251 results on '"Doriese, W."'
Search Results
2. System Performance of a TDM Test-Bed with Long Flex Harness Toward the New X-IFU FPA-DM
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Vaccaro, D., de Wit, M., van der Kuur, J., Gottardi, L., Ravensberg, K., Taralli, E., Adams, J., Bandler, S. R., Chervenak, J. A., Doriese, W. B., Durkin, M., Reintsema, C., Sakai, K., Smith, S. J., Wakeham, N. A., Jackson, B., Khosropanah, P., Gao, J.-R., den Herder, J. W. A., and Roelfsema, P.
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- 2024
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3. Indium Bump Bonding: Advanced Integration Techniques for Low-Temperature Detectors and Readout
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Lucas, T. J., Biesecker, J. P., Doriese, W. B., Duff, S. M., Durkin, M. S., Lew, R. A., Ullom, J. N., Vissers, M. R., and Schmidt, D. R.
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- 2024
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4. Development of an End-to-End Demonstration Readout Chain for Athena/X-IFU
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Beaumont, S., Pajot, F., Roudil, G., Adams, J. S., Bandler, S. R., Bertrand, B., Betancourt-Martinez, G., Castellani, F., Chervenak, J. A., Daniel, C., Denison, E. V., Doriese, W. B., Dupieux, M., Durkin, M., Geoffray, H., Hilton, G. C., Parot, Y., Peille, P., Prêle, D., Ravera, L., Reintsema, C. D., Sakai, K., Smith, S. J., Stevens, R. W., Ullom, J. N., Vale, L. R., and Wakeham, N. A.
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- 2022
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5. Developments of Laboratory-Based Transition-Edge Sensor Readout Electronics Using Commercial-Off-The-Shelf Modules
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Sakai, K., Adams, J. S., Bandler, S. R., Beaumont, S., Chervenak, J. A., Doriese, W. B., Durkin, M., Finkbeiner, F. M., Hull, S. V., Kelley, R. L., Kilbourne, C. A., Muramatsu, H., Porter, F. S., Reintsema, C. D., Smith, S. J., Wakeham, N. A., and Wassel, E. J.
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- 2022
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6. Indium Bump Process for Low-Temperature Detectors and Readout
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Lucas, T. J., Biesecker, J. P., Doriese, W. B., Duff, S. M., Hilton, G. C., Ullom, J. N., Vissers, M. R., and Schmidt, D. R.
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- 2022
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7. X-ray Spectroscopy of Muonic Atoms Isolated in Vacuum with Transition Edge Sensors
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Okada, S., Azuma, T., Bennett, D. A., Caradonna, P., Doriese, W. B., Durkin, M. S., Fowler, J. W., Gard, J. D., Hashimoto, T., Hayakawa, R., Hilton, G. C., Ichinohe, Y., Indelicato, P., Isobe, T., Kanda, S., Katsuragawa, M., Kawamura, N., Kino, Y., Miyake, Y., Morgan, K. M., Ninomiya, K., Noda, H., O’Neil, G. C., Okumura, T., Reintsema, C. D., Schmidt, D. R., Shimomura, K., Strasser, P., Swetz, D. S., Takahashi, T., Takeda, S., Takeshita, S., Tatsuno, H., Ueno, Y., Ullom, J. N., Watanabe, S., and Yamada, S.
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- 2020
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8. First Operation of TES Microcalorimeters in Space with the Micro-X Sounding Rocket
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Adams, J. S., Baker, R., Bandler, S. R., Bastidon, N., Danowski, M. E., Doriese, W. B., Eckart, M. E., Figueroa-Feliciano, E., Goldfinger, D. C., Heine, S. N. T., Hilton, G. C., Hubbard, A. J. F., Kelley, R. L., Kilbourne, C. A., Manzagol-Harwood, R. E., McCammon, D., Okajima, T., Porter, F. S., Reintsema, C. D., Serlemitsos, P., Smith, S. J., Ullom, J. N., and Wikus, P.
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- 2020
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9. On Low-Energy Tail Distortions in the Detector Response Function of X-Ray Microcalorimeter Spectrometers
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O’Neil, G. C., Szypryt, P., Takacs, E., Tan, J. N., Buechele, S. W., Naing, A. S., Joe, Y. I., Swetz, D., Schmidt, D. R., Doriese, W. B., Gard, J. D., Reintsema, C. D., Ullom, J. N., Villarrubia, J. S., and Ralchenko, Yu.
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- 2020
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10. Micro-X Sounding Rocket: Transitioning from First Flight to a Dark Matter Configuration
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Adams, J. S., Anderson, A. J., Baker, R., Bandler, S. R., Bastidon, N., Castro, D., Danowski, M. E., Doriese, W. B., Eckart, M. E., Figueroa-Feliciano, E., Goldfinger, D. C., Heine, S. N. T., Hilton, G. C., Hubbard, A. J. F., Kelley, R. L., Kilbourne, C. A., Manzagol-Harwood, R. E., McCammon, D., Okajima, T., Porter, F. S., Reintsema, C. D., Serlemitsos, P., Smith, S. J., and Wikus, P.
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- 2020
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11. TES X-ray Spectrometer at SLAC LCLS-II
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Li, Dale, Alpert, B. K., Becker, D. T., Bennett, D. A., Carini, G. A., Cho, H.-M., Doriese, W. B., Dusatko, J. E., Fowler, J. W., Frisch, J. C., Gard, J. D., Guillet, S., Hilton, G. C., Holmes, M. R., Irwin, K. D., Kotsubo, V., Lee, S.-J., Mates, J. A. B., Morgan, K. M., Nakahara, K., Pappas, C. G., Reintsema, C. D., Schmidt, D. R., Smith, S. R., Swetz, D. S., Thayer, J. B., Titus, C. J., Ullom, J. N., Vale, L. R., Van Winkle, D. D., Wessels, A., and Zhang, L.
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- 2018
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12. Detector Calibration for the Micro-X Sounding Rocket X-ray Telescope
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Goldfinger, D. C., Adams, J. S., Baker, R., Bandler, S. R., Bastidon, N., Danowski, M. E., Doriese, W. B., Eckart, M. E., Figueroa-Feliciano, E., Heine, S. N. T., Hilton, G. C., Hubbard, A. J. F., Kelley, R. L., Kilbourne, C. A., Manzagol-Harwood, R. E., McCammon, D., Okajima, T., Porter, F. S., Reintsema, C. D., Serlemitsos, P., Smith, S. J., and Wikus, P.
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- 2018
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13. Error-Correcting Codes for Code-Division Multiplexed TES Detectors
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Titus, C. J., Chaudhuri, S., Cho, H.-M., Dawson, C., Doriese, W. B., Fowler, J. W., Hilton, G. C., Irwin, K. D., Kuenstner, S., Li, D., Morgan, K., Reintsema, C. D., Swetz, D. S., Ullom, J. N., and Young, B. A.
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- 2018
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14. Approaches to the Optimal Nonlinear Analysis of Microcalorimeter Pulses
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Fowler, J. W., Pappas, C. G., Alpert, B. K., Doriese, W. B., O’Neil, G. C., Ullom, J. N., and Swetz, D. S.
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- 2018
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15. A Highly Linear Calibration Metric for TES X-ray Microcalorimeters
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Pappas, C. G., Fowler, J. W., Bennett, D. A., Doriese, W. B., Joe, Y. I., Morgan, K. M., O’Neil, G. C., Ullom, J. N., and Swetz, D. S.
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- 2018
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16. Line Emission Mapper (LEM): Probing the physics of cosmic ecosystems
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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
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- 2022
17. A 50 mK test bench for demonstration of the readout chain of Athena/X-IFU
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Florent Castellani, Sophie Beaumont, François Pajot, Gilles Roudil, Joseph Adams, Simon Bandler, James Chervenak, Christophe Daniel, Denison, Edward V., Bertrand Doriese, W., Michel Dupieux, Malcolm Durkin, Hervé Geoffray, Hilton, Gene C., David Murat, Yann Parot, Philippe Peille, Damien Prêle, Laurent Ravera, Reintsema, Carl D., Kazuhiro Sakai, Stevens, Robert W., Ullom, Joel N., Vale, Leila R., Nicholas Wakeham, 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), NASA Goddard Space Flight Center (GSFC), Centre National d'Études Spatiales [Toulouse] (CNES), National Institute of Standards and Technology [Boulder] (NIST), 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, and Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité)
- Subjects
Athena/X-IFU ,X-ray instrumentation ,FOS: Physical sciences ,[PHYS.PHYS.PHYS-INS-DET]Physics [physics]/Physics [physics]/Instrumentation and Detectors [physics.ins-det] ,[PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph] ,Astrophysics - Instrumentation and Methods for Astrophysics ,Instrumentation and Methods for Astrophysics (astro-ph.IM) ,end-to-end cryogenic readout ,[SDU.ASTR.IM]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Instrumentation and Methods for Astrophysic [astro-ph.IM] - Abstract
The X-IFU (X-ray Integral Field Unit) onboard the large ESA mission Athena (Advanced Telescope for High ENergy Astrophysics), planned to be launched in the mid 2030s, will be a cryogenic X-ray imaging spectrometer operating at 55 mK. It will provide unprecedented spatially resolved high-resolution spectroscopy (2.5 eV FWHM up to 7 keV) in the 0.2-12 keV energy range thanks to its array of TES (Transition Edge Sensors) microcalorimeters of more than 2k pixel. The detection chain of the instrument is developed by an international collaboration: the detector array by NASA/GSFC, the cold electronics by NIST, the cold amplifier by VTT, the WFEE (Warm Front-End Electronics) by APC, the DRE (Digital Readout Electronics) by IRAP and a focal plane assembly by SRON. To assess the operation of the complete readout chain of the X-IFU, a 50 mK test bench based on a kilo-pixel array of microcalorimeters from NASA/GSFC has been developed at IRAP in collaboration with CNES. Validation of the test bench has been performed with an intermediate detection chain entirely from NIST and Goddard. Next planned activities include the integration of DRE and WFEE prototypes in order to perform an end-to-end demonstration of a complete X-IFU detection chain., Proceedings-of-the-SPIE-The-International-Society-for-Optical-Engineering SPIE-Int. Soc. Opt. Eng, In press
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- 2022
18. Absolute Energy Calibration of X-ray TESs with 0.04 eV Uncertainty at 6.4 keV in a Hadron-Beam Environment
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Tatsuno, H., Doriese, W. B., Bennett, D. A., Curceanu, C., Fowler, J. W., Gard, J., Gustafsson, F. P., Hashimoto, T., Hayano, R. S., Hays-Wehle, J. P., Hilton, G. C., Iliescu, M., Ishimoto, S., Itahashi, K., Iwasaki, M., Kuwabara, K., Ma, Y., Marton, J., Noda, H., O’Neil, G. C., Okada, S., Outa, H., Reintsema, C. D., Sato, M., Schmidt, D. R., Shi, H., Suzuki, K., Suzuki, T., Uhlig, J., Ullom, J. N., Widmann, E., Yamada, S., Zmeskal, J., and Swetz, D. S.
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- 2016
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19. Microcalorimeter Array Development for the ATHENA X-Ray Integral Field Unit
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Smith, Stephen, Adams, J. S, Bandler, S. R, Chervenak, James A, Datesman, Aaron M, Eckart, M. E, Ewin, A. J, Finkbeiner, F. M, Hummatov, R, Kelley, R. L, Kilbourne, C. A, Miniussi, A. R, Porter, F. S, Sadleir, J. S, Sakai, K, Wakeham, N, Wassell, E. J, Akamatsu, H, Gottardi, L, den Hartog, R. H, Jackson, B. D, van der Kuur, J, Bennett, D. A, Doriese, W. R, Hilton, G. C, Swetz, D, and Ullom, J. N
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Astrophysics - Abstract
The X-ray integral field unit (X-IFU) for ESA's Athena X-ray observatory will consist of 3840 AC-biased transition edge sensors (TESs), read out using frequency domain multiplexing (FDM). In this paper we describe details of the latest pixels geometries that are being designed for the current baseline array configuration. This includes details on how important TES properties (transition parameters, thermal design of the pixels, absorber composition) are being optimized to meet the target energy resolution, count-rate and quantum efficiency. We also present the latest design optimizations specifically targeted at mitigating AC-bias phenomena in Mo/Au TESs that can degrade performance.
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- 2018
20. The Practice of Pulse Processing
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Fowler, J. W., Alpert, B. K., Doriese, W. B., Joe, Y. -I., O’Neil, G. C., Ullom, J. N., and Swetz, D. S.
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- 2016
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21. Developments in Time-Division Multiplexing of X-ray Transition-Edge Sensors
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Doriese, W. B., Morgan, K. M., Bennett, D. A., Denison, E. V., Fitzgerald, C. P., Fowler, J. W., Gard, J. D., Hays-Wehle, J. P., Hilton, G. C., Irwin, K. D., Joe, Y. I., Mates, J. A. B., O’Neil, G. C., Reintsema, C. D., Robbins, N. O., Schmidt, D. R., Swetz, D. S., Tatsuno, H., Vale, L. R., and Ullom, J. N.
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- 2016
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22. High-Resolution Kaonic-Atom X-ray Spectroscopy with Transition-Edge-Sensor Microcalorimeters
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Okada, S., Bennett, D. A., Doriese, W. B., Fowler, J. W., Irwin, K. D., Ishimoto, S., Sato, M., Schmidt, D. R., Swetz, D. S., Tatsuno, H., Ullom, J. N., and Yamada, S.
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- 2014
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23. Transition-Edge Sensors for Particle Induced X-ray Emission Measurements
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Palosaari, M. R. J., Kinnunen, K. M., Julin, J., Laitinen, M., Napari, M., Sajavaara, T., Doriese, W. B., Fowler, J., Reintsema, C., Swetz, D., Schmidt, D., Ullom, J., and Maasilta, I. J.
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- 2014
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24. Status of the Micro-X Sounding Rocket X-Ray Spectrometer
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Goldfinger, D. C, Adams, J. S, Baker, R, Bandler, S. R, Danowski, M. E, Doriese, W. B, Eckart, M. E, Figueroa-Feliciano, E, Hilton, G. C, Hubbard, A. J. F, Kelley, R. L, Kilbourne, C. A, McCammon, D, Okajima, T, Porter, F. S, Reintsema, C. D, Serlemitsos, P, Smith, S. J, Heine, S. N. T, and Wikus, P
- Subjects
Astronomy - Abstract
Micro-X is a sounding rocket borne X-ray telescope that utilizes transition edge sensors to perform imaging spectroscopy with a high level of energy resolution. Its 2.1m focal length X-ray optic has an effective area of 300 sq cm, a field of view of 11.8 arcmin, and a bandpass of 0.12.5 keV. The detector array has 128 pixels and an intrinsic energy resolution of 4.5 eV FWHM. The integration of the system has progressed with functional tests of the detectors and electronics complete, and performance characterization of the detectors is underway. We present an update of ongoing progress in preparation for the upcoming launch of the instrument.
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- 2016
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25. Transition-Edge Sensor Pixel Parameter Design of the Microcalorimeter Array for the X-Ray Integral Field Unit on Athena
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Smith, S. J, Adams, J. S, Bandler, S. R, Betancourt-Martinez, G. L, Chervenak, J. A, Chiao, M. P, Eckart, M. E, Finkbeiner, F. M, Kelley, R. L, Kilbourne, C. A, Miniussi, A. R, Porter, F. S, Sadleir, J. E, Sakai, K, Wakeham, N. A, Wassell, E. J, Yoon, W, Bennett, D. A, Doriese, W. B, Fowler, J. W, Hilton, G. C, Morgan, K. M, Pappas, C. G, Reintsema, C. N, Swetz, D. S, Ullom, J. N, Irwin, K. D, Akamatsu, H, Gottardi, L, den Hartog, R, Jackson, B. D, van der Kuur, J, Barret, D, and Peille, P
- Subjects
Astrophysics - Abstract
The focal plane of the X-ray integral field unit (X-IFU) for ESA's Athena X-ray observatory will consist of approximately 4000 transition edge sensor (TES) x-ray microcalorimeters optimized for the energy range of 0.2 to 12 kiloelectronvolts. The instrument will provide unprecedented spectral resolution of approximately 2.5 electronvolts at energies of up to 7 kiloelectronvolts and will accommodate photon fluxes of 1 milliCrab (90 counts per second) for point source observations. The baseline configuration is a uniform large pixel array (LPA) of 4.28 arcseconds pixels that is read out using frequency domain multiplexing (FDM). However, an alternative configuration under study incorporates an 18 by × 18 small pixel array (SPA) of 2 arcseconds pixels in the central approximately 36 arcseconds region. This hybrid array configuration could be designed to accommodate higher fluxes of up to 10 milliCrabs (900 counts per second) or alternately for improved spectral performance (less than 1.5 electronvolts) at low count-rates. In this paper we report on the TES pixel designs that are being optimized to meet these proposed LPA and SPA configurations. In particular we describe details of how important TES parameters are chosen to meet the specific mission criteria such as energy resolution, count-rate and quantum efficiency, and highlight performance trade-offs between designs. The basis of the pixel parameter selection is discussed in the context of existing TES arrays that are being developed for solar and x-ray astronomy applications. We describe the latest results on DC biased diagnostic arrays as well as large format kilo-pixel arrays and discuss the technical challenges associated with integrating different array types on to a single detector die.
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- 2016
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26. Advanced Code-Division Multiplexers for Superconducting Detector Arrays
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Irwin, K. D., Cho, H. M., Doriese, W. B., Fowler, J. W., Hilton, G. C., Niemack, M. D., Reintsema, C. D., Schmidt, D. R., Ullom, J. N., and Vale, L. R.
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- 2012
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27. Optimization and Analysis of Code-Division Multiplexed TES Microcalorimeters
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Fowler, J. W., Doriese, W. B., Hilton, G., Irwin, K., Schmidt, D., Stiehl, G., Swetz, D., Ullom, J. N., and Vale, L.
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- 2012
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28. Optimization of the TES-Bias Circuit for a Multiplexed Microcalorimeter Array
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Doriese, W. B., Alpert, B. K., Fowler, J. W., Hilton, G. C., Hojem, A. S., Irwin, K. D., Reintsema, C. D., Schmidt, D. R., Stiehl, G. M., Swetz, D. S., Ullom, J. N., and Vale, L. R.
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- 2012
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29. Predicted Energy Resolution of a Running-Sum Algorithm for Microcalorimeters
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Alpert, Bradley K., Doriese, W. Bertrand, Fowler, Joseph W., and Ullom, Joel N.
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- 2012
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30. Microcalorimeter arrays for ultra-high energy resolution X- and gamma-ray detection
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Hoover, A. S., Bacrania, M. K., Hoteling, N. J., Karpius, P. J., Rabin, M. W., Rudy, C. R., Vo, D. T., Beall, J. A., Bennett, D. A., Doriese, W. B., Hilton, G. C., Horansky, R. D., Irwin, K. D., Ullom, J. N., and Vale, L. R.
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- 2009
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31. Toward a 256-Pixel Array of Gamma-Ray Microcalorimeters for Nuclear-Materials Analysis
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Doriese, W. B., Ullom, J. N., Beall, J. A., Duncan, W. D., Ferreira, L., Hilton, G. C., Horansky, R. D., Irwin, K. D., Mates, J. A. B., Reintsema, C. D., Schmidt, D. R., Vale, L. R., Xu, Y., Zink, B. L., Bacrania, M. K., Hoover, A. S., Rudy, C. R., Rabin, M. W., Kilbourne, C. A., Boyce, K. R., Brown, L. E., King, J. M., and Porter, F. S.
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- 2008
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32. Micro-X: Mission Overview and Science Goals
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Figueroa-Feliciano, E., Bandler, S. R., Bautz, M., Brown, G., Deiker, S., Doriese, W. B., Flanagan, K., Galeazzi, M., Hilton, G. C., Hwang, U., Irwin, K. D., Kallman, T., Kelley, R. L., Kilbourne, C. A., Kissel, S., Levine, A., Loewenstein, M., Martinez-Galarce, D., McCammon, D., Mushotzky, R., Petre, R., Porter, F. S., Reistema, C. D., Saab, T., Serlemitsos, P., Schulz, N., Smith, R., and Ullom, J. N.
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- 2008
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33. A TDMA Hybrid SQUID Multiplexer
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Reintsema, C. D., Beall, J., Doriese, W., Duncan, W., Ferreira, L., Hilton, G. C., Irwin, K. D., Schmidt, D., Ullom, J., Vale, L., and Xu, Y.
- Published
- 2008
- Full Text
- View/download PDF
34. The EBIT Calorimeter Spectrometer: A New, Permanent User Facility at the LLNL EBIT
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Porter, F. S., Beiersdorfer, P., Brown, G. V., Doriese, W., Gygax, J., Kelley, R. L., Kilbourne, C. A., King, J., Irwin, K., Reintsema, C., and Ullom, J.
- Published
- 2008
- Full Text
- View/download PDF
35. A Kilopixel Array of TES Bolometers for ACT: Development, Testing, and First Light
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Niemack, M. D., Zhao, Y., Wollack, E., Thornton, R., Switzer, E. R., Swetz, D. S., Staggs, S. T., Page, L., Stryzak, O., Moseley, H., Marriage, T. A., Limon, M., Lau, J. M., Klein, J., Kaul, M., Jarosik, N., Irwin, K. D., Hincks, A. D., Hilton, G. C., Halpern, M., Fowler, J. W., Fisher, R. P., Dünner, R., Doriese, W. B., Dicker, S. R., Devlin, M. J., Chervenak, J., Burger, B., Battistelli, E. S., Appel, J., Amiri, M., Allen, C., and Aboobaker, A. M.
- Published
- 2008
- Full Text
- View/download PDF
36. The Atacama Cosmology Telescope: Cosmological Parameters from Three Seasons of Data
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Seivers, Jonathan L, Hlozek, Renee A, Nolta, Michael R, Acquaviva, Viviana, Addison, Graeme E, Ade, Peter A. R, Aguirre, Paula, Amiri, Mandana, Appel, John W, Barrientos, L. Felipe, Battistelli, Elia S, Battaglia, Nick, Bond, J. Richard, Brown, Ben, Burger, Bryce, Calabrese, Erminia, Chervenak, Jay, Crichton, Devin, Das, Sudeep, Devlin, Mark J, Doriese, W. Bertrand, Dunkley, Joanna, Moseley, Harvey, and Wollack, Ed
- Subjects
Space Radiation ,Physics Of Elementary Particles And Fields ,Astrophysics - Abstract
We present constraints on cosmological and astrophysical parameters from highresolution microwave background maps at 148 GHz and 218 GHz made by the Atacama Cosmology Telescope (ACT) in three seasons of observations from 2008 to 2010. A model of primary cosmological and secondary foreground parameters is fit to the map power spectra and lensing deflection power spectrum, including contributions from both the thermal Sunyaev-Zeldovich (tSZ) effect and the kinematic Sunyaev-Zeldovich (kSZ) effect, Poisson and correlated anisotropy from unresolved infrared sources, radio sources, and the correlation between the tSZ effect and infrared sources. The power l(sup 2)C(sub l)/2pi of the thermal SZ power spectrum at 148 GHz is measured to be 3.4 +/- 1.4 micro-K(sup 2) at l = 3000, while the corresponding amplitude of the kinematic SZ power spectrum has a 95% confidence level upper limit of 8.6 micro-K(sup 2). Combining ACT power spectra with the WMAP 7-year temperature and polarization power spectra, we find excellent consistency with the LCDM model. We constrain the number of effective relativistic degrees of freedom in the early universe to be N(sub eff) = 2.79 +/- 0.56, in agreement with the canonical value of N(sub eff) = 3.046 for three massless neutrinos. We constrain the sum of the neutrino masses to be sigma(mν) is less than 0.39 eV at 95% confidence when combining ACT and WMAP 7-year data with BAO and Hubble constant measurements. We constrain the amount of primordial helium to be Y(sub p) = 0.225 +/- 0.034, and measure no variation in the fine structure constant alpha since recombination, with alpha/alpha(sub 0) = 1.004 +/- 0.005. We also find no evidence for any running of the scalar spectral index, derivative(n(sub s))/derivative(ln k) = −0.004 +/- 0.012.
- Published
- 2013
- Full Text
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37. The Atacama Cosmology Telescope: Data Characterization and Map Making
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Duenner, Rolando, Hasselfield, Matthew, Marriage, Tobias A, Sievers, Jon, Acquaviva, Viviana, Addison, Graeme E, Ade, Peter A. R, Aguirre, Paula, Amiri, Mandana, Appel, John William, Barrientos, L. Felipe, Battistelli, Elia S, Bond, J. Richard, Brown, Ben, Burger, Bryce, Chervenak, Jay, Calabrese, Erminia, Das, Sudeep, Devlin, Mark J, Dicker, Simon R, Doriese, W. Bertrand, Dunkley, Joanna, Essinger-Hileman, Thomas, Moseley, Harvey, and Wollack, Ed
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Astronomy - Abstract
We present a description of the data reduction and mapmaking pipeline used for the 2008 observing season of the Atacama Cosmology Telescope (ACT). The data presented here at 148 GHz represent 12% or the 90 TB collected by ACT from 2007 to 2010. In 2008 we observed for 136 days, producing a total of 142h of data (11 TB for the 148 GHz band only), with a daily average of 10.5 h of observation. From these, 108.5 h were devoted to 850 sq deg stripe (11.2 h by 9 deg.1) centered on a declination of -52 deg.7, while 175 h were devoted to a 280 square deg stripe (4.5 h by 4 deg.8) centered at the celestial equator. We discuss sources of statistical and systematic noise, calibration, telescope pointing and data selection. Out of 1260 survey hours and 1024 detectors per array, 816 h and 593 effective detectors remain after data selection for this frequency band, yielding a 38 % survey efficiency. The total sensitivity in 2008, determined from the noise level between 5 Hz and 20 Hz in the time-ordered data stream (TOD), is 32 muK square root of s in CMB units. Atmospheric brightness fluctuations constitute the main contaminant in the data and dominate the detector and noise covariance at low frequencies in the TOD. The maps were made by solving the lease squares problem using the Preconditioned Conjugate Gradient method, incorporating the details of the detector and noise correlations. Cross-correlation with WMAP sky maps as well as analysis from simulations reveal the our maps are unbiased at l > 300. This paper accompanies the public release of the 148 GHz southern stripe maps from 2008. The techniques described here will be applied to future maps and data releases.
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- 2012
- Full Text
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38. Development of Kilo-Pixel Arrays of Transition-Edge Sensors for X-Ray Spectroscopy
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Adams, J. S, Bandler, S. R, Busch, S. E, Chervenak, J. A, Chiao, M. P, Eckart, M. E, Ewin, A. J, Finkbeiner, F. M, Kelley, R. L, Kelly, D. P, Kilbourne, C. A, Leutenegger, M. A, Porst, J.-P, Porter, F. S, Ray, C. A, Sadleir, J. E, Smith, S. J, Wassell, E. J, Doriese, W. B, Fowler, J. W, Hilton, G. C, Irwin, K. D, Reintsema, C. D, Smith, D. R, and Swetz, D. S
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Astronomy - Abstract
We are developing kilo-pixel arrays of transition-edge sensor (TES) microcalorimeters for future X-ray astronomy observatories or for use in laboratory astrophysics applications. For example, Athena/XMS (currently under study by the european space agency) would require a close-packed 32x32 pixel array on a 250-micron pitch with < 3.0 eV full-width-half-maximum energy resolution at 6 keV and at count-rates of up to 50 counts/pixel/second. We present characterization of 32x32 arrays. These detectors will be readout using state of the art SQUID based time-domain multiplexing (TDM). We will also present the latest results in integrating these detectors and the TDM readout technology into a 16 row x N column field-able instrument.
- Published
- 2012
39. Enabling Technologies for the High-Resolution Imaging Spectrometer of the Next NASA X-Ray Astronomy Mission - Options, Status, and Roadmap
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Kilbourne, Caroline, Bander, S, Chervenak, J, Doriese, W. B, Hilton, G, Irwin, K, Kelley, R, Porter, F. S, Reintsema, C, and Ulom, J
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Astronomy - Published
- 2011
40. The Atacama Cosmology Telescope: Calibration with the Wilkinson Microwave Anisotropy Probe Using Cross-Correlations
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Hajian, Amir, Acquaviva, Viviana, Ade, Peter A. R, Aguirre, Paula, Amiri, Mandana, Appel, John William, Barrientos, L. Felipe, Battistelli, Elia S, Bond, John R, Brown, Ben, Burger, Bryce, Chervenak, Jay, Das, Sudeep, Devlin, Mark J, Dicker, Simon R, Bertrand Doriese, W, Dunkley, Joanna, Dunner, Rolando, Essinger-Hileman, Thomas, Fisher, Ryan P, Fowler, Joseph W, Halpern, Mark, Hasselfield, Matthew, Moseley, Harvey, and Wollack, Ed
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Astronomy - Abstract
We present a new calibration method based on cross-correlations with the Wilkinson Microwave Anisotropy Probe (WMAP) and apply it to data from the Atacama Cosmology Telescope (ACT). ACT's observing strategy and mapmaking procedure allows an unbiased reconstruction of the modes in the maps over a wide range of multipoles. By directly matching the ACT maps to WMAP observations in the multipole range of 400 < I < 1000, we determine the absolute calibration with an uncertainty of 2% in temperature. The precise measurement of the calibration error directly impacts the uncertainties in the cosmological parameters estimated from the ACT power spectra. We also present a combined map based on ACT and WMAP data that has a high signal-to-noise ratio over a wide range of multipoles.
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- 2011
- Full Text
- View/download PDF
41. The Atacama Cosmology Telescope: Cosmological Parameters from the 2008 Power Spectrum
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Dunkley, J, Hlozek, R, Sievers, J, Acquaviva, V, Ade, P. A. R, Aguirre, P, Amiri, M, Appel, J. W, Barrientos, L. F, Battistelli, E. S, Bond, J. R, Brown, B, Burger, B, Chervenak, J, Das, S, Devlin, M. J, Dicker, S. R, Bertrand Doriese, W, Dunner, R, Essinger-Hileman, T, Fisher, R. P, Fowler, J. W, Hajian, A, Moseley, H, and Wollack, E
- Subjects
Astrophysics - Abstract
We present cosmological parameters derived from the angular power spectrum of the cosmic microwave background (CMB) radiation observed at 148 GHz and 218 GHz over 296 deg(exp 2) with the Atacama Cosmology Telescope (ACT) during its 2008 season. ACT measures fluctuations at scales 500 < l < 10,000. We fit a model for the lensed CMB, Sunyaev-Zel'dovich (SZ), and foreground contribution to the 148 GHz and 218 GHz power spectra, including thermal and kinetic SZ, Poisson power from radio and infrared point sources, and clustered power from infrared point sources. At l = 3000, about half the power at 148 GHz comes from primary CMB after masking bright radio sources. The power from thermal and kinetic SZ is estimated to be Beta(sub 3000) is identical to 6.8 +/- 2.9 mu K (exp 2), where Beta (sub l) is identical to l(l + 1) C(sub l)/2pi. The IR Poisson power at 148 GHz is Bewta(sub 3000) 7.8 +/- 0.7 muK(exp 2) (C(sub l) = 5.5 +/- 0.5 nK(exp 2)), and a clustered IR component is required with Beta (sub 3000) = 4.6 +/- 0.9 muK(exp 2), assuming an analytic model for its power spectrum shape. At 218 GHz only about 15% of the power, approximately 27 mu K(exp 2), is CMB anisotropy at l = 3000. The remaining 85% is attributed to IR sources (approximately 50% Poisson and 35% clustered), with spectral index alpha = 3.69 +/- 0.14 for flux scaling as S(nu) varies as nu(sup alpha). We estimate primary cosmological parameters from the less contaminated 148 GHz spectrum, marginalizing over SZ and source power. The ACDM cosmological model is a good fit to the data (chi square/dof = 29/46), and ACDM parameters estimated from ACT+Wilkinson Microwave Anisotropy Probe (WMAP) are consistent with the seven-year WMAP limits, with scale invariant n(sub s) = 1 excluded at 99.7% confidence level (CL) (3 sigma). A model with no CMB lensing is disfavored at 2.8 sigma. By measuring the third to seventh acoustic peaks, and probing the Silk damping regime, the ACT data improve limits on cosmological parameters that affect the small-scale CMB power. The ACT data combined with WMAP give a 6 sigma detection of primordial helium, with Y(sub p) = 0.313 +/- 0.044, and a 4 sigma detection of relativistic species, assumed to be neutrinos, with N(sub eff) = 5.3 +/- 1.3 (4.6 +/- 0.8 with BAO+H(sub 0) data). From the CMB alone the running of the spectral index is constrained to be d(sub s) / d ln k = -0,034 +/- 0,018, the limit on the tensor-to-scalar ratio is r < 0,25 (95% CL), and the possible contribution of Nambu cosmic strings to the power spectrum is constrained to string tension G(sub mu) < 1.6 x 10(exp -7) (95% CL)
- Published
- 2011
- Full Text
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42. The Atacama Cosmology Telescope: Sunyaev-Zel'dovich-Selected Galaxy Clusters AT 148 GHz in the 2008 Survey
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Marriage, Tobias A, Acquaviva, Viviana, Ade, Peter A. R, Aguirre, Paula, Amiri, Mandana, Appel, John William, Barrientos, L. Felipe, Battistelli, Elia S, Bond, J. Richard, Brown, Ben, Burger, Bryce, Chervenak, Jay, Das, Sudeep, Devlin, Mark J, Dicker, Simon R, Doriese, W. Bertrand, Dunkley, Joanna, Dunner, Rolando, Essinger-Hileman, Thomas, Fisher, Ryan P, Fowler, Joseph W, Hajian, Amir, Halpern, Mark, Moseley, Harvey, and Wollack, Ed
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Astronomy - Abstract
We report on 23 clusters detected blindly as Sunyaev-Zel'dovich (SZ) decrements in a 148 GHz, 455 deg (exp 2) map of the southern sky made with data from the Atacama Cosmology Telescope 2008 observing season. All SZ detections announced in this work have confirmed optical counterparts. Ten of the clusters are new discoveries. One newly discovered cluster, ACT-CL 10102-4915, with a redshift of 0.75 (photometric), has an SZ decrement comparable to the most massive systems at lower redshifts. Simulations of the cluster recovery method reproduce the sample purity measured by optical follow-up. In particular, for clusters detected with a signal-to-noise ratio greater than six, simulations are consistent with optical follow-up that demonstrated this subsample is 100% pure, The simulations further imply that the total sample is 80% complete for clusters with mass in excess of 6 x 10(exp 14) solar masses referenced to the cluster volume characterized by 500 times the critical density. The Compton gamma-X-ray luminosity mass comparison for the 11 best-detected clusters visually agrees with both self-similar and non-adiabatic, simulation-derived scaling laws
- Published
- 2011
- Full Text
- View/download PDF
43. Development of a Real-Time Pulse Processing Algorithm for TES-Based X-Ray Microcalorimeters
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Tan, Hui, Hennig, Wolfgang, Warburton, William K, Doriese, W. Bertrand, and Kilbourne, Caroline A
- Subjects
Electronics And Electrical Engineering - Abstract
We report here a real-time pulse processing algorithm for superconducting transition-edge sensor (TES) based x-ray microcalorimeters. TES-based. microca1orimeters offer ultra-high energy resolutions, but the small volume of each pixel requires that large arrays of identical microcalorimeter pixe1s be built to achieve sufficient detection efficiency. That in turn requires as much pulse processing as possible must be performed at the front end of readout electronics to avoid transferring large amounts of data to a host computer for post-processing. Therefore, a real-time pulse processing algorithm that not only can be implemented in the readout electronics but also achieve satisfactory energy resolutions is desired. We have developed an algorithm that can be easily implemented. in hardware. We then tested the algorithm offline using several data sets acquired with an 8 x 8 Goddard TES x-ray calorimeter array and 2x16 NIST time-division SQUID multiplexer. We obtained an average energy resolution of close to 3.0 eV at 6 keV for the multiplexed pixels while preserving over 99% of the events in the data sets.
- Published
- 2011
- Full Text
- View/download PDF
44. The Atacama Cosmology Telescope: Extragalactic Sources at 148 GHz in the 2008 Survey
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Marriage, T. A, Juin, J. B, Lin, Y. T, Marsden, D, Nolta, M. R, Partridge, B, Ade, P. A. R, Aguirre, P, Amiri, M, Appel, J. W, Barrientos, L. F, Battistelli, E. S, Bond, J. R, Brown, B, Burger, B, Chervenak, J, Das, S, Devlin, M. J, Dicker, S. R, Doriese, W. B, Dunkley, J, Dunner, R, Essinger-Hileman, T, Fisher, R. P, and Fowler, J. W
- Subjects
Astronomy - Abstract
We report on extragalactic sources detected in a 455 square-degree map of the southern sky made with data at a frequency of 148 GHz from the Atacama Cosmology Telescope 2008 observing season. We provide a catalog of 157 sources with flux densities spanning two orders of magnitude: from 15 mJy to 1500 mJy. Comparison to other catalogs shows that 98% of the ACT detections correspond to sources detected at lower radio frequencies. Three of the sources appear to be associated with the brightest cluster galaxies of low redshift X-ray selected galaxy clusters. Estimates of the radio to mm-wave spectral indices and differential counts of the sources further bolster the hypothesis that they are nearly all radio sources, and that their emission is not dominated by re-emission from warm dust. In a bright (> 50 mJy) 148 GHz-selected sample with complete cross-identifications from the Australia Telescope 20 GHz survey, we observe an average steepening of the spectra between .5, 20, and 148 GHz with median spectral indices of alp[ha (sub 5-20) = -0.07 +/- 0.06, alpha (sub 20-148) -0.39 +/- 0.04, and alpha (sub 5-148) = -0.20 +/- 0.03. When the measured spectral indices are taken into account, the 148 GHz differential source counts are consistent with previous measurements at 30 GHz in the context of a source count model dominated by radio sources. Extrapolating with an appropriately rescaled model for the radio source counts, the Poisson contribution to the spatial power spectrum from synchrotron-dominated sources with flux density less than 20 mJy is C(sup Sync) = (2.8 +/- 0.3) x 1O (exp-6) micro K(exp 2).
- Published
- 2011
45. The Atacama Cosmology Telescope (ACT): Beam Profiles and First SZ Cluster Maps
- Author
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Hincks, A. D, Acquaviva, V, Ade, P. A, Aguirre, P, Amiri, M, Appel, J. W, Barrientos, L. F, Battistelli, E. S, Bond, J. R, Brown, B, Burger, B, Chervenak, J, Das, S, Devlin, M. J, Dicker, S. R, Doriese, W. B, Dunkley, J, Duenner, R, Essinger-Hileman, T, Fisher, R. P, Fowler, J. W, Hajian, A, Halpern, M, Hasselfield, M, and Wollack, Ed
- Subjects
Astronomy - Abstract
The Atacama Cosmology Telescope (ACT) is currently observing the cosmic microwave background with arcminute resolution at 148 GHz, 218 GHz, and 277 GHz, In this paper, we present ACT's first results. Data have been analyzed using a maximum-likelihood map-making method which uses B-splines to model and remove the atmospheric signal. It has been used to make high-precision beam maps from which we determine the experiment's window functions, This beam information directly impacts all subsequent analyses of the data. We also used the method to map a sample of galaxy clusters via the Sunyaev-Ze1'dovich (SZ) effect, and show five clusters previously detected with X-ray or SZ observations, We provide integrated Compton-y measurements for each cluster. Of particular interest is our detection of the z = 0.44 component of A3128 and our current non-detection of the low-redshift part, providing strong evidence that the further cluster is more massive as suggested by X-ray measurements. This is a compelling example of the redshift-independent mass selection of the SZ effect.
- Published
- 2010
46. The Atacama Cosmology Telescope: Cosmology from Galaxy Clusters Detected Via the Sunyaev-Zel'dovich Effect
- Author
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Sehgal, Neelima, Trac, Hy, Acquaviva, Viviana, Ade, Peter A. R, Aguirre, Paula, Amiri, Mandana, Appel, John W, Barrientos, L. Felipe, Battistelli, Elia S, Bond, J. Richard, Brown, Ben, Burger, Bryce, Chervenak, Jay, Das, Sudeep, Devlin, Mark J, Dicker, Simon R, Doriese, W. Bertrand, Dunkley, Joanna, Duenner, Rolando, Essinger-Hileman, Thomas, Fisher, Ryan P, Fowler, Joseph W, Hajian, Amir, Halpern, Mark, and Wollack, Ed
- Subjects
Astrophysics - Abstract
We present constraints on cosmological parameters based on a sample of Sunyaev-Zel'dovich-selected galaxy clusters detected in a millimeter-wave survey by the Atacama Cosmology Telescope. The cluster sample used in this analysis consists of 9 optically-confirmed high-mass clusters comprising the high-significance end of the total cluster sample identified in 455 square degrees of sky surveyed during 2008 at 148 GHz. We focus on the most massive systems to reduce the degeneracy between unknown cluster astrophysics and cosmology derived from SZ surveys. We describe the scaling relation between cluster mass and SZ signal with a 4-parameter fit. Marginalizing over the values of the parameters in this fit with conservative priors gives (sigma)8 = 0.851 +/- 0.115 and w = -1.14 +/- 0.35 for a spatially-flat wCDM cosmological model with WMAP 7-year priors on cosmological parameters. This gives a modest improvement in statistical uncertainty over WMAP 7-year constraints alone. Fixing the scaling relation between cluster mass and SZ signal to a fiducial relation obtained from numerical simulations and calibrated by X-ray observations, we find (sigma)8 + 0.821 +/- 0.044 and w = -1.05 +/- 0.20. These results are consistent with constraints from WMAP 7 plus baryon acoustic oscillations plus type Ia supernova which give (sigma)8 = 0.802 +/- 0.038 and w = -0.98 +/- 0.053. A stacking analysis of the clusters in this sample compared to clusters simulated assuming the fiducial model also shows good agreement. These results suggest that, given the sample of clusters used here, both the astrophysics of massive clusters and the cosmological parameters derived from them are broadly consistent with current models.
- Published
- 2010
47. The Atacama Cosmology Telescope: A Measurement of the Cosmic Microwave Background Power Spectrum at 148 AND 218 GHz from the 2008 Southern Survey
- Author
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Das, Sudeep, Marriage, Tobias A, Ade, Peter A. R, Aguirre, Paula, Amiri, Mandana, Appel, John W, Barrientos, L. Felipe, Battistelli, Elia A, Bond, J. Richard, Brown, Ben, Burger, Bryce, Chervenak, Jay, Devlin, Mark J, Dicker, Simon R, Doriese, W. Bertrand, Dunkley, Joanna, Duenner, Rolando, Essinger-Hileman, Thomas, Fisher, Ryan P, Fowler, Joseph W, Hajian, Amir, Halpern, Mark, Hasselfield, Matthew, Hernandez-Monteagudo, Carlos, and Wollack, Ed
- Subjects
Optics - Abstract
We present measurements of the cosmic microwave background (CMB) power spectrum made by the Atacama Cosmology Telescope at 148 GHz and 218 GHz, as well as the cross-frequency spectrum between the two channels. Our results dearly show the second through the seventh acoustic peaks in the CMB power spectrum. The measurements of these higher-order peaks provide an additional test of the ACDM cosmological model. At l > 3000, we detect power in excess of the primary anisotropy spectrum of the CMB. At lower multipoles 500 < l < 3000, we find evidence for gravitational lensing of the CMB in the power spectrum at the 2.8(sigma) level. We also detect a low level of Galactic dust in our maps, which demonstrates that we can recover known faint, diffuse signals.
- Published
- 2010
48. The Atacama Cosmology Telescope: A Measurement of the 600 less than l less than 8000 Cosmic Microwave Background Power Spectrum at 148 GHz
- Author
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Fowler, J. W, Acquaviva, V, Ade, P. A. R, Aguirre, P, Amiri, M, Appel, J. W, Barrientos, L. F, Bassistelli, E. S, Bond, J. R, Brown, B, Burger, B, Chervenak, J, Das, S, Devlin, M. J, Dicker, S. R, Doriese, W. B, Dunkley, J, Duenner, R, Essinger-Hileman, T, Fisher, R. P, Hajian, A, Halpern, M, Hasselfield, M, Moseley, H, and Wollack, Ed
- Subjects
Astrophysics - Abstract
We present a measurement of the angular power spectrum of the cosmic microwave background (CMB) radiation observed at 148 GHz. The measurement uses maps with 1.4' angular resolution made with data from the Atacama Cosmology Telescope (ACT). The observations cover 228 deg(sup 2) of the southern sky, in a 4 deg. 2-wide strip centered on declination 53 deg. South. The CMB at arc minute angular scales is particularly sensitive to the Silk damping scale, to the Sunyaev-Zel'dovich (SZ) effect from galaxy dusters, and to emission by radio sources and dusty galaxies. After masking the 108 brightest point sources in our maps, we estimate the power spectrum between 600 less than l less than 8000 using the adaptive multi-taper method to minimize spectral leakage and maximize use of the full data set. Our absolute calibration is based on observations of Uranus. To verify the calibration and test the fidelity of our map at large angular scales, we cross-correlate the ACT map to the WMAP map and recover the WMAP power spectrum from 250 less than l less than 1150. The power beyond the Silk damping tail of the CMB (l approximately 5000) is consistent with models of the emission from point sources. We quantify the contribution of SZ clusters to the power spectrum by fitting to a model normalized to sigma 8 = 0.8. We constrain the model's amplitude A(sub sz) less than 1.63 (95% CL). If interpreted as a measurement of as, this implies sigma (sup SZ) (sub 8) less than 0.86 (95% CL) given our SZ model. A fit of ACT and WMAP five-year data jointly to a 6-parameter ACDM model plus point sources and the SZ effect is consistent with these results.
- Published
- 2010
49. The Atacama Cosmology Telescope: The Receiver and Instrumentation
- Author
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Swetz, D. S, Ade, P. A. R, Amiri, M, Appel, J. W, Burger, B, Devlin, M. J, Dicker, S. R, Doriese, W. B, Essinger-Hileman, T, Fisher, R. P, Fowler, J. W, Halpern, M, Hasselfield, M, Hilton, G. C, Hincks, A. D, Irwin, K. D, Jarosik, N, Kaul, M, Klein, J, Marsden, D, Thornton, R, Mauskopf, P, Niemack, M. D, Page, L. A, and Parker, L
- Subjects
Astronomy - Abstract
The Atacama Cosmology Telescope was designed to measure small-scale anisotropies in the Cosmic Microwave Background and detect galaxy clusters through the Sunyaev-Zel'dovich effect. The instrument is located on Cerro Taco in the Atacama Desert, at an altitude of 5190 meters. A six-met.er off-axis Gregorian telescope feeds a new type of cryogenic receiver, the Millimeter Bolometer Array Camera. The receiver features three WOO-element arrays of transition-edge sensor bolometers for observations at 148 GHz, 218 GHz, and 277 GHz. Each detector array is fed by free space mm-wave optics. Each frequency band has a field of view of approximately 22' x 26'. The telescope was commissioned in 2007 and has completed its third year of operations. We discuss the major components of the telescope, camera, and related systems, and summarize the instrument performance.
- Published
- 2010
50. Resonant soft x-ray scattering from stripe-ordered La$_{2-x}$Ba$_x$CuO$_4$ detected by a transition edge sensor array detector
- Author
-
Joe, Y. I., Fang, Y., Lee, S., Sun, S. X. L., de la Pe��a, G. A., Doriese, W. B., Morgan, K. M., Fowler, J. W., Vale, L. R., Rodolakis, F., McChesney, J. L., Ullom, J. N., Swetz, D. S., and Abbamonte, P.
- Subjects
Condensed Matter - Strongly Correlated Electrons ,Quantum Physics ,Physics - Instrumentation and Detectors ,Strongly Correlated Electrons (cond-mat.str-el) ,FOS: Physical sciences ,Instrumentation and Detectors (physics.ins-det) ,Quantum Physics (quant-ph) - Abstract
Resonant soft x-ray scattering (RSXS) is a leading probe of valence band order in materials best known for detecting charge density wave order in the copper-oxide superconductors. One of the biggest limitations on the RSXS technique is the presence of a severe fluorescence background which, like the RSXS cross section itself, is enhanced under resonant conditions. This background prevents the study of weak signals such as diffuse scattering from glassy or fluctuating order that is spread widely over momentum space. Recent advances in superconducting transition edge sensor (TES) detectors have led to major improvements in energy resolution and detection efficiency in the soft x-ray range. Here, we perform a RSXS study of stripe-ordered La$_{2-x}$Ba$_x$CuO$_4$ at the Cu $L_{3/2}$ edge (932.2 eV) using a TES detector with 1.5 eV resolution, to evaluate its utility for mitigating the fluorescence background problem. We find that, for suitable degree of detuning from the resonance, the TES rejects the fluorescence background, leading to a 5 to 10 times improvement in the statistical quality of the data compared to an equivalent, energy-integrated measurement. We conclude that a TES presents a promising approach to reducing background in RSXS studies and may lead to new discoveries in materials exhibiting valence band order that is fluctuating or glassy., 10 pages, 6 figures
- Published
- 2019
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