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243 results on '"Eckart, Megan E."'

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

Author

den Herder, Jan-Willem A., Takahashi, Tadayuki, Bautz, Marshall, Ishisaki, Yoshitaka, Yamada, Shinya, Seta, Hiromi, Tashiro, Makoto S., Takeda, Sawako, Terada, Yukikatsu, Kato, Yuka, Tsujimoto, Masahiro, Koyama, Shu, MItsuda, Kazuhisa, Sawada, Makoto, Boyce, Kevin R., Chiao, Meng P., Watanabe, Tomomi, Leutenegger, Maurice A., Eckart, Megan E., Porter, F. Scott, Kilbourne, Caroline A., and Kelley, Richard L.

Published
2016
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202. In-flight verification of the calibration and performance of the ASTRO-H (Hitomi) Soft X-Ray Spectrometer

Author

den Herder, Jan-Willem A., Takahashi, Tadayuki, Bautz, Marshall, Leutenegger, Maurice A., Audard, Marc, Boyce, Kevin R., Brown, Gregory V., Chiao, Meng P., Eckart, Megan E., Fujimoto, Ryuichi, Furuzawa, Akihiro, Guainazzi, Matteo, Haas, Daniel, den Herder, Jan-Willem, Hayashi, Takayuki, Iizuka, Ryo, Ishida, Manabu, Ishisaki, Yoshitaka, Kelley, Richard L., Kikuchi, Naomichi, Kilbourne, Caroline A., Koyama, Shu, Kurashima, Sho, Maeda, Yoshitomo, Markevitch, Maxim, McCammon, Dan, Mitsuda, Kazuhisa, Mori, Hideyuki, Nakaniwa, Nozomi, Okajima, Takashi, Paltani, Stéphane, Petre, Robert, Porter, F. Scott, Sato, Kosuke, Sato, Toshiki, Sawada, Makoto, Serlemitsos, Peter J., Seta, Hiromi, Sneiderman, Gary, Soong, Yang, Sugita, Satoshi, Szymkowiak, Andrew E., Takei, Yoh, Tashiro, Makoto, Tawara, Yuzuru, Tsujimoto, Masahiro, de Vries, Cor P., Watanabe, Tomomi, Yamada, Shinya, and Yamasaki, Noriko

Published
2016
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203. Performance of the helium dewar and cryocoolers of ASTRO-H SXS

Author

den Herder, Jan-Willem A., Takahashi, Tadayuki, Bautz, Marshall, Fujimoto, Ryuichi, Takei, Yoh, Mitsuda, Kazuhisa, Yamasaki, Noriko Y., Tsujimoto, Masahiro, Koyama, Shu, Ishikawa, Kumi, Sugita, Hiroyuki, Sato, Yoichi, Shinozaki, Keisuke, Okamoto, Atsushi, Kitamoto, Shunji, Hoshino, Akio, Sato, Kosuke, Ezoe, Yuichiro, Ishisaki, Yoshitaka, Yamada, Shinya, Seta, Hiromi, Ohashi, Takaya, Tamagawa, Toru, Noda, Hirofumi, Sawada, Makoto, Tashiro, Makoto, Yatsu, Yoichi, Mitsuishi, Ikuyuki, Kanao, Kenichi, Yoshida, Seiji, Miyaoka, Mikio, Tsunematsu, Shoji, Otsuka, Kiyomi, Narasaki, Katsuhiro, DiPirro, Michael J., Shirron, Peter J., Sneiderman, Gary A., Kilbourne, Caroline A., Porter, F. Scott, Chiao, Meng P., Eckart, Megan E., and Kelley, Richard L.

Published
2016
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204. The design, implementation, and performance of the Astro-H SXS aperture assembly and blocking filters

Author

den Herder, Jan-Willem A., Takahashi, Tadayuki, Bautz, Marshall, Kilbourne, Caroline A., Adams, Joseph S., Arsenovic, Petar, Ayers, Travis, Chiao, Meng P., Dipirro, Michael J., Eckart, Megan E., Fujimoto, Ryuichi, Kazeva, John D., Kelley, Richard L., Kripps, Kari L., Lairson, Bruce, Leutenegger, Maurice A., Lopez, Heidi, McCammon, Dan, McGuinness, Daniel S., Mitsuda, Kazuhisa, Moseley, Samuel J., Porter, F. S., Schweiss, Andrea N., Takei, Yoh, Thorpe, Rosemary S., Watanabe, Tomomi, Yamasaki, Noriko Y., and Yoshida, Seiji

Published
2016
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205. Cryogen-free operation of the Soft X-ray Spectrometer instrument

Author

den Herder, Jan-Willem A., Takahashi, Tadayuki, Bautz, Marshall, Sneiderman, Gary A., Shirron, Peter J., Fujimoto, Ryuichi, Bialas, Thomas G., Boyce, Kevin R., Chiao, Meng P., DiPirro, Michael J., Eckart, Megan E., Hartz, Leslie, Ishisaki, Yoshitaka, Kelley, Richard L., Kilbourne, Caroline A., Masters, Candace, McCammon, Dan, Mitsuda, Kazuhisa, Noda, Hirofumi, Porter, Frederick S., Szymkowiak, Andrew E., Takei, Yoh, Tsujimoto, Masahiro, and Yoshida, Seiji

Published
2016
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206. The design, implementation, and performance of the Atro-H SXS calorimeter array and anti-coincidence detector

Author

den Herder, Jan-Willem A., Takahashi, Tadayuki, Bautz, Marshall, Kilbourne, Caroline A., Adams, Joseph S., Brekosky, Regis P., Chervenak, James A., Chiao, Meng P., Eckart, Megan E., Figueroa-Feliciano, Enectali, Galeazzi, Massimiliano, Grein, Christoph, Jhabvala, Christine A., Kelley, Richard L., Kelly, Daniel P., Leutenegger, Maurice A., McCammon, Dan, Porter, F. S., Szymkowiak, Andrew E., Watanabe, Tomomi, and Zhao, Jun

Published
2016
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207. Vibration isolation system for cryocoolers of Soft X-ray Spectrometer (SXS) onboard ASTRO-H (Hitomi)

Author

den Herder, Jan-Willem A., Takahashi, Tadayuki, Bautz, Marshall, Takei, Yoh, Yasuda, Susumu, Ishimura, Kosei, Iwata, Naoko, Okamoto, Atsushi, Sato, Yoichi, Ogawa, Mina, Sawada, Makoto, Kawano, Taro, Obara, Shingo, Natsukari, Chikara, Wada, Atsushi, Yamada, Shinya, Fujimoto, Ryuichi, Kokubun, Motohide, Yamasaki, Noriko Y., Sugita, Hiroyuki, Minesugi, Kenji, Nakamura, Yasuo, Mitsuda, Kazuhisa, Takahashi, Tadayuki, Yoshida, Seiji, Tsunematsu, Shoji, Kanao, Kenichi, Narasaki, Katsuhiro, Otsuka, Kiyomi, Kelley, Richard L., Porter, F. S., Kilbourne, Caroline A., Chiao, Meng P., Eckart, Megan E., Sneiderman, Gary A., Pontius, James T., McCammon, Dan, Wilke, Paul, and Basile, John

Published
2016
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208. In-flight performance of the Soft X-ray Spectrometer detector system on Astro-H

Author

den Herder, Jan-Willem A., Takahashi, Tadayuki, Bautz, Marshall, Porter, Frederick S., Boyce, Kevin R., Chiao, Meng P., Eckart, Megan E., Fujimoto, Ryuichi, Ishisaki, Yoshitaka, Kelley, Richard L., Kilbourne, Caroline A., Leutenegger, Maurice A., McCammon, Dan, Mitsuda, Kazuhisa, Sato, Kosuke, Seta, Hiromi, Sawada, Makoto, Sneiderman, Gary A., Szymkowiak, Andrew E., Takei, Yoh, Tashiro, Makoto S., Tsujimoto, Masahiro, Watanabe, Tomomi, and Yamada, Shinya

Published
2016
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209. The Astro-H high resolution soft x-ray spectrometer

Author

den Herder, Jan-Willem A., Takahashi, Tadayuki, Bautz, Marshall, Kelley, Richard L., Akamatsu, Hiroki, Azzarello, Phillipp, Bialas, Tom, Boyce, Kevin R., Brown, Gregory V., Canavan, Edgar, Chiao, Meng P., Costantini, Elisa, DiPirro, Michael J., Eckart, Megan E., Ezoe, Yuichiro, Fujimoto, Ryuichi, Haas, Daniel, den Herder, Jan-Willem, Hoshino, Akio, Ishikawa, Kumi, Ishisaki, Yoshitaka, Iyomoto, Naoko, Kilbourne, Caroline A., Kimball, Mark O., Kitamoto, Shunji, Konami, Saori, Koyama, Shu, Leutenegger, Maurice A., McCammon, Dan, Mitsuda, Kazuhisa, Mitsuishi, Ikuyuki, Moseley, Harvey, Murakami, Hiroshi, Murakami, Masahide, Noda, Hirofumi, Ogawa, Mina, Ohashi, Takaya, Okamoto, Atsushi, Ota, Naomi, Paltani, Stéphane, Porter, F. S., Sakai, Kazuhiro, Sato, Kosuke, Sato, Yohichi, Sawada, Makoto, Seta, Hiromi, Shinozaki, Keisuke, Shirron, Peter J., Sneiderman, Gary A., Sugita, Hiroyuki, Szymkowiak, Andrew E., Takei, Yoh, Tamagawa, Toru, Tashiro, Makoto, Terada, Yukikatsu, Tsujimoto, Masahiro, de Vries, Cor P., Yamada, Shinya, Yamasaki, Noriko Y., and Yatsu, Yoichi

Published
2016
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210. In-orbit operation of the ASTRO-H SXS

Author

den Herder, Jan-Willem A., Takahashi, Tadayuki, Bautz, Marshall, Tsujimoto, Masahiro, Mitsuda, Kazuhisa, Kelley, Richard L., den Herder, Jan-Willem A., Akamatsu, Hiroki, Bialas, Thomas G., Boyce, Kevin R., Brown, Gregory V., Chiao, Meng P., Costantini, Elisa, de Vries, Cor P., DiPirro, Michael J., Eckart, Megan E., Ezoe, Yuichiro, Fujimoto, Ryuichi, Haas, Daniel, Hoshino, Akio, Ishikawa, Kumi, Ishisaki, Yoshitaka, Iyomoto, Naoko, Kilbourne, Caroline A., Kitamoto, Shunji, Koyama, Shu, Leutenegger, Maurice A., McCammon, Dan, Mitsuishi, Ikuyuki, Murakami, Hiroshi, Murakami, Masahide, Noda, Hirofumi, Ogawa, Mina, Ota, Naomi, Paltani, Stéphane, Porter, Frederick S., Sato, Kosuke, Sato, Yoichi, Sawada, Makoto, Seta, Hiromi, Shinozaki, Keisuke, Shirron, Peter J., Sneiderman, Gary A., Sugita, Hiroyuki, Szymkowiak, Andrew E., Takei, Yoh, Tamagawa, Toru, Tashiro, Makoto S., Terada, Yukikatsu, Yamada, Shinya, Yamasaki, Noriko Y., and Yatsu, Yoichi

Published
2016
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211. Development of x-ray microcalorimeter imaging spectrometers for the X-ray Surveyor mission concept

Author

den Herder, Jan-Willem A., Takahashi, Tadayuki, Bautz, Marshall, Bandler, Simon R., Adams, Joseph S., Chervenak, James A., Datesman, Aaron M., Eckart, Megan E., Finkbeiner, Fred M., Kelley, Richard L., Kilbourne, Caroline A., Betancourt-Martinez, Gabriele, Miniussi, Antoine R., Porter, Frederick S., Sadleir, John E., Sakai, Kazuhiro, Smith, Stephen J., Stevenson, Thomas R., Wakeham, Nicholas A., Wassell, Edward J., Yoon, Wonsik, Becker, Dan, Bennett, Douglas, Doriese, William B., Fowler, Joseph W., Gard, Johnathan D., Hilton, Gene C., Mates, Benjamin, Morgan, Kelsey M., Reintsema, Carl D., Swetz, Daniel, Ullom, Joel N., Chaudhuri, Saptarshi, Irwin, Kent D., Lee, Sang-Jun, and Vikhlinin, Alexey

Published
2016
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212. Development, of Position-Sensitive Transition-Edge Sensor X-Ray Detectors.

Author

Smith, Stephen James, Bandler, Simon R., Brekosky, Regis P., Brown, Ari-David, Chervenak, Jay A., Eckart, Megan E., Figueroa-Feliciano, Encetali, Finkbeiner, Fred M., Kelley, Richard L., Kilbourne, Caroline A., Porter, Frederick Scott, and Sadleir, John E.

Subjects
NOISE measurement, CALORIMETERS, THERMAL conductivity, IMPEDANCE spectroscopy, DETECTORS
Abstract

We report on the development of position-sensitive transition-edge sensors (PoST's) for future X-ray astronomy missions such as the International X-ray Observatory (IXO), under study by NASA and ESA. PoST's consist of multiple absorbers each with a different thermal coupling to one or more transition-edge sensors (TESs). This results in a characteristic pulse shape for each absorber element and allows position discrimination. PoST development is motivated by a desire to achieve maximum focal-plane area with the fewest number of readout channels. We report detailed characterization of our single TES PoST's or Hydras, which consist of four electroplated AuIBi absorbers coupled to a low noise Mo/Au TES. Using a numerical model of the Hydra we fit to measured complex impedance curves and determine device parameters that allow us to accurately reproduce the measured pulse shapes and noise spectra. Results from Hydras with different internal thermal conductances reveal the trade-offs in optimizing for energy resolution or position-sensitivity. We report a best achievable energy resolution of <6.0 eV across all pixels for a device with transition temperature of 86 mK, coupled with straightforward position discrimination by rise-time. [ABSTRACT FROM AUTHOR]

Published
2009
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213. Soft x-ray spectrometer (SXS): the high-resolution cryogenic spectrometer onboard ASTRO-H

Author

Takahashi, Tadayuki, den Herder, Jan-Willem A., Bautz, Mark, Mitsuda, Kazuhisa, Kelley, Richard L., Akamatsu, Hiroki, Bialas, Thomas, Boyce, Kevin R., Brown, Gregory V., Canavan, Edgar, Chiao, Meng, Costantini, Elisa, den Herder, Jan-Willem, de Vries, Cor, DiPirro, Michael J., Eckart, Megan E., Ezoe, Yuichiro, Fujimoto, Ryuichi, Haas, Daniel, Hoshino, Akio, Ishikawa, Kumi, Ishisaki, Yoshitaka, Iyomoto, Naoko, Kilbourne, Caroline A., Kimball, Mark, Kitamoto, Shunji, Konami, Saori, Leutenegger, Maurice A., McCammon, Dan, Miko, Joseph, Mitsuishi, Ikuyuki, Murakami, Hiroshi, Murakami, Masahide, Noda, Hirofumi, Ogawa, Mina, Ohashi, Takaya, Okamoto, Atsushi, Ota, Naomi, Paltani, Stéphane, Porter, F. Scott, Sato, Kosuke, Sato, Yoichi, Sawada, Makoto, Seta, Hiromi, Shinozaki, Keisuke, Shirron, Peter J., Sneiderman, Gary A., Sugita, Hiroyuki, Szymkowiak, Andrew, Takei, Yoh, Tamagawa, Toru, Tashiro, Makoto S., Terada, Yukikatsu, Tsujimoto, Masahiro, Yamada, Shinya, and Yamasaki, Noriko Y.

Published
2014
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216. First operation of transition-edge sensors in space with the Micro-X sounding rocket.

Author

Holland, Andrew D., Beletic, James, Adams, Joseph S., Baker, Robert, Bandler, Simon R., Bastidon, Noëmie, Danowski, Meredith E., Doriese, William B., Eckart, Megan E., Figueroa-Feliciano, Enectalí, Fuhrman, Joshua, Goldfinger, David C., Heine, Sarah N. T., Hilton, Gene C., Hubbard, Antonia J. F., Jardin, Daniel, Kelley, Richard L., Kilbourne, Caroline A., Manzagol-Harwood, Renée E., and McCammon, Dan

Published
2020
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217. A COMPARISON OF X-RAY AND MID-INFRARED SELECTION OF OBSCURED ACTIVE GALACTIC NUCLEI

Author

Eckart, Megan E., McGreer, Ian D., Stern, Daniel, Harrison, Fiona A., and Helfand, David J.

Abstract

We compare the relative merits of active galactic nuclei (AGNs) selection at X-ray and mid-infrared wavelengths using data from moderately deep fields observed by both Chandra and Spitzer. The X-ray-selected AGN sample and associated photometric and spectroscopic optical follow-up are drawn from a subset of fields studied as part of the Serendipitous Extragalactic X-ray Source Identification (SEXSI) program. Mid-infrared data in these fields are derived from targeted and archival Spitzer imaging, and mid-infrared AGN selection is accomplished primarily through application of the Infrared Array Camera (IRAC) color-color AGN "wedge" selection technique. Nearly all X-ray sources in these fields which exhibit clear spectroscopic signatures of AGN activity have mid-infrared colors consistent with IRAC AGN selection. These are predominantly the most luminous X-ray sources. X-ray sources that lack high-ionization and/or broad lines in their optical spectra are far less likely to be selected as AGNs by mid-infrared color selection techniques. The fraction of X-ray sources identified as AGNs in the mid-infrared increases monotonically as the X-ray luminosity increases. Conversely, only 22% of mid-infrared-selected AGNs are detected at X-ray energies in the moderately deep ([?]t exp[?] [?] 100 ks) SEXSI Chandra data. We hypothesize that IRAC sources with AGN colors that lack X-ray detections are predominantly high-luminosity AGNs that are obscured and/or lie at high redshift. A stacking analysis of X-ray-undetected sources shows that objects in the mid-infrared AGN selection wedge have average X-ray fluxes in the 2-8 keV band 3 times higher than sources that fall outside the wedge. Their X-ray spectra are also harder. The hardness ratio of the wedge-selected stack is consistent with moderate intrinsic obscuration, but is not suggestive of a highly obscured, Compton-thick source population. It is evident from this comparative study that in order to create a complete, unbiased census of supermassive black hole growth and evolution, a combination of sensitive infrared, X-ray, and hard X-ray selection is required. We conclude by discussing what samples will be provided by upcoming survey missions such as WISE, eROSITA, and NuSTAR.

Published
2010

218. A Galaxy at z = 6.545 and Constraints on the Epoch of Reionization

Author

Stern, Daniel, Yost, Sarah A., Eckart, Megan E., Harrison, Fiona A., Helfand, David J., Malhotra, Sangeeta, and Rhoads, James E.

Abstract

We report the discovery of a Lya-emitting galaxy at redshift z = 6.545 serendipitously identified in the course of spectroscopic follow-up of hard X-ray sources on behalf of the Serendipitous Extragalactic X-Ray Source Identification (SEXSI) survey. The line flux of the galaxy, 2.1 x 10-17 ergs cm-2 s-1, is similar to line fluxes probed by narrowband imaging surveys; the 5.2 arcmin2 surveyed implies a surface density of z [?] 6.5 Lya emitters somewhat higher than that inferred from narrowband surveys. This source marks the sixth Lya-emitting galaxy identified at z [?] 6.5, a redshift putatively beyond the epoch of reionization when the damping wings of the neutral hydrogen of the intergalactic medium is capable of severely attenuating Lya emission. By comparing the Lya luminosity functions at z [?] 5.7 and z [?] 6.5, we infer that the intergalactic medium may remain largely reionized from the local universe out to z [?] 6.5.

Published
2005

219. Poisson vs. Gaussian statistics for sparse X-ray data: Application to the soft X-ray spectrometer.

Author

Yamada, Shinya, Axelsson, Magnus, Ishisaki, Yoshitaka, Konami, Saori, Takemura, Nozomi, Kelley, Richard L, Kilbourne, Caroline A, Leutenegger, Maurice A, Porter, F Scott, Eckart, Megan E, and Szymkowiak, Andrew

Subjects
SOFT X rays, X-ray spectrometers, X-rays, MAXIMUM likelihood statistics, STATISTICS
Abstract

Reliable results when fitting X-ray data require proper consideration of the statistics involved. We probe the impact of Gaussian versus Poisson statistics at low count levels using both the standard χ2 method and maximum likelihood based on Poisson (C) statistics. The difference is studied and quantified through simulated spectra with known properties. We then test the results through analysis of Mn Kα calibration data taken with the flight spare microcalorimeter for the Hitomi soft X-ray spectrometer. Through comparison with simulations, our results show that the χ2 method tends to give overly optimistic estimates of the detector energy resolution, in particular when there are few counts. Given an energy resolution of ∼5 eV and a line with about 100 photons, the line width becomes ∼10% lower in the χ2 method than in Poisson statistics. This is a consequence of the uncertainties being dominated by counting statistics, and therefore highlights the need to choose the appropriate fit statistic. [ABSTRACT FROM AUTHOR]

Published
2019
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220. Lynx X-Ray Observatory: an overview.

Author

Gaskin, Jessica A., Swartz, Douglas A., Vikhlinin, Alexey, Özel, Feryal, Gelmis, Karen E., Arenberg, Jonathan W., Bandler, Simon R., Bautz, Mark W., Civitani, Marta M., Dominguez, Alexandra, Eckart, Megan E., Falcone, Abraham D., Figueroa-Feliciano, Enectali, Freeman, Mark D., Günther, Hans M., Havey, Keith A., Heilmann, Ralf K., Kilaru, Kiranmayee, Kraft, Ralph P., and McCarley, Kevin S.

Published
2019
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221. Lynx x-ray microcalorimeter.

Author

Bandler, Simon R., Chervenak, James A., Datesman, Aaron M., Devasia, Archana M., DiPirro, Michael, Sakai, Kazuhiro, Smith, Stephen J., Stevenson, Thomas R., Yoon, Wonsik, Bennett, Douglas, Mates, Benjamin, Swetz, Daniel, Ullom, Joel N., Irwin, Kent D., Eckart, Megan E., Figueroa-Feliciano, Enectali, McCammon, Dan, Ryu, Kevin, Olson, Jeffrey, and Zeiger, Ben

Published
2019
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223. Multiabsorber transition-edge sensors for x-ray astronomy.

Author

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

Published
2019
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224. Fabrication of a Hybrid Transition Edge Sensor Array for Lynx

Author

Wassell, Edward, Adams, Joseph S., Bandler, Simon R., Chang, Meng-Ping, Chervenak, James A., Datesman, Aaron M., Eckart, Megan E., Ewin, Audrey J., Finkbeiner, Fred M., Yoon Ha, Jong, Kelley, R., Kilbourne, Caroline A., Miniussi, Antoine R., Porter, F., Sadleir, John E., Sakai, Kazuhiro, Smith, Stephen J., and Wakehan, Nicholas

Subjects
hybrid, lynx, transition, fabrication, array, edge sensor
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225. High-resolution laboratory measurements of M-shell Fe EUV line emission using EBIT-I.

Author

Fairchild, Alexander J., Hell, Natalie, Beiersdorfer, Peter, Brown, Gregory V., Eckart, Megan E., Hahn, Michael, and Savin, Daniel W.

Abstract

Solar physicists routinely utilize observations of Ar-like Fe IX and Cl-like Fe X emission to study a variety of solar structures. However, unidentified lines exist in the Fe IX and Fe X spectra, greatly impeding the spectroscopic diagnostic potential of these ions. Here, we present measurements using the Lawrence Livermore National Laboratory EBIT-I electron beam ion trap in the wavelength range 238–258 Å. These studies enable us to unambiguously identify the charge state associated with each of the observed lines. This wavelength range is of particular interest because it contains the Fe IX density diagnostic line ratio 241.74 Å/244.91 Å, which is predicted to be one of the best density diagnostics of the solar corona, as well as the Fe X 257.26 Å magnetic-field-induced transition. We compare our measurements to the Fe IX and Fe X lines tabulated in CHIANTI v10.0.1, which is used for modeling the solar spectrum. In addition, we have measured previously unidentified Fe X lines that will need to be added to CHIANTI and other spectroscopic databases. [ABSTRACT FROM AUTHOR]

Published
2024
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226. Cryogen-free operation of the Soft X-ray Spectrometer instrument

Author

Sneiderman, Gary A., Shirron, Peter J., Fujimoto, Ryuichi, Bialas, Thomas G., Boyce, Kevin R., Chiao, Meng P., DiPirro, Michael J., Eckart, Megan E., Hartz, Leslie, Ishisaki, Yoshitaka, Kilbourne, Caroline A., Masters, Candace, McCammon, Dan, Mitsuda, Kazuhisa, Noda, Hirofumi, Porter, Frederick S., Szymkowiak, Andrew E., Takei, Yoh, Tsujimoto, Mashiro, and Yoshida, Seiji

Published
2018
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227. Ground calibration of the Astro-H (Hitomi) soft x-ray spectrometer

Author

Eckart, Megan E., Adams, Joseph S., Boyce, Kevin R., Brown, Gregory V., Chiao, Meng P., Fujimoto, Ryuichi, Haas, Daniel, den Herder, Jan-Willem, Hoshino, Akio, Ishisaki, Yoshitaka, Kilbourne, Caroline A., Kitamoto, Shunji, Leutenegger, Maurice A., McCammon, Dan, Mitsuda, Kazuhisa, Porter, F. Scott, Sato, Kosuke, Sawada, Makoto, Seta, Hiromi, Sneiderman, Gary A., Szymkowiak, Andrew E., Takei, Yoh, Tashiro, Makoto S., Tsujimoto, Masahiro, de Vries, Cor P., Watanabe, Tomomi, Yamada, Shinya, and Yamasaki, Noriko Y.

Published
2018
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228. Hitomi (ASTRO-H) X-ray Astronomy Satellite

Author

Takahashi, Tadayuki, Kokubun, Motohide, Mitsuda, Kazuhisa, Kelley, Richard L., Ohashi, Takaya, Aharonian, Felix, Akamatsu, Hiroki, Akimoto, Fumie, Allen, Steven W., Anabuki, Naohisa, Angelini, Lorella, Arnaud, Keith, Asai, Makoto, Audard, Marc, Awaki, Hisamitsu, Axelsson, Magnus, Azzarello, Philipp, Baluta, Chris, Bamba, Aya, Bando, Nobutaka, Bautz, Marshall W., Bialas, Thomas, Blandford, Roger, Boyce, Kevin, Brenneman, Laura W., Brown, Gregory V., Bulbul, Esra, Cackett, Edward M., Canavan, Edgar, Chernyakova, Maria, Chiao, Meng P., Coppi, Paolo S., Costantini, Elisa, O’ Dell, Steve, DiPirro, Michael, Done, Chris, Dotani, Tadayasu, Doty, John, Ebisawa, Ken, Eckart, Megan E., Enoto, Teruaki, Ezoe, Yuichiro, Fabian, Andrew C., Ferrigno, Carlo, Foster, Adam R., Fujimoto, Ryuichi, Fukazawa, Yasushi, Funk, Stefan, Furuzawa, Akihiro, Galeazzi, Massimiliano, Gallo, Luigi C., Gandhi, Poshak, Gilmore, Kirk, Giustini, Margherita, Goldwurm, Andrea, Gu, Liyi, Guainazzi, Matteo, Haas, Daniel, Haba, Yoshito, Hagino, Kouichi, Hamaguchi, Kenji, Harrus, Ilana M., Hatsukade, Isamu, Hayashi, Takayuki, Hayashi, Katsuhiro, Hayashida, Kiyoshi, den Herder, Jan-Willem, Hiraga, Junko S., Hirose, Kazuyuki, Hornschemeier, Ann, Hoshino, Akio, Hughes, John P., Ichinohe, Yuto, Iizuka, Ryo, Inoue, Hajime, Inoue, Yoshiyuki, Ishibashi, Kazunori, Ishida, Manabu, Ishikawa, Kumi, Ishimura, Kosei, Ishisaki, Yoshitaka, Itoh, Masayuki, Iwai, Masachika, Iwata, Naoko, Iyomoto, Naoko, Jewell, Chris, Kaastra, Jelle, Kallman, Tim, Kamae, Tsuneyoshi, Kara, Erin, Kataoka, Jun, Katsuda, Satoru, Katsuta, Junichiro, Kawaharada, Madoka, Kawai, Nobuyuki, Kawano, Taro, Kawasaki, Shigeo, Khangulyan, Dmitry, Kilbourne, Caroline A., Kimball, Mark, King, Ashley, Kitaguchi, Takao, Kitamoto, Shunji, Kitayama, Tetsu, Kohmura, Takayoshi, Konami, Saori, Kosaka, Tatsuro, Koujelev, Alex, Koyama, Katsuji, Koyama, Shu, Kretschmar, Peter, Krimm, Hans A., Kubota, Aya, Kunieda, Hideyo, Laurent, Philippe, Lee, Shiu-Hang, Leutenegger, Maurice A., Limousin, Olivier, Loewenstein, Michael, Long, Knox S., Lumb, David, Madejski, Greg, Maeda, Yoshitomo, Maier, Daniel, Makishima, Kazuo, Markevitch, Maxim, Masters, Candace, Matsumoto, Hironori, Matsushita, Kyoko, McCammon, Dan, Mcguinness, Daniel, McNamara, Brian R., Mehdipour, Missagh, Miko, Joseph, Miller, Eric D., Miller, Jon M., Mineshige, Shin, Minesugi, Kenji, Mitsuishi, Ikuyuki, Miyazawa, Takuya, Mizuno, Tsunefumi, Mori, Hideyuki, Mori, Koji, Moroso, Franco, Moseley, Harvey, Muench, Theodore, Mukai, Koji, Murakami, Hiroshi, Murakami, Toshio, Mushotzky, Richard F., Nagano, Housei, Nagino, Ryo, Nakagawa, Takao, Nakajima, Hiroshi, Nakamori, Takeshi, Nakano, Toshio, Nakashima, Shinya, Nakazawa, Kazuhiro, Namba, Yoshiharu, Natsukari, Chikara, Nishioka, Yusuke, Nobukawa, Kumiko K., Nobukawa, Masayoshi, Noda, Hirofumi, Nomachi, Masaharu, Odaka, Hirokazu, Ogawa, Hiroyuki, Ogawa, Mina, Ogi, Keiji, Ohno, Masanori, Ohta, Masayuki, Okajima, Takashi, Okamoto, Atsushi, Okazaki, Tsuyoshi, Ota, Naomi, Ozaki, Masanobu, Paerels, Frits, Paltani, Stéphane, Parmar, Arvind, Petre, Robert, Pinto, Ciro, de Plaa, Jelle, Pohl, Martin, Pontius, James, Porter, Frederick S., Pottschmidt, Katja, Ramsey, Brian, Reynolds, Christopher, Russell, Helen, Safi-Harb, Samar, Saito, Shinya, Sakai, Kazuhiro, Sakai, Shin-ichiro, Sameshima, Hiroaki, Sasaki, Toru, Sato, Goro, Sato, Kosuke, Sato, Rie, Sato, Yoichi, Sawada, Makoto, Schartel, Norbert, Serlemitsos, Peter J., Seta, Hiromi, Shibano, Yasuko, Shida, Maki, Shidatsu, Megumi, Shimada, Takanobu, Shinozaki, Keisuke, Shirron, Peter, Simionescu, Aurora, Simmons, Cynthia, Smith, Randall K., Sneiderman, Gary, Soong, Yang, Stawarz, Łukasz, Sugawara, Yasuharu, Sugita, Satoshi, Sugita, Hiroyuki, Szymkowiak, Andrew, Tajima, Hiroyasu, Takahashi, Hiromitsu, Takeda, Shin’ichiro, Takei, Yoh, Tamagawa, Toru, Tamura, Takayuki, Tamura, Keisuke, Tanaka, Takaaki, Tanaka, Yasuo, Tanaka, Yasuyuki T., Tashiro, Makoto S., Tawara, Yuzuru, Terada, Yukikatsu, Terashima, Yuichi, Tombesi, Francesco, Tomida, Hiroshi, Tsuboi, Yohko, Tsujimoto, Masahiro, Tsunemi, Hiroshi, Tsuru, Takeshi Go, Uchida, Hiroyuki, Uchiyama, Hideki, Uchiyama, Yasunobu, Ueda, Shutaro, Ueda, Yoshihiro, Ueno, Shiro, Uno, Shin’ichiro, Urry, C. Megan, Ursino, Eugenio, de Vries, Cor P., Wada, Atsushi, Watanabe, Shin, Watanabe, Tomomi, Werner, Norbert, Wik, Daniel R., Wilkins, Dan R., Williams, Brian J., Yamada, Shinya, Yamada, Takahiro, Yamaguchi, Hiroya, Yamaoka, Kazutaka, Yamasaki, Noriko Y., Yamauchi, Makoto, Yamauchi, Shigeo, Yaqoob, Tahir, Yatsu, Yoichi, Yonetoku, Daisuke, Yoshida, Atsumasa, Yuasa, Takayuki, Zhuravleva, Irina, and Zoghbi, Abderahmen

Published
2018
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229. Hitomi X-ray observation of the pulsar wind nebula G21.5−0.9

Author

Aharonian, Felix, Akamatsu, Hiroki, Akimoto, Fumie, Allen, Steven W, Angelini, Lorella, Audard, Marc, Awaki, Hisamitsu, Axelsson, Magnus, Bamba, Aya, Bautz, Marshall W, Blandford, Roger, Brenneman, Laura W, Brown, Gregory V, Bulbul, Esra, Cackett, Edward M, Chernyakova, Maria, Chiao, Meng P, Coppi, Paolo S, Costantini, Elisa, de Plaa, Jelle, de Vries, Cor P, den Herder, Jan-Willem, Done, Chris, Dotani, Tadayasu, Ebisawa, Ken, Eckart, Megan E, Enoto, Teruaki, Ezoe, Yuichiro, Fabian, Andrew C, Ferrigno, Carlo, Foster, Adam R, Fujimoto, Ryuichi, Fukazawa, Yasushi, Furuzawa, Akihiro, Galeazzi, Massimiliano, Gallo, Luigi C, Gandhi, Poshak, Giustini, Margherita, Goldwurm, Andrea, Gu, Liyi, Guainazzi, Matteo, Haba, Yoshito, Hagino, Kouichi, Hamaguchi, Kenji, Harrus, Ilana M, Hatsukade, Isamu, Hayashi, Katsuhiro, Hayashi, Takayuki, Hayashida, Kiyoshi, Hiraga, Junko S, Hornschemeier, Ann, Hoshino, Akio, Hughes, John P, Ichinohe, Yuto, Iizuka, Ryo, Inoue, Hajime, Inoue, Yoshiyuki, Ishida, Manabu, Ishikawa, Kumi, Ishisaki, Yoshitaka, Iwai, Masachika, Kaastra, Jelle, Kallman, Tim, Kamae, Tsuneyoshi, Kataoka, Jun, Katsuda, Satoru, Kawai, Nobuyuki, Kelley, Richard L, Kilbourne, Caroline A, Kitaguchi, Takao, Kitamoto, Shunji, Kitayama, Tetsu, Kohmura, Takayoshi, Kokubun, Motohide, Koyama, Katsuji, Koyama, Shu, Kretschmar, Peter, Krimm, Hans A, Kubota, Aya, Kunieda, Hideyo, Laurent, Philippe, Lee, Shiu-Hang, Leutenegger, Maurice A, Limousin, Olivier, Loewenstein, Michael, Long, Knox S, Lumb, David, Madejski, Greg, Maeda, Yoshitomo, Maier, Daniel, Makishima, Kazuo, Markevitch, Maxim, Matsumoto, Hironori, Matsushita, Kyoko, McCammon, Dan, McNamara, Brian R, Mehdipour, Missagh, Miller, Eric D, Miller, Jon M, Mineshige, Shin, Mitsuda, Kazuhisa, Mitsuishi, Ikuyuki, Miyazawa, Takuya, Mizuno, Tsunefumi, Mori, Hideyuki, Mori, Koji, Mukai, Koji, Murakami, Hiroshi, Mushotzky, Richard F, Nakagawa, Takao, Nakajima, Hiroshi, Nakamori, Takeshi, Nakashima, Shinya, Nakazawa, Kazuhiro, Nobukawa, Kumiko K, Nobukawa, Masayoshi, Noda, Hirofumi, Odaka, Hirokazu, Ohashi, Takaya, Ohno, Masanori, Okajima, Takashi, Ota, Naomi, Ozaki, Masanobu, Paerels, Frits, Paltani, Stéphane, Petre, Robert, Pinto, Ciro, Porter, Frederick S, Pottschmidt, Katja, Reynolds, Christopher S, Safi-Harb, Samar, Saito, Shinya, Sakai, Kazuhiro, Sasaki, Toru, Sato, Goro, Sato, Kosuke, Sato, Rie, Sawada, Makoto, Schartel, Norbert, Serlemtsos, Peter J, Seta, Hiromi, Shidatsu, Megumi, Simionescu, Aurora, Smith, Randall K, Soong, Yang, Stawarz, Łukasz, Sugawara, Yasuharu, Sugita, Satoshi, Szymkowiak, Andrew, Tajima, Hiroyasu, Takahashi, Hiromitsu, Takahashi, Tadayuki, Takeda, Shin’ichiro, Takei, Yoh, Tamagawa, Toru, Tamura, Takayuki, Tanaka, Takaaki, Tanaka, Yasuo, Tanaka, Yasuyuki T, Tashiro, Makoto S, Tawara, Yuzuru, Terada, Yukikatsu, Terashima, Yuichi, Tombesi, Francesco, Tomida, Hiroshi, Tsuboi, Yohko, Tsujimoto, Masahiro, Tsunemi, Hiroshi, Tsuru, Takeshi Go, Uchida, Hiroyuki, Uchiyama, Hideki, Uchiyama, Yasunobu, Ueda, Shutaro, Ueda, Yoshihiro, Uno, Shin’ichiro, Urry, C Megan, Ursino, Eugenio, Watanabe, Shin, Werner, Norbert, Wilkins, Dan R, Williams, Brian J, Yamada, Shinya, Yamaguchi, Hiroya, Yamaoka, Kazutaka, Yamasaki, Noriko Y, Yamauchi, Makoto, Yamauchi, Shigeo, Yaqoob, Tahir, Yatsu, Yoichi, Yonetoku, Daisuke, Zhuravleva, Irina, Zoghbi, Abderahmen, Sato, Toshiki, Nakaniwa, Nozomu, Murakami, Hiroaki, and Guest, Benson

Abstract

We present results from the Hitomi X-ray observation of a young composite-type supernova remnant (SNR) G21.5−0.9, whose emission is dominated by the pulsar wind nebula (PWN) contribution. The X-ray spectra in the 0.8–80 keV range obtained with the Soft X-ray Spectrometer (SXS), Soft X-ray Imager, and Hard X-ray Imager (HXI) show a significant break in the continuum as previously found with the NuSTAR observation. After taking into account all known emissions from the SNR other than the PWN itself, we find that the Hitomi spectra can be fitted with a broken power law with photon indices of Γ1= 1.74 ± 0.02 and Γ2= 2.14 ± 0.01 below and above the break at 7.1 ± 0.3 keV, which is significantly lower than the NuSTAR result (∼9.0 keV). The spectral break cannot be reproduced by time-dependent particle injection one-zone spectral energy distribution models, which strongly indicates that a more complex emission model is needed, as suggested by recent theoretical models. We also search for narrow emission or absorption lines with the SXS, and perform a timing analysis of PSR J1833−1034 with the HXI and the Soft Gamma-ray Detector. No significant pulsation is found from the pulsar. However, unexpectedly, narrow absorption line features are detected in the SXS data at 4.2345 keV and 9.296 keV with a significance of 3.65 σ. While the origin of these features is not understood, their mere detection opens up a new field of research and was only possible with the high resolution, sensitivity, and ability to measure extended sources provided by an X-ray microcalorimeter.

Published
2018
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230. Atomic data and spectral modeling constraints from high-resolution X-ray observations of the Perseus cluster with Hitomi*

Author

Collaboration, Hitomi, Aharonian, Felix, Akamatsu, Hiroki, Akimoto, Fumie, Allen, Steven W, Angelini, Lorella, Audard, Marc, Awaki, Hisamitsu, Axelsson, Magnus, Bamba, Aya, Bautz, Marshall W, Blandford, Roger, Brenneman, Laura W, Brown, Gregory V, Bulbul, Esra, Cackett, Edward M, Chernyakova, Maria, Chiao, Meng P, Coppi, Paolo S, Costantini, Elisa, de Plaa, Jelle, de Vries, Cor P, den Herder, Jan-Willem, Done, Chris, Dotani, Tadayasu, Ebisawa, Ken, Eckart, Megan E, Enoto, Teruaki, Ezoe, Yuichiro, Fabian, Andrew C, Ferrigno, Carlo, Foster, Adam R, Fujimoto, Ryuichi, Fukazawa, Yasushi, Furuzawa, Akihiro, Galeazzi, Massimiliano, Gallo, Luigi C, Gandhi, Poshak, Giustini, Margherita, Goldwurm, Andrea, Gu, Liyi, Guainazzi, Matteo, Haba, Yoshito, Hagino, Kouichi, Hamaguchi, Kenji, Harrus, Ilana M, Hatsukade, Isamu, Hayashi, Katsuhiro, Hayashi, Takayuki, Hayashida, Kiyoshi, Hell, Natalie, Hiraga, Junko S, Hornschemeier, Ann, Hoshino, Akio, Hughes, John P, Ichinohe, Yuto, Iizuka, Ryo, Inoue, Hajime, Inoue, Yoshiyuki, Ishida, Manabu, Ishikawa, Kumi, Ishisaki, Yoshitaka, Iwai, Masachika, Kaastra, Jelle, Kallman, Tim, Kamae, Tsuneyoshi, Kataoka, Jun, Katsuda, Satoru, Kawai, Nobuyuki, Kelley, Richard L, Kilbourne, Caroline A, Kitaguchi, Takao, Kitamoto, Shunji, Kitayama, Tetsu, Kohmura, Takayoshi, Kokubun, Motohide, Koyama, Katsuji, Koyama, Shu, Kretschmar, Peter, Krimm, Hans A, Kubota, Aya, Kunieda, Hideyo, Laurent, Philippe, Lee, Shiu-Hang, Leutenegger, Maurice A, Limousin, Olivier, Loewenstein, Michael, Long, Knox S, Lumb, David, Madejski, Greg, Maeda, Yoshitomo, Maier, Daniel, Makishima, Kazuo, Markevitch, Maxim, Matsumoto, Hironori, Matsushita, Kyoko, McCammon, Dan, McNamara, Brian R, Mehdipour, Missagh, Miller, Eric D, Miller, Jon M, Mineshige, Shin, Mitsuda, Kazuhisa, Mitsuishi, Ikuyuki, Miyazawa, Takuya, Mizuno, Tsunefumi, Mori, Hideyuki, Mori, Koji, Mukai, Koji, Murakami, Hiroshi, Mushotzky, Richard F, Nakagawa, Takao, Nakajima, Hiroshi, Nakamori, Takeshi, Nakashima, Shinya, Nakazawa, Kazuhiro, Nobukawa, Kumiko K, Nobukawa, Masayoshi, Noda, Hirofumi, Odaka, Hirokazu, Ohashi, Takaya, Ohno, Masanori, Okajima, Takashi, Ota, Naomi, Ozaki, Masanobu, Paerels, Frits, Paltani, Stéphane, Petre, Robert, Pinto, Ciro, Porter, Frederick S, Pottschmidt, Katja, Reynolds, Christopher S, Safi-Harb, Samar, Saito, Shinya, Sakai, Kazuhiro, Sasaki, Toru, Sato, Goro, Sato, Kosuke, Sato, Rie, Sawada, Makoto, Schartel, Norbert, Serlemtsos, Peter J, Seta, Hiromi, Shidatsu, Megumi, Simionescu, Aurora, Smith, Randall K, Soong, Yang, Stawarz, Łukasz, Sugawara, Yasuharu, Sugita, Satoshi, Szymkowiak, Andrew, Tajima, Hiroyasu, Takahashi, Hiromitsu, Takahashi, Tadayuki, Takeda, Shin’ichiro, Takei, Yoh, Tamagawa, Toru, Tamura, Takayuki, Tanaka, Takaaki, Tanaka, Yasuo, Tanaka, Yasuyuki T, Tashiro, Makoto S, Tawara, Yuzuru, Terada, Yukikatsu, Terashima, Yuichi, Tombesi, Francesco, Tomida, Hiroshi, Tsuboi, Yohko, Tsujimoto, Masahiro, Tsunemi, Hiroshi, Tsuru, Takeshi Go, Uchida, Hiroyuki, Uchiyama, Hideki, Uchiyama, Yasunobu, Ueda, Shutaro, Ueda, Yoshihiro, Uno, Shin’ichiro, Urry, C Megan, Ursino, Eugenio, Watanabe, Shin, Werner, Norbert, Wilkins, Dan R, Williams, Brian J, Yamada, Shinya, Yamaguchi, Hiroya, Yamaoka, Kazutaka, Yamasaki, Noriko Y, Yamauchi, Makoto, Yamauchi, Shigeo, Yaqoob, Tahir, Yatsu, Yoichi, Yonetoku, Daisuke, Zhuravleva, Irina, Zoghbi, Abderahmen, and Raassen, A J J

Abstract

The Hitomi Soft X-ray Spectrometer spectrum of the Perseus cluster, with ∼5 eV resolution in the 2–9 keV band, offers an unprecedented benchmark of the atomic modeling and database for hot collisional plasmas. It reveals both successes and challenges of the current atomic data and models. The latest versions of AtomDB/APEC (3.0.8), SPEX (3.03.00), and CHIANTI (8.0) all provide reasonable fits to the broad-band spectrum, and are in close agreement on best-fit temperature, emission measure, and abundances of a few elements such as Ni. For the Fe abundance, the APEC and SPEX measurements differ by 16%, which is 17 times higher than the statistical uncertainty. This is mostly attributed to the differences in adopted collisional excitation and dielectronic recombination rates of the strongest emission lines. We further investigate and compare the sensitivity of the derived physical parameters to the astrophysical source modeling and instrumental effects. The Hitomi results show that accurate atomic data and models are as important as the astrophysical modeling and instrumental calibration aspects. Substantial updates of atomic databases and targeted laboratory measurements are needed to get the current data and models ready for the data from the next Hitomi-level mission.

Published
2018
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231. Search for thermal X-ray features from the Crab nebula with the Hitomi soft X-ray spectrometer*

Author

Collaboration, Hitomi, Aharonian, Felix, Akamatsu, Hiroki, Akimoto, Fumie, Allen, Steven W, Angelini, Lorella, Audard, Marc, Awaki, Hisamitsu, Axelsson, Magnus, Bamba, Aya, Bautz, Marshall W, Blandford, Roger, Brenneman, Laura W, Brown, Gregory V, Bulbul, Esra, Cackett, Edward M, Chernyakova, Maria, Chiao, Meng P, Coppi, Paolo S, Costantini, Elisa, de Plaa, Jelle, de Vries, Cor P, den Herder, Jan-Willem, Done, Chris, Dotani, Tadayasu, Ebisawa, Ken, Eckart, Megan E, Enoto, Teruaki, Ezoe, Yuichiro, Fabian, Andrew C, Ferrigno, Carlo, Foster, Adam R, Fujimoto, Ryuichi, Fukazawa, Yasushi, Furuzawa, Akihiro, Galeazzi, Massimiliano, Gallo, Luigi C, Gandhi, Poshak, Giustini, Margherita, Goldwurm, Andrea, Gu, Liyi, Guainazzi, Matteo, Haba, Yoshito, Hagino, Kouichi, Hamaguchi, Kenji, Harrus, Ilana M, Hatsukade, Isamu, Hayashi, Katsuhiro, Hayashi, Takayuki, Hayashida, Kiyoshi, Hiraga, Junko S, Hornschemeier, Ann, Hoshino, Akio, Hughes, John P, Ichinohe, Yuto, Iizuka, Ryo, Inoue, Hajime, Inoue, Yoshiyuki, Ishida, Manabu, Ishikawa, Kumi, Ishisaki, Yoshitaka, Kaastra, Jelle, Kallman, Tim, Kamae, Tsuneyoshi, Kataoka, Jun, Katsuda, Satoru, Kawai, Nobuyuki, Kelley, Richard L, Kilbourne, Caroline A, Kitaguchi, Takao, Kitamoto, Shunji, Kitayama, Tetsu, Kohmura, Takayoshi, Kokubun, Motohide, Koyama, Katsuji, Koyama, Shu, Kretschmar, Peter, Krimm, Hans A, Kubota, Aya, Kunieda, Hideyo, Laurent, Philippe, Lee, Shiu-Hang, Leutenegger, Maurice A, Limousin, Olivier, Loewenstein, Michael, Long, Knox S, Lumb, David, Madejski, Greg, Maeda, Yoshitomo, Maier, Daniel, Makishima, Kazuo, Markevitch, Maxim, Matsumoto, Hironori, Matsushita, Kyoko, McCammon, Dan, McNamara, Brian R, Mehdipour, Missagh, Miller, Eric D, Miller, Jon M, Mineshige, Shin, Mitsuda, Kazuhisa, Mitsuishi, Ikuyuki, Miyazawa, Takuya, Mizuno, Tsunefumi, Mori, Hideyuki, Mori, Koji, Mukai, Koji, Murakami, Hiroshi, Mushotzky, Richard F, Nakagawa, Takao, Nakajima, Hiroshi, Nakamori, Takeshi, Nakashima, Shinya, Nakazawa, Kazuhiro, Nobukawa, Kumiko K, Nobukawa, Masayoshi, Noda, Hirofumi, Odaka, Hirokazu, Ohashi, Takaya, Ohno, Masanori, Okajima, Takashi, Ota, Naomi, Ozaki, Masanobu, Paerels, Frits, Paltani, Stéphane, Petre, Robert, Pinto, Ciro, Porter, Frederick S, Pottschmidt, Katja, Reynolds, Christopher S, Safi-Harb, Samar, Saito, Shinya, Sakai, Kazuhiro, Sasaki, Toru, Sato, Goro, Sato, Kosuke, Sato, Rie, Sato, Toshiki, Sawada, Makoto, Schartel, Norbert, Serlemtsos, Peter J, Seta, Hiromi, Shidatsu, Megumi, Simionescu, Aurora, Smith, Randall K, Soong, Yang, Stawarz, Łukasz, Sugawara, Yasuharu, Sugita, Satoshi, Szymkowiak, Andrew, Tajima, Hiroyasu, Takahashi, Hiromitsu, Takahashi, Tadayuki, Takeda, Shin΄ichiro, Takei, Yoh, Tamagawa, Toru, Tamura, Takayuki, Tanaka, Takaaki, Tanaka, Yasuo, Tanaka, Yasuyuki T, Tashiro, Makoto S, Tawara, Yuzuru, Terada, Yukikatsu, Terashima, Yuichi, Tombesi, Francesco, Tomida, Hiroshi, Tsuboi, Yohko, Tsujimoto, Masahiro, Tsunemi, Hiroshi, Tsuru, Takeshi Go, Uchida, Hiroyuki, Uchiyama, Hideki, Uchiyama, Yasunobu, Ueda, Shutaro, Ueda, Yoshihiro, Uno, Shin΄ichiro, Urry, C Megan, Ursino, Eugenio, Watanabe, Shin, Werner, Norbert, Wilkins, Dan R, Williams, Brian J, Yamada, Shinya, Yamaguchi, Hiroya, Yamaoka, Kazutaka, Yamasaki, Noriko Y, Yamauchi, Makoto, Yamauchi, Shigeo, Yaqoob, Tahir, Yatsu, Yoichi, Yonetoku, Daisuke, Zhuravleva, Irina, Zoghbi, Abderahmen, Tominaga, Nozomu, and Moriya, Takashi J

Abstract

The Crab nebula originated from a core-collapse supernova (SN) explosion observed in 1054 ad. When viewed as a supernova remnant (SNR), it has an anomalously low observed ejecta mass and kinetic energy for an Fe-core-collapse SN. Intensive searches have been made for a massive shell that solves this discrepancy, but none has been detected. An alternative idea is that SN 1054 is an electron-capture (EC) explosion with a lower explosion energy by an order of magnitude than Fe-core-collapse SNe. X-ray imaging searches were performed for the plasma emission from the shell in the Crab outskirts to set a stringent upper limit on the X-ray emitting mass. However, the extreme brightness of the source hampers access to its vicinity. We thus employed spectroscopic technique using the X-ray micro-calorimeter on board the Hitomi satellite. By exploiting its superb energy resolution, we set an upper limit for emission or absorption features from as yet undetected thermal plasma in the 2–12 keV range. We also re-evaluated the existing Chandra and XMM-Newton data. By assembling these results, a new upper limit was obtained for the X-ray plasma mass of ≲ 1 M⊙for a wide range of assumed shell radius, size, and plasma temperature values both in and out of collisional equilibrium. To compare with the observation, we further performed hydrodynamic simulations of the Crab SNR for two SN models (Fe-core versus EC) under two SN environments (uniform interstellar medium versus progenitor wind). We found that the observed mass limit can be compatible with both SN models if the SN environment has a low density of ≲ 0.03 cm−3(Fe core) or ≲ 0.1 cm−3(EC) for the uniform density, or a progenitor wind density somewhat less than that provided by a mass loss rate of 10−5M⊙yr−1at 20 km s−1for the wind environment.

Published
2018
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232. Hitomi observation of radio galaxy NGC 1275: The first X-ray microcalorimeter spectroscopy of Fe-Kα line emission from an active galactic nucleus*

Author

Collaboration, Hitomi, Aharonian, Felix, Akamatsu, Hiroki, Akimoto, Fumie, Allen, Steven W, Angelini, Lorella, Audard, Marc, Awaki, Hisamitsu, Axelsson, Magnus, Bamba, Aya, Bautz, Marshall W, Blandford, Roger, Brenneman, Laura W, Brown, Gregory V, Bulbul, Esra, Cackett, Edward M, Chernyakova, Maria, Chiao, Meng P, Coppi, Paolo S, Costantini, Elisa, de Plaa, Jelle, de Vries, Cor P, den Herder, Jan-Willem, Done, Chris, Dotani, Tadayasu, Ebisawa, Ken, Eckart, Megan E, Enoto, Teruaki, Ezoe, Yuichiro, Fabian, Andrew C, Ferrigno, Carlo, Foster, Adam R, Fujimoto, Ryuichi, Fukazawa, Yasushi, Furuzawa, Akihiro, Galeazzi, Massimiliano, Gallo, Luigi C, Gandhi, Poshak, Giustini, Margherita, Goldwurm, Andrea, Gu, Liyi, Guainazzi, Matteo, Haba, Yoshito, Hagino, Kouichi, Hamaguchi, Kenji, Harrus, Ilana M, Hatsukade, Isamu, Hayashi, Katsuhiro, Hayashi, Takayuki, Hayashida, Kiyoshi, Hiraga, Junko S, Hornschemeier, Ann, Hoshino, Akio, Hughes, John P, Ichinohe, Yuto, Iizuka, Ryo, Inoue, Hajime, Inoue, Yoshiyuki, Ishida, Manabu, Ishikawa, Kumi, Ishisaki, Yoshitaka, Iwai, Masachika, Kaastra, Jelle, Kallman, Tim, Kamae, Tsuneyoshi, Kataoka, Jun, Katsuda, Satoru, Kawai, Nobuyuki, Kelley, Richard L, Kilbourne, Caroline A, Kitaguchi, Takao, Kitamoto, Shunji, Kitayama, Tetsu, Kohmura, Takayoshi, Kokubun, Motohide, Koyama, Katsuji, Koyama, Shu, Kretschmar, Peter, Krimm, Hans A, Kubota, Aya, Kunieda, Hideyo, Laurent, Philippe, Lee, Shiu-Hang, Leutenegger, Maurice A, Limousin, Olivier O, Loewenstein, Michael, Long, Knox S, Lumb, David, Madejski, Greg, Maeda, Yoshitomo, Maier, Daniel, Makishima, Kazuo, Markevitch, Maxim, Matsumoto, Hironori, Matsushita, Kyoko, McCammon, Dan, McNamara, Brian R, Mehdipour, Missagh, Miller, Eric D, Miller, Jon M, Mineshige, Shin, Mitsuda, Kazuhisa, Mitsuishi, Ikuyuki, Miyazawa, Takuya, Mizuno, Tsunefumi, Mori, Hideyuki, Mori, Koji, Mukai, Koji, Murakami, Hiroshi, Mushotzky, Richard F, Nakagawa, Takao, Nakajima, Hiroshi, Nakamori, Takeshi, Nakashima, Shinya, Nakazawa, Kazuhiro, Nobukawa, Kumiko K, Nobukawa, Masayoshi, Noda, Hirofumi, Odaka, Hirokazu, Ohashi, Takaya, Ohno, Masanori, Okajima, Takashi, Ota, Naomi, Ozaki, Masanobu, Paerels, Frits, Paltani, Stéphane, Petre, Robert, Pinto, Ciro, Porter, Frederick S, Pottschmidt, Katja, Reynolds, Christopher S, Safi-Harb, Samar, Saito, Shinya, Sakai, Kazuhiro, Sasaki, Toru, Sato, Goro, Sato, Kosuke, Sato, Rie, Sawada, Makoto, Schartel, Norbert, Serlemitsos, Peter J, Seta, Hiromi, Shidatsu, Megumi, Simionescu, Aurora, Smith, Randall K, Soong, Yang, Stawarz, Łukasz, Sugawara, Yasuharu, Sugita, Satoshi, Szymkowiak, Andrew, Tajima, Hiroyasu, Takahashi, Hiromitsu, Takahashi, Tadayuki, Takeda, Shin’ichiro, Takei, Yoh, Tamagawa, Toru, Tamura, Takayuki, Tanaka, Takaaki, Tanaka, Yasuo, Tanaka, Yasuyuki T, Tashiro, Makoto S, Tawara, Yuzuru, Terada, Yukikatsu, Terashima, Yuichi, Tombesi, Francesco, Tomida, Hiroshi, Tsuboi, Yohko, Tsujimoto, Masahiro, Tsunemi, Hiroshi, Tsuru, Takeshi Go, Uchida, Hiroyuki, Uchiyama, Hideki, Uchiyama, Yasunobu, Ueda, Shutaro, Ueda, Yoshihiro, Uno, Shin’ichiro, Urry, C Megan, Ursino, Eugenio, Watanabe, Shin, Werner, Norbert, Wilkins, Dan R, Williams, Brian J, Yamada, Shinya, Yamaguchi, Hiroya, Yamaoka, Kazutaka, Yamasaki, Noriko Y, Yamauchi, Makoto, Yamauchi, Shigeo, Yaqoob, Tahir, Yatsu, Yoichi, Yonetoku, Daisuke, Zhuravleva, Irina, Zoghbi, Abderahmen, and Kawamuro, Taiki

Abstract

The origin of the narrow Fe-Kα fluorescence line at 6.4 keV from active galactic nuclei has long been under debate; some of the possible sites are the outer accretion disk, the broad line region, a molecular torus, or interstellar/intracluster media. In 2016 February–March, we performed the first X-ray microcalorimeter spectroscopy with the Soft X-ray Spectrometer (SXS) on board the Hitomi satellite of the Fanaroff–Riley type I radio galaxy NGC 1275 at the center of the Perseus cluster of galaxies. With the high-energy resolution of ∼5 eV at 6 keV achieved by Hitomi/SXS, we detected the Fe-Kα line with ∼5.4 σ significance. The velocity width is constrained to be 500–1600 km s−1(FWHM for Gaussian models) at 90% confidence. The SXS also constrains the continuum level from the NGC 1275 nucleus up to ∼20 keV, giving an equivalent width of ∼20 eV for the 6.4 keV line. Because the velocity width is narrower than that of the broad Hα line of ∼2750 km s−1, we can exclude a large contribution to the line flux from the accretion disk and the broad line region. Furthermore, we performed pixel map analyses on the Hitomi/SXS data and image analyses on the Chandra archival data, and revealed that the Fe-Kα line comes from a region within ∼1.6 kpc of the NGC 1275 core, where an active galactic nucleus emission dominates, rather than that from intracluster media. Therefore, we suggest that the source of the Fe-Kα line from NGC 1275 is likely a low-covering-fraction molecular torus or a rotating molecular disk which probably extends from a parsec to hundreds of parsecs scale in the active galactic nucleus system.

Published
2018
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233. Hitomi X-ray studies of giant radio pulses from the Crab pulsar*

Author

Collaboration, Hitomi, Aharonian, Felix, Akamatsu, Hiroki, Akimoto, Fumie, Allen, Steven W, Angelini, Lorella, Audard, Marc, Awaki, Hisamitsu, Axelsson, Magnus, Bamba, Aya, Bautz, Marshall W, Blandford, Roger, Brenneman, Laura W, Brown, Gregory V, Bulbul, Esra, Cackett, Edward M, Chernyakova, Maria, Chiao, Meng P, Coppi, Paolo S, Costantini, Elisa, de Plaa, Jelle, de Vries, Cor P, den Herder, Jan-Willem, Done, Chris, Dotani, Tadayasu, Ebisawa, Ken, Eckart, Megan E, Enoto, Teruaki, Ezoe, Yuichiro, Fabian, Andrew C, Ferrigno, Carlo, Foster, Adam R, Fujimoto, Ryuichi, Fukazawa, Yasushi, Furuzawa, Akihiro, Galeazzi, Massimiliano, Gallo, Luigi C, Gandhi, Poshak, Giustini, Margherita, Goldwurm, Andrea, Gu, Liyi, Guainazzi, Matteo, Haba, Yoshito, Hagino, Kouichi, Hamaguchi, Kenji, Harrus, Ilana M, Hatsukade, Isamu, Hayashi, Katsuhiro, Hayashi, Takayuki, Hayashida, Kiyoshi, Hiraga, Junko S, Hornschemeier, Ann, Hoshino, Akio, Hughes, John P, Ichinohe, Yuto, Iizuka, Ryo, Inoue, Hajime, Inoue, Yoshiyuki, Ishida, Manabu, Ishikawa, Kumi, Ishisaki, Yoshitaka, Iwai, Masachika, Kaastra, Jelle, Kallman, Tim, Kamae, Tsuneyoshi, Kataoka, Jun, Katsuda, Satoru, Kawai, Nobuyuki, Kelley, Richard L, Kilbourne, Caroline A, Kitaguchi, Takao, Kitamoto, Shunji, Kitayama, Tetsu, Kohmura, Takayoshi, Kokubun, Motohide, Koyama, Katsuji, Koyama, Shu, Kretschmar, Peter, Krimm, Hans A, Kubota, Aya, Kunieda, Hideyo, Laurent, Philippe, Lee, Shiu-Hang, Leutenegger, Maurice A, Limousin, Olivier O, Loewenstein, Michael, Long, Knox S, Lumb, David, Madejski, Greg, Maeda, Yoshitomo, Maier, Daniel, Makishima, Kazuo, Markevitch, Maxim, Matsumoto, Hironori, Matsushita, Kyoko, McCammon, Dan, McNamara, Brian R, Mehdipour, Missagh, Miller, Eric D, Miller, Jon M, Mineshige, Shin, Mitsuda, Kazuhisa, Mitsuishi, Ikuyuki, Miyazawa, Takuya, Mizuno, Tsunefumi, Mori, Hideyuki, Mori, Koji, Mukai, Koji, Murakami, Hiroshi, Mushotzky, Richard F, Nakagawa, Takao, Nakajima, Hiroshi, Nakamori, Takeshi, Nakashima, Shinya, Nakazawa, Kazuhiro, Nobukawa, Kumiko K, Nobukawa, Masayoshi, Noda, Hirofumi, Odaka, Hirokazu, Ohashi, Takaya, Ohno, Masanori, Okajima, Takashi, Oshimizu, Kenya, Ota, Naomi, Ozaki, Masanobu, Paerels, Frits, Paltani, Stéphane, Petre, Robert, Pinto, Ciro, Porter, Frederick S, Pottschmidt, Katja, Reynolds, Christopher S, Safi-Harb, Samar, Saito, Shinya, Sakai, Kazuhiro, Sasaki, Toru, Sato, Goro, Sato, Kosuke, Sato, Rie, Sawada, Makoto, Schartel, Norbert, Serlemtsos, Peter J, Seta, Hiromi, Shidatsu, Megumi, Simionescu, Aurora, Smith, Randall K, Soong, Yang, Stawarz, Łukasz, Sugawara, Yasuharu, Sugita, Satoshi, Szymkowiak, Andrew, Tajima, Hiroyasu, Takahashi, Hiromitsu, Takahashi, Tadayuki, Takeda, Shiníchiro, Takei, Yoh, Tamagawa, Toru, Tamura, Takayuki, Tanaka, Takaaki, Tanaka, Yasuo, Tanaka, Yasuyuki T, Tashiro, Makoto S, Tawara, Yuzuru, Terada, Yukikatsu, Terashima, Yuichi, Tombesi, Francesco, Tomida, Hiroshi, Tsuboi, Yohko, Tsujimoto, Masahiro, Tsunemi, Hiroshi, Tsuru, Takeshi Go, Uchida, Hiroyuki, Uchiyama, Hideki, Uchiyama, Yasunobu, Ueda, Shutaro, Ueda, Yoshihiro, Uno, Shiníchiro, Urry, C Megan, Ursino, Eugenio, Watanabe, Shin, Werner, Norbert, Wilkins, Dan R, Williams, Brian J, Yamada, Shinya, Yamaguchi, Hiroya, Yamaoka, Kazutaka, Yamasaki, Noriko Y, Yamauchi, Makoto, Yamauchi, Shigeo, Yaqoob, Tahir, Yatsu, Yoichi, Yonetoku, Daisuke, Zhuravleva, Irina, Zoghbi, Abderahmen, Terasawa, Toshio, Sekido, Mamoru, Takefuji, Kazuhiro, Kawai, Eiji, Misawa, Hiroaki, Tsuchiya, Fuminori, Yamazaki, Ryo, Kobayashi, Eiji, Kisaka, Shota, and Aoki, Takahiro

Abstract

To search for giant X-ray pulses correlated with the giant radio pulses (GRPs) from the Crab pulsar, we performed a simultaneous observation of the Crab pulsar with the X-ray satellite Hitomi in the 2–300 keV band and the Kashima NICT radio telescope in the 1.4–1.7 GHz band with a net exposure of about 2 ks on 2016 March 25, just before the loss of the Hitomi mission. The timing performance of the Hitomi instruments was confirmed to meet the timing requirement and about 1000 and 100 GRPs were simultaneously observed at the main pulse and inter-pulse phases, respectively, and we found no apparent correlation between the giant radio pulses and the X-ray emission in either the main pulse or inter-pulse phase. All variations are within the 2 σ fluctuations of the X-ray fluxes at the pulse peaks, and the 3 σ upper limits of variations of main pulse or inter-pulse GRPs are 22% or 80% of the peak flux in a 0.20 phase width, respectively, in the 2–300 keV band. The values for main pulse or inter-pulse GRPs become 25% or 110%, respectively, when the phase width is restricted to the 0.03 phase. Among the upper limits from the Hitomi satellite, those in the 4.5–10 keV and 70–300 keV bands are obtained for the first time, and those in other bands are consistent with previous reports. Numerically, the upper limits of the main pulse and inter-pulse GRPs in the 0.20 phase width are about (2.4 and 9.3) × 10−11erg cm−2, respectively. No significant variability in pulse profiles implies that the GRPs originated from a local place within the magnetosphere. Although the number of photon-emitting particles should temporarily increase to account for the brightening of the radio emission, the results do not statistically rule out variations correlated with the GRPs, because the possible X-ray enhancement may appear due to a >0.02% brightening of the pulse-peak flux under such conditions.

Published
2018
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234. Hitomi observations of the LMC SNR N 132 D: Highly redshifted X-ray emission from iron ejecta*

Author

Collaboration, Hitomi, Aharonian, Felix, Akamatsu, Hiroki, Akimoto, Fumie, Allen, Steven W, Angelini, Lorella, Audard, Marc, Awaki, Hisamitsu, Axelsson, Magnus, Bamba, Aya, Bautz, Marshall W, Blandford, Roger, Brenneman, Laura W, Brown, Gregory V, Bulbul, Esra, Cackett, Edward M, Chernyakova, Maria, Chiao, Meng P, Coppi, Paolo S, Costantini, Elisa, de Plaa, Jelle, de Vries, Cor P, den Herder, Jan-Willem, Done, Chris, Dotani, Tadayasu, Ebisawa, Ken, Eckart, Megan E, Enoto, Teruaki, Ezoe, Yuichiro, Fabian, Andrew C, Ferrigno, Carlo, Foster, Adam R, Fujimoto, Ryuichi, Fukazawa, Yasushi, Furuzawa, Akihiro, Galeazzi, Massimiliano, Gallo, Luigi C, Gandhi, Poshak, Giustini, Margherita, Goldwurm, Andrea, Gu, Liyi, Guainazzi, Matteo, Haba, Yoshito, Hagino, Kouichi, Hamaguchi, Kenji, Harrus, Ilana M, Hatsukade, Isamu, Hayashi, Katsuhiro, Hayashi, Takayuki, Hayashida, Kiyoshi, Hiraga, Junko S, Hornschemeier, Ann, Hoshino, Akio, Hughes, John P, Ichinohe, Yuto, Iizuka, Ryo, Inoue, Hajime, Inoue, Yoshiyuki, Ishida, Manabu, Ishikawa, Kumi, Ishisaki, Yoshitaka, Iwai, Masachika, Kaastra, Jelle, Kallman, Tim, Kamae, Tsuneyoshi, Kataoka, Jun, Katsuda, Satoru, Kawai, Nobuyuki, Kelley, Richard L, Kilbourne, Caroline A, Kitaguchi, Takao, Kitamoto, Shunji, Kitayama, Tetsu, Kohmura, Takayoshi, Kokubun, Motohide, Koyama, Katsuji, Koyama, Shu, Kretschmar, Peter, Krimm, Hans A, Kubota, Aya, Kunieda, Hideyo, Laurent, Philippe, Lee, Shiu-Hang, Leutenegger, Maurice A, Limousin, Olivier, Loewenstein, Michael, Long, Knox S, Lumb, David, Madejski, Greg, Maeda, Yoshitomo, Maier, Daniel, Makishima, Kazuo, Markevitch, Maxim, Matsumoto, Hironori, Matsushita, Kyoko, McCammon, Dan, McNamara, Brian R, Mehdipour, Missagh, Miller, Eric D, Miller, Jon M, Mineshige, Shin, Mitsuda, Kazuhisa, Mitsuishi, Ikuyuki, Miyazawa, Takuya, Mizuno, Tsunefumi, Mori, Hideyuki, Mori, Koji, Mukai, Koji, Murakami, Hiroshi, Mushotzky, Richard F, Nakagawa, Takao, Nakajima, Hiroshi, Nakamori, Takeshi, Nakashima, Shinya, Nakazawa, Kazuhiro, Nobukawa, Kumiko K, Nobukawa, Masayoshi, Noda, Hirofumi, Odaka, Hirokazu, Ohashi, Takaya, Ohno, Masanori, Okajima, Takashi, Ota, Naomi, Ozaki, Masanobu, Paerels, Frits, Paltani, Stéphane, Petre, Robert, Pinto, Ciro, Porter, Frederick S, Pottschmidt, Katja, Reynolds, Christopher S, Safi-Harb, Samar, Saito, Shinya, Sakai, Kazuhiro, Sasaki, Toru, Sato, Goro, Sato, Kosuke, Sato, Rie, Sato, Toshiki, Sawada, Makoto, Schartel, Norbert, Serlemtsos, Peter J, Seta, Hiromi, Shidatsu, Megumi, Simionescu, Aurora, Smith, Randall K, Soong, Yang, Stawarz, Łukasz, Sugawara, Yasuharu, Sugita, Satoshi, Szymkowiak, Andrew, Tajima, Hiroyasu, Takahashi, Hiromitsu, Takahashi, Tadayuki, Takeda, Shin’ichiro, Takei, Yoh, Tamagawa, Toru, Tamura, Takayuki, Tanaka, Takaaki, Tanaka, Yasuo, Tanaka, Yasuyuki T, Tashiro, Makoto S, Tawara, Yuzuru, Terada, Yukikatsu, Terashima, Yuichi, Tombesi, Francesco, Tomida, Hiroshi, Tsuboi, Yohko, Tsujimoto, Masahiro, Tsunemi, Hiroshi, Tsuru, Takeshi Go, Uchida, Hiroyuki, Uchiyama, Hideki, Uchiyama, Yasunobu, Ueda, Shutaro, Ueda, Yoshihiro, Uno, Shin’ichiro, Urry, C Megan, Ursino, Eugenio, Watanabe, Shin, Werner, Norbert, Wilkins, Dan R, Williams, Brian J, Yamada, Shinya, Yamaguchi, Hiroya, Yamaoka, Kazutaka, Yamasaki, Noriko Y, Yamauchi, Makoto, Yamauchi, Shigeo, Yaqoob, Tahir, Yatsu, Yoichi, Yonetoku, Daisuke, Zhuravleva, Irina, and Zoghbi, Abderahmen

Abstract

We present Hitomi observations of N 132 D, a young, X-ray bright, O-rich core-collapse supernova remnant in the Large Magellanic Cloud (LMC). Despite a very short observation of only 3.7 ks, the Soft X-ray Spectrometer (SXS) easily detects the line complexes of highly ionized S K and Fe K with 16–17 counts in each. The Fe feature is measured for the first time at high spectral resolution. Based on the plausible assumption that the Fe K emission is dominated by He-like ions, we find that the material responsible for this Fe emission is highly redshifted at ∼ 800 km s−1compared to the local LMC interstellar medium (ISM), with a 90% credible interval of 50–1500 km s−1if a weakly informative prior is placed on possible line broadening. This indicates (1) that the Fe emission arises from the supernova ejecta, and (2) that these ejecta are highly asymmetric, since no blueshifted component is found. The S K velocity is consistent with the local LMC ISM, and is likely from swept-up ISM material. These results are consistent with spatial mapping that shows the He-like Fe concentrated in the interior of the remnant and the S tracing the outer shell. The results also show that even with a very small number of counts, direct velocity measurements from Doppler-shifted lines detected in extended objects like supernova remnants are now possible. Thanks to the very low SXS background of ∼ 1 event per spectral resolution element per 100 ks, such results are obtainable during short pointed or slew observations with similar instruments. This highlights the power of high-spectral-resolution imaging observations, and demonstrates the new window that has been opened with Hitomi and will be greatly widened with future missions such as the X-ray Astronomy Recovery Mission (XARM) and Athena.

Published
2018
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235. In-flight calibration of Hitomi Soft X-ray Spectrometer. (1) Background

Author

Kilbourne, Caroline A, Sawada, Makoto, Tsujimoto, Masahiro, Angellini, Lorella, Boyce, Kevin R, Eckart, Megan E, Fujimoto, Ryuichi, Ishisaki, Yoshitaka, Kelley, Richard L, Koyama, Shu, Leutenegger, Maurice A, Loewenstein, Michael, McCammon, Dan, Mitsuda, Kazuhisa, Nakashima, Shinya, Porter, Frederick S, Seta, Hiromi, Takei, Yoh, Tashiro, Makoto S, Terada, Yukikatsu, Yamada, Shinya, and Yamasaki, Noriko Y

Abstract

The X-Ray Spectrometer (XRS) instrument of Suzaku provided the first measurement of the non-X-ray background (NXB) of an X-ray calorimeter spectrometer, but the data set was limited. The Soft X-ray Spectrometer (SXS) instrument of Hitomi was able to provide a more detailed picture of X-ray calorimeter background, with more than 360 ks of data while pointed at the Earth, and a comparable amount of blank-sky data. These data are important not only for analyzing SXS science data, but also for categorizing the contributions to the NXB in X-ray calorimeters as a class. In this paper, we present the contributions to the SXS NXB, the types and effectiveness of the screening, the interaction of the screening with the broad-band redistribution, and the residual background spectrum as a function of magnetic cut-off rigidity. The orbit-averaged SXS NXB in the range 0.3–12 keV was 4 × 10−2counts s−1cm−2. This very low background in combination with groundbreaking spectral resolution gave SXS unprecedented sensitivity to weak spectral lines.

Published
2018
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236. Optimal filtering of overlapped pulses in microcalorimeter data.

Author

Wulf, Dallas, Jaeckel, Felix, McCammon, Dan, Chervenak, James A, and Eckart, Megan E

Subjects
*PHOTON counting, *ALGORITHMS, *ELECTRONIC data processing, *FILTERS & filtration
Abstract

In this study, we present a general algorithm for processing microcalorimeter data with special applicability to data with high photon count rates. Conventional optimal filtering, which has become ubiquitous in microcalorimeter data processing, suffers from its inability to recover overlapped pulses without sacrificing spectral resolution. The technique presented here was developed to address this particular shortcoming and does so without imposing any assumptions beyond those made by the conventional technique. We demonstrate the performance of the algorithm with a dataset that approximately satisfies these assumptions and which is representative of a wide range of microcalorimeter applications. We also apply the technique to a highly non-linear dataset, examining the impact on performance in the limit that these assumptions break down. [ABSTRACT FROM AUTHOR]

Published
2020
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237. High-resolution Laboratory Measurements of K-shell X-Ray Line Polarization and Excitation Cross Sections in Helium-like S XV Ions.

Author

Shah, Chintan, Hell, Natalie, Hubbard, Antonia, Gu, Ming Feng, MacDonald, Michael J., Eckart, Megan E., Kelley, Richard L., Kilbourne, Caroline A., Leutenegger, Maurice A., Porter, F. Scott, and Brown, Gregory V.

Subjects
*ELECTRON capture, *INNER-shell ionization, *ELECTRON beams, *LINEAR polarization, *ION traps, *X-rays
Abstract

We report measurements of electron-impact excitation cross sections for the strong K-shell n = 2 → 1 transitions in S xv, using the LLNL EBIT-I electron beam ion trap, two crystal spectrometers, and the EBIT Calorimeter Spectrometer. The cross sections are determined by direct normalization to the well-known cross sections of radiative electron capture, measured simultaneously. Using contemporaneous polarization measurements with the two crystal spectrometers, whose dispersion planes are oriented parallel and perpendicular to the electron beam direction, the polarization of the direct excitation line emission is determined, and in turn the isotropic total cross sections are extracted. We further experimentally investigate various line-formation mechanisms, finding that radiative cascades and collisional inner-shell ionization dominate the degree of linear polarization and total line-emission cross sections of the forbidden line, z. [ABSTRACT FROM AUTHOR]

Published
2021
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238. Design of Magnetic Shielding and Field Coils for a TES X-ray Microcalorimeter Test Platform.

Author

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

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

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

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

Author

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

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

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

Published
2018
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240. Reduced-Scale Transition-Edge Sensor Detectors for Solar and X-Ray Astrophysics.

Author

Datesman, Aaron M., Adams, Joseph S., Bandler, Simon R., Betancourt-Martinez, Gabriele L., Chang, Meng-Ping, Chervenak, James A., Eckart, Megan E., Ewin, Audrey E., Finkbeiner, Fred M., Ha, Jong Yoon, Kelley, Richard L., Kilbourne, Caroline A., Miniussi, Antoine R., Porter, Frederick S., Sadleir, John E., Sakai, Kazuhiro, Smith, Stephen J., Wakeham, Nicholas A., Williams, Elissa H., and Wassell, Edward J.

Subjects
*CALORIMETER calibration, *PROXIMITY effect (Superconductivity), *CRITICAL currents, *MICROSTRIP circuits, *PHOTON detectors
Abstract

We have developed large-format, close-packed X-ray microcalorimeter arrays fabricated on solid substrates, designed to achieve high energy resolution with count rates up to a few hundred counts per second per pixel for X-ray photon energies up to 8 keV. Our most recent arrays feature 31-micron absorbers on a 35-micron pitch, reducing the size of pixels by about a factor of two. This change will enable an instrument with significantly higher angular resolution. In order to wire out large format arrays with an increased density of smaller pixels, we have reduced the lateral size of both the microstrip wiring and the Mo/Au transition-edge sensors (TES). We report on the key physical properties of these small TESs and the fine Nb leads attached, including the critical currents and weak-link properties associated with the longitudinal proximity effect. [ABSTRACT FROM PUBLISHER]

Published
2017
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241. The Magnetically-Tuned Transition-Edge Sensor.

Author

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

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

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

Published
2014
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242. Testing the X-IFU calibration requirements: an example for quantum efficiency and energy resolution

Author

Gabriele Betancourt-Martinez, Simon R. Bandler, Didier Barret, Stephen J. Smith, Marco Barbera, Etienne Pointecouteau, Megan E. Eckart, François Pajot, Edoardo Cucchetti, Massimo Cappi, Philippe Peille, Caroline A. Kilbourne, Institut de recherche en astrophysique et planétologie (IRAP), Institut national des sciences de l'Univers (INSU - CNRS)-Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Observatoire Midi-Pyrénées (OMP), Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Centre National de la Recherche Scientifique (CNRS), Centre National d'Études Spatiales [Toulouse] (CNES), Lawrence Livermore National Laboratory (LLNL), Cucchetti, Edoardo, Pajot, Françoi, Pointecouteau, Etienne, Peille, Philippe, Betancourt-Martinez, Gabriele, Smith, Stephen J., Barbera, Marco, Eckart, Megan E., Bandler, Simon R., Kilbourne, Caroline A., Cappi, Massimo, and Barret, Didier

Subjects
Field (physics), FOS: Physical sciences, Condensed Matter Physic, 01 natural sciences, 7. Clean energy, X-ray, Settore FIS/05 - Astronomia E Astrofisica, Band-pass filter, 0103 physical sciences, Calibration, Athena, Electrical and Electronic Engineering, 010306 general physics, 010303 astronomy & astrophysics, Instrumentation and Methods for Astrophysics (astro-ph.IM), ComputingMilieux_MISCELLANEOUS, Physics, X-IFU, [SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph], Electronic, Optical and Magnetic Material, Detector, Astrophysics::Instrumentation and Methods for Astrophysics, Computer Science Applications1707 Computer Vision and Pattern Recognition, Filter (signal processing), Computational physics, Applied Mathematic, Performance verification, Transmission (telecommunications), Quantum efficiency, Astrophysics - Instrumentation and Methods for Astrophysics, Energy (signal processing)
Abstract

With its array of 3840 Transition Edge Sensors (TESs) operated at 90 mK, the X-Ray Integral Field Unit (X-IFU) on board the ESA L2 mission Athena will provide spatially resolved high-resolution spectroscopy (2.5 eV FWHM up to 7 keV) over the 0.2 to 12 keV bandpass. The in-flight performance of the X-IFU will be strongly affected by the calibration of the instrument. Uncertainties in the knowledge of the overall system, from the filter transmission to the energy scale, may introduce systematic errors in the data, which could potentially compromise science objectives - notably those involving line characterisation e.g. turbulence velocity measurements - if not properly accounted for. Defining and validating calibration requirements is therefore of paramount importance. In this paper, we put forward a simulation tool based on the most up-to-date configurations of the various subsystems (e.g. filters, detector absorbers) which allows us to estimate systematic errors related to uncertainties in the instrumental response. Notably, the effect of uncertainties in the energy resolution and of the instrumental quantum efficiency on X-IFU observations is assessed, by taking as a test case the measurements of the iron K complex in the hot gas surrounding clusters of galaxies. In-flight and ground calibration of the energy resolution and the quantum efficiency is also addressed. We demonstrate that provided an accurate calibration of the instrument, such effects should be low in both cases with respect to statistics during observations., Comment: 9 pages, 4 figures, SPIE proceeding Austin 2018

Published
2018
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243. Mapping of the resistance of a superconducting transition edge sensor as a function of temperature, current, and applied magnetic field.

Author

Zhang S, Eckart ME, Jaeckel FT, Kripps KL, McCammon D, Morgan KM, and Zhou Y

Abstract

We have measured the resistance R ( T, I , B ) of a superconducting transition edge sensor over the entire transition region on a fine scale, producing a 4-dimensional map of the resistance surface. The dimensionless temperature and current sensitivities ( α ≡ ∂ log R / ∂ log T | I and β ≡ ∂ log R / ∂ log I | T ) of the TES resistance have been determined at each point. ext ) of a superconducting transition edge sensor over the entire transition region on a fine scale, producing a 4-dimensional map of the resistance surface. The dimensionless temperature and current sensitivities ( α ≡ ∂ log R / ∂ log T | I and β ≡ ∂ log R / ∂ log I | T ) of the TES resistance have been determined at each point. α and β are closely related to the sensor performance, but show a great deal of complex, large amplitude fine structure over large portions of the surface that is sensitive to the applied magnetic field. We discuss the relation of this structure to the presence of Josephson "weak link" fringes.

Published
2017
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