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1. TOI-2285b: A 1.7 Earth-radius planet near the habitable zone around a nearby M dwarf

Author

Fukui, Akihiko, Kimura, Tadahiro, Hirano, Teruyuki, Narita, Norio, Kodama, Takanori, Hori, Yasunori, Ikoma, Masahiro, Pallé, Enric, Murgas, Felipe, Parviainen, Hannu, Kawauchi, Kiyoe, Mori, Mayuko, Esparza-Borges, Emma, Bieryla, Allyson, Irwin, Jonathan, Safonov, Boris S, Stassun, Keivan G, Alvarez-Hernandez, Leticia, Béjar, Víctor J S, Casasayas-Barris, Núria, Chen, Guo, Crouzet, Nicolas, de Leon, Jerome P, Isogai, Keisuke, Kagetani, Taiki, Klagyivik, Peter, Korth, Judith, Kurita, Seiya, Kusakabe, Nobuhiko, Livingston, John, Luque, Rafael, Madrigal-Aguado, Alberto, Morello, Giuseppe, Nishiumi, Taku, Orell-Miquel, Jaume, Oshagh, Mahmoudreza, Sánchez-Benavente, Manuel, Stangret, Monika, Terada, Yuka, Watanabe, Noriharu, Zou, Yujie, Tamura, Motohide, Kurokawa, Takashi, Kuzuhara, Masayuki, Nishikawa, Jun, Omiya, Masashi, Vievard, Sébastien, Ueda, Akitoshi, Latham, David W, Quinn, Samuel N, Strakhov, Ivan S, Belinski, Alexandr A, Jenkins, Jon M, Ricker, George R, Seager, Sara, Vanderspek, Roland, Winn, Joshua N, Charbonneau, David, Ciardi, David R, Collins, Karen A, Doty, John P, Bachelet, Etienne, and Harbeck, Daniel

Abstract

We report the discovery of TOI-2285b, a sub-Neptune-sized planet transiting a nearby (42 pc) M dwarf with a period of 27.3 d. We identified the transit signal from the Transiting Exoplanet Survey Satellite photometric data, which we confirmed with ground-based photometric observations using the multiband imagers MuSCAT2 and MuSCAT3. Combining these data with other follow-up observations including high-resolution spectroscopy with the Tillinghast Reflector Echelle Spectrograph, high-resolution imaging with the SPeckle Polarimeter, and radial velocity (RV) measurements with the InfraRed Doppler instrument, we find that the planet has a radius of $1.74 \pm 0.08\, R_\oplus$, a mass of $\lt \!\!19.5\,M_\oplus$($95\%$c.l.), and an insolation flux of 1.54 ± 0.14 times that of the Earth. Although the planet resides just outside the habitable zone for a rocky planet, if the planet harbors an H2O layer under a hydrogen-rich atmosphere, then liquid water could exist on the surface of the H2O layer depending on the planetary mass and water mass fraction. The bright host star in the near-infrared (Ks= 9.0) makes this planet an excellent target for further RV and atmospheric observations to improve our understanding of the composition, formation, and habitability of sub-Neptune-sized planets.

Published
2022
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2. Impact of Chemoprophylaxis on Thromboembolism Following Operative Fixation of Pelvic Fractures

Author

Berning, Bennett J., Magnotti, Louis J., Lewis, Richard H., Corley, Catherine E., Lim, Garrett H., Doty, John B., Fabian, Timothy C., Croce, Martin A., and Sharpe, John P.

Abstract

Background Venous thromboembolism (VTE) is a common cause of serious morbidity and mortality. While chemoprophylaxis decreases VTE, there is the theoretical risk of increased hemorrhagic complications. The purpose of this study was to evaluate the impact of preoperative anticoagulation on VTE and bleeding complications in patients with blunt pelvic fractures requiring operative fixation.Methods Patients with blunt pelvic fractures requiring operative fixation over 10.5 years were identified. Patients were stratified by age, severity of shock, operative management, and timing and duration of anticoagulation. Outcomes were evaluated to determine risk factors for bleeding complications and VTE.Results 310 patients were identified: 212 patients received at least one dose of preoperative anticoagulation and 98 received no preoperative anticoagulation. 68% were male with a mean injury severity score and Glasgow Coma Scale of 26 and 13, respectively. Bleeding complications occurred in 24 patients and 21 patients suffered VTE. Patients with VTE had a greater initial severity of shock (resuscitation transfusions, 4 vs. 2 units, P= .02). Despite longer time to mobilization (4 vs. 3 days, P= .001), patients who received their scheduled preoperative doses within 48 hours of arrival had no significant differences in the number of deep vein thrombosis events (5.2% vs. 5.7%, P= .99), but fewer episodes of pulmonary embolism (PE) (1.5% vs. 6.8%, P= .03) with no difference in bleeding complications (7.5% vs. 8%, P= .87) compared to either patients who had their doses held until after 48 hours of arrival or received no preoperative anticoagulation.Discussion Preoperative anticoagulation prior to pelvic fixation reduced the risk of PE without increasing bleeding complications. Preoperative anticoagulation is safe and beneficial in this group of patients.

Published
2022
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3. Impact of a focused review course in cardiovascular and thoracic surgery on test performance

Author

Doty, John R., Nguyen, Michael, Snyder, Richard J., McCann, Ulysse G., and Doty, Donald B.

Abstract

The Core Curriculum Review Course in Cardiovascular and Thoracic Surgery is a 4-day educational program consisting of 77 didactic lectures that provide a comprehensive review of the material required for surgeons preparing for the American Board of Thoracic Surgery competency written examination. The lectures are supplemented with a written syllabus and interactive audience participation system. We sought to determine whether participation in this course could improve participants' performance on a cardiothoracic subject-based test.

Published
2021
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4. A giant planet candidate transiting a white dwarf

Author

Vanderburg, Andrew, Rappaport, Saul A., Xu, Siyi, Crossfield, Ian J. M., Becker, Juliette C., Gary, Bruce, Murgas, Felipe, Blouin, Simon, Kaye, Thomas G., Palle, Enric, Melis, Carl, Morris, Brett M., Kreidberg, Laura, Gorjian, Varoujan, Morley, Caroline V., Mann, Andrew W., Parviainen, Hannu, Pearce, Logan A., Newton, Elisabeth R., Carrillo, Andreia, Zuckerman, Ben, Nelson, Lorne, Zeimann, Greg, Brown, Warren R., Tronsgaard, René, Klein, Beth, Ricker, George R., Vanderspek, Roland K., Latham, David W., Seager, Sara, Winn, Joshua N., Jenkins, Jon M., Adams, Fred C., Benneke, Björn, Berardo, David, Buchhave, Lars A., Caldwell, Douglas A., Christiansen, Jessie L., Collins, Karen A., Colón, Knicole D., Daylan, Tansu, Doty, John, Doyle, Alexandra E., Dragomir, Diana, Dressing, Courtney, Dufour, Patrick, Fukui, Akihiko, Glidden, Ana, Guerrero, Natalia M., Guo, Xueying, Heng, Kevin, Henriksen, Andreea I., Huang, Chelsea X., Kaltenegger, Lisa, Kane, Stephen R., Lewis, John A., Lissauer, Jack J., Morales, Farisa, Narita, Norio, Pepper, Joshua, Rose, Mark E., Smith, Jeffrey C., Stassun, Keivan G., and Yu, Liang

Abstract

Astronomers have discovered thousands of planets outside the Solar System1, most of which orbit stars that will eventually evolve into red giants and then into white dwarfs. During the red giant phase, any close-orbiting planets will be engulfed by the star2, but more distant planets can survive this phase and remain in orbit around the white dwarf3,4. Some white dwarfs show evidence for rocky material floating in their atmospheres5, in warm debris disks6–9or orbiting very closely10–12, which has been interpreted as the debris of rocky planets that were scattered inwards and tidally disrupted13. Recently, the discovery of a gaseous debris disk with a composition similar to that of ice giant planets14demonstrated that massive planets might also find their way into tight orbits around white dwarfs, but it is unclear whether these planets can survive the journey. So far, no intact planets have been detected in close orbits around white dwarfs. Here we report the observation of a giant planet candidate transiting the white dwarf WD 1856+534 (TIC 267574918) every 1.4 days. We observed and modelled the periodic dimming of the white dwarf caused by the planet candidate passing in front of the star in its orbit. The planet candidate is roughly the same size as Jupiter and is no more than 14 times as massive (with 95 per cent confidence). Other cases of white dwarfs with close brown dwarf or stellar companions are explained as the consequence of common-envelope evolution, wherein the original orbit is enveloped during the red giant phase and shrinks owing to friction. In this case, however, the long orbital period (compared with other white dwarfs with close brown dwarf or stellar companions) and low mass of the planet candidate make common-envelope evolution less likely. Instead, our findings for the WD 1856+534 system indicate that giant planets can be scattered into tight orbits without being tidally disrupted, motivating the search for smaller transiting planets around white dwarfs.

Published
2020
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5. A planet within the debris disk around the pre-main-sequence star AU Microscopii

Author

Plavchan, Peter, Barclay, Thomas, Gagné, Jonathan, Gao, Peter, Cale, Bryson, Matzko, William, Dragomir, Diana, Quinn, Sam, Feliz, Dax, Stassun, Keivan, Crossfield, Ian J. M., Berardo, David A., Latham, David W., Tieu, Ben, Anglada-Escudé, Guillem, Ricker, George, Vanderspek, Roland, Seager, Sara, Winn, Joshua N., Jenkins, Jon M., Rinehart, Stephen, Krishnamurthy, Akshata, Dynes, Scott, Doty, John, Adams, Fred, Afanasev, Dennis A., Beichman, Chas, Bottom, Mike, Bowler, Brendan P., Brinkworth, Carolyn, Brown, Carolyn J., Cancino, Andrew, Ciardi, David R., Clampin, Mark, Clark, Jake T., Collins, Karen, Davison, Cassy, Foreman-Mackey, Daniel, Furlan, Elise, Gaidos, Eric J., Geneser, Claire, Giddens, Frank, Gilbert, Emily, Hall, Ryan, Hellier, Coel, Henry, Todd, Horner, Jonathan, Howard, Andrew W., Huang, Chelsea, Huber, Joseph, Kane, Stephen R., Kenworthy, Matthew, Kielkopf, John, Kipping, David, Klenke, Chris, Kruse, Ethan, Latouf, Natasha, Lowrance, Patrick, Mennesson, Bertrand, Mengel, Matthew, Mills, Sean M., Morton, Tim, Narita, Norio, Newton, Elisabeth, Nishimoto, America, Okumura, Jack, Palle, Enric, Pepper, Joshua, Quintana, Elisa V., Roberge, Aki, Roccatagliata, Veronica, Schlieder, Joshua E., Tanner, Angelle, Teske, Johanna, Tinney, C. G., Vanderburg, Andrew, von Braun, Kaspar, Walp, Bernie, Wang, Jason, Wang, Sharon Xuesong, Weigand, Denise, White, Russel, Wittenmyer, Robert A., Wright, Duncan J., Youngblood, Allison, Zhang, Hui, and Zilberman, Perri

Abstract

AU Microscopii (AU Mic) is the second closest pre-main-sequence star, at a distance of 9.79 parsecs and with an age of 22 million years1. AU Mic possesses a relatively rare2and spatially resolved3edge-on debris disk extending from about 35 to 210 astronomical units from the star4, and with clumps exhibiting non-Keplerian motion5–7. Detection of newly formed planets around such a star is challenged by the presence of spots, plage, flares and other manifestations of magnetic ‘activity’ on the star8,9. Here we report observations of a planet transiting AU Mic. The transiting planet, AU Mic b, has an orbital period of 8.46 days, an orbital distance of 0.07 astronomical units, a radius of 0.4 Jupiter radii, and a mass of less than 0.18 Jupiter masses at 3σconfidence. Our observations of a planet co-existing with a debris disk offer the opportunity to test the predictions of current models of planet formation and evolution.

Published
2020
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6. Electromagnetic Navigation Bronchoscopy for Peripheral Pulmonary Lesions: One-Year Results of the Prospective, Multicenter NAVIGATE Study

Author

Folch, Erik E., Pritchett, Michael A., Nead, Michael A., Bowling, Mark R., Murgu, Septimiu D., Krimsky, William S., Murillo, Boris A., LeMense, Gregory P., Minnich, Douglas J., Bansal, Sandeep, Ellis, Blesilda Q., Mahajan, Amit K., Gildea, Thomas R., Bechara, Rabih I., Sztejman, Eric, Flandes, Javier, Rickman, Otis B., Benzaquen, Sadia, Hogarth, D. Kyle, Linden, Philip A., Wahidi, Momen M., Mattingley, Jennifer S., Hood, Kristin L., Lin, Haiying, Wolvers, Jennifer J., Khandhar, Sandeep J., Anciano, Carlos, Aragaki, Alejandro, Arenberg, Douglas, Awais, Omar, Balestra, Ricardo, Bansal, Sandeep, Barisione, Emanuela, Bechara, Rabih, Benzaquen, Sadia, Bezzi, Michela, Bhadra, Krishnendu, Bird, Julio, Blanco, Alessandro, Bowling, Mark, Cerfolio, Robert, Christensen, Merete, Cicenia, Joseph, Courey, Antony, Doty, John, Eggleston, Kevin, Ellis, Blesilda, Fernandez, Iker, Flandes, Javier, Folch, Erik, Furman, Alexandre, Gass, George David, Gildea, Thomas, Gogineni, Anil, Grabcanovic, Musija Fikreta, Hinze, John David, Hogarth, David Kyle, Karunakara, Raj, Kazakov, Jordan, Khandhar, Sandeep, Khurana, Sandhya, Krimsky, William, Krishna, Ganesh, Krol, Roman, Kropfmüller, Roland, Lamprecht, Bernd, Lau, Kelvin, Lee, Andrew, LeMense, Gregory, Linden, Philip, Lutz, Peter, Mahajan, Amit, Mahmood, Kamran, Maldonado, Fabien, Martinez, Rafael, Mattingley, Jennifer, Minnich, Douglas, Murgu, Septimiu, Murillo, Boris, Nason, Katie, Nead, Michael, Parks, Christopher, Perret, Kenneth, Porsch, Peter, Pritchett, Michael, Rickman, Otis, Rosario, Maydee, Salio, Mario, Sarkar, Saiyad, Seevaratnam, Andrew, Sethi, Sonali, Singh, Jaspal, Studnicka, Michael, Sztejman, Eric, Takubo, Tamejiro, Teba, Catalina, Towe, Christopher, Trigiani, Marco, Vergnon, JeanRichel, Viby, Niels-Erik, Wahidi, Momen, Waller, Ernest, Wei, Benjamin, Zanchi, Dragos, and Zgoda, Michael

Abstract

Electromagnetic navigation bronchoscopy (ENB) is a minimally invasive technology that guides endoscopic tools to pulmonary lesions. ENB has been evaluated primarily in small, single-center studies; thus, the diagnostic yield in a generalizable setting is unknown.

Published
2019
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7. Fast simulation of the NICER instrument

Author

den Herder, Jan-Willem A., Takahashi, Tadayuki, Bautz, Marshall, Doty, John P., Wampler-Doty, Matthew P., Prigozhin, Gregory Y., Okajima, Takashi, Arzoumanian, Zaven, and Gendreau, Keith

Published
2016
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8. NICER instrument detector subsystem: description and performance

Author

den Herder, Jan-Willem A., Takahashi, Tadayuki, Bautz, Marshall, Prigozhin, Gregory, Gendreau, Keith, Doty, John P., Foster, Richard, Remillard, Ronald, Malonis, Andrew, LaMarr, Beverly, Vezie, Michael, Egan, Mark, Villasenor, Jesus, Arzoumanian, Zaven, Baumgartner, Wayne, Scholze, Frank, Laubis, Christian, Krumrey, Michael, and Huber, Alan

Published
2016
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9. The Neutron star Interior Composition Explorer (NICER): design and development

Author

den Herder, Jan-Willem A., Takahashi, Tadayuki, Bautz, Marshall, Gendreau, Keith C., Arzoumanian, Zaven, Adkins, Phillip W., Albert, Cheryl L., Anders, John F., Aylward, Andrew T., Baker, Charles L., Balsamo, Erin R., Bamford, William A., Benegalrao, Suyog S., Berry, Daniel L., Bhalwani, Shiraz, Black, J. Kevin, Blaurock, Carl, Bronke, Ginger M., Brown, Gary L., Budinoff, Jason G., Cantwell, Jeffrey D., Cazeau, Thoniel, Chen, Philip T., Clement, Thomas G., Colangelo, Andrew T., Coleman, Jerry S., Coopersmith, Jonathan D., Dehaven, William E., Doty, John P., Egan, Mark D., Enoto, Teruaki, Fan, Terry W., Ferro, Deneen M., Foster, Richard, Galassi, Nicholas M., Gallo, Luis D., Green, Chris M., Grosh, Dave, Ha, Kong Q., Hasouneh, Monther A., Heefner, Kristofer B., Hestnes, Phyllis, Hoge, Lisa J., Jacobs, Tawanda M., Jørgensen, John L., Kaiser, Michael A., Kellogg, James W., Kenyon, Steven J., Koenecke, Richard G., Kozon, Robert P., LaMarr, Beverly, Lambertson, Mike D., Larson, Anne M., Lentine, Steven, Lewis, Jesse H., Lilly, Michael G., Liu, Kuochia Alice, Malonis, Andrew, Manthripragada, Sridhar S., Markwardt, Craig B., Matonak, Bryan D., Mcginnis, Isaac E., Miller, Roger L., Mitchell, Alissa L., Mitchell, Jason W., Mohammed, Jelila S., Monroe, Charles A., Montt de Garcia, Kristina M., Mulé, Peter D., Nagao, Louis T., Ngo, Son N., Norris, Eric D., Norwood, Dwight A., Novotka, Joseph, Okajima, Takashi, Olsen, Lawrence G., Onyeachu, Chimaobi O., Orosco, Henry Y., Peterson, Jacqualine R., Pevear, Kristina N., Pham, Karen K., Pollard, Sue E., Pope, John S., Powers, Daniel F., Powers, Charles E., Price, Samuel R., Prigozhin, Gregory Y., Ramirez, Julian B., Reid, Winston J., Remillard, Ronald A., Rogstad, Eric M., Rosecrans, Glenn P., Rowe, John N., Sager, Jennifer A., Sanders, Claude A., Savadkin, Bruce, Saylor, Maxine R., Schaeffer, Alexander F., Schweiss, Nancy S., Semper, Sean R., Serlemitsos, Peter J., Shackelford, Larry V., Soong, Yang, Struebel, Jonathan, Vezie, Michael L., Villasenor, Joel S., Winternitz, Luke B., Wofford, George I., Wright, Michael R., Yang, Mike Y., and Yu, Wayne H.

Published
2016
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10. The ASTRO-H (Hitomi) x-ray astronomy satellite

Author

den Herder, Jan-Willem A., Takahashi, Tadayuki, Bautz, Marshall, Takahashi, Tadayuki, Kokubun, Motohide, Mitsuda, Kazuhisa, Kelley, Richard, Ohashi, Takaya, Aharonian, Felix, Akamatsu, Hiroki, Akimoto, Fumie, Allen, Steve, Anabuki, Naohisa, Angelini, Lorella, Arnaud, Keith, Asai, Makoto, Audard, Marc, Awaki, Hisamitsu, Axelsson, Magnus, Azzarello, Philipp, Baluta, Chris, Bamba, Aya, Bando, Nobutaka, Bautz, Marshall, Bialas, Thomas, Blandford, Roger, Boyce, Kevin, Brenneman, Laura, Brown, Greg, Bulbul, Esra, Cackett, Edward, Canavan, Edgar, Chernyakova, Maria, Chiao, Meng, Coppi, Paolo, Costantini, Elisa, de Plaa, Jelle, den Herder, Jan-Willem, DiPirro, Michael, Done, Chris, Dotani, Tadayasu, Doty, John, Ebisawa, Ken, Eckart, Megan, Enoto, Teruaki, Ezoe, Yuichiro, Fabian, Andrew, Ferrigno, Carlo, Foster, Adam, Fujimoto, Ryuichi, Fukazawa, Yasushi, Furuzawa, Akihiro, Galeazzi, Massimiliano, Gallo, Luigi, Gandhi, Poshak, Gilmore, Kirk, Giustini, Margherita, Goldwurm, Andrea, Gu, Liyi, Guainazzi, Matteo, Haas, Daniel, Haba, Yoshito, Hagino, Kouichi, Hamaguchi, Kenji, Harayama, Atsushi, Harrus, Ilana, Hatsukade, Isamu, Hayashi, Takayuki, Hayashi, Katsuhiro, Hayashida, Kiyoshi, Hiraga, Junko, Hirose, Kazuyuki, Hornschemeier, Ann, Hoshino, Akio, Hughes, John, Ichinohe, Yuto, Iizuka, Ryo, Inoue, Yoshiyuki, Inoue, Hajime, Ishibashi, Kazunori, Ishida, Manabu, Ishikawa, Kumi, Ishimura, Kosei, Ishisaki, Yoshitaka, Itoh, Masayuki, Iwata, Naoko, Iyomoto, Naoko, Jewell, Chris, Kaastra, Jelle, Kallman, Timothy, Kamae, Tuneyoshi, Kara, Erin, Kataoka, Jun, Katsuda, Satoru, Katsuta, Junichiro, Kawaharada, Madoka, Kawai, Nobuyuki, Kawano, Taro, Kawasaki, Shigeo, Khangulyan, Dmitry, Kilbourne, Caroline, Kimball, Mark, King, Ashley, Kitaguchi, Takao, Kitamoto, Shunji, Kitayama, Tetsu, Kohmura, Takayoshi, Kosaka, Tatsuro, Koujelev, Alex, Koyama, Katsuji, Koyama, Shu, Kretschmar, Peter, Krimm, Hans, Kubota, Aya, Kunieda, Hideyo, Laurent, Philippe, Lebrun, François, Lee, Shiu-Huang, Leutenegger, Maurice, Limousin, Olivier, Loewenstein, Michael, Long, Knox, Lumb, David, Madejski, Grzegorz, Maeda, Yoshitomo, Maier, Daniel, Makishima, Kazuo, Markevitch, Maxim, Masters, Candace, Matsumoto, Hironori, Matsushita, Kyoko, McCammon, Dan, McGuinness, Daniel, McNamara, Brian, Mehdipour, Missagh, Miko, Joseph, Miller, Jon, Miller, Eric, Mineshige, Shin, Minesugi, Kenji, Mitsuishi, Ikuyuki, Miyazawa, Takuya, Mizuno, Tsunefumi, Mori, Koji, Mori, Hideyuki, Moroso, Franco, Moseley, Harvey, Muench, Theodore, Mukai, Koji, Murakami, Hiroshi, Murakami, Toshio, Mushotzky, Richard, Nagano, Housei, Nagino, Ryo, Nakagawa, Takao, Nakajima, Hiroshi, Nakamori, Takeshi, Nakano, Toshio, Nakashima, Shinya, Nakazawa, Kazuhiro, Namba, Yoshiharu, Natsukari, Chikara, Nishioka, Yusuke, Nobukawa, Masayoshi, Nobukawa, Kumiko, Noda, Hirofumi, Nomachi, Masaharu, O'Dell, Steve, Odaka, Hirokazu, Ogawa, Hiroyuki, Ogawa, Mina, Ogi, Keiji, Ohno, Masanori, Ohta, Masayuki, Okajima, Takashi, Okamoto, Atsushi, Okazaki, Tsuyoshi, Ota, Naomi, Ozaki, Masanobu, Paerels, Frederik, Paltani, Stéphane, Parmar, Arvind, Petre, Robert, Pinto, Ciro, Pohl, Martin, Pontius, James, Porter, F. Scott, Pottschmidt, Katja, Ramsey, Brian, Reynolds, Christopher, Russell, Helen, Safi-Harb, Samar, Saito, Shinya, Sakai, Shin-ichiro, Sakai, Kazuhiro, Sameshima, Hiroaki, Sasaki, Toru, Sato, Goro, Sato, Yoichi, Sato, Kosuke, Sato, Rie, Sawada, Makoto, Schartel, Norbert, Serlemitsos, Peter, Seta, Hiromi, Shibano, Yasuko, Shida, Maki, Shidatsu, Megumi, Shimada, Takanobu, Shinozaki, Keisuke, Shirron, Peter, Simionescu, Aurora, Simmons, Cynthia, Smith, Randall, Sneiderman, Gary, Soong, Yang, Stawarz, Łukasz, Sugawara, Yasuharu, Sugita, Hiroyuki, Sugita, Satoshi, Szymkowiak, Andrew, Tajima, Hiroyasu, Takahashi, Hiromitsu, Takeda, Shin'ichiro, Takei, Yoh, Tamagawa, Toru, Tamura, Takayuki, Tamura, Keisuke, Tanaka, Takaaki, Tanaka, Yasuo, Tanaka, Yasuyuki, Tashiro, Makoto, Tawara, Yuzuru, Terada, Yukikatsu, Terashima, Yuichi, Tombesi, Francesco, Tomida, Hiroshi, Tsuboi, Yohko, Tsujimoto, Masahiro, Tsunemi, Hiroshi, Tsuru, Takeshi, Uchida, Hiroyuki, Uchiyama, Yasunobu, Uchiyama, Hideki, Ueda, Yoshihiro, Ueda, Shutaro, Ueno, Shiro, Uno, Shin'ichiro, Urry, Meg, Ursino, Eugenio, de Vries, Cor, Wada, Atsushi, Watanabe, Shin, Watanabe, Tomomi, Werner, Norbert, Wik, Daniel, Wilkins, Dan, Williams, Brian, Yamada, Takahiro, Yamada, Shinya, Yamaguchi, Hiroya, Yamaoka, Kazutaka, Yamasaki, Noriko, Yamauchi, Makoto, Yamauchi, Shigeo, Yaqoob, Tahir, Yatsu, Yoichi, Yonetoku, Daisuke, Yoshida, Atsumasa, Yuasa, Takayuki, Zhuravleva, Irina, and Zoghbi, Abderahmen

Published
2016
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11. The Soft X-ray Imager (SXI) for the ASTRO-H Mission

Author

Siegmund, Oswald H., Tanaka, Takaaki, Tsunemi, Hiroshi, Hayashida, Kiyoshi, Tsuru, Takeshi G., Dotani, Tadayasu, Nakajima, Hiroshi, Anabuki, Naohisa, Nagino, Ryo, Uchida, Hiroyuki, Nobukawa, Masayoshi, Ozaki, Masanobu, Natsukari, Chikara, Tomida, Hiroshi, Ueda, Shutaro, Kimura, Masashi, Hiraga, Junko S., Kohmura, Takayoshi, Murakami, Hiroshi, Mori, Koji, Yamauchi, Makoto, Hatsukade, Isamu, Nishioka, Yusuke, Bamba, Aya, and Doty, John P.

Published
2015
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12. Lactic Acidosis After Cardiac Transplantation

Author

Nixon, Jennifer L., Kfoury, Abdallah G., McCubrey, Raymond, Brunisholz, Kim, Bair, Tami, Balling, Kyle D., Budge, Deborah, Doty, John, Rasmusson, Brad, Reid, Bruce, Smith, Hildegard, Thomsen, George, Goddard, Mark, and Alharethi, Rami

Abstract

Lactic acidosis (LA) frequently occurs after heart transplantation (HTx). It is hypothesized to be related to inotropic support or metabolic derangements from chronic heart failure. As such, restoring hemodynamic stability with mechanical circulatory support before HTx should mitigate this problem. Our aim was to evaluate the incidence and outcomes of LA after HTx.

Published
2015
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14. Surgical Treatment of Isolated (Lone) Atrial Fibrillation with Gemini-S Ablation and Left Atrial Appendage Excision (GALAXY Procedure)

Author

Doty, John R. and Clayson, Stephen E.

Abstract

Objective Surgical ablation with radiofrequency is a safe and effective treatment for atrial fibrillation. Recent advances in instrumentation have allowed for the application of bipolar radiofrequency through a minimally invasive approach using small bilateral thoracotomies for pulmonary vein isolation, destruction of autonomic ganglia, and excision of the left atrial appendage (GALAXY procedure).Methods Thirty-two patients underwent surgical ablation of atrial fibrillation with the GALAXY procedure over a 43-month period. Data were collected in a prospective manner during hospitalization and at 1-, 3-, 6-, and 12-month intervals for rhythm, medications, and subsequent interventions.Results There were no operative mortality, no myocardial infarction, and no stroke. One patient required reexploration for bleeding. Mean follow-up was 28 months (range, 4–43 months). Freedom from atrial fibrillation at 12 and 24 months, respectively, was 90% and 67% for patients with paroxysmal fibrillation and 80% and 63% for patients with persistent atrial fibrillation. Of the patients who were not in sinus rhythm, four reverted to atrial fibrillation and two reverted to atrial flutter.Conclusions The GALAXY procedure is a safe and effective, minimally invasive method for treatment of isolated (lone) atrial fibrillation. The operation provides excellent short-term freedom from atrial fibrillation and should be considered in patients with isolated paroxysmal atrial fibrillation.

Published
2012
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15. Surgical Treatment of Isolated (Lone) Atrial Fibrillation with Gemini-S Ablation and Left Atrial Appendage Excision (GALAXY Procedure)

Author

Doty, John R. and Clayson, Stephen E.

Abstract

Objective Surgical ablation with radiofrequency is a safe and effective treatment for atrial fibrillation. Recent advances in instrumentation have allowed for the application of bipolar radiofrequency through a minimally invasive approach using small bilateral thoracotomies for pulmonary vein isolation, destruction of autonomic ganglia, and excision of the left atrial appendage (GALAXY procedure).Methods Thirty-two patients underwent surgical ablation of atrial fibrillation with the GALAXY procedure over a 43-month period. Data were collected in a prospective manner during hospitalization and at 1-, 3-, 6-, and 12-month intervals for rhythm, medications, and subsequent interventions.Results There were no operative mortality, no myocardial infarction, and no stroke. One patient required reexploration for bleeding. Mean follow-up was 28 months (range, 4–43 months). Freedom from atrial fibrillation at 12 and 24 months, respectively, was 90% and 67% for patients with paroxysmal fibrillation and 80% and 63% for patients with persistent atrial fibrillation. Of the patients who were not in sinus rhythm, four reverted to atrial fibrillation and two reverted to atrial flutter.Conclusions The GALAXY procedure is a safe and effective, minimally invasive method for treatment of isolated (lone) atrial fibrillation. The operation provides excellent short-term freedom from atrial fibrillation and should be considered in patients with isolated paroxysmal atrial fibrillation.

Published
2012
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16. Spectral-Lag Relations in GRB Pulses Detected with HETE-2

Author

Arimoto, Makoto, Kawai, Nobuyuki, Asano, Katsuaki, Hurley, Kevin, Suzuki, Motoko, Nakagawa, Yujin E., Shimokawabe, Takashi, Pazmino, Nicolas Vasquez, Sato, Rie, Matsuoka, Masaru, Yoshida, Atsumasa, Tamagawa, Toru, Shirasaki, Yuji, Sugita, Satoshi, Takahashi, Ichiro, Atteia, Jean-Luc, Pelangeon, Alexandre, Vanderspek, Roland, Graziani, Carlo, Prigozhin, Gregory, Villasenor, Joel, Jernigan, J. Garrett, Crew, Geoffrey B., Sakamoto, Takanori, Ricker, George R., Woosley, Stanford E., Butler, Nat, Levine, Alan, Doty, John P., Donaghy, Timothy Q., Lamb, Donald Q., Fenimore, Edward, Galassi, Mark, Boer, Michel, Dezalay, Jean-Pascal, Olive, Jean-François, Braga, João, Manchanda, Ravi, and Pizzichini, Graziella

Abstract

Using a pulse-fit method, we investigated the spectral lags between the traditional gamma-ray band (50–400 keV) and the X-ray band (6–25 keV) for 8 GRBs with known redshifts (GRB 010921, GRB 020124, GRB 020127, GRB 021211, GRB 030528, GRB 040924, GRB 041006, and GRB 050408), detected with the WXM and FREGATE instruments aboard the HETE-2 satellite. We found several relations for individual GRB pulses between the spectral lag and other observables, such as the luminosity, pulse duration, and peak energy, $E_{\rm peak}$. The obtained results are consistent with those for BATSE, indicating that the BATSE correlations are still valid at lower energies (6–25 keV). Furthermore, we found that the photon energy dependence for the spectral lags can be reconciled with the simple curvature effect model. We discuss the implications of these results from various points of view.

Published
2010
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17. HETE-2 Observations of the X-Ray Flash XRF 040916

Author

Arimoto, Makoto, Kawai, Nobuyuki, Suzuki, Motoko, Sato, Rie, Pazmino, Nicolas Vasquez, Shimokawabe, Takashi, Ishimura, Takuto, Kotoku, Jun’ichi, Yoshida, Atsumasa, Tamagawa, Toru, Shirasaki, Yuji, Matsuoka, Masaru, Nakagawa, Yujin, Ishikawa, Nobuyuki, Kobayashi, Akina, Sugita, Satoshi, Takahashi, Ichiro, Kuwahara, Makoto, Yamauchi, Makoto, Takagishi, Kunio, Hatsukade, Isamu, Atteia, Jean-Luc, Pelangeon, Alexandre, Vanderspek, Roland, Graziani, Carlo, Prigozhin, Gregory, Villasenor, Joel, Jernigan, J. Garrett, Crew, Geoffrey B., Hurley, Kevin, Sakamoto, Takanori, Ricker, George R., Woosley, Stanford E., Butler, Nat, Levine, Al, Doty, John P., Donaghy, Timothy Q., Lamb, Donald Q., Fenimore, Edward E., Galassi, Mark, Boer, Michel, Dezalay, Jean-Pascal, Olive, Jean-François, Braga, Joao, Manchanda, Ravi, and Pizzichini, Graziella

Abstract

A long X-ray flash was detected and localized by instruments aboard the High Energy Transient Explorer II (HETE-2) at 00:03:30 UT on 2004 September 16. The position was reported to the GRB Coordinates Network (GCN) approximately 2 hours after the burst. This burst consisted of two peaks separated by $\sim 200$s, with durations of about 110 s and 60 s. We analyzed the energy spectra of the 1st and 2nd peaks observed with the Wide Field X-Ray Monitor (WXM) and the French Gamma Telescope (FREGATE). We discuss the origin of the 2nd peak in terms of the flux variabilities and timescales. We find that it is most likely to be part of prompt emission, and is explained by a long-acting engine model. This feature is similar to some bright X-ray flares detected in the early afterglow phase of bursts observed by the Swift satellite.

Published
2007
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18. A Comprehensive Study of Short Bursts from SGR1806$-$20 and SGR1900$+$14 Detected by HETE-2

Author

Nakagawa, Yujin E., Yoshida, Atsumasa, Hurley, Kevin, Atteia, Jean-Luc, Maetou, Miki, Tamagawa, Toru, Suzuki, Motoko, Yamazaki, Tohru, Tanaka, Kaoru, Kawai, Nobuyuki, Shirasaki, Yuji, Pelangeon, Alexandre, Matsuoka, Masaru, Vanderspek, Roland, Crew, Geoff B., Villasenor, Joel S., Sato, Rie, Sugita, Satoshi, Kotoku, Jun’ichi, Arimoto, Makoto, Pizzichini, Graziella, Doty, John P., and Ricker, George R.

Abstract

Temporal and spectral studies of short bursts ($\lesssim$a few hundred milliseconds) are presented for the soft gamma repeaters (SGRs) 1806$-$20 and 1900$+$14 using the HETE-2 samples. In five years from 2001 to 2005, HETE-2 localized 50 bursts from SGR1806$-$20 and 5 bursts from SGR 1900 $+$14. The cumulative number–intensity distribution of SGR 1806$-$20 in the active year 2004 is well described by a power-law model with an index of $-$1.1$\pm$0.6. It is consistent with previous studies, but burst data taken in other years clearly give a steeper distribution. This may suggest that more energetic bursts could occur more frequently in periods of greater activity. From the data, the spectral evolution during bursts with a time scale of $\gtrsim$20 ms does not seem to be common in the HETE-2 sample. The spectra of all short bursts are well reproduced by a two blackbody function with temperatures of $\sim 4$and $\sim 11$keV. From a timing analysis to the SGR 1806$-$20 data, a time lag of 2.2$\pm$0.4 ms is found between the 30–100 keV and 2–10 keV radiation bands. This may imply (1) a very rapid spectral softening and energy reinjection, (2) diffused (elongated) emission plasma along the magnetic field lines in pseudo-equilibrium with multi-temperatures, or (3) a separate (located at $\lesssim$700 Km) emission region of a softer component (say, $\sim$4 keV), which could be reprocessed X-rays by higher energy ($\gtrsim$11 keV) photons from an emission region near the stellar surface.

Published
2007
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19. X-Ray Imaging Spectrometer (XIS) on Board Suzaku

Author

Koyama, Katsuji, Tsunemi, Hiroshi, Dotani, Tadayasu, Bautz, Mark W., Hayashida, Kiyoshi, Tsuru, Takeshi Go, Matsumoto, Hironori, Ogawara, Yoshiaki, Ricker, George R., Doty, John, Kissel, Steven E., Foster, Rick, Nakajima, Hiroshi, Yamaguchi, Hiroya, Mori, Hideyuki, Sakano, Masaaki, Hamaguchi, Kenji, Nishiuchi, Mamiko, Miyata, Emi, Torii, Ken’ichi, Namiki, Masaaki, Katsuda, Satoru, Matsuura, Daisuke, Miyauchi, Tomofumi, Anabuki, Naohisa, Tawa, Noriaki, Ozaki, Masanobu, Murakami, Hiroshi, Maeda, Yoshitomo, Ichikawa, Yoshinori, Prigozhin, Gregory Y., Boughan, Edward A., LaMarr, Beverly, Miller, Eric D., Burke, Barry E., Gregory, James A., Pillsbury, Allen, Bamba, Aya, Hiraga, Junko S., Senda, Atsushi, Katayama, Haruyoshi, Kitamoto, Shunji, Tsujimoto, Masahiro, Kohmura, Takayoshi, Tsuboi, Yohko, and Awaki, Hisamitsu

Abstract

The XIS is an X-ray Imaging Spectrometer system, consisting of state-of-the-art charge-coupled devices (CCDs) optimized for X-ray detection, camera bodies, and control electronics. Four sets of XIS sensors are placed at the focal planes of the grazing-incidence, nested thin-foil mirrors (XRT: X-Ray Telescope) onboard the Suzaku satellite. Three of the XIS sensors have front-illuminated CCDs, while the other has a back-illuminated CCD. Coupled with the XRT, the energy range of 0.2–12 keV with energy resolution of 130 eV at 5.9 keV, and a field of view of $18^\prime \times 18^\prime$are realized. Since the Suzaku launch on 2005 July 10, the XIS has been functioning well.

Published
2007
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20. The X-Ray Observatory Suzaku

Author

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

Abstract

High-sensitivity wide-band X-ray spectroscopy is the key feature of the Suzaku X-ray observatory, launched on 2005 July 10. This paper summarizes the spacecraft, in-orbit performance, operations, and data processing that are related to observations. The scientific instruments, the high-throughput X-ray telescopes, X-ray CCD cameras, non-imaging hard X-ray detector are also described.

Published
2007
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21. An Optically Dark GRB Observed by HETE-2: GRB 051022

Author

Nakagawa, Yujin E., Yoshida, Atsumasa, Sugita, Satoshi, Tanaka, Kaoru, Ishikawa, Nobuyuki, Tamagawa, Toru, Suzuki, Motoko, Shirasaki, Yuji, Kawai, Nobuyuki, Matsuoka, Masaru, Atteia, Jean-Luc, Pelangeon, Alexandre, Vanderspek, Roland, Crew, Geoffrey B., Villasenor, Joel S., Butler, Nat, Doty, John P., Ricker, George R., Pizzichini, Graziella, Donaghy, Timothy Q., Lamb, Donald Q., Graziani, Carlo, Sato, Rie, Maetou, Miki, Arimoto, Makoto, Kotoku, Jun’ichi, Jernigan, J. Garrett, Sakamoto, Takanori, Olive, Jean-François, Boer, Michel, Fenimore, Edward E., Galassi, Mark, Woosley, Stanford E., Yamauchi, Makoto, Takagishi, Kunio, and Hatsukade, Isamu

Abstract

GRB 051022 was detected at 13:07:58 on 2005 October 22 UT by HETE-2. The location of GRB 051022 was determined immediately by the flight localization system. This burst contained multiple pulses, and had a rather long duration of about 190 s. The detections of candidate X-ray and radio afterglows were reported, whereas no optical afterglow was found. Optical spectroscopic observations of the host galaxy revealed a redshift of $z = 0.8$. Using data derived by a HETE-2 observation of the prompt emission, we found absorption of $N_{\mathrm{H}} = (8.8_{-2.9}^{+3.1}) \times 10^{22} \,\mathrm{cm}^{-2}$and visual extinction of $A_{V} = 49_{-16}^{+17}$mag in the host galaxy. If this is the case, no detection of any optical transient would be quite reasonable. The absorption derived by Swift XRT observations of the afterglow is fully consistent with those obtained from an early HETE-2 observation of the prompt emission. Our analysis implies an interpretation that the absorbing medium may be outside the external shock at $R \sim 10^{16} \,\mathrm{cm}$, which could be a dusty molecular cloud.

Published
2006
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22. HETE-2 Localization and Observations of the Gamma-Ray Burst GRB 020813

Author

Sato, Rie, Sakamoto, Takanori, Kataoka, Jun, Yoshida, Atsumasa, Suzuki, Motoko, Kotoku, Junichi, Urata, Yuji, Yamamoto, Yoshihisa, Arimoto, Makoto, Tamagawa, Toru, Shirasaki, Yuji, Torii, Ken’ichi, Matsuoka, Masaru, Nakagawa, Yujin, Yamazaki, Toru, Tanaka, Kaoru, Maetou, Miki, Yamauchi, Makoto, Takagishi, Kunio, Lamb, Donald Q., Atteia, Jean-Luc, Vanderspek, Roland, Graziani, Carlo, Prigozhin, Gregory, Villasenor, Joel, Jernigan, J. Garrett, Crew, Geoffrey B., Hurley, Kevin, Ricker, George R., Woosley, Stanford E., Butler, Nat, Levine, Al, Doty, John P., Donaghy, Timothy Q., Fenimore, Edward E., Galassi, Mark, Boer, Michel, Dezalay, Jean-Pascal, Olive, Jean-François, Braga, Joao, Manchanda, Ravi, Pizzichini, Graziella, and Kawai, Nobuyuki

Abstract

A bright, long gamma-ray burst (GRB) was detected and localized by the instruments on board the High Energy Transient Explorer 2 satellite (HETE-2) at 02:44:19.17 UTC (9859.17 s UT) on 2002 August 13. The location was reported to the GRB Coordinates Network (GCN) about 4 min after the burst. In the prompt emission, the burst had a duration of approximately 125 s, and more than four peaks. We analyzed the time-resolved 2–400 keV energy spectra of the prompt emission of GRB 020813 using the Wide Field X-Ray Monitor (WXM) and the French Gamma Telescope (FREGATE) in detail. We found that the early part of the burst (17–52 s after the burst trigger) shows a depletion of low-energy photons below about 50 keV. It is difficult to explain the depletion by either synchrotron self-absorption or Comptonization. One possibility is that the low-energy depletion may be understood as a mixture of “jitter” radiation with the usual synchrotron radiation component.

Published
2005
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25. Bypass of superior vena cava

Author

Doty, Donald B., Doty, John R., and Jones, Kent W.

Abstract

Nine patients had operations for obstruction of the superior vena cava with superior vena caval syndrome caused by benign disease. Three patients had fibrosing mediastinitis, four had fibrosing mediastinitis with caseous necrosis, one had thrombosis of the superior vena cava around a pacemaker electrode, and one had spontaneous thrombosis of the superior vena cava. Patients ranged in age from 25 to 68 years. All bypass operations were performed with a composite spiral vein graft constructed from the patient's own saphenous vein, split longitudinally and wrapped around a stent in spiral fashion. The edges of the vein were sutured together to form a large conduit ranging in diameter from 9.5 to 15.0 mm. Six grafts were from the left innominate vein and three grafts were from the internal jugular vein. The grafts were placed into the right atrial appendage in all except one case, in which the graft was to the distal superior vena cava. Follow-up extends from 1 to 15 years. One patient required reoperation at 4 days for thrombosis at the innominate vein-graft anastomosis. Resection of the anastomosis and reconstruction of the graft rendered the patient symptom free. Two grafts closed during the first year after operation. One patient had advancing fibrosing mediastinitis, and a second bypass graft from the external jugular veins remain patent. Another patient had recurrence of spontaneous venous thrombosis. Thus seven of nine grafts remain patent for up to nearly 15 years and all but one patient is free of superior vena caval syndrome. These data show that bypass of the obstructed superior vena cava with a spiral vein graft relieves superior vena caval syndrome and demonstrate long-term patency of the graft.

Published
1990
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26. Immediate reports of GRBs in progress from HETE

Author

Vanderspek, Roland, Doty, John P., Crew, Geoffrey B., and Ricker, George R.

Abstract

The High Energy Transient Experiment (HETE) will be able to perform multiwavelength observations of?-ray and X-ray bursts. HETE will potentially be able to localize?-ray bursts to a precision of ~20 arc-minutes if significant X-ray flux is detected from the burst; a precision of ~20 arc-seconds is possible if there is also significant UV radiation from the burst. HETE will broadcast information about bursts detected within seconds of their detection. This VHF-band broadcast will be received at a number of secondary ground stations (SGS) dedicated to HETE, and forwarded to a central distribution site at MIT, from which it is sent to interested observers via Internet.

Published
1995
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27. The UV cameras on the High Energy Transient Experiment (HETE)

Author

Vanderspek, Roland, Atlas, Alia, Brady, Tye M., Crew, Geoffrey B., Doty, John P., Kissel, Steven E., Ricker, George R., Tappan, Peter C., Martel, Francois, and Tim Jones, M.

Abstract

The High Energy Transient Experiment (HETE), scheduled for launch this year, is a small satellite dedicated to multiwavelength observations of ?-ray and X-ray bursts. The HETE spacecraft will be equipped with gamma-ray detectors, X-ray detectors with a coded mask, and ultraviolet-sensitive CCD cameras. The UV cameras on HETE are wide-field imagers which will a) provide UV images of the regions in which ?-ray or X-ray bursts are detected, before, duringand after the burst, b) detect UV transients, whether associated with a high-energy transient or not, c) monitor the brightnesses of field stars for variability over a wide range of timescales, and d) serve as star trackers for HETE. In this poster, we describe the HETE UV instrumentation, control software, and data products.

Published
1995
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28. Publisher Correction: A planet within the debris disk around the pre-main-sequence star AU Microscopii

Author

Plavchan, Peter, Barclay, Thomas, Gagné, Jonathan, Gao, Peter, Cale, Bryson, Matzko, William, Dragomir, Diana, Quinn, Sam, Feliz, Dax, Stassun, Keivan, Crossfield, Ian J. M., Berardo, David A., Latham, David W., Tieu, Ben, Anglada-Escudé, Guillem, Ricker, George, Vanderspek, Roland, Seager, Sara, Winn, Joshua N., Jenkins, Jon M., Rinehart, Stephen, Krishnamurthy, Akshata, Dynes, Scott, Doty, John, Adams, Fred, Afanasev, Dennis A., Beichman, Chas, Bottom, Mike, Bowler, Brendan P., Brinkworth, Carolyn, Brown, Carolyn J., Cancino, Andrew, Ciardi, David R., Clampin, Mark, Clark, Jake T., Collins, Karen, Davison, Cassy, Foreman-Mackey, Daniel, Furlan, Elise, Gaidos, Eric J., Geneser, Claire, Giddens, Frank, Gilbert, Emily, Hall, Ryan, Hellier, Coel, Henry, Todd, Horner, Jonathan, Howard, Andrew W., Huang, Chelsea, Huber, Joseph, Kane, Stephen R., Kenworthy, Matthew, Kielkopf, John, Kipping, David, Klenke, Chris, Kruse, Ethan, Latouf, Natasha, Lowrance, Patrick, Mennesson, Bertrand, Mengel, Matthew, Mills, Sean M., Morton, Tim, Narita, Norio, Newton, Elisabeth, Nishimoto, America, Okumura, Jack, Palle, Enric, Pepper, Joshua, Quintana, Elisa V., Roberge, Aki, Roccatagliata, Veronica, Schlieder, Joshua E., Tanner, Angelle, Teske, Johanna, Tinney, C. G., Vanderburg, Andrew, von Braun, Kaspar, Walp, Bernie, Wang, Jason, Wang, Sharon Xuesong, Weigand, Denise, White, Russel, Wittenmyer, Robert A., Wright, Duncan J., Youngblood, Allison, Zhang, Hui, and Zilberman, Perri

Abstract

An amendment to this paper has been published and can be accessed via a link at the top of the paper.

Published
2020
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30. 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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31. In-orbit performance of the soft X-ray imaging system aboard Hitomi (ASTRO-H)*

Author

Nakajima, Hiroshi, Maeda, Yoshitomo, Uchida, Hiroyuki, Tanaka, Takaaki, Tsunemi, Hiroshi, Hayashida, Kiyoshi, Tsuru, Takeshi G, Dotani, Tadayasu, Nagino, Ryo, Inoue, Shota, Ozaki, Masanobu, Tomida, Hiroshi, Natsukari, Chikara, Ueda, Shutaro, Mori, Koji, Yamauchi, Makoto, Hatsukade, Isamu, Nishioka, Yusuke, Sakata, Miho, Beppu, Tatsuhiko, Honda, Daigo, Nobukawa, Masayoshi, Hiraga, Junko S, Kohmura, Takayoshi, Murakami, Hiroshi, Nobukawa, Kumiko K, Bamba, Aya, Doty, John P, Iizuka, Ryo, Sato, Toshiki, Kurashima, Sho, Nakaniwa, Nozomi, Asai, Ryota, Ishida, Manadu, Mori, Hideyuki, Soong, Yang, Okajima, Takashi, Serlemitsos, Peter, Tawara, Yuzuru, Mitsuishi, Ikuyuki, Ishibashi, Kazunori, Tamura, Keisuke, Hayashi, Takayuki, Furuzawa, Akihiro, Sugita, Satoshi, Miyazawa, Takuya, Awaki, Hisamitsu, Miller, Eric D, and Yamaguchi, Hiroya

Abstract

We describe the in-orbit performance of the soft X-ray imaging system consisting of the Soft X-ray Telescope and the Soft X-ray Imager aboard Hitomi. Verification and calibration of imaging and spectroscopic performance are carried out, making the best use of the limited data of less than three weeks. Basic performance, including a large field of view of ${38^{\prime }}$× ${38^{\prime }}$, is verified with the first-light image of the Perseus cluster of galaxies. Amongst the small number of observed targets, the on-minus-off pulse image for the out-of-time events of the Crab pulsar enables us to measure the half-power diameter of the telescope as ∼${1 {^{\prime}_{.}} 3}$. The average energy resolution measured with the onboard calibration source events at 5.89 keV is 179 ± 3 eV in full width at half maximum. Light leak and crosstalk issues affected the effective exposure time and the effective area, respectively, because all the observations were performed before optimizing an observation schedule and the parameters for the dark-level calculation. Screening the data affected by these two issues, we measure the background level to be 5.6 × 10−6counts s−1arcmin−2cm−2in the energy band of 5–12 keV, which is seven times lower than that of the Suzaku XIS-BI.

Published
2018
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32. Soft x-ray imager (SXI) onboard ASTRO-H

Author

den Herder, Jan-Willem A., Takahashi, Tadayuki, Bautz, Marshall, Tsunemi, Hiroshi, Hayashida, Kiyoshi, Tsuru, Takeshi Go, Dotani, Tadayasu, Nakajima, Hiroshi, Anabuki, Naohisa, Nagino, Ryo, Tanaka, Takaaki, Uchida, Hiroyuki, Ozaki, Masanobu, Natsukari, Chikara, Tomida, Hiroshi, Ueda, Shutaro, Iwai, Masachika, Nobukawa, Masayoshi, Hiraga, Junko S., Kohmura, Takayoshi, Murakami, Hiroshi, Mori, Koji, Yamauchi, Makoto, Hatsukade, Isamu, Nishioka, Yusuke, Bamba, Aya, Nobukawa, Kumiko K., and Doty, John

Published
2016
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33. Bronchial Rupture as a Complication of Response to Combination Chemotherapy in Metastatic Testicular Carcinoma

Author

Doty, John D., Lynch, Garrett R., Smith, Frank E., and Lane, Montague

Abstract

Chemotherapy for a metastatic germ cell tumor of the testis was complicated by a life-threatening bronchial rupture secondary to lysis of an endobronchial tumor. Subsequent chemotherapy was delayed because of this complication. Other pulmonary complications of chemotherapy-induced tumor lysis, including abscess formation, empyema and pneumothorax, are discussed.

Published
1984
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34. Transiting Exoplanet Survey Satellite

Author

Ricker, George R., Winn, Joshua N., Vanderspek, Roland, Latham, David W., Bakos, Gáspár Á., Bean, Jacob L., Berta-Thompson, Zachory K., Brown, Timothy M., Buchhave, Lars, Butler, Nathaniel R., Butler, R. Paul, Chaplin, William J., Charbonneau, David, Christensen-Dalsgaard, Jørgen, Clampin, Mark, Deming, Drake, Doty, John, De Lee, Nathan, Dressing, Courtney, Dunham, Edward W., Endl, Michael, Fressin, Francois, Ge, Jian, Henning, Thomas, Holman, Matthew J., Howard, Andrew W., Ida, Shigeru, Jenkins, Jon M., Jernigan, Garrett, Johnson, John Asher, Kaltenegger, Lisa, Kawai, Nobuyuki, Kjeldsen, Hans, Laughlin, Gregory, Levine, Alan M., Lin, Douglas, Lissauer, Jack J., MacQueen, Phillip, Marcy, Geoffrey, McCullough, Peter R., Morton, Timothy D., Narita, Norio, Paegert, Martin, Palle, Enric, Pepe, Francesco, Pepper, Joshua, Quirrenbach, Andreas, Rinehart, Stephen A., Sasselov, Dimitar, Sato, Bun’ei, Seager, Sara, Sozzetti, Alessandro, Stassun, Keivan G., Sullivan, Peter, Szentgyorgyi, Andrew, Torres, Guillermo, Udry, Stephane, and Villasenor, Joel

Published
2014
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35. Transiting Exoplanet Survey Satellite (TESS)

Author

Oschmann, Jacobus M., Clampin, Mark, Fazio, Giovanni G., MacEwen, Howard A., Ricker, George R., Winn, Joshua N., Vanderspek, Roland, Latham, David W., Bakos, Gáspár Á., Bean, Jacob L., Berta-Thompson, Zachory K., Brown, Timothy M., Buchhave, Lars, Butler, Nathaniel R., Butler, R. Paul, Chaplin, William J., Charbonneau, David, Christensen-Dalsgaard, Jørgen, Clampin, Mark, Deming, Drake, Doty, John, De Lee, Nathan, Dressing, Courtney, Dunham, E. W., Endl, Michael, Fressin, Francois, Ge, Jian, Henning, Thomas, Holman, Matthew J., Howard, Andrew W., Ida, Shigeru, Jenkins, Jon, Jernigan, Garrett, Johnson, John A., Kaltenegger, Lisa, Kawai, Nobuyuki, Kjeldsen, Hans, Laughlin, Gregory, Levine, Alan M., Lin, Douglas, Lissauer, Jack J., MacQueen, Phillip, Marcy, Geoffrey, McCullough, P. R., Morton, Timothy D., Narita, Norio, Paegert, Martin, Palle, Enric, Pepe, Francesco, Pepper, Joshua, Quirrenbach, Andreas, Rinehart, S. A., Sasselov, Dimitar, Sato, Bun'ei, Seager, Sara, Sozzetti, Alessandro, Stassun, Keivan G., Sullivan, Peter, Szentgyorgyi, Andrew, Torres, Guillermo, Udry, Stephane, and Villasenor, Joel

Published
2014
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36. The ASTRO-H X-ray astronomy satellite

Author

Takahashi, Tadayuki, den Herder, Jan-Willem A., Bautz, Mark, Takahashi, Tadayuki, Mitsuda, Kazuhisa, Kelley, Richard, Aharonian, Felix, Akamatsu, Hiroki, Akimoto, Fumie, Allen, Steve, Anabuki, Naohisa, Angelini, Lorella, Arnaud, Keith, Asai, Makoto, Audard, Marc, Awaki, Hisamitsu, Azzarello, Philipp, Baluta, Chris, Bamba, Aya, Bando, Nobutaka, Bautz, Marshall, Bialas, Thomas, Blandford, Roger D., Boyce, Kevin, Brenneman, Laura, Brown, Gregory, Cackett, Ed, Canavan, Edgar, Chernyakova, Maria, Chiao, Meng, Coppi, Paolo, Costantini, Elisa, de Plaa, Jelle, den Herder, Jan-Willem, DiPirro, Michael, Done, Chris, Dotani, Tadayasu, Doty, John, Ebisawa, Ken, Enoto, Teruaki, Ezoe, Yuichiro, Fabian, Andrew, Ferrigno, Carlo, Foster, Adam, Fujimoto, Ryuichi, Fukazawa, Yasushi, Funk, Stefan, Furuzawa, Akihiro, Galeazzi, Massimiliano, Gallo, Luigi, Gandhi, Poshak, Gilmore, Kirk, Guainazzi, Matteo, Haas, Daniel, Haba, Yoshito, Hamaguchi, Kenji, Harayama, Atsushi, Hatsukade, Isamu, Hayashi, Katsuhiro, Hayashi, Takayuki, Hayashida, Kiyoshi, Hiraga, Junko, Hirose, Kazuyuki, Hornschemeier, Ann, Hoshino, Akio, Hughes, John, Hwang, Una, Iizuka, Ryo, Inoue, Yoshiyuki, Ishibashi, Kazunori, Ishida, Manabu, Ishikawa, Kumi, Ishimura, Kosei, Ishisaki, Yoshitaka, Itoh, Masayuki, Iwata, Naoko, Iyomoto, Naoko, Jewell, Chris, Kaastra, Jelle, Kallman, Timothy, Kamae, Tuneyoshi, Kataoka, Jun, Katsuda, Satoru, Katsuta, Junichiro, Kawaharada, Madoka, Kawai, Nobuyuki, Kawano, Taro, Kawasaki, Shigeo, Khangaluyan, Dmitry, Kilbourne, Caroline, Kimball, Mark, Kimura, Masashi, Kitamoto, Shunji, Kitayama, Tetsu, Kohmura, Takayoshi, Kokubun, Motohide, Konami, Saori, Kosaka, Tatsuro, Koujelev, Alexander, Koyama, Katsuji, Krimm, Hans, Kubota, Aya, Kunieda, Hideyo, LaMassa, Stephanie, Laurent, Philippe, Lebrun, François, Leutenegger, Maurice, Limousin, Olivier, Loewenstein, Michael, Long, Knox, Lumb, David, Madejski, Grzegorz, Maeda, Yoshitomo, Makishima, Kazuo, Markevitch, Maxim, Masters, Candace, Matsumoto, Hironori, Matsushita, Kyoko, McCammon, Dan, McGuinness, Daniel, McNamara, Brian, Miko, Joseph, Miller, Jon, Miller, Eric, Mineshige, Shin, Minesugi, Kenji, Mitsuishi, Ikuyuki, Miyazawa, Takuya, Mizuno, Tsunefumi, Mori, Koji, Mori, Hideyuki, Moroso, Franco, Muench, Theodore, Mukai, Koji, Murakami, Hiroshi, Murakami, Toshio, Mushotzky, Richard, Nagano, Housei, Nagino, Ryo, Nakagawa, Takao, Nakajima, Hiroshi, Nakamori, Takeshi, Nakashima, Shinya, Nakazawa, Kazuhiro, Namba, Yoshiharu, Natsukari, Chikara, Nishioka, Yusuke, Nobukawa, Masayoshi, Noda, Hirofumi, Nomachi, Masaharu, O'Dell, Steve, Odaka, Hirokazu, Ogawa, Hiroyuki, Ogawa, Mina, Ogi, Keiji, Ohashi, Takaya, Ohno, Masanori, Ohta, Masayuki, Okajima, Takashi, Okazaki, Tsuyoshi, Ota, Naomi, Ozaki, Masanobu, Paerels, Frits, Paltani, Stéphane, Parmar, Arvind, Petre, Robert, Pinto, Ciro, Pohl, Martin, Pontius, James, Porter, F. S., Pottschmidt, Katja, Ramsey, Brian, Reis, Rubens, Reynolds, Christopher, Ricci, Claudio, Russell, Helena, Safi-Harb, Samar, Saito, Shinya, Sakai, Shin-ichiro, Sameshima, Hiroaki, Sato, Kosuke, Sato, Rie, Sato, Goro, Sawada, Makoto, Serlemitsos, Peter, Seta, Hiromi, Shibano, Yasuko, Shida, Maki, Shimada, Takanobu, Shirron, Peter, Simionescu, Aurora, Simmons, Cynthia, Smith, Randall, Sneiderman, Gary, Soong, Yang, Stawarz, Lukasz, Sugawara, Yasuharu, Sugita, Satoshi, Szymkowiak, Andrew, Tajima, Hiroyasu, Takahashi, Hiroaki, Takahashi, Hiromitsu, Takeda, Shin-ichiro, Takei, Yoh, Tamagawa, Toru, Tamura, Keisuke, Tamura, Takayuki, Tanaka, Takaaki, Tanaka, Yasuyuki, Tanaka, Yasuo, Tashiro, Makoto, Tawara, Yuzuru, Terada, Yukikatsu, Terashima, Yuichi, Tombesi, Francesco, Tomida, Hiroshi, Tsuboi, Yoko, Tsujimoto, Masahiro, Tsunemi, Hiroshi, Tsuru, Takeshi, Uchida, Hiroyuki, Uchiyama, Hideki, Uchiyama, Yasunobu, Ueda, Yoshihiro, Ueda, Shutaro, Ueno, Shiro, Uno, Shinichiro, Urry, Meg, Ursino, Eugenio, de Vries, Cor, Wada, Atsushi, Watanabe, Shin, Watanabe, Tomomi, Werner, Norbert, White, Nicholas, Wilkins, Dan, Yamada, Shinya, Yamada, Takahiro, Yamaguchi, Hiroya, Yamaoka, Kazutaka, Yamasaki, Noriko, Yamauchi, Makoto, Yamauchi, Shigeo, Yaqoob, Tahir, Yatsu, Yoichi, Yonetoku, Daisuke, Yoshida, Atsumasa, Yuasa, Takayuki, Zhuravleva, Irina, Zoghbi, Abderahmen, and ZuHone, John

Published
2014
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37. Soft X-ray Imager (SXI) onboard ASTRO-H

Author

Takahashi, Tadayuki, den Herder, Jan-Willem A., Bautz, Mark, Hayashida, Kiyoshi, Tsunemi, Hiroshi, Tsuru, Takeshi G., Dotani, Tadayasu, Nakajima, Hiroshi, Anabuki, Naohisa, Nagino, Ryo, Ueda, Shutaro, Tanaka, Takaaki, Uchida, Hiroyuki, Nobukawa, Masayoshi, Ozaki, Masayuki, Natsukari, Chikara, Hiraga, Junko S., Tomida, Hiroshi, Kimura, Masashi, Kohmura, Tadayoshi, Murakami, Hiroshi, Mori, Koji, Yamauchi, Makoto, Hatsukade, Isamu, Nishioka, Yusuke, Bamba, Aya, Katada, Shuhei, Nobukawa, Kumiko K., Iwai, Masachika, Kondo, Keisuke, Takeyoshi, Tukasa, and Doty, John P.

Published
2014
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38. Development of the soft x-ray imager (SXI) for ASTRO-H

Author

Hayashida, Kiyoshi, Tsunemi, Hiroshi, Tsuru, Takeshi Go, Dotani, Tadayasu, Nakajima, Hiroshi, Anabuki, Naohisa, Ozaki, Masanobu, Natsukari, Chikara, Hiraga, Junko S., Tomida, Hiroshi, Kohmura, Takayoshi, Murakami, Hiroshi, Mori, Koji, Yamauchi, Makoto, Hatsukade, Isamu, Bamba, Aya, Uchida, Hiroyuki, Nobukawa, Masayoshi, Ueda, Shutaro, Fujinaga, Takahisa, Matsuta, Keiko, Ohnishi, Takao, and Doty, John P.

Abstract

Soft X-ray Imager (SXI) is a CCD camera onboard the ASTRO-H satellite which is scheduled to be launched in 2014. The SXI camera contains four CCD chips, each with an imaing aread of 31mmx31 mm, arrayed in mosaic, which cover the whole FOV area of 38'x38'. The SXI CCD of which model name is HPK Pch-NeXT4 is a P-channel type, back-illuminated, fully depleted device with a thickness of 200m. We have developed an engineering model of the SXI camera body with coolers, and analog electronics for them. Combined with the bread board digital electronics, we succeeded in operation the whole the SXI system. The CCDs are cooled down to -120°C with this system, and X-rays from 55Fe sources are detected. Although optimization of the system is in progress, the energy resolution of typical 200 eV and best 156 eV (FWHM) at 5.9 keV are obtained. The readout noise is 10 e-to 15 e-, and to be improved its goal value of 5 e-. On-going function tests and environment tests reveal some issues to be solved until the producntion of the SXI flight model in 2012.

Published
2011
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39. Multiple-Component Analysis of the Time-Resolved Spectra of GRB041006: A Clue to the Nature of the Underlying Soft Component of GRBs

Author

Shirasaki, Yuji, Yoshida, Atsumasa, Kawai, Nobuyuki, Tamagawa, Toru, Sakamoto, Takanori, Suzuki, Motoko, Nakagawa, Yujin, Kobayashi, Akina, Sugita, Satoshi, Takahashi, Ichiro, Arimoto, Makoto, Shimokawabe, Takashi, Pazmino, Nicolas Vasquez, Ishimura, Takuto, Sato, Rie, Matsuoka, Masaru, Fenimore, Edward E., Galassi, Mark, Lamb, Donald Q., Graziani, Carlo, Donaghy, Timothy Q., Atteia, Jean-Luc, Pelangeon, Alexandre, Vanderspek, Roland, Crew, Geoffrey B., Doty, John P., Villasenor, Joel, Prigozhin, Gregory, Butler, Nat, Ricker, George R., Hurley, Kevin, Woosley, Stanford E., and Pizzichini, Graziella

Abstract

GRB041006 was detected by HETE-2 on 2004 October 06. The light curves in four different energy bands display different features. At higher energy bands several peaks are seen in the light curve, while at lower energy bands a single broader bump dominates. It is expected that these different features are the result of a mixture of several components, each of which has different energetics and variability. We analyzed the time-resolved spectra, which were resolved into several components. These components can be classified into two distinct classes. One is a component that has an exponential decay of $E_{\rm p}$ with a characteristic timescale shorter than $\sim\;$30 s; its spectrum is well represented by a broken power-law function, which is frequently observed in many prompt GRB emissions, so it should have an internal-shock origin. Another is a component whose $E_{\rm p}$ is almost unchanged with a characteristic timescale longer than $\sim\;$60 s, and shows a very soft emission and slower variability. The spectrum is characterized by either a broken power law or a black-body spectrum. By assuming that the soft component is a thermal emission, the radiation radius is initially $4.4 \times 10^{6}$km, which is a typical radius of a blue supergiant, and its expansion velocity is $2.4 \times 10^{5}$km s$^{-1}$ in the source frame.

Published
2008
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