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4,163 results on '"Matsuoka, M."'

2. Comparison of optical spectra between asteroids Ryugu and Bennu: II. High-precision analysis for space weathering trends

Author

Yumoto, K., Tatsumi, E., Kouyama, T., Golish, D. R., Cho, Y., Morota, T., Kameda, S., Sato, H., Rizk, B., DellaGiustina, D. N., Yokota, Y., Suzuki, H., de León, J., Campins, H., Licandro, J., Popescu, M., Rizos, J. L., Honda, R., Yamada, M., Sakatani, N., Honda, C., Matsuoka, M., Hayakawa, M., Sawada, H., Ogawa, K., Yamamoto, Y., Lauretta, D. S., and Sugita, S.

Subjects
Astrophysics - Earth and Planetary Astrophysics, Physics - Space Physics
Abstract

The influence of space weathering on the observed spectra of C-complex asteroids remains uncertain. This has long hindered our understanding of their composition through telescope observations. Multi-band imaging of Ryugu by ONC-T on Hayabusa2 and that of Bennu by MapCam on OSIRIS-REx found opposite spectral trends of space weathering; Ryugu darkened/reddened while Bennu brightened/blued. How the spectra of Ryugu and Bennu evolved relative to each other would place a constraint for understanding their origins and evolutions. In this study, we compared the space weathering trends on Ryugu and Bennu by applying the results of cross calibration between ONC-T and MapCam. We show that the average Bennu surface is brighter by 18.0 $\pm$ 1.5% at 550 nm and bluer by 0.18 $\pm$ 0.03 $\mu$m$^{-1}$ (480-850 nm slope) than Ryugu. The spectral slopes of surface materials are more uniform on Bennu than on Ryugu at spatial scales $\gtrsim$1 m, but Bennu is more heterogeneous at $\lesssim$1 m. This suggests that lateral mixing due to resurfacing may have been more efficient on Bennu. The reflectance-spectral slope distributions of craters on Ryugu and Bennu appeared to follow two trend lines with an offset before cross calibration, but they converged to a single straight trend without a bend after cross calibration. We show that the spectra of the freshest craters on Ryugu and Bennu are indistinguishable within the uncertainty of cross calibration. These results suggest that Ryugu and Bennu initially had similar spectra before space weathering and that they evolved in completely opposite directions along the same trend line, subsequently evolving into asteroids with different disk-averaged spectra. These findings further suggest that space weathering likely expanded the spectral slope variation of C-complex asteroids, implying that they may have formed from materials with more uniform spectral slopes.

Published
2024
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3. Comparison of optical spectra between asteroids Ryugu and Bennu:I. Cross calibration between Hayabusa2/ONC-T and OSIRIS-REx/MapCam

Author

Yumoto, K., Tatsumi, E., Kouyama, T., Golish, D. R., Cho, Y., Morota, T., Kameda, S., Sato, H., Rizk, B., DellaGiustina, D. N., Yokota, Y., Suzuki, H., de Leon, J., Campins, H., Licandro, J., Popescu, M., Rizos, J. L., Honda, R., Yamada, M., Sakatani, N., Honda, C., Matsuoka, M., Hayakawa, M., Sawada, H., Ogawa, K., Yamamoto, Y., Lauretta, D. S., and Sugita, S.

Subjects
Astrophysics - Earth and Planetary Astrophysics
Abstract

Asteroids (162173) Ryugu and (101955) Bennu observed by Hayabusa2 and OSIRIS-REx share many properties, but spectral observations by the telescopic Optical Navigation Camera (ONC-T) and MapCam detected subtle but significant differences, which may reflect differences in their origin and evolution. Comparing these differences on the same absolute scale is necessary for understanding their causes. However, ONC-T and MapCam have a large imager-to-imager systematic error of up to 15% caused by the difference in radiometric calibration targets. To resolve this problem, we cross calibrated albedo and color data between the two instruments using the Moon as the common calibration standard. The images of the Moon taken by ONC-T and MapCam were compared with those simulated using photometry models developed from lunar orbiter data. Our results show that the cross-calibrated reflectance of Ryugu and Bennu can be obtained by upscaling the pre-cross-calibrated reflectance of Bennu by 13.3 +/- 1.6% at b band, 13.2 +/- 1.5% at v band, 13.6 +/- 1.7% at w band, and 14.8 +/- 1.8% at x band, while those for Ryugu are kept the same. These factors compensate for the imager-to-imager bias caused by differences in targets used for radiometric calibration and solar irradiance models used for data reduction. Need for such large upscaling underscore the importance of using the cross-calibrated data for accurately comparing the Ryugu and Bennu data. The uncertainty in these factors show that the reflectance of Ryugu and Bennu can be compared with <2% accuracy after applying our results. By applying our cross calibration, the geometric albedo of Bennu became consistent with those observed by ground-based telescopes and OVIRS. Our result can be simply applied by multiplying a constant to the publicly available data and enables accurate comparison of the optical spectra of Ryugu and Bennu in future studies.

Published
2023
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5. Combination of a Topical Anti-Inflammatory Drug and a Moisturizer, Both with a Lamellar Structure Containing Synthetic Pseudo-Ceramides, for the Treatment of Patients with Mild-to-Moderate Atopic Dermatitis

Author

Okoshi K, Ito S, Matsuoka M, Kinugasa Y, Shimizu E, Tanaka K, Okada J, Nishizaka T, Nagasawa A, Seki T, Iijima M, Abe M, and Nemoto O

Subjects
base formulations, lamellar structure, steroid, heparinoid, barrier function, tewl, Dermatology, RL1-803
Abstract

Keita Okoshi,1 Shotaro Ito,1 Megumi Matsuoka,1 Yoshinori Kinugasa,1 Eri Shimizu,2 Kosei Tanaka,2 Joji Okada,3 Takahiro Nishizaka,1 Azumi Nagasawa,1 Tsuyoshi Seki,1 Makoto Iijima,1 Masatoshi Abe,4 Osamu Nemoto4 1Human Health Care Products Research, Kao Corporation, Tokyo, Japan; 2Analytical Science Research, Kao Corporation, Tochigi, Japan; 3Skin Care Products Research, Kao Corporation, Tokyo, Japan; 4Sapporo Skin Clinic, Sapporo, JapanCorrespondence: Azumi Nagasawa, Human Health Care Products Research, Kao Corporation, 2-1-3, Bunka, Sumida-ku, Tokyo, 131-8501, Japan, Tel +81-3-5630-7690, Fax +81-3-5630-9342, Email nagasawa.azumi@kao.comPurpose: Atopic dermatitis is characterized by chronic inflammation and dryness accompanied by severe itching. The combined use of moisturizers and topical anti-inflammatory drugs is essential for alleviating atopic dermatitis. We have developed a topical anti-inflammatory drug with a steroid and a moisturizer with heparinoid, both in lamellar structure-based formulations containing synthetic pseudo-ceramides. Here, assessed the efficacy of this combination in the treatment of atopic dermatitis.Methods: We included 22 patients with mild to moderate atopic dermatitis and subjected them to a seven-week treatment with the test formulations, followed by a four-week post-treatment period.Results: Clinical findings and the quality of life of participants remarkably improved after one week of treatment. Furthermore, skin hydration and transepidermal water loss considerably improved at weeks one and three, respectively. The Cer [NP]/[NS] ratio, an indicator of epidermal turnover, substantially increased during the treatment period and remained elevated even thereafter. The improvement in stratum corneum function was distinctive in participants with lower barrier function.Conclusion: These findings indicated that the combined use of the anti-inflammatory drug and moisturizer, both in lamellar structure-based formulations, is effective in treating atopic dermatitis in patients with fragile barrier function.Keywords: base formulations, lamellar structure, steroid, heparinoid, barrier function, TEWL

Published
2024

6. Comparison of optical spectra between asteroids Ryugu and Bennu: I. Cross calibration between Hayabusa2/ONC-T and OSIRIS-REx/MapCam

Author

Yumoto, K., Tatsumi, E., Kouyama, T., Golish, D.R., Cho, Y., Morota, T., Kameda, S., Sato, H., Rizk, B., DellaGiustina, D.N., Yokota, Y., Suzuki, H., de León, J., Campins, H., Licandro, J., Popescu, M., Rizos, J.L., Honda, R., Yamada, M., Sakatani, N., Honda, C., Matsuoka, M., Hayakawa, M., Sawada, H., Ogawa, K., Yamamoto, Y., Lauretta, D.S., and Sugita, S.

Published
2024
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7. Evidence of global space weathering by solar wind on asteroid 162173 Ryugu

Author

Hiroi, T., Milliken, R.E., Robertson, K.M., Schultz, C.D., Amano, K., Nakamura, T., Yurimoto, H., Noguchi, T., Okazaki, R., Naraoka, H., Yabuta, H., Sakamoto, K., Yada, T., Nishimura, M., Nakato, A., Miyazaki, A., Yogata, K., Abe, M., Okada, T., Usui, T., Yoshikawa, M., Saiki, T., Tanaka, S., Nakazawa, S., Yokota, Y., Tatsumi, E., Tsuda, Y., Tachibana, S., Fuyuto, T., Watanabe, S., Sasaki, S., Kaiden, H., Kitazato, K., and Matsuoka, M.

Published
2023
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8. Overview of the search for signs of space weathering on the low-albedo asteroid (101955) Bennu

Author

Clark, B.E., Sen, A., Zou, X.-D., DellaGiustina, D.N., Sugita, S., Sakatani, N., Thompson, M., Trang, D., Tatsumi, E., Barucci, M.A., Barker, M., Campins, H., Morota, T., Lantz, C., Hendrix, A.R., Vilas, F., Keller, L., Hamilton, V.E., Kitazato, K., Sasaki, S., Matsuoka, M., Nakamura, T., Praet, A., Ferrone, S.M., Hiroi, T., Kaplan, H.H., Bottke, W.F., Li, J.-Y., Le Corre, L., Molaro, J.L., Ballouz, R.-L., Hergenrother, C.W., Rizk, B., Burke, K.N., Bennett, C.A., Golish, D.R., Howell, E.S., Becker, K., Ryan, A.J., Emery, J.P., Fornasier, S., Simon, A.A., Reuter, D.C., Lim, L.F., Poggiali, G., Michel, P., Delbo, M., Barnouin, O.S., Jawin, E.R., Pajola, M., Riu, L., Okada, T., Deshapriya, J.D.P., Brucato, J.R., Binzel, R.P., and Lauretta, D.S.

Published
2023
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9. Poor Asthma Control in Schoolchildren May Lead to Lower Lung Function Trajectory from Childhood to Early Adulthood: A Japanese Cohort Study

Author

Tsuneyoshi S, Kawayama T, Sasaki J, Kinoshita T, Yano C, Tokunaga Y, Matsuoka M, Imaoka H, Matsunaga K, Furukawa K, and Hoshino T

Subjects
childhood asthma, airflow limitation, japanese, transition, school-age children, Immunologic diseases. Allergy, RC581-607
Abstract

Shingo Tsuneyoshi,1 Tomotaka Kawayama,1 Jun Sasaki,1 Takashi Kinoshita,1 Chiyo Yano,1 Yoshihisa Tokunaga,1 Masanobu Matsuoka,1 Haruki Imaoka,1 Kazuko Matsunaga,1 Kyoji Furukawa,2 Tomoaki Hoshino1 1Division of Respirology, Neurology, and Rheumatology, Department of Medicine, Kurume University School of Medicine, Kurume, Japan; 2Biostatistics Center, Kurume University School of Medicine, Kurume, JapanCorrespondence: Tomotaka Kawayama, Division of Respirology, Neurology, and Rheumatology, Department of Medicine, Kurume University School of Medicine, 67 Asahi-machi, Kurume, 830-0011, Japan, Email kawayama_tomotaka@med.kurume-u.ac.jpPurpose: Although childhood asthma is a risk factor for adult lung function disorders, the correlation between childhood asthma control level and lung function growth remains unclear in Japan. The correlation between childhood asthma control and early adulthood lung function growth was investigated in this study.Patients and Methods: We included 505 children with asthma from the Omuta City Air Pollution-Related Health Damage Cohort Program. The characteristics and lung function of girls and boys aged 6– 11 years and 12– 17 years were compared between poor and good asthma control groups.Results: Among the 505 children, 214 (42.4%) showed poor asthma control. The mean percentage forced expiratory volume in 1 second predicted for girls and boys aged 6– 11 years (80.2% and 79.2%, respectively) and 12– 17 years (80.0% and 81.1%, respectively) in the poor control group was significantly lower than those of girls and boys aged 6– 11 years (87.9% and 87.3%, respectively) and 12– 17 years (88.1% and 87.8%, respectively) in the good control group. However, a linear regression model did not reveal between-group differences in the slopes of lung function growth for both sexes. Girls (24.6%, P < 0.0001) and boys (24.4%, P = 0.0026) in the poor control group had a significantly higher proportion of young adults with obstructive ventilatory patterns than girls (1.4%) and boys (8.1%) in the good control group.Conclusion: Our findings revealed that poor childhood asthma control leaded to lung function disorders, which suggest the importance of early asthma control in school children.Keywords: childhood asthma, airflow limitation, Japanese, transition, school-age children

Published
2022

11. Particle size distributions inside and around the artificial crater produced by the Hayabusa2 impact experiment on Ryugu

Author

Ogawa, K., Sakatani, N., Kadono, T., Arakawa, M., Honda, R., Wada, K., Shirai, K., Shimaki, Y., Ishibashi, K., Yokota, Y., Saiki, T., Imamura, H., Tsuda, Y., Nakazawa, S., Takagi, Y., Hayakawa, M., Yano, H., Okamoto, C., Iijima, Y., Morota, T., Kameda, S., Tatsumi, E., Cho, Y., Yoshioka, K., Sawada, H., Matsuoka, M., Yamada, M., Kouyama, T., Suzuki, H., Honda, C., and Sugita, S.

Published
2022
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13. Efficacy of Heparinoid Cream Containing Pseudo-Ceramide for Remission of Atopic Dermatitis

Author

Matsuoka M, Okoshi K, Ito S, Kume T, Seki T, Nishizaka T, Okada J, Nagasawa A, Iijima M, Abe M, and Nemoto O

Subjects
atopic dermatitis, barrier, lamellar, heparinoid, ceramide, skin hydration, transepidermal water loss, Dermatology, RL1-803
Abstract

Megumi Matsuoka,1 Keita Okoshi,1 Shotaro Ito,1 Takuji Kume,2 Tsuyoshi Seki,1 Takahiro Nishizaka,1 Joji Okada,3 Azumi Nagasawa,1 Makoto Iijima,1 Masatoshi Abe,4 Osamu Nemoto4 1Health & Wellness Products Research, Kao Corporation, Sumida-ku, Tokyo, Japan; 2Analytical Science Research, Kao Corporation, Wakayama, Japan; 3Skin Care Products Research, Kao Corporation, Sumida-ku, Tokyo, Japan; 4Sapporo Skin Clinic, Sapporo, Hokkaido, JapanCorrespondence: Azumi NagasawaHealth & Wellness Products Research, Kao Corporation, 2-1-3, Bunka, Sumida-ku, Tokyo, 131-8501, JapanTel +81-3-5630-9443Fax +81-3-5630-9342Email nagasawa.azumi@kao.comPurpose: Atopic dermatitis (AD) is characterized by chronic inflammation, which frequently recurs, is exacerbated, and enters remission. A maintenance remission period is important for AD patients. We developed a formulation for use during AD remission, containing heparinoid and pseudo-ceramide that forms a lamellar structure. We evaluated the allergen permeability and examined the formulation’s efficacy in maintaining remission in patients with AD.Materials and Methods: Seventeen AD patients applied a cream containing 0.3% heparinoid and pseudo-ceramide (test cream group, n = 10), or a general cream containing 0.3% heparinoid (control cream group, n = 7) to their arm for four weeks after inducing remission with the application of a steroid cream for two weeks.Results: The lamellar structure of the test cream was confirmed with small- and wide-angle x-ray scattering analysis and observation by transmission electron microscopy. The test cream inhibited the penetration of V8 protease significantly compared to the control cream in vitro. According to AD severity score by dermatologists, the effects remission maintenance of the test cream group were comparable to those of the control cream group. However, the test cream group had a significantly increased skin hydration value compared to the control cream group. A significant decrease in transepidermal water loss, an indicator of skin barrier function, was shown in the test cream group compared to the control cream group.Conclusion: The cream with lamellar structures containing heparinoid and pseudo-ceramides may inhibit allergen penetration. Moreover, skin properties improved during the remission period; thus, the formulation we developed was suitable for use during the AD remission period.Keywords: atopic dermatitis, barrier, lamellar, heparinoid, ceramide, skin hydration, transepidermal water loss

Published
2021

16. Supplement: Localization and broadband follow-up of the gravitational-wave transient GW150914

Author

Abbott, B. P., Abbott, R., Abbott, T. D., Abernathy, M. R., Acernese, F., Ackley, K., Adams, C., Adams, T., Addesso, P., Adhikari, R. X., Adya, V. B., Affeldt, C., Agathos, M., Agatsuma, K., Aggarwal, N., Aguiar, O. D., Aiello, L., Ain, A., Ajith, P., Allen, B., Allocca, A., Altin, P. A., Anderson, S. B., Anderson, W. G., Arai, K., Araya, M. C., Arceneaux, C. C., Areeda, J. S., Arnaud, N., Arun, K. G., Ascenzi, S., Ashton, G., Ast, M., Aston, S. M., Astone, P., Aufmuth, P., Aulbert, C., Babak, S., Bacon, P., Bader, M. K. M., Baker, P. T., Baldaccini, F., Ballardin, G., Ballmer, S. W., Barayoga, J. C., Barclay, S. E., Barish, B. C., Barker, D., Barone, F., Barr, B., Barsotti, L., Barsuglia, M., Barta, D., Barthelmy, S., Bartlett, J., Bartos, I., Bassiri, R., Basti, A., Batch, J. C., Baune, C., Bavigadda, V., Bazzan, M., Behnke, B., Bejger, M., Bell, A. S., Bell, C. J., Berger, B. K., Bergman, J., Bergmann, G., Berry, C. P. L., Bersanetti, D., Bertolini, A., Betzwieser, J., Bhagwat, S., Bhandare, R., Bilenko, I. A., Billingsley, G., Birch, J., Birney, R., Biscans, S., Bisht, A., Bitossi, M., Biwer, C., Bizouard, M. A., Blackburn, J. K., Blair, C. D., Blair, D. G., Blair, R. M., Bloemen, S., Bock, O., Bodiya, T. P., Boer, M., Bogaert, G., Bogan, C., Bohe, A., Bojtos, P., Bond, C., Bondu, F., Bonnand, R., Boom, B. A., Bork, R., Boschi, V., Bose, S., Bouffanais, Y., Bozzi, A., Bradaschia, C., Brady, P. R., Braginsky, V. B., Branchesi, M., Brau, J. E., Briant, T., Brillet, A., Brinkmann, M., Brisson, V., Brockill, P., Brooks, A. F., Brown, D. A., Brown, D. D., Brown, N. M., Buchanan, C. C., Buikema, A., Bulik, T., Bulten, H. J., Buonanno, A., Buskulic, D., Buy, C., Byer, R. L., Cadonati, L., Cagnoli, G., Cahillane, C., Bustillo, J. C., Callister, T., Calloni, E., Camp, J. B., Cannon, K. C., Cao, J., Capano, C. D., Capocasa, E., Carbognani, F., Caride, S., Diaz, J. C., Casentini, C., Caudill, S., Cavaglià, M., Cavalier, F., Cavalieri, R., Cella, G., Cepeda, C. B., Baiardi, L. C., Cerretani, G., Cesarini, E., Chakraborty, R., Chalermsongsak, T., Chamberlin, S. J., Chan, M., Chao, S., Charlton, P., Chassande-Mottin, E., Chen, H. Y., Chen, Y., Cheng, C., Chincarini, A., Chiummo, A., Cho, H. S., Cho, M., Chow, J. H., Christensen, N., Chu, Q., Chua, S., Chung, S., Ciani, G., Clara, F., Clark, J. A., Cleva, F., Coccia, E., Cohadon, P. -F., Colla, A., Collette, C. G., Cominsky, L., Constancio Jr., M., Conte, A., Conti, L., Cook, D., Corbitt, T. R., Cornish, N., Corsi, A., Cortese, S., Costa, C. A., Coughlin, M. W., Coughlin, S. B., Coulon, J. -P., Countryman, S. T., Couvares, P., Cowan, E. E., Coward, D. M., Cowart, M. J., Coyne, D. C., Coyne, R., Craig, K., Creighton, J. D. E., Cripe, J., Crowder, S. G., Cumming, A., Cunningham, L., Cuoco, E., Canton, T. Dal, Danilishin, S. L., D'Antonio, S., Danzmann, K., Darman, N. S., Dattilo, V., Dave, I., Daveloza, H. P., Davier, M., Davies, G. S., Daw, E. J., Day, R., DeBra, D., Debreczeni, G., Degallaix, J., De Laurentis, M., Deléglise, S., Del Pozzo, W., Denker, T., Dent, T., Dereli, H., Dergachev, V., DeRosa, R. T., De Rosa, R., DeSalvo, R., Dhurandhar, S., Díaz, M. C., Di Fiore, L., Di Giovanni, M., Di Lieto, A., Di Pace, S., Di Palma, I., Di Virgilio, A., Dojcinoski, G., Dolique, V., Donovan, F., Dooley, K. L., Doravari, S., Douglas, R., Downes, T. P., Drago, M., Drever, R. W. P., Driggers, J. C., Du, Z., Ducrot, M., Dwyer, S. E., Edo, T. B., Edwards, M. C., Effler, A., Eggenstein, H. -B., Ehrens, P., Eichholz, J., Eikenberry, S. S., Engels, W., Essick, R. C., Etzel, T., Evans, M., Evans, T. M., Everett, R., Factourovich, M., Fafone, V., Fair, H., Fairhurst, S., Fan, X., Fang, Q., Farinon, S., Farr, B., Farr, W. M., Favata, M., Fays, M., Fehrmann, H., Fejer, M. M., Ferrante, I., Ferreira, E. C., Ferrini, F., Fidecaro, F., Fiori, I., Fiorucci, D., Fisher, R. P., Flaminio, R., Fletcher, M., Fournier, J. -D., Franco, S., Frasca, S., Frasconi, F., Frei, Z., Freise, A., Frey, R., Frey, V., Fricke, T. T., Fritschel, P., Frolov, V. V., Fulda, P., Fyffe, M., Gabbard, H. A. G., Gair, J. R., Gammaitoni, L., Gaonkar, S. G., Garufi, F., Gatto, A., Gaur, G., Gehrels, N., Gemme, G., Gendre, B., Genin, E., Gennai, A., George, J., Gergely, L., Germain, V., Ghosh, A., Ghosh, S., Giaime, J. A., Giardina, K. D., Giazotto, A., Gill, K., Glaefke, A., Goetz, E., Goetz, R., Gondan, L., González, G., Castro, J. M. G., Gopakumar, A., Gordon, N. A., Gorodetsky, M. L., Gossan, S. E., Gosselin, M., Gouaty, R., Graef, C., Graff, P. B., Granata, M., Grant, A., Gras, S., Gray, C., Greco, G., Green, A. C., Groot, P., Grote, H., Grunewald, S., Guidi, G. M., Guo, X., Gupta, A., Gupta, M. K., Gushwa, K. E., Gustafson, E. K., Gustafson, R., Hacker, J. J., Hall, B. R., Hall, E. D., Hammond, G., Haney, M., Hanke, M. M., Hanks, J., Hanna, C., Hannam, M. D., Hanson, J., Hardwick, T., Haris, K., Harms, J., Harry, G. M., Harry, I. W., Hart, M. J., Hartman, M. T., Haster, C. -J., Haughian, K., Heidmann, A., Heintze, M. C., Heitmann, H., Hello, P., Hemming, G., Hendry, M., Heng, I. S., Hennig, J., Heptonstall, A. W., Heurs, M., Hild, S., Hoak, D., Hodge, K. A., Hofman, D., Hollitt, S. E., Holt, K., Holz, D. E., Hopkins, P., Hosken, D. J., Hough, J., Houston, E. A., Howell, E. J., Hu, Y. M., Huang, S., Huerta, E. A., Huet, D., Hughey, B., Husa, S., Huttner, S. H., Huynh-Dinh, T., Idrisy, A., Indik, N., Ingram, D. R., Inta, R., Isa, H. N., Isac, J. -M., Isi, M., Islas, G., Isogai, T., Iyer, B. R., Izumi, K., Jacqmin, T., Jang, H., Jani, K., Jaranowski, P., Jawahar, S., Jiménez-Forteza, F., Johnson, W. W., Jones, D. I., Jones, R., Jonker, R. J. G., Ju, L., Kalaghatgi, C. V., Kalogera, V., Kandhasamy, S., Kang, G., Kanner, J. B., Karki, S., Kasprzack, M., Katsavounidis, E., Katzman, W., Kaufer, S., Kaur, T., Kawabe, K., Kawazoe, F., Kéfélian, F., Kehl, M. S., Keitel, D., Kelley, D. B., Kells, W., Kennedy, R., Key, J. S., Khalaidovski, A., Khalili, F. Y., Khan, I., Khan, S., Khan, Z., Khazanov, E. A., Kijbunchoo, N., Kim, C., Kim, J., Kim, K., Kim, N., Kim, Y. -M., King, E. J., King, P. J., Kinzel, D. L., Kissel, J. S., Kleybolte, L., Klimenko, S., Koehlenbeck, S. M., Kokeyama, K., Koley, S., Kondrashov, V., Kontos, A., Korobko, M., Korth, W. Z., Kowalska, I., Kozak, D. B., Kringel, V., Królak, A., Krueger, C., Kuehn, G., Kumar, P., Kuo, L., Kutynia, A., Lackey, B. D., Landry, M., Lange, J., Lantz, B., Lasky, P. D., Lazzarini, A., Lazzaro, C., Leaci, P., Leavey, S., Lebigot, E. O., Lee, C. H., Lee, H. K., Lee, H. M., Lee, K., Lenon, A., Leonardi, M., Leong, J. R., Leroy, N., Letendre, N., Levin, Y., Levine, B. M., Li, T. G. F., Libson, A., Littenberg, T. B., Lockerbie, N. A., Logue, J., Lombardi, A. L., Lord, J. E., Lorenzini, M., Loriette, V., Lormand, M., Losurdo, G., Lough, J. D., Lück, H., Lundgren, A. P., Luo, J., Lynch, R., Ma, Y., MacDonald, T., Machenschalk, B., MacInnis, M., Macleod, D. M., Magaña-Sandoval, F., Magee, R. M., Mageswaran, M., Majorana, E., Maksimovic, I., Malvezzi, V., Man, N., Mandel, I., Mandic, V., Mangano, V., Mansell, G. L., Manske, M., Mantovani, M., Marchesoni, F., Marion, F., Márka, S., Márka, Z., Markosyan, A. S., Maros, E., Martelli, F., Martellini, L., Martin, I. W., Martin, R. M., Martynov, D. V., Marx, J. N., Mason, K., Masserot, A., Massinger, T. J., Masso-Reid, M., Matichard, F., Matone, L., Mavalvala, N., Mazumder, N., Mazzolo, G., McCarthy, R., McClelland, D. E., McCormick, S., McGuire, S. C., McIntyre, G., McIver, J., McManus, D. J., McWilliams, S. T., Meacher, D., Meadors, G. D., Meidam, J., Melatos, A., Mendell, G., Mendoza-Gandara, D., Mercer, R. A., Merilh, E., Merzougui, M., Meshkov, S., Messenger, C., Messick, C., Meyers, P. 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Subjects
Astrophysics - High Energy Astrophysical Phenomena, General Relativity and Quantum Cosmology
Abstract

This Supplement provides supporting material for arXiv:1602.08492 . We briefly summarize past electromagnetic (EM) follow-up efforts as well as the organization and policy of the current EM follow-up program. We compare the four probability sky maps produced for the gravitational-wave transient GW150914, and provide additional details of the EM follow-up observations that were performed in the different bands., Comment: For the main Letter, see arXiv:1602.08492

Published
2016
Full Text
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17. Localization and broadband follow-up of the gravitational-wave transient GW150914

Author

Abbott, B. P., Abbott, R., Abbott, T. D., Abernathy, M. R., Acernese, F., Ackley, K., Adams, C., Adams, T., Addesso, P., Adhikari, R. X., Adya, V. B., Affeldt, C., Agathos, M., Agatsuma, K., Aggarwal, N., Aguiar, O. D., Aiello, L., Ain, A., Ajith, P., Allen, B., Allocca, A., Altin, P. A., Anderson, S. B., Anderson, W. G., Arai, K., Araya, M. C., Arceneaux, C. C., Areeda, J. S., Arnaud, N., Arun, K. G., Ascenzi, S., Ashton, G., Ast, M., Aston, S. M., Astone, P., Aufmuth, P., Aulbert, C., Babak, S., Bacon, P., Bader, M. K. M., Baker, P. T., Baldaccini, F., Ballardin, G., Ballmer, S. W., Barayoga, J. C., Barclay, S. E., Barish, B. C., Barker, D., Barone, F., Barr, B., Barsotti, L., Barsuglia, M., Barta, D., Barthelmy, S., Bartlett, J., Bartos, I., Bassiri, R., Basti, A., Batch, J. C., Baune, C., Bavigadda, V., Bazzan, M., Behnke, B., Bejger, M., Bell, A. S., Bell, C. J., Berger, B. K., Bergman, J., Bergmann, G., Berry, C. P. L., Bersanetti, D., Bertolini, A., Betzwieser, J., Bhagwat, S., Bhandare, R., Bilenko, I. A., Billingsley, G., Birch, J., Birney, R., Biscans, S., Bisht, A., Bitossi, M., Biwer, C., Bizouard, M. A., Blackburn, J. K., Blair, C. D., Blair, D. G., Blair, R. M., Bloemen, S., Bock, O., Bodiya, T. P., Boer, M., Bogaert, G., Bogan, C., Bohe, A., Bojtos, P., Bond, C., Bondu, F., Bonnand, R., Boom, B. A., Bork, R., Boschi, V., Bose, S., Bouffanais, Y., Bozzi, A., Bradaschia, C., Brady, P. R., Braginsky, V. B., Branchesi, M., Brau, J. E., Briant, T., Brillet, A., Brinkmann, M., Brisson, V., Brockill, P., Brooks, A. F., Brown, D. A., Brown, D. D., Brown, N. M., Buchanan, C. C., Buikema, A., Bulik, T., Bulten, H. J., Buonanno, A., Buskulic, D., Buy, C., Byer, R. L., Cadonati, L., Cagnoli, G., Cahillane, C., Bustillo, J. C., Callister, T., Calloni, E., Camp, J. B., Cannon, K. C., Cao, J., Capano, C. D., Capocasa, E., Carbognani, F., Caride, S., Diaz, J. 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C., Franckowiak, A., Fukazawa, Y., Funk, S., Fusco, P., Gargano, F., Gasparrini, D., Giglietto, N., Giommi, P., Giordano, F., Giroletti, M., Glanzman, T., Godfrey, G., Gomez-Vargas, G. A., Green, D., Grenier, I. A., Grove, J. E., Guiriec, S., Hadasch, D., Harding, A. K., Hays, E., Hewitt, J. W., Hill, A. B., Horan, D., Jogler, T., Jóhannesson, G., Johnson, A. S., Kensei, S., Kocevski, D., Kuss, M., La Mura, G., Larsson, S., Latronico, L., Li, J., Li, L., Longo, F., Loparco, F., Lovellette, M. N., Lubrano, P., Magill, J., Maldera, S., Manfreda, A., Marelli, M., Mayer, M., Mazziotta, M. N., McEnery, J. E., Meyer, M., Michelson, P. F., Mirabal, N., Mizuno, T., Moiseev, A. A., Monzani, M. E., Moretti, E., Morselli, A., Moskalenko, I. V., Negro, M., Nuss, E., Ohsugi, T., Omodei, N., Orienti, M., Orlando, E., Ormes, J. F., Paneque, D., Perkins, J. S., Pesce-Rollins, M., Piron, F., Pivato, G., Porter, T. A., Racusin, J. L., Rainò, S., Rando, R., Razzaque, S., Reimer, A., Reimer, O., Salvetti, D., Parkinson, P. M. Saz, Sgrò, C., Simone, D., Siskind, E. J., Spada, F., Spandre, G., Spinelli, P., Suson, D. J., Tajima, H., Thayer, J. B., Thompson, D. J., Tibaldo, L., Torres, D. F., Troja, E., Uchiyama, Y., Venters, T. M., Vianello, G., Wood, K. S., Wood, M., Zhu, S., Zimmer, S., Brocato, E., Cappellaro, E., Covino, S., Grado, A., Nicastro, L., Palazzi, E., Pian, E., Amati, L., Antonelli, L. A., Capaccioli, M., D'Avanzo, P., D'Elia, V., Getman, F., Giuffrida, G., Iannicola, G., Limatola, L., Lisi, M., Marinoni, S., Marrese, P., Melandri, A., Piranomonte, S., Possenti, A., Pulone, L., Rossi, A., Stamerra, A., Stella, L., Testa, V., Tomasella, L., Yang, S., Bazzano, A., Bozzo, E., Brandt, S., Courvoisier, T. J. -L., Ferrigno, C., Hanlon, L., Kuulkers, E., Laurent, P., Mereghetti, S., Roques, J. P., Savchenko, V., Ubertini, P., Kasliwal, M. M., Singer, L. P., Cao, Y., Duggan, G., Kulkarni, S. R., Bhalerao, V., Miller, A. A., Barlow, T., Bellm, E., Manulis, I., Rana, J., Laher, R., Masci, F., Surace, J., Rebbapragada, U., Van Sistine, A., Sesar, B., Perley, D., Ferreti, R., Prince, T., Kendrick, R., Horesh, A., Hurley, K., Golenetskii, S. V., Aptekar, R. L., Frederiks, D. D., Svinkin, D. S., Rau, A., Zhang, X., Smith, D. M., Cline, T., Krimm, H., Abe, F., Doi, M., Fujisawa, K., Kawabata, K. S., Morokuma, T., Motohara, K., Tanaka, M., Ohta, K., Yanagisawa, K., Yoshida, M., Baltay, C., Rabinowitz, D., Ellman, N., Rostami, S., Bersier, D. F., Bode, M. F., Collins, C. A., Copperwheat, C. M., Darnley, M. J., Galloway, D. K., Gomboc, A., Kobayashi, S., Mazzali, P., Mundell, C. G., Piascik, A. S., Pollacco, Don, Steele, I. A., Ulaczyk, K., Broderick, J. W., Fender, R. P., Jonker, P. G., Rowlinson, A., Stappers, B. W., Wijers, R. A. M. J., Lipunov, V., Gorbovskoy, E., Tyurina, N., Kornilov, V., Balanutsa, P., Kuznetsov, A., Buckley, D., Rebolo, R., Serra-Ricart, M., Israelian, G., Budnev, N. M., Gress, O., Ivanov, K., Poleshuk, V., Tlatov, A., Yurkov, V., Kawai, N., Serino, M., Negoro, H., Nakahira, S., Mihara, T., Tomida, H., Ueno, S., Tsunemi, H., Matsuoka, M., Croft, S., Feng, L., Franzen, T. M. O., Gaensler, B. M., Johnston-Hollitt, M., Kaplan, D. L., Morales, M. F., Tingay, S. J., Wayth, R. B., Williams, A., Smartt, S. J., Chambers, K. C., Smith, K. W., Huber, M. E., Young, D. R., Wright, D. E., Schultz, A., Denneau, L., Flewelling, H., Magnier, E. A., Primak, N., Rest, A., Sherstyuk, A., Stalder, B., Stubbs, C. W., Tonry, J., Waters, C., Willman, M., E., F. Olivares, Campbell, H., Kotak, R., Sollerman, J., Smith, M., Dennefeld, M., Anderson, J. P., Botticella, M. T., Chen, T. -W., Valle, M. D., Elias-Rosa, N., Fraser, M., Inserra, C., Kankare, E., Kupfer, T., Harmanen, J., Galbany, L., Guillou, L. Le, Lyman, J. D., Maguire, K., Mitra, A., Nicholl, M., Razza, A., Terreran, G., Valenti, S., Gal-Yam, A., Ćwiek, A., Ćwiok, M., Mankiewicz, L., Opiela, R., Zaremba, M., Żarnecki, A. F., Onken, C. A., Scalzo, R. A., Schmidt, B. P., Wolf, C., Yuan, F., Evans, P. A., Kennea, J. A., Burrows, D. N., Campana, S., Cenko, S. B., Marshall, F. E., Nousek, J., O'Brien, P., Osborne, J. P., Palmer, D., Perri, M., Siegel, M., Tagliaferri, G., Klotz, A., Turpin, D., Laugier, R., Beroiz, M., Peñuela, T., Macri, L. M., Oelkers, R. J., Lambas, D. G., Vrech, R., Cabral, J., Colazo, C., Dominguez, M., Sanchez, B., Gurovich, S., Lares, M., Marshall, J. L., DePoy, D. L., Padilla, N., Pereyra, N. A., Benacquista, M., Tanvir, N. R., Wiersema, K., Levan, A. J., Steeghs, D., Hjorth, J., Fynbo, J. P. U., Malesani, D., Milvang-Jensen, B., Watson, D., Irwin, M., Fernandez, C. G., McMahon, R. G., Banerji, M., Gonzalez-Solares, E., Schulze, S., Postigo, A. de U., Thoene, C. C., Cano, Z., and Rosswog, S.

Subjects
Astrophysics - High Energy Astrophysical Phenomena, General Relativity and Quantum Cosmology
Abstract

A gravitational-wave (GW) transient was identified in data recorded by the Advanced Laser Interferometer Gravitational-wave Observatory (LIGO) detectors on 2015 September 14. The event, initially designated G184098 and later given the name GW150914, is described in detail elsewhere. By prior arrangement, preliminary estimates of the time, significance, and sky location of the event were shared with 63 teams of observers covering radio, optical, near-infrared, X-ray, and gamma-ray wavelengths with ground- and space-based facilities. In this Letter we describe the low-latency analysis of the GW data and present the sky localization of the first observed compact binary merger. We summarize the follow-up observations reported by 25 teams via private Gamma-ray Coordinates Network circulars, giving an overview of the participating facilities, the GW sky localization coverage, the timeline and depth of the observations. As this event turned out to be a binary black hole merger, there is little expectation of a detectable electromagnetic (EM) signature. Nevertheless, this first broadband campaign to search for a counterpart of an Advanced LIGO source represents a milestone and highlights the broad capabilities of the transient astronomy community and the observing strategies that have been developed to pursue neutron star binary merger events. Detailed investigations of the EM data and results of the EM follow-up campaign are being disseminated in papers by the individual teams., Comment: For Supplement, see https://arxiv.org/abs/1604.07864

Published
2016
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18. Probing the stellar wind environment of Vela X-1 with MAXI

Author

Malacaria, C., Mihara, T., Santangelo, A., Makishima, K., Matsuoka, M., Morii, M., and Sugizaki, M.

Subjects
Astrophysics - High Energy Astrophysical Phenomena
Abstract

Vela X-1 is among the best studied and most luminous accreting X-ray pulsars. The supergiant optical companion produces a strong radiatively-driven stellar wind, which is accreted onto the neutron star producing highly variable X-ray emission. A complex phenomenology, due to both gravitational and radiative effects, needs to be taken into account in order to reproduce orbital spectral variations. We have investigated the spectral and light curve properties of the X-ray emission from Vela X-1 along the binary orbit. These studies allow to constrain the stellar wind properties and its perturbations induced by the compact object. We took advantage of the All Sky Monitor MAXI/GSC data to analyze Vela X-1 spectra and light curves. By studying the orbital profiles in the $4-10$ and $10-20$ keV energy bands, we extracted a sample of orbital light curves (${\sim}15$% of the total) showing a dip around the inferior conjunction, i.e., a double-peaked shape. We analyzed orbital phase-averaged and phase-resolved spectra of both the double-peaked and the standard sample. The dip in the double-peaked sample needs $N_H\sim2\times10^{24}\,$cm$^{-2}$ to be explained by absorption solely, which is not observed in our analysis. We show how Thomson scattering from an extended and ionized accretion wake can contribute to the observed dip. Fitted by a cutoff power-law model, the two analyzed samples show orbital modulation of the photon index, hardening by ${\sim}0.3$ around the inferior conjunction, compared to earlier and later phases, hinting a likely inadequacy of this model. On the contrary, including a partial covering component at certain orbital phase bins allows a constant photon index along the orbital phases, indicating a highly inhomogeneous environment. We discuss our results in the framework of possible scenarios., Comment: 10 pages, 9 figures, accepted for publication in A&A

Published
2016
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19. Anomalously porous boulders on (162173) Ryugu as primordial materials from its parent body

Author

Sakatani, N., Tanaka, S., Okada, T., Fukuhara, T., Riu, L., Sugita, S., Honda, R., Morota, T., Kameda, S., Yokota, Y., Tatsumi, E., Yumoto, K., Hirata, N., Miura, A., Kouyama, T., Senshu, H., Shimaki, Y., Arai, T., Takita, J., Demura, H., Sekiguchi, T., Müller, T. G., Hagermann, A., Biele, J., Grott, M., Hamm, M., Delbo, M., Neumann, W., Taguchi, M., Ogawa, Y., Matsunaga, T., Wada, T., Hasegawa, S., Helbert, J., Hirata, N., Noguchi, R., Yamada, M., Suzuki, H., Honda, C., Ogawa, K., Hayakawa, M., Yoshioka, K., Matsuoka, M., Cho, Y., Sawada, H., Kitazato, K., Iwata, T., Abe, M., Ohtake, M., Matsuura, S., Matsumoto, K., Noda, H., Ishihara, Y., Yamamoto, K., Higuchi, A., Namiki, N., Ono, G., Saiki, T., Imamura, H., Takagi, Y., Yano, H., Shirai, K., Okamoto, C., Nakazawa, S., Iijima, Y., Arakawa, M., Wada, K., Kadono, T., Ishibashi, K., Terui, F., Kikuchi, S., Yamaguchi, T., Ogawa, N., Mimasu, Y., Yoshikawa, K., Takahashi, T., Takei, Y., Fujii, A., Takeuchi, H., Yamamoto, Y., Hirose, C., Hosoda, S., Mori, O., Shimada, T., Soldini, S., Tsukizaki, R., Ozaki, M., Tachibana, S., Ikeda, H., Ishiguro, M., Yabuta, H., Yoshikawa, M., Watanabe, S., and Tsuda, Y.

Published
2021
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20. Thermally altered subsurface material of asteroid (162173) Ryugu

Author

Kitazato, K., Milliken, R. E., Iwata, T., Abe, M., Ohtake, M., Matsuura, S., Takagi, Y., Nakamura, T., Hiroi, T., Matsuoka, M., Riu, L., Nakauchi, Y., Tsumura, K., Arai, T., Senshu, H., Hirata, N., Barucci, M. A., Brunetto, R., Pilorget, C., Poulet, F., Bibring, J.-P., Domingue, D. L., Vilas, F., Takir, D., Palomba, E., Galiano, A., Perna, D., Osawa, T., Komatsu, M., Nakato, A., Arai, T., Takato, N., Matsunaga, T., Arakawa, M., Saiki, T., Wada, K., Kadono, T., Imamura, H., Yano, H., Shirai, K., Hayakawa, M., Okamoto, C., Sawada, H., Ogawa, K., Iijima, Y., Sugita, S., Honda, R., Morota, T., Kameda, S., Tatsumi, E., Cho, Y., Yoshioka, K., Yokota, Y., Sakatani, N., Yamada, M., Kouyama, T., Suzuki, H., Honda, C., Namiki, N., Mizuno, T., Matsumoto, K., Noda, H., Ishihara, Y., Yamada, R., Yamamoto, K., Yoshida, F., Abe, S., Higuchi, A., Yamamoto, Y., Okada, T., Shimaki, Y., Noguchi, R., Miura, A., Hirata, N., Tachibana, S., Yabuta, H., Ishiguro, M., Ikeda, H., Takeuchi, H., Shimada, T., Mori, O., Hosoda, S., Tsukizaki, R., Soldini, S., Ozaki, M., Terui, F., Ogawa, N., Mimasu, Y., Ono, G., Yoshikawa, K., Hirose, C., Fujii, A., Takahashi, T., Kikuchi, S., Takei, Y., Yamaguchi, T., Nakazawa, S., Tanaka, S., Yoshikawa, M., Watanabe, S., and Tsuda, Y.

Published
2021
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22. Grain size effects on the infrared spectrum of mineral mixtures with dark components: new laboratory experiments to interpret low-albedo rocky planetary surfaces

Author

Poggiali, G., primary, Fossi, L., additional, Wargnier, A., additional, Beccarelli, J., additional, Brucato, J.R., additional, Barucci, M.A., additional, Beck, P., additional, Matsuoka, M., additional, Nakamura, T., additional, Merlin, F., additional, Fornasier, S., additional, Pajola, M., additional, Doressoundiram, A., additional, Gautier, T., additional, and David, G., additional

Published
2024
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23. Collisional history of Ryugu’s parent body from bright surface boulders

Author

Tatsumi, E., Sugimoto, C., Riu, L., Sugita, S., Nakamura, T., Hiroi, T., Morota, T., Popescu, M., Michikami, T., Kitazato, K., Matsuoka, M., Kameda, S., Honda, R., Yamada, M., Sakatani, N., Kouyama, T., Yokota, Y., Honda, C., Suzuki, H., Cho, Y., Ogawa, K., Hayakawa, M., Sawada, H., Yoshioka, K., Pilorget, C., Ishida, M., Domingue, D., Hirata, N., Sasaki, S., de León, J., Barucci, M. A., Michel, P., Suemitsu, M., Saiki, T., Tanaka, S., Terui, F., Nakazawa, S., Kikuchi, S., Yamaguchi, T., Ogawa, N., Ono, G., Mimasu, Y., Yoshikawa, K., Takahashi, T., Takei, Y., Fujii, A., Yamamoto, Y., Okada, T., Hirose, C., Hosoda, S., Mori, O., Shimada, T., Soldini, S., Tsukizaki, R., Mizuno, T., Iwata, T., Yano, H., Ozaki, M., Abe, M., Ohtake, M., Namiki, N., Tachibana, S., Arakawa, M., Ikeda, H., Ishiguro, M., Wada, K., Yabuta, H., Takeuchi, H., Shimaki, Y., Shirai, K., Hirata, N., Iijima, Y., Tsuda, Y., Watanabe, S., and Yoshikawa, M.

Published
2021
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24. Extraordinary luminous soft X-ray transient MAXI J0158-744 as an ignition of a nova on a very massive O-Ne white dwarf

Author

Morii, M., Tomida, H., Kimura, M., Suwa, F., Negoro, H., Serino, M., Kennea, J. A., Page, K. L., Curran, P. A., Walter, F. M., Kuin, N. P. M., Pritchard, T., Nakahira, S., Hiroi, K., Usui, R., Kawai, N., Osborne, J. P., Mihara, T., Sugizaki, M., Gehrels, N., Kohama, M., Kotani, T., Matsuoka, M., Nakajima, M., Roming, P. W. A., Sakamoto, T., Sugimori, K., Tsuboi, Y., Tsunemi, H., Ueda, Y., Ueno, S., and Yoshida, A.

Subjects
Astrophysics - High Energy Astrophysical Phenomena
Abstract

We present the observation of an extraordinary luminous soft X-ray transient, MAXI J0158-744, by the Monitor of All-sky X-ray Image (MAXI) on 2011 November 11. This transient is characterized by a soft X-ray spectrum, a short duration (1.3 x 10^3 s < \Delta T_d < 1.10 x 10^4 s), a very rapid rise (< 5.5 x 10^3 s), and a huge peak luminosity of 2 x 10^40 erg s^-1 in 0.7-7.0 keV band. With Swift observations and optical spectroscopy from the Small and Moderate Aperture Research Telescope System (SMARTS), we confirmed that the transient is a nova explosion, on a white dwarf in a binary with a Be star, located near the Small Magellanic Cloud. An extremely early turn-on of the super-soft X-ray source (SSS) phase (< 0.44 d), the short SSS phase duration of about one month, and a 0.92 keV neon emission line found in the third MAXI scan, 1296 s after the first detection, suggest that the explosion involves a small amount of ejecta and is produced on an unusually massive O-Ne white dwarf close to, or possibly over, the Chandrasekhar limit. We propose that the huge luminosity detected with MAXI was due to the fireball phase, a direct manifestation of the ignition of the thermonuclear runaway process in a nova explosion., Comment: 33 pages, 5 figures, Accepted for publication by ApJ

Published
2013
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25. Propeller-Effect Interpretation of MAXI/GSC Light Curves of 4U 1608-52 and AqlX-1 and application to XTE J1701-462

Author

Asai, K., Matsuoka, M., Mihara, T., Sugizaki, M., Serino, M., Nakahira, S., Negoro, H., Ueda, Y., and Yamaoka, K.

Subjects
Astrophysics - High Energy Astrophysical Phenomena
Abstract

We present the luminosity dwell-time distributions during the hard states of low-mass X-ray binaries containing a neutron star, 4U 1608-52 and AqlX-1, observed with MAXI/GSC. The luminosity distributions show a steep cut-off in the low-luminosity side at $\sim1.0 \times 10^{36}$ erg s$^{-1}$ in both the two sources. The cut-off implies a rapid luminosity decrease in their outburst decay phases, and the feature can be interpreted as due the propeller effect. We estimated the surface magnetic field of the neutron star to be (0.5--1.6) $\times 10^8$ G in 4U 1608-52 and (0.6--1.9) $\times 10^8$ G in AqlX-1 from the cut-off luminosity. We applied the same propeller mechanism to the similar rapid luminosity decrease observed in the transient Z-source, XTE J1701-462, with RXTE/ASM. Assuming that spin period of the neutron star is in the order of milliseconds, the observed cut-off luminosity deduces surface magnetic field in the order of $10^9$ G., Comment: 14 pages, 5 figures

Published
2013
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26. Footprints in the wind of Vela X-1 traced with MAXI

Author

Doroshenko, V., Santangelo, A., Nakahira, S., Mihara, T., Sugizaki, M., Matsuoka, M., Nakajima, M., and Makishima, K.

Subjects
Astrophysics - High Energy Astrophysical Phenomena
Abstract

The stellar wind around the compact object in luminous wind-accreting high mass X-ray binaries is expected to be strongly ionized with the X-rays coming from the compact object. The stellar wind of hot stars is mostly driven by light absorption in lines of heavier elements, and X-ray photo-ionization significantly reduces the radiative force within the so-called Stroemgren region leading to wind stagnation around the compact object. In close binaries like Vela X-1 this effect might alter the wind structure throughout the system. Using the spectral data from Monitor of All-sky X-ray Image (MAXI), we study the observed dependence of the photoelectric absorption as function of orbital phase in Vela X-1, and find that it is inconsistent with expectations for a spherically-symmetric smooth wind. Taking into account previous investigations we develop a simple model for wind structure with a stream-like photoionization wake region of slower and denser wind trailing the neutron star responsible for the observed absorption curve., Comment: 5 pages, 3 figures, accepted in A&A

Published
2013
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28. A contribution of stellar flares to the GRXE -- based on MAXI observations --

Author

Matsuoka, M., Sugizaki, M., Tsuboi, Y., Yamazaki, K., Matsumura, T., Mihara, T., Serino, M., Nakahira, S., Yamamoto, T., Ueno, S., Negoro, H., and team, MAXI

Subjects
Astrophysics - High Energy Astrophysical Phenomena
Abstract

Using unbiased observations of MAXI/GSC the potential contribution of stellar flares and CVs to GRXE luminosity is estimated in the energy range of 2 - 10 keV. Currently, a reasonable luminosity has been obtained extrapolating the number of stellar flares and that of CVs toward the Galactic ridge from those of the observed flares and CVs near the solar system. The ionized emission lines of Si to Fe are also simulated making the composite thermal spectrum which is based on MAXI observations of stellar flares and CVs. The present estimated result strongly supports a picture that the cumulative stellar flares contribute primarily to the GRXE in terms of the composite thermal spectrum with emission lines and secondary contribution is due to the thermal spectrum with high temperature from CVs.

Published
2011
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29. Spectral Lag Relations in GRB Pulses Detected with HETE-2

Author

Arimoto, M., Kawai, N., Asano, K., Hurley, K., Suzuki, M., Nakagawa, Y. E., Shimokawabe, T., Pazmino, N. V., Sato, R., Matsuoka, M., Yoshida, A., Tamagawa, T., Shirasaki, Y., Sugita, S., Takahashi, I., Atteia, J. -L., Pelangeon, A., Vanderspek, R., Graziani, C., Prigozhin, G., Villasenor, J., Jernigan, J. G., Crew, G. B., Sakamoto, T., Ricker, G. R., Woosley, S. E., Butler, N., Levine, A., Doty, J. P., Donaghy, T. Q., Lamb, D. Q., Fenimore, E., Galassi, M., Boer, M., Dezalay, J. -P., Olive, J. -F., Braga, J., Manchanda, R., and Pizzichini, G.

Subjects
Astrophysics - High Energy Astrophysical Phenomena
Abstract

Using a pulse-fit method, we investigate 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, GRB 050408) detected with the WXM and FREGATE instruments aboard the HETE-2 satellite. We find several relations for the individual GRB pulses between the spectral lag and other observables, such as the luminosity, pulse duration, and peak energy (Epeak). 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 find that the photon energy dependence for the spectral lags can reconcile the simple curvature effect model. We discuss the implication of these results from various points of view., Comment: 13 pages, 9 figures, accepted for the publication in PASJ (minor corrections)

Published
2010
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30. Antimicrobial resistance in leprosy: results of the first prospective open survey conducted by a WHO surveillance network for the period 2009–15

Author

Kriswamati, A., Al-Samie, Abdul Rahim, Issoufou, Ahamed, Tiendrebeogo, Alexandre, Kingalu, AmriMiraju, Randrianantoandro, Andriamira, Kumar, Anil, Chauffour, Aurelie, Win, Aye Aye, Pandey, Basudev, Agrawal, C.M., Widaningrum, Christiana, Schmotzer, Christine, Kafando, Christophe, Bhandari, Chuda Mani, Sema, Cynthia, Vidanagama, D.S., Scollard, David M., Beyene, Demmissew, Morelo, Eliane Faria, Kassa, Elizabeth Dizaneh, Ramarolahy, Enerantien Benoit, Claco, Eric, Villalon, Ernesto ES., Sidibe, Famoussa, Sakho, Fatoumata, Abdoulaye, Fomba, Guilengue, Francisco F., Gajete, Fransesca, Babu, Gadde Rajan, Moussa, Gado, Thakur, Garib Das, Cabanos, Gemma, Sock, Gouressi, Clugston, Greame, Zaidy, Hany, Watanabe, Haruo, Kawuma, Herman Joseph, Mallari, Irene Balenton, Goulart, Isabella Maria Bernandes, Ahamed, Issoufou, Subbanna, J., Houzeo, Jean Gabin, Luengu, Jean Norbert Mputu, Bertolli, Jeanne, Lloyd-Owen, Jonathan, Matheu, Jorge, Brunelli, José Pereira, Alzate, Juan Camilo Beltran, Neupane, Kapil Dev, Osuga, Katsunori, Yamaguchi, Kazuko, Azam, Khalid, Lin, Khin Maung, Momoudu, Kodia, Kyaw, Kyaw, Bide, Landry, Doanh, Le Huu, My, Ley Huyen, Shah, Mahesh, Kodio, Mamadou, Sidibe, Mamadou, Ebenezer, Mannam, Grossi, Maria Aparecida de Faria, Balagon, Marivic F., Canlonon, Marlience, Makino, Masahiko, Htoo, Maung Maung, Ahmed, Md Jamsheed, Nadine, Mintsey-mi-Makuth, Roferos, Florenda Orcullo, Krismawati, Hana, Thida, Mya, Htoon, Myo Thet, Neupane, K.D., Nguyen Phuc, Nhu Ha, Van, NguyenThi Hai, Hai, Ngyuen Phuc Nhu, Ishii, Norisha, Soe, Oke, Amiel, Olga, Tossou, Omar, Konare, Ousmane, Joshi, P.L., Ranganadha Rao, P.V., Krishnamurthy, Padebettu, Brennan, Patrick J., Busso, Phillipe, Bhatia, Rajesh, Rakoto Andrianarivelo, Mala, Ramdas, D.R., Chabi, Raoul, Gusmao, Renato, DjupuriIzwardy, Rita, Soares, Rosa Castalia Franca Riberio, Jhadav, Rupendra, Buhrer, Samira, Cho, Sang-Nae Ray, Jianping, Shen, Lzumi, Shinzo, Barua, Sumana, Chaitanya, Sundeep, Tiendrebeogo, Sylvestre Marie Roget, Khang, Tan Hau, Gillis, Thomas P., Mori, Toru, Vijayalakshmi, V., Kamara, Vedastus Deusdedit, Wei, Wang, Smith, W.Cairn S., Li, Wei, Lew, Woojin, Al-Qubati, Yasin, Suzuki, Yasuhiko, Nanba, Yoshio, Cambau, E., Saunderson, P., Matsuoka, M., Cole, S.T., Kai, M., Suffys, P., Rosa, P.S., Williams, D., Gupta, U.D., Lavania, M., Cardona-Castro, N., Miyamoto, Y., Hagge, D., Srikantam, A., Hongseng, W., Indropo, A., Vissa, V., Johnson, R.C., Cauchoix, B., Pannikar, V.K., Cooreman, E.A.W.D., Pemmaraju, V.R.R., and Gillini, L.

Published
2018
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31. The Truth, the Whole Truth, and Nothing but the Ground-Truth: Methods to Advance Environmental Justice and Researcher-Community Partnerships

Author

Sadd, J, Morello-Frosch, R, Pastor, M, Matsuoka, M, Prichard, M, and Carter, V

Abstract

Environmental justice advocates often argue that environmental hazards and their health effects vary by neighborhood, income, and race. To assess these patterns and advance preventive policy, their colleagues in the research world often use complex and methodologically sophisticated statistical and geospatial techniques. One way to bridge the gap between the technical work and the expert knowledge of local residents is through community-based participatory research strategies. We document how an environmental justice screening method was coupled with "ground-truthing"-a project in which community members worked with researchers to collect data across six Los Angeles neighborhoods-which demonstrated the clustering of potentially hazardous facilities, high levels of air pollution, and elevated health risks. We discuss recommendations and implications for future research and collaborations between researchers and community-based organizations. © 2013 Society for Public Health Education.

Published
2014

34. Intrinsic properties of a complete sample of HETE-2 gamma-ray bursts. A measure of the GRB rate in the Local Universe

Author

Pélangeon, A., Atteia, J. -L., Nakagawa, Y. E., Hurley, K., Yoshida, A., Vanderspek, R., Suzuki, M., Kawai, N., Pizzichini, G., Boër, M., Braga, J., Crew, G., Donaghy, T. Q., Dezalay, J. P., Doty, J., Fenimore, E. E., Galassi, M., Graziani, C., Jernigan, J. G., Lamb, D. Q., Levine, A., Manchanda, J., Martel, F., Matsuoka, M., Olive, J. -F., Prigozhin, G., Ricker, G. R., Sakamoto, T., Shirasaki, Y., Sugita, S., Takagishi, K., Tamagawa, T., Villasenor, J., Woosley, S. E., and Yamauchi, M.

Subjects
Astrophysics
Abstract

Aims: Taking advantage of the forthcoming Catalog of the HETE-2 mission, the aim of this paper is to evaluate the main properties of HETE-2 GRBs - the E_peak, the T_90 and the E_iso - in their source frames and to derive their unbiased distribution. Methods: We first construct a complete sample containing all the bursts localized by the WXM on-board HETE-2, which are selected with a uniform criterion and whose observed parameters can be constrained. We then derive the intrinsic E_peak, T_90 and E_iso distributions using their redshift when it is available, or their pseudo-redshift otherwise. We finally compute the number of GRB (N_Vmax) within the visibility volume (V_max) of each GRB, in order to derive a weight for each detected burst accounting both for the detection significance and the star formation history of the universe. Results: The unbiased distributions obtained clearly show the predominence of X-ray flashes (XRFs) in the global GRB population. We also derive the rate of local GRBs: R0^H2 > 11 Gpc-3 yr-1, which is intermediate between the local rate obtained by considering only the high-luminosity bursts (~1 Gpc-3 yr-1) and that obtained by including the low-luminosity bursts (>200 Gpc-3 yr-1)., Comment: 20 pages, 14 figures, 3 tables (editor version: 15 pages, 14 figures, tables 2 and 3 only available in electronic form at http://www.aanda.org)

Published
2008
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35. GRBS OBSERVED BY MAXI

Author

Serino, M., primary, Sakamoto, T., additional, Yoshida, A., additional, Kawai, N., additional, Morii, M., additional, Sugizaki, M., additional, Nakahira, S., additional, Negoro, H., additional, Mihara, T., additional, Nishimura, Y., additional, Ogawa, Y., additional, and Matsuoka, M., additional

Published
2020
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36. EXPLORING GROUND SEGMENTATION FROM LIDAR SCANNING-DERIVED IMAGES USING CONVOLUTIONAL NEURAL NETWORKS

Author

Lagahit, M. L. R., Li, Z., Sakaguchi, K., and Matsuoka, M.

Abstract

Recent works have attempted to extract features such as road markings from sparse mobile LiDAR scanning point cloud-derived images via convolutional neural networks (CNN). In this paper, the use of such methods for ground segmentation was explored. To begin, point clouds from each channel will be projected onto the y-z plane to generate the images that will be used for training and testing the CNN model. Then, for the main workflow, the following steps were performed for each channel: (1) point cloud-to-image conversion; (2) CNN classification; and (3) image-to-point cloud projection. Then utilizing multi-threading, each channel is processed in parallel to generate our ground-segmented sparse point cloud. Our findings have shown successful ground segmentation, achieving an f1-score of 98.9%. However, it performed 27.81% slower as compared to RANSAC. Overall, this initial investigation has demonstrated that ground segmentation from sparse point cloud-derived imagery is possible, and with further improvements to the CNN model, to make it faster, it has good potential to act as an alternative to conventional point cloud processing.

Published
2023

37. Discovery of a New X-Ray Burst/Millisecond Accreting Pulsar HETE J1900.1-2455

Author

Suzuki, M., Kawai, N., Tamagawa, T., Yoshida, A., Nakagawa, Y. E., Tanaka, K., Shirasaki, Y., Matsuoka, M., Ricker, G. R., Vanderspek, R., Butler, N., Lamb, D. Q., Graziani, C., Pizzichini, G., Sato, R., Arimoto, M., Kotoku, J., Maetou, M., and Yamauchi, M.

Subjects
Astrophysics
Abstract

A class of low-mass X-ray binary sources are known to be both X-ray burst sources and millisecond pulsars at the same time. A new source of this class was discovered by High Energy Transient Explorer 2 (HETE-2) on 14 June 2005 as a source of type-I X-ray bursts, which was named HETE J1900.1-2455. Five X-ray bursts from HETE J1900.1-2455 were observed during the summer of 2005. The time resolved spectral analysis of these bursts have revealed that their spectra are consistent with the blackbody radiation throughout the bursts. The bursts show the indication of radius expansion. The bolometric flux remains almost constant during the photospheric radius expansion while blackbody temperature dropped during the same period. Assuming that the flux reached to the Eddington limit on a standard 1.4 solar mass neutron star with a helium atmosphere, we estimate the distance to the source to be $\sim$ 4 kpc., Comment: 7 pages, 4 figures

Published
2006
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38. X-ray Flashes or soft Gamma-ray Bursts? The case of the likely distant XRF 040912

Author

Stratta, G., Basa, S., Butler, N., Atteia, J. L., Gendre, B., Pelangeon, A., Malacrino, F., Mellier, Y., Kann, D. A., Klose, S., Zeh, A., Masetti, N., Palazzi, E., Gorosabel, J., Castro-Tirado, A. J., Postigo, A. de Ugarte, Jelinek, M., Cepa, J., Castaneda, H., Martinez-Delgado, D., Boer, M., Braga, J., Crew, G., Donaghy, T. Q., Dezalay, J. -P., Doty, J., Fenimore, E. E., Galassi, M., Graziani, C., Jernigan, J. G., Kawai, N., Lamb, D. Q., Levine, A., Manchanda, J., Martel, F., Matsuoka, M., Nakagawa, Y., Olive, J. -F., Pizzichini, G., Prigozhin, G., Ricker, G., Sakamoto, T., Shirasaki, Y., Sugita, S., Suzuki, M., Takagishi, K., Tamagawa, T., Vanderspek, R., Villasenor, J., Woosley, S. E., Yamauchi, M., and Yoshida, A.

Subjects
Astrophysics
Abstract

In this work, we present a multi-wavelength study of XRF 040912, aimed at measuring its distance scale and the intrinsic burst properties. We performed a detailed spectral and temporal analysis of both the prompt and the afterglow emission and we estimated the distance scale of the likely host galaxy. We then used the currently available sample of XRFs with known distance to discuss the connection between XRFs and classical Gamma-ray Bursts (GRBs). We found that the prompt emission properties unambiguously identify this burst as an XRF, with an observed peak energy of E_p=17+/-13 keV and a burst fluence ratio S(2-30keV)/S(30-400keV)>1. A non-fading optical source with R~24 mag and with an apparently extended morphology is spatially consistent with the X-ray afterglow, likely the host galaxy. XRF 040912 is a very dark burst since no afterglow optical counterpart is detected down to R>25 mag (3 sigma limiting magnitude) at 13.6 hours after the burst. The host galaxy spectrum detected from 3800A to 10000A, shows a single emission line at 9552A. The lack of any other strong emission lines blue-ward of the detected one and the absence of the Ly alpha cut-off down to 3800A are consistent with the hypothesis of the [OII] line at redshift z=1.563+/-0.001. The intrinsic spectral properties rank this XRF among the soft GRBs in the E_peak-E_iso diagram. Similar results were obtained for most XRFs at known redshift. Only XRF 060218 and XRF 020903 represent a good example of instrinsic XRF(i-XRF) and are possibly associated with a different progenitor population. This scenario may calls for a new definition of XRFs., Comment: 10 pages, 7 figures, accepted for publication in Astronomy & Astrophysics

Published
2006
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39. HETE-2 Localizations and Observations of Four Short Gamma-Ray Bursts: GRBs 010326B, 040802, 051211 and 060121

Author

Donaghy, T. Q., Lamb, D. Q., Sakamoto, T., Norris, J. P., Nakagawa, Y., Villasenor, J., Atteia, J. -L., Vanderspek, R., Graziani, C., Kawai, N., Ricker, G. R., Crew, G. B., Doty, J., Prigozhin, G., Jernigan, J. G., Shirasaki, Y., Suzuki, M., Butler, N., Hurley, K., Tamagawa, T., Yoshida, A., Matsuoka, M., Fenimore, E. E., Galassi, M., Boer, M., Dezalay, J. -P., Olive, J. -F., Levine, A., Martel, F., Morgan, E., Sato, R., Woosley, S. E., Braga, J., Manchanda, R., Pizzichini, G., Takagishi, K., and Yamauchi, M.

Subjects
Astrophysics
Abstract

Here we report the localizations and properties of four short-duration GRBs localized by the High Energy Transient Explorer 2 satellite (HETE-2): GRBs 010326B, 040802, 051211 and 060121, all of which were detected by the French Gamma Telescope (Fregate) and localized with the Wide-field X-ray Monitor (WXM) and/or Soft X-ray Camera (SXC) instruments. We discuss eight possible criteria for determining whether these GRBs are "short population bursts" (SPBs) or "long population bursts" (LPBs). These criteria are (1) duration, (2) pulse widths, (3) spectral hardness, (4) spectral lag, (5) energy Egamma radiated in gamma rays (or equivalently, the kinetic energy E_KE of the GRB jet), (6) existence of a long, soft bump following the burst, (7) location of the burst in the host galaxy, and (8) type of host galaxy. In particular, we have developed a likelihood method for determining the probability that a burst is an SPB or a LPB on the basis of its T90 duration alone. A striking feature of the resulting probability distribution is that the T90 duration at which a burst has an equal probability of being a SPB or a LPB is T90 = 5 s, not T90 = 2 s, as is often used. All four short-duration bursts discussed in detail in this paper have T90 durations in the Fregate 30-400 keV energy band of 1.90, 2.31, 4.25, and 1.97 sec, respectively, yielding probabilities P(S|T90) = 0.97, 0.91, 0.60, and 0.95 that these bursts are SPBs on the basis of their T90 durations alone. All four bursts also have spectral lags consistent with zero. These results provide strong evidence that all four GRBs are SPBs (abstract continues)., Comment: 60 pages, 19 figures, submitted to ApJ; added new references and corrected typos

Published
2006

40. Discovery of the short gamma-ray burst GRB 050709

Author

Villasenor, J. S., Lamb, D. Q., Ricker, G. R., Atteia, J. -L., Kawai, N., Butler, N., Nakagawa, Y., Jernigan, J. G., Boer, M., Crew, G. B., Donaghy, T. Q., Doty, J., Fenimore, E. E., Galassi, M., Graziani, C., Hurley, K., Levine, A., Martel, F., Matsuoka, M., Olive, J. -F., Prigozhin, G., Sakamoto, T., Shirasaki, Y., Suzuki, M., Tamagawa, T., Vanderspek, R., Woosley, S. E., Yoshida, A., Braga, J., Manchanda, R., Pizzichini, G., Takagishi, K., and Yamauchi, M.

Subjects
Astrophysics
Abstract

Gamma-Ray Bursts (GRBs) fall into two classes: short-hard and long-soft bursts. The latter are now known to have X-ray and optical afterglows, to occur at cosmological distances in star-forming galaxies, and to be associated with the explosion of massive stars. In contrast, the distance scale, the energy scale, and the progenitors of short bursts have remained a mystery. Here we report the discovery of a short-hard burst whose accurate localization has led to follow-up observations that have identified the X-ray afterglow and (for the first time) the optical afterglow of a short-hard burst. These, in turn, have led to identification of the host galaxy of the burst as a late-type galaxy at z=0.16 showing that at least some short-hard bursts occur at cosmological distances in the outskirts of galaxies, and are likely to be due to the merging of compact binaries., Comment: 19 pages, 4 figures. Submitted to Nature

Published
2005
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41. HETE-2 Observation of two gamma-ray bursts at z > 3

Author

Atteia, J. -L., Kawai, N., Vanderspek, R., Pizzichini, G., Ricker, G. R., Barraud, C., Boer, M., Braga, J., Butler, N., Cline, T., Crew, G. B., Dezalay, J. -P., Donaghy, T. Q., Doty, J., Fenimore, E. E., Galassi, M., Graziani, C., Hurley, K., Jernigan, J. G., Lamb, D. Q., Levine, A., Manchanda, R., Martel, F., Matsuoka, M., Morgan, E., Nakagawa, Y., Olive, J. -F., Prigozhin, G., Sakamoto, T., Sato, R., Shirasaki, Y., Suzuki, M., Takagishi, K., Tamagawa, T., Torii, K., Villasenor, J., Woosley, S. E., Yamauchi, M., and Yoshida, A.

Subjects
Astrophysics
Abstract

GRB 020124 and GRB 030323 constitute half the sample of gamma-ray bursts with a measured redshift greater than 3. This paper presents the temporal and spectral properties of these two gamma-ray bursts detected and localized with HETE-2. While they have nearly identical redshifts (z=3.20 for GRB 020124, and z=3.37 for GRB 030323), these two GRBs span about an order of magnitude in fluence, thus sampling distinct regions of the GRB luminosity function. The properties of these two bursts are compared with those of the bulk of the GRB population detected by HETE-2. We also discuss the energetics of GRB 020124 and GRB 030323 and show that they are compatible with the Epeak - Eiso relation discovered by Amati et al. (2002). Finally, we compute the maximum redshifts at which these bursts could have been detected by HETE-2 and we address various issues connected with the detection and localization of high-z GRBs., Comment: 19 pages, 4 figures, submitted to ApJ

Published
2005
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42. XMM observations of the high-redshift quasar RXJ1028.6-0844 at z=4.276: soft X-ray spectral flattening

Author

Yuan, W., Fabian, A. C., Celotti, A., McMahon, R. G., and Matsuoka, M.

Subjects
Astrophysics
Abstract

We present results from a new XMM-Newton observation of the high-redshift quasar RXJ1028.6-0844 at a redshift of 4.276. The soft X-ray spectral flattening, as reported by a study with ASCA previously (Yuan et al. 2000, ApJ 545, 625), is confirmed to be present, however, with reduced column density when modelled by absorption. The inferred column density for absorption intrinsic to the quasar is 2.1(+0.4-0.3)x10^22 (cm^-2) for cold matter, and higher for ionised gas. The spectral flattening shows remarkable similarity with those of two similar objects, GB1428+4217 (Worsley et al. 2004, MNRAS 350, L67) and PMNJ0525-3343 (Worsley et al. 2004, MNRAS 350, 207). The results improve upon those obtained from a previous short-exposure observation for RXJ1028.6-0844 with XMM-Newton (Grupe et al. 2004, AJ 127, 1). A comparative study of the two XMM-Newton observations reveals a change in the power-law photon index from Gamma ~1.3 to 1.5 on timescales of about one year. A tentative excess emission feature in the rest-frame 5-10keV band is suggested, which is similar to that marginally suggested for GB1428+4217., Comment: 9 pages, accepted for publication in MNRAS; minor changes (added footnote commenting on the use of the F-test, added references)

Published
2004
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43. Global Characteristics of X-Ray Flashes and X-Ray-Rich GRBs Observed by HETE-2

Author

Sakamoto, T., Lamb, D. Q., Graziani, C., Donaghy, T. Q., Suzuki, M., Ricker, G., Atteia, J-L., Kawai, N., Yoshida, A., Shirasaki, Y., Tamagawa, T., Torii, K., Matsuoka, M., Fenimore, E. E., Galassi, M., Doty, J., Vanderspek, R., Crew, G. B., Villasenor, J., Butler, N., Prigozhin, G., Jernigan, J. G., Barraud, C., Boer, M., Dezalay, J-P., Olive, J-F., Hurley, K., Levine, A., Monnelly, G., Martel, F., Morgan, E., Woosley, S. E., Cline, T., Braga, J., Manchanda, R., Pizzichini, G., Takagishi, K., and Yamauchi, M.

Subjects
Astrophysics
Abstract

We describe and discuss the global properties of 45 gamma-ray bursts (GRBs) observed by HETE-2 during the first three years of its mission, focusing on the properties of X-Ray Flashes (XRFs) and X-ray-rich GRBs (XRRs). We find that the numbers of XRFs, XRRs, and GRBs are comparable. We find that the durations and the sky distributions of XRFs and XRRs are similar to those of GRBs. We also find that the spectral properties of XRFs and XRRs are similar to those of GRBs, except that the values of the peak energy $E^{\rm obs}_{\rm peak}$ of the burst spectrum in $\nu F_\nu$, the peak energy flux $\Fp$, and the energy fluence $S_E$ of XRFs are much smaller -- and those of XRRs are smaller -- than those of GRBs. Finally, we find that the distributions of all three kinds of bursts form a continuum in the [$S_E$(2-30 keV),$S_E$(30-400) keV]-plane, the [$S_E$(2-400 keV), $E_{\rm peak}$]-plane, and the [$F_{\rm peak}$(50-300 keV), $E_{\rm peak}$]-plane. These results provide strong evidence that all three kinds of bursts arise from the same phenomenon., Comment: 33 pages, 15 figures, submitted to ApJ

Published
2004
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44. High Energy Observations of XRF 030723: Evidence for an Off-axis Gamma-Ray Burst?

Author

Butler, N. R., Sakamoto, T., Suzuki, M., Kawai, N., Lamb, D. Q., Graziani, C., Donaghy, T. Q., Dullighan, A., Vanderspek, R., Crew, G. B., Ford, P., Ricker, G., Atteia, J-L., Yoshida, A., Shirasaki, Y., Tamagawa, T., Torii, K., Matsuoka, M., Fenimore, E. E., Galassi, M., Doty, J., Villasenor, J., Prigozhin, G., Jernigan, J. G., Barraud, C., Boer, M., Dezalay, J-P., Olive, J-F., Hurley, K., Levine, A., Martel, F., Morgan, E., Woosley, S. E., Cline, T., Braga, J., Manchanda, R., and Pizzichini, G.

Subjects
Astrophysics
Abstract

We report High Energy Transient Explorer 2 (HETE-2) Wide Field X-ray Monitor/French Gamma Telescope observations of XRF030723 along with observations of the XRF afterglow made using the 6.5m Magellan Clay telescope and the Chandra X-ray Observatory. The observed peak energy E_pk_obs of the nu F_nu burst spectrum is found to lie within (or below) the WXM 2-25 keV passband at 98.5% confidence, and no counts are detected above 30 keV. Our best fit value is E_pk_obs=8.4+3.5/-3.4 keV. The ratio of X-ray to Gamma-ray flux for the burst follows a correlation found for GRBs observed with HETE-2, and the duration of the burst is similar to that typical of long-duration GRBs. If we require that the burst isotropic equivalent energy E_iso and E_pk_rest satisfy the relation discovered by Amati et al. (2002), a redshift of z=0.38+0.36/-0.18 can be determined, in agreement with constraints determined from optical observations. We are able to fit the X-ray afterglow spectrum and to measure its temporal fade. Although the best-fit fade is shallower than the concurrent fade in the optical, the spectral similarity between the two bands indicates that the X-ray fade may actually trace the optical fade. If this is the case, the late time rebrightening observed in the optical cannot be due to a supernova bump. We interpret the prompt and afterglow X-ray emission as arising from a jetted GRB observed off-axis and possibly viewed through a complex circumburst medium due to a progenitor wind., Comment: 14 pages, 9 figures, to appear in ApJ

Published
2004
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45. HETE Observations of the Gamma-Ray Burst GRB030329: Evidence for an Underlying Soft X-ray Component

Author

Vanderspek, R., Sakamoto, T., Barraud, C., Tamagawa, T., Graziani, C., Suzuki, M., Shirasaki, Y., Prigozhin, G., Villasenor, J., Jernigan, J. G., Crew, G. B., Atteia, J. -L., Hurley, K., Kawai, N., Lamb, D. Q., Ricker, G. R., Woosley, S. E., Butler, N., Doty, J. P., Dullighan, A., Donaghy, T. Q., Fenimore, E. E., Galassi, M., Pizzichini, G., Matsuoka, M ., Takagishi, K., Torii, K., Yoshida, A., Boer, M., Dezalay, J. -P., Olive, J. -F., Braga, J., and Manchanda, R.

Subjects
Astrophysics
Abstract

An exceptionally intense gamma-ray burst, GRB030329, was detected and localized by the instruments on board the High Energy Transient Explorer satellite (HETE) at 11:37:14 UT on 29 March 2003. The burst consisted of two \~10s pulses of roughly equal brightness and an X-ray tail lasting >100s. The energy fluence in the 30-400 keV energy band was 1.08e-4 erg/cm2, making GRB030329 one of the brightest GRBs ever detected. Communication of a 2 arcmin error box 73 minutes after the burst allowed the rapid detection of a counterpart in the optical, X-ray, radio and the ensuing discovery of a supernova with most unusual characteristics. Analyses of the burst lightcurves reveal the presence of a distinct, bright, soft X-ray component underlying the main GRB: the 2-10 keV fluence of this component is ~7e-6 erg/cm2. The main pulses of GRB030329 were preceded by two soft, faint, non-thermal bumps. We present details of the HETE observations of GRB030329., Comment: 22 pages, 5 figures, to be published in ApJ 617, no. 2 (10 December 2004). Referee comments have been incorporated; results of improved spectral analysis are included

Published
2004
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46. Design and Performance of the Wide-Field X-Ray Monitor on Board the High-Energy Transient Explorer 2

Author

Shirasaki, Y., Kawai, N., Yoshida, A., Matsuoka, M., Tamagawa, T., Torii, K., Sakamoto, T., Suzuki, M., Urata, Y., Sato, R., Nakagawa, Y., Takahashi, D., Fenimore, E. E., Galassi, M., Lamb, D. Q., Graziani, C., Donaghy, T. Q., Vanderspek, R., Yamauchi, M., Takagishi, K., and Hatsukade, I.

Subjects
Astrophysics
Abstract

The Wide-field X-ray Monitor (WXM) is one of the scientific instruments carried on the High Energy Transient Explorer 2 (HETE-2) satellite launched on 2000 October 9. HETE-2 is an international mission consisting of a small satellite dedicated to provide broad-band observations and accurate localizations of gamma-ray bursts (GRBs). A unique feature of this mission is its capability to determine and transmit GRB coordinates in almost real-time through the burst alert network. The WXM consists of three elements: four identical Xe-filled one-dimensional position-sensitive proportional counters, two sets of one-dimensional coded apertures, and the main electronics. The WXM counters are sensitive to X-rays between 2 keV and 25 keV within a field-of-view of about 1.5 sr, with a total detector area of about 350 cm$^2$. The in-flight triggering and localization capability can produce a real-time GRB location of several to 30 arcmin accuracy, with a limiting sensitivity of $10^{-7}$ erg cm$^{-2}$. In this report, the details of the mechanical structure, electronics, on-board software, ground and in-flight calibration, and in-flight performance of the WXM are discussed., Comment: 28 pages, 24 figures

Published
2003
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47. Highlights of the HETE-2 Mission

Author

Lamb, D. Q., Ricker, G. R., Atteia, J. -L., Barraud, C., Boer, M., Braga, J., Butler, N., Cline, T., Crew, G. B., Dezalay, J. -P., Donaghy, T. Q., Doty, J. P., Dullighan, A., Fenimore, E. E., Galassi, M., Graziani, C., Hurley, K., Jernigan, J. G., Kawai, N., Levine, A., Manchanda, R., Matsuoka, M., Martel, F., Monnelly, G., Morgan, E., Olive, J. -F., Pizzichini, G., Prigozhin, G., Sakamoto, T., Shirasaki, Y., Suzuki, M., Takagishi, K., Tamagawa, T., Torii, K., Vanderspek, R., Vedrenne, G., Villasenor, J., Woosley, S. E., Yamauchi, M., and Yoshida, A.

Subjects
Astrophysics
Abstract

The HETE-2 mission has been highly productive. It has observed more than 250 GRBs so far. It is currently localizing 25 - 30 GRBs per year, and has localized 43 GRBs to date. Twenty-one of these localizations have led to the detection of X-ray, optical, or radio afterglows, and as of now, 11 of the bursts with afterglows have redshift determinations. HETE-2 has also observed more than 45 bursts from soft gamma-ray repeaters, and more than 700 X-ray bursts. HETE-2 has confirmed the connection between GRBs and Type Ic supernovae, a singular achievement and certainly one of the scientific highlights of the mission so far. It has provided evidence that the isotropic-equivalent energies and luminosities of GRBs may be correlated with redshift; such a correlation would imply that GRBs and their progenitors evolve strongly with redshift. Both of these results have profound implications for the nature of GRB progenitors and for the use of GRBs as a probe of cosmology and the early universe. HETE-2 has placed severe constraints on any X-ray or optical afterglow of a short GRB. It has made it possible to explore the previously unknown behavior optical afterglows at very early times, and has opened up the era of high-resolution spectroscopy of GRB optical afterglows. It is also solving the mystery of "optically dark" GRBs, and revealing the nature of X-ray flashes (XRFs)., Comment: 12 pages, 6 figures, to appear in proc. 2nd VERITAS Symposium on TeV Astrophysics, Chicago, Illinois; revised text, added refs

Published
2003
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48. Scientific Highlights of the HETE-2 Mission

Author

Lamb, D. Q., Ricker, G. R., Atteia, J-L., Barraud, C., Boer, M., Braga, J., Butler, N., Cline, T., Crew, G. B., Dezalay, J. -P., Donaghy, T. Q., Doty, J. P., Dullighan, A., Fenimore, E. E., Galassi, M., Graziani, C., Hurley, K., Jernigan, J. G., Kawai, N., Levine, A., Manchanda, R., Matsuoka, M., Martel, F., Monnelly, G., Morgan, G., Olive, J. -F., Pizzichini, G., Prigozhin, G., Sakamoto, T., Shirasaki, Y., Suzuki, M., Takagishi, K., Tamagawa, T., Torii, K., Vanderspek, R., Vedrenne, G., Villasenor, J., Woosley, S. E., Yamauchi, M., and Yoshida, A.

Subjects
Astrophysics
Abstract

The HETE-2 mission has been highly productive. It has observed more than 250 GRBs so far. It is currently localizing 25 - 30 GRBs per year, and has localized 43 GRBs to date. Twenty-one of these localizations have led to the detection of X-ray, optical, or radio afterglows, and as of now, 11 of the bursts with afterglows have known redshifts. HETE-2 has confirmed the connection between GRBs and Type Ic supernovae, a singular achievement and certainly one of the scientific highlights of the mission so far. It has provided evidence that the isotropic-equivalent energies and luminosities of GRBs are correlated with redshift, implying that GRBs and their progenitors evolve strongly with redshift. Both of these results have profound implications for the nature of GRB progenitors and for the use of GRBs as a probe of cosmology and the early universe. HETE-2 has placed severe constraints on any X-ray or optical afterglow of a short GRB. It is also solving the mystery of "optically dark' GRBs, and revealing the nature of X-ray flashes., Comment: 10 pages, 9 figures, to appear in proc. "The Restless High-Energy Universe", Royal Tropical Institute, Amsterdam; revised text, added refs

Published
2003
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49. HETE-2 Observations of the Extremely Soft X-Ray Flash XRF 020903

Author

Sakamoto, T., Lamb, D. Q., Graziani, C., Donaghy, T. Q., Suzuki, M., Ricker, G., Atteia, J-L., Kawai, N., Yoshida, A., Shirasaki, Y., Tamagawa, T., Torii, K., Matsuoka, M., Fenimore, E. E., Galassi, M., Tavenner, T., Doty, J., Vanderspek, R., Crew, G. B., Villasenor, J., Butler, N., Prigozhin, G., Jernigan, J. G., Barraud, C., Boer, M., Dezalay, J-P., Olive, J-F., Hurley, K., Levine, A., Monnelly, G., Martel, F., Morgan, E., Woosley, S. E., Cline, T., Braga, J., Manchanda, R., Pizzichini, G., Takagishi, K., and Yamauchi, M.

Subjects
Astrophysics
Abstract

We report HETE-2 WXM/FREGATE observations of the X-ray flash, XRF 020903. This event was extremely soft: the ratio log(S_X/S_gamma) = 0.7, where S_X and S_gamma are the fluences in the 2-30 and 30-400 keV energy bands, is the most extreme value observed so far by HETE-2. In addition, the spectrum has an observed peak energy E^{obs}_{peak} < 5.0 keV (99.7 % probability upper limit) and no photons were detected above ~10 keV. The burst is shorter at higher energies, which is similar to the behavior of long GRBs. We consider the possibility that the burst lies at very high redshift and that the low value of E^{obs}_{peak} is due to the cosmological redshift, and show that this is very unlikely. We find that the properties of XRF 020903 are consistent with the relation between the fluences S(7-30 keV) and S(30-400 keV) found by Barraud et al. for GRBs and X-ray-rich GRBs, and are consistent with the extension by a decade of the hardness-intensity correlation (Mallozzi et al. 1995) found by the same authors. Assuming that XRF 020903 lies at a redshift z = 0.25 as implied by the host galaxy of the candidate optical and radio afterglows of this burst, we find that the properties of XRF 020903 are consistent with an extension by a factor ~300 of the relation between the isotropic-equivalent energy E_iso and the peak E_peak of the nu F_nu spectrum (in the source frame of the burst) found by Amati et al. for GRBs. The results presented in this paper therefore provide evidence that XRFs, X-ray-rich GRBs, and GRBs form a continuum and are a single phenomenon. The results also impose strong constraints on models of XRFs and X-ray-rich GRBs., Comment: 32 pages, 12 figures, revised, accepted by ApJ

Published
2003
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50. HETE-2 Localization and Observation of the Bright, X-Ray-Rich Gamma-Ray Burst GRB021211

Author

Crew, G. B., Lamb, D. Q., Ricker, G. R., Atteia, J. -L., Kawai, N., Vanderspek, R., Villasenor, J., Doty, J., Prigozhin, G., Jernigan, J. G., Graziani, C., Shirasaki, Y., Sakamoto, T., Suzuki, M., Butler, N., Hurley, K., Tamagawa, T., Yoshida, A., Matsuoka, M., Fenimore, E. E., Galassi, M., Barraud, C., Boer, M., Dezalay, J. -P., Olive, J. -F., Levine, A., Monnelly, G., Martel, F., Morgan, E., Donaghy, T. Q., Torii, K., Woosley, S. E., Cline, T., Braga, J., Manchanda, R., Pizzichini, G., Takagishi, K., and Yamauchi, M.

Subjects
Astrophysics
Abstract

A bright, x-ray-rich GRB was detected by HETE-2 at 11:18:34.03 UT on 11 Dec 2002. The WXM localization was to 14' and relayed to the GCN 22 s after the start of the burst. The ground SXC localization was within 2' of R.A. 08h 09m 00s, Dec 06d 44' 20" (J2000). GRB021211 consists of a single, FRED-like pulse with t90s of 2.3 s (85-400 keV) and 8.5 s (2-10 keV). The peak photon number and photon energy fluxes in the 2-400 keV band, are 34.0 +/- 1.8 ph cm^-2 s^-1 and 1.68 +/- 0.11 x 10^-6 erg cm^-2 s^-1, respectively. The energy fluences in the 2-30 keV and 30-400 kev energy bands are S_X = 1.36 +/- 0.05 x 10^-6 erg cm^-2 and S_gamma 2.17 +/- 0.15 x 10^-6 erg cm^-2, respectively. Thus GRB021211 is an X-ray-rich GRB (S_X/S_gamma = 0.63 > 0.32). The spectrum is well-fit by a Band function (alpha = -0.805, beta = -2.37, E_peak = 46.8 keV). The prompt localization allowed the detection of an optical afterglow for what would otherwise have been an ``optically dark'' GRB. GRB 021211 demonstrates that some fraction of burst afterglows are ``optically dark'' because their optical afterglows at times > 1 hr after the burst are very faint, and thus have often escaped detection. GRB 021211 shows that such ``optically dim'' bursts can have very bright afterglows at times < 20 min after the burst., Comment: 21 pages, 4 figures, accepted by ApJ, abstract. condensed; revised

Published
2003
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