Computational physics, 010309 optics, Crab Nebula, Space and Planetary Science, 0103 physical sciences, Calibration, Satellite, methods: observational, space vehicles: instruments, Astrophysics - Instrumentation and Methods for Astrophysics, Astrophysics - High Energy Astrophysical Phenomena, 010303 astronomy & astrophysics, Event (particle physics), Instrumentation and Methods for Astrophysics (astro-ph.IM), instrumentation: spectrographs
Abstract: 著者人数: 17名, Accepted: 2018-01-05, 資料番号: SA1170317000
Published: 2018
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18. Search for thermal X-ray features from the Crab nebula with Hitomi Soft X-ray Spectrometer

Author: Aharonian, Felix, Akamatsu, Hiroki, Akimoto, Fumie, Allen, Steven W., Angelini, Lorella, Audard, Marc, Awaki, Hisamitsu, Axelsson, Magnus, Bamba, Aya, Bautz, Marshall W., Blandford, Roger, Brenneman, Laura W., Brown, Greg V., Bulbul, Esra, Cackett, Edward M., Chernyakova, Maria, Chiao, Meng P., Coppi, Paolo S., Costantini, Elisa, de Plaa, Jelle, de Vries, Cor P., den Herder, Jan-Willem, Done, Chris, Dotani, Tadayasu, Ebisawa, Ken, Eckart, Megan E., Enoto, Teruaki, Ezoe, Yuichiro, Fabian, Andrew C., Ferrigno, Carlo, Foster, Adam R., Fujimoto, Ryuichi, Fukazawa, Yasushi, Furuzawa, Akihiro, Galeazzi, Massimiliano, Gallo, Luigi C., Gandhi, Poshak, Giustini, Margherita, Goldwurm, Andrea, Gu, Liyi, Guainazzi, Matteo, Haba, Yoshito, Hagino, Kouichi, Hamaguchi, Kenji, Harrus, Ilana M., Hatsukade, Isamu, Hayashi, Katsuhiro, Hayashi, Takayuki, Hayashida, Kiyoshi, Hiraga, Junko S., Hornschemeier, Ann, Hoshino, Akio, Hughes, John P., Ichinohe, Yuto, Iizuka, Ryo, Inoue, Hajime, Inoue, Yoshiyuki, Ishida, Manabu, Ishikawa, Kumi, Ishisaki, Yoshitaka, Kaastra, Jelle, Kallman, Tim, Kamae, Tsuneyoshi, Kataoka, Jun, Katsuda, Satoru, Kawai, Nobuyuki, Kelley, Richard L., Kilbourne, Caroline A., Kitaguchi, Takao, Kitamoto, Shunji, Kitayama, Tetsu, Kohmura, Takayoshi, Kokubun, Motohide, Koyama, Katsuji, Koyama, Shu, Kretschmar, Peter, Krimm, Hans A., Kubota, Aya, Kunieda, Hideyo, Laurent, Philippe, Lee, Shiu-Hang, Leutenegger, Maurice A., Limousin, Olivier O., Loewenstein, Michael, Long, Knox S., Lumb, David, Madejski, Greg, Maeda, Yoshitomo, Maier, Daniel, Makishima, Kazuo, Markevitch, Maxim, Matsumoto, Hironori, Matsushita, Kyoko, McCammon, Dan, McNamara, Brian R., Mehdipour, Missagh, Miller, Eric D., Miller, Jon M., Mineshige, Shin, Mitsuda, Kazuhisa, Mitsuishi, Ikuyuki, Miyazawa, Takuya, Mizuno, Tsunefumi, Mori, Hideyuki, Mori, Koji, Mukai, Koji, Murakami, Hiroshi, Mushotzky, Richard F., Nakagawa, Takao, Nakajima, Hiroshi, Nakamori, Takeshi, Nakashima, Shinya, Nakazawa, Kazuhiro, Nobukawa, Kumiko K., Nobukawa, Masayoshi, Noda, Hirofumi, Odaka, Hirokazu, Ohashi, Takaya, Ohno, Masanori, Okajima, Takashi, Ota, Naomi, Ozaki, Masanobu, Paerels, Frits, Paltani, Stephane, Petre, Robert, Pinto, Ciro, Porter, Frederick S., Pottschmidt, Katja, Reynolds, Christopher S., Safi-Harb, Samar, Saito, Shinya, Sakai, Kazuhiro, Sasaki, Toru, Sato, Goro, Sato, Kosuke, Sato, Rie, Sato, Toshiki, Sawada, Makoto, Schartel, Norbert, Serlemtsos, Peter J., Seta, Hiromi, Shidatsu, Megumi, Simionescu, Aurora, Smith, Randall K., Soong, Yang, Stawarz, Lukasz, Sugawara, Yasuharu, Sugita, Satoshi, Szymkowiak, Andrew, Tajima, Hiroyasu, Takahashi, Hiromitsu, Takahashi, Tadayuki, Takeda, Shinichiro, Takei, Yoh, Tamagawa, Toru, Tamura, Takayuki, Tanaka, Takaaki, Tanaka, Yasuo, Tanaka, Yasuyuki T., Tashiro, Makoto S., Tawara, Yuzuru, Terada, Yukikatsu, Terashima, Yuichi, Tombesi, Francesco, Tomida, Hiroshi, Tsuboi, Yohko, Tsujimoto, Masahiro, Tsunemi, Hiroshi, Tsuru, Takeshi Go, Uchida, Hiroyuki, Uchiyama, Hideki, Uchiyama, Yasunobu, Ueda, Shutaro, Ueda, Yoshihiro, Uno, Shinichiro, Urry, C. Megan, Ursino, Eugenio, Watanabe, Shin, Werner, Norbert, Wilkins, Dan R., Williams, Brian J., Yamada, Shinya, Yamaguchi, Hiroya, Yamaoka, Kazutaka, Yamasaki, Noriko Y., Yamauchi, Makoto, Yamauchi, Shigeo, Yaqoob, Tahir, Yatsu, Yoichi, Yonetoku, Daisuke, Zhuravleva, Irina, Zoghbi, Abderahmen, Tominaga, Nozomu, and Moriya, Takashi J.
Subjects: Astrophysics::High Energy Astrophysical Phenomena, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics::Galaxy Astrophysics
Abstract: The Crab nebula originated from a core-collapse supernova (SN) explosion observed in 1054 A.D. When viewed as a supernova remnant (SNR), it has an anomalously low observed ejecta mass and kinetic energy for an Fe-core collapse SN. Intensive searches were made for a massive shell that solves this discrepancy, but none has been detected. An alternative idea is that the SN1054 is an electron-capture (EC) explosion with a lower explosion energy by an order of magnitude than Fe-core collapse SNe. In the X-rays, imaging searches were performed for the plasma emission from the shell in the Crab outskirts to set a stringent upper limit to the X-ray emitting mass. However, the extreme brightness of the source hampers access to its vicinity. We thus employed spectroscopic technique using the X-ray micro-calorimeter onboard the Hitomi satellite. By exploiting its superb energy resolution, we set an upper limit for emission or absorption features from yet undetected thermal plasma in the 2-12 keV range. We also re-evaluated the existing Chandra and XMM-Newton data. By assembling these results, a new upper limit was obtained for the X-ray plasma mass of
Published: 2017

19. Hitomi Observation of Radio Galaxy NGC 1275: The First X-ray Microcalorimeter Spectroscopy of Fe-K�� Line Emission from an Active Galactic Nucleus

Author: Hitomi Collaboration, Aharonian, Felix, Akamatsu, Hiroki, Akimoto, Fumie, Allen, Steven W., Angelini, Lorella, Audard, Marc, Awaki, Hisamitsu, Axelsson, Magnus, Bamba, Aya, Bautz, Marshall W., Blandford, Roger, Brenneman, Laura W., Brown, Gregory V., Bulbul, Esra, Cackett, Edward M., Chernyakova, Maria, Chiao, Meng P., Coppi, Paolo S., Costantini, Elisa, de Plaa, Jelle, de Vries, Cor P., Herder, Jan-Willem den, Done, Chris, Dotani, Tadayasu, Ebisawa, Ken, Eckart, Megan E., Enoto, Teruaki, Ezoe, Yuichiro, Fabian, Andrew C., Ferrigno, Carlo, Foster, Adam R., Fujimoto, Ryuichi, Fukazawa, Yasushi, Furuzawa, Akihiro, Galeazzi, Massimiliano, Gallo, Luigi C., Gandhi, Poshak, Giustini, Margherita, Goldwurm, Andrea, Gu, Liyi, Guainazzi, Matteo, Haba, Yoshito, Hagino, Kouichi, Hamaguchi, Kenji, Harrus, Ilana M., Hatsukade, Isamu, Hayashi, Katsuhiro, Hayashi, Takayuki, Hayashida, Kiyoshi, Hiraga, Junko S., Hornschemeier, Ann, Hoshino, Akio, Hughes, John P., Ichinohe, Yuto, Iizuka, Ryo, Inoue, Hajime, Inoue, Yoshiyuki, Ishida, Manabu, Ishikawa, Kumi, Ishisaki, Yoshitaka, Iwai, Masachika, Kaastra, Jelle, Kallman, Tim, Kamae, Tsuneyoshi, Kataoka, Jun, Katsuda, Satoru, Kawai, Nobuyuki, Kelley, Richard L., Kilbourne, Caroline A., Kitaguchi, Takao, Kitamoto, Shunji, Kitayama, Tetsu, Kohmura, Takayoshi, Kokubun, Motohide, Koyama, Katsuji, Koyama, Shu, Kretschmar, Peter, Krimm, Hans A., Kubota, Aya, Kunieda, Hideyo, Laurent, Philippe, Lee, Shiu-Hang, Leutenegger, Maurice A., Limousin, Olivier O., Loewenstein, Michael, Long, Knox S., Lumb, David, Madejski, Greg, Maeda, Yoshitomo, Maier, Daniel, Makishima, Kazuo, Markevitch, Maxim, Matsumoto, Hironori, Matsushita, Kyoko, McCammon, Dan, McNamara, Brian R., Mehdipour, Missagh, Miller, Eric D., Miller, Jon M., Mineshige, Shin, Mitsuda, Kazuhisa, Mitsuishi, Ikuyuki, Miyazawa, Takuya, Mizuno, Tsunefumi, Mori, Hideyuki, Mori, Koji, Mukai, Koji, Murakami, Hiroshi, Mushotzky, Richard F., Nakagawa, Takao, Nakajima, Hiroshi, Nakamori, Takeshi, Nakashima, Shinya, Nakazawa, Kazuhiro, Nobukawa, Kumiko K., Nobukawa, Masayoshi, Noda, Hirofumi, Odaka, Hirokazu, Ohashi, Takaya, Ohno, Masanori, Okajima, Takashi, Ota, Naomi, Ozaki, Masanobu, Paerels, Frits, Paltani, St��phane, Petre, Robert, Pinto, Ciro, Porter, Frederick S., Pottschmidt, Katja, Reynolds, Christopher S., Safi-Harb, Samar, Saito, Shinya, Sakai, Kazuhiro, Sasaki, Toru, Sato, Goro, Sato, Kosuke, Sato, Rie, Sawada, Makoto, Schartel, Norbert, Serlemitsos, Peter J., Seta, Hiromi, Shidatsu, Megumi, Simionescu, Aurora, Smith, Randall K., Soong, Yang, Stawarz, ��ukasz, Sugawara, Yasuharu, Sugita, Satoshi, Szymkowiak, Andrew, Tajima, Hiroyasu, Takahashi, Hiromitsu, Takahashi, Tadayuki, Takeda, Shin'ichiro, Takei, Yoh, Tamagawa, Toru, Tamura, Takayuki, Tanaka, Takaaki, Tanaka, Yasuo, Tanaka, Yasuyuki T., Tashiro, Makoto S., Tawara, Yuzuru, Terada, Yukikatsu, Terashima, Yuichi, Tombesi, Francesco, Tomida, Hiroshi, Tsuboi, Yohko, Tsujimoto, Masahiro, Tsunemi, Hiroshi, Tsuru, Takeshi Go, Uchida, Hiroyuki, Uchiyama, Hideki, Uchiyama, Yasunobu, Ueda, Shutaro, Ueda, Yoshihiro, Uno, Shin'ichiro, Urry, C. Megan, Ursino, Eugenio, Watanabe, Shin, Werner, Norbert, Wilkins, Dan R., Williams, Brian J., Yamada, Shinya, Yamaguchi, Hiroya, Yamaoka, Kazutaka, Yamasaki, Noriko Y., Yamauchi, Makoto, Yamauchi, Shigeo, Yaqoob, Tahir, Yatsu, Yoichi, Yonetoku, Daisuke, Zhuravleva, Irina, Zoghbi, Abderahmen, and Kawamuro, Taiki
Subjects: High Energy Astrophysical Phenomena (astro-ph.HE), Astrophysics::High Energy Astrophysical Phenomena, FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics::Galaxy Astrophysics
Abstract: The origin of the narrow Fe-K�� fluorescence line at 6.4 keV from active galactic nuclei has long been under debate; some of the possible sites are the outer accretion disk, the broad line region, a molecular torus, or interstellar/intracluster media. In February-March 2016, we performed the first X-ray microcalorimeter spectroscopy with the Soft X-ray Spectrometer (SXS) onboard the Hitomi satellite of the Fanaroff-Riley type I radio galaxy NGC 1275 at the center of the Perseus cluster of galaxies. With the high energy resolution of ~5 eV at 6 keV achieved by Hitomi/SXS, we detected the Fe-K�� line with ~5.4 �� significance. The velocity width is constrained to be 500-1600 km s$^{-1}$ (FWHM for Gaussian models) at 90% confidence. The SXS also constrains the continuum level from the NGC 1275 nucleus up to ~20 keV, giving an equivalent width ~20 eV of the 6.4 keV line. Because the velocity width is narrower than that of broad H�� line of ~2750 km s$^{-1}$, we can exclude a large contribution to the line flux from the accretion disk and the broad line region. Furthermore, we performed pixel map analyses on the Hitomi/SXS data and image analyses on the Chandra archival data, and revealed that the Fe-K�� line comes from a region within ~1.6 kpc from the NGC 1275 core, where an active galactic nucleus emission dominates, rather than that from intracluster media. Therefore, we suggest that the source of the Fe-K�� line from NGC 1275 is likely a low-covering fraction molecular torus or a rotating molecular disk which probably extends from a pc to hundreds pc scale in the active galactic nucleus system., 20 pages, 8 figures, 6 tables, accepted for publication in PASJ
Published: 2017
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20. $Hitomi$ constraints on the 3.5 keV line in the Perseus galaxy cluster

Author: Hitomi Collaboration, Aharonian, Felix A., Akamatsu, Hiroki, Akimoto, Fumie, Allen, Steven W., Angelini, Lorella, Arnaud, Keith A., Audard, Marc, Awaki, Hisamitsu, Axelsson, Magnus, Bamba, Aya, Bautz, Marshall W., Blandford, Roger D., Brenneman, Laura W., Brown, Gregory V., Bulbul, Esra, Cackett, Edward M., Chernyakova, Maria, Chiao, Meng P., Coppi, Paolo, Costantini, Elisa, de Plaa, Jelle, Herder, Jan-Willem den, Done, Chris, Dotani, Tadayasu, Ebisawa, Ken, Eckart, Megan E., Enoto, Teruaki, Ezoe, Yuichiro, Fabian, Andrew C., Ferrigno, Carlo, Foster, Adam R., Fujimoto, Ryuichi, Fukazawa, Yasushi, Furuzawa, Akihiro, Galeazzi, Massimiliano, Gallo, Luigi C., Gandhi, Poshak, Giustini, Margherita, Goldwurm, Andrea, Gu, Liyi, Guainazzi, Matteo, Haba, Yoshito, Hagino, Kouichi, Hamaguchi, Kenji, Harrus, Ilana, Hatsukade, Isamu, Hayashi, Katsuhiro, Hayashi, Takayuki, Hayashida, Kiyoshi, Hiraga, Junko, Hornschemeier, Ann E., Hoshino, Akio, Hughes, John P., Ichinohe, Yuto, Iizuka, Ryo, Inoue, Hajime, Inoue, Shota, Inoue, Yoshiyuki, Ishibashi, Kazunori, Ishida, Manabu, Ishikawa, Kumi, Ishisaki, Yoshitaka, Itoh, Masayuki, Iwai, Masachika, Iyomoto, Naoko, Kaastra, Jelle S., Kallman, Timothy, Kamae, Tuneyoshi, Kara, Erin, Kataoka, Jun, Katsuda, Satoru, Katsuta, Junichiro, Kawaharada, Madoka, Kawai, Nobuyuki, Kelley, Richard L., Khangulyan, Dmitry, Kilbourne, Caroline A., King, Ashley L., Kitaguchi, Takao, Kitamoto, Shunji, Kitayama, Tetsu, Kohmura, Takayoshi, Kokubun, Motohide, Koyama, Shu, Koyama, Katsuji, Kretschmar, Peter, Krimm, Hans A., Kubota, Aya, Kunieda, Hideyo, Laurent, Philippe, Lebrun, Francois, Lee, Shiu-Hang, Leutenegger, Maurice, Limousin, Olivier, Loewenstein, Michael, Long, Knox S., Lumb, David, Madejski, Grzegorz M., Maeda, Yoshitomo, Maier, Daniel, Makishima, Kazuo, Markevitch, Maxim, Matsumoto, Hironori, Matsushita, Kyoko, McCammon, Dan, McNamara, Brian R., Mehdipour, Missagh, Miller, Eric D., Miller, Jon M., Mineshige, Shin, Mitsuda, Kazuhisa, Mitsuishi, Ikuyuki, Miyazawa, Takuya, Mizuno, Tsunefumi, Mori, Hideyuki, Mori, Koji, Moseley, Harvey, Mukai, Koji, Murakami, Hiroshi, Murakami, Toshio, Mushotzky, Richard F., Nakagawa, Takao, Nakajima, Hiroshi, Nakamori, Takeshi, Nakano, Toshio, Nakashima, Shinya, Nakazawa, Kazuhiro, Nobukawa, Kumiko, Nobukawa, Masayoshi, Noda, Hirofumi, Nomachi, Masaharu, O'Dell, Steve L., Odaka, Hirokazu, Ohashi, Takaya, Ohno, Masanori, Okajima, Takashi, Ota, Naomi, Ozaki, Masanobu, Paerels, Frits, Paltani, Stephane, Parmar, Arvind, Petre, Robert, Pinto, Ciro, Pohl, Martin, Porter, F. Scott, Pottschmidt, Katja, Ramsey, Brian D., Reynolds, Christopher S., Russell, Helen R., Safi-Harb, Samar, Saito, Shinya, Sakai, Kazuhiro, Sameshima, Hiroaki, Sasaki, Toru, Sato, Goro, Sato, Kosuke, Sato, Rie, Sawada, Makoto, Schartel, Norbert, Serlemitsos, Peter J., Seta, Hiromi, Shidatsu, Megumi, Simionescu, Aurora, Smith, Randall K., Soong, Yang, Stawarz, Lukasz, Sugawara, Yasuharu, Sugita, Satoshi, Szymkowiak, Andrew E., Tajima, Hiroyasu, Takahashi, Hiromitsu, Takahashi, Tadayuki, Takeda, Shin'ichiro, Takei, Yoh, Tamagawa, Toru, Tamura, Keisuke, Tamura, Takayuki, Tanaka, Takaaki, Tanaka, Yasuo, Tanaka, Yasuyuki, Tashiro, Makoto, Tawara, Yuzuru, Terada, Yukikatsu, Terashima, Yuichi, Tombesi, Francesco, Tomida, Hiroshi, Tsuboi, Yohko, Tsujimoto, Masahiro, Tsunemi, Hiroshi, Tsuru, Takeshi, Uchida, Hiroyuki, Uchiyama, Hideki, Uchiyama, Yasunobu, Ueda, Shutaro, Ueda, Yoshihiro, Ueno, Shiro, Uno, Shin'ichiro, Urry, C. Meg, Ursino, Eugenio, de Vries, Cor P., Watanabe, Shin, Werner, Norbert, Wik, Daniel R., Wilkins, Dan R., Williams, Brian J., Yamada, Shinya, Yamaguchi, Hiroya, Yamaoka, Kazutaka, Yamasaki, Noriko Y., Yamauchi, Makoto, Yamauchi, Shigeo, Yaqoob, Tahir, Yatsu, Yoichi, Yonetoku, Daisuke, Yoshida, Atsumasa, Zhuravleva, Irina, Zoghbi, Abderahmen, Laboratoire AIM, Université Paris Diderot - Paris 7 ( UPD7 ) -Centre d'Etudes de Saclay, Hitomi, Astrophysique Interprétation Modélisation (AIM (UMR_7158 / UMR_E_9005 / UM_112)), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris Diderot - Paris 7 (UPD7), Astrophysique Interprétation Modélisation (AIM (UMR7158 / UMR_E_9005 / UM_112)), and Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS)
Subjects: galaxies: clusters: individual, Cosmology and Nongalactic Astrophysics (astro-ph.CO), galaxies: clusters: intracluster medium, clusters: individual: A426 [galaxies], Astrophysics::High Energy Astrophysical Phenomena, [ PHYS.ASTR ] Physics [physics]/Astrophysics [astro-ph], Dark matter, FOS: Physical sciences, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, galaxies: clusters: individual (A426), 01 natural sciences, dark matter, X-ray, Settore FIS/05 - Astronomia e Astrofisica, gas, 0103 physical sciences, calorimeter, Emission spectrum, Spectroscopy, 010303 astronomy & astrophysics, Galaxy cluster, Astrophysics::Galaxy Astrophysics, Line (formation), High Energy Astrophysical Phenomena (astro-ph.HE), Physics, Nebula, 010308 nuclear & particles physics, dark matter: decay, Astronomy and Astrophysics, charge exchange, Astrophysics - Astrophysics of Galaxies, K-line, Galaxy, flux, Space and Planetary Science, clusters: intracluster medium [galaxies], Astrophysics of Galaxies (astro-ph.GA), X-rays: galaxies: clusters, galaxy: cluster, galaxies: clusters [X-rays], Astrophysics - High Energy Astrophysical Phenomena, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], signature, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: High-resolution X-ray spectroscopy with Hitomi was expected to resolve the origin of the faint unidentified E=3.5 keV emission line reported in several low-resolution studies of various massive systems, such as galaxies and clusters, including the Perseus cluster. We have analyzed the Hitomi first-light observation of the Perseus cluster. The emission line expected for Perseus based on the XMM-Newton signal from the large cluster sample under the dark matter decay scenario is too faint to be detectable in the Hitomi data. However, the previously reported 3.5 keV flux from Perseus was anomalously high compared to the sample-based prediction. We find no unidentified line at the reported high flux level. Taking into account the XMM measurement uncertainties for this region, the inconsistency with Hitomi is at a 99% significance for a broad dark-matter line and at 99.7% for a narrow line from the gas. We do not find anomalously high fluxes of the nearby faint K line or the Ar satellite line that were proposed as explanations for the earlier 3.5 keV detections. We do find a hint of a broad excess near the energies of high-n transitions of Sxvi (E=3.44 keV rest-frame) -- a possible signature of charge exchange in the molecular nebula and another proposed explanation for the unidentified line. While its energy is consistent with XMM pn detections, it is unlikely to explain the MOS signal. A confirmation of this interesting feature has to wait for a more sensitive observation with a future calorimeter experiment., Discussion of systematics significantly expanded. 9 pages, 5 figures; ApJ Lett. in press
Published: 2017
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21. Design, implementation, and performance of the Astro-H soft x-ray spectrometer aperture assembly and blocking filters

Author: Kilbourne, Caroline A., Adams, Joseph S., Arsenovic, Petar, Ayers, Travis, Chiao, Meng P., DiPirro, Michael J., Eckart, Megan E., Kazeva, John D., Kripps, Kari L., Lairson, Bruce M., Leutenegger, Maurice A., Lopez, Heidi C., McCammon, Dan, McGuinness, Daniel S., Moseley, Samuel J., Porter, F. Scott, Schweiss, Andrea N., Thorpe, Rosemary Schmidt, Watanabe, Tomomi, Fujimoto, Ryuichi, Mitsuda, Kazuhisa, Takei, Yoh, Yamasaki, Noriko Y., and Yoshida, Seiji
Subjects: x-ray calorimeter, Aperture, 02 engineering and technology, microcalorimeter, Radiation, 01 natural sciences, radiation-blocking filters, law.invention, 010309 optics, Optics, law, 0103 physical sciences, Instrumentation, Noise-equivalent power, Physics, Spectrometer, Calorimeter (particle physics), business.industry, Mechanical Engineering, Bolometer, Detector, Astrophysics::Instrumentation and Methods for Astrophysics, Astronomy and Astrophysics, 021001 nanoscience & nanotechnology, Astro-H, Electronic, Optical and Magnetic Materials, aperture cylinder, Hitomi, Space and Planetary Science, Control and Systems Engineering, Thermal radiation, 0210 nano-technology, business
Abstract: 著者人数: 24名, Accepted: 2018-01-22, 資料番号: SA1170313000
Published: 2018
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22. Cooling system for the soft X-ray spectrometer onboard Astro-H

Author: DiPirro, Mike, Shirron, Peter, Sneiderman, Gary, Kelley, Richard L., Porter, F. Scott, Kilbourne, Caroline A., Crow, John, Mattern, Andrea, Kashani, Ali, McCammon, Dan, Fujimoto, Ryuichi, Mitsuda, Kazuhisa, Yamasaki, Noriko, Takei, Yoh, Tsujimoto, Masahiro, Sugita, Hiroyuki, Sato, Yoichi, Shinozaki, Keisuke, Ohashi, Takaya, Ishisaki, Yoshitaka, Ezoe, Yuichiro, Murakami, Masahide, Kitamoto, Shunji, Murakami, Hiroshi, Tamagawa, Toru, Kawaharada, Madoka, Yamaguchi, Hiroya, Sato, Kosuke, Kanao, Kenichi, and Yoshida, Seiji
Subjects: Stirling engine, Physics::Instrumentation and Detectors, Astrophysics::High Energy Astrophysical Phenomena, Refrigerator car, General Physics and Astronomy, Thermodynamics, Cryogenics, law.invention, E. Adiabatic demagnetization, symbols.namesake, Optics, law, Water cooling, General Materials Science, E. He II systems, Physics, Spectrometer, Liquid helium, business.industry, Joule–Thomson effect, Astrophysics::Instrumentation and Methods for Astrophysics, Cryocooler, F. Space cryogenics, symbols, E. Stirling, business, E. Joule-Thomson coolers
Abstract: 著者人数：31名, Accepted: 2010-02-22, 資料番号: SA1002674000
Published: 2010

23. Searching for keV Sterile Neutrino Dark Matter with X-ray Microcalorimeter Sounding Rockets

Author: Figueroa-Feliciano, Enectali, Anderson, Adam J., Castro, Daniel, Goldfinger, David C., Rutherford, John, Eckart, Megan E., Kelley, Richard L., Kilbourne, Caroline A., McCammon, Dan, Morgan, Kelsey, Porter, Frederick Scott, and Szymkowiak, Andrew E.
Subjects: High Energy Astrophysical Phenomena (astro-ph.HE), Cosmology and Nongalactic Astrophysics (astro-ph.CO), Physics::Instrumentation and Detectors, Astrophysics::High Energy Astrophysical Phenomena, High Energy Physics::Phenomenology, FOS: Physical sciences, High Energy Physics::Experiment, Astrophysics - High Energy Astrophysical Phenomena, Astrophysics - Instrumentation and Methods for Astrophysics, Instrumentation and Methods for Astrophysics (astro-ph.IM), Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: High-resolution X-ray spectrometers onboard suborbital sounding rockets can search for dark matter candidates that produce X-ray lines, such as decaying keV-scale sterile neutrinos. Even with exposure times and effective areas far smaller than XMM-Newton and Chandra observations, high-resolution, wide field-of-view observations with sounding rockets have competitive sensitivity to decaying sterile neutrinos. We analyze a subset of the 2011 observation by the X-ray Quantum Calorimeter instrument centered on Galactic coordinates l = 165, b = -5 with an effective exposure of 106 seconds, obtaining a limit on the sterile neutrino mixing angle of sin^2(2 theta) < 7.2e-10 at 95% CL for a 7 keV neutrino. Better sensitivity at the level of sin^2(2 theta) ~ 2.1e-11 at 95\% CL for a 7 keV neutrino is achievable with future 300-second observations of the galactic center by the Micro-X instrument, providing a definitive test of the sterile neutrino interpretation of the reported 3.56 keV excess from galaxy clusters., 13 pages, 13 figures, submitted to ApJ
Published: 2015

24. Performance of the helium dewar and the cryocoolers of the Hitomi soft x-ray spectrometer

Author: DiPirro, Michael J., Shirron, Peter J., Sneiderman, Gary A., Kilbourne, Caroline A., Porter, Frederick Scott, Chiao, Meng P., Eckart, Megan E., Fujimoto, Ryuichi, Takei, Yoh, Mitsuda, Kazuhisa, Yamasaki, Noriko Y., Tsujimoto, Masahiro, Koyama, Shu, Ishikawa, Kumi, Sugita, Hiroyuki, Sato, Yoichi, Shinozaki, Keisuke, Okamoto, Atsushi, Kitamoto, Shunji, Hoshino, Akio, Sato, Kosuke, Ezoe, Yuichiro, Ishisaki, Yoshitaka, Yamada, Shinya, Seta, Hiromi, Ohashi, Takaya, Tamagawa, Toru, Noda, Hirofumi, Sawada, Makoto, Tashiro, Makoto, Yatsu, Yoichi, Mitsuishi, Ikuyuki, Kanao, Kenichi, Yoshida, Seiji, Miyaoka, Mikio, Tsunematsu, Shoji, Otsuka, Kiyomi, and Narasaki, Katsuhiro
Subjects: x-ray microcalorimeter, Materials science, Stirling engine, Physics::Instrumentation and Detectors, Nuclear engineering, Refrigerator car, chemistry.chemical_element, Heat sink, 01 natural sciences, law.invention, 010309 optics, law, space cryogenics, 0103 physical sciences, 010306 general physics, Instrumentation, Joule-Thomson cryocooler, Helium, superfluid liquid helium, Spectrometer, Liquid helium, Mechanical Engineering, Astrophysics::Instrumentation and Methods for Astrophysics, Astronomy and Astrophysics, Cryocooler, Electronic, Optical and Magnetic Materials, Stirling cryocooler, Hitomi, chemistry, Space and Planetary Science, Control and Systems Engineering, Satellite
Abstract: 著者人数: 38名, Accepted: 2017-11-27, 資料番号: SA1170327000
Published: 2017
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25. Laboratory X-ray Spectra From L-shell Sulfur Ions Following Charge-exchange Collisions With Two Different Neutral Targets: SF6 And He

Author: Koutroumpa, Dimitra, Beiersdorfer, P., Brown, G. V., Kelley, R. L., Kilbourne, Caroline A., Leutenegger, M. A., Porter, F. S., HELIOS - LATMOS, Laboratoire Atmosphères, Milieux, Observations Spatiales (LATMOS), Université de Versailles Saint-Quentin-en-Yvelines (UVSQ)-Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université de Versailles Saint-Quentin-en-Yvelines (UVSQ)-Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), NASA Goddard Space Flight Center (GSFC), Lawrence Livermore National Laboratory (LLNL), and Koutroumpa, Dimitra
Subjects: [SDU] Sciences of the Universe [physics], [SDU.ASTR.IM] Sciences of the Universe [physics]/Astrophysics [astro-ph]/Instrumentation and Methods for Astrophysic [astro-ph.IM], [SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph], [SDU]Sciences of the Universe [physics], [SDU.ASTR] Sciences of the Universe [physics]/Astrophysics [astro-ph], [SDU.ASTR.IM]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Instrumentation and Methods for Astrophysic [astro-ph.IM]
Abstract: International audience; We present new high resolution X-ray spectra in the 0.1 - 0.7 keV energy range from L-shell sulfur ions produced by charge exchange (CX) with He atoms at the Lawrence Livermore National Laboratory's Electron beam ion trap (EBIT-I) and measured with the NASA/GSFC EBIT Calorimeter Spectrometer (ECS). We discuss the results and focus mainly on the differences between the new spectra and spectra from sulfur ions following CX with SF6 molecules previously obtained with the EBIT and ECS. Part of this work was prepared by Lawrence Livermore National Laboratory under Contract DE-AC52-07NA27344. We also gratefully acknowledge funding through NASA's laboratory astrophysics program.
Published: 2010

26. Spectral Signatures Of Charge Exchange In K-shell X-ray Spectra Of Ar, P, And S Measured With The LLNL Electron Beam Ion Trap

Author: Leutenegger, Maurice A., Beiersdorfer, Peter, Brown, Gregory V., Kelley, Richard L., Kilbourne, Caroline A., Koutroumpa, Dimitra, Porter, Frederick S., NASA Goddard Space Flight Center (GSFC), Lawrence Livermore National Laboratory (LLNL), HELIOS - LATMOS, Laboratoire Atmosphères, Milieux, Observations Spatiales (LATMOS), Université de Versailles Saint-Quentin-en-Yvelines (UVSQ)-Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université de Versailles Saint-Quentin-en-Yvelines (UVSQ)-Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), and Koutroumpa, Dimitra
Subjects: [SDU] Sciences of the Universe [physics], [SDU.ASTR.IM] Sciences of the Universe [physics]/Astrophysics [astro-ph]/Instrumentation and Methods for Astrophysic [astro-ph.IM], [SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph], [SDU]Sciences of the Universe [physics], Astrophysics::High Energy Astrophysical Phenomena, [SDU.ASTR] Sciences of the Universe [physics]/Astrophysics [astro-ph], [SDU.ASTR.IM]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Instrumentation and Methods for Astrophysic [astro-ph.IM]
Abstract: International audience; Charge exchange is an important process in numerous astrophysical contexts, including the interaction of the solar wind with neutral material throughout the solar system, which is hypothesized to contribute a large fraction of the soft X-ray background, and is thus highly relevant to studies of diffuse X-ray emission from the warm-hot phase of the intergalactic medium. It may also be important in supernova remnants, as hot, shocked gas interacts with the surrounding neutral ISM. It will be increasingly important to understand charge exchange in the near future, when the Micro-X rocket mission and the Astro-H SXS become the first imaging high-resolution X-ray spectrometers, allowing observations of highly extended sources with sufficient spectral resolution to easily detect spectral signatures of charge exchange. Charge exchange in the limit of low collision energy is still poorly understood, and measurements benchmarking theoretical predictions of cross-sections and spectra are desirable. We present high resolution K-shell X-ray spectra of highly ionized Ar, P, and S produced by low collision energy charge exchange in the LLNL electron beam ion trap and measured by the NASA/GSFC EBIT calorimeter spectrometer (ECS) and XRS/EBIT instruments. We investigate the scaling of the hardness ratios of the hydrogenic spectra with atomic number, as well as their dependence on the neutral electron donor species. We also find that the He-like triplet line ratios are strongly diagnostic of the neutral electron donor species. Part of this work was prepared by Lawrence Livermore National Laboratory under Contract DE-AC52-07NA27344.
Published: 2010

27. Spectroscopic Laboratory Astrophysics Experiments Conducted at the LLNL EBIT Facility in Support of NASA's X-ray Astronomy Flight Program

Author: Brown, Gregory V., Adams, Joseph S., Beiersdorfer, Peter, Chen, Hui, Clementson, Joel, Frankel, Miriam, Graf, A., Gu, M. F., Kahn, Steven M., Kelley, Richard, Kilbourne, Caroline A., Koutroumpa, Dimitra, Leutenegger, M., Porter, Frederick, Wargelin, B., Lawrence Livermore National Laboratory (LLNL), NASA Goddard Space Flight Center (GSFC), Space Sciences Laboratory [Berkeley] (SSL), University of California [Berkeley] (UC Berkeley), University of California (UC)-University of California (UC), HELIOS - LATMOS, Laboratoire Atmosphères, Milieux, Observations Spatiales (LATMOS), Université de Versailles Saint-Quentin-en-Yvelines (UVSQ)-Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université de Versailles Saint-Quentin-en-Yvelines (UVSQ)-Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Université libre de Bruxelles (ULB), Smithsonian Astrophysical Observatory, Smithsonian Institution, University of California [Berkeley], and University of California-University of California
Subjects: [SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph], [SDU]Sciences of the Universe [physics], [SDU.ASTR.IM]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Instrumentation and Methods for Astrophysic [astro-ph.IM]
Abstract: International audience; The electron beam ion trap (EBIT) facility located at the Lawrence Livermore National Laboratory has been used for laboratory astrophysics experiments for over 15 years. During this time, several unique spectrometers and operating modes have been developed and implemented, including high resolution grating and crystal spectrometers, a high-resolution, high-efficiency NASA/GSFC microcalorimeter array, and the ability to operate and record datawith the electron beam turned off, i.e., in the so-called magnetic trapping mode. Targeted experiments conducted at this facility have addressed specific problems faced by the X-ray astrophysics community and have provided accurate, complete sets of atomic data such as relative and absolute excitation cross sections, transition wavelengths, line polarization, and X-ray signatures of charge exchange recombination. Here we will present a brief overview of our facility and some of the more recent results including 1/4 keV band X- ray emission produced by charge exchange between L-shell sulfur ions and neutral gas, wavelengths and relative intensities of satellite X- ray lines from Na-like Fe XVI and their contribution to the Fe XVII line emission, and the relative intensities of the 3s-2p/3d-2p lines in F-like Fe XVIII and Ni XX. Part of this work was performed under the auspices of the U. S. Department of Energy by Lawrence Livermore National Laboratory under Contract DE-AC52-07NA27344 and is also supported by NASA grants to LLNL, GSFC, and Stanford University.
Published: 2009

28. The X-ray observatory Suzaku

Author: Bautz, Mark, Kelley, Richard L., Petre, Robert, Figueroa, Enectali, Soong, Yang, Gendreau, Keith, Griffiths, Richard E., Harrus, Ilana, White, Nicholas E., Hasinger, Gunther, Henry, Patrick J., Holt, Stephen S., Hornschemeier, Ann, Hughes, John P., Hwang, Una, Smith, Randall, Kahn, Steven M., Kilbourne, Caroline, Kissel, Steve, Szymkowiak, Andrew E., Madejski, Greg M., Markowitz, Alex, Matsumoto, Chiho, Matsumoto, Hironori, Mccammon, Dan, Moseley, Harvey, Mushotzky, Richard, Nousek, John A., Chan, Kai-Wing, Ozawa, Hideki, Parmer, Arvind N., Pence, William D., Turner, Martin J. L., Angelini, Lorella, Arnaud, Keith, Boyce, Kevin, Brown, Gregory V., Porter, F. Scott, Cottam, Jean, Reeves, James N., Ricker, George R., Doty, John, Sanders, Wilton T., Fabian, Andrew C., Serlemitsos, Peter, Tashiro, Makoto, Tawara, Yuzuru, Terada, Yukikatsu, Terashima, Yuichi, Tomida, Hiroshi, Torii, Ken'ichi, Tsuboi, Yohko, Tsujimoto, Masahiro, Tsuru, Takeshi Go, Ueda, Yoshihiro, Ueno, Shiro, Ueno, Masaru, Uno, Shin'ichiro, Urata, Yuji, Watanabe, Shin, Yamamoto, Norimasa, Ishida, Manabu, Yamaoka, Kazutaka, Yamasaki, Noriko Y., Ishisaki, Yoshitaka, Isobe, Naoki, Itoh, Masayuki, Iyomoto, Naoko, Kamae, Tuneyoshi, Katagiri, Hideaki, Kataoka, Jun, Mitsuda, Kazuhisa, Inoue, Hajime, Katayama, Haruyoshi, Koyama, Katsuji, Kunieda, Hideyo, Makishima, Kazuo, Ogawara, Yoshiaki, Takahashi, Tadayuki, Tsunemi, Hiroshi, Anabuki, Naohisa, Kawai, Nobuyuki, Awaki, Hisamitsu, Bamba, Aya, Dotani, Tadayasu, Ebisawa, Ken, Ezoe, Yuichiro, Fujimoto, Ryuichi, Fukazawa, Yasushi, Furusho, Tae, Furuzawa, Akihiro, Kinugasa, Kenzo, Haba, Yoshito, Hamaguchi, Kenji, Hatsukade, Isamu, Hayashida, Kiyoshi, Hiraga, Junko S., Kitamoto, Shunji, Kohama, Mitsuhiro, Kohmura, Takayoshi, Kokubun, Motohide, Kotani, Taro, Kotoku, Jun'ichi, Kubota, Aya, Maeda, Yoshitomo, Makino, Fumiyoshi, Matsuoka, Masaru, Matsushita, Kyoko, Mihara, Tatehiko, Misaki, Kazutami, Miyata, Emi, Mizuno, Tsunefumi, Mori, Koji, Mori, Hideyuki, Morii, Mikio, Mukai, Koji, Murakami, Hiroshi, Murakami, Toshio, Nagase, Fumiaki, Namiki, Masaaki, Negoro, Hitoshi, Nakazawa, Kazuhiro, Okajima, Takashi, Ogasaka, Yasushi, Ohashi, Takaya, Oshima, Tai, Ota, Naomi, Ozaki, Masanobu, Sakurai, Ikuya, Senda, Atsushi, Shibata, Ryo, Suzuki, Motoko, Takahashi, Hiromitsu, Tamagawa, Toru, Tamura, Keisuke, Tamura, Takayuki, and Tanaka, Yasuo
Subjects: Physics, Scientific instrument, instrumentation, Spacecraft, business.industry, Astrophysics::High Energy Astrophysical Phenomena, Detector, Astrophysics::Instrumentation and Methods for Astrophysics, Astronomy, Astronomy and Astrophysics, Astrophysics, X-rays: general, Space and Planetary Science, Observatory, space vehicles, space vehicles: instruments, business
Abstract: 著者人数: 143名, Accepted: 2006-09-27, 資料番号: SA1000631000

29. Fabrication of a Hybrid Transition Edge Sensor Array for Lynx

Author: Wassell, Edward, Adams, Joseph S., Bandler, Simon R., Chang, Meng-Ping, Chervenak, James A., Datesman, Aaron M., Eckart, Megan E., Ewin, Audrey J., Finkbeiner, Fred M., Yoon Ha, Jong, Kelley, R., Kilbourne, Caroline A., Miniussi, Antoine R., Porter, F., Sadleir, John E., Sakai, Kazuhiro, Smith, Stephen J., and Wakehan, Nicholas
Subjects: hybrid, lynx, transition, fabrication, array, edge sensor
Full Text: View/download PDF

30. X-ray spectral study of the extended emission, 'the Cap', located 11.6 kpc above the disk of M 82

Author: Tsuru, Takeshi Go, Ozawa, Midori, Hyodo, Yoshiaki, Matsumoto, Hironori, Koyama, Katsuji, Awaki, Hisamitsu, Fujimoto, Ryuichi, Griffiths, Richard, Kilbourne, Caroline, Matsushita, Kyoko, Mitsuda, Kazuhisa, Ptak, Andrew, Piero Ranalli, and Yamasaki, Noriko Y.

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

Author: Didier Barret, Vincent Albouys, Jan-Willem den Herder, Luigi Piro, Massimo Cappi, Juhani Huovelin, Richard Kelley, J. Miguel Mas-Hesse, Stéphane Paltani, Gregor Rauw, Agata Rozanska, Jiri Svoboda, Joern Wilms, Noriko Yamasaki, Marc Audard, Simon Bandler, Marco Barbera, Xavier Barcons, Enrico Bozzo, Maria Teresa Ceballos, Ivan Charles, Elisa Costantini, Thomas Dauser, Anne Decourchelle, Lionel Duband, Jean-Marc Duval, Fabrizio Fiore, Flavio Gatti, Andrea Goldwurm, Roland den Hartog, Brian Jackson, Peter Jonker, Caroline Kilbourne, Seppo Korpela, Claudio Macculi, Mariano Mendez, Kazuhisa Mitsuda, Silvano Molendi, François Pajot, Etienne Pointecouteau, Frederick Porter, Gabriel W. Pratt, Damien Prêle, Laurent Ravera, Kosuke Sato, Joop Schaye, Keisuke Shinozaki, Konrad Skup, Jan Soucek, Tanguy Thibert, Jacco Vink, Natalie Webb, Laurence Chaoul, Desi Raulin, Aurora Simionescu, Jose Miguel Torrejon, Fabio Acero, Graziella Branduardi-Raymont, Stefano Ettori, Alexis Finoguenov, Nicolas Grosso, Jelle Kaastra, Pasquale Mazzotta, Jon Miller, Giovanni Miniutti, Fabrizio Nicastro, Salvatore Sciortino, Hiroya Yamaguchi, Sophie Beaumont, Edoardo Cucchetti, Matteo D’Andrea, Megan Eckart, Philippe Ferrando, Elias Kammoun, Simone Lotti, Jean-Michel Mesnager, Lorenzo Natalucci, Philippe Peille, Jelle de Plaa, Florence Ardellier, Andrea Argan, Elise Bellouard, Jérôme Carron, Elisabetta Cavazzuti, Mauro Fiorini, Pourya Khosropanah, Sylvain Martin, James Perry, Frederic Pinsard, Alice Pradines, Manuela Rigano, Peter Roelfsema, Denis Schwander, Guido Torrioli, Joel Ullom, Isabel Vera, Eduardo Medinaceli Villegas, Monika Zuchniak, Frank Brachet, Ugo Lo Cicero, William Doriese, Malcom Durkin, Valentina Fioretti, Hervé Geoffray, Lionel Jacques, Christian Kirsch, Stephen Smith, Joseph Adams, Emilie Gloaguen, Ruud Hoogeveen, Paul van der Hulst, Mikko Kiviranta, Jan van der Kuur, Aurélien Ledot, Bert-Joost van Leeuwen, Dennis van Loon, Bertrand Lyautey, Yann Parot, Kazuhiro Sakai, Henk van Weers, Shariefa Abdoelkariem, Thomas Adam, Christophe Adami, Corinne Aicardi, Hiroki Akamatsu, Pablo Eleazar Merino Alonso, Roberta Amato, Jérôme André, Matteo Angelinelli, Manuel Anon-Cancela, Shebli Anvar, Ricardo Atienza, Anthony Attard, Natalia Auricchio, Ana Balado, Florian Bancel, Lorenzo Ferrari Barusso, Arturo Bascuñan, Vivian Bernard, Alicia Berrocal, Sylvie Blin, Donata Bonino, François Bonnet, Patrick Bonny, Peter Boorman, Charles Boreux, Ayoub Bounab, Martin Boutelier, Kevin Boyce, Daniele Brienza, Marcel Bruijn, Andrea Bulgarelli, Simona Calarco, Paul Callanan, Alberto Prada Campello, Thierry Camus, Florent Canourgues, Vito Capobianco, Nicolas Cardiel, Florent Castellani, Oscar Cheatom, James Chervenak, Fabio Chiarello, Laurent Clerc, Nicolas Clerc, Beatriz Cobo, Odile Coeur-Joly, Alexis Coleiro, Stéphane Colonges, Leonardo Corcione, Mickael Coriat, Alexandre Coynel, Francesco Cuttaia, Antonino D’Ai, Fabio D’anca, Mauro Dadina, Christophe Daniel, Lea Dauner, Natalie DeNigris, Johannes Dercksen, Michael DiPirro, Eric Doumayrou, Luc Dubbeldam, Michel Dupieux, Simon Dupourqué, Jean Louis Durand, Dominique Eckert, Valvanera Eiriz, Eric Ercolani, Christophe Etcheverry, Fred Finkbeiner, Mariateresa Fiocchi, Hervé Fossecave, Philippe Franssen, Martin Frericks, Stefano Gabici, Florent Gant, Jian-Rong Gao, Fabio Gastaldello, Ludovic Genolet, Simona Ghizzardi, Ma Angeles Alcacera Gil, Elisa Giovannini, Olivier Godet, Javier Gomez-Elvira, Raoul Gonzalez, Manuel Gonzalez, Luciano Gottardi, Dolorès Granat, Michel Gros, Nicolas Guignard, Paul Hieltjes, Adolfo Jesús Hurtado, Kent Irwin, Christian Jacquey, Agnieszka Janiuk, Jean Jaubert, Maria Jiménez, Antoine Jolly, Thierry Jourdan, Sabine Julien, Bartosz Kedziora, Andrew Korb, Ingo Kreykenbohm, Ole König, Mathieu Langer, Philippe Laudet, Philippe Laurent, Monica Laurenza, Jean Lesrel, Sebastiano Ligori, Maximilian Lorenz, Alfredo Luminari, Bruno Maffei, Océane Maisonnave, Lorenzo Marelli, Didier Massonet, Irwin Maussang, Alejandro Gonzalo Melchor, Isabelle Le Mer, Francisco Javier San Millan, Jean-Pierre Millerioux, Teresa Mineo, Gabriele Minervini, Alexeï Molin, David Monestes, Nicola Montinaro, Baptiste Mot, David Murat, Kenichiro Nagayoshi, Yaël Nazé, Loïc Noguès, Damien Pailot, Francesca Panessa, Luigi Parodi, Pascal Petit, Enrico Piconcelli, Ciro Pinto, Jose Miguel Encinas Plaza, Borja Plaza, David Poyatos, Thomas Prouvé, Andy Ptak, Simonetta Puccetti, Elena Puccio, Pascale Ramon, Manuel Reina, Guillaume Rioland, Louis Rodriguez, Anton Roig, Bertrand Rollet, Mauro Roncarelli, Gilles Roudil, Tomasz Rudnicki, Julien Sanisidro, Luisa Sciortino, Vitor Silva, Michael Sordet, Javier Soto-Aguilar, Pierre Spizzi, Christian Surace, Miguel Fernández Sánchez, Emanuele Taralli, Guilhem Terrasa, Régis Terrier, Michela Todaro, Pietro Ubertini, Michela Uslenghi, Jan Geralt Bij de Vaate, Davide Vaccaro, Salvatore Varisco, Peggy Varnière, Laurent Vibert, María Vidriales, Fabrizio Villa, Boris Martin Vodopivec, Angela Volpe, Cor de Vries, Nicholas Wakeham, Gavin Walmsley, Michael Wise, Martin de Wit, Grzegorz Woźniak, Barret, Didier, Albouys, Vincent, Herder, Jan-Willem den, Piro, Luigi, Cappi, Massimo, Huovelin, Juhani, Kelley, Richard, Mas-Hesse, J. Miguel, Paltani, Stéphane, Rauw, Gregor, Rozanska, Agata, Svoboda, Jiri, Wilms, Joern, Yamasaki, Noriko, Audard, Marc, Bandler, Simon, Barbera, Marco, Barcons, Xavier, Bozzo, Enrico, Ceballos, Maria Teresa, Charles, Ivan, Costantini, Elisa, Dauser, Thoma, Decourchelle, Anne, Duband, Lionel, Duval, Jean-Marc, Fiore, Fabrizio, Gatti, Flavio, Goldwurm, Andrea, Hartog, Roland den, Jackson, Brian, Jonker, Peter, Kilbourne, Caroline, Korpela, Seppo, Macculi, Claudio, Mendez, Mariano, Mitsuda, Kazuhisa, Molendi, Silvano, Pajot, Françoi, Pointecouteau, Etienne, Porter, Frederick, Pratt, Gabriel W., Prêle, Damien, Ravera, Laurent, Sato, Kosuke, Schaye, Joop, Shinozaki, Keisuke, Skup, Konrad, Soucek, Jan, Thibert, Tanguy, Vink, Jacco, Webb, Natalie, Chaoul, Laurence, Raulin, Desi, Simionescu, Aurora, Torrejon, Jose Miguel, Acero, Fabio, Branduardi-Raymont, Graziella, Ettori, Stefano, Finoguenov, Alexi, Grosso, Nicola, Kaastra, Jelle, Mazzotta, Pasquale, Miller, Jon, Miniutti, Giovanni, Nicastro, Fabrizio, Sciortino, Salvatore, Yamaguchi, Hiroya, Beaumont, Sophie, Cucchetti, Edoardo, D’Andrea, Matteo, Eckart, Megan, Ferrando, Philippe, Kammoun, Elia, Lotti, Simone, Mesnager, Jean-Michel, Natalucci, Lorenzo, Peille, Philippe, de Plaa, Jelle, Ardellier, Florence, Argan, Andrea, Bellouard, Elise, Carron, Jérôme, Cavazzuti, Elisabetta, Fiorini, Mauro, Khosropanah, Pourya, Martin, Sylvain, Perry, Jame, Pinsard, Frederic, Pradines, Alice, Rigano, Manuela, Roelfsema, Peter, Schwander, Deni, Torrioli, Guido, Ullom, Joel, Vera, Isabel, Villegas, Eduardo Medinaceli, Zuchniak, Monika, Brachet, Frank, Cicero, Ugo Lo, Doriese, William, Durkin, Malcom, Fioretti, Valentina, Geoffray, Hervé, Jacques, Lionel, Kirsch, Christian, Smith, Stephen, Adams, Joseph, Gloaguen, Emilie, Hoogeveen, Ruud, van der Hulst, Paul, Kiviranta, Mikko, van der Kuur, Jan, Ledot, Aurélien, van Leeuwen, Bert-Joost, van Loon, Denni, Lyautey, Bertrand, Parot, Yann, Sakai, Kazuhiro, van Weers, Henk, Abdoelkariem, Shariefa, Adam, Thoma, Adami, Christophe, Aicardi, Corinne, Akamatsu, Hiroki, Alonso, Pablo Eleazar Merino, Amato, Roberta, André, Jérôme, Angelinelli, Matteo, Anon-Cancela, Manuel, Anvar, Shebli, Atienza, Ricardo, Attard, Anthony, Auricchio, Natalia, Balado, Ana, Bancel, Florian, Barusso, Lorenzo Ferrari, Bascuñan, Arturo, Bernard, Vivian, Berrocal, Alicia, Blin, Sylvie, Bonino, Donata, Bonnet, Françoi, Bonny, Patrick, Boorman, Peter, Boreux, Charle, Bounab, Ayoub, Boutelier, Martin, Boyce, Kevin, Brienza, Daniele, Bruijn, Marcel, Bulgarelli, Andrea, Calarco, Simona, Callanan, Paul, Campello, Alberto Prada, Camus, Thierry, Canourgues, Florent, Capobianco, Vito, Cardiel, Nicola, Castellani, Florent, Cheatom, Oscar, Chervenak, Jame, Chiarello, Fabio, Clerc, Laurent, Clerc, Nicola, Cobo, Beatriz, Coeur-Joly, Odile, Coleiro, Alexi, Colonges, Stéphane, Corcione, Leonardo, Coriat, Mickael, Coynel, Alexandre, Cuttaia, Francesco, D’Ai, Antonino, D’anca, Fabio, Dadina, Mauro, Daniel, Christophe, Dauner, Lea, DeNigris, Natalie, Dercksen, Johanne, DiPirro, Michael, Doumayrou, Eric, Dubbeldam, Luc, Dupieux, Michel, Dupourqué, Simon, Durand, Jean Loui, Eckert, Dominique, Eiriz, Valvanera, Ercolani, Eric, Etcheverry, Christophe, Finkbeiner, Fred, Fiocchi, Mariateresa, Fossecave, Hervé, Franssen, Philippe, Frericks, Martin, Gabici, Stefano, Gant, Florent, Gao, Jian-Rong, Gastaldello, Fabio, Genolet, Ludovic, Ghizzardi, Simona, Gil, Ma Angeles Alcacera, Giovannini, Elisa, Godet, Olivier, Gomez-Elvira, Javier, Gonzalez, Raoul, Gonzalez, Manuel, Gottardi, Luciano, Granat, Dolorè, Gros, Michel, Guignard, Nicola, Hieltjes, Paul, Hurtado, Adolfo Jesú, Irwin, Kent, Jacquey, Christian, Janiuk, Agnieszka, Jaubert, Jean, Jiménez, Maria, Jolly, Antoine, Jourdan, Thierry, Julien, Sabine, Kedziora, Bartosz, Korb, Andrew, Kreykenbohm, Ingo, König, Ole, Langer, Mathieu, Laudet, Philippe, Laurent, Philippe, Laurenza, Monica, Lesrel, Jean, Ligori, Sebastiano, Lorenz, Maximilian, Luminari, Alfredo, Maffei, Bruno, Maisonnave, Océane, Marelli, Lorenzo, Massonet, Didier, Maussang, Irwin, Melchor, Alejandro Gonzalo, Le Mer, Isabelle, Millan, Francisco Javier San, Millerioux, Jean-Pierre, Mineo, Teresa, Minervini, Gabriele, Molin, Alexeï, Monestes, David, Montinaro, Nicola, Mot, Baptiste, Murat, David, Nagayoshi, Kenichiro, Nazé, Yaël, Noguès, Loïc, Pailot, Damien, Panessa, Francesca, Parodi, Luigi, Petit, Pascal, Piconcelli, Enrico, Pinto, Ciro, Plaza, Jose Miguel Encina, Plaza, Borja, Poyatos, David, Prouvé, Thoma, Ptak, Andy, Puccetti, Simonetta, Puccio, Elena, Ramon, Pascale, Reina, Manuel, Rioland, Guillaume, Rodriguez, Loui, Roig, Anton, Rollet, Bertrand, Roncarelli, Mauro, Roudil, Gille, Rudnicki, Tomasz, Sanisidro, Julien, Sciortino, Luisa, Silva, Vitor, Sordet, Michael, Soto-Aguilar, Javier, Spizzi, Pierre, Surace, Christian, Sánchez, Miguel Fernández, Taralli, Emanuele, Terrasa, Guilhem, Terrier, Régi, Todaro, Michela, Ubertini, Pietro, Uslenghi, Michela, de Vaate, Jan Geralt Bij, Vaccaro, Davide, Varisco, Salvatore, Varnière, Peggy, Vibert, Laurent, Vidriales, María, Villa, Fabrizio, Vodopivec, Boris Martin, Volpe, Angela, de Vries, Cor, Wakeham, Nichola, Walmsley, Gavin, Wise, Michael, de Wit, Martin, Woźniak, Grzegorz, 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, Astronomía y Astrofísica, 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), Institut de recherche en astrophysique et planétologie (IRAP), Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire Midi-Pyrénées (OMP), Institut de Recherche pour le Développement (IRD)-Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Institut de Recherche pour le Développement (IRD)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Centre National de la Recherche Scientifique (CNRS), SRON Netherlands Institute for Space Research (SRON), Department of Physics [Helsinki], Falculty of Science [Helsinki], Helsingin yliopisto = Helsingfors universitet = University of Helsinki-Helsingin yliopisto = Helsingfors universitet = University of Helsinki, Institut d'Astrophysique et de Géophysique [Liège], Université de Liège, Centrum Astronomiczne im. M. Kopernika, Warszawa (CAMK), Faculty of Civil Engineering [Prague] (FSV CTU), Czech Technical University in Prague (CTU), Columbia Astrophysics Laboratory (CAL), Columbia University [New York], NASA Goddard Space Flight Center (GSFC), AstroParticule et Cosmologie (APC (UMR_7164)), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité), Institut d'astrophysique spatiale (IAS), and Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris-Saclay-Centre National de la Recherche Scientifique (CNRS)-Centre National d’Études Spatiales [Paris] (CNES)
Subjects: X-IFU: The X-ray Integral Field Unit, Cosmology and Nongalactic Astrophysics (astro-ph.CO), The X-ray Integral Field Unit [X-IFU], Solar and stellar astrophysics, FOS: Physical sciences, [PHYS.ASTR.CO]Physics [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], Settore FIS/05 - Astronomia E Astrofisica, X-rays, SDG 7 - Affordable and Clean Energy, Instrumentation and Methods for Astrophysics (astro-ph.IM), Solar and Stellar Astrophysics (astro-ph.SR), High Energy Astrophysical Phenomena (astro-ph.HE), Astrophysics of Galaxies, Athena: the advanced telescope for high energy astrophysics, Astronomy and Astrophysics, Astrophysics - Astrophysics of Galaxies, Astrophysical phenomena, Space instrumentation, Astrophysics - Solar and Stellar Astrophysics, High energy, Space and Planetary Science, Astrophysics of Galaxies (astro-ph.GA), [PHYS.GRQC]Physics [physics]/General Relativity and Quantum Cosmology [gr-qc], the advanced telescope for high energy astrophysics [Athena], Athena: the advanced telescope for high energy astrophysics · X-IFU: The X-ray Integral Field Unit · Space instrumentation · X-rays · Observatory, Observatory, Astrophysics - Instrumentation and Methods for Astrophysics, Astrophysics - High Energy Astrophysical Phenomena, SDG 12 - Responsible Consumption and Production, Astrophysics - Cosmology and Nongalactic Astrophysics
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, 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. (abridged)., Comment: 48 pages, 29 figures, Accepted for publication in Experimental Astronomy with minor editing
Published: 2023
Full Text: View/download PDF

32. X-IFU photon shot noise analysis

Author: LO CICERO, UGO, BARBERA, Marco, ITA, Peille, Philippe, den Hartog, Roland, Kilbourne, Caroline, and Smith, Steve
Abstract: The aim of this technical note is to describe the approach used to calculate the photon shot noise contribution to the energy resolution budget, and to present results from different simulated configurations driving the current preliminary design of the thermal filters in the X-IFU cryostat. The simple code used for the THF conceptual design available at the I-PRR has now migrated into a sophisticated ray-tracing code capable of simulating different configurations of the filter stack environment, allowing to perform a trade-off analysis, failure analysis, and estimating the impact of different sources of uncertainties in the implemented modeling.
Published: 2022

33. Testing the X-IFU calibration requirements: an example for quantum efficiency and energy resolution

Author: Gabriele Betancourt-Martinez, Simon R. Bandler, Didier Barret, Stephen J. Smith, Marco Barbera, Etienne Pointecouteau, Megan E. Eckart, François Pajot, Edoardo Cucchetti, Massimo Cappi, Philippe Peille, Caroline A. Kilbourne, Institut de recherche en astrophysique et planétologie (IRAP), Institut national des sciences de l'Univers (INSU - CNRS)-Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Observatoire Midi-Pyrénées (OMP), Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Centre National de la Recherche Scientifique (CNRS), Centre National d'Études Spatiales [Toulouse] (CNES), Lawrence Livermore National Laboratory (LLNL), Cucchetti, Edoardo, Pajot, Françoi, Pointecouteau, Etienne, Peille, Philippe, Betancourt-Martinez, Gabriele, Smith, Stephen J., Barbera, Marco, Eckart, Megan E., Bandler, Simon R., Kilbourne, Caroline A., Cappi, Massimo, and Barret, Didier
Subjects: Field (physics), FOS: Physical sciences, Condensed Matter Physic, 01 natural sciences, 7. Clean energy, X-ray, Settore FIS/05 - Astronomia E Astrofisica, Band-pass filter, 0103 physical sciences, Calibration, Athena, Electrical and Electronic Engineering, 010306 general physics, 010303 astronomy & astrophysics, Instrumentation and Methods for Astrophysics (astro-ph.IM), ComputingMilieux_MISCELLANEOUS, Physics, X-IFU, [SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph], Electronic, Optical and Magnetic Material, Detector, Astrophysics::Instrumentation and Methods for Astrophysics, Computer Science Applications1707 Computer Vision and Pattern Recognition, Filter (signal processing), Computational physics, Applied Mathematic, Performance verification, Transmission (telecommunications), Quantum efficiency, Astrophysics - Instrumentation and Methods for Astrophysics, Energy (signal processing)
Abstract: With its array of 3840 Transition Edge Sensors (TESs) operated at 90 mK, the X-Ray Integral Field Unit (X-IFU) on board the ESA L2 mission Athena will provide spatially resolved high-resolution spectroscopy (2.5 eV FWHM up to 7 keV) over the 0.2 to 12 keV bandpass. The in-flight performance of the X-IFU will be strongly affected by the calibration of the instrument. Uncertainties in the knowledge of the overall system, from the filter transmission to the energy scale, may introduce systematic errors in the data, which could potentially compromise science objectives - notably those involving line characterisation e.g. turbulence velocity measurements - if not properly accounted for. Defining and validating calibration requirements is therefore of paramount importance. In this paper, we put forward a simulation tool based on the most up-to-date configurations of the various subsystems (e.g. filters, detector absorbers) which allows us to estimate systematic errors related to uncertainties in the instrumental response. Notably, the effect of uncertainties in the energy resolution and of the instrumental quantum efficiency on X-IFU observations is assessed, by taking as a test case the measurements of the iron K complex in the hot gas surrounding clusters of galaxies. In-flight and ground calibration of the energy resolution and the quantum efficiency is also addressed. We demonstrate that provided an accurate calibration of the instrument, such effects should be low in both cases with respect to statistics during observations., Comment: 9 pages, 4 figures, SPIE proceeding Austin 2018
Published: 2018
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33 results on '"Kilbourne, Caroline"'

1. Circumgalactic Medium on the Largest Scales: Detecting X-ray Absorption Lines with Large-Area Microcalorimeters

2. Ground test results of the electromagnetic interference for the x-ray microcalorimeter onboard XRISM

3. Ground test results of the micro-vibration interference for the x-ray microcalorimeter onboard XRISM

4. Line Emission Mapper (LEM): Probing the physics of cosmic ecosystems

5. First Flight Performance of the Micro-X Microcalorimeter X-Ray Sounding Rocket

6. X線分光撮像衛星(XRISM)搭載Resolveの開発状況

7. In-orbit Operation of the Soft X-ray Spectrometer onboard the Hitomi satellite

8. The ATHENA X-ray Integral Field Unit (X-IFU)

9. X線分光撮像衛星 (XRISM) 搭載 Resolve の開発状況

10. The Athena X-ray Integral Field Unit

11. Design and on-orbit operation of the soft x-ray spectrometer adiabatic demagnetization refrigerator on the Hitomi observatory

12. Cryogen-free operation of the Soft X-ray Spectrometer instrument

13. In-flight calibration of Hitomi Soft X-ray Spectrometer. (1) Background

14. In-flight performance of the soft x-ray spectrometer detector system on Astro-H

15. In-flight performance of pulse-processing system of the ASTRO-H/Hitomi soft x-ray spectrometer

16. Ground calibration of the Astro-H (Hitomi) soft x-ray spectrometer

17. In-flight Calibration of Hitomi Soft X-ray Spectrometer (3) Effective Area

18. Search for thermal X-ray features from the Crab nebula with Hitomi Soft X-ray Spectrometer

19. Hitomi Observation of Radio Galaxy NGC 1275: The First X-ray Microcalorimeter Spectroscopy of Fe-K�� Line Emission from an Active Galactic Nucleus

20. $Hitomi$ constraints on the 3.5 keV line in the Perseus galaxy cluster

21. Design, implementation, and performance of the Astro-H soft x-ray spectrometer aperture assembly and blocking filters

22. Cooling system for the soft X-ray spectrometer onboard Astro-H

23. Searching for keV Sterile Neutrino Dark Matter with X-ray Microcalorimeter Sounding Rockets

24. Performance of the helium dewar and the cryocoolers of the Hitomi soft x-ray spectrometer

25. Laboratory X-ray Spectra From L-shell Sulfur Ions Following Charge-exchange Collisions With Two Different Neutral Targets: SF6 And He

26. Spectral Signatures Of Charge Exchange In K-shell X-ray Spectra Of Ar, P, And S Measured With The LLNL Electron Beam Ion Trap

27. Spectroscopic Laboratory Astrophysics Experiments Conducted at the LLNL EBIT Facility in Support of NASA's X-ray Astronomy Flight Program

28. The X-ray observatory Suzaku

29. Fabrication of a Hybrid Transition Edge Sensor Array for Lynx

30. X-ray spectral study of the extended emission, 'the Cap', located 11.6 kpc above the disk of M 82

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

32. X-IFU photon shot noise analysis

33. Testing the X-IFU calibration requirements: an example for quantum efficiency and energy resolution

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