269 results on '"Meidinger, Norbert"'
Search Results
2. CMOS Active Pixel Sensors
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Stefanov, Konstantin D., Holland, Andrew D., den Herder, Jan-Willen, Section editor, Feroci, Marco, Section editor, Meidinger, Norbert, Section editor, Bambi, Cosimo, editor, and Santangelo, Andrea, editor
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- 2024
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3. DEPFET Active Pixel Sensors
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Meidinger, Norbert, Müller-Seidlitz, Johannes, Bambi, Cosimo, editor, and Santangelo, Andrea, editor
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- 2024
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4. X-ray Detectors for Astrophysics
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Herder, J. W. den, Feroci, Marco, Meidinger, Norbert, Bambi, Cosimo, editor, and Santangelo, Andrea, editor
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- 2024
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5. DEPFET Active Pixel Sensors
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Meidinger, Norbert and Müller-Seidlitz, Johannes
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Astrophysics - Instrumentation and Methods for Astrophysics ,Physics - Instrumentation and Detectors - Abstract
An array of DEPFET pixels is one of several concepts to implement an active pixel sensor. Similar to PNCCD and SDD detectors, the typically 0.45 mm thick silicon sensor is fully depleted by the principle of sideward depletion. They have furthermore in common to be back-illuminated detectors, which allows for ultra-thin and homogeneous photon entrance windows. This enables relatively high quantum efficiencies at low energies and close to 100% for photon energies between 1 keV and 10 keV. Steering of the DEPFET sensor is enabled by a so-called Switcher ASIC and readout is performed by e.g. a VERITAS ASIC. The configuration enables a readout time of a few microseconds per row. This results in full frame readout times of a few milliseconds for a 512 x 512 pixel array in a rolling shutter mode. The read noise is then typically three electrons equivalent noise charge RMS. DEPFET detectors can be applied in particular for spectroscopy in the energy band from 0.2 keV to 20 keV. For example, an energy resolution of about 130 eV FWHM is achieved at an energy of 6 keV which is close to the theoretical limit given by Fano noise. Pixel sizes of a few tens of microns up to a centimetre are feasible by the DEPFET concept., Comment: Invited chapter for the "Handbook of X-ray and Gamma-ray Astrophysics" (Eds. C. Bambi and A. Santangelo, Springer Singapore, 2022)
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- 2022
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6. Mitigating the effects of particle background on the Athena Wide-Field Imager
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Miller, Eric D., Grant, Catherine E., Bautz, Marshall W., Molendi, Silvano, Kraft, Ralph, Nulsen, Paul, Bulbul, Esra, Allen, Steven, Burrows, David N., Eraerds, Tanja, Fioretti, Valentina, Gastaldello, Fabio, Hall, David, Hubbard, Michael W. J., Keelan, Jonathan, Meidinger, Norbert, Perinati, Emanuele, Rau, Arne, and Wilkins, Dan
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Astrophysics - Instrumentation and Methods for Astrophysics - Abstract
The Wide Field Imager (WFI) flying on Athena will usher in the next era of studying the hot and energetic Universe. WFI observations of faint, diffuse sources will be limited by uncertainty in the background produced by high-energy particles. These particles produce easily identified "cosmic-ray tracks" along with signals from secondary photons and electrons generated by particle interactions with the instrument. The signal from these secondaries is identical to the X-rays focused by the optics, and cannot be filtered without also eliminating these precious photons. As part of a larger effort to understand the WFI background, we here present results from a study of background-reduction techniques that exploit the spatial correlation between cosmic-ray particle tracks and secondary events. We use Geant4 simulations to generate a realistic particle background, sort this into simulated WFI frames, and process those frames in a similar way to the expected flight and ground software to produce a WFI observation containing only particle background. The technique under study, Self Anti-Coincidence or SAC, then selectively filters regions of the detector around particle tracks, turning the WFI into its own anti-coincidence detector. We show that SAC is effective at improving the systematic uncertainty for observations of faint, diffuse sources, but at the cost of statistical uncertainty due to a reduction in signal. If sufficient pixel pulse-height information is telemetered to the ground for each frame, then this technique can be applied selectively based on the science goals, providing flexibility without affecting the data quality for other science. The results presented here are relevant for any future silicon-based pixelated X-ray imaging detector, and could allow the WFI and similar instruments to probe to truly faint X-ray surface brightness., Comment: 38 pages, 27 figures. Accepted for publication in JATIS. arXiv admin note: text overlap with arXiv:2012.01347
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- 2022
7. Design and performance of the focal plane camera for FXT onboard the Einstein Probe satellite
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Cui, Weiwei, Wang, Hao, Zhao, Xiaofan, Zhang, Juan, Meidinger, Norbert, Yang, Yanji, Keil, Isabell, Zhang, Ziliang, Huo, Jia, Wang, Juan, Song, Zeyu, Lu, Fangjun, Ma, Jia, Wang, Yusa, Xu, Jingjing, Zhu, Yuxuan, Li, Tianming, Li, Wei, Luo, Laidan, Han, Dawei, Zhao, Zijian, Hou, Dongjie, Yang, Xiongtao, Geng, Haoyang, Li, Shuo, Chen, HouLei, Tang, QingJun, Chen, Yehai, and Chen, Yong
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- 2023
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8. Characterisation of the Particle-Induced Background of XMM-Newton EPIC-pn: Short and Long Term Variability
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Bulbul, Esra, Kraft, Ralph, Nulsen, Paul, Freyberg, Michael, Miller, Eric D., Grant, Catherine, Bautz, Mark W., Burrows, David N., Allen, Steven, Eraerds, Tanja, Fioretti, Valentina, Gasteldello, Fabio, Ghirardini, Vittorio, Hall, David, Meidinger, Norbert, Molendi, Silvano, Rau, Arne, Wilkins, Dan, and Wilms, Joern
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Astrophysics - High Energy Astrophysical Phenomena - Abstract
The particle-induced background of X-ray observatories is produced by Galactic Cosmic Ray (GCR) primary protons, electrons, and He ions. Events due to direct interaction with the detector are usually removed by on board processing. The interactions of these primary particles with the detector environment produce secondary particles that mimic X-ray events from celestial sources and are much more difficult to identify. The filter wheel closed data from the XMM-Newton EPIC-pn camera in small window mode (SWM) contains both the X-ray-like background events and the events due to direct interactions with the primary particles. From this data we demonstrate that X-ray-like background events are spatially correlated with the primary particle interaction. This result can be used to further characterise and reduce the non-X-ray background in silicon-based X-ray detectors in current and future missions. We also show that spectrum and pattern fractions of secondary particle events are different from those produced by cosmic X-rays., Comment: 18 pages, 10 figures, 5 tables. Accepted for publication in ApJ
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- 2019
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9. The enhanced X-ray Timing and Polarimetry mission - eXTP
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Zhang, ShuangNan, Santangelo, Andrea, Feroci, Marco, Xu, YuPeng, Lu, FangJun, Chen, Yong, Feng, Hua, Zhang, Shu, Brandt, Søren, Hernanz, Margarita, Baldini, Luca, Bozzo, Enrico, Campana, Riccardo, De Rosa, Alessandra, Dong, YongWei, Evangelista, Yuri, Karas, Vladimir, Meidinger, Norbert, Meuris, Aline, Nandra, Kirpal, Pan, Teng, Pareschi, Giovanni, Orleanski, Piotr, Huang, QiuShi, Schanne, Stephane, Sironi, Giorgia, Spiga, Daniele, Svoboda, Jiri, Tagliaferri, Gianpiero, Tenzer, Christoph, Vacchi, Andrea, Zane, Silvia, Walton, Dave, Wang, ZhanShan, Winter, Berend, Wu, Xin, Zand, Jean J. M. in 't, Ahangarianabhari, Mahdi, Ambrosi, Giovanni, Ambrosino, Filippo, Barbera, Marco, Basso, Stefano, Bayer, Jörg, Bellazzini, Ronaldo, Bellutti, Pierluigi, Bertucci, Bruna, Bertuccio, Giuseppe, Borghi, Giacomo, Cao, XueLei, Cadoux, Franck, Ceraudo, Francesco, Chen, TianXiang, Chen, YuPeng, Chevenez, Jerome, Civitani, Marta, Cui, Wei, Cui, WeiWei, Dauser, Thomas, Del Monte, Ettore, Di Cosimo, Sergio, Diebold, Sebastian, Doroshenko, Victor, Dovciak, Michal, Du, YuanYuan, Ducci, Lorenzo, Fan, QingMei, Favre, Yannick, Fuschino, Fabio, Gálvez, José Luis, Gao, Min, Ge, MingYu, Gevin, Olivier, Grassi, Marco, Gu, QuanYing, Gu, YuDong, Han, DaWei, Hong, Bin, Hu, Wei, Ji, Long, Jia, ShuMei, Jiang, WeiChun, Kennedy, Thomas, Kreykenbohm, Ingo, Kuvvetli, Irfan, Labanti, Claudio, Latronico, Luca, Li, Gang, Li, MaoShun, Li, Xian, Li, Wei, Li, ZhengWei, Limousin, Olivier, Liu, HongWei, Liu, XiaoJing, Lu, Bo, Luo, Tao, Macera, Daniele, Malcovati, Piero, Martindale, Adrian, Michalska, Malgorzata, Meng, Bin, Minuti, Massimo, Morbidini, Alfredo, Muleri, Fabio, Paltani, Stephane, Perinati, Emanuele, Picciotto, Antonino, Piemonte, Claudio, Qu, JinLu, Rachevski, Alexandre, Rashevskaya, Irina, Rodriguez, Jerome, Schanz, Thomas, Shen, ZhengXiang, Sheng, LiZhi, Song, JiangBo, Song, LiMing, Sgro, Carmelo, Sun, Liang, Tan, Ying, Uttley, Phil, Wang, Juan, Wang, LangPing, Wang, YuSa, Watts, Anna L., Wen, XiangYang, Wilms, Jörn, Xiong, ShaoLin, Yang, JiaWei, Yang, Sheng, Yang, YanJi, Yu, Nian, Zhang, WenDa, Zampa, Gianluigi, Zampa, Nicola, Zdziarski, Andrzej A., Zhang, AiMei, Zhang, ChengMo, Zhang, Fan, Zhang, Long, Zhang, Tong, Zhang, Yi, Zhang, XiaoLi, Zhang, ZiLiang, Zhao, BaoSheng, Zheng, ShiJie, Zhou, YuPeng, Zorzi, Nicola, and Zwart, J. Frans
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Astrophysics - Instrumentation and Methods for Astrophysics ,Astrophysics - High Energy Astrophysical Phenomena - Abstract
In this paper we present the enhanced X-ray Timing and Polarimetry mission - eXTP. eXTP is a space science mission designed to study fundamental physics under extreme conditions of density, gravity and magnetism. The mission aims at determining the equation of state of matter at supra-nuclear density, measuring effects of QED, and understanding the dynamics of matter in strong-field gravity. In addition to investigating fundamental physics, eXTP will be a very powerful observatory for astrophysics that will provide observations of unprecedented quality on a variety of galactic and extragalactic objects. In particular, its wide field monitoring capabilities will be highly instrumental to detect the electro-magnetic counterparts of gravitational wave sources. The paper provides a detailed description of: (1) the technological and technical aspects, and the expected performance of the instruments of the scientific payload; (2) the elements and functions of the mission, from the spacecraft to the ground segment., Comment: Accepted for publication on Sci. China Phys. Mech. Astron. (2019)
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- 2018
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10. Magnetic shielding of soft protons in future X-ray telescopes: the case of the ATHENA Wide Field Imager
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Fioretti, Valentina, Bulgarelli, Andrea, Molendi, Silvano, Lotti, Simone, Macculi, Claudio, Barbera, Marco, Mineo, Teresa, Piro, Luigi, Cappi, Massimo, Dadina, Mauro, Meidinger, Norbert, von Kienlin, Andreas, and Rau, Arne
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Astrophysics - Instrumentation and Methods for Astrophysics - Abstract
Both the interplanetary space and the Earth magnetosphere are populated by low energy ($\leq300$ keV) protons that are potentially able to scatter on the reflecting surface of Wolter-I optics of X-ray focusing telescopes and reach the focal plane. This phenomenon, depending on the X-ray instrumentation, can dramatically increase the background level, reducing the sensitivity or, in the most extreme cases, compromising the observation itself. The use of a magnetic diverter, deflecting protons away from the field of view, requires a detailed characterization of their angular and energy distribution when exiting the mirror. We present the first end-to-end Geant4 simulation of proton scattering by X-ray optics and the consequent interaction with the diverter field and the X-ray detector assembly, selecting the ATHENA Wide Field Imager as a case study for the evaluation of the residual soft proton induced background. We obtain that, in absence of a magnetic diverter, protons are indeed funneled towards the focal plane, with a focused Non X-ray Background well above the level required by ATHENA science objectives ($5\times10^{-4}$ counts cm$^{-2}$ s$^{-1}$ keV$^{-1}$), for all the plasma regimes encountered in both L1 and L2 orbits. These results set the proton diverter as a mandatory shielding system on board the ATHENA mission and all high throughput X-ray telescopes operating in the interplanetary space. For a magnetic field computed to deflect 99\% of the protons that would otherwise reach the WFI, Geant4 simulations show that this configuration, in the assumption of a uniform field, would efficiently shield the focal plane, yielding a residual background level of the order or below the requirement., Comment: Accepted for publication on The Astrophysical Journal on 28/08/2018
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- 2018
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11. The Wide Field Imager Instrument for Athena
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Meidinger, Norbert, Eder, Josef, Eraerds, Tanja, Nandra, Kirpal, Pietschner, Daniel, Plattner, Markus, Rau, Arne, and Strecker, Rafael
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Astrophysics - Instrumentation and Methods for Astrophysics - Abstract
The WFI (Wide Field Imager) instrument is planned to be one of two complementary focal plane cameras on ESA's next X-ray observatory Athena. It combines unprecedented survey power through its large field of view of 40 amin x 40 amin together with excellent count rate capability (larger than 1 Crab). The energy resolution of the silicon sensor is state-of-the-art in the energy band of interest from 0.2 keV to 15 keV, e.g. the full width at half maximum of a line at 7 keV will be better than 170 eV until the end of the nominal mission phase. This performance is accomplished by using DEPFET active pixel sensors with a pixel size of 130 x 130 microns is well suited to the on-axis angular resolution of 5 arcsec half energy width (HEW) of the mirror system. Each DEPFET pixel is a combined sensor-amplifier structure with a MOSFET integrated onto a fully depleted 450 micron thick silicon bulk. Two detectors are planned for the WFI instrument: A large-area detector comprising four sensors with a total of 1024 x 1024 pixels and a fast detector optimized for high count rate observations. This high count rate capable detector permits for bright point sources with an intensity of 1 Crab a throughput of more than 80% and a pile-up of less than 1 %. The fast readout of the DEPFET pixel matrices is facilitated by an ASIC development, called VERITAS-2. Together with the Switcher-A, a control ASIC that allows for operation of the DEPFET in rolling shutter mode, these elements form the key components of the WFI detectors. The detectors are surrounded by a graded-Z shield, which has in particular the purpose to avoid fluorescence lines that would contribute to the instrument background...[Abridged], Comment: 12 pages, 6 figures, SPIE Astronomical Telescopes and Instrumentation, Edinburgh (26 June - 1 July, 2016)
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- 2017
12. DEPFET Active Pixel Sensors
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Meidinger, Norbert, primary and Müller-Seidlitz, Johannes, additional
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- 2022
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13. Athena Wide Field Imager Key Science Drivers
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Rau, Arne, Nandra, Kirpal, Aird, James, Comastri, Andrea, Dauser, Thomas, Merloni, Andrea, Pratt, Gabriel W., Reiprich, Thomas H., Fabian, Andy C., Georgakakis, Antonis, Güdel, Manuel, Różańska, Agata, Sanders, Jeremy S., Sasaki, Manami, Vaughan, Simon, Wilms, Jörn, and Meidinger, Norbert
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Astrophysics - Instrumentation and Methods for Astrophysics ,Astrophysics - High Energy Astrophysical Phenomena - Abstract
The Wide Field Imager (WFI) is one of two instruments for the Advanced Telescope for High-ENergy Astrophysics (Athena). In this paper we summarise three of the many key science objectives for the WFI - the formation and growth of supermassive black holes, non-gravitational heating in clusters of galaxies, and spin measurements of stellar mass black holes - and describe their translation into the science requirements and ultimately instrument requirements. The WFI will be designed to provide excellent point source sensitivity and grasp for performing wide area surveys, surface brightness sensitivity, survey power, and absolute temperature and density calibration for in-depth studies of the outskirts of nearby clusters of galaxies and very good high-count rate capability, throughput, and low pile-up, paired with very good spectral resolution, for detailed explorations of bright Galactic compact objects., Comment: 11 pages, 10 figures, 1 table, SPIE Astronomical Telescopes and Instrumentation, Edinburgh (26 June - 1 July, 2016)
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- 2016
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14. Characterization of the detection chain of the Micro-channel X-ray Telescope
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Ceraudo, Francesco, Meuris, Aline, Doumayrou, Eric, Dumaye, Luc, Goetschy, Alain, Lavanant, Tony, Lortholary, Michel, Le Mer, Isabelle, Nico, François, Pinsard, Frédéric, Prieur, Marin, Renaud, Diana, Schneider, Benjamin, Tourrette, Thierry, Visticot, François, Meidinger, Norbert, Mießner, Danilo, and Götz, Diego
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- 2020
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15. Characterization of the x-ray beam at PANTER
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Hartner, Gisela, primary, Burwitz, Vadim, additional, Müller, Thomas, additional, Rukdee, Surangkhana, additional, Schmidt, Thomas, additional, Langmeier, Andreas, additional, Dennerl, Konrad, additional, and Meidinger, Norbert, additional
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- 2023
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16. eROSITA on SRG
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Predehl, Peter, Boehringer, Hans, Brunner, Hermann, Brusa, Marcella, Burwitz, Vadim, Cappelluti, Nico, Churazov, Evgeniy, Dennerl, Konrad, Finoguenov, Alexis, Freyberg, Michael, Friedrich, Peter, Hasinger, Guenther, Kendziorra, Eckhard, Kreykenbohm, Ingo, Schmid, Christian, Wilms, Joern, Lamer, Georg, Meidinger, Norbert, Muehlegger, Martin, Pavlinsky, Mikhail, Robrade, Jan, Santangelo, Andrea, Schmitt, Juergen, Schwope, Axel, Steinmetz, Matthias, Strueder, Lothar, Sunyaev, Rashid, and Tenzer, Chris
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Astrophysics - Cosmology and Nongalactic Astrophysics ,Astrophysics - High Energy Astrophysical Phenomena - Abstract
eROSITA (extended ROentgen Survey with an Imaging Telescope Array) is the core instrument on the Russian Spektrum-Roentgen-Gamma (SRG) mission which is scheduled for launch in late 2012. eROSITA is fully approved and funded by the German Space Agency DLR and the Max-Planck-Society.The design driving science is the detection of 50-100 thousands Clusters of Galaxies up to redshift z~1.3 in order to study the large scale structure in the Universe and test cosmological models, especially Dark Energy. This will be accomplished by an all-sky survey lasting for four years plus a phase of pointed observations. eROSITA consists of seven Wolter-I telescope modules, each equipped with 54 Wolter-I shells having an outer diameter of 360 mm. This would provide and effective area at 1.5 keV of ~1500 cm2 and an on axis PSF HEW of 15" which would provide an effective angular resolution of 25"-30". In the focus of each mirror module, a fast frame-store pn-CCD will provide a field of view of 1deg in diameter for an active FOV of ~0.83 deg2. At the time of writing the instrument development is currently in phase C/D., Comment: 6 Pages, 3 Figure, Proceedings of the conference "X-ray Astronomy 2009", Bologna, September 2009
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- 2010
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17. Improving XMM-Newton EPIC pn data at low energies: method and application to the Vela SNR
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Dennerl, Konrad, Aschenbach, Bernd, Briel, Ulrich G., Brunner, Hermann, Burwitz, Vadim, Englhauser, Jakob, Freyberg, Michael J., Haberl, Frank, Hartner, Gisela, Iyudin, Anatoli F., Kendziorra, Eckhard, Meidinger, Norbert, Pfeffermann, Elmar, Pietsch, Wolfgang, Strueder, Lothar, and Zavlin, Vyacheslav E.
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Astrophysics - Abstract
High quantum efficiency over a broad spectral range is one of the main properties of the EPIC pn camera on-board XMM-Newton. The quantum efficiency rises from ~75% at 0.2 keV to ~100% at 1 keV, stays close to 100% until 8 keV, and is still ~90% at 10 keV. The EPIC pn camera is attached to an X-ray telescope which has the highest collecting area currently available, in particular at low energies (more than 1400 cm2 between 0.1 and 2.0 keV). Thus, this instrument is very sensitive to the low-energy X-ray emission. However, X-ray data at energies below ~0.2 keV are considerably affected by detector effects, which become more and more important towards the lowest transmitted energies. In addition to that, pixels which have received incorrect offsets during the calculation of the offset map at the beginning of each observation, show up as bright patches in low-energy images. Here we describe a method which is not only capable of suppressing the contaminations found at low energies, but which also improves the data quality throughout the whole EPIC pn spectral range. This method is then applied to data from the Vela supernova remnant., Comment: Proc. SPIE Vol. 5488: Astronomical Telescopes and Instrumentation, UV - Gamma-Ray Space Telescope Systems, Eds. Guenther Hasinger and Martin J. Turner, 22-24 June 2004, Glasgow, Scotland United Kingdom
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- 2004
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18. Design and acoustic tests of the ATHENA WFI filter wheel assembly development model towards TRL5
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Polak, Szymon, primary, Musiał, Jacek, additional, Pietrzak, Robert, additional, Sikorski, Adam, additional, Dumin, Mateusz, additional, Dacko, Adam, additional, Rataj, Mirosiław, additional, Barciński, Tomasz, additional, Kamisiński, Tadeusz, additional, Pilch, Adam, additional, Binek, Wojciech, additional, Woźniak, Grzegorz, additional, Zuchniak, Monika, additional, Różańska, Agata, additional, Meidinger, Norbert, additional, Plattner, Marcus, additional, Frank, Jintin, additional, Strecker, Rafael, additional, von Kienlin, Andreas, additional, Barbera, Marco, additional, D’Anca, Fabio, additional, Gulli, Daniele, additional, Lo Cicero, Ugo, additional, Montinaro, Nicola, additional, Parodi, Giancarlo, additional, Bozzo, Enrico, additional, and Paltani, Stephane, additional
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- 2023
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19. The enhanced x-ray timing and polarimetry mission: eXTP: an update on its scientific cases, mission profile and development status
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Zhang, Shuang Nan, Santangelo, Andrea, Xu, Yupeng, Feroci, Marco, Hernanz, Margarita, Lu, Fangjun, Chen, Yong, Feng, Hua, Nandra, Kirpal, Jiang, Weichun, Svoboda, Jiri, Brandt, Søren, Schanne, Stéphane, Zand, Jean, Michalska, Malgorzata, Bozzo, Enrico, Kalemci, Emrah, Agudo, Ivan, Ahangarianabhari, Mahdi, Aitink-Kroes, Gabby, Ambrosi, Giovanni, Ambrosino, Filippo, An, Zhenghua, Perez Torres, Miguel Angel, Antonelli, Matias, Argan, Andrea, Babinec, Viktor, Baldini, Luca, Barbera, Marco, van Baren, Coen, Baudin, David, Bayer, Jörg, Bellazzini, Ronaldo, Bellutti, Pierluigi, Bertucci, Bruna, Bertuccio, Giuseppe, Bi, Xingzi, Boezio, Mirko, Bonvicini, Valter, Bonvicini, Walter, Bordas, Pol, Borghese, Alice, Borghi, Giacomo, Bouyjou, Florent, Bozkurt, Ayhan, Brez, Alessandro, Brienza, Daniele, Cadoux, Franck, Campana, Riccardo, Cao, Jiewei, Cao, Xuelei, Casares, Jorge, Cavazzuti, Elisabetta, Ceraudo, Francesco, Chen, Tianxiang, Chen, Wen, Chen, Can, Chen, Yupeng, Chen, Xin, Chen, Yehai, Chenevez, Jerome, Cheng, Yaodong, Cirrincione, Daniela, Civitani, Marta, Cong, Min, Zelati, Francesco Coti, Cui, Weiwei, Cui, Tao, Cui, Wei, Dai, Boyu, Dauser, Thomas, De Angelis, Nicolas, De Marco, Barbara, De Rosa, Alessandra, Monte, Ettore Del, Cosimo, Sergio Di, Diebold, Sebastian, Dilillo, Giuseppe, Ding, Fei, Dohnal, Roman, Dong, Zefang, Donnarumma, Immacolata, Dovciak, Michal, Du, Yuanyuan, Ducci, Lorenzo, Evangelista, Yuri, Fan, Qingmei, Favre, Yannick, Ferrés, Patrícia, Fiandrini, Emanuele, Ficorella, Francesco, Fuschino, Fabio, Gálvez, José Luis, Gao, Na, Gao, Min, Ge, Yuqiang, Ge, Mingyu, Gevin, Olivier, Grassi, Marco, Gu, Yudong, Gu, Quanying, Guan, Ju, Guedel, Manuel, Han, Xingbo, Han, Dawei, He, Huilin, He, Junwang, Hedderman, Paul, den Herder, Jan Willem, Hong, Bin, Hormaetxe, Ander, Hou, Dongjie, Hu, Zexun, Hu, Hao, Hu, Qingbao, Hu, Yu, Huang, Yue, Huang, Jiangjiang, Huang, Qiushi, Huo, Jia, Hynek, Richard, Iwasawa, Kazumi, Izzo, Lucca, Ji, Long, Jia, Shumei, Jiang, Bowen, Jiang, Wei, Jiang, Jiechen, Jiang, Xiaowei, Jiao, Yang, Jin, Ge, Jin, Fan, Jose, Jordi, Karas, Vladimir, Kennedy, Thomas, Kirsch, Christian, Kole, Merlin, Komarek, Martin, Kreykenbohm, Ingo, Kuiper, Lucien, Kuvvetli, Irfan, Labanti, Claudio, Latronico, Luca, Laubert, Phillip, Li, Tao, Li, Longhui, Li, Hong, Li, Duo, Li, Wei, Li, Maoshun, Li, Gang, Li, Xiaobo, Li, Chengkui, Li, Bing, Li, Haibo, Liang, Hong, Liao, Qiuyan, Liao, Jinyuan, Limousin, Olivier, Lin, Yanjian, Linares, Manuel, Liu, Rui, Liu, Yichen, Liu, Zhihao, Liu, Hongwei, Liu, Xiaojing, Liu, Xiaohua, Cicero, Ugo Lo, Loehring, Jens, Lombardi, Giovanni, Lorenz, Maximilian, Lu, Bing, Lucchesi, Leonardo, Luo, Tao, Luo, Laidan, Ma, Jia, Ma, Xiang, Macera, Daniele, Malcovati, Piero, Manfreda, Alberto, Paredes, Josep Maria, Marinucci, Andrea, Martindale, Adrian, Meidinger, Norbert, Mele, Filippo, Mendes, Vasco, Meng, Bin, Merkl, Martin, Meuris, Aline, Miniutti, Giovanni, Minuti, Massimo, Morbidini, Alfredo, Morgante, Gianluca, Muleri, Fabio, Munini, Riccardo, Mussolin, Lorenzo, Negri, Barbara, Nie, Jianyin, Novák, Petr, Nowosielski, Witold, Nuti, Alessio, Onat, Ahmet, Orleanski, Piotr, Orsini, Leonardo, Ottensamer, Roland, Ou, Ge, Pacciani, Luigi, Paltani, Stephane, Pan, Teng, Pan, Kai, Pareschi, Giovanni, Patruno, Alessandro, Pepponi, Giancarlo, Perinati, Emanuele, Piazzolla, Raffaele, Picciotto, Antonino, Piemonte, Claudio, Pinchera, Michele, Pliego, Samuel, Poutanen, Juri, Qi, Liqiang, Qi, Fazhi, Qiang, Pengfei, Qiao, Fangjian, Qiao, Zheng, Qiu, Xiangbiao, Qiu, Chengbo, Qu, Jinlu, Rachevski, Alexandre, Rashevskaia, Irina, Rea, Nanda, Ribo, Marc, de la Rie, Rob, Rodriguez, Jerome, Gil, Pablo Rodríguez, Sala, Gloria, Schanz, Thomas, Serafinelli, Roberto, Sgro, Carmelo, Shen, Zhengxiang, Sheng, Lizhi, Shi, Jingyan, Sironi, Giorgia, Skup, Konrad, Song, Liming, Song, Zeyu, Song, Jiangbo, Spandre, Gloria, Spiga, Daniele, Su, Yongquan, Sun, Liang, Sungur, Müberra, Svéda, Libor, Tagliaferri, Gianpiero, Tan, Ying, Tao, Lian, Tcherniak, Denis, Tenzer, Chris, Todaro, Michela, Tolos, Laura, Torok, Gabriel, Torres, Diego F., Trois, Alessio, Turhan, Onur, Uttley, Phil, Vacchi, Andrea, Virgilli, Enrico, Vogel, Channah, Walton, Dave, Wang, Jian, Wang, Xianqi, Wang, Bo, Wang, Langping, Wang, Xiaofeng, Wang, Dianlong, Wang, Yusa, Wang, Juan, Wang, Hao, Wang, Ruijie, Wang, Ping, Wang, Lingjun, Wang, Wenshuai, Wang, Tian, Wang, Haoyu, Wang, Zhanshan, Watts, Anna L., Wen, Xiangyang, Wilms, Jörn, Winter, Berend, Wu, Xin, Wu, Chao, Wu, Zhenyu, Wu, Qiong, Wu, Kaiji, Xiong, Hao, Xiong, Shaolin, Xu, Wei, Xu, Zhao, Xu, Jingjing, Xu, Xiongwei, Xue, Jiadai, Yan, Yongqing, Yan, Xingtao, Yang, Xianghui, Yang, Yanji, Yang, Xiongtao, Yang, Sheng, Yang, Jiawei, Yang, Yingquan, Yi, Shuxu, Yu, Yonggao, Yu, Ke, Zampa, Ganluigi, Zampa, Nicola, Zane, Silvia, Zdziarski, Andrzej A., Zhang, Long, Zhang, Shu, Zhang, Wenda, Zhang, Xiaoli, Zhang, Zhen, Zhang, Jiawei, Zhang, Fan, Zhang, Ziliang, Zhang, Dali, Zhang, Honglin, Zhang, Aimei, Zhang, Tong, Zhang, Hongmei, Zhang, Juan, Zhang, Liang, Zhang, Yueting, Zhao, Li, Zhao, Baosheng, Zhao, Zijian, Zhao, Xiaofan, Zhao, Haisheng, Zhao, Xiaoyun, Zheng, Shijie, Zhou, Yupeng, Zhou, Xiaohong, Zhu, Jiahuan, Zhu, Yuxuan, Zhu, Cheng, Zhu, Zhencai, Zorzi, Nicola, Zwart, Frans, den Herder, Jan-Willem A., Nikzad, Shouleh, Nakazawa, Kazuhiro, Chinese Academy of Sciences, Agenzia Spaziale Italiana, Ministerio de Ciencia e Innovación (España), Federal Ministry of Economics and Technology (Germany), and Foundation for Polish Science
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Equation of state ,Extreme gravity ,Black hole ,X-ray timing ,X-ray polarimetry ,Neutron star ,Extreme magnetism ,Extreme density - Abstract
Space Telescopes and Instrumentation 2022: Ultraviolet to Gamma Ray (2022), Montreal, Jul 17-22, 2022.--Proceedings of SPIE - The International Society for Optical Engineering vol. 12181 Article number 121811W.-- Full list of authors: Zhang, Shuang-Nan; Santangelo, Andrea; Xu, Yupeng; Feroci, Marco; Hernanz, Margarita; Lu, Fangjun; Chen, Yong; Feng, Hua; Nandra, Kirpal; Jiang, Weichun; Svoboda, Jiri; Brandt, Soren; Schanne, Stephane; in't Zand, Jean; Michalska, Malgorzata; Bozzo, Enrico; Kalemci, Emrah; Agudo, Ivan; Ahangarianabhari, Mahdi; Aitink-Kroes, Gabby; Ambrosi, Giovanni; Ambrosino, Filippo; An, Zhenghua; Perez Torres, Miguel Angel; Antonelli, Matias; Argan, Andrea; Babinec, Viktor; Baldini, Luca; Barbera, Marco; van Baren, Coen; Baudin, David; Bayer, Joerg; Bellazzini, Ronaldo; Bellutti, Pierluigi; Bertucci, Bruna; Bertuccio, Giuseppe; Bi, Xingzi; Boezio, Mirko; Bonvicini, Valter; Bonvicini, Walter; Bordas, Pol; Borghese, Alice; Borghi, Giacomo; Bouyjou, Florent; Bozkurt, Ayhan; Brez, Alessandro; Brienza, Daniele; Cadoux, Franck; Campana, Riccardo; Cao, Jiewei; Cao, Xuelei; Casares, Jorge; Cavazzuti, Elisabetta; Ceraudo, Francesco; Chen, Tianxiang; Chen, Wen; Chen, Can; Chen, Yupeng; Chen, Xin; Chen, Yehai; Chenevez, Jerome; Cheng, Yaodong; Cirrincione, Daniela; Civitani, Marta; Cong, Min; Coti Zelati, Francesco; Cui, Weiwei; Cui, Tao; Cui, Wei; Dai, Boyu; Dauser, Thomas; De Angelis, Nicolas; De Marco, Barbara; De Rosa, Alessandra; Del Monte, Ettore; Di Cosimo, Sergio; Diebold, Sebastian; Dilillo, Giuseppe; Ding, Fei; Dohnal, Roman; Dong, Zefang; Donnarumma, Immacolata; Dovciak, Michal; Du, Yuanyuan; Ducci, Lorenzo; Evangelista, Yuri; Fan, Qingmei; Favre, Yannick; Ferres, Patricia; Fiandrini, Emanuele; Ficorella, Francesco; Fuschino, Fabio; Luis Galvez, Jose; Gao, Na; Gao, Min; Ge, Yuqiang; Ge, Mingyu; Gevin, Olivier; Grassi, Marco; Gu, Yudong; Gu, Quanying; Guan, Ju; Guedel, Manuel; Han, Xingbo; Han, Dawei; He, Huilin; He, Junwang; Hedderman, Paul; den Herder, Jan-Willem; Hong, Bin; Hormaetxe, Ander; Hou, Dongjie; Hu, Zexun; Hu, Hao; Hu, Qingbao; Hu, Yu; Huang, Yue; Huang, Jiangjiang; Huang, Qiushi; Huo, Jia; Hynek, Richard; Iwasawa, Kazumi; Izzo, Lucca; Ji, Long; Jia, Shumei; Jiang, Bowen; Jiang, Wei; Jiang, Jiechen; Jiang, Xiaowei; Jiao, Yang; Jin, Ge; Jin, Fan; Jose, Jordi; Karas, Vladimir; Kennedy, Thomas; Kirsch, Christian; Kole, Merlin; Komarek, Martin; Kreykenbohm, Ingo; Kuiper, Lucien; Kuvvetli, Irfan; Labanti, Claudio; Latronico, Luca; Laubert, Phillip; Li, Tao; Li, Longhui; Li, Hong; Li, Duo; Li, Wei; Li, Maoshun; Li, Gang; Li, Xiaobo; Li, Chengkui; Li, Bing; Li, Haibo; Liang, Hong; Liao, Qiuyan; Liao, Jinyuan; Limousin, Olivier; Lin, Yanjian; Linares, Manuel; Liu, Rui; Liu, Yichen; Liu, Zhihao; Liu, Hongwei; Liu, Xiaojing; Liu, Xiaohua; Lo Cicero, Ugo; Loehring, Jens; Lombardi, Giovanni; Lorenz, Maximilian; Lu, Bing; Lucchesi, Leonardo; Luo, Tao; Luo, Laidan; Ma, Jia; Ma, Xiang; Macera, Daniele; Malcovati, Piero; Manfreda, Alberto; Maria Paredes, Josep; Marinucci, Andrea; Martindale, Adrian; Meidinger, Norbert; Mele, Filippo; Mendes, Vasco; Meng, Bin; Merkl, Martin; Meuris, Aline; Miniutti, Giovanni; Minuti, Massimo; Morbidini, Alfredo; Morgante, Gianluca; Muleri, Fabio; Munini, Riccardo; Mussolin, Lorenzo; Negri, Barbara; Nie, Jianyin; Novak, Petr; Nowosielski, Witold; Nuti, Alessio; Onat, Ahmet; Orleanski, Piotr; Orsini, Leonardo; Ottensamer, Roland; Ou, Ge; Pacciani, Luigi; Paltani, Stephane; Pan, Teng; Pan, Kai; Pareschi, Giovanni; Patruno, Alessandro; Pepponi, Giancarlo; Perinati, Emanuele; Piazzolla, Raffaele; Picciotto, Antonino; Piemonte, Claudio; Pinchera, Michele; Pliego, Samuel; Poutanen, Juri; Qi, Liqiang; Qi, Fazhi; Qiang, Pengfei; Qiao, Fangjian; Qiao, Zheng; Qiu, Xiangbiao; Qiu, Chengbo; Qu, Jinlu; Rachevski, Alexandre; Rashevskaia, Irina; Rea, Nanda; Ribo, Marc; de la Rie, Rob; Rodriguez, Jerome; Rodriguez Gil, Pablo; Sala, Gloria; Schanz, Thomas; Serafinelli, Roberto; Sgro, Carmelo; Shen, Zhengxiang; Sheng, Lizhi; Shi, Jingyan; Sironi, Giorgia; Skup, Konrad; Song, Liming; Song, Zeyu; Song, Jiangbo; Spandre, Gloria; Spiga, Daniele; Su, Yongquan; Sun, Liang; Sungur, Muberra; Sveda, Libor; Tagliaferri, Gianpiero; Tan, Ying; Tao, Lian; Tcherniak, Denis; Tenzer, Chris; Todaro, Michela; Tolos, Laura; Torok, Gabriel; Torres, Diego F.; Trois, Alessio; Turhan, Onur; Uttley, Phil; Vacchi, Andrea; Virgilli, Enrico; Vogel, Channah; Walton, Dave; Wang, Jian; Wang, Xianqi; Wang, Bo; Wang, Langping; Wang, Xiaofeng; Wang, Dianlong; Wang, Yusa; Wang, Juan; Wang, Hao; Wang, Ruijie; Wang, Ping; Wang, Lingjun; Wang, Wenshuai; Wang, Tian; Wang, Haoyu; Wang, Zhanshan; Watts, Anna L.; Wen, Xiangyang; Wilms, Joern; Winter, Berend; Wu, Xin; Wu, Chao; Wu, Zhenyu; Wu, Qiong; Wu, Kaiji; Xiong, Hao; Xiong, Shaolin; Xu, Wei; Xu, Zhao; Xu, Jingjing; Xu, Xiongwei; Xue, Jiadai; Yan, Yongqing; Yan, Xingtao; Yang, Xianghui; Yang, Yanji; Yang, Xiongtao; Yang, Sheng; Yang, Jiawei; Yang, Yingquan; Yi, Shuxu; Yu, Yonggao; Yu, Ke; Zampa, Ganluigi; Zampa, Nicola; Zane, Silvia; Zdziarski, Andrzej A.; Zhang, Long; Zhang, Shu; Zhang, Wenda; Zhang, Xiaoli; Zhang, Zhen; Zhang, Jiawei; Zhang, Fan; Zhang, Ziliang; Zhang, Dali; Zhang, Honglin; Zhang, Aimei; Zhang, Tong; Zhang, Hongmei; Zhang, Juan; Zhang, Liang; Zhang, Yueting; Zhao, Li; Zhao, Baosheng; Zhao, Zijian; Zhao, Xiaofan; Zhao, Haisheng; Zhao, Xiaoyun; Zheng, Shijie; Zhou, Yupeng; Zhou, Xiaohong; Zhu, Jiahuan; Zhu, Yuxuan; Zhu, Cheng; Zhu, Zhencai; Zorzi, Nicola; Zwart, Frans, The enhanced X-ray Timing and Polarimetry mission (eXTP) is a flagship observatory for X-ray timing, spectroscopy and polarimetry developed by an International Consortium. Thanks to its very large collecting area, good spectral resolution and unprecedented polarimetry capabilities, eXTP will explore the properties of matter and the propagation of light in the most extreme conditions found in the Universe. eXTP will, in addition, be a powerful X-ray observatory. The mission will continuously monitor the X-ray sky, and will enable multiwavelength and multi-messenger studies. The mission is currently in phase B, which will be completed in the middle of 2022. © 2022 SPIE. All rights reserved., The Chinese team acknowledges support by the Chinese Academy of Sciences through the Strategic Priority Research Program, Grant No. XDA15020100. The Italian authors acknowledge funding support by the Italian Space Agency (under agreement n. 2020-3-HH.0 and ASI-INAF n.2017-14-H.O) and INFN (project XRO -X-ray Observatories). The Spanish authors acknowledge funding support from the MICIN/AEI grant PID2019-108709GB-I00. The German team acknowledges support from the Bundesministerium fur Wirtschaft und Technologie through the Deutsches Zentrum fur Luft-und Raumfahrt e.V. (DLR) under the grant number FKZ 50 OO 1902. The Polish team acknowledges FNP grant POIR.04.04.00-00-5C65/17. The Czech team acknowledges support from the GACR project 21-06825X. The Turkish team acknowledges support from the Turkish Space Agency., With funding from the Spanish government through the Severo Ochoa Centre of Excellence accreditation SEV-2017-0709
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- 2022
20. SRG/eROSITA status and operations during the first four all-sky surveys
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Coutinho, Diogo, primary, Ramos, Miriam, additional, Dennerl, Konrad, additional, Haberl, Frank, additional, Meidinger, Norbert, additional, Merloni, Andrea, additional, Predehl, Peter, additional, Stewart, Ian, additional, Freyberg, Michael, additional, Bornemann, Walter, additional, Brunner, Hermann, additional, Burwitz, Vadim, additional, Czesla, Stefan, additional, Eder, J., additional, Friedrich, Susanne, additional, Gaida, Roland, additional, Gueguen, Alain, additional, Hartner, Gisela, additional, Kink, Walter, additional, Kreykenbohm, Ingo, additional, Lamer, Georg, additional, Maitra, Chandreyee, additional, Mernik, Thomas, additional, Müller, Siegfried, additional, Nandra, Kirpal, additional, Pfefferman, Elmar, additional, and Robrade, Jan, additional
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- 2022
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21. SRG/eROSITA micrometeoroid hits and effects
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Freyberg, Michael J., primary, Müller, Thomas, additional, Perinati, Emanuele, additional, Krüger, Harald, additional, Strub, Peter, additional, Tenzer, Christopher, additional, Merloni, Andrea, additional, Meidinger, Norbert, additional, Predehl, Peter, additional, Friedrich, Susanne, additional, Coutinho, Diogo, additional, Ramos-Ceja, Miriam, additional, Maitra, Chandreyee, additional, Dennerl, Konrad, additional, and Pommranz, Christian, additional
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- 2022
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22. Results of the development of the MXT x-ray telescope for the SVOM mission
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Mercier, Karine, primary, Gonzalez, François, additional, Götz, Diego, additional, Boutelier, Martin, additional, Boufracha, Narjiss, additional, Clamagirand, Sebastien, additional, Fort, Adrien, additional, Gomes, Albert, additional, Guilhem, Emmanuel, additional, Le Duigou, Jean-Michel, additional, MAZEAU, Sophie, additional, Sanisidro, Julien, additional, Meuris, Aline, additional, Feldman, Charlotte F., additional, Pearson, James F., additional, Willingale, Richard, additional, Burwitz, Vadim, additional, Meidinger, Norbert, additional, and Robinet, Florent, additional
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- 2022
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23. X-Ray Detectors and XRF Detection Channels
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Scholze, Frank, Longoni, Antonio, Fiorini, Carlo, Strüder, Lothar, Meidinger, Norbert, Hartmann, Robert, Kawahara, Naoki, Shoji, Takashi, Beckhoff, Burkhard, editor, Kanngießer, habil. Birgit, editor, Langhoff, Norbert, editor, Wedell, Reiner, editor, and Wolff, Helmut, editor
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- 2006
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24. A pnCCD Detector System for High Speed Optical Applications
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Hartmann, Robert, Gorke, Hubert, Meidinger, Norbert, Soltau, Heike, Strüder, Lothar, Beletic, Jenna E., editor, Beletic, James W., editor, and Amico, Paola, editor
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- 2006
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25. Mitigating the effects of particle background on the Athena Wide Field Imager
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Miller, Eric D., primary, Grant, Catherine E., additional, Bautz, Marshall W., additional, Molendi, Silvano, additional, Kraft, Ralph, additional, Nulsen, Paul, additional, Bulbul, Esra, additional, Allen, Steven, additional, Burrows, David N., additional, Eraerds, Tanja, additional, Fioretti, Valentina, additional, Gastaldello, Fabio, additional, Hall, David, additional, Hubbard, Michael W. J., additional, Keelan, Jonathan, additional, Meidinger, Norbert, additional, Perinati, Emanuele, additional, Rau, Arne, additional, and Wilkins, Dan, additional
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- 2022
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26. Development of the focal plane PNCCD camera system for the X-ray space telescope eROSITA
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Meidinger, Norbert, Andritschke, Robert, Ebermayer, Stefanie, Elbs, Johannes, Hälker, Olaf, Hartmann, Robert, Herrmann, Sven, Kimmel, Nils, Schächner, Gabriele, Schopper, Florian, Soltau, Heike, Strüder, Lothar, and Weidenspointner, Georg
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- 2010
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27. Large-format, high-speed, X-ray pnCCDs combined with electron and ion imaging spectrometers in a multipurpose chamber for experiments at 4th generation light sources
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Strüder, Lothar, Epp, Sascha, Rolles, Daniel, Hartmann, Robert, Holl, Peter, Lutz, Gerhard, Soltau, Heike, Eckart, Rouven, Reich, Christian, Heinzinger, Klaus, Thamm, Christian, Rudenko, Artem, Krasniqi, Faton, Kühnel, Kai-Uwe, Bauer, Christian, Schröter, Claus-Dieter, Moshammer, Robert, Techert, Simone, Miessner, Danilo, Porro, Matteo, Hälker, Olaf, Meidinger, Norbert, Kimmel, Nils, Andritschke, Robert, Schopper, Florian, Weidenspointner, Georg, Ziegler, Alexander, Pietschner, Daniel, Herrmann, Sven, Pietsch, Ullrich, Walenta, Albert, Leitenberger, Wolfram, Bostedt, Christoph, Möller, Thomas, Rupp, Daniela, Adolph, Marcus, Graafsma, Heinz, Hirsemann, Helmut, Gärtner, Klaus, Richter, Rainer, Foucar, Lutz, Shoeman, Robert L., Schlichting, Ilme, and Ullrich, Joachim
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- 2010
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28. Enhanced simulations on the Athena/Wide Field Imager instrumental background
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Eraerds, Tanja, primary, Antonelli, Valeria, additional, Davis, Chris, additional, Hall, David, additional, Hetherington, Oliver, additional, Holland, Andrew, additional, Hubbard, Michael, additional, Meidinger, Norbert, additional, Miller, Eric, additional, Molendi, Silvano, additional, Perinati, Emanuele, additional, Pietschner, Daniel, additional, and Rau, Arne, additional
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- 2021
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29. eROSITA camera array on the SRG satellite
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Meidinger, Norbert, primary, Andritschke, Robert, additional, Dennerl, Konrad, additional, Emberger, Valentin, additional, Eraerds, Tanja, additional, Hälker, Olaf, additional, Hartner, Gisela, additional, Pietschner, Daniel, additional, and Reiffers, Jonas, additional
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- 2021
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30. Enhanced simulations on the ATHENA/WFI instrumental background
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Eraerds, Tanja, Antonelli, Valeria, Davis, Chris, Hall, David, Hetherington, Oliver, Holland, Andrew, Keelan, Jonathan, Meidinger, Norbert, Miller, Eric D., Molendi, Silvano, Perinati, Emanuele, pietschner@mpe.mpg.de, Daniel, Rau, Arne, den Herder, Jan-Willem A., Nakazawa, Kazuhiro, and Nikzad, Shouleh
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Physics ,COSMIC cancer database ,Astrophysics::High Energy Astrophysical Phenomena ,Astrophysics::Instrumentation and Methods for Astrophysics ,Lagrangian point ,Astronomy ,Astrophysics::Cosmology and Extragalactic Astrophysics ,Radiation ,law.invention ,Telescope ,Cardinal point ,Observatory ,law ,Halo ,Halo orbit - Abstract
The Wide Field Imager (WFI) is one of two focal plane instruments of the Advanced Telescope for High-Energy Astrophysics (Athena), ESA’s next large X-ray observatory, planned for launch in the early 2030’s. The current baseline halo orbit is around L2, the first Lagrangian point of the Sun-Earth system, L1 is under consideration. For both potential halo orbits the radiation environment, solar and cosmic protons, electrons and He-ions will affect the performance of the instruments. A further critical contribution to the instrument background arises from the unfocused cosmic hard X-ray background. It is important to understand and estimate the expected instrumental background and to investigate measures, like design modifications or analysis methods, which could improve the expected background level in order to achieve the challenging scientific requirement (< 5 × 10−3 cts/cm2/keV/s at 2 - 7 keV). Previous WFI background simulations1 done in Geant4 have been improved by taking into account new information about the proton flux at L2. In addition, the simulation model of the WFI instrument and its surroundings employed in GEANT4 simulations has been refined to follow the technological development of the WFI camera.
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- 2020
31. SRG/eROSITA early phase and commissioning operations
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Coutinho, Diogo, primary, Bornemann, Walter, additional, Gaida, Roland, additional, Hartner, Gisela, additional, Kink, Walter, additional, Meidinger, Norbert, additional, Müller, Siegfried, additional, and Predehl, Peter, additional
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- 2020
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32. Structural analysis of Athena WFI large detector array
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Frank, Jintin, primary, Beitler, Christian, additional, Pietschner, Daniel, additional, Strecker, Rafael, additional, Antonelli, Valeria, additional, Plattner, Markus, additional, and Meidinger, Norbert, additional
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- 2020
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33. The calibration of eROSITA on SRG
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Dennerl, Konrad, primary, Andritschke, Robert, additional, Bräuninger, Heinrich, additional, Burkert, Wolfgang, additional, Burwitz, Vadim, additional, Emberger, Valentin, additional, Freyberg, Michael, additional, Friedrich, Peter, additional, Gaida, Roland, additional, Granato, Stefanie, additional, Hartner, Gisela, additional, von Kienlin, Andreas, additional, Meidinger, Norbert, additional, Menz, Benedikt, additional, and Predehl, Peter, additional
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- 2020
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34. Development status of the wide field imager instrument for Athena
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Meidinger, Norbert, primary, Albrecht, Sebastian, additional, Beitler, Christian, additional, Bonholzer, Michael, additional, Emberger, Valentin, additional, Frank, Jintin, additional, Lederhuber, Andreas, additional, Müller-Seidlitz, Johannes, additional, Nandra, Kirpal, additional, Oser, Julian, additional, Ott, Sabine, additional, Plattner, Markus, additional, and Strecker, Rafael, additional
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- 2020
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35. SRG/eROSITA in-flight background at L2
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Freyberg, Michael, primary, Perinati, Emanuele, additional, Pacaud, Florian, additional, Eraerds, Tanja, additional, Churazov, Eugene, additional, Dennerl, Konrad, additional, Predehl, Peter, additional, Merloni, Andrea, additional, Meidinger, Norbert, additional, Bulbul, Esra, additional, Friedrich, Susanne, additional, Gilfanov, Marat, additional, Tenzer, Chris, additional, Pommranz, Christian, additional, Eckert, Dominique, additional, Schmitt, Juergen, additional, Brusa, Marcella, additional, and Santangelo, Andrea, additional
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- 2020
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36. Status of the follow-up x-ray telescope onboard the Einstein Probe satellite
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Chen, Yong, primary, Cui, WeiWei, additional, Han, DaWei, additional, Wang, Juan, additional, Yang, YanJi, additional, Wang, YuSa, additional, Li, Wei, additional, Ma, Jia, additional, Xu, YuPeng, additional, Lu, FangJun, additional, Chen, HouLei, additional, Tang, QingJun, additional, Yuan, Weimin, additional, Friedrich, Peter, additional, Meidinger, Norbert, additional, Keil, Isabell, additional, Burwitz, Vadim, additional, Eder, Josef, additional, Hartmann, Katinka, additional, Nandra, Kirpal, additional, Keereman, Arnoud, additional, Santovincenzo, Andrea, additional, Vernani, Dervis, additional, Bianucci, Giovanni, additional, Valsecchi, Giuseppe, additional, Wang, Bo, additional, Wang, LangPing, additional, Wang, DianLong, additional, Li, Duo, additional, Sheng, LiZhi, additional, Qiang, PengFei, additional, Shi, RongRong, additional, Chao, XiangYu, additional, Song, ZeYu, additional, Zhang, Ziliang, additional, Huo, Jia, additional, Wang, Hao, additional, Cong, Min, additional, Yang, XiongTao, additional, Hou, DongJie, additional, Zhao, XiaoFan, additional, Zhao, ZiJian, additional, Chen, TianXiang, additional, Li, MaoShun, additional, Zhang, Tong, additional, Luo, LaiDan, additional, Xu, JingJing, additional, Li, Gang, additional, Zhang, Qian, additional, Bi, XiYan, additional, Zhu, YuXuan, additional, Yu, Nian, additional, Chen, Can, additional, Lv, ZhongHua, additional, Lu, Bing, additional, and Zhang, JiaWei, additional
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- 2020
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37. Technology development of Athena WFI frame processor electronics and verification of its real-time performance
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Plattner, Markus, primary, Albrecht, Sebastian, additional, Haelker, Olaf, additional, Lederhuber, Andreas, additional, Meidinger, Norbert, additional, Ott, Sabine, additional, Pliego, Samuel, additional, Reiffers, Jonas, additional, Schanz, Thomas, additional, and Tenzer, Chris, additional
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- 2020
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38. The eROSITA camera array on the SRG satellite
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Meidinger, Norbert, primary, Andritschke, Robert, additional, Dennerl, Konrad, additional, Emberger, Valentin, additional, Eraerds, Tanja, additional, Haelker, Olaf, additional, Hartner, Gisela, additional, Pietschner, Daniel, additional, and Reiffers, Jonas, additional
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- 2020
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39. Results of the development of the MXT x-ray telescope for the SVOM mission
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den Herder, Jan-Willem A., Nikzad, Shouleh, Nakazawa, Kazuhiro, Mercier, Karine, Gonzalez, François, Götz, Diego, Boutelier, Martin, Boufracha, Narjiss, Clamagirand, Sebastien, Fort, Adrien, Gomes, Albert, Guilhem, Emmanuel, Le Duigou, Jean-Michel, Mazeau, Sophie, Sanisidro, Julien, Meuris, Aline, Feldman, Charlotte, Pearson, Jim, Willingale, Richard, Burwitz, Vadim, Meidinger, Norbert, and Robinet, Florent
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- 2022
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40. The direct measurement of the signal charge behavior in pnCCDs with subpixel resolution
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Kimmel, Nils, Hiraga, Junko S., Hartmann, Robert, Meidinger, Norbert, and Strüder, Lothar
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- 2006
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41. Next generation of pnCCDs for X-ray spectroscopy and imaging
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Meidinger, Norbert, Andritschke, Robert, Hälker, Olaf, Hartmann, Robert, Herrmann, Sven, Holl, Peter, Lutz, Gerhard, Kimmel, Nils, Schaller, Gerhard, Schnecke, Martina, Schopper, Florian, Soltau, Heike, and Strüder, Lothar
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- 2006
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42. pnCCD for photon detection from near-infrared to X-rays
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Meidinger, Norbert, Andritschke, Robert, Hartmann, Robert, Herrmann, Sven, Holl, Peter, Lutz, Gerhard, and Strüder, Lothar
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- 2006
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43. Characterization of the Particle-induced Background of XMM-Newton EPIC-pn: Short- and Long-term Variability
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Bulbul, Esra, primary, Kraft, Ralph, additional, Nulsen, Paul, additional, Freyberg, Michael, additional, Miller, Eric D., additional, Grant, Catherine, additional, Bautz, Mark W., additional, Burrows, David N., additional, Allen, Steven, additional, Eraerds, Tanja, additional, Fioretti, Valentina, additional, Gastaldello, Fabio, additional, Ghirardini, Vittorio, additional, Hall, David, additional, Meidinger, Norbert, additional, Molendi, Silvano, additional, Rau, Arne, additional, Wilkins, Dan, additional, and Wilms, Joern, additional
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- 2020
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44. Alpha particle, proton and x-ray damage in fully depleted PN-junction CCD detectors for x-ray imaging and spectroscopy
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Meidinger, Norbert, Schmalhofer, Bernhard, and Struder, Lothar
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Charge coupled devices -- Evaluation ,Electronic equipment and supplies, Effect of radiation on -- Research ,Ionizing radiation -- Research ,Nuclear counters -- Evaluation ,Semiconductors, Effect of radiation on -- Research ,Business ,Electronics ,Electronics and electrical industries - Abstract
The development of a novel charge coupled device, the fully depleted ph-junction CCD (pn-CCD), has been completed. It will be used as focal plane detector for X-ray imaging and spectroscopy on two scientific satellite missions, XMM and ABRIXAS. A comprehensive, quantitative study of the radiation damage in the pn-CCD was performed with 10-MeV protons, 5.5 MeV alpha-particles and soft X-rays. The irradiation by soft X-rays with a dose of 23 krad(Si) caused no performance degradation. The A-centre (oxygen-vacancy defect) and the divacancy trap were generated by particle irradiations which are both inevitably in silicon. But no other trap type affected the charge transfer in the tested operating temperature range between 75 K and 240 K. The formation probability of the dominant trap type, the A-centre, is presented for proton and alpha-particle irradiation. We have measured the effects of particle fluence and temperature on trap generation as well as the variation of trap concentration. The measured energy resolution of the irradiated pn-CCDs proves the high radiation hardness of this type of charge coupled device. The full width at half maximum of the Mn - [K.sub.Alpha] line (5894 eV) was increased from 135 eV to 175 eV (FWHM/E = 3%) after exposure to a 10-MeV proton fluence of 2 [Center dot] [10.sup.9] [cm.sup.-2]. The results differ from that of other charge coupled devices because of the different detector concept and fabrication process.
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- 1998
45. pnCCDs on XMM-Newton—42 months in orbit
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Strüder, Lothar, Englhauser, Jakob, Hartmann, Robert, Holl, Peter, Meidinger, Norbert, Soltau, Heike, Briel, Ulrich, Dennerl, Konrad, Freyberg, Michael, Haberl, Frank, Hartner, Gisela, Pfeffermann, Elmar, Stadlbauer, Thomas, and Kendziorra, Eckehard
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- 2003
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46. First measurements with a frame store PN-CCD X-ray detector
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Meidinger, Norbert, Bonerz, Stefan, Eckhardt, Rouven, Englhauser, Jakob, Hartmann, Robert, Hasinger, Günther, Holl, Peter, Krause, Norbert, Lutz, Gerhard, Richter, Rainer, Soltau, Heike, Strüder, Lothar, and Trümper, Joachim
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- 2003
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47. Status of the wide field imager instrument for Athena
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Meidinger, Norbert, primary, Albrecht, Sebastian, additional, Bonholzer, Michael, additional, Müller-Seidlitz, Johannes, additional, Nandra, Kirpal, additional, Ott, Sabine, additional, Plattner, Markus, additional, and Treberspurg, Wolfgang, additional
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- 2019
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48. Electrical characterization of prototype DEPFET detectors for Athena's Wide Field Imager
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Bonholzer, Michael, primary, Andritschke, Robert, additional, Emberger, Valentin, additional, Meidinger, Norbert, additional, Müller-Seidlitz, Johannes, additional, and Treberspurg, Wolfgang, additional
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- 2019
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49. The enhanced X-ray Timing and Polarimetry mission—eXTP
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Zhang, ShuangNan, primary, Santangelo, Andrea, additional, Feroci, Marco, additional, Xu, YuPeng, additional, Lu, FangJun, additional, Chen, Yong, additional, Feng, Hua, additional, Zhang, Shu, additional, Brandt, Søren, additional, Hernanz, Margarita, additional, Baldini, Luca, additional, Bozzo, Enrico, additional, Campana, Riccardo, additional, De Rosa, Alessandra, additional, Dong, YongWei, additional, Evangelista, Yuri, additional, Karas, Vladimir, additional, Meidinger, Norbert, additional, Meuris, Aline, additional, Nandra, Kirpal, additional, Pan, Teng, additional, Pareschi, Giovanni, additional, Orleanski, Piotr, additional, Huang, QiuShi, additional, Schanne, Stephane, additional, Sironi, Giorgia, additional, Spiga, Daniele, additional, Svoboda, Jiri, additional, Tagliaferri, Gianpiero, additional, Tenzer, Christoph, additional, Vacchi, Andrea, additional, Zane, Silvia, additional, Walton, Dave, additional, Wang, ZhanShan, additional, Winter, Berend, additional, Wu, Xin, additional, in’ t Zand, Jean J. M., additional, Ahangarianabhari, Mahdi, additional, Ambrosi, Giovanni, additional, Ambrosino, Filippo, additional, Barbera, Marco, additional, Basso, Stefano, additional, Bayer, Jörg, additional, Bellazzini, Ronaldo, additional, Bellutti, Pierluigi, additional, Bertucci, Bruna, additional, Bertuccio, Giuseppe, additional, Borghi, Giacomo, additional, Cao, XueLei, additional, Cadoux, Franck, additional, Ceraudo, Francesco, additional, Chen, TianXiang, additional, Chen, YuPeng, additional, Chevenez, Jerome, additional, Civitani, Marta, additional, Cui, Wei, additional, Cui, WeiWei, additional, Dauser, Thomas, additional, Del Monte, Ettore, additional, Di Cosimo, Sergio, additional, Diebold, Sebastian, additional, Doroshenko, Victor, additional, Dovciak, Michal, additional, Du, YuanYuan, additional, Ducci, Lorenzo, additional, Fan, QingMei, additional, Favre, Yannick, additional, Fuschino, Fabio, additional, Gálvez, José Luis, additional, Gao, Min, additional, Ge, MingYu, additional, Gevin, Olivier, additional, Grassi, Marco, additional, Gu, QuanYing, additional, Gu, YuDong, additional, Han, DaWei, additional, Hong, Bin, additional, Hu, Wei, additional, Ji, Long, additional, Jia, ShuMei, additional, Jiang, WeiChun, additional, Kennedy, Thomas, additional, Kreykenbohm, Ingo, additional, Kuvvetli, Irfan, additional, Labanti, Claudio, additional, Latronico, Luca, additional, Li, Gang, additional, Li, MaoShun, additional, Li, Xian, additional, Li, Wei, additional, Li, ZhengWei, additional, Limousin, Olivier, additional, Liu, HongWei, additional, Liu, XiaoJing, additional, Lu, Bo, additional, Luo, Tao, additional, Macera, Daniele, additional, Malcovati, Piero, additional, Martindale, Adrian, additional, Michalska, Malgorzata, additional, Meng, Bin, additional, Minuti, Massimo, additional, Morbidini, Alfredo, additional, Muleri, Fabio, additional, Paltani, Stephane, additional, Perinati, Emanuele, additional, Picciotto, Antonino, additional, Piemonte, Claudio, additional, Qu, JinLu, additional, Rachevski, Alexandre, additional, Rashevskaya, Irina, additional, Rodriguez, Jerome, additional, Schanz, Thomas, additional, Shen, ZhengXiang, additional, Sheng, LiZhi, additional, Song, JiangBo, additional, Song, LiMing, additional, Sgro, Carmelo, additional, Sun, Liang, additional, Tan, Ying, additional, Uttley, Phil, additional, Wang, Bo, additional, Wang, DianLong, additional, Wang, GuoFeng, additional, Wang, Juan, additional, Wang, LangPing, additional, Wang, YuSa, additional, Watts, Anna L., additional, Wen, XiangYang, additional, Wilms, Jörn, additional, Xiong, ShaoLin, additional, Yang, JiaWei, additional, Yang, Sheng, additional, Yang, YanJi, additional, Yu, Nian, additional, Zhang, WenDa, additional, Zampa, Gianluigi, additional, Zampa, Nicola, additional, Zdziarski, Andrzej A., additional, Zhang, AiMei, additional, Zhang, ChengMo, additional, Zhang, Fan, additional, Zhang, Long, additional, Zhang, Tong, additional, Zhang, Yi, additional, Zhang, XiaoLi, additional, Zhang, ZiLiang, additional, Zhao, BaoSheng, additional, Zheng, ShiJie, additional, Zhou, YuPeng, additional, Zorzi, Nicola, additional, and Zwart, J. Frans, additional
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- 2018
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50. Magnetic Shielding of Soft Protons in Future X-Ray Telescopes: The Case of the ATHENA Wide Field Imager
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Fioretti, Valentina, primary, Bulgarelli, Andrea, additional, Molendi, Silvano, additional, Lotti, Simone, additional, Macculi, Claudio, additional, Barbera, Marco, additional, Mineo, Teresa, additional, Piro, Luigi, additional, Cappi, Massimo, additional, Dadina, Mauro, additional, Meidinger, Norbert, additional, von Kienlin, Andreas, additional, and Rau, Arne, additional
- Published
- 2018
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