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11 results on '"Shimizu I"'

1. Combined Pre-supernova Alert System with KamLAND and Super-Kamiokande

Author

Abe, S, Eizuka, M, Futagi, S, Gando, A, Gando, Y, Goto, S, Hachiya, T, Hata, K, Ichimura, K, Ieki, S, Ikeda, H, Inoue, K, Ishidoshiro, K, Kamei, Y, Kawada, N, Kishimoto, Y, Koga, M, Kurasawa, M, Mitsui, T, Miyake, H, Morita, D, Nakahata, T, Nakajima, R, Nakamura, K, Nakamura, R, Nakane, J, Ozaki, H, Saito, K, Sakai, T, Shimizu, I, Shirai, J, Shiraishi, K, Shoji, R, Suzuki, A, Takeuchi, A, Tamae, K, Watanabe, H, Watanabe, K, Yoshida, S, Umehara, S, Fushimi, K, Kotera, K, Urano, Y, Berger, BE, Fujikawa, BK, Learned, JG, Maricic, J, Fu, Z, Smolsky, J, Winslow, LA, Efremenko, Y, Karwowski, HJ, Markoff, DM, Tornow, W, Dell’Oro, S, O’Donnell, T, Detwiler, JA, Enomoto, S, Decowski, MP, Weerman, KM, Grant, C, Song, H, Li, A, Axani, SN, Garcia, M, Collaboration, The KamLAND, Abe, K, Bronner, C, Hayato, Y, Hiraide, K, Hosokawa, K, Ieki, K, Ikeda, M, Kameda, J, Kanemura, Y, Kaneshima, R, Kashiwagi, Y, Kataoka, Y, Miki, S, Mine, S, Miura, M, Moriyama, S, Nakahata, M, Nakano, Y, Nakayama, S, Noguchi, Y, Sato, K, Sekiya, H, Shiba, H, Shimizu, K, Shiozawa, M, Sonoda, Y, Suzuki, Y, Takeda, A, Takemoto, Y, Tanaka, H, Yano, T, and Han, S

Subjects
Nuclear and Plasma Physics, Particle and High Energy Physics, Physical Sciences, Astronomical and Space Sciences, Atomic, Molecular, Nuclear, Particle and Plasma Physics, Physical Chemistry (incl. Structural), Astronomy & Astrophysics, Astronomical sciences, Particle and high energy physics, Space sciences
Abstract

Preceding a core-collapse supernova (CCSN), various processes produce an increasing amount of neutrinos of all flavors characterized by mounting energies from the interior of massive stars. Among them, the electron antineutrinos are potentially detectable by terrestrial neutrino experiments such as KamLAND and Super-Kamiokande (SK) via inverse beta decay interactions. Once these pre-supernova (pre-SN) neutrinos are observed, an early warning of the upcoming CCSN can be provided. In light of this, KamLAND and SK, both located in the Kamioka mine in Japan, have been monitoring pre-SN neutrinos since 2015 and 2021, respectively. Recently, we performed a joint study between KamLAND and SK on pre-SN neutrino detection. A pre-SN alert system combining the KamLAND detector and the SK detector was developed and put into operation, which can provide a supernova alert to the astrophysics community. Fully leveraging the complementary properties of these two detectors, the combined alert is expected to resolve a pre-SN neutrino signal from a 15 M ⊙ star within 510 pc of the Earth at a significance level corresponding to a false alarm rate of no more than 1 per century. For a Betelgeuse-like model with optimistic parameters, it can provide early warnings up to 12 hr in advance.

Published
2024

2. Search for Supernova Neutrinos and Constraint on the Galactic Star Formation Rate with the KamLAND Data

Author

Abe, S, Asami, S, Eizuka, M, Futagi, S, Gando, A, Gando, Y, Gima, T, Goto, A, Hachiya, T, Hata, K, Hosokawa, K, Ichimura, K, Ieki, S, Ikeda, H, Inoue, K, Ishidoshiro, K, Kamei, Y, Kawada, N, Kishimoto, Y, Koga, M, Kurasawa, M, Maemura, N, Mitsui, T, Miyake, H, Nakahata, T, Nakamura, K, Nakamura, R, Ozaki, H, Sakai, T, Sambonsugi, H, Shimizu, I, Shirai, J, Shiraishi, K, Suzuki, A, Suzuki, Y, Takeuchi, A, Tamae, K, Watanabe, H, Yoshida, Y, Obara, S, Ichikawa, A, Yoshida, S, Umehara, S, Fushimi, K, Kotera, K, Urano, Y, Berger, BE, Fujikawa, BK, Learned, JG, Maricic, J, Axani, SN, Winslow, LA, Fu, Z, Smolsky, J, Efremenko, Y, Karwowski, HJ, Markoff, DM, Tornow, W, Li, A, Detwiler, JA, Enomoto, S, Decowski, MP, Grant, C, Song, H, O’Donnell, T, and Dell’Oro, S

Subjects
Astronomical and Space Sciences, Atomic, Molecular, Nuclear, Particle and Plasma Physics, Physical Chemistry (incl. Structural), Astronomy & Astrophysics
Abstract

We present the results of a search for core-collapse supernova neutrinos, using long-term KamLAND data from 2002 March 9 to 2020 April 25. We focus on the electron antineutrinos emitted from supernovae in the energy range of 1.8-111 MeV. Supernovae will make a neutrino event cluster with the duration of ∼10 s in the KamLAND data. We find no neutrino clusters and give the upper limit on the supernova rate to be 0.15 yr−1 with a 90% confidence level. The detectable range, which corresponds to a >95% detection probability, is 40-59 kpc and 65-81 kpc for core-collapse supernovae and failed core-collapse supernovae, respectively. This paper proposes to convert the supernova rate obtained by the neutrino observation to the Galactic star formation rate. Assuming a modified Salpeter-type initial mass function, the upper limit on the Galactic star formation rate is

Published
2022

3. A Search for Correlated Low-energy Electron Antineutrinos in KamLAND with Gamma-Ray Bursts

Author

Abe, S, Asami, S, Gando, A, Gando, Y, Gima, T, Goto, A, Hachiya, T, Hata, K, Hosokawa, K, Ichimura, K, Ieki, S, Ikeda, H, Inoue, K, Ishidoshiro, K, Kamei, Y, Kawada, N, Kishimoto, Y, Kinoshita, T, Koga, M, Maemura, N, Mitsui, T, Miyake, H, Nakamura, K, Nakamura, R, Ozaki, H, Sakai, T, Sambonsugi, H, Shimizu, I, Shirai, J, Shiraishi, K, Suzuki, A, Suzuki, Y, Takeuchi, A, Tamae, K, Eizuka, M, Kurasawa, M, Nakahata, T, Futagi, S, Watanabe, H, Yoshida, Y, Obara, S, Ichikawa, AK, Yoshida, S, Umehara, S, Fushimi, K, Berger, BE, Fujikawa, BK, Learned, JG, Maricic, J, Axani, SN, Smolsky, J, Laber-Smith, C, Winslow, LA, Fu, Z, Ouellet, J, Efremenko, Y, Karwowski, HJ, Markoff, DM, Tornow, W, Li, A, Detwiler, JA, Enomoto, S, Decowski, MP, Grant, C, Song, H, O’Donnell, T, and Dell’Oro, S

Subjects
Astronomical and Space Sciences, Atomic, Molecular, Nuclear, Particle and Plasma Physics, Physical Chemistry (incl. Structural), Astronomy & Astrophysics
Abstract

We present the results of a time-coincident event search for low-energy electron antineutrinos in the KamLAND detector with gamma-ray bursts (GRBs) from the Gamma-ray Coordinates Network and Fermi Gamma-ray Burst Monitor. Using a variable coincidence time window of ±500 s plus the duration of each GRB, no statistically significant excess above the background is observed. We place the world's most stringent 90% confidence level upper limit on the electron antineutrino fluence below 17.5 MeV. Assuming a Fermi-Dirac neutrino energy spectrum from the GRB source, we use the available redshift data to constrain the electron antineutrino luminosity and effective temperature.

Published
2022

4. Limits on Astrophysical Antineutrinos with the KamLAND Experiment

Author

Abe, S, Asami, S, Gando, A, Gando, Y, Gima, T, Goto, A, Hachiya, T, Hata, K, Hayashida, S, Hosokawa, K, Ichimura, K, Ieki, S, Ikeda, H, Inoue, K, Ishidoshiro, K, Kamei, Y, Kawada, N, Kishimoto, Y, Kinoshita, T, Koga, M, Maemura, N, Mitsui, T, Miyake, H, Nakamura, K, Nakamura, R, Ozaki, H, Sakai, T, Sambonsugi, H, Shimizu, I, Shirahata, Y, Shirai, J, Shiraishi, K, Suzuki, A, Suzuki, Y, Takeuchi, A, Tamae, K, Ueshima, K, Wada, Y, Watanabe, H, Yoshida, Y, Obara, S, Ichikawa, AK, Kozlov, A, Chernyak, D, Takemoto, Y, Yoshida, S, Umehara, S, Fushimi, K, Hirata, S, Nakamura, KZ, Yoshida, M, Berger, BE, Fujikawa, BK, Learned, JG, Maricic, J, Axani, SN, Winslow, LA, Fu, Z, Ouellet, J, Efremenko, Y, Karwowski, HJ, Markoff, DM, Tornow, W, Li, A, Detwiler, JA, Enomoto, S, Decowski, MP, Grant, C, O’Donnell, T, and Dell’Oro, S

Subjects
Astronomical and Space Sciences, Atomic, Molecular, Nuclear, Particle and Plasma Physics, Physical Chemistry (incl. Structural), Astronomy & Astrophysics
Abstract

We report on a search for electron antineutrinos ( ) from astrophysical sources in the neutrino energy range 8.3-30.8 MeV with the KamLAND detector. In an exposure of 6.72 kton-year of the liquid scintillator, we observe 18 candidate events via the inverse beta decay reaction. Although there is a large background uncertainty from neutral current atmospheric neutrino interactions, we find no significant excess over background model predictions. Assuming several supernova relic neutrino spectra, we give upper flux limits of 60-110 cm-2 s-1 (90% confidence level, CL) in the analysis range and present a model-independent flux. We also set limits on the annihilation rates for light dark matter pairs to neutrino pairs. These data improve on the upper probability limit of 8B solar neutrinos converting into , (90% CL) assuming an undistorted shape. This corresponds to a solar flux of 60 cm-2 s-1 (90% CL) in the analysis energy range.

Published
2022

5. Search for Solar Flare Neutrinos with the KamLAND Detector

Author

Abe, S, Asami, S, Gando, A, Gando, Y, Gima, T, Goto, A, Hachiya, T, Hata, K, Hayashida, S, Hosokawa, K, Ichimura, K, Ieki, S, Ikeda, H, Inoue, K, Ishidoshiro, K, Kamei, Y, Kawada, N, Kishimoto, Y, Kinoshita, T, Koga, M, Maemura, N, Mitsui, T, Miyake, H, Nakamura, K, Nakamura, R, Ozaki, H, Sakai, T, Sambonsugi, H, Shimizu, I, Shirai, J, Shiraishi, K, Suzuki, A, Suzuki, Y, Takeuchi, A, Tamae, K, Ueshima, K, Wada, Y, Watanabe, H, Yoshida, Y, Obara, S, Ichikawa, AK, Kozlov, A, Chernyak, D, Takemoto, Y, Yoshida, S, Umehara, S, Fushimi, K, Nakamura, KZ, Yoshida, M, Berger, BE, Fujikawa, BK, Learned, JG, Maricic, J, Axani, SN, Winslow, LA, Fu, Z, Ouellet, J, Efremenko, Y, Karwowski, HJ, Markoff, DM, Tornow, W, Li, A, Detwiler, JA, Enomoto, S, Decowski, MP, Grant, C, O’Donnell, T, and Dell’Oro, S

Subjects
Astronomical and Space Sciences, Atomic, Molecular, Nuclear, Particle and Plasma Physics, Physical Chemistry (incl. Structural), Astronomy & Astrophysics
Abstract

We report the result of a search for neutrinos in coincidence with solar flares from the GOES flare database. The search was performed on a 10.8 kton-year exposure of KamLAND collected from 2002 to 2019. This large exposure allows us to explore previously unconstrained parameter space for solar flare neutrinos. We found no statistical excess of neutrinos and established 90% confidence level upper limits of 8.4 × 107 cm-2 (3.0 × 109 cm-2) on the electron antineutrino (electron neutrino) fluence at 20 MeV normalized to the X12 flare, assuming that the neutrino fluence is proportional to the X-ray intensity.

Published
2022

6. Search for Low-energy Electron Antineutrinos in KamLAND Associated with Gravitational Wave Events

Author

Abe, S, Asami, S, Gando, A, Gando, Y, Gima, T, Goto, A, Hachiya, T, Hata, K, Hayashida, S, Hosokawa, K, Ichimura, K, Ieki, S, Ikeda, H, Inoue, K, Ishidoshiro, K, Kamei, Y, Kawada, N, Kishimoto, Y, Kinoshita, T, Koga, M, Maemura, N, Mitsui, T, Miyake, H, Nakamura, K, Nakamura, R, Ozaki, H, Sakai, T, Sambonsugi, H, Shimizu, I, Shirai, J, Shiraishi, K, Suzuki, A, Suzuki, Y, Takeuchi, A, Tamae, K, Ueshima, K, Wada, Y, Watanabe, H, Yoshida, Y, Obara, S, Kozlov, A, Chernyak, D, Takemoto, Y, Yoshida, S, Umehara, S, Fushimi, K, Ichikawa, AK, Nakamura, KZ, Yoshida, M, Berger, BE, Fujikawa, BK, Learned, JG, Maricic, J, Axani, SN, Winslow, LA, Fu, Z, Ouellet, J, Efremenko, Y, Karwowski, HJ, Markoff, DM, Tornow, W, Li, A, Detwiler, JA, Enomoto, S, Decowski, MP, Grant, C, O’Donnell, T, and Dell’Oro, S

Subjects
Neutrino astronomy, Gravitational waves, astro-ph.HE, hep-ex, Astronomical and Space Sciences, Atomic, Molecular, Nuclear, Particle and Plasma Physics, Physical Chemistry (incl. Structural), Astronomy & Astrophysics
Abstract

We present the results of a search for MeV-scale electron antineutrino events in KamLAND coincident with the 60 gravitational wave events/candidates reported by the LIGO/Virgo collaboration during their second and third observing runs. We find no significant coincident signals within a 500 s timing window from each gravitational wave and present 90% C.L. upper limits on the electron antineutrino fluence between 108 and 1013 cm-2 for neutrino energies in the energy range of 1.8-111 MeV.

Published
2021

7. KamLAND SENSITIVITY TO NEUTRINOS FROM PRE-SUPERNOVA STARS

Author

Asakura, K, Gando, A, Gando, Y, Hachiya, T, Hayashida, S, Ikeda, H, Inoue, K, Ishidoshiro, K, Ishikawa, T, Ishio, S, Koga, M, Matsuda, S, Mitsui, T, Motoki, D, Nakamura, K, Obara, S, Oura, T, Shimizu, I, Shirahata, Y, Shirai, J, Suzuki, A, Tachibana, H, Tamae, K, Ueshima, K, Watanabe, H, Xu, BD, Kozlov, A, Takemoto, Y, Yoshida, S, Fushimi, K, Piepke, A, Banks, TI, Berger, BE, Fujikawa, BK, O’Donnell, T, Learned, JG, Maricic, J, Matsuno, S, Sakai, M, Winslow, LA, Efremenko, Y, Karwowski, HJ, Markoff, DM, Tornow, W, Detwiler, JA, Enomoto, S, and Decowski, MP

Subjects
neutrinos, supernovae: general, astro-ph.HE, hep-ex, physics.ins-det, Astronomical and Space Sciences, Atomic, Molecular, Nuclear, Particle and Plasma Physics, Physical Chemistry (incl. Structural), Astronomy & Astrophysics
Abstract

In the late stages of nuclear burning for massive stars (M > 8 Mȯ), the production of neutrino-antineutrino pairs through various processes becomes the dominant stellar cooling mechanism. As the star evolves, the energy of these neutrinos increases and in the days preceding the supernova a significant fraction of emitted electron anti-neutrinos exceeds the energy threshold for inverse beta decay on free hydrogen. This is the golden channel for liquid scintillator detectors because the coincidence signature allows for significant reductions in background signals. We find that the kiloton-scale liquid scintillator detector KamLAND can detect these pre-supernova neutrinos from a star with a mass of 25 Mȯ at a distance less than 690 pc with 3σ significance before the supernova. This limit is dependent on the neutrino mass ordering and background levels. KamLAND takes data continuously and can provide a supernova alert to the community.

Published
2016

8. Supernova Model Discrimination with Hyper-Kamiokande

Author

Abe, K., primary, Adrich, P., additional, Aihara, H., additional, Akutsu, R., additional, Alekseev, I., additional, Ali, A., additional, Ameli, F., additional, Anghel, I., additional, Anthony, L. H. V., additional, Antonova, M., additional, Araya, A., additional, Asaoka, Y., additional, Ashida, Y., additional, Aushev, V., additional, Ballester, F., additional, Bandac, I., additional, Barbi, M., additional, Barker, G. J., additional, Barr, G., additional, Batkiewicz-Kwasniak, M., additional, Bellato, M., additional, Berardi, V., additional, Bergevin, M., additional, Bernard, L., additional, Bernardini, E., additional, Berns, L., additional, Bhadra, S., additional, Bian, J., additional, Blanchet, A., additional, Blaszczyk, F. d. M., additional, Blondel, A., additional, Boiano, A., additional, Bolognesi, S., additional, Bonavera, L., additional, Booth, N., additional, Borjabad, S., additional, Boschi, T., additional, Bose, D., additional, Boyd, S . B., additional, Bozza, C., additional, Bravar, A., additional, Bravo-Berguño, D., additional, Bronner, C., additional, Brown, L., additional, Bubak, A., additional, Buchowicz, A., additional, Buizza Avanzini, M., additional, Cafagna, F. S., additional, Calabria, N. F., additional, Calvo-Mozota, J. M., additional, Cao, S., additional, Cartwright, S. L., additional, Carroll, A., additional, Catanesi, M. G., additional, Cebriàn, S., additional, Chabera, M., additional, Chakraborty, S., additional, Checchia, C., additional, Choi, J. H., additional, Choubey, S., additional, Cicerchia, M., additional, Coleman, J., additional, Collazuol, G., additional, Cook, L., additional, Cowan, G., additional, Cuen-Rochin, S., additional, Danilov, M., additional, Díaz López, G., additional, De la Fuente, E., additional, de Perio, P., additional, De Rosa, G., additional, Dealtry, T., additional, Densham, C. J., additional, Dergacheva, A., additional, Deshmukh, N., additional, Devi, M. M., additional, Di Lodovico, F., additional, Di Meo, P., additional, Di Palma, I., additional, Doyle, T. A., additional, Drakopoulou, E., additional, Drapier, O., additional, Dumarchez, J., additional, Dunne, P., additional, Dziewiecki, M., additional, Eklund, L., additional, El Hedri, S., additional, Ellis, J., additional, Emery, S., additional, Esmaili, A., additional, Esteve, R., additional, Evangelisti, A., additional, Feely, M., additional, Fedotov, S., additional, Feng, J., additional, Fernandez, P., additional, Fernández-Martinez, E., additional, Ferrario, P., additional, Ferrazzi, B., additional, Feusels, T., additional, Finch, A., additional, Finley, C., additional, Fiorentini, A., additional, Fiorillo, G., additional, Fitton, M., additional, Frankiewicz, K., additional, Friend, M., additional, Fujii, Y., additional, Fukuda, Y., additional, Galinski, G., additional, Gao, J., additional, Garde, C., additional, Garfagnini, A., additional, Garode, S., additional, Gialanella, L., additional, Giganti, C., additional, Gomez-Cadenas, J. J., additional, Gonin, M., additional, González-Nuevo, J., additional, Gorin, A., additional, Gornea, R., additional, Gousy-Leblanc, V., additional, Gramegna, F., additional, Grassi, M., additional, Grella, G., additional, Guigue, M., additional, Gumplinger, P., additional, Hadley, D. R., additional, Harada, M., additional, Hartfiel, B., additional, Hartz, M., additional, Hassani, S., additional, Hastings, N. C., additional, Hayato, Y., additional, Hernando-Morata, J. A., additional, Herrero, V., additional, Hill, J., additional, Hiraide, K., additional, Hirota, S., additional, Holin, A., additional, Horiuchi, S., additional, Hoshina, K., additional, Hultqvist, K., additional, Iacob, F., additional, Ichikawa, A. K., additional, Idrissi Ibnsalih, W., additional, Iijima, T., additional, Ikeda, M., additional, Inomoto, M., additional, Inoue, K., additional, Insler, J., additional, Ioannisian, A., additional, Ishida, T., additional, Ishidoshiro, K., additional, Ishino, H., additional, Ishitsuka, M., additional, Ito, H., additional, Ito, S., additional, Itow, Y., additional, Iwamoto, K., additional, Izmaylov, A., additional, Izumi, N., additional, Izumiyama, S., additional, Jakkapu, M., additional, Jamieson, B., additional, Jang, H. I., additional, Jang, J. S., additional, Jenkins, S. J., additional, Jeon, S. H., additional, Jiang, M., additional, Jo, H. S., additional, Jonsson, P., additional, Joo, K. K., additional, Kajita, T., additional, Kakuno, H., additional, Kameda, J., additional, Kano, Y., additional, Kalaczynski, P., additional, Karlen, D., additional, Kasperek, J., additional, Kataoka, Y., additional, Kato, A., additional, Katori, T., additional, Kazarian, N., additional, Kearns, E., additional, Khabibullin, M., additional, Khotjantsev, A., additional, Kikawa, T., additional, Kekic, M., additional, Kim, J. H., additional, Kim, J. Y., additional, Kim, S. B., additional, Kim, S. Y., additional, King, S., additional, Kinoshita, T., additional, Kisiel, J., additional, Klekotko, A., additional, Kobayashi, T., additional, Koch, L., additional, Koga, M., additional, Koerich, L., additional, Kolev, N., additional, Konaka, A., additional, Kormos, L. L., additional, Koshio, Y., additional, Korzenev, A., additional, Kotsar, Y., additional, Kouzakov, K. A., additional, Kowalik, K. L., additional, Kravchuk, L., additional, Kryukov, A. P., additional, Kudenko, Y., additional, Kumita, T., additional, Kurjata, R., additional, Kutter, T., additional, Kuze, M., additional, Kwak, K., additional, La Commara, M., additional, Labarga, L., additional, Lagoda, J., additional, Lamers James, M., additional, Lamoureux, M., additional, Laveder, M., additional, Lavitola, L., additional, Lawe, M., additional, Learned, J. G., additional, Lee, J., additional, Leitner, R., additional, Lezaun, V., additional, Lim, I. T., additional, Lindner, T., additional, Litchfield, R. P., additional, Long, K. R., additional, Longhin, A., additional, Loverre, P., additional, Lu, X., additional, Ludovici, L., additional, Maekawa, Y., additional, Magaletti, L., additional, Magar, K., additional, Mahn, K., additional, Makida, Y., additional, Malek, M., additional, Malinský, M., additional, Marchi, T., additional, Maret, L., additional, Mariani, C., additional, Marinelli, A., additional, Martens, K., additional, Marti, Ll., additional, Martin, J. F., additional, Martin, D., additional, Marzec, J., additional, Matsubara, T., additional, Matsumoto, R., additional, Matsuno, S., additional, Matusiak, M., additional, Mazzucato, E., additional, McCarthy, M., additional, McCauley, N., additional, McElwee, J., additional, McGrew, C., additional, Mefodiev, A., additional, Medhi, A., additional, Mehta, P., additional, Mellet, L., additional, Menjo, H., additional, Mermod, P., additional, Metelko, C., additional, Mezzetto, M., additional, Migenda, J., additional, Migliozzi, P., additional, Mijakowski, P., additional, Miki, S., additional, Miller, E. W., additional, Minakata, H., additional, Minamino, A., additional, Mine, S., additional, Mineev, O., additional, Mitra, A., additional, Miura, M., additional, Moharana, R., additional, Mollo, C. M., additional, Mondal, T., additional, Mongelli, M., additional, Monrabal, F., additional, Moon, D. H., additional, Moon, C. S., additional, Mora, F. J., additional, Moriyama, S., additional, Mueller, Th. A., additional, Munteanu, L., additional, Murase, K., additional, Nagao, Y., additional, Nakadaira, T., additional, Nakagiri, K., additional, Nakahata, M., additional, Nakai, S., additional, Nakajima, Y., additional, Nakamura, K., additional, Nakamura, KI., additional, Nakamura, H., additional, Nakano, Y., additional, Nakaya, T., additional, Nakayama, S., additional, Nakayoshi, K., additional, Nascimento Machado, L., additional, Naseby, C. E. R., additional, Navarro-Garcia, B., additional, Needham, M., additional, Nicholls, T., additional, Niewczas, K., additional, Nishimura, Y., additional, Noah, E., additional, Nova, F., additional, Nugent, J. C., additional, Nunokawa, H., additional, Obrebski, W., additional, Ochoa-Ricoux, J. P., additional, O’Connor, E., additional, Ogawa, N., additional, Ogitsu, T., additional, Ohta, K., additional, Okamoto, K., additional, O’Keeffe, H. M., additional, Okumura, K., additional, Onishchuk, Y., additional, Orozco-Luna, F., additional, Oshlianskyi, A., additional, Ospina, N., additional, Ostrowski, M., additional, O’Sullivan, E., additional, O’Sullivan, L., additional, Ovsiannikova, T., additional, Oyama, Y., additional, Ozaki, H., additional, Pac, M. Y., additional, Paganini, P., additional, Palladino, V., additional, Paolone, V., additional, Pari, M., additional, Parsa, S., additional, Pasternak, J., additional, Pastore, C., additional, Pastuszak, G., additional, Patel, D. A., additional, Pavin, M., additional, Payne, D., additional, Peña-Garay, C., additional, Pidcott, C., additional, Pinzon Guerra, E., additional, Playfer, S., additional, Pointon, B. W., additional, Popov, A., additional, Popov, B., additional, Porwit, K., additional, Posiadala-Zezula, M., additional, Poutissou, J.-M., additional, Pozimski, J., additional, Pronost, G., additional, Prouse, N. W., additional, Przewlocki, P., additional, Quilain, B., additional, Quiroga, A. A., additional, Radicioni, E., additional, Radics, B., additional, Rajda, P. J., additional, Renner, J., additional, Rescigno, M., additional, Retiere, F., additional, Ricciardi, G., additional, Riccio, C., additional, Richards, B., additional, Rondio, E., additional, Rose, H. J., additional, Roskovec, B., additional, Roth, S., additional, Rott, C., additional, Rountree, S. D., additional, Rubbia, A., additional, Ruggeri, A. C., additional, Ruggles, C., additional, Russo, S., additional, Rychter, A., additional, Ryu, D., additional, Sakashita, K., additional, Samani, S., additional, Sánchez, F., additional, Sánchez, M. L., additional, Sanchez, M. C., additional, Sano, S., additional, Santos, J. D., additional, Santucci, G., additional, Sarmah, P., additional, Sashima, I., additional, Sato, K., additional, Scott, M., additional, Seiya, Y., additional, Sekiguchi, T., additional, Sekiya, H., additional, Seo, J. W., additional, Seo, S. H., additional, Sgalaberna, D., additional, Shaikhiev, A., additional, Shan, Z., additional, Shaykina, A., additional, Shimizu, I., additional, Shin, C. D., additional, Shinoki, M., additional, Shiozawa, M., additional, Sinnis, G., additional, Skrobova, N., additional, Skwarczynski, K., additional, Smy, M. B., additional, Sobczyk, J., additional, Sobel, H. W., additional, Soler, F. J. P., additional, Sonoda, Y., additional, Spina, R., additional, Spisso, B., additional, Spradlin, P., additional, Stankevich, K. L., additional, Stawarz, L., additional, Stellacci, S. M., additional, Stopa, K., additional, Studenikin, A. I., additional, Suárez Gómez, S. L., additional, Suganuma, T., additional, Suvorov, S., additional, Suwa, Y., additional, Suzuki, A. T., additional, Suzuki, S. Y., additional, Suzuki, Y., additional, Svirida, D., additional, Svoboda, R., additional, Taani, M., additional, Tada, M., additional, Takeda, A., additional, Takemoto, Y., additional, Takenaka, A., additional, Taketa, A., additional, Takeuchi, Y., additional, Takhistov, V., additional, Tanaka, H., additional, Tanaka, H. A., additional, Tanaka, H. I., additional, Tanaka, M., additional, Tashiro, T., additional, Thiesse, M., additional, Thompson, L. F., additional, Toledo, J., additional, Tomatani-Sánchez, A. K., additional, Tortone, G., additional, Tsui, K. M., additional, Tsukamoto, T., additional, Tzanov, M., additional, Uchida, Y., additional, Vagins, M. R., additional, Valder, S., additional, Valentino, V., additional, Vasseur, G., additional, Vijayvargi, A., additional, Vilela, C., additional, Vinning, W. G. S., additional, Vivolo, D., additional, Vladisavljevic, T., additional, Vogelaar, R. B., additional, Vyalkov, M. M., additional, Wachala, T., additional, Walker, J., additional, Wark, D., additional, Wascko, M. O., additional, Wendell, R. A., additional, Wilkes, R. J., additional, Wilking, M. J., additional, Wilson, J. R., additional, Wronka, S., additional, Xia, J., additional, Xie, Z., additional, Xin, T., additional, Yamaguchi, Y., additional, Yamamoto, K., additional, Yanagisawa, C., additional, Yano, T., additional, Yen, S., additional, Yershov, N., additional, Yeum, D. N., additional, Yokoyama, M., additional, Yonenaga, M., additional, Yoo, J., additional, Yu, I., additional, Yu, M., additional, Zakrzewski, T., additional, Zaldivar, B., additional, Zalipska, J., additional, Zaremba, K., additional, Zarnecki, G., additional, Ziembicki, M., additional, Zietara, K., additional, Zito, M., additional, and Zsoldos, S., additional

Published
2021
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10. SEARCH FOR EXTRATERRESTRIAL ANTINEUTRINO SOURCES WITH THE KamLAND DETECTOR

Author

Gando, A., primary, Gando, Y., additional, Ichimura, K., additional, Ikeda, H., additional, Inoue, K., additional, Kibe, Y., additional, Kishimoto, Y., additional, Koga, M., additional, Minekawa, Y., additional, Mitsui, T., additional, Morikawa, T., additional, Nagai, N., additional, Nakajima, K., additional, Nakamura, K., additional, Narita, K., additional, Shimizu, I., additional, Shimizu, Y., additional, Shirai, J., additional, Suekane, F., additional, Suzuki, A., additional, Takahashi, H., additional, Takahashi, N., additional, Takemoto, Y., additional, Tamae, K., additional, Watanabe, H., additional, Xu, B. D., additional, Yabumoto, H., additional, Yoshida, H., additional, Yoshida, S., additional, Enomoto, S., additional, Kozlov, A., additional, Murayama, H., additional, Grant, C., additional, Keefer, G., additional, Piepke, A., additional, Banks, T. I., additional, Bloxham, T., additional, Detwiler, J. A., additional, Freedman, S. J., additional, Fujikawa, B. K., additional, Han, K., additional, Kadel, R., additional, O'Donnell, T., additional, Steiner, H. M., additional, Dwyer, D. A., additional, McKeown, R. D., additional, Zhang, C., additional, Berger, B. E., additional, Lane, C. E., additional, Maricic, J., additional, Miletic, T., additional, Batygov, M., additional, Learned, J. G., additional, Matsuno, S., additional, Sakai, M., additional, Horton-Smith, G. A., additional, Downum, K. E., additional, Gratta, G., additional, Efremenko, Y., additional, Kamyshkov, Y., additional, Perevozchikov, O., additional, Karwowski, H. J., additional, Markoff, D. M., additional, Tornow, W., additional, Heeger, K. M., additional, and Decowski, M. P., additional

Published
2012
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11. THEAGORAHIGH-RESOLUTION GALAXY SIMULATIONS COMPARISON PROJECT. II. ISOLATED DISK TEST

Author

Daniel Ceverino, Thomas P. Quinn, Oscar Agertz, Brian W. O'Shea, Ikkoh Shimizu, Ben W. Keller, Vadim A. Semenov, Colin DeGraf, Spencer Clark Wallace, John H. Wise, Joel R. Primack, Alessandro Lupi, Nir Mandelker, Lucio Mayer, Keita Todoroki, Britton D. Smith, Jun-Hwan Choi, Avishai Dekel, Robert Thompson, Samantha M. Benincasa, Philip F. Hopkins, Kentaro Nagamine, Sijing Shen, Robert Feldmann, Cameron Hummels, Nickolay Y. Gnedin, Tom Abel, Kenza S. Arraki, Samuel N. Leitner, Sukanya Chakrabarti, James Wadsley, Michael J. Butler, Santi Roca-Fàbrega, Anatoly Klypin, Romain Teyssier, Christine M. Simpson, Piero Madau, Sarah Nickerson, Nathan J. Goldbaum, Matthew J. Turk, Ji-hoon Kim, Yves Revaz, Hui Li, Kim, J, Agertz, O, Teyssier, R, Butler, M, Ceverino, D, Choi, J, Feldmann, R, Keller, B, Lupi, A, Quinn, T, Revaz, Y, Wallace, S, Gnedin, N, Leitner, S, Shen, S, Smith, B, Thompson, R, Turk, M, Abel, T, Arraki, K, Benincasa, S, Chakrabarti, S, Degraf, C, Dekel, A, Goldbaum, N, Hopkins, P, Hummels, C, Klypin, A, Li, H, Madau, P, Mandelker, N, Mayer, L, Nagamine, K, Nickerson, S, O'Shea, B, Primack, J, Roca-Fabrega, S, Semenov, V, Shimizu, I, Simpson, C, Todoroki, K, Wadsley, J, and Wise, J

Subjects
Cosmology and Nongalactic Astrophysics (astro-ph.CO), formation [galaxies], Radiative cooling, ISM: structure, astro-ph.GA, FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, Astronomy & Astrophysics, Physical Chemistry, Atomic, 01 natural sciences, methods: numerical, 010305 fluids & plasmas, Particle and Plasma Physics, kinematics and dynamics [galaxies], 0103 physical sciences, Galaxy formation and evolution, galaxies: formation, Nuclear, theory, 010303 astronomy & astrophysics, evolution [galaxies], Astrophysics::Galaxy Astrophysics, Galaxy rotation curve, Physics, theory [cosmology], Star formation, Molecular, numerical [methods], Astronomy and Astrophysics, Scale height, Astrophysics - Astrophysics of Galaxies, Galaxy, Supernova, Distribution function, Space and Planetary Science, Astrophysics of Galaxies (astro-ph.GA), astro-ph.CO, galaxies: kinematics and dynamic, structure [ISM], galaxies: evolution, Astronomical and Space Sciences, Astrophysics - Cosmology and Nongalactic Astrophysics, Physical Chemistry (incl. Structural)
Abstract

Using an isolated Milky Way-mass galaxy simulation, we compare results from 9 state-of-the-art gravito-hydrodynamics codes widely used in the numerical community. We utilize the infrastructure we have built for the AGORA High-resolution Galaxy Simulations Comparison Project. This includes the common disk initial conditions, common physics models (e.g., radiative cooling and UV background by the standardized package Grackle) and common analysis toolkit yt, all of which are publicly available. Subgrid physics models such as Jeans pressure floor, star formation, supernova feedback energy, and metal production are carefully constrained across code platforms. With numerical accuracy that resolves the disk scale height, we find that the codes overall agree well with one another in many dimensions including: gas and stellar surface densities, rotation curves, velocity dispersions, density and temperature distribution functions, disk vertical heights, stellar clumps, star formation rates, and Kennicutt-Schmidt relations. Quantities such as velocity dispersions are very robust (agreement within a few tens of percent at all radii) while measures like newly-formed stellar clump mass functions show more significant variation (difference by up to a factor of ~3). Systematic differences exist, for example, between mesh-based and particle-based codes in the low density region, and between more diffusive and less diffusive schemes in the high density tail of the density distribution. Yet intrinsic code differences are generally small compared to the variations in numerical implementations of the common subgrid physics such as supernova feedback. Our experiment reassures that, if adequately designed in accordance with our proposed common parameters, results of a modern high-resolution galaxy formation simulation are more sensitive to input physics than to intrinsic differences in numerical schemes., 28 pages, 35 figures, Accepted for publication in the Astrophysical Journal, Image resolution greatly reduced, High-resolution version of this article is available at http://www.jihoonkim.org/agora/AGORA_Paper4_draft.pdf, The first paper of the AGORA Initiative is at http://adsabs.harvard.edu/abs/2014ApJS..210...14K, More information on AGORA is at http://www.AGORAsimulations.org/

Published
2016

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