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271,623 results on '"The TH"'

301. MIRI/JWST observations reveal an extremely obscured starburst in the z=6.9 system SPT0311-58

Author

Álvarez-Márquez, J., Gómez, A. Crespo, Colina, L., Neeleman, M., Walter, F., Labiano, A., Pérez-González, P., Bik, A., Noorgaard-Nielsen, H. U., Ostlin, G., Wright, G., Alonso-Herrero, A., Azollini, R., Caputi, K. I., Eckart, A., Fèvre, O. Le, García-Marín, M., Greve, T. R., Hjorth, J., Ilbert, O., Kendrew, S., Pye, J. P., Tikkanen, T., Topinka, M., van der Werf, P., Ward, M., van Dishoeck, E. F., Güdel, M., Henning, Th., Lagage, P. O., Ray, T., and Waelkens, C.

Subjects
Astrophysics - Astrophysics of Galaxies
Abstract

Using MIRI on-board JWST we present mid-infrared sub-arcsec imaging (MIRIM) and spectroscopy (MRS) of the hyperluminous infrared system SPT0311-58 at z=6.9. MIRI observations are compared with existing ALMA far-infrared continuum and [CII]158$\mu$m imaging. Even though the ALMA observations suggests very high star formation rates (SFR) in the eastern (E) and western (W) galaxies of the system, the H$\alpha$ line is not detected. This, together with the detection of the Pa$\alpha$ line, implies very high optical nebular extinction with lower limits of 4.2 (E) and 3.9 mag (W), and even larger 5.6 (E) and 10.0 (W) for SED derived values. The extinction-corrected Pa$\alpha$ SFRs are 383 and 230M$_{\odot}$yr$^{-1}$ for the E and W galaxies, respectively. This represents 50% of the SFRs derived from the [CII]158$\mu$m line and infrared light for the E galaxy and as low as 6% for the W galaxy. The MIRI observations reveal a clumpy stellar structure, with each clump having 3 to 5 $\times$10$^{9}$M$_\mathrm{\odot}$, leading to a total stellar mass of 2.0 and 1.5$\times$10$^{10}$M$_\mathrm{\odot}$ for the E and W galaxies, respectively. The specific SFR in the stellar clumps ranges from 25 to 59Gyr$^{-1}$, which are 3 to 10 times larger than the values measured in galaxies of similar mass at redshifts 6 to 8. The overall gas mass fraction is $M_\mathrm{gas}$/$M_*\sim3$, similar to that of z=4.5-6 star-forming galaxies. The observed properties of SPT0311-58 such as the clumpy distribution at sub(kpc) scales and the very high average extinction are similar to those observed in low- and intermediate-z LIRGs and ULIRGs, even though SPT0311-58 is observed only 800 Myr after the Big Bang. Massive, heavily obscured, clumpy starburst systems like SPT0311-58 likely represent the early phases in the formation of massive high-z bulge/spheroids and luminous quasars., Comment: 18 pages, 8 figures, final published version in A&A

Published
2023
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307. Hint for a TeV neutrino emission from the Galactic Ridge with ANTARES

Author

Albert, A., Alves, S., André, M., Ardid, M., Ardid, S., Aubert, J. -J., Aublin, J., Baret, B., Basa, S., Becherini, Y., Belhorma, B., Bendahman, M., Benfenati, F., Bertin, V., Biagi, S., Bissinger, M., Boumaaza, J., Bouta, M., Bouwhuis, M. C., Brânzaş, H., Bruijn, R., Brunner, J., Busto, J., Caiffi, B., Calvo, D., Campion, S., Capone, A., Caramete, L., Carenini, F., Carr, J., Carretero, V., Celli, S., Cerisy, L., Chabab, M., Chau, T. N., Moursli, R. Cherkaoui El, Chiarusi, T., Circella, M., Coelho, J. A. B., Coleiro, A., Coniglione, R., Coyle, P., Creusot, A., Díaz, A. F., De Martino, B., Distefano, C., Di Palma, I., Domi, A., Donzaud, C., Dornic, D., Drouhin, D., Eberl, T., van Eeden, T., van Eijk, D., Hedri, S. El, Khayati, N. El, Enzenhöfer, A., Fasano, M., Fermani, P., Ferrara, G., Filippini, F., Fusco, L., Gagliardini, S., García, J., Oliver, C. Gatius, Gay, P., Geißelbrecht, N., Glotin, H., Gozzini, R., Ruiz, R. Gracia, Graf, K., Guidi, C., Haegel, L., Hallmann, S., van Haren, H., Heijboer, A. J., Hello, Y., Hernández-Rey, J. J., Hößl, J., Hofestädt, J., Huang, F., Illuminati, G., James, C. W., Jisse-Jung, B., de Jong, M., de Jong, P., Kadler, M., Kalekin, O., Katz, U., Kouchner, A., Kreykenbohm, I., Kulikovskiy, V., Lahmann, R., Lamoureux, M., Lazo, A., Lefèvre, D., Leonora, E., Levi, G., Stum, S. Le, Lopez-Coto, D., Loucatos, S., Maderer, L., Manczak, J., Marcelin, M., Margiotta, A., Marinelli, A., Martínez-Mora, J. A., Migliozzi, P., Moussa, A., Muller, R., Nauta, L., Navas, S., Neronov, A., Nezri, E., Fearraigh, B. Ó, Păun, A., Păvălaş, G. E., Perrin-Terrin, M., Pestel, V., Piattelli, P., Poirè, C., Popa, V., Pradier, T., Randazzo, N., Real, D., Reck, S., Riccobene, G., Romanov, A., Sánchez-Losa, A., Saina, A., Greus, F. Salesa, Samtleben, D. F. E., Sanguineti, M., Sapienza, P., Savchenko, D., Schnabel, J., Schumann, J., Schüssler, F., Seneca, J., Spurio, M., Stolarczyk, Th., Taiuti, M., Tayalati, Y., Tingay, S. J., Vallage, B., Vannoye, G., Van Elewyck, V., Viola, S., Vivolo, D., Wilms, J., Zavatarelli, S., Zegarelli, A., Zornoza, J. D., and Zúñiga, J.

Subjects
Astrophysics - High Energy Astrophysical Phenomena
Abstract

Interactions of cosmic ray protons, atomic nuclei, and electrons in the interstellar medium in the inner part of the Milky Way produce a $\gamma$-ray flux from the Galactic Ridge. If the $\gamma$-ray emission is dominated by proton and nuclei interactions, a neutrino flux comparable to the $\gamma$-ray flux is expected from the same sky region. Data collected by the ANTARES neutrino telescope are used to constrain the neutrino flux from the Galactic Ridge in the 1-100 TeV energy range. Neutrino events reconstructed both as tracks and showers are considered in the analysis and the selection is optimized for the search of an excess in the region $|l| < 30\deg$, $|b| < 2\deg$. The expected background in the search region is estimated using an off-zone region with similar sky coverage. Neutrino signal originating from a power-law spectrum with spectral index ranging from $\Gamma_\nu=1$ to $4$ is simulated in both channels. The observed energy distributions are fitted to constrain the neutrino emission from the Ridge. The energy distributions in the signal region are inconsistent with the background expectation at $\sim 96\%$ confidence level. The mild excess over the background is consistent with a neutrino flux with a power law with a spectral index $2.45^{+0.22}_{-0.34}$ and a flux normalization $dN_\nu/dE_\nu = 4.0^{+2.7}_{-2.0} \times 10^{-16} \text{GeV}^{-1} \text{cm}^{-2} \text{s}^{-1} \text{sr}^{-1}$ at 40 TeV reference energy. Such flux is consistent with the expected neutrino signal if the bulk of the observed $\gamma$-ray flux from the Galactic Ridge originates from interactions of cosmic ray protons and nuclei with a power-law spectrum extending well into the PeV energy range., Comment: 8 pages, 5 figures

Published
2022
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308. Measurement of the cosmogenic neutron yield in Super-Kamiokande with gadolinium loaded water

Author

Collaboration, Super-Kamiokande, Shinoki, M., Abe, K., 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., Nakano, Y., Nakahata, M., Nakayama, S., Noguchi, Y., Okamoto, K., Sato, K., Sekiya, H., Shiba, H., Shimizu, K., Shiozawa, M., Sonoda, Y., Suzuki, Y., Takeda, A., Takemoto, Y., Takenaka, A., Tanaka, H., Watanabe, S., Yano, T., Han, S., Kajita, T., Okumura, K., Tashiro, T., Tomiya, T., Wang, X., Yoshida, S., Megias, G. D., Fernandez, P., Labarga, L., Ospina, N., Zaldivar, B., Pointon, B. W., Kearns, E., Raaf, J. L., Wan, L., Wester, T., Bian, J., Griskevich, N. J., Kropp, W. R., Locke, S., Smy, M. B., Sobel, H. W., Takhistov, V., Yankelevich, A., Hill, J., Lee, S. H., Moon, D. H., Park, R. G., Bodur, B., Scholberg, K., Walter, C. W., Beauchêne, A., Bernard, L., Coffani, A., Drapier, O., Hedri, S. El, Giampaolo, A., Mueller, Th. A., Santos, A. D., Paganini, P., Quilain, B., Ishizuka, T., Nakamura, T., Jang, J. S., Learned, J. G., Choi, K., Cao, S., Anthony, L. H. V., Martin, D., Scott, M., Sztuc, A. A., Uchida, Y., Berardi, V., Catanesi, M. G., Radicioni, E., Calabria, N. F., Langella, A., Machado, L. N., De Rosa, G., Collazuol, G., Iacob, F., Lamoureux, M., Mattiazzi, M., Ludovici, L., Gonin, M., Pronost, G., Fujisawa, C., Maekawa, Y., Nishimura, Y., Akutsu, R., Friend, M., Hasegawa, T., Ishida, T., Kobayashi, T., Jakkapu, M., Matsubara, T., Nakadaira, T., Nakamura, K., Oyama, Y., Sakashita, K., Sekiguchi, T., Tsukamoto, T., Bhuiyan, N., Boschi, T., Burton, G. T., Di Lodovico, F., Gao, J., Goldsack, A., Katori, T., Migenda, J., Taani, M., Xie, Z., Zsoldos, S., Kotsar, Y., Ozaki, H., Suzuki, A. T., Takeuchi, Y., Bronner, C., Feng, J., Kikawa, T., Mori, M., Nakaya, T., Wendell, R. A., Yasutome, K., Jenkins, S. J., McCauley, N., Mehta, P., Tarrant, A., Tsui, K. M., Fukuda, Y., Itow, Y., Menjo, H., Ninomiya, K., Lagoda, J., Lakshmi, S. M., Mandal, M., Mijakowski, P., Prabhu, Y. S., Zalipska, J., Jia, M., Jiang, J., Jung, C. K., Wilking, M. J., Yanagisawa, C., Harada, M., Ishino, H., Ito, S., Kitagawa, H., Koshio, Y., Nakanishi, F., Sakai, S., Barr, G., Barrow, D., Cook, L., Samani, S., Wark, D., Holin, A., Nova, F., Yang, J. Y., Yang, B. S., Yoo, J., Fannon, J. E. P., Kneale, L., Malek, M., McElwee, J. M., Stone, O., Thiesse, M. D., Thompson, L. F., Okazawa, H., Kim, S. B., Kwon, E., Seo, J. W., Yu, I., Ichikawa, A. K., Nakamura, K. D., Tairafune, S., Nishijima, K., Koshiba, M., Iwamoto, K., Nakagiri, K., Nakajima, Y., Shima, S., Taniuchi, N., Yokoyama, M., Martens, K., de Perio, P., Vagins, M. R., Xia, J., Kuze, M., Izumiyama, S., Inomoto, M., Ishitsuka, M., Ito, H., Kinoshita, T., Matsumoto, R., Ommura, Y., Shigeta, N., Suganuma, T., Yamauchi, K., Martin, J. F., Tanaka, H. A., Towstego, T., Gaur, R., Gousy-Leblanc, V., Hartz, M., Konaka, A., Li, X., Prouse, N. W., Chen, S., Xu, B. D., Zhang, B., Posiadala-Zezula, M., Boyd, S. B., Hadley, D., Nicholson, M., O'Flaherty, M., Richards, B., Ali, A., Jamieson, B., Marti, Ll., Minamino, A., Pintaudi, G., Sano, S., Suzuki, S., and Wada, K.

Subjects
High Energy Physics - Experiment
Abstract

Cosmic-ray muons that enter the Super-Kamiokande detector cause hadronic showers due to spallation in water, producing neutrons and radioactive isotopes. Those are a major background source for studies of MeV-scale neutrinos and searches for rare events. Since 2020, gadolinium was introduced in the ultra-pure water in the Super-Kamiokande detector to improve the detection efficiency of neutrons. In this study, the cosmogenic neutron yield was measured using data acquired during the period after the gadolinium loading. The yield was found to be $(2.76 \pm 0.02\,\mathrm{(stat.) \pm 0.19\,\mathrm{(syst.)}}) \times 10^{-4}\,\mu^{-1} \mathrm{g^{-1} cm^{2}}$ at 259 GeV of average muon energy at the Super-Kamiokande detector., Comment: 10 pages, 10 figures, 3 tables

Published
2022

309. Excited states of zero seniority based on a pair condensate

Author

Popa, Th., Sandulescu, N., and Sambataro, M.

Subjects
Nuclear Theory
Abstract

We study the excited states of zero seniority for various like-particle systems interacting by pairing forces and by general two-body interactions. We consider two types of excitations, generated from a ground state described by a pair condensate. One type is obtained by breaking a pair from the ground state condensate and replacing it by "excited" collective pairs built on time-reversed single-particle orbits. The second type of zero seniority excited states is described by a condensate of identical excited pairs. The structure of these excited states is analysed for the picked fence model and for the valence neutrons of $^{108}$Sn. For a state-depending pairing interaction, the first type of excited states agree well with the J=0 states which are known in $^{108}$Sn. At the same time, these states can be also associated unambiguously with those exact states which are the closest in energy to the experimental levels. The states corresponding to the excited pair condensate appear at low energies, around the energy of the second excited state of the first type, and they do not have a simple correspondence with exact eigenstates. However, at a much higher excitation energy there is an exact state which is similar in structure to an EPC state. It is shown that this EPC state has the features of a giant pairing vibration., Comment: 22 pages, 6 figures

Published
2022
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310. Two temperate Earth-mass planets orbiting the nearby star GJ1002

Author

Mascareño, A. Suárez, González-Álvarez, E., Osorio, M. R. Zapatero, Lillo-Box, J., Faria, J. P., Passegger, V. M., Hernández, J. I. González, Figueira, P., Sozzetti, A., Rebolo, R., Pepe, F., Santos, N. C., Cristiani, S., Lovis, C., Silva, A. M., Ribas, I., Amado, P. J., Caballero, J. A., Quirrenbach, A., Reiners, A., Zechmeister, M., Adibekyan, V., Alibert, Y., Béjar, V. J. S., Benatti, S., D'Odorico, V., Damasso, M., Delisle, J. -B., Dreizler, P. Di Marcantonio S., Ehrenreich, D., Hatzes, A. P., Hara, N. C., Henning, Th., Kaminski, A., López-González, M. J., Martins, C. J. A. P., Micela, G., Montes, D., Pallé, E., Pedraz, S., Rodríguez, E., Rodríguez-López, C., Tal-Or, L., Sousa, S., and Udry, S.

Subjects
Astrophysics - Earth and Planetary Astrophysics, Astrophysics - Solar and Stellar Astrophysics
Abstract

We report the discovery and characterisation of two Earth-mass planets orbiting in the habitable zone of the nearby M-dwarf GJ~1002 based on the analysis of the radial-velocity (RV) time series from the ESPRESSO and CARMENES spectrographs. The host star is the quiet M5.5~V star GJ~1002 (relatively faint in the optical, $V \sim 13.8$ mag, but brighter in the infrared, $J \sim 8.3$ mag), located at 4.84 pc from the Sun. We analyse 139 spectroscopic observations taken between 2017 and 2021. We performed a joint analysis of the time series of the RV and full-width half maximum (FWHM) of the cross-correlation function (CCF) to model the planetary and stellar signals present in the data, applying Gaussian process regression to deal with the stellar activity. We detect the signal of two planets orbiting GJ~1002. GJ~1002~b is a planet with a minimum mass $m_p \sin i $ of 1.08 $\pm$ 0.13 M$_{\oplus}$ with an orbital period of 10.3465 $\pm$ 0.0027 days at a distance of 0.0457 $\pm$ 0.0013 au from its parent star, receiving an estimated stellar flux of 0.67 $F_{\oplus}$. GJ~1002 c is a planet with a minimum mass $m_p \sin i $ of 1.36 $\pm$ 0.17 M$_{\oplus}$ with an orbital period of 21.202 $\pm$ 0.013 days at a distance of 0.0738 $\pm$ 0.0021 au from its parent star, receiving an estimated stellar flux of 0.257 $F_{\oplus}$. We also detect the rotation signature of the star, with a period of 126 $\pm$ 15 days. GJ~1002 is one of the few known nearby systems with planets that could potentially host habitable environments. The closeness of the host star to the Sun makes the angular sizes of the orbits of both planets ($\sim$ 9.7 mas and $\sim$ 15.7 mas, respectively) large enough for their atmosphere to be studied via high-contrast high-resolution spectroscopy with instruments such as the future spectrograph ANDES for the ELT or the LIFE mission., Comment: 23 pages, 20 figures, 3 tables ; Replacement to fix some typos

Published
2022
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311. Evaluation of a general model for multimodal unsaturated soil hydraulic properties

Author

Seki, Katsutoshi, Toride, Nobuo, and van Genuchten, Martinus Th.

Subjects
Physics - Geophysics, Physics - Fluid Dynamics
Abstract

Many soils and other porous media exhibit dual- or multi-porosity type features. In a previous study (Seki et al., 2022) we presented multimodal water retention and closed-form hydraulic conductivity equations for such media. The objective of this study is to show that the proposed equations are practically useful. Specifically, dual-BC (Brooks and Corey)-CH (common head) (DBC), dual-VG (van Genuchten)-CH (DVC), and KO (Kosugi)$_1$BC$_2$-CH (KBC) models were evaluated for a broad range of soil types. The three models showed good agreement with measured water retention and hydraulic conductivity data over a wide range of pressure heads. Results were obtained by first optimizing water retention parameters and then optimizing the saturated hydraulic conductivity (K_s) and two parameters (p, q) or (p, r) in the general hydraulic conductivity equation. Although conventionally the tortuosity factor p is optimized and (q, r) fixed, sensitivity analyses showed that optimization of two parameters (p+r, qr) is required for the multimodal models. For 20 soils from the UNSODA database, the average $R^2$ for log (hydraulic conductivity) was highest (0.985) for the KBC model with r=1 and optimization of (Ks, p, q). This result was almost equivalent (0.973) to the DVC model with q=1 and optimization of (Ks, p, r); both were higher than $R^2$ for the widely used Peters model (0.956) when optimizing (Ks, p, a, $\omega$). The proposed equations are useful for practical applications while mathematically being simple and consistent.

Published
2022
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312. Fair Generative Models via Transfer Learning

Author

Teo, Christopher TH, Abdollahzadeh, Milad, and Cheung, Ngai-Man

Subjects
Computer Science - Machine Learning, Computer Science - Computers and Society
Abstract

This work addresses fair generative models. Dataset biases have been a major cause of unfairness in deep generative models. Previous work had proposed to augment large, biased datasets with small, unbiased reference datasets. Under this setup, a weakly-supervised approach has been proposed, which achieves state-of-the-art quality and fairness in generated samples. In our work, based on this setup, we propose a simple yet effective approach. Specifically, first, we propose fairTL, a transfer learning approach to learn fair generative models. Under fairTL, we pre-train the generative model with the available large, biased datasets and subsequently adapt the model using the small, unbiased reference dataset. We find that our fairTL can learn expressive sample generation during pre-training, thanks to the large (biased) dataset. This knowledge is then transferred to the target model during adaptation, which also learns to capture the underlying fair distribution of the small reference dataset. Second, we propose fairTL++, where we introduce two additional innovations to improve upon fairTL: (i) multiple feedback and (ii) Linear-Probing followed by Fine-Tuning (LP-FT). Taking one step further, we consider an alternative, challenging setup when only a pre-trained (potentially biased) model is available but the dataset that was used to pre-train the model is inaccessible. We demonstrate that our proposed fairTL and fairTL++ remain very effective under this setup. We note that previous work requires access to the large, biased datasets and is incapable of handling this more challenging setup. Extensive experiments show that fairTL and fairTL++ achieve state-of-the-art in both quality and fairness of generated samples. The code and additional resources can be found at bearwithchris.github.io/fairTL/., Comment: Accepted in AAAI-2023

Published
2022

314. Reconstruction of $B \to \rho \ell \nu_\ell$ decays identified using hadronic decays of the recoil $B$ meson in 2019 -- 2021 Belle II data

Author

Belle II Collaboration, Abudinén, F., Adachi, I., Adamczyk, K., Aggarwal, L., Ahlburg, P., Ahmed, H., Ahn, J. K., Aihara, H., Akopov, N., Aloisio, A., Ameli, F., Andricek, L., Ky, N. Anh, Asner, D. M., Atmacan, H., Aulchenko, V., Aushev, T., Aushev, V., Babu, V., Bacher, S., Bae, H., Baehr, S., Bahinipati, S., Bakich, A. M., Bambade, P., Banerjee, Sw., Bansal, S., Barrett, M., Batignani, G., Baudot, J., Bauer, M., Baur, A., Beaubien, A., Becker, J., Behera, P. K., Bennett, J. V., Bernieri, E., Bernlochner, F. U., Bertacchi, V., Bertemes, M., Bertholet, E., Bessner, M., Bettarini, S., Bhardwaj, V., Bhuyan, B., Bianchi, F., Bilka, T., Bilokin, S., Biswas, D., Bobrov, A., Bodrov, D., Bolz, A., Bondar, A., Bonvicini, G., Borah, J., Bozek, A., Bračko, M., Branchini, P., Braun, N., Briere, R. A., Browder, T. E., Brown, D. N., Budano, A., Bussino, S., Campajola, M., Cao, L., Casarosa, G., Cecchi, C., Cerasoli, J., Červenkov, D., Chang, M. -C., Chang, P., Cheaib, R., Cheema, P., Chekelian, V., Chen, C., Chen, Y. Q., Chen, Y. -T., Cheon, B. G., Chilikin, K., Chirapatpimol, K., Cho, H. -E., Cho, K., Cho, S. -J., Choi, S. -K., Choudhury, S., Cinabro, D., Corona, L., Cremaldi, L. M., Cunliffe, S., Czank, T., Das, S., Dash, N., Dattola, F., De La Cruz-Burelo, E., De La Motte, S. A., de Marino, G., De Nardo, G., De Nuccio, M., De Pietro, G., de Sangro, R., Deschamps, B., Destefanis, M., Dey, S., De Yta-Hernandez, A., Dhamija, R., Di Canto, A., Di Capua, F., Di Carlo, S., Dingfelder, J., Doležal, Z., Jiménez, I. Domínguez, Dong, T. V., Dorigo, M., Dort, K., Dossett, D., Dreyer, S., Dubey, S., Duell, S., Dujany, G., Ecker, P., Eidelman, S., Eliachevitch, M., Epifanov, D., Feichtinger, P., Ferber, T., Ferlewicz, D., Fillinger, T., Finck, C., Finocchiaro, G., Fischer, P., Flood, K., Fodor, A., Forti, F., Frey, A., Friedl, M., Fulsom, B. G., Gabrielli, A., Gabyshev, N., Ganiev, E., Garcia-Hernandez, M., Garg, R., Garmash, A., Gaur, V., Gaz, A., Gebauer, U., Gellrich, A., Ghevondyan, G., Giakoustidis, G., Giordano, R., Giri, A., Glazov, A., Gobbo, B., Godang, R., Goldenzweig, P., Golob, B., Gong, G., Grace, P., Gradl, W., Grammatico, T., Granderath, S., Graziani, E., Greenwald, D., Gruberová, Z., Gu, T., Guan, Y., Gudkova, K., Guilliams, J., Hadjivasiliou, C., Halder, S., Hara, K., Hara, T., Hartbrich, O., Hayasaka, K., Hayashii, H., Hazra, S., Hearty, C., Hedges, M. T., de la Cruz, I. Heredia, Villanueva, M. Hernández, Hershenhorn, A., Higuchi, T., Hill, E. C., Hirata, H., Hoek, M., Hohmann, M., Hollitt, S., Hotta, T., Hsu, C. -L., Huang, K., Humair, T., Iijima, T., Inami, K., Inguglia, G., Ipsita, N., Jabbar, J. Irakkathil, Ishikawa, A., Ito, S., Itoh, R., Iwasaki, M., Iwasaki, Y., Jackson, P., Jacobs, W. W., Jaffe, D. E., Jang, E. -J., Jeon, H. B., Ji, Q. P., Jia, S., Jin, Y., Joo, K. K., Junkerkalefeld, H., Kadenko, I., Kahn, J., Kakuno, H., Kaleta, M., Kalita, D., Kaliyar, A. B., Kandra, J., Kang, K. H., Kang, S., Kapusta, P., Karl, R., Karyan, G., Kato, Y., Kawasaki, T., Ketter, C., Kichimi, H., Kiesling, C., Kim, C. -H., Kim, D. Y., Kim, H. J., Kim, K. -H., Kim, Y. -K., Kim, Y. J., Kimmel, T. D., Kindo, H., Kinoshita, K., Kleinwort, C., Kodyš, P., Koga, T., Kohani, S., Kojima, K., Komarov, I., Konno, T., Korobov, A., Korpar, S., Kovalchuk, N., Kovalenko, E., Kowalewski, R., Kraetzschmar, T. M. G., Križan, P., Krohn, J. F., Krokovny, P., Krüger, H., Kuehn, W., Kuhr, T., Kumar, J., Kumar, M., Kumar, R., Kumara, K., Kumita, T., Kunigo, T., Kurz, S., Kuzmin, A., Kvasnička, P., Kwon, Y. -J., Lacaprara, S., Lai, Y. -T., La Licata, C., Lalwani, K., Lam, T., Lanceri, L., Lange, J. S., Laurenza, M., Lautenbach, K., Laycock, P. J., Leboucher, R., Diberder, F. R. Le, Lee, I. -S., Lee, S. C., Leitl, P., Levit, D., Lewis, P. M., Li, C., Li, L. K., Li, S. X., Li, Y. B., Libby, J., Lieret, K., Lin, J., Liptak, Z., Liu, Q. Y., Liu, Z. A., Liu, Z. Q., Liventsev, D., Longo, S., Lozar, A., Lueck, T., Luo, T., Lyu, C., Ma, Y., MacQueen, C., Maggiora, M., Maiti, R., Maity, S., Manfredi, R., Manoni, E., Manthei, A. C., Marcello, S., Marinas, C., Martel, L., Martellini, C., Martini, A., Martinov, T., Massaccesi, L., Masuda, M., Matsuda, T., Matsuoka, K., Matvienko, D., Maurya, S. K., McKenna, J. A., McNeil, J., Meggendorfer, F., Meier, F., Merola, M., Metzner, F., Milesi, M., Miller, C., Miyabayashi, K., Miyake, H., Miyata, H., Mizuk, R., Azmi, K., Mohanty, G. B., Molina-Gonzalez, N., Moneta, S., Moon, H., Moon, T., Moser, H. -G., Mrvar, M., Müller, F. J., Muller, Th., Mussa, R., Nakamura, I., Nakamura, K. R., Nakano, E., Nakao, M., Nakayama, H., Nakazawa, H., Nakazawa, Y., Charan, A. Narimani, Naruki, M., Narwal, D., Natkaniec, Z., Natochii, A., Nayak, L., Nayak, M., Nazaryan, G., Niebuhr, C., Niiyama, M., Ninkovic, J., Nisar, N. K., Nishida, S., Nishimura, K., Nouxman, M. H. A., Ogawa, K., Ogawa, S., Olsen, S. L., Onishchuk, Y., Ono, H., Onuki, Y., Oskin, P., Otani, F., Oxford, E. R., Ozaki, H., Pakhlov, P., Pakhlova, G., Paladino, A., Pang, T., Panta, A., Paoloni, E., Pardi, S., Parham, K., Park, H., Park, J., Park, S. -H., Paschen, B., Passeri, A., Pathak, A., Patra, S., Paul, S., Pedlar, T. K., Peruzzi, I., Peschke, R., Pestotnik, R., Pham, F., Piccolo, M., Piilonen, L. E., Angioni, G. Pinna, Podesta-Lerma, P. L. M., Podobnik, T., Pokharel, S., Polat, L., Popov, V., Praz, C., Prell, S., Prencipe, E., Prim, M. T., Purohit, M. V., Purwar, H., Rad, N., Rados, P., Raiz, S., Morales, A. Ramirez, Rasheed, R., Rauls, N., Reif, M., Reiter, S., Remnev, M., Ripp-Baudot, I., Ritter, M., Ritzert, M., Rizzo, G., Rizzuto, L. B., Robertson, S. H., Pérez, D. Rodríguez, Roney, J. M., Rosenfeld, C., Rostomyan, A., Rout, N., Rozanska, M., Russo, G., Roehrken, M., Sahoo, D., Sakai, Y., Sanders, D. A., Sandilya, S., Sangal, A., Santelj, L., Sartori, P., Sato, Y., Savinov, V., Scavino, B., Schmitz, J., Schnepf, M., Schreeck, H., Schueler, J., Schwanda, C., Schwartz, A. J., Schwenker, B., Schwickardi, M., Seino, Y., Selce, A., Senyo, K., Serrano, J., Sevior, M. E., Sfienti, C., Shan, W., Sharma, C., Shebalin, V., Shen, C. P., Shi, X. D., Shibuya, H., Shillington, T., Shimasaki, T., Shiu, J. -G., Shtol, D., Shwartz, B., Sibidanov, A., Simon, F., Singh, J. B., Skambraks, S., Skorupa, J., Smith, K., Sobie, R. J., Soffer, A., Sokolov, A., Soloviev, Y., Solovieva, E., Spataro, S., Spruck, B., Starič, M., Stefkova, S., Stottler, Z. S., Stroili, R., Strube, J., Stypula, J., Sue, Y., Sugiura, R., Sumihama, M., Sumisawa, K., Sutcliffe, W., Suzuki, S. Y., Svidras, H., Tabata, M., Takahashi, M., Takizawa, M., Tamponi, U., Tanaka, S., Tanida, K., Tanigawa, H., Taniguchi, N., Tao, Y., Tenchini, F., Thaller, A., Tiwary, R., Tonelli, D., Torassa, E., Toutounji, N., Trabelsi, K., Tsaklidis, I., Tsuboyama, T., Tsuzuki, N., Uchida, M., Ueda, I., Uehara, S., Uematsu, Y., Ueno, T., Uglov, T., Unger, K., Unno, Y., Uno, K., Uno, S., Urquijo, P., Ushiroda, Y., Usov, Y. V., Vahsen, S. E., van Tonder, R., Varner, G. S., Varvell, K. E., Vinokurova, A., Vitale, L., Vobbilisetti, V., Vorobyev, V., Vossen, A., Vismaya, V. S., Wach, B., Waheed, E., Wakeling, H. M., Abdullah, W. Wan, Wang, B., Wang, C. H., Wang, E., Wang, M. -Z., Wang, X. L., Warburton, A., Watanabe, M., Watanuki, S., Webb, J., Wehle, S., Welsch, M., Werbycka, O., Wessel, C., Wiechczynski, J., Wieduwilt, P., Windel, H., Won, E., Wu, L. J., Xu, X. P., Yabsley, B. D., Yamada, S., Yan, W., Yang, S. B., Ye, H., Yelton, J., Yin, J. H., Yook, Y. M., Yoshihara, K., Yuan, C. Z., Yusa, Y., Zani, L., Zhai, Y., Zhang, J. Z., Zhang, Y., Zhang, Z., Zhilich, V., Zhou, J. S., Zhou, Q. D., Zhou, X. Y., Zhukova, V. I., Zhulanov, V., and Žlebčík, R.

Subjects
High Energy Physics - Experiment
Abstract

We present results on the semileptonic decays $B^0 \to \rho^- \ell^+ \nu_\ell$ and $B^+ \to \rho^0 \ell^+ \nu_\ell$ in a sample corresponding to 189.9/fb of Belle II data at the SuperKEKB $e^- e^+$ collider. Signal decays are identified using full reconstruction of the recoil $B$ meson in hadronic final states. We determine the total branching fractions via fits to the distributions of the square of the "missing" mass in the event and the dipion mass in the signal candidate and find ${\mathcal{B}(B^0\to\rho^-\ell^+ \nu_\ell) = (4.12 \pm 0.64(\mathrm{stat}) \pm 1.16(\mathrm{syst})) \times 10^{-4}}$ and ${\mathcal{B}({B^+\to\rho^0\ell^+\nu_\ell}) = (1.77 \pm 0.23 (\mathrm{stat}) \pm 0.36 (\mathrm{syst})) \times 10^{-4}}$ where the dominant systematic uncertainty comes from modeling the nonresonant $B\to (\pi\pi)\ell^+\nu_\ell$ contribution.

Published
2022

315. Revisiting the atmosphere of the exoplanet 51 Eridani b with VLT/SPHERE

Author

Brown-Sevilla, S. B., Maire, A. -L., Mollière, P., Samland, M., Feldt, M., Brandner, W., Henning, Th., Gratton, R., Janson, M., Stolker, T., Hagelberg, J., Zurlo, A., Cantalloube, F., Boccaletti, A., Bonnefoy, M., Chauvin, G., Desidera, S., D'Orazi, V., Lagrange, A. -M., Langlois, M., Menard, F., Mesa, D., Meyer, M., Pavlov, A., Petit, C., Rochat, S., Rouan, D., Schmidt, T., Vigan, A., and Weber, L.

Subjects
Astrophysics - Earth and Planetary Astrophysics
Abstract

[Full abstract in the paper] We aim to better constrain the atmospheric properties of the directly imaged exoplanet 51~Eri~b by using a retrieval approach on higher signal-to-noise data than previously reported. In this context, we also compare the results of using the atmospheric retrieval code \texttt{petitRADTRANS} vs a self-consistent model to fit atmospheric parameters. We present a higher signal-to-noise $YH$ spectrum of the planet and revised $K1K2$ photometry (M$_{K1} = 15.11 \pm 0.04$ mag, M$_{K2} = 17.11 \pm 0.38$ mag). The best-fit parameters obtained using an atmospheric retrieval differ from previous results using self-consistent models. In general, we find that our solutions tend towards cloud-free atmospheres (e.g. log $\tau_{\rm clouds} = -5.20 \pm 1.44$). For our ``nominal'' model with new data, we find a lower metallicity ([Fe/H] $= 0.26\pm$0.30 dex) and C/O ratio ($0.38\pm0.09$), and a slightly higher effective temperature (T$_{\rm{eff}} = 807\pm$45 K) than previous studies. The surface gravity (log $g = 4.05\pm0.37$) is in agreement with the reported values in the literature within uncertainties. We estimate the mass of the planet to be between 2 and 4 M$_{\rm{Jup}}$. When comparing with self-consistent models, we encounter a known correlation between the presence of clouds and the shape of the $P-T$ profiles. Our findings support the idea that results from atmospheric retrievals should not be discussed in isolation, but rather along with self-consistent temperature structures obtained using the retrieval's best-fit parameters., Comment: Accepted for publication in A&A. 21 pages, 7 figures in the main text and 9 figures in the Appendix

Published
2022
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316. The VLT-FLAMES Tarantula Survey: Observational evidence for two distinct populations of massive runaway stars in 30 Doradus

Author

Sana, H., Ramírez-Agudelo, O. H., Hénault-Brunet, V., Mahy, L., Almeida, L. A., de Koter, A., Bestenlehner, J. M., Evans, C. J., Langer, N., Schneider, F. R. N., Crowther, P. A., de Mink, S. E., Herrero, A., Lennon, D. J., Gieles, M., Apellániz, J. Maíz, Renzo, M., Sabbi, E., van Loon, J. Th., and Vink, J. S.

Subjects
Astrophysics - Solar and Stellar Astrophysics, Astrophysics - Astrophysics of Galaxies
Abstract

Two main scenarios have been proposed for origin of massive runaway stars -- dynamical ejection or release from a binary at the first core collapse -- but their relative contribution remains debated. Using two large spectroscopic campaigns towards massive stars in 30 Doradus, we aim to provide observational constraints on the properties of the O-type runaway population in the most massive active star-forming region in the Local group. We use RV measurements of the O-type star populations in 30 Doradus obtained by the VLT-FLAMES Tarantula Survey and the Tarantula Massive Binary Monitoring to identify single and binary O-type runaways. We discuss their rotational properties and qualitatively compare observations with expectations of ejection scenarios. We identify 23 single and one binary O-type runaway objects, most of them outside the main star-forming regions in 30 Doradus. We find an overabundance of rapid rotators (vsini > 200km/s) among the runaway population, providing an explanation of the overabundance of rapidly rotating stars in the 30 Doradus field. Considerations of the projected rotation rates and runaway line-of-sight (los) velocities reveal a conspicuous absence of rapidly rotating (vsini > 210k/ms), fast moving (v_{los} > 60km/s) runaways, and suggest the presence of two different populations of runaway stars: a population of rapidly-spinning but slowly moving runaways and a population of fast moving but slowly rotating ones. These are detected with a ratio close to 2:1 in our sample. We argue that slowly moving but rapidly spinning runaways result from binary ejections, while rapidly moving but slowly spinning runaways could result from dynamical ejections. Given that detection biases will more strongly impact the slow-moving population, our results suggest that the binary evolution scenario dominates the current massive runaway population in 30 Doradus., Comment: Accepted for publication in A&A Letters; 9 pages, 5 figures

Published
2022
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317. Telling emissions apart in a multiphoton resonance: visualizing a conditional evolution

Author

Mavrogordatos, Th. K.

Subjects
Quantum Physics, Condensed Matter - Mesoscale and Nanoscale Physics
Abstract

We find that the phase-space representation of the electromagnetic field inside a driven cavity strongly coupled to a two-level atom can be employed to distinguish photon emissions along a ladder of dressed states sustaining a two-photon resonance. The emissions are told apart by means of the different quantum beats generated by the conditional states they prepare. Sample quantum trajectories explicitly reveal the difference in the transient due to the initial condition, in a background set by the Jaynes-Cummings spectrum and revealed by the strong-coupling limit. Their ensemble-averaged evolution is tracked for a time period similar to that waited for the loss of a next photon as the maximum non-exclusive probability, indicated by the peak of the intensity correlation function., Comment: 10 pages, 4 figures, 56 references, as published in the Journal of Optics

Published
2022
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318. First CLAS12 measurement of DVCS beam-spin asymmetries in the extended valence region

Author

CLAS Collaboration, Christiaens, G., Defurne, M., Sokhan, D., Achenbach, P., Akbar, Z., Amaryan, M. J., Atac, H., Avakian, H., Gayoso, C. Ayerbe, Baashen, L., Baltzell, N. A., Barion, L., Bashkanov, M., Battaglieri, M., Bedlinskiy, I., Benkel, B., Benmokhtar, F., Bianconi, A., Biselli, A. S., Bondi, M., Booth, W. A., Bossù, F., Boiarinov, S., Brinkmann, K. -Th., Briscoe, W. J., Bueltmann, S., Bulumulla, D., Burkert, V. D., Cao, T., Carman, D. S., Carvajal, J. C., Celentano, A., Chatagnon, P., Chesnokov, V., Chetry, T., Ciullo, G., Clash, G., Cole, P. L., Contalbrigo, M., Costantini, G., D'Angelo, A., Dashyan, N., De Vita, R., Deur, A., Diehl, S., Dilks, C., Djalali, C., Dupre, R., Egiyan, H., Ehrhart, M., Alaoui, A. El, Fassi, L. El, Elouadrhiri, L., Fegan, S., Filippi, A., Gates, K., Gavalian, G., Ghandilyan, Y., Gilfoyle, G. P., Girod, F. X., Glazier, D. I., Golubenko, A. A., Gosta, G., Gothe, R. W., Gotra, Y., Griffioen, K. A., Guidal, M., Hafidi, K., Hakobyan, H., Hattawy, M., Hauenstein, F., Hayward, T. B., Heddle, D., Hobart, A., Holmberg, D. E., Holtrop, M., Ilieva, Y., Ireland, D. G., Isupov, E. L., Jo, H. S., Kabir, M. L., Keller, D., Khachatryan, M., Khanal, A., Kim, W., Kripko, A., Kubarovsky, V., Kuhn, S. E., Lagerquist, V., Lanza, L., Leali, M., Lee, S., Lenisa, P., Li, X., Livingston, K., MacGregor, I . J . D., Marchand, D., Mascagna, V., Matousek, G., McKinnon, B., McLauchlin, C., Meziani, Z. E., Migliorati, S., Milner, R. G., Mineeva, T., Mirazita, M., Mokeev, V., Molina, E., Camacho, C. Munoz, Nadel-Turonski, P., Naidoo, P., Neupane, K., Niccolai, S., Nicol, M., Niculescu, G., Osipenko, M., Ouillon, M., Pandey, P., Paolone, M., Pappalardo, L. L., Paremuzyan, R., Pasyuk, E., Paul, S. J., Phelps, W., Pilleux, N., Pokhrel, M., Poudel, J., Price, J. W., Prok, Y., Radic, A., Ramasubramanian, N., Raue, B. A., Reed, T., Richards, J., Ripani, M., Ritman, J., Rossi, P., Sabatié, F., Salgado, C., Schadmand, S., Schmidt, A., Scott, M. B. C., Sharabian, Y. G., Shirokov, E. V., Shrestha, U., Simmerling, P., Sparveris, N., Spreafico, M., Stepanyan, S., Strakovsky, I. I., Strauch, S., Tan, J. A., Trotta, N., Turisini, M., Tyson, R., Ungaro, M., Vallarino, S., Venturelli, L., Voskanyan, H., Voutier, E., Watts, D. P., Wei, X., Williams, R., Wishart, R., Wood, M. H., Zachariou, N., Zhang, J., Zhao, Z. W., Ziegler, V., and Zurek, M.

Subjects
High Energy Physics - Experiment
Abstract

Deeply virtual Compton scattering (DVCS) allows one to probe Generalized Parton Distributions (GPDs) describing the 3D structure of the nucleon. We report the first measurement of the DVCS beam-spin asymmetry using the CLAS12 spectrometer with a 10.2 and 10.6 GeV electron beam scattering from unpolarised protons. The results greatly extend the $Q^2$ and Bjorken-$x$ phase space beyond the existing data in the valence region and provide over 2000 new data points measured with unprecedented statistical uncertainty, setting new, tight constraints for future phenomenological studies., Comment: Revised Figure 4 and discussion around the number of effective ANNs after Bayesian reweighting

Published
2022

319. The Isaac Newton Telescope monitoring survey of Local Group dwarf galaxies--V. The star formation history of Sagittarius dwarf irregular galaxy derived from long period variable stars

Author

Parto, Tahere, Dehghani, Shahrzad, Javadi, Atefeh, Saremi, Elham, van Loon, Jacco Th., Khosroshahi, Habib G., McDonald, Iain, Mirtorabi, Mohammad T., Navabi, Mahdieh, and Saberi, Maryam

Subjects
Astrophysics - Astrophysics of Galaxies, Astrophysics - Solar and Stellar Astrophysics
Abstract

We conducted an optical monitoring survey of the Sagittarius dwarf irregular galaxy (SagDIG) during the period of June 2016 -- October 2017, using the 2.5-m Isaac Newton Telescope (INT) at La Palama. Our goal was to identify Long Period Variable stars (LPVs), namely asymptotic giant branch stars (AGBs) and red supergiant stars (RSGs), to obtain the Star Formation History (SFH) of isolated, metal-poor SagDIG. For our purpose, we used a method that relies on evaluating the relation between luminosity and the birth mass of these most evolved stars. We found $27$ LPV candidates within two half-light radii of SagDIG. $10$ LPV candidates were in common with previous studies, including one very dusty AGB (x-AGB). By adopting the metallicity $Z = 0.0002$ for older population and $Z=0.0004$ for younger ages, we estimated that the star formation rate changes from $0.0005\pm0.0002$ M$_{\odot}$yr$^{-1}$kpc$^{-2}$ ($13$ Gyr ago) to $0.0021 \pm 0.0010$ M$_{\odot}$yr$^{-1}$kpc$^{-2}$ ($0.06$ Gyr ago). Like many dwarf irregular galaxies, SagDIG has had continuous star formation activity across its lifetime, though with different rates, and experiences an enhancement of star formation since $z \simeq 1$. We also evaluated the total stellar mass within two half-light radii of SagDIG for three choices of metallicities. For metallicity $Z = 0.0002$ and $Z=0.0004$ we estimated the stellar mass M$_*$ = ($5.4 \pm 2.3$) $\times$ $10^ 6$ and ($3.0 \pm 1.3$) $\times$ $10^ 6$ M$_{\odot}$, respectively. Additionally, we determined a distance modulus $\mu$ = $25.27\pm0.05$ mag, using the tip of the red giant branch (TRGB)., Comment: 16 pages, Accepted for publication in ApJ

Published
2022
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320. Particle Physics at the European Spallation Source

Author

Abele, H., Alekou, A., Algora, A., Andersen, K., Baessler, S., Barron-Palos, L., Barrow, J., Baussan, E., Bentley, P., Berezhiani, Z., Bessler, Y., Bhattacharyya, A. K., Bianchi, A., Bijnens, J., Blanco, C., Kraljevic, N. Blaskovic, Blennow, M., Bodek, K., Bogomilov, M., Bohm, C., Bolling, B., Bouquerel, E., Brooijmans, G., Broussard, L. J., Buchan, O., Burgman, A., Calen, H., Carlile, C. J., Cederkall, J., Chanel, E., Christiansen, P., Cirigliano, V., Collar, J. I., Collins, M., Crawford, C. B., Morales, E. Cristaldo, Cupial, P., D'Alessi, L., Damian, J. I. M., Danared, H., Dancila, D., de Andre, J. P. A. M., Delahaye, J. P., Degenkolb, S., Di Julio, D. D., Dracos, M., Dunne, K., Efthymiopoulos, I., Ekelof, T., Eklund, L., Eshraqi, M., Esteban, I., Fanourakis, G., Farricker, A., Fernandez-Martinez, E., Ferreira, M. J., Fertl, M., Fierlinger, P., Folsom, B., Frank, A., Fratangelo, A., Friman-Gayer, U., Fukuda, T., Fynbo, H . O . U., Sosa, A. Garcia, Gazis, N., Galnander, B., Geralis, Th., Ghosh, M., Gokbulut, G., Gomez-Cadenas, J . J., Gonzalez-Alonso, M., Gonzalez, F., Halic, L., Happe, C., Heil, P., Heinz, A., Herde, H., Holl, M., Jenke, T., Jenssen, M., Jericha, E., Johansson, H. T., Johansson, R., Johansson, T., Kamyshkov, Y., Topaksu, A. Kayis, Kildetoft, B., Kirch, K., Klicek, B., Klinkby, E., Kolevatov, R., Konrad, G., Koziol, M., Krhac, K., Kupsc, A., Lacny, L., Larizgoitia, L., Lewis, C. M., Lindroos, M., Lychagin, E., Lytken, E., Maiano, C., Marciniewski, P., Markaj, G., Markisch, B., Marrelli, C., Martins, C., Meirose, B., Mezzetto, M., Milas, N., Milstead, D., Monrabal, F., Muhrer, G., Nepomuceno, A., Nesvizhevsky, V., Nilsson, T., Novella, P., Oglakci, M., Ohlsson, T., Olvegard, M., Oskarsson, A., Ota, T., Park, J., Patrzalek, D., Perrey, H., Persoz, M., Petkov, G., Piegsa, F. M., Pistillo, C., Poussot, P., Privitera, P., Rataj, B., Ries, D., Rizzi, N., Rosauro-Alcaraz, S., Rozpedzik, D., Saiang, D., Santoro, V., Schmidt, U., Schober, H., Schulthess, I., Silverstein, S., Simon, A., Sina, H., Snamina, J., Snow, W. M., Soldner, T., Stavropoulos, G., Stipcevic, M., Szybinski, B., Takibayev, A., Tang, Z., Tarkeshian, R., Theroine, C., Thorne, J., Terranova, F., Thomas, J., Tolba, T., Torres-Sanchez, P., Trachanas, E., Tsenov, R., Uggerhoj, U. I., Vankova-Kirilova, G., Vassilopoulos, N., Wagner, R., Wang, X., Wildner, E., Wolke, M., Wurtz, J., Yiu, S. C., Yoon, S. G., Young, A. R., Zanini, L., Zejma, J., Zerzion, D., Zimmer, O., Zormpa, O., and Zou, Y.

Subjects
Physics - Instrumentation and Detectors, High Energy Physics - Experiment, High Energy Physics - Phenomenology, Nuclear Experiment
Abstract

Presently under construction in Lund, Sweden, the European Spallation Source (ESS) will be the world's brightest neutron source. As such, it has the potential for a particle physics program with a unique reach and which is complementary to that available at other facilities. This paper describes proposed particle physics activities for the ESS. These encompass the exploitation of both the neutrons and neutrinos produced at the ESS for high precision (sensitivity) measurements (searches)., Comment: 121 pages, updated version after referee comments

Published
2022
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321. Radial Velocity Survey for Planets around Young stars (RVSPY) A transiting warm super-Jovian planet around HD 114082, a young star with a debris disk

Author

Zakhozhay, O., Launhardt, R., Trifonov, T., Kürster, M., Reffert, S., Henning, Th., Brahm, R., Vinés, J., Marleau, G. -D., and Patel, J.

Subjects
Astrophysics - Earth and Planetary Astrophysics, Astrophysics - Solar and Stellar Astrophysics
Abstract

Aiming to detect planetary companions to young stars with debris disks via the radial velocity method, we observed HD114082 during April 2018 - August 2022 as one of the targets of our RVSPY program (Radial Velocity Survey for Planets around Young stars). We used the FEROS spectrograph, mounted to the MPG/ESO 2.2 m telescope in Chile, to obtain high signal-to-noise spectra and time series of precise radial velocities (RVs). Additionally, we analyzed archival HARPS spectra and TESS photometric data. We used the CERES, CERES++ and SERVAL pipelines to derive RVs and activity indicators and ExoStriker for the independent and combined analysis of the RVs and TESS photometry. We report the discovery of a warm super-Jovian companion around HD114082 based on a 109.8$\pm$0.4 day signal in the combined RV data from FEROS and HARPS, and on one transit event in the TESS photometry. The best-fit model indicates a 8.0$\pm$1.0 Mjup companion with a radius of 1.00$\pm$0.03 Rjup in an orbit with a semi-major axis of 0.51$\pm$0.01 au and an eccentricity of 0.4$\pm$0.04. The companions orbit is in agreement with the known near edge-on debris disk located at about 28 au. HD114082b is possibly the youngest (15$\pm$6 Myr), and one of only three younger than 100 Myr giant planetary companions for which both their mass and radius have been determined observationally. It is probably the first properly model-constraining giant planet that allows distinguishing between hot and cold-start models. It is significantly more compatible with the cold-start model., Comment: 10 pages, 9 figures, 5 tables; Accepted for publication in A&A Letters

Published
2022
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322. Review of the online analyses of multi-messenger alerts and electromagnetic transient events with the ANTARES neutrino telescope

Author

Albert, A., Alves, S., André, M., Ardid, M., Ardid, S., Aubert, J. -J., Aublin, J., Baret, B., Basa, S., Belhorma, B., Bendahman, M., Benfenati, F., Bertin, V., Biagi, S., Bissinger, M., Boumaaza, J., Bouta, M., Bouwhuis, M. C., Brânzaş, H., Bruijn, R., Brunner, J., Busto, J., Caiffi, B., Calvo, D., Campion, S., Capone, A., Caramete, L., Carr, J., Carretero, V., Celli, S., Chabab, M., Chau, T. N., Moursli, R. Cherkaoui El, Chiarusi, T., Circella, M., Coelho, J. A. B., Coleiro, A., Coniglione, R., Coyle, P., Creusot, A., Díaz, A. F., De Martino, B., Distefano, C., Di Palma, I., Domi, A., Donzaud, C., Dornic, D., Drouhin, D., Eberl, T., van Eeden, T., van Eijk, D., Khayati, N. El, Enzenhöfer, A., Fasano, M., Fermani, P., Ferrara, G., Filippini, F., Fusco, L., Gagliardini, S., García, J., Gay, P., Geißelbrecht, N., Glotin, H., Gozzini, R., Ruiz, R. Gracia, Graf, K., Guidi, C., Haegel, L., Hallmann, S., van Haren, H., Heijboer, A. J., Hello, Y., Hernández-Rey, J. J., Hößl, J., Hofestädt, J., Huang, F., Illuminati, G., James, C. W., Jisse-Jung, B., de Jong, M., de Jong, P., Kadler, M., Kalekin, O., Katz, U., Kouchner, A., Kreykenbohm, I., Kulikovskiy, V., Lahmann, R., Lamoureux, M., Lefèvre, D., Leonora, E., Levi, G., Stum, S. Le, Lopez-Coto, D., Loucatos, S., Maderer, L., Manczak, J., Marcelin, M., Margiotta, A., Marinelli, A., Martínez-Mora, J. A., Melis, K., Migliozzi, P., Moussa, A., Muller, R., Nauta, L., Navas, S., Nezri, E., Fearraigh, B. Ó, Păun, A., Păvălaş, G. E., Pellegrino, C., Perrin-Terrin, M., Pestel, V., Piattelli, P., Pieterse, C., Poirè, C., Popa, V., Pradier, T., Randazzo, N., Real, D., Reck, S., Riccobene, G., Romanov, A., Saina, A., Sánchez-Losa, A., Greus, F. Salesa, Samtleben, D. F. E., Sanguineti, M., Sapienza, P., Schnabel, J., Schumann, J., Schüssler, F., Seneca, J., Spurio, M., Stolarczyk, Th., Taiuti, M., Tayalati, Y., Tingay, S. J., Vallage, B., Van Elewyck, V., Versari, F., Viola, S., Vivolo, D., Wilms, J., Zavatarelli, S., Zegarelli, A., Zornoza, J. D., and Zúñiga, J.

Subjects
Astrophysics - High Energy Astrophysical Phenomena
Abstract

By constantly monitoring at least one complete hemisphere of the sky, neutrino telescopes are well designed to detect neutrinos emitted by transient astrophysical events. Real-time searches with the ANTARES telescope have been performed to look for neutrino candidates coincident with gamma-ray bursts detected by the Swift and Fermi satellites, highenergy neutrino events registered by IceCube, transient events from blazars monitored by HAWC, photon-neutrino coincidences by AMON notices and gravitational wave candidates observed by LIGO/Virgo. By requiring temporal coincidence, this approach increases the sensitivity and the significance of a potential discovery. Thanks to the good angular accuracy of neutrino candidates reconstructed with the ANTARES telescope, a coincident detection can also improve the positioning area of non-well localised triggers such as those detected by gravitational wave interferometers. This paper summarises the results of the follow-up performed by the ANTARES telescope between 01/2014 and 02/2022, which corresponds to the end of the data taking period., Comment: 21 pages, 10 figures, JCAP08 (2023) 072 (19 pp

Published
2022

323. The first look at Narrow-Line Seyfert 1 Galaxies with eROSITA

Author

Grünwald, G., Boller, Th., Rakshit, S., Buchner, J., Dauser, T., Freyberg, M., Liu, T., Salvato, M., and Schichtel, A.

Subjects
Astrophysics - High Energy Astrophysical Phenomena
Abstract

We present the first look at the spectral and timing analysis of Narrow-Line Seyfert 1 Galaxies (NLS1s) with the extended ROentgen Survey with an Imaging Telescope Array (eROSITA) on board the Spectrum-Roentgen-Gamma (SRG) mission. The sample of about 1,200 NLS1s was obtained via cross-match of the first eROSITA All-Sky Survey (eRASS1) catalogue with the catalogue of spectroscopically selected NLS1s from the Sloan Digital Sky Survey (SDSS) DR12 by Rakshit et al. [ApJS, 229, 39 (2017)]. The X-ray spectral analysis is based on a simple power-law fit. The photon index distribution has a mean value of about 2.81+-0.03, as expected from previous X-ray studies of NLS1s. Interestingly, it is positively skewed, and about 10 percent of the sources are located in the super-soft tail of photon indices larger than 4. These sources are of further interest as their source counts run into the X-ray background at values at around 1 keV. We argue that ionised outflows have been detected by eROSITA and may account for some of the extreme spectral steepness, which is supported by correlations found between the photon index and optical outflows parameters. We analysed the intrinsic X-ray variability of the eRASS1 to eRASS3 light curves of the sample but do not find significant variability neither during the individual survey scans nor between them., Comment: 11 pages, 10 figures, accepted for publication in Section 4. Extragalactic astronomy of Astronomy and Astrophysics

Published
2022
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324. Spectral identification and classification of dusty stellar sources using spectroscopic and multiwavelength observations through machine learning

Author

Ghaziasgar, Sepideh, Masoudnezhad, Amirhossein, Javadi, Atefeh, van Loon, Jacco Th., Khosroshahi, Habib G., and Khosravaninezhad, Negin

Subjects
Astrophysics - Astrophysics of Galaxies, Astrophysics - Solar and Stellar Astrophysics
Abstract

We proposed a machine learning approach to identify and distinguish dusty stellar sources employing supervised and unsupervised methods and categorizing point sources, mainly evolved stars, using photometric and spectroscopic data collected over the IR sky. Spectroscopic data is typically used to identify specific infrared sources. However, our goal is to determine how well these sources can be identified using multiwavelength data. Consequently, we developed a robust training set of spectra of confirmed sources from the Large and Small Magellanic Clouds derived from SAGE-Spec Spitzer Legacy and SMC-Spec Spitzer Infrared Spectrograph (IRS) spectral catalogs. Subsequently, we applied various learning classifiers to distinguish stellar subcategories comprising young stellar objects (YSOs), C-rich asymptotic giant branch (CAGB), O-rich AGB stars (OAGB), Red supergiant (RSG), and post-AGB stars. We have classified around 700 counts of these sources. It should be highlighted that despite utilizing the limited spectroscopic data we trained, the accuracy and models' learning curve provided outstanding results for some of the models. Therefore, the Support Vector Classifier (SVC) is the most accurate classifier for this limited dataset., Comment: 6 pages, 3 figures, 3 tables, Proceeding of IAU Symposium 368: "Machine Learning in Astronomy: Possibilities and Pitfalls", to be published in the "IAU Proceedings Series"

Published
2022

326. Non-linear Extreme Ultraviolet Applications with Attosecond Pulses

Author

Skantzakis, E., Orfanos, I., Nayak, A., Makos, I., Vassakis, E., Lamprou, Th., Tsafas, V., Csizmadia, T., Diveki, Z., Nagyillés, B., Farkas, B., Mukhopadhyay, S., Rajak, D., Madas, S., Upadhyay Kahaly, M., Kahaly, S., Weissenbilder, R., Eng-Johnsson, P., Appi, E., L’Huillier, A., Sansone, G., Varju, K., Nikolopoulos, L. A. A., Emmanouilidou, A., Tzallas, P., Charalambidis, D., Lee, Young Pak, Series Editor, Lockwood, David J., Series Editor, Ossi, Paolo M., Series Editor, Yamanouchi, Kaoru, Series Editor, DiMauro, Louis F., editor, and Hill, III, Wendell T., editor

Published
2024
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329. Progressive Healthcare Pedagogy: An Application Merging ChatGPT and AI-Video Technologies for Gamified and Cost-Effective Scenario-Based Learning

Author

Pears, Matthew, Poussa, Cherry, Konstantinidis, Stathis Th., Kacprzyk, Janusz, Series Editor, Gomide, Fernando, Advisory Editor, Kaynak, Okyay, Advisory Editor, Liu, Derong, Advisory Editor, Pedrycz, Witold, Advisory Editor, Polycarpou, Marios M., Advisory Editor, Rudas, Imre J., Advisory Editor, Wang, Jun, Advisory Editor, Auer, Michael E., editor, and Tsiatsos, Thrasyvoulos, editor

Published
2024
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330. Breeding Potentials of Wild Forest Rattans Palms to Ensure Food Security

Author

Haokip, Dimjaneng, Senjam Jinus, S., Longmei, Ningthaipuilu, Sharma, Sanjukta Samurailatpam, Bhaigyabati, Th., Devi, Yendrembam K., Devi, Akoijam Ranjita, Lalramhlimi, B., Mutum, Vandana, Swapana, Ningombam, Kalpana, Athokpam, Vanitha, J., Ramawat, Kishan Gopal, Series Editor, Jatav, Hanuman Singh, editor, Rajput, Vishnu D., editor, Minkina, Tatiana, editor, Van Hullebusch, Eric D., editor, and Dutta, Asik, editor

Published
2024
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331. Attosecond Physics and Quantum Information Science

Author

Lewenstein, M., Baldelli, N., Bhattacharya, U., Biegert, J., Ciappina, M. F., Grass, T., Grochowski, P. T., Johnson, A. S., Lamprou, Th., Maxwell, A. S., Ordóñez, A., Pisanty, E., Rivera-Dean, J., Stammer, P., Tzallas, P., Argenti, Luca, editor, Chini, Michael, editor, and Fang, Li, editor

Published
2024
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332. HEALINT4ALL Digital Interactive Platform for European and National Placements Audit for Medicine and Allied Health Professions Following a User-Centered Design

Author

Konstantinidis, Stathis Th., Poultourtzidis, Ioannis, Papamalis, Foivos, Spachos, Dimitris, Savvidis, Theodoros, Athanasopoulos, Nikolaos, Nikolaidou, Maria, Tilley, Zoe, Ko, Stan, Henderson, James, Cunningham, Sheila, Pam, Hodge, Höijer-Brear, Viveka, Törne, Mari, Lillo-Crespo, Manuel, Catala Rodriguez, Maria Pilar, Stefanowicz-Kocol, Anna, Jankowicz-Szymanska, Agnieszka, Grochowska, Aneta, Kołpa, Małgorzata, Hall, Carol, Bamidis, Panagiotis D., Kacprzyk, Janusz, Series Editor, Gomide, Fernando, Advisory Editor, Kaynak, Okyay, Advisory Editor, Liu, Derong, Advisory Editor, Pedrycz, Witold, Advisory Editor, Polycarpou, Marios M., Advisory Editor, Rudas, Imre J., Advisory Editor, Wang, Jun, Advisory Editor, Auer, Michael E., editor, and Tsiatsos, Thrasyvoulos, editor

Published
2024
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334. Estimating LNAPL Volumes in Unimodal and Multimodal Subsurface Pore Systems

Author

Alfaro Soto, Miguel A., van Genuchten, Martinus Th., Lenhard, Robert J., Chang, Hung K., Bennett, Erin R., Series Editor, Panagiotakis, Iraklis, Series Editor, Chrysochoou, Maria, Advisory Editor, Dermatas, Dimitris, Advisory Editor, di Palma, Luca, Advisory Editor, Lekkas, Demetris Francis, Advisory Editor, Menone, Mirta, Advisory Editor, Metcalfe, Chris, Advisory Editor, Moore, Matthew, Advisory Editor, García-Rincón, Jonás, editor, Gatsios, Evangelos, editor, Lenhard, Robert J., editor, Atekwana, Estella A., editor, and Naidu, Ravi, editor

Published
2024
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336. The Relationship between EFL Oral Reading Fluency and Silent Reading Fluency: What Can a Speed Reading Course Tell Us?

Author

Y?n, Tr?n Th? Ng?c

Abstract

A great deal of past research in reading fluency has focused on oral reading fluency in L1, but literature in EFL oral reading and silent reading is still in its infancy. This study attempts to examine the development of silent reading fluency in a speed reading course and aims to determine whether an improvement in silent reading speed facilitates oral reading fluency development. The participants were from four intact classes at a university in Vietnam. While the four groups were following the usual English program at the university, the two treatment groups were also following a speed reading course, which lasted two months. In each session of the course, they were asked to read a 550-word text and answered 10 comprehension questions that accompanied the text. The results indicated that the treatment groups significantly improved their reading fluency in and outside the speed reading course, but made minimal increases in oral reading speed.

Published
2021

337. New measurement of double-β decays of Mo100 to excited states of Ru100 with the CUPID-Mo experiment

Author

Augier, C, Barabash, AS, Bellini, F, Benato, G, Beretta, M, Bergé, L, Billard, J, Borovlev, Yu A, Cardani, L, Casali, N, Cazes, A, Chapellier, M, Chiesa, D, Dafinei, I, Danevich, FA, De Jesus, M, Dixon, T, Dumoulin, L, Eitel, K, Ferri, F, Fujikawa, BK, Gascon, J, Gironi, L, Giuliani, A, Grigorieva, VD, Gros, M, Helis, DL, Huang, HZ, Huang, R, Imbert, L, Johnston, J, Juillard, A, Khalife, H, Kleifges, M, Kobychev, VV, Kolomensky, Yu G, Konovalov, SI, Kotila, J, Loaiza, P, Ma, L, Makarov, EP, de Marcillac, P, Mariam, R, Marini, L, Marnieros, S, Navick, X-F, Nones, C, Norman, EB, Olivieri, E, Ouellet, JL, Pagnanini, L, Pattavina, L, Paul, B, Pavan, M, Peng, H, Pessina, G, Pirro, S, Poda, DV, Polischuk, OG, Pozzi, S, Previtali, E, Redon, Th, Rojas, A, Rozov, S, Sanglard, V, Scarpaci, JA, Schmidt, B, Shen, Y, Shlegel, VN, Singh, V, Tomei, C, Tretyak, VI, Umatov, VI, Vagneron, L, Velázquez, M, Welliver, B, Winslow, L, Xue, M, Yakushev, E, Zarytskyy, M, and Zolotarova, AS

Subjects
Nuclear and Plasma Physics, Particle and High Energy Physics, Physical Sciences, Nuclear and plasma physics
Abstract

The CUPID-Mo experiment, located at the Laboratoire Souterrain de Modane (France), was a demonstrator experiment for CUPID. It consisted of an array of 20Li2Mo100O4 (LMO) calorimeters, each equipped with a Ge light detector for particle identification. In this work, we present the result of a search for two-neutrino and neutrinoless double-β decays of Mo100 to the first 0+ and 2+ excited states of Ru100 using the full CUPID-Mo exposure (2.71kgyr of LMO). We measure the half-life of 2νββ decay to the 01+ state as T1/22ν→01+=(7.5±0.8(stat.)-0.3+0.4(syst.))×1020yr. The bolometric technique enables measurement of the electron energies as well as the γ rays from nuclear deexcitation and this allows us to set new limits on the two-neutrino decay to the 21+ state of T1/22ν→21+>4.4×1021yr(90% c.i.) and on the neutrinoless modes of T1/20ν→21+>2.1×1023yr(90% c.i.), T1/20ν→01+>1.2×1023yr(90% c.i.). Information on the electrons' spectral shape is obtained, which allows us to make the first comparison of the single and higher state dominance 2νββ decay models for the 01+ excited state of Ru100.

Published
2023

338. Star Formation History of Two Fields in the Halo of NGC5128

Author

Aghdam, Sima T., Javadi, Atefeh, Hashemi, Seyedazim, van Loon, Jacco Th., Khosroshahi, Habib, Golshan, Roya H., Saremi, Elham, and Saberi, Maryam

Subjects
Astrophysics - Astrophysics of Galaxies, Astrophysics - Solar and Stellar Astrophysics
Abstract

NGC5128 galaxy is a giant elliptical galaxy located in the Centaurus group of galaxies at 3.8 Mpc. We aim to study the star formation history (SFH) of two different fields of the galaxy. The northeastern field (Field 1) is located at a distance of 18.8 kpc, while the southern field (Field 2) is at 9.9 kpc. We use a photometric method that is based on identifying long period variable (LPV) stars and asymptotic giant branch (AGB) stars, as they are strong tracers of star formation and galaxy evolution due to their luminosity and variability; 395 LPVs in Field 1 and 671 LPVs in Field 2 have been identified. These two fields present similar SFHs, although the SF rate of Field 2 is more enhanced. We find that the galaxy has three major star formation episodes t $\sim$ 800 Myr ago, t $\sim$ 3.2 Gyr ago, and t $\sim$ 10 Gyr ago, where t is look-back time. The rate of star formation at $\sim$ 800 Myr ago agrees with previous studies suggesting that the galaxy experienced a merger around that time. Furthermore, NGC5128 has experienced a lower star formation rate in its recent history which could have been driven by jet-induction star formation and multiple outbursts of AGN activity in this galaxy, as well as a minor merger around 400 Myr ago., Comment: 4 pages, 1 figure, Proceeding Paper of IAU Symposium 373

Published
2022
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339. A multidimensional study of the structure function ratio $\sigma_{LT'}/\sigma_{0}$ from hard exclusive $\pi^+$ electro-production off protons in the GPD regime

Author

Diehl, S., Kim, A., Joo, K., Achenbach, P., Akbar, Z., Amaryan, M. J., Atac, H., Avagyan, H., Gayoso, C. Ayerbe, Baashen, L., Barion, L., Bashkanov, M., Battaglieri, M., Bedlinskiy, I., Benkel, B., Benmokhtar, F., Bianconi, A., Biselli, A. S., Bondi, M., Booth, W. A., Bossu, F., Boiarinov, S., Brinkmann, K. -Th., Briscoe, W. J., Bueltmann, S., Bulumulla, D., Burkert, V. D., Carman, D. S., Celentano, A., Chatagnon, P., Chesnokov, V., Chetry, T., Ciullo, G., Clash, G., Cole, P. L., Contalbrigo, M., Costantini, G., D'Angelo, A., Dashyan, N., De Vita, R., Defurne, M., Deur, A., Djalali, C., Dupre, R., Egiyan, H., Ehrhart, M., Alaoui, A. El, Fassi, L. El, Elouadrhiri, L., Fegan, S., Filippi, A., Gavalian, G., Ghandilyan, Y., Gilfoyle, G. P., Glazier, D. I., Golubenko, A. A., Gosta, G., Gothe, R. W., Gotra, Y., Grifoen, K. A., Guidal, M., Hafdi, K., Hakobyan, H., Hattawy, M., Hayward, T. B., Heddle, D., Hobart, A., Holtrop, M., Ilieva, Y., Ireland, D. G., Isupov, E. L., Jo, H. S., Khachatryan, M., Khanal, A., Kim, W., Kripko, A., Kubarovsky, V., Lagerquist, V., Laget, J. -M., Lanza, L., Leali, M., Lee, S., Lenisa, P., Li, X., Livingston, K., MacGregor, I . J. D., Marchand, D., Mascagna, V., McKinnon, B., Meziani, Z. E., Migliorati, S., Mineeva, T., Mirazita, M., Mokeev, V., Molina, Esteban, Montgomery, R. A., Camacho, C. Munoz, Nadel-Turonski, P., Naidoo, P., Neupane, K., Niccolai, S., Nicol, M., Niculescu, G., Osipenko, M., Ouillon, M., Pandey, P., Paolone, M., Pappalardo, L. L., Paremuzyan, R., Pasyuk, E., Paul, S. J., Phelps, W., Pilleux, N., Pokhrel, M., Poudel, J., Price, J. W., Prok, Y., Reed, Trevor, Richards, J., Ripani, M., Ritman, J., Rossi, P., Sabatie, F., Salgado, C., Schadmand, S., Schmidt, A., Sharabian, Y., Shirokov, E. V., Shrestha, U., Simmerling, P., Sokhan, D., Sparveris, N., Spreafco, M., Stepanyan, S., Strakovsky, I. I., Strauch, S., Tan, J. A., Trotta, N., Turisini, M., Tyson, R., Ungaro, M., Vallarino, S., Venturelli, L., Voskanyan, H., Voutier, E., Watts, D. P., Wei, X., Williams, R., Wishart, R., Wood, M. H., Zachariou, N., Zhang, J., Zhao, Z. W., and Zurek, M.

Subjects
High Energy Physics - Experiment
Abstract

A multidimensional extraction of the structure function ratio $\sigma_{LT'}/\sigma_{0}$ from the hard exclusive $\vec{e} p \to e^\prime n \pi^+$ reaction above the resonance region has been performed. The study was done based on beam-spin asymmetry measurements using a 10.6 GeV incident electron beam on a liquid-hydrogen target and the CLAS12 spectrometer at Jefferson Lab. The measurements focus on the very forward regime ($t/Q^{2}$ $\ll$ 1) with a wide kinematic range of $x_{B}$ in the valence regime (0.17 $<$ $x_{B}$ $<$ 0.55), and virtualities $Q^{2}$ ranging from 1.5 GeV$^{2}$ up to 6 GeV$^{2}$. The results and their comparison to theoretical models based on Generalized Parton Distributions demonstrate the sensitivity to chiral-odd GPDs and the directly related tensor charge of the nucleon. In addition, the data is compared to an extension of a Regge formalism at high photon virtualities. It was found that the Regge model provides a better description at low $Q^{2}$, while the GPD model is more appropriate at high $Q^{2}$., Comment: arXiv admin note: text overlap with arXiv:2007.15677

Published
2022
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340. Determination of $|V_{cb}|$ from $B\to D\ell\nu$ decays using 2019-2021 Belle II data

Author

Belle II collaboration, Abudinén, F., Adachi, I., Adamczyk, K., Aggarwal, L., Ahlburg, P., Ahmed, H., Ahn, J. K., Aihara, H., Akopov, N., Aloisio, A., Ameli, F., Andricek, L., Ky, N. Anh, Asner, D. M., Atmacan, H., Aulchenko, V., Aushev, T., Aushev, V., Aziz, T., Babu, V., Bacher, S., Bae, H., Baehr, S., Bahinipati, S., Bakich, A. M., Bambade, P., Banerjee, Sw., Bansal, S., Barrett, M., Batignani, G., Baudot, J., Bauer, M., Baur, A., Beaubien, A., Beaulieu, A., Becker, J., Behera, P. K., Bennett, J. V., Bernieri, E., Bernlochner, F. U., Bertacchi, V., Bertemes, M., Bertholet, E., Bessner, M., Bettarini, S., Bhardwaj, V., Bhuyan, B., Bianchi, F., Bilka, T., Bilokin, S., Biswas, D., Bobrov, A., Bodrov, D., Bolz, A., Bondar, A., Bonvicini, G., Bozek, A., Bračko, M., Branchini, P., Braun, N., Briere, R. A., Browder, T. E., Brown, D. N., Budano, A., Burmistrov, L., Bussino, S., Campajola, M., Cao, L., Casarosa, G., Cecchi, C., Červenkov, D., Chang, M. -C., Chang, P., Cheaib, R., Cheema, P., Chekelian, V., Chen, C., Chen, Y. Q., Chen, Y. -T., Cheon, B. G., Chilikin, K., Chirapatpimol, K., Cho, H. -E., Cho, K., Cho, S. -J., Choi, S. -K., Choudhury, S., Cinabro, D., Corona, L., Cremaldi, L. M., Cunliffe, S., Czank, T., Das, S., Dash, N., Dattola, F., De La Cruz-Burelo, E., De La Motte, S. A., de Marino, G., De Nardo, G., De Nuccio, M., De Pietro, G., de Sangro, R., Deschamps, B., Destefanis, M., Dey, S., De Yta-Hernandez, A., Dhamija, R., Di Canto, A., Di Capua, F., Di Carlo, S., Dingfelder, J., Doležal, Z., Jiménez, I. Domínguez, Dong, T. V., Dorigo, M., Dort, K., Dossett, D., Dreyer, S., Dubey, S., Duell, S., Dujany, G., Ecker, P., Eidelman, S., Eliachevitch, M., Epifanov, D., Feichtinger, P., Ferber, T., Ferlewicz, D., Fillinger, T., Finck, C., Finocchiaro, G., Fischer, P., Flood, K., Fodor, A., Forti, F., Frey, A., Friedl, M., Fulsom, B. G., Gabriel, M., Gabrielli, A., Gabyshev, N., Ganiev, E., Garcia-Hernandez, M., Garg, R., Garmash, A., Gaur, V., Gaz, A., Gebauer, U., Gellrich, A., Gemmler, J., Geßler, T., Ghevondyan, G., Giakoustidis, G., Giordano, R., Giri, A., Glazov, A., Gobbo, B., Godang, R., Goldenzweig, P., Golob, B., Gomis, P., Gong, G., Grace, P., Gradl, W., Granderath, S., Graziani, E., Greenwald, D., Gu, T., Guan, Y., Gudkova, K., Guilliams, J., Hadjivasiliou, C., Halder, S., Hara, K., Hara, T., Hartbrich, O., Hayasaka, K., Hayashii, H., Hazra, S., Hearty, C., Hedges, M. T., de la Cruz, I. Heredia, Villanueva, M. Hernández, Hershenhorn, A., Higuchi, T., Hill, E. C., Hirata, H., Hoek, M., Hohmann, M., Hollitt, S., Horak, P., Hotta, T., Hsu, C. -L., Huang, K., Humair, T., Iijima, T., Inami, K., Inguglia, G., Ipsita, N., Jabbar, J. Irakkathil, Ishikawa, A., Ito, S., Itoh, R., Iwasaki, M., Iwasaki, Y., Iwata, S., Jackson, P., Jacobs, W. W., Jaffe, D. E., Jang, E. -J., Jeandron, M., Jeon, H. B., Ji, Q. P., Jia, S., Jin, Y., Joo, C., Joo, K. K., Junkerkalefeld, H., Kadenko, I., Kahn, J., Kakuno, H., Kaleta, M., Kaliyar, A. B., Kandra, J., Kang, K. H., Kang, S., Kapusta, P., Karl, R., Karyan, G., Kato, Y., Kawai, H., Kawasaki, T., Ketter, C., Kichimi, H., Kiesling, C., Kim, C. -H., Kim, D. Y., Kim, H. J., Kim, K. -H., Kim, K., Kim, S. -H., Kim, Y. -K., Kim, Y., Kimmel, T. D., Kindo, H., Kinoshita, K., Kleinwort, C., Knysh, B., Kodyš, P., Koga, T., Kohani, S., Kojima, K., Komarov, I., Konno, T., Korobov, A., Korpar, S., Kovalchuk, N., Kovalenko, E., Kowalewski, R., Kraetzschmar, T. M. G., Krinner, F., Križan, P., Kroeger, R., Krohn, J. F., Krokovny, P., Krüger, H., Kuehn, W., Kuhr, T., Kumar, J., Kumar, M., Kumar, R., Kumara, K., Kumita, T., Kunigo, T., Künzel, M., Kurz, S., Kuzmin, A., Kvasnička, P., Kwon, Y. -J., Lacaprara, S., Lai, Y. -T., La Licata, C., Lalwani, K., Lam, T., Lanceri, L., Lange, J. S., Laurenza, M., Lautenbach, K., Laycock, P. J., Leboucher, R., Diberder, F. R. Le, Lee, I. -S., Lee, S. C., Leitl, P., Levit, D., Lewis, P. M., Li, C., Li, L. K., Li, S. X., Li, Y. B., Libby, J., Lieret, K., Lin, J., Liptak, Z., Liu, Q. Y., Liu, Z. A., Liventsev, D., Longo, S., Loos, A., Lozar, A., Lu, P., Lueck, T., Luetticke, F., Luo, T., Lyu, C., MacQueen, C., Maggiora, M., Maiti, R., Maity, S., Manfredi, R., Manoni, E., Manthei, A., Marcello, S., Marinas, C., Martel, L., Martini, A., Massaccesi, L., Masuda, M., Matsuda, T., Matsuoka, K., Matvienko, D., McKenna, J. A., McNeil, J., Meggendorfer, F., Meier, F., Merola, M., Metzner, F., Milesi, M., Miller, C., Miyabayashi, K., Miyake, H., Miyata, H., Mizuk, R., Azmi, K., Mohanty, G. B., Molina-Gonzalez, N., Moneta, S., Moon, H., Moon, T., Grimaldo, J. A. Mora, Morii, T., Moser, H. -G., Mrvar, M., Müller, F. J., Muller, Th., Muroyama, G., Murphy, C., Mussa, R., Nakamura, I., Nakamura, K. R., Nakano, E., Nakao, M., Nakayama, H., Nakazawa, H., Charan, A. Narimani, Naruki, M., Natkaniec, Z., Natochii, A., Nayak, L., Nayak, M., Nazaryan, G., Neverov, D., Niebuhr, C., Niiyama, M., Ninkovic, J., Nisar, N. K., Nishida, S., Nishimura, K., Nouxman, M. H. A., Ogawa, K., Ogawa, S., Olsen, S. L., Onishchuk, Y., Ono, H., Onuki, Y., Oskin, P., Otani, F., Oxford, E. R., Ozaki, H., Pakhlov, P., Pakhlova, G., Paladino, A., Pang, T., Panta, A., Paoloni, E., Pardi, S., Parham, K., Park, H., Park, S. -H., Paschen, B., Passeri, A., Pathak, A., Patra, S., Paul, S., Pedlar, T. K., Peruzzi, I., Peschke, R., Pestotnik, R., Pham, F., Piccolo, M., Piilonen, L. E., Angioni, G. Pinna, Podesta-Lerma, P. L. M., Podobnik, T., Pokharel, S., Polat, L., Popov, V., Praz, C., Prell, S., Prencipe, E., Prim, M. T., Purohit, M. V., Purwar, H., Rad, N., Rados, P., Raiz, S., Morales, A. Ramirez, Rasheed, R., Rauls, N., Reif, M., Reiter, S., Remnev, M., Ripp-Baudot, I., Ritter, M., Ritzert, M., Rizzo, G., Rizzuto, L. B., Robertson, S. H., Pérez, D. Rodríguez, Roney, J. M., Rosenfeld, C., Rostomyan, A., Rout, N., Rozanska, M., Russo, G., Sahoo, D., Sakai, Y., Sanders, D. A., Sandilya, S., Sangal, A., Santelj, L., Sartori, P., Sato, Y., Savinov, V., Scavino, B., Schnepf, M., Schram, M., Schreeck, H., Schueler, J., Schwanda, C., Schwartz, A. J., Schwenker, B., Schwickardi, M., Seino, Y., Selce, A., Senyo, K., Seong, I. S., Serrano, J., Sevior, M. E., Sfienti, C., Shebalin, V., Shen, C. P., Shibuya, H., Shillington, T., Shimasaki, T., Shiu, J. -G., Shwartz, B., Sibidanov, A., Simon, F., Singh, J. B., Skambraks, S., Skorupa, J., Smith, K., Sobie, R. J., Soffer, A., Sokolov, A., Soloviev, Y., Solovieva, E., Spataro, S., Spruck, B., Starič, M., Stefkova, S., Stottler, Z. S., Stroili, R., Strube, J., Stypula, J., Sue, Y., Sugiura, R., Sumihama, M., Sumisawa, K., Sumiyoshi, T., Sutcliffe, W., Suzuki, S. Y., Svidras, H., Tabata, M., Takahashi, M., Takizawa, M., Tamponi, U., Tanaka, S., Tanida, K., Tanigawa, H., Taniguchi, N., Tao, Y., Taras, P., Tenchini, F., Tiwary, R., Tonelli, D., Torassa, E., Toutounji, N., Trabelsi, K., Tsaklidis, I., Tsuboyama, T., Tsuzuki, N., Uchida, M., Ueda, I., Uehara, S., Uematsu, Y., Ueno, T., Uglov, T., Unger, K., Unno, Y., Uno, K., Uno, S., Urquijo, P., Ushiroda, Y., Usov, Y. V., Vahsen, S. E., van Tonder, R., Varner, G. S., Varvell, K. E., Vinokurova, A., Vitale, L., Vobbilisetti, V., Vorobyev, V., Vossen, A., Wach, B., Waheed, E., Wakeling, H. M., Wan, K., Abdullah, W. Wan, Wang, B., Wang, C. H., Wang, E., Wang, M. -Z., Wang, X. L., Warburton, A., Watanabe, M., Watanuki, S., Webb, J., Wehle, S., Welsch, M., Wessel, C., Wiechczynski, J., Wieduwilt, P., Windel, H., Won, E., Wu, L. J., Xu, X. P., Yabsley, B. D., Yamada, S., Yan, W., Yang, S. B., Ye, H., Yelton, J., Yin, J. H., Yonenaga, M., Yook, Y. M., Yoshihara, K., Yoshinobu, T., Yuan, C. Z., Yusa, Y., Zani, L., Zhai, Y., Zhang, J. Z., Zhang, Y., Zhang, Z., Zhilich, V., Zhou, J., Zhou, Q. D., Zhou, X. Y., Zhukova, V. I., and Zhulanov, V.

Subjects
High Energy Physics - Experiment
Abstract

We present a determination of the magnitude of the Cabibbo-Kobayashi-Maskawa (CKM) matrix element $V_{cb}$ using $B\to D\ell\nu$ decays. The result is based on $e^+e^-\to\Upsilon(4S)$ data recorded by the Belle II detector corresponding to 189.2/fb of integrated luminosity. The semileptonic decays $B^0\to D^-(\to K^+\pi^-\pi^-)\ell^+\nu_\ell$ and $B^+\to\bar D^0(\to K^+\pi^-)\ell^+\nu_\ell$ are reconstructed, where $\ell$ is either electron or a muon. The second $B$ meson in the $\Upsilon(4S)$ event is not explicitly reconstructed. Using the diamond-frame method, we determine the $B$ meson four-momentum and thus the hadronic recoil. We extract the partial decay rates as functions of $w$ and perform a fit to the decay form-factor and the CKM parameter $|V_{cb}|$ using the BGL parameterization of the form factor and lattice QCD input from the FNAL/MILC and HPQCD collaborations. We obtain $\eta_{EW}|V_{cb}|=(38.53\pm 1.15)\times 10^{-3}$, where $\eta_{EW}$ is an electroweak correction, and the error accounts for theoretical and experimental sources of uncertainty., Comment: 20 pages, 4 figures

Published
2022

341. The GRAVITY Young Stellar Object survey -- IX. Spatially resolved kinematics of hot hydrogen gas in the star/disk interaction region of T Tauri stars

Author

GRAVITY Collaboration, Wojtczak, J. A., Labadie, L., Perraut, K., Tessore, B., Soulain, A., Ganci, V., Bouvier, J., Dougados, C., Alécian, E., Nowacki, H., Cozzo, G., Brandner, W., Garatti, A. Caratti o, Garcia, P., Lopez, R. Garcia, Sanchez-Bermudez, J., Amorim, A., Benisty, M., Berger, J. -P., Bourdarot, G., Caselli, P., Clénet, Y., de Zeeuw, P. T., Davies, R., Drescher, A., Duvert, G., Eckart, A., Eisenhauer, F., Eupen, F., Föster-Schreiber, N. M., Gendron, E., Gillessen, S., Grant, S., Grellmann, R., Heißel, G., Henning, Th., Hippler, S., Horrobin, M., Hubert, Z., Jocou, L., Kervella, P., Labour, S., Lapeyrère, V., Bouquin, J. -B. Le, Léna, P., Lutz, D., Mang, F., Ott, T., Paumard, T., Perrin, G., Scheithauer, S., Shangguan, J., Shimizu, T., Spezzano, S., Straub, O., Straubmeier, C., Sturm, E., van Dishoeck, E., Vincent, F., and Widmann, F.

Subjects
Astrophysics - Solar and Stellar Astrophysics
Abstract

Aims: We aim to spatially and spectrally resolve the Br-gamma hydrogen emission line with the methods of interferometry in order to examine the kinematics of the hydrogen gas emission region in the inner accretion disk of a sample of solar-like young stellar objects. The goal is to identify trends and categories among the sources of our sample and to discuss whether or not they can be tied to different origin mechanisms associated with Br-gamma emission in T Tauri stars, chiefly and most prominently magnetospheric accretion. Methods: We observed a sample of seven T Tauri stars for the first time with VLTI GRAVITY, recording spectra and spectrally dispersed interferometric quantities across the Br-gamma line in the NIR K-band. We use them to extract the size of the Br-gamma emission region and the photocenter shifts. To assist in the interpretation, we also make use of radiative transfer models of magnetospheric accretion to establish a baseline of expected interferometric signatures if accretion is the primary driver of Br-gamma emission. Results: From among our sample, we find that five of the seven T~Tauri stars show an emission region with a half-flux radius in the range broadly expected for magnetospheric truncation. Two of the five objects also show Br-gamma emission primarily originating from within the corotation radius, while two other objects exhibit extended emission on a scale beyond 10 R$_*$, one of them even beyond the K~band continuum half-flux radius of 11.3 R$_*$. Conclusions: We find strong evidence to suggest that for the two weakest accretors in the sample, magnetospheric accretion is the primary driver of Br-gamma radiation. The results for the remaining sources imply either partial or strong contributions coming from spatially extended emission components in the form of outflows, such as stellar or disk winds., Comment: Version corresponds to the one in A&A production. The author list has been amended with "GRAVITY Collaboration" as first entry in keeping with the convention established for papers published by the GRAVITY consortium in recent years

Published
2022
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342. Searching for neutrinos from solar flares across solar cycles 23 and 24 with the Super-Kamiokande detector

Author

Okamoto, K., Abe, K., Hayato, Y., Hiraide, K., Hosokawa, K., Ieki, K., Ikeda, M., Kameda, J., Kanemura, Y., Kaneshima, Y., Kataoka, Y., Kashiwagi, Y., Miki, S., Mine, S., Miura, M., Moriyama, S., Nagao, Y., Nakahata, M., Nakano, Y., Nakayama, S., Noguchi, Y., Sato, K., Sekiya, H., Shimizu, K., Shiozawa, M., Shiba, H., Sonoda, Y., Suzuki, Y., Takeda, A., Takemoto, Y., Takenaka, A., Tanaka, H., Watanabe, S., Yano, T., Han, S., Kajita, T., Okumura, K., Tashiro, T., Tomiya, T., Wang, X., Xia, J., Yoshida, S., Megias, G. D., Fernandez, P., Labarga, L., Ospina, N., Zaldivar, B., Pointon, B. W., Kearns, E., Raaf, J. L., Wan, L., Wester, T., Bian, J., Griskevich, N. J., Kropp, W. R., Locke, S., Smy, M. B., Sobel, H. W., Takhistov, V., Yankelevich, A., Hill, J., Kim, J. Y., Lee, S. H., Lim, I. T., Moon, D. H., Park, R. G., Bodur, B., Scholberg, K., Walter, C. W., Beauchene, A., Bernard, L., Coffani, A., Drapier, O., Hedri, S. El, Giampaolo, A., Mueller, Th. A., Santos, A. D., Paganini, P., Quilain, B., Ishizuka, T., Nakamura, T., Jang, J. S., Learned, J. G., Choi, K., Cao, S., Anthony, L. H. V., Martin, D., Scott, M., Sztuc, A. A., Uchida, Y., Berardi, V., Catanesi, M. G., Radicioni, E., Calabria, N. F., Machado, L. N., De Rosa, G., Collazuol, G., Iacob, F., Lamoureux, M., Mattiazzi, M., Ludovici, L., Gonin, M., Pronost, G., Fujisawa, C., Maekawa, Y., Nishimura, Y., Friend, M., Hasegawa, T., Ishida, T., Kobayashi, T., Jakkapu, M., Matsubara, T., Nakadaira, T., Nakamura, K., Oyama, Y., Sakashita, K., Sekiguchi, T., Tsukamoto, T., Bhuiyan, N., Boschi, T., Burton, G. T., Di Lodovico, F., Gao, J., Goldsack, A., Katori, T., Migenda, J., Taani, M., Xie, Z., Zsoldos, S., Kotsar, Y., Ozaki, H., Suzuki, A. T., Takeuchi, Y., Yamamoto, S., Bronner, C., Feng, J., Kikawa, T., Mori, M., Nakaya, T., Wendell, R. A., Yasutome, K., Jenkins, S. J., McCauley, N., Mehta, P., Tarrant, A., Tsui, K. M., Fukuda, Y., Itow, Y., Menjo, H., Ninomiya, K., Lagoda, J., Lakshmi, S. M., Mandal, M., Mijakowski, P., Prabhu, Y. S., Zalipska, J., Jia, M., Jiang, J., Jung, C. K., Vilela, C., Wilking, M. J., Yanagisawa, C., Harada, M., Ishino, H., Ito, S., Kitagawa, H., Koshio, Y., Ma, W., Nakanishi, F., Piplani, N., Sakai, S., Barr, G., Barrow, D., Cook, L., Samani, S., Wark, D., Holin, A., Nova, F., Yang, J. Y., Fannon, J. E. P., Malek, M., McElwee, J. M., Stone, O., Thiesse, M. D., Thompson, L. F., Okazawa, H., Kim, S. B., Kwon, E., Seo, J. W., Yu, I., Ichikawa, A. K., Nakamura, K. D., Tairafune, S., Nishijima, K., Koshiba, M., Iwamoto, K., Nakagiri, K., Nakajima, Y., Shima, S., Taniuchi, N., Yokoyama, M., Martens, K., de Perio, P., Vagins, M. R., Kuze, M., Izumiyama, S., Inomoto, M., Ishitsuka, M., Ito, H., Kinoshita, T., Matsumoto, R., Ommura, Y., Shigeta, N., Shinoki, M., Suganuma, T., Yamauchi, K., Martin, J. F., Tanaka, H. A., Towstego, T., Akutsu, R., Gaur, R., Gousy-Leblanc, V., Hartz, M., Konaka, A., Li, X., Prouse, N. W., Chen, S., Xu, B. D., Zhang, B., Posiadala-Zezula, M., Boyd, S. B., Hadley, D., Nicholson, M., O'Flaherty, M., Richards, B., Ali, A., Jamieson, B., Walker, J., Marti, Ll., Minamino, A., Pintaudi, G., Sano, S., Sasaki, R., Suzuki, S., and Wada, K.

Subjects
Astrophysics - Solar and Stellar Astrophysics, Astrophysics - High Energy Astrophysical Phenomena, High Energy Physics - Experiment, Physics - Space Physics
Abstract

Neutrinos associated with solar flares (solar-flare neutrinos) provide information on particle acceleration mechanisms during the impulsive phase of solar flares. We searched using the Super-Kamiokande detector for neutrinos from solar flares that occurred during solar cycles $23$ and $24$, including the largest solar flare (X28.0) on November 4th, 2003. In order to minimize the background rate we searched for neutrino interactions within narrow time windows coincident with $\gamma$-rays and soft X-rays recorded by satellites. In addition, we performed the first attempt to search for solar-flare neutrinos from solar flares on the invisible side of the Sun by using the emission time of coronal mass ejections (CMEs). By selecting twenty powerful solar flares above X5.0 on the visible side and eight CMEs whose emission speed exceeds $2000$ $\mathrm{km \, s^{-1}}$ on the invisible side from 1996 to 2018, we found two (six) neutrino events coincident with solar flares occurring on the visible (invisible) side of the Sun, with a typical background rate of $0.10$ ($0.62$) events per flare in the MeV-GeV energy range. No significant solar-flare neutrino signal above the estimated background rate was observed. As a result we set the following upper limit on neutrino fluence at the Earth $\mathit{\Phi}<1.1\times10^{6}$ $\mathrm{cm^{-2}}$ at the $90\%$ confidence level for the largest solar flare. The resulting fluence limits allow us to constrain some of the theoretical models for solar-flare neutrino emission., Comment: 36 pages, 18 figures, 9 tables (Figure 12 was replaced because it was incorrect in version 1.)

Published
2022

343. First Measurement of $\Lambda$ Electroproduction off Nuclei in the Current and Target Fragmentation Regions

Author

Chetry, T., Fassi, L. El, Brooks, W. K., Dupré, R., Alaoui, A. El, Hafidi, K., Achenbach, P., Adhikari, K. P., Akbar, Z., Armstrong, W. R., Arratia, M., Atac, H., Avakian, H., Baashen, L., Baltzell, N. A., Barion, L., Bashkanov, M., Battaglieri, M., Bedlinskiy, I., Benkel, B., Benmokhtar, F., Bianconi, A., Biselli, A. S., Bondi, M., Booth, W. A., Bossù, F., Boiarinov, S., Brinkmann, K. -Th., Briscoe, W. J., Bulumulla, D., Burkert, V. D., Carman, D. S., Carvajal, J. C., Celentano, A., Chatagnon, P., Chesnokov, V., Ciullo, G., Cole, P. L., Contalbrigo, M., Costantini, G., D'Angelo, A., Dashyan, N., De Vita, R., Defurne, M., Deur, A., Diehl, S., Djalali, C., Egiyan, H., Elouadrhiri, L., Eugenio, P., Fegan, S., Filippi, A., Gavalian, G., Ghandilyan, Y., Gilfoyle, G. P., Glazier, D. I., Golubenko, A. A., Gosta, G., Gothe, R. W., Griffioen, K. A., Guidal, M., Guo, L., Hakobyan, H., Hattawy, M., Hayward, T. B., Heddle, D., Hobart, A., Holtrop, M., Ilieva, Y., Ireland, D. G., Isupov, E. L., Jenkins, D., Jo, H. S., Kabir, M. L., Khanal, A., Khandaker, M., Kim, A., Kim, W., Klein, F. J., Kripko, A., Kubarovsky, V., Lagerquist, V., Lanza, L., Leali, M., Lee, S., Lenisa, P., Li, X., Livingston, K., MacGregor, I. J. D., Marchand, D., Mascagna, V., McKinnon, B., McLauchlin, C., Meziani, Z. E., Migliorati, S., Mineeva, T., Mirazita, M., Mokeev, V., Camacho, C. Munoz, Nadel-Turonski, P., Neupane, K., Niccolai, S., Nicol, M., Niculescu, G., Osipenko, M., Ostrovidov, A. I., Pandey, P., Paolone, M., Pappalardo, L. L., Paremuzyan, R., Pasyuk, E., Paul, S. J., Phelps, W., Pilleux, N., Pokhrel, M., Poudel, J., Price, J. W., Prok, Y., Raue, B. A., Reed, T., Richards, J., Ripani, M., Ritman, J., Rosner, G., Sabatié, F., Salgado, C., Schadmand, S., Schmidt, A., Schumacher, R. A., Sharabian, Y. G., Shirokov, E. V., Shrestha, U., Simmerling, P., Sokhan, D., Sparveris, N., Stepanyan, S., Strakovsky, I. I., Strauch, S., Tan, J. A., Trotta, N., Tyson, R., Ungaro, M., Vallarino, S., Venturelli, L., Voskanyan, H., Voutier, E., Wei, X., Weinstein, L. B., Williams, R., Wishart, R., Wood, M. H., Zachariou, N., Zhao, Z. W., and Zurek, M.

Subjects
Nuclear Experiment, High Energy Physics - Experiment
Abstract

We report results of $\Lambda$ hyperon production in semi-inclusive deep-inelastic scattering off deuterium, carbon, iron, and lead targets obtained with the CLAS detector and the Continuous Electron Beam Accelerator Facility 5.014~GeV electron beam. These results represent the first measurements of the $\Lambda$ multiplicity ratio and transverse momentum broadening as a function of the energy fraction~($z$) in the current and target fragmentation regions. The multiplicity ratio exhibits a strong suppression at high~$z$~and~an enhancement at~low~$z$. The measured transverse momentum broadening is an order of magnitude greater than that seen for light mesons. This indicates that the propagating entity interacts very strongly with the nuclear medium, which suggests that propagation of diquark configurations in the nuclear medium takes place at least part of the time, even at high~$z$. The trends of these results are qualitatively described by the Giessen Boltzmann-Uehling-Uhlenbeck transport model, particularly for the multiplicity ratios. These observations will potentially open a new era of studies of the structure of the nucleon as well as of strange baryons., Comment: 14 pages, 6 figures

Published
2022
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344. Measurement of the photon-energy spectrum in inclusive $B\rightarrow X_{s}\gamma$ decays identified using hadronic decays of the recoil $B$ meson in 2019-2021 Belle II data

Author

Belle II Collaboration, Abudinén, F., Adachi, I., Adamczyk, K., Aggarwal, L., Ahlburg, P., Ahmed, H., Ahn, J. K., Aihara, H., Akopov, N., Aloisio, A., Ameli, F., Andricek, L., Ky, N. Anh, Asner, D. M., Atmacan, H., Aulchenko, V., Aushev, T., Aushev, V., Aziz, T., Babu, V., Bacher, S., Bae, H., Baehr, S., Bahinipati, S., Bakich, A. M., Bambade, P., Banerjee, Sw., Bansal, S., Barrett, M., Batignani, G., Baudot, J., Bauer, M., Baur, A., Beaubien, A., Beaulieu, A., Becker, J., Behera, P. K., Bennett, J. V., Bernieri, E., Bernlochner, F. U., Bertacchi, V., Bertemes, M., Bertholet, E., Bessner, M., Bettarini, S., Bhardwaj, V., Bhuyan, B., Bianchi, F., Bilka, T., Bilokin, S., Biswas, D., Bobrov, A., Bodrov, D., Bolz, A., Bondar, A., Bonvicini, G., Bozek, A., Bračko, M., Branchini, P., Braun, N., Briere, R. A., Browder, T. E., Brown, D. N., Budano, A., Burmistrov, L., Bussino, S., Campajola, M., Cao, L., Casarosa, G., Cecchi, C., Červenkov, D., Chang, M. -C., Chang, P., Cheaib, R., Cheema, P., Chekelian, V., Chen, C., Chen, Y. Q., Chen, Y. -T., Cheon, B. G., Chilikin, K., Chirapatpimol, K., Cho, H. -E., Cho, K., Cho, S. -J., Choi, S. -K., Choudhury, S., Cinabro, D., Corona, L., Cremaldi, L. M., Cunliffe, S., Czank, T., Das, S., Dash, N., Dattola, F., De La Cruz-Burelo, E., De La Motte, S. A., de Marino, G., De Nardo, G., De Nuccio, M., De Pietro, G., de Sangro, R., Deschamps, B., Destefanis, M., Dey, S., De Yta-Hernandez, A., Dhamija, R., Di Canto, A., Di Capua, F., Di Carlo, S., Dingfelder, J., Doležal, Z., Jiménez, I. Domínguez, Dong, T. V., Dorigo, M., Dort, K., Dossett, D., Dreyer, S., Dubey, S., Duell, S., Dujany, G., Ecker, P., Eidelman, S., Eliachevitch, M., Epifanov, D., Feichtinger, P., Ferber, T., Ferlewicz, D., Fillinger, T., Finck, C., Finocchiaro, G., Fischer, P., Flood, K., Fodor, A., Forti, F., Frey, A., Friedl, M., Fulsom, B. G., Gabriel, M., Gabrielli, A., Gabyshev, N., Ganiev, E., Garcia-Hernandez, M., Garg, R., Garmash, A., Gaur, V., Gaz, A., Gebauer, U., Gellrich, A., Gemmler, J., Geßler, T., Ghevondyan, G., Giakoustidis, G., Giordano, R., Giri, A., Glazov, A., Gobbo, B., Godang, R., Goldenzweig, P., Golob, B., Gomis, P., Gong, G., Grace, P., Gradl, W., Granderath, S., Graziani, E., Greenwald, D., Gu, T., Guan, Y., Gudkova, K., Guilliams, J., Hadjivasiliou, C., Halder, S., Hara, K., Hara, T., Hartbrich, O., Hayasaka, K., Hayashii, H., Hazra, S., Hearty, C., Hedges, M. T., de la Cruz, I. Heredia, Villanueva, M. Hernández, Hershenhorn, A., Higuchi, T., Hill, E. C., Hirata, H., Hoek, M., Hohmann, M., Hollitt, S., Hotta, T., Hsu, C. -L., Huang, K., Humair, T., Iijima, T., Inami, K., Inguglia, G., Ipsita, N., Jabbar, J. Irakkathil, Ishikawa, A., Ito, S., Itoh, R., Iwasaki, M., Iwasaki, Y., Iwata, S., Jackson, P., Jacobs, W. W., Jaffe, D. E., Jang, E. -J., Jeandron, M., Jeon, H. B., Ji, Q. P., Jia, S., Jin, Y., Joo, C., Joo, K. K., Junkerkalefeld, H., Kadenko, I., Kahn, J., Kakuno, H., Kaleta, M., Kaliyar, A. B., Kandra, J., Kang, K. H., Kang, S., Kapusta, P., Karl, R., Karyan, G., Kato, Y., Kawai, H., Kawasaki, T., Ketter, C., Kichimi, H., Kiesling, C., Kim, C. -H., Kim, D. Y., Kim, H. J., Kim, K. -H., Kim, K., Kim, S. -H., Kim, Y. -K., Kim, Y., Kimmel, T. D., Kindo, H., Kinoshita, K., Kleinwort, C., Knysh, B., Kodyš, P., Koga, T., Kohani, S., Kojima, K., Komarov, I., Konno, T., Korobov, A., Korpar, S., Kovalchuk, N., Kovalenko, E., Kowalewski, R., Kraetzschmar, T. M. G., Krinner, F., Križan, P., Kroeger, R., Krohn, J. F., Krokovny, P., Krüger, H., Kuehn, W., Kuhr, T., Kumar, J., Kumar, M., Kumar, R., Kumara, K., Kumita, T., Kunigo, T., Künzel, M., Kurz, S., Kuzmin, A., Kvasnička, P., Kwon, Y. -J., Lacaprara, S., Lai, Y. -T., La Licata, C., Lalwani, K., Lam, T., Lanceri, L., Lange, J. S., Laurenza, M., Lautenbach, K., Laycock, P. J., Leboucher, R., Diberder, F. R. Le, Lee, I. -S., Lee, S. C., Leitl, P., Levit, D., Lewis, P. M., Li, C., Li, L. K., Li, S. X., Li, Y. B., Libby, J., Lieret, K., Lin, J., Liptak, Z., Liu, Q. Y., Liu, Z. A., Liventsev, D., Longo, S., Loos, A., Lozar, A., Lu, P., Lueck, T., Luetticke, F., Luo, T., Lyu, C., MacQueen, C., Maggiora, M., Maiti, R., Maity, S., Manfredi, R., Manoni, E., Manthei, A., Marcello, S., Marinas, C., Martel, L., Martini, A., Martinov, T., Massaccesi, L., Masuda, M., Matsuda, T., Matsuoka, K., Matvienko, D., McKenna, J. A., McNeil, J., Meggendorfer, F., Meier, F., Merola, M., Metzner, F., Milesi, M., Miller, C., Miyabayashi, K., Miyake, H., Miyata, H., Mizuk, R., Azmi, K., Mohanty, G. B., Molina-Gonzalez, N., Moneta, S., Moon, H., Moon, T., Grimaldo, J. A. Mora, Morii, T., Moser, H. -G., Mrvar, M., Müller, F. J., Muller, Th., Muroyama, G., Murphy, C., Mussa, R., Nakamura, I., Nakamura, K. R., Nakano, E., Nakao, M., Nakayama, H., Nakazawa, H., Charan, A. Narimani, Naruki, M., Natkaniec, Z., Natochii, A., Nayak, L., Nayak, M., Nazaryan, G., Neverov, D., Niebuhr, C., Niiyama, M., Ninkovic, J., Nisar, N. K., Nishida, S., Nishimura, K., Nouxman, M. H. A., Ogawa, K., Ogawa, S., Olsen, S. L., Onishchuk, Y., Ono, H., Onuki, Y., Oskin, P., Otani, F., Oxford, E. R., Ozaki, H., Pakhlov, P., Pakhlova, G., Paladino, A., Pang, T., Panta, A., Paoloni, E., Pardi, S., Parham, K., Park, H., Park, S. -H., Paschen, B., Passeri, A., Pathak, A., Patra, S., Paul, S., Pedlar, T. K., Peruzzi, I., Peschke, R., Pestotnik, R., Pham, F., Piccolo, M., Piilonen, L. E., Angioni, G. Pinna, Podesta-Lerma, P. L. M., Podobnik, T., Pokharel, S., Polat, L., Popov, V., Praz, C., Prell, S., Prencipe, E., Prim, M. T., Purohit, M. V., Purwar, H., Rad, N., Rados, P., Raiz, S., Morales, A. Ramirez, Rasheed, R., Rauls, N., Reif, M., Reiter, S., Remnev, M., Ripp-Baudot, I., Ritter, M., Ritzert, M., Rizzo, G., Rizzuto, L. B., Röhrken, M., Robertson, S. H., Pérez, D. Rodríguez, Roney, J. M., Rosenfeld, C., Rostomyan, A., Rout, N., Rozanska, M., Russo, G., Sahoo, D., Sakai, Y., Sanders, D. A., Sandilya, S., Sangal, A., Santelj, L., Sartori, P., Sato, Y., Savinov, V., Scavino, B., Schnepf, M., Schram, M., Schreeck, H., Schueler, J., Schwanda, C., Schwartz, A. J., Schwenker, B., Schwickardi, M., Seino, Y., Selce, A., Senyo, K., Seong, I. S., Serrano, J., Sevior, M. E., Sfienti, C., Shebalin, V., Shen, C. P., Shibuya, H., Shillington, T., Shimasaki, T., Shiu, J. -G., Shwartz, B., Sibidanov, A., Simon, F., Singh, J. B., Skambraks, S., Skorupa, J., Smith, K., Sobie, R. J., Soffer, A., Sokolov, A., Soloviev, Y., Solovieva, E., Spataro, S., Spruck, B., Starič, M., Stefkova, S., Stottler, Z. S., Stroili, R., Strube, J., Stypula, J., Sue, Y., Sugiura, R., Sumihama, M., Sumisawa, K., Sumiyoshi, T., Sutcliffe, W., Suzuki, S. Y., Svidras, H., Tabata, M., Tackmann, K., Takahashi, M., Takizawa, M., Tamponi, U., Tanaka, S., Tanida, K., Tanigawa, H., Taniguchi, N., Tao, Y., Taras, P., Tenchini, F., Tiwary, R., Tonelli, D., Torassa, E., Toutounji, N., Trabelsi, K., Tsaklidis, I., Tsuboyama, T., Tsuzuki, N., Uchida, M., Ueda, I., Uehara, S., Uematsu, Y., Ueno, T., Uglov, T., Unger, K., Unno, Y., Uno, K., Uno, S., Urquijo, P., Ushiroda, Y., Usov, Y. V., Vahsen, S. E., van Tonder, R., Varner, G. S., Varvell, K. E., Vinokurova, A., Vitale, L., Vobbilisetti, V., Vorobyev, V., Vossen, A., Wach, B., Waheed, E., Wakeling, H. M., Wan, K., Abdullah, W. Wan, Wang, B., Wang, C. H., Wang, E., Wang, M. -Z., Wang, X. L., Warburton, A., Watanabe, M., Watanuki, S., Webb, J., Wehle, S., Welsch, M., Wessel, C., Wiechczynski, J., Wieduwilt, P., Windel, H., Won, E., Wu, L. J., Xu, X. P., Yabsley, B. D., Yamada, S., Yan, W., Yang, S. B., Ye, H., Yelton, J., Yin, J. H., Yonenaga, M., Yook, Y. M., Yoshihara, K., Yoshinobu, T., Yuan, C. Z., Yusa, Y., Zani, L., Zhai, Y., Zhang, J. Z., Zhang, Y., Zhang, Z., Zhilich, V., Zhou, J., Zhou, Q. D., Zhou, X. Y., Zhukova, V. I., Zhulanov, V., and Žlebčík, R.

Subjects
High Energy Physics - Experiment
Abstract

We measure the photon-energy spectrum in radiative bottom-meson ($B$) decays into inclusive final states involving a strange hadron and a photon. We use SuperKEKB electron-positron collisions corresponding to $189~\mathrm{fb}^{-1}$ of integrated luminosity collected at the $\Upsilon(4S)$ resonance by the Belle II experiment. The partner $B$ candidates are fully reconstructed using a large number of hadronic channels. The $B \rightarrow X_s \gamma$ partial branching fractions are measured as a function of photon energy in the signal $B$ meson rest frame in eight bins above $1.8~\mathrm{GeV}$. The background-subtracted signal yield for this photon energy region is $343 \pm 122$ events. Integrated branching fractions for three photon energy thresholds of $1.8~\mathrm{GeV}$, $2.0~\mathrm{GeV}$, and $2.1~\mathrm{GeV}$ are also reported, and found to be in agreement with world averages., Comment: 14 pages, 3 figures

Published
2022

345. On Einstein submanifolds of Euclidean space

Author

Dajczer, M., Onti, C. -R., and Vlachos, Th.

Subjects
Mathematics - Differential Geometry, 53C25, 53C40, 53C42
Abstract

Let the warped product $M^n=L^m\times_\varphi F^{n-m}$, $n\geq m+3\geq 8$, of Riemannian manifolds be an Einstein manifold with Ricci curvature $\rho$ that admits an isometric immersion into Euclidean space with codimension two. Under the assumption that $L^m$ is also Einstein, but not of constant sectional curvature, it is shown that $\rho=0$ and that the submanifold is locally a cylinder with an Euclidean factor of dimension at least $n-m$. Hence $L^m$ is also Ricci flat. If $M^n$ is complete, then the same conclusion holds globally if the assumption on $L^m$ is replaced by the much weaker condition that either its scalar curvature $S_L$ is constant or that $S_L\leq (2m-n)\rho$.

Published
2022

346. Characterization of the TruSense S310 Laser Range System for Contact-less Measurement of Liquid Levels in Large-Volume Neutrino Detectors

Author

Steiger, H. Th. J., Theisen, E., Oberauer, L., Pilarczyk, O., and Wurm, M.

Subjects
Physics - Instrumentation and Detectors
Abstract

Neutrino experiments often use large volumes of water, organic scintillators or noble liquids as active detection material. Due to the large hydrostatic and buoyancy forces involved, precise knowledge of the liquid levels inside the detector tank are mandatory. Here we present the main characteristics of the TruSense S310 Laser Range System. Level measurements can be performed without direct contact to the liquid and through a gas-proof acrylic window, thus preserving the strict radiopurity and chemical requirements of the target liquid. We report the results of a suit of laboratory experiments for short-term precision tests ($\pm$5\,mm) and long-term stability studies. Moreover, we demonstrate that the infrared laser can be used while standard bi-alkali PMTs are operational. We discuss the mechanical layout and integration of the system in the OSIRIS pre-detector that will monitor the radiopurity of the liquid scintillator for the large-volume neutrino experiment JUNO.

Published
2022
Full Text
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347. New ASKAP Radio Supernova Remnants and Candidates in the Large Magellanic Cloud

Author

Bozzetto, Luke M., Filipović, Miroslav D., Sano, H., Alsaberi, R. Z. E., Barnes, L. A., Bojičić, I. S., Brose, R., Chomiuk, L., Crawford, E. J., Dai, S., Ghavam, M., Haberl, F., Hill, T., Hopkins, A. M., Ingallinera, A., Jarrett, T., Kavanagh, P. J., Koribalski, B. S., Kothes, R., Leahy, D., Lenc, E., Leonidaki, I., Maggi, P., Maitra, C., Matthew, C., Payne, J. L., Pennock, C. M., Points, S., Reid, W., Riggi, S., Rowell, G., Sasaki, M., Safi-Harb, S., van Loon, J. Th., Tothill, N. F. H., Urošević, D., and Zangrandi, F.

Subjects
Astrophysics - High Energy Astrophysical Phenomena, Astrophysics - Astrophysics of Galaxies
Abstract

We present a new Australian Square Kilometre Array Pathfinder (ASKAP) sample of 14 radio Supernova Remnant (SNR) candidates in the Large Magellanic Cloud (LMC). This new sample is a significant increase to the known number of older, larger and low surface brightness LMC SNRs. We employ a multi-frequency search for each object and found possible traces of optical and occasionally X-ray emission in several of these 14 SNR candidates. One of these 14 SNR candidates (MCSNR J0522-6543) has multi-frequency properties that strongly indicate a bona fide SNR. We also investigate a sample of 20 previously suggested LMC SNR candidates and confirm the SNR nature of MCSNR J0506-6815. We detect lower surface brightness SNR candidates which were likely formed by a combination of shock waves and strong stellar winds from massive progenitors (and possibly surrounding OB stars). Some of our new SNR candidates are also found in a lower density environments in which SNe type Ia explode inside a previously excavated interstellar medium (ISM)., Comment: accepted for publication in MNRAS, this version corrects arXiv metadata only

Published
2022
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348. Determination of $|V_{ub}|$ from untagged $B^0\to\pi^- \ell^+ \nu_{\ell}$ decays using 2019-2021 Belle II data

Author

Belle II Collaboration, Adamczyk, K., Aggarwal, L., Ahlburg, P., Ahmed, H., Ahn, J. K., Aihara, H., Akopov, N., Aloisio, A., Ameli, F., Andricek, L., Ky, N. Anh, Asner, D. M., Atmacan, H., Aulchenko, V., Aushev, T., Aushev, V., Aziz, T., Babu, V., Bacher, S., Bae, H., Baehr, S., Bahinipati, S., Bakich, A. M., Bambade, P., Banerjee, Sw., Bansal, S., Barrett, M., Batignani, G., Baudot, J., Bauer, M., Baur, A., Beaubien, A., Beaulieu, A., Becker, J., Behera, P. K., Bennett, J. V., Bernieri, E., Bernlochner, F. U., Bertacchi, V., Bertemes, M., Bertholet, E., Bessner, M., Bettarini, S., Bhardwaj, V., Bhuyan, B., Bianchi, F., Bilka, T., Bilokin, S., Biswas, D., Bobrov, A., Bodrov, D., Bolz, A., Bondar, A., Bonvicini, G., Bozek, A., Bračko, M., Branchini, P., Braun, N., Briere, R. A., Browder, T. E., Brown, D. N., Budano, A., Burmistrov, L., Bussino, S., Campajola, M., Cao, L., Casarosa, G., Cecchi, C., Červenkov, D., Chang, M. -C., Chang, P., Cheaib, R., Cheema, P., Chekelian, V., Chen, C., Chen, Y. Q., Chen, Y. -T., Cheon, B. G., Chilikin, K., Chirapatpimol, K., Cho, H. -E., Cho, K., Cho, S. -J., Choi, S. -K., Choudhury, S., Cinabro, D., Corona, L., Cremaldi, L. M., Cunliffe, S., Czank, T., Das, S., Dash, N., Dattola, F., De La Cruz-Burelo, E., De La Motte, S. A., de Marino, G., De Nardo, G., De Nuccio, M., De Pietro, G., de Sangro, R., Deschamps, B., Destefanis, M., Dey, S., De Yta-Hernandez, A., Dhamija, R., Di Canto, A., Di Capua, F., Di Carlo, S., Dingfelder, J., Doležal, Z., Jiménez, I. Domínguez, Dong, T. V., Dorigo, M., Dort, K., Dossett, D., Dreyer, S., Dubey, S., Duell, S., Dujany, G., Ecker, P., Eidelman, S., Eliachevitch, M., Epifanov, D., Feichtinger, P., Ferber, T., Ferlewicz, D., Fillinger, T., Finck, C., Finocchiaro, G., Fischer, P., Flood, K., Fodor, A., Forti, F., Frey, A., Friedl, M., Fulsom, B. G., Gabriel, M., Gabrielli, A., Gabyshev, N., Ganiev, E., Garcia-Hernandez, M., Garg, R., Garmash, A., Gaur, V., Gaz, A., Gebauer, U., Gellrich, A., Gemmler, J., Geßler, T., Ghevondyan, G., Giakoustidis, G., Giordano, R., Giri, A., Glazov, A., Gobbo, B., Godang, R., Goldenzweig, P., Golob, B., Gomis, P., Gong, G., Grace, P., Gradl, W., Granderath, S., Graziani, E., Greenwald, D., Gu, T., Guan, Y., Gudkova, K., Guilliams, J., Hadjivasiliou, C., Halder, S., Hara, K., Hara, T., Hartbrich, O., Hayasaka, K., Hayashii, H., Hazra, S., Hearty, C., Hedges, M. T., de la Cruz, I. Heredia, Villanueva, M. Hernández, Hershenhorn, A., Higuchi, T., Hill, E. C., Hirata, H., Hoek, M., Hohmann, M., Hollitt, S., Hotta, T., Hsu, C. -L., Huang, K., Humair, T., Iijima, T., Inami, K., Inguglia, G., Ipsita, N., Jabbar, J. Irakkathil, Ishikawa, A., Ito, S., Itoh, R., Iwasaki, M., Iwasaki, Y., Iwata, S., Jackson, P., Jacobs, W. W., Jaffe, D. E., Jang, E. -J., Jeandron, M., Jeon, H. B., Ji, Q. P., Jia, S., Jin, Y., Joo, C., Joo, K. K., Junkerkalefeld, H., Kadenko, I., Kahn, J., Kakuno, H., Kaleta, M., Kaliyar, A. B., Kandra, J., Kang, K. H., Kang, S., Kapusta, P., Karl, R., Karyan, G., Kato, Y., Kawai, H., Kawasaki, T., Ketter, C., Kichimi, H., Kiesling, C., Kim, C. -H., Kim, D. Y., Kim, H. J., Kim, K. -H., Kim, K., Kim, S. -H., Kim, Y. -K., Kim, Y., Kimmel, T. D., Kindo, H., Kinoshita, K., Kleinwort, C., Knysh, B., Kodyš, P., Koga, T., Kohani, S., Kojima, K., Komarov, I., Konno, T., Korobov, A., Korpar, S., Kovalchuk, N., Kovalenko, E., Kowalewski, R., Kraetzschmar, T. M. G., Krinner, F., Križan, P., Kroeger, R., Krohn, J. F., Krokovny, P., Krüger, H., Kuehn, W., Kuhr, T., Kumar, J., Kumar, M., Kumar, R., Kumara, K., Kumita, T., Kunigo, T., Künzel, M., Kurz, S., Kuzmin, A., Kvasnička, P., Kwon, Y. -J., Lacaprara, S., Lai, Y. -T., La Licata, C., Lalwani, K., Lam, T., Lanceri, L., Lange, J. S., Laurenza, M., Lautenbach, K., Laycock, P. J., Leboucher, R., Diberder, F. R. Le, Lee, I. -S., Lee, S. C., Leitl, P., Levit, D., Lewis, P. M., Li, C., Li, L. K., Li, S. X., Li, Y. B., Libby, J., Lieret, K., Lin, J., Liptak, Z., Liu, Q. Y., Liu, Z. A., Liventsev, D., Longo, S., Loos, A., Lozar, A., Lu, P., Lueck, T., Luetticke, F., Luo, T., Lyu, C., MacQueen, C., Maggiora, M., Maiti, R., Maity, S., Manfredi, R., Manoni, E., Manthei, A., Marcello, S., Marinas, C., Martel, L., Martini, A., Massaccesi, L., Masuda, M., Matsuda, T., Matsuoka, K., Matvienko, D., McKenna, J. A., McNeil, J., Meggendorfer, F., Meier, F., Merola, M., Metzner, F., Milesi, M., Miller, C., Miyabayashi, K., Miyake, H., Miyata, H., Mizuk, R., Azmi, K., Mohanty, G. B., Molina-Gonzalez, N., Moneta, S., Moon, H., Moon, T., Grimaldo, J. A. Mora, Morii, T., Moser, H. -G., Mrvar, M., Müller, F. J., Muller, Th., Muroyama, G., Murphy, C., Mussa, R., Nakamura, I., Nakamura, K. R., Nakano, E., Nakao, M., Nakayama, H., Nakazawa, H., Charan, A. Narimani, Naruki, M., Natkaniec, Z., Natochii, A., Nayak, L., Nayak, M., Nazaryan, G., Neverov, D., Niebuhr, C., Niiyama, M., Ninkovic, J., Nisar, N. K., Nishida, S., Nishimura, K., Nouxman, M. H. A., Ogawa, K., Ogawa, S., Olsen, S. L., Onishchuk, Y., Ono, H., Onuki, Y., Oskin, P., Otani, F., Oxford, E. R., Ozaki, H., Pakhlov, P., Pakhlova, G., Paladino, A., Pang, T., Panta, A., Paoloni, E., Pardi, S., Parham, K., Park, H., Park, S. -H., Paschen, B., Passeri, A., Pathak, A., Patra, S., Paul, S., Pedlar, T. K., Peruzzi, I., Peschke, R., Pestotnik, R., Pham, F., Piccolo, M., Piilonen, L. E., Angioni, G. Pinna, Podesta-Lerma, P. L. M., Podobnik, T., Pokharel, S., Polat, L., Popov, V., Praz, C., Prell, S., Prencipe, E., Prim, M. T., Purohit, M. V., Purwar, H., Rad, N., Rados, P., Raiz, S., Morales, A. Ramirez, Rasheed, R., Rauls, N., Reif, M., Reiter, S., Remnev, M., Ripp-Baudot, I., Ritter, M., Ritzert, M., Rizzo, G., Rizzuto, L. B., Robertson, S. H., Pérez, D. Rodríguez, Roney, J. M., Rosenfeld, C., Rostomyan, A., Rout, N., Rozanska, M., Russo, G., Sahoo, D., Sakai, Y., Sanders, D. A., Sandilya, S., Sangal, A., Santelj, L., Sartori, P., Sato, Y., Savinov, V., Scavino, B., Schnepf, M., Schram, M., Schreeck, H., Schueler, J., Schwanda, C., Schwartz, A. J., Schwenker, B., Schwickardi, M., Seino, Y., Selce, A., Senyo, K., Seong, I. S., Serrano, J., Sevior, M. E., Sfienti, C., Shebalin, V., Shen, C. P., Shibuya, H., Shillington, T., Shimasaki, T., Shiu, J. -G., Shwartz, B., Sibidanov, A., Simon, F., Singh, J. B., Skambraks, S., Skorupa, J., Smith, K., Sobie, R. J., Soffer, A., Sokolov, A., Soloviev, Y., Solovieva, E., Spataro, S., Spruck, B., Starič, M., Stefkova, S., Stottler, Z. S., Stroili, R., Strube, J., Stypula, J., Sue, Y., Sugiura, R., Sumihama, M., Sumisawa, K., Sumiyoshi, T., Sutcliffe, W., Suzuki, S. Y., Svidras, H., Tabata, M., Takahashi, M., Takizawa, M., Tamponi, U., Tanaka, S., Tanida, K., Tanigawa, H., Taniguchi, N., Tao, Y., Taras, P., Tenchini, F., Tiwary, R., Tonelli, D., Torassa, E., Toutounji, N., Trabelsi, K., Tsaklidis, I., Tsuboyama, T., Tsuzuki, N., Uchida, M., Ueda, I., Uehara, S., Uematsu, Y., Ueno, T., Uglov, T., Unger, K., Unno, Y., Uno, K., Uno, S., Urquijo, P., Ushiroda, Y., Usov, Y. V., Vahsen, S. E., van Tonder, R., Varner, G. S., Varvell, K. E., Vinokurova, A., Vitale, L., Vobbilisetti, V., Vorobyev, V., Vossen, A., Wach, B., Waheed, E., Wakeling, H. M., Wan, K., Abdullah, W. Wan, Wang, B., Wang, C. H., Wang, E., Wang, M. -Z., Wang, X. L., Warburton, A., Watanabe, M., Watanuki, S., Webb, J., Wehle, S., Welsch, M., Wessel, C., Wiechczynski, J., Wieduwilt, P., Windel, H., Won, E., Wu, L. J., Xu, X. P., Yabsley, B. D., Yamada, S., Yan, W., Yang, S. B., Ye, H., Yelton, J., Yin, J. H., Yonenaga, M., Yook, Y. M., Yoshihara, K., Yoshinobu, T., Yuan, C. Z., Yusa, Y., Zani, L., Zhai, Y., Zhang, J. Z., Zhang, Y., Zhang, Z., Zhilich, V., Zhou, J., Zhou, Q. D., Zhou, X. Y., Zhukova, V. I., Zhulanov, V., and Žlebčík, R.

Subjects
High Energy Physics - Experiment
Abstract

We present an analysis of the charmless semileptonic decay $B^0\to\pi^- \ell^+ \nu_{\ell}$, where $\ell = e, \mu$, from 198.0 million pairs of $B\bar{B}$ mesons recorded by the Belle II detector at the SuperKEKB electron-positron collider. The decay is reconstructed without identifying the partner $B$ meson. The partial branching fractions are measured independently for $B^0\to\pi^- e^+ \nu_{e}$ and $B^0\to\pi^- \mu^+ \nu_{\mu}$ as functions of $q^{2}$ (momentum transfer squared), using 3896 $B^0\to\pi^- e^+ \nu_{e}$ and 5466 $B^0\to\pi^- \mu^+ \nu_{\mu}$ decays. The total branching fraction is found to be $(1.426 \pm 0.056 \pm 0.125) \times 10^{-4}$ for $B^0\to\pi^- \ell^+ \nu_{\ell}$ decays, where the uncertainties are statistical and systematic, respectively. By fitting the measured partial branching fractions as functions of $q^{2}$, together with constraints on the nonperturbative hadronic contribution from lattice QCD calculations, the magnitude of the Cabibbo-Kobayashi-Maskawa matrix element $V_{ub}$, $(3.55 \pm 0.12 \pm 0.13 \pm 0.17) \times 10^{-3}$, is extracted. Here, the first uncertainty is statistical, the second is systematic and the third is theoretical.

Published
2022

349. Dynamical masses of the primary Be star and the secondary sdB star in the single-lined binary kappa Dra (B6 IIIe)

Author

Klement, R., Baade, D., Rivinius, Th., Gies, D. R., Wang, L., Labadie-Bartz, J., Santos, P. Ticiani Dos, Monnier, J. D., Carciofi, A. C., Mérand, A., Anugu, N., Schaefer, G. H., Bouquin, J. -B. Le, Davies, C. L., Ennis, J., Gardner, T., Kraus, S., Setterholm, B. R., and Labdon, A.

Subjects
Astrophysics - Solar and Stellar Astrophysics
Abstract

Because many classical Be stars may owe their nature to mass and angular-momentum transfer in a close binary, the present masses, temperatures, and radii of their components are of high interest for comparison to stellar evolution models. Kappa Dra is a 61.5-day single-lined binary with a B6 IIIe primary. With the CHARA Array instruments MIRC/MIRC-X and MYSTIC, we detected the secondary at (approximately photospheric) flux ratios of 1.49 +- 0.10% and 1.63 +- 0.09% in the H and K band, respectively. From a large and diverse optical spectroscopic database only the radial velocity curve of the Be star could be extracted. However, employing the parallaxes from Hipparcos and Gaia, which agree within their nominal 1-sigma errors, we could derive the total mass and found component masses of 3.65 +- 0.48 Msun and 0.426 +- 0.043 Msun for the Be star and the companion, respectively. Previous cross-correlation of the observed far-UV spectrum with sdO spectral model templates had not detected a companion belonging to the hot O-type subdwarf (sdO) population known from ~20 earlier-type Be stars. Guided by our full 3D orbital solution, we found a strong cross-correlation signal for a stripped subdwarf B-type companion (far-UV flux ratio of 2.3 +- 0.5%), enabling the first firm characterization of such a star, and making kappa Dra the first mid- to late-type Be star with a directly-observed subdwarf companion., Comment: Accepted to ApJ. Figure sets available on request

Published
2022
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350. Search for Cosmic-ray Boosted Sub-GeV Dark Matter using Recoil Protons at Super-Kamiokande

Author

Collaboration, The Super-Kamiokande, Abe, K., Hayato, Y., Hiraide, K., Ieki, K., Ikeda, M., Kameda, J., Kanemura, Y., Kaneshima, R., Kashiwagi, Y., Kataoka, Y., Miki, S., Mine, S., Miura, M., Moriyama, S., Nakano, Y., Nakahata, M., Nakayama, S., Noguchi, Y., Okamoto, K., Sato, K., Sekiya, H., Shiba, H., Shimizu, K., Shiozawa, M., Sonoda, Y., Suzuki, Y., Takeda, A., Takemoto, Y., Takenaka, A., Tanaka, H., Watanabe, S., Yano, T., Han, S., Kajita, T., Okumura, K., Tashiro, T., Tomiya, T., Wang, X., Xia, J., Yoshida, S., Megias, G. D., Fernandez, P., Labarga, L., Ospina, N., Zaldivar, B., Pointon, B. W., Kearns, E., Raaf, J. L., Wan, L., Wester, T., Bian, J., Griskevich, N. J., Kropp, W. R., Locke, S., Smy, M. B., Sobel, H. W., Takhistov, V., Yankelevich, A., Hill, J., Park, R. G., Bodur, B., Scholberg, K., Walter, C. W., Bernard, L., Coffani, A., Drapier, O., Hedri, S. El, Giampaolo, A., Mueller, Th. A., Santos, A. D., Paganini, P., Quilain, B., Ishizuka, T., Nakamura, T., Jang, J. S., Learned, J. G., Choi, K., Cao, S., Anthony, L. H. V., Martin, D., Scott, M., Sztuc, A. A., Uchida, Y., Berardi, V., Catanesi, M. G., Radicioni, E., Calabria, N. F., Machado, L. N., De Rosa, G., Collazuol, G., Iacob, F., Lamoureux, M., Mattiazzi, M., Ludovici, L., Gonin, M., Pronost, G., Fujisawa, C., Maekawa, Y., Nishimura, Y., Friend, M., Hasegawa, T., Ishida, T., Kobayashi, T., Jakkapu, M., Matsubara, T., Nakadaira, T., Nakamura, K., Oyama, Y., Sakashita, K., Sekiguchi, T., Tsukamoto, T., Boschi, T., Di Lodovico, F., Gao, J., Goldsack, A., Katori, T., Migenda, J., Taani, M., Zsoldos, S., Kotsar, Y., Ozaki, H., Suzuki, A. T., Takeuchi, Y., Bronner, C., Feng, J., Kikawa, T., Mori, M., Nakaya, T., Wendell, R. A., Yasutome, K., Jenkins, S. J., McCauley, N., Mehta, P., Tsui, K. M., Fukuda, Y., Itow, Y., Menjo, H., Ninomiya, K., Lagoda, J., Lakshmi, S. M., Mandal, M., Mijakowski, P., Prabhu, Y. S., Zalipska, J., Jia, M., Jiang, J., Jung, C. K., Wilking, M. J., Yanagisawa, C., Harada, M., Ishino, H., Ito, S., Kitagawa, H., Koshio, Y., Nakanishi, F., Sakai, S., Barr, G., Barrow, D., Cook, L., Samani, S., Wark, D., Nova, F., Yang, J. Y., Malek, M., McElwee, J. M., Stone, O., Thiesse, M. D., Thompson, L. F., Okazawa, H., Kim, S. B., Seo, J. W., Yu, I., Ichikawa, A. K., Nakamura, K. D., Tairafune, S., Nishijima, K., Iwamoto, K., Nakagiri, K., Nakajima, Y., Taniuchi, N., Yokoyama, M., Martens, K., de Perio, P., Vagins, M. R., Kuze, M., Izumiyama, S., Inomoto, M., Ishitsuka, M., Ito, H., Kinoshita, T., Matsumoto, R., Ommura, Y., Shigeta, N., Shinoki, M., Suganuma, T., Yamauchi, K., Martin, J. F., Tanaka, H. A., Towstego, T., Akutsu, R., Gousy-Leblanc, V., Hartz, M., Konaka, A., Prouse, N. W., Chen, S., Xu, B. D., Zhang, B., Posiadala-Zezula, M., Hadley, D., Nicholson, M., O'Flaherty, M., Richards, B., Ali, A., Jamieson, B., Marti, Ll., Minamino, A., Pintaudi, G., Sano, S., Suzuki, S., and Wada, K.

Subjects
High Energy Physics - Experiment
Abstract

We report a search for cosmic-ray boosted dark matter with protons using the 0.37 megaton$\times$years data collected at Super-Kamiokande experiment during the 1996-2018 period (SKI-IV phase). We searched for an excess of proton recoils above the atmospheric neutrino background from the vicinity of the Galactic Center. No such excess is observed, and limits are calculated for two reference models of dark matter with either a constant interaction cross-section or through a scalar mediator. This is the first experimental search for boosted dark matter with hadrons using directional information. The results present the most stringent limits on cosmic-ray boosted dark matter and exclude the dark matter-nucleon elastic scattering cross-section between $10^{-33}\text{ cm}^{2}$ and $10^{-27}\text{ cm}^{2}$ for dark matter mass from 10 MeV/$c^2$ to 1 GeV/$c^2$., Comment: With 1-page appendix. A bug was found in July 2023. This version is updated to match the erratum

Published
2022
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