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Monday 8 June

High Energy Physics (Experiment)

Measurement of the ratio of branching fractions $\mathcal{B}(B_c^+ \to J/\psi \tau^+ \nu_{\tau})/\mathcal{B}(B_c^+ \to J/\psi \mu^+ \nu_{\mu})$

LHCb collaboration: R. Aaij, M. Abdelfatah, A.S.W. Abdelmotteleb et al. (+1143 more)

A measurement of the ratio of semileptonic branching fractions $\mathcal{R}(J\psi )$, defined as $\mathcal{R}(J/\psi ) \equiv \mathcal{B}(B_c^+ \to J/\psi \tau^+ \nu_{\tau})/\mathcal{B}(B_c^+ \to J/\psi \mu^+ \nu_{\mu})$, is reported using a sample of proton-proton collision data corresponding to an integrated luminosity of 5.4 fb$^{-1}$ recorded by the LHCb experiment in 2016–2018 at a center-of-mass energy of 13 TeV. The measured value is found to be $\mathcal{R}(J/\psi) = 0.51 \pm 0.12\text{(stat)} \pm 0.08\text{(syst)}$, which is within 1.8 standard deviations of the predictions from the Standard Model assuming lepton flavor universality.
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All authors LHCb collaboration: R. Aaij, M. Abdelfatah, A.S.W. Abdelmotteleb, C. Abellan Beteta, F. Abudinén, T. Ackernley, A.A. Adefisoye, B. Adeva, M. Adinolfi, P. Adlarson, C. Agapopoulou, C.A. Aidala, S. Akar, K. Akiba, H. Al Saleh, P. Albicocco, J. Albrecht, R. Aleksiejunas, F. Alessio, P. Alvarez Cartelle, S. Amato, J.L. Amey, Y. Amhis, L. An, L. Anderlini, M. Andersson, P. Andreola, M. Andreotti, S. Andres Estrada, A. Anelli, D. Ao, C. Arata, F. Archilli, Z. Areg, M. Argenton, S. Arguedas Cuendis, L. Arnone, M. Artuso, E. Aslanides, R. Ataíde Da Silva, M. Atzeni, B. Audurier, J.A. Authier, D. Bacher, I. Bachiller Perea, S. Bachmann, M. Bachmayer, J.J. Back, Z.B. Bai, V. Balagura, A. Balboni, W. Baldini, Z. Baldwin, L. Balzani, H. Bao, J. Baptista de Souza Leite, C. Barbero Pretel, M. Barbetti, I.R. Barbosa, R.J. Barlow, M. Barnyakov, S. Baron, S. Barsuk, W. Barter, J. Bartz, S. Bashir, B. Batsukh, P.B. Battista, A. Bavarchee, A. Bay, A. Beck, M. Becker, F. Bedeschi, I.B. Bediaga, N.A. Behling, S. Belin, A. Bellavista, I. Belyaev, G. Bencivenni, E. Ben-Haim, J.L.M. Berkey, R. Bernet, A. Bertolin, F. Betti, J. Bex, O. Bezshyyko, S. Bhattacharya, M.S. Bieker, N.V. Biesuz, A. Biolchini, M. Birch, F.C.R. Bishop, A. Bitadze, A. Bizzeti, T. Blake, F. Blanc, J.E. Blank, S. Blusk, J.A. Boelhauve, O. Boente Garcia, T. Boettcher, A. Bohare, C. Bolognani, R.B. Bonacci, A. Bordelius, F. Borgato, S. Borghi, M. Borsato, J.T. Borsuk, E. Bottalico, S.A. Bouchiba, M. Bovill, T.J.V. Bowcock, A. Boyer, C. Bozzi, J.D. Brandenburg, A. Brea Rodriguez, N. Breer, C. Breitfeld, J. Brodzicka, J. Brown, E. Buchanan, M. Burgos Marcos, C. Burr, C. Buti, J.S. Butter, J. Buytaert, W. Byczynski, S. Cadeddu, H. Cai, Y. Cai, A. Caillet, R. Calabrese, L. Calefice, M. Calvi, M. Calvo Gomez, P. Camargo Magalhaes, J.I. Cambon Bouzas, P. Campana, D.H. Campora Perez, A.C. Campos, A.F. Campoverde Quezada, Y. Cao, S. Capelli, M. Caporale, L. Capriotti, R. Caravaca-Mora, A. Carbone, L. Carcedo Salgado, R. Cardinale, A. Cardini, P. Carniti, L. Carus, A. Casais Vidal, R. Caspary, G. Casse, M. Cattaneo, G. Cavallero, V. Cavallini, S. Celani, I. Celestino, S. Cesare, A.J. Chadwick, I. Chahrour, M. Charles, Ph. Charpentier, E. Chatzianagnostou, R. Cheaib, M. Chefdeville, C. Chen, J. Chen, S. Chen, Z. Chen, A. Chen Hu, M. Cherif, S. Chernyshenko, X. Chiotopoulos, G. Chizhik, V. Chobanova, A. Christakakis, M. Chrzaszcz, V. Chulikov, P. Ciambrone, X. Cid Vidal, P. Cifra, P.E.L. Clarke, M. Clemencic, H.V. Cliff, J. Closier, C. Cocha Toapaxi, V. Coco, J. Cogan, E. Cogneras, L. Cojocariu, S. Collaviti, P. Collins, T. Colombo, M. Colonna, A. Comerma-Montells, L. Congedo, J. Connaughton, A. Contu, N. Cooke, G. Cordova, C. Coronel, I. Corredoira, A. Correia, G. Corti, G.C. Costantino, J. Cottee Meldrum, B. Couturier, D.C. Craik, N. Crepet, M. Cruz Torres, M. Cubero Campos, E. Curras Rivera, R. Currie, C.L. Da Silva, X. Dai, J. Dalseno, C. D'Ambrosio, G. Darze, A. Davidson, J.E. Davies, O. De Aguiar Francisco, C. De Angelis, F. De Benedetti, J. de Boer, K. De Bruyn, S. De Capua, M. De Cian, U. De Freitas Carneiro Da Graca, E. De Lucia, J.M. De Miranda, L. De Paula, M. De Serio, P. De Simone, F. De Vellis, J.A. de Vries, F. Debernardis, D. Decamp, S. Dekkers, L. Del Buono, B. Delaney, J. Deng, V. Denysenko, O. Deschamps, F. Dettori, B. Dey, P. Di Nezza, S. Ding, Y. Ding, L. Dittmann, A.D. Docheva, A. Doheny, C. Dong, F. Dordei, A.C. dos Reis, J. Dos Santos Oliveira, A.D. Dowling, L. Dreyfus, W. Duan, P. Duda, L. Dufour, V. Duk, P. Durante, M.M. Duras, J.M. Durham, O.D. Durmus, K. Duwe, A. Dziurda, S. Easo, E. Eckstein, U. Egede, S. Eisenhardt, E. Ejopu, L. Eklund, M. Elashri, D. Elizondo Blanco, J. Ellbracht, S. Ely, A. Ene, T. Evans, F. Fabiano, S. Faghih, L.N. Falcao, B. Fang, R. Fantechi, L. Fantini, M. Faria, K. Farmer, F. Fassin, D. Fazzini, L. Felkowski, C. Feng, M. Feng, A. Fernandez Casani, M. Fernandez Gomez, A.D. Fernez, F. Ferrari, F. Ferreira Rodrigues, M. Ferro-Luzzi, R.A. Fini, M. Fiorini, M. Firlej, D.S. Fitzgerald, C. Fitzpatrick, T. Fiutowski, F. Fleuret, A. Fomin, M. Fontana, M. Fontes Vaz, L.A. Foreman, R. Forty, D. Foulds-Holt, V. Franco Lima, M. Franco Sevilla, M. Frank, E. Franzoso, G. Frau, C. Frei, D.A. Friday, J. Fu, Y. Fu, Q. Führing, T. Fulghesu, G. Galati, M.D. Galati, A. Gallas Torreira, D. Galli, S. Gambetta, M. Gandelman, P. Gandini, B. Ganie, H. Gao, R. Gao, T.Q. Gao, Y. Gao, Y. Gao, Y. Gao, L.M. Garcia Martin, P. Garcia Moreno, J. García Pardiñas, P. Gardner, L. Garrido, C. Gaspar, A. Gavrikov, E. Gersabeck, M. Gersabeck, T. Gershon, S. Ghizzo, Z. Ghorbanimoghaddam, F.I. Giasemis, V. Gibson, H.K. Giemza, A.L. Gilman, M. Giovannetti, A. Gioventù, L. Girardey, M.A. Giza, F.C. Glaser, V.V. Gligorov, C. Göbel, L. Golinka-Bezshyyko, E. Golobardes, A. Golutvin, S. Gomez Fernandez, W. Gomulka, F. Goncalves Abrantes, I. Gonçales Vaz, M. Goncerz, G. Gong, J.A. Gooding, C. Gotti, E. Govorkova, J.P. Grabowski, L.A. Granado Cardoso, R. Grande Quartieri, E. Graugés, E. Graverini, L. Grazette, G. Graziani, A.T. Grecu, N.A. Grieser, L. Grillo, C. Gu, M. Guarise, L. Guerry, A.-K. Guseinov, Y. Guz, T. Gys, K. Habermann, T. Hadavizadeh, C. Hadjivasiliou, G. Haefeli, C. Haen, S. Haken, G. Hallett, P.M. Hamilton, Q. Han, S. Han, X. Han, S. Hansmann-Menzemer, N. Harnew, T.J. Harris, L. Hartman, M. Hartmann, S. Hashmi, J. He, N. Heatley, A. Hedes, F. Hemmer, C. Henderson, R. Henderson, R.D.L. Henderson, A.M. Hennequin, K. Hennessy, J. Herd, P. Herrero Gascon, J. Heuel, A. Heyn, A. Hicheur, G. Hijano Mendizabal, J. Horswill, R. Hou, Y. Hou, D.C. Houston, N. Howarth, W. Hu, X. Hu, W. Huang, W. Hulsbergen, R.J. Hunter, D. Hutchcroft, M. Idzik, P. Ilten, A. Iohner, H. Jage, S.J. Jaimes Elles, S. Jakobsen, T. Jakoubek, E. Jans, A. Jawahery, C. Jayaweera, A. Jelavic, V. Jevtic, Z. Jia, E. Jiang, X. Jiang, Y. Jiang, Y.J. Jiang, E. Jimenez Moya, N. Jindal, M. John, A. John Rubesh Rajan, D. Johnson, C.R. Jones, S. Joshi, B. Jost, J. Juan Castella, N. Jurik, I. Juszczak, K. Kalecinska, D. Kaminaris, S. Kandybei, M. Kane, Y. Kang, C. Kar, M. Karacson, A. Kauniskangas, J.W. Kautz, M.K. Kazanecki, F. Keizer, M. Kenzie, T. Ketel, B. Khanji, S. Kholodenko, G. Khreich, F. Kiraz, T. Kirn, V.S. Kirsebom, N. Kleijne, A. Kleimenova, D.K. Klekots, K. Klimaszewski, M.R. Kmiec, T. Knospe, R. Kolb, S. Koliiev, L. Kolk, A. Konoplyannikov, P. Kopciewicz, P. Koppenburg, A. Korchin, I. Kostiuk, O. Kot, S. Kotriakhova, E. Kowalczyk, O. Kravcov, M. Kreps, W. Krupa, W. Krzemien, O. Kshyvanskyi, S. Kubis, M. Kucharczyk, A. Kupsc, V. Kushnir, B. Kutsenko, J. Kvapil, I. Kyryllin, D. Lacarrere, P. Laguarta Gonzalez, A. Lai, A. Lampis, D. Lancierini, C. Landesa Gomez, J.J. Lane, G. Lanfranchi, C. Langenbruch, T. Latham, F. Lazzari, C. Lazzeroni, R. Le Gac, H. Lee, R. Lefèvre, M. Lehuraux, E. Lemos Cid, O. Leroy, T. Lesiak, E.D. Lesser, B. Leverington, A. Li, C. Li, C. Li, H. Li, J. Li, K. Li, L. Li, P. Li, P.-R. Li, Q. Li, T. Li, T. Li, W. Li, Y. Li, Y. Li, Y. Li, Z. Li, Z. Lian, Q. Liang, X. Liang, Z. Liang, S. Libralon, A. Lightbody, T. Lin, R. Lindner, H. Linton, R. Litvinov, D. Liu, F.L. Liu, G. Liu, K. Liu, S. Liu, W. Liu, Y. Liu, Y. Liu, Y.L. Liu, G. Loachamin Ordonez, I. Lobo, A. Lobo Salvia, A. Loi, T. Long, F.C.L. Lopes, J.H. Lopes, A. Lopez Huertas, C. Lopez Iribarnegaray, Q. Lu, C. Lucarelli, D. Lucchesi, M. Lucio Martinez, Y. Luo, A. Lupato, M. Lupberger, E. Luppi, K. Lynch, S. Lyu, X.-R. Lyu, H. Ma, S. Maccolini, F. Machefert, F. Maciuc, B. Mack, I. Mackay, L.M. Mackey, L.R. Madhan Mohan, M.J. Madurai, D. Magdalinski, J.J. Malczewski, S. Malde, L. Malentacca, G. Manca, G. Mancinelli, C. Mancuso, R. Manera Escalero, A. Mangalasseri, F.M. Manganella, D. Manuzzi, S. Mao, D. Marangotto, J.F. Marchand, R. Marchevski, U. Marconi, E. Mariani, S. Mariani, C. Marin Benito, J. Marks, A.M. Marshall, L. Martel, G. Martelli, G. Martellotti, L. Martinazzoli, M. Martinelli, C. Martinez, D. Martinez Gomez, D. Martinez Santos, F. Martinez Vidal, A. Martorell i Granollers, A. Massafferri, R. Matev, A. Mathad, C. Matteuzzi, K.R. Mattioli, A. Mauri, E. Maurice, J. Mauricio, P. Mayencourt, J. Mazorra de Cos, M. Mazurek, D. Mazzanti Tarancon, M. McCann, N.T. McHugh, A. McNab, R. McNulty, B. Meadows, S.E.R. Medaer, D. Melnychuk, D. Mendoza Granada, P. Menendez Valdes Perez, F.M. Meng, M. Merk, A. Merli, L. Meyer Garcia, D. Miao, H. Miao, M. Mikhasenko, D.A. Milanes, A. Minotti, E. Minucci, B. Mitreska, D.S. Mitzel, R. Mocanu, A. Modak, L. Moeser, R.D. Moise, E.F. Molina Cardenas, T. Mombächer, M. Monk, T. Monnard, S. Monteil, A. Morcillo Gomez, G. Morello, M.J. Morello, M.P. Morgenthaler, A. Moro, J. Moron, W. Morren, A.B. Morris, A.G. Morris, R. Mountain, Z. Mu, N. Muangkod, E. Muhammad, F. Muheim, M. Mulder, K. Müller, F. Muñoz-Rojas, V. Mytrochenko, P. Naik, T. Nakada, R. Nandakumar, G. Napoletano, I. Nasteva, M. Needham, N. Neri, S. Neubert, N. Neufeld, J. Nicolini, D. Nicotra, E.M. Niel, L. Nisi, Q. Niu, B.K. Njoki, P. Nogarolli, P. Nogga, J. Nombela Royo, C. Normand, J. Novoa Fernandez, G. Nowak, H.N. Nur, A. Oblakowska-Mucha, T. Oeser, O. Okhrimenko, R. Oldeman, F. Oliva, E. Olivart Pino, M. Olocco, C.J.G. Onderwater, R.H. O'Neil, J.S. Ordonez Soto, D. Osthues, J.M. Otalora Goicochea, P. Owen, A. Oyanguren, O. Ozcelik, F. Paciolla, A. Padee, K.O. Padeken, B. Pagare, T. Pajero, A. Palano, L. Palini, M. Palutan, C. Pan, X. Pan, S. Panebianco, S. Paniskaki, L. Paolucci, A. Papanestis, M. Pappagallo, L.L. Pappalardo, C. Pappenheimer, C. Parkes, D. Parmar, G. Passaleva, D. Passaro, A. Pastore, M. Patel, J. Patoc, C. Patrignani, A. Paul, C.J. Pawley, A. Pellegrino, J. Peng, X. Peng, M. Pepe Altarelli, S. Perazzini, H. Pereira Da Costa, M. Pereira Martinez, A. Pereiro Castro, C. Perez, P. Perret, A. Perrevoort, A. Perro, M.J. Peters, K. Petridis, A. Petrolini, S. Pezzulo, J.P. Pfaller, H. Pham, L. Pica, M. Piccini, L. Piccolo, B. Pietrzyk, R.N. Pilato, D. Pinci, F. Pisani, M. Pizzichemi, V.M. Placinta, M. Plo Casasus, T. Poeschl, F. Polci, M. Poli Lener, A. Poluektov, I. Polyakov, E. Polycarpo, S. Ponce, D. Popov, K. Popp, K. Prasanth, C. Prouve, D. Provenzano, V. Pugatch, A. Puicercus Gomez, G. Punzi, J.R. Pybus, Q. Qian, W. Qian, N. Qin, R. Quagliani, R.I. Rabadan Trejo, B. Rachwal, R. Racz, J.H. Rademacker, M. Rama, M. Ramírez García, V. Ramos De Oliveira, M. Ramos Pernas, G. Ramsey, M.S. Rangel, G. Raven, M. Rebollo De Miguel, F. Redi, J. Reich, F. Reiss, Z. Ren, P.K. Resmi, M. Ribalda Galvez, R. Ribatti, G. Ricart, D. Riccardi, S. Ricciardi, K. Richardson, M. Richardson-Slipper, F. Riehn, K. Rinnert, P. Robbe, G. Robertson, E. Rodrigues, A. Rodriguez Alvarez, E. Rodriguez Fernandez, J.A. Rodriguez Lopez, E. Rodriguez Rodriguez, J. Roensch, A. Rogovskiy, D.L. Rolf, P. Roloff, V. Romanovskiy, A. Romero Vidal, G. Romolini, F. Ronchetti, T. Rong, W. Rose, M. Rotondo, M.S. Rudolph, M. Ruiz Diaz, J. 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High Energy Astrophysical Phenomena

Refined anti-proton and anti-deuteron fluxes from weak-scale Dark Matter

Marco Cirelli, Mattia Di Mauro and Arpan Kar

We provide the cosmic-ray (CR) fluxes of antiprotons and antideuterons produced by the Galactic annihilation or decay of weak-scale dark matter (DM) particles of masses in the range from a few GeV to 100 TeV. We estimate these fluxes based on the updated models for the propagation of charged particles in the Galaxy and using the improved $\bar{p}$ and $\bar{d}$ spectra provided by $\texttt{CosmiXs}$. For the updated propagation models we consider the MIN/MED/MAX sets under the new SLIM/BIG/QUAINT schemes. We treat the Galactic propagation in a semi-analytic way including different possible effects such as spatial diffusion, energy-losses, convection and diffusive reacceleration. For the DM distribution in the Galactic halo we consider NFW, Einasto and Burkert profiles with the most updated parameters. Moreover, we also incorporate the latest models for the inelastic cross-sections of $\bar{p}$ and $\bar{d}$ based on ALICE data. We validate our calculations with those available in the literature or those obtained from other publicly available numerical packages. We compare the CR fluxes obtained in this work with those provided previously by $\texttt{PPPC4DMID}$ which were based on old propagation scenarios. We find that the CR fluxes obtained here with the new propagation models are much more robust (compared to the older ones) under the variation MIN - MAX. We also discuss the impact of this in the improvement of the discovery potential of a possible DM signal in the light of the present and upcoming CR observations. We provide all our results for the DM-induced interstellar CR fluxes in a tabulated format (for the kinetic energy range 0.1 GeV - 100 TeV) in the $\texttt{GitHub}$ repository of the newly created $\texttt{CosmiXsPPPC}$ project. The results are ready to be used for studies related to DM indirect searches.
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High Energy Astrophysical Phenomena

X-rays breaking out of pre-explosion ejecta mark a supernova's first light

Weimin Yuan, Qiu-Ju Huang, Jin-Ping Zhu et al. (+130 more)

Massive stars die as core-collapse supernovae, whose optical light emerges days after the implosion. Theory predicts that the initial collapse-driven shock, upon breaking through the star and dense circumstellar medium, emits a brief thermal flash of soft X-rays and ultraviolet. Yet these elusive first signals have remained largely undetected, owing to limited wide-field soft X-ray monitoring. Here we report the discovery of a soft X-ray flash, EP260321a, followed days later by a broad-lined supernova from an envelope-stripped progenitor. Its X-ray spectrum, best modeled with blackbody, establishes it as the long-sought archetypal shock breakout. The burst's duration and energetics place the breakout at a radius of 300 solar radii, tracing a dense surrounding shell and revealing abrupt mass ejection within the final month before collapse.
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All authors Weimin Yuan, Qiu-Ju Huang, Jin-Ping Zhu, Yun-Wei Yu, Dong Xu, Chen Zhang, Zhuo Li, Yuan Liu, Tao An, Giulia Gianfagna, Weikang Zheng, Guowang Du, Xing Liu, Ji-An Jiang, Johan P.U. Fynbo, Alexei S. Pozanenko, Junjie Jin, Yi Yang, Jinsong Deng, Hui Sun, Guang-Lei Wu, Yu-Hao Zhang, Bao Wang, Yu Wang, Xiangyu Wang, Bin-Bin Zhang, Yong Chen, Yonghe Zhang, Bo Wang, Xiaofeng Wang, Xuefeng Wu, Zigao Dai, Jie An, G.C. Anupama, Arvind Balasubramanian, Congying Bao, Aru Beri, Varun Bhalerao, Thomas G. Brink, Gabriele Bruni, Minxuan Cai, Zhiming Cai, Krittapas Chanchaiworawit, Yehai Chen, Huaqing Cheng, Bertrand Cordier, Chenzhou Cui, Weiwei Cui, Cuiyuan Dai, D. Eappachen, M. V. Eselevich, Xiao Fan, Zhou Fan, Yuan Fang, Hua Feng, Alexei V. Filippenko, Shaoyu Fu, He Gao, Jinjun Geng, Vitaly Goranskij, Ju Guan, Dawei Han, Jinxin Hao, Linbo He, Min He, Jingwei Hu, Maohai Huang, Shumei Jia, Ziqing Jia, Shuaiqing Jiang, Chichuan Jin, Ge Jin, Peter Jonker, E. V. Klunko, Albert K. H. Kong, Chengkui Li, Dongyue Li, Rui-Zhi Li, Wenxiong Li, Run-Duo Liang, Zhixing Ling, Congzhan Liu, Huaqiu Liu, Liangduan Liu, Xiangkun Liu, Xiaowei Liu, Yuanqi Liu, Zhengwei Liu, Fangjun Lu, Jirong Mao, Xuan Mao, A. S. Moskvitin, Haiyang Mu, Kirpal Nandra, Jan-Uwe Ness, Kangrui Ni, Kanthanakorn Noysena, Paul O'Brien, Haiwu Pan, Yu Pan, N.S. Pankov, Luigi Piro, J. Quirola-Vasquez, Arne Rau, Nanda Rea, D.K. Sahu, Aditya Pawan Saikia, Jeremy Sanders, Liming Song, Olga Spiridonova, Ning-Chen Sun, Shengli Sun, Xiaojin Sun, Yuyin Tan, Aishwarya Linesh Thakur, Samaporn Tinyanont, Valery Vlasyuk, A.V. Volnova, Ailing Wang, Hong Wu, Qianrui Wu, Haitao Xu, Zelin Xu, Changbin Xue, Yi-Han Iris Yin, I. A. Zaznobin, Jia-Sen Zhang, Shuang-Nan Zhang, Songbo Zhang, Yu Zhang, Zipei Zhu, Zecheng Zou, Bing Zhang

High Energy Astrophysical Phenomena

Limits on primordial black holes from the extragalactic gamma-ray background; current status and future projections

Ilias Cholis, Iason Krommydas and John Carlini

Primordial black holes (PBHs), possibly formed from the collapse of early universe perturbations, will evaporate via Hawking radiation with a lifetime comparable to the age of the universe, if their mass is $O(10^{14})$ g. Such black holes can contribute to the observed gamma-ray fluxes in the MeV and GeV range. Using the observed extragalactic gamma-ray background (EGRB) from the Fermi Large Area Telescope, the EGRET, and the COMPTEL telescopes that cover gamma-ray energies from 0.5 MeV to 1 TeV, we evaluate limits on the abundance of PBHs with masses of $10^{14}$ to $10^{17}$ g. We study both monochromatic and extended mass distributions of PBHs. To model the EGRB spectrum, we calculate the contribution from extragalactic sources including blazars, star-forming galaxies and radio galaxies and also account for ultra-high-energy cosmic rays that produce gamma rays when interacting with the infrared background. Our EGRB modeling uses information from the Fermi gamma-ray point sources catalog, from observations at X-rays, the visible spectrum, the infrared and radio waves, and also accounts for modeling uncertainties and variations on the properties within each class of these sources. Moreover, we use recent work on the modeling of the PBHs' gamma-ray emission, that includes the direct Hawking radiation, gamma rays produced in the hadronization and decay of unstable particles, final state radiation and gamma rays from pair annihilations in the interstellar medium. As the contribution of final state radiation and the annihilation of positrons enhances the low-energy part of the produced gamma-ray spectra from PBHs, we find that the EGRB observations can set the tightest limits on their abundance among all indirect dark matter probes, within the mass range of interest.[abridged]
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Earth and Planetary Astrophysics

Complex gas flows in magnetized protoplanetary disks promote the formation of dust traps at low fragmentation velocities

Vignesh Vaikundaraman, Joanna Drazkowska, Nerea Gurrutxaga et al. (+1 more)

Non-ideal magnetohydrodynamic simulations of protoplanetary disks show a plethora of complex gas structures, including winds, rings, and gaps. These affect dust transport and help form dust traps, which are essential for planetesimal formation. Although studies have explored the evolution of dust in such systems, they have done so either in 1D or without dust coagulation, and the effect of such systems on dust growth is still an active area of research. This work aims to investigate the effect of a complex gas flow architecture on global dust evolution, including dust growth and transport. We examine the timescales of different processes impacting dust evolution and discuss prospects of forming planetesimals. We post-process gas velocity output from a 2D non-ideal magnetohydrodynamic simulation using a 2D (r-z) Monte Carlo dust coagulation code to perform global simulations of dust growth and evolution. We perform three runs, one with a typical steady-state disk and two with the gas velocity from the MHD simulation, where we vary the fragmentation velocity. Our results show that the advection of small particles by the gas due to strong gas velocities can play an important role in setting the dust size distributions around protoplanetary disks. The gas flow structure has a transition region, and this region acts as a location of a dust pile-up, increasing the pebble-to-gas ratio by a factor of 2.5 when compared to the steady state disk. Lowering the fragmentation velocity improves the stability of the pile-up, but the pebble concentration is not as high. This scenario acts as a way to form a dust trap in a disk without a pressure bump. We discuss the possibilities for planetesimal formation in such a trap.
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All authors Vignesh Vaikundaraman, Joanna Drazkowska, Nerea Gurrutxaga, Xue-Ning Bai

High Energy Astrophysical Phenomena

A Multi-Wavelength View of the First Type Ic-BL Supernova with an Einstein Probe X-ray Shock Breakout

Jillian C. Rastinejad, Gokul Srinivasaragavan, Nikhil Sarin et al. (+36 more)

In March 2026, the Einstein Probe (EP) discovered its most nearby (z = 0.0343) Fast X-ray Transient (FXT), EP260321a, the first EP FXT to provide a strong match to expectations for X-ray "shock breakout'" (SBO) emission. Here, we present our multi-wavelength follow-up campaign of EP260321a and its broad-line Type Ic (Ic-BL) supernova (SN) counterpart, SN2026gzf. We show that our radio follow-up extending over 5.8 - 54.5 days post-FXT rules out an on-axis jet counterpart of isotropic-equivalent kinetic energy $E_{K} \gtrsim 10^{49}$ erg for circumburst densities $n > 10^{-2}~{\rm cm}^{-3}$ and assuming microphysical parameters $\epsilon_e = \epsilon_B = 0.1$. Our radio data also constrains a median mass-loss rate of $\dot{M} \lesssim 1.2 \times 10^{-5} M_{\odot}~{\rm yr}^{-1}$ for a Wolf-Rayet progenitor. In addition, we derive SN2026gzf's properties, including $^{56}$Ni mass, diffusion timescale, and expansion velocities, from our $\sim$nightly-cadence optical data and compare them with those of optically discovered Type Ic-BL SNe, finding that SN 2026gzf is well within the 90% confidence interval across all properties. We further fit SN2026gzf's light curve and determine that combined emission from both interaction with CSM and $^{56}$Ni radioactive decay provides the best fit with plausible model parameters. Finally, using the rate of Ic-BL SNe from the ZTF Bright Transient Survey and assuming all Type Ic-BL SNe produce EP260321a-like FXTs, we infer an expected rate of EP-detected SBOs of 4.4 - 16 year$^{-1}$. This is inconsistent at the 90% confidence level with current EP detection rates, potentially indicating that most Type Ic-BL SNe produce less luminous X-ray SBO signals compared to EP260321a.
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All authors Jillian C. Rastinejad, Gokul Srinivasaragavan, Nikhil Sarin, Tanner O'Dwyer, S. Bradley Cenko, James K. Leung, Anya E. Nugent, Daniel A. Perley, Genevieve Schroeder, Shreya Anand, Tomas Ahumada, Igor Andreoni, Aleksandra Bochenek, Alessandra Corsi, Christoffer Fremling, Anna Y. Q. Ho, Mansi M. Kasliwal, Geoffrey Mo, Anirudh Salgundi, Kendall I. Sippy, J. Sollerman, Eric C. Bellm, Tracy X. Chen, Michael W. Coughlin, Michael C. Davis, Fabio De Colle, Danielle Frostig, Christopher L. Fryer, Michael J. Graham, Xander J. Hall, K. -R. Hinds, Luca Izzo, Wynn Jacobson-Galan, Nathan P. Lourie, Keiichi Maeda, Josiah Purdum, Ben Rusholme, Avinash Singh, Robert Stein

High Energy Astrophysical Phenomena

Decadal pre-explosion activity and circumstellar interaction in a supernova

Ting-Wan Chen, Amar Aryan, Sheng Yang et al. (+52 more)

When a massive star explodes as a supernova, crucial information about its immediate environment is lost within hours. Here we report rapid optical observations from Lulin Observatory of the broad-lined Type Ic supernova SN 2026gzf, beginning 1.25 hours after Einstein Probe detected the X-ray transient EP260321a. Our data led to the discovery of the optical counterpart and showed a luminous blue first-day excess that cannot be reproduced by standard radioactive models. We find that interaction between the ejecta and $\approx 0.02$ M$_{\odot}$ of circumstellar material accounts for the early excess. Archival Panoramic Survey Telescope and Rapid Response System (Pan-STARRS) images show variability at the explosion site over the previous $\sim 12$ years, with the source brightening by a factor of $\sim 1.5$ in the final $\sim 3$ years before explosion, providing rare evidence for pre-explosion activity in a stripped-envelope progenitor system. The precursor brightening suggests enhanced eruptive mass loss during late-stage oxygen burning before core collapse, while an additional silicon-burning episode shortly before explosion may have created the compact nearby material responsible for the X-ray shock-breakout signal. SN 2026gzf therefore offers the first view of how a stripped progenitor modifies its immediate environment shortly before death, linking long-term precursor variability, circumstellar interaction and the explosion itself.
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All authors Ting-Wan Chen, Amar Aryan, Sheng Yang, Stephen J. Smartt, Takashi J. Moriya, Seán J. Brennan, Maximilian D. Stritzinger, Bailey Martin, Matt Nicholl, Albert K. H. Kong, James H. Gillanders, Anirban Dutta, Brian P. Schmidt, Yu-Chi Cheng, Mark E. Huber, Cheng-Han Lai, Chien-Hsiu Lee, Yu-Hsing Lee, Chow-Choong Ngeow, Ken W. Smith, Christopher Ashall, Katie Auchettl, Chris R. Burns, Kenneth C. Chambers, Zhi-Yue Chen, Thomas de Boer, Eric Y. Hsiao, Khoa Ngo Thanh Ho, Willem B. Hoogendam, David O. Jones, Erkki Kankare, Tom L. Killestein, Hanindyo Kuncarayakti, Meng-Han Lee, Chuan-Jui Li, Chien-Cheng Lin, Christopher Lidman, Thomas B. Lowe, Eugene A. Magnier, Kyle Medler, Anais Möller, Thomas Moore, Nidia Morrell, Gregory S. H. Paek, Cameron M. Pfeffer, Da-Chun Qiang, Liana Rauf, Thomas M. Reynolds, Aiswarya Sankar.K, Shubham Srivastav, Jack Tweddle, Richard Wainscoat, Ze-Ning Wang, Huangfei Xiao, Zonghong Zhu

Cosmology and Nongalactic Astrophysics

Mixed Dark Matter: Limits from the Milky Way Satellite Galaxies

Wendy Crumrine, Dominic Pang, Ethan O. Nadler et al. (+2 more)

The Standard Model of particle physics contains a diverse set of particle species, motivating the possibility of a similarly complex dark sector. Here we study two-component dark matter (DM) mixtures, in which one component behaves as standard CDM while the other suppresses the formation of small-scale structure, either through an astrophysically relevant de~Broglie wavelength (fuzzy DM; FDM) or collisional damping from temperature-independent scattering (interacting DM; IDM). Using the observed population of Milky Way satellite galaxies, we derive new leading constraints on the parameter spaces of mixed FDM and of mixed IDM coupled to photons ($\gamma$-DM), neutrinos ($\nu$-DM), or baryons ($p$-DM), for beyond-CDM fractions down to $50\%$. We require that the linear matter power spectra of allowed models remain less suppressed than a constrained reference model. The resulting $95\%$ confidence bounds on FDM mass and IDM cross section weaken systematically with decreasing fraction, following distinct power-law scalings. At $50\%$ fraction, IDM cross section bounds weaken by a factor of $\sim$2–6 and FDM mass bounds by $\sim$1.5, relative to the $100\%$ case. We forecast that idealized future satellite surveys, which adopt approximate LSST sensitivity thresholds, can improve these $100\%$ bounds by a factor of $\sim$1.6–14 for IDM and $\sim$3 for FDM. Self-consistent cosmological simulations of mixed DM scenarios will be essential to more robustly characterize the degeneracy between particle physics parameters and fractional contribution, to extend constraints to lower fractions, and to identify signatures beyond satellite abundance to further inform these models.
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All authors Wendy Crumrine, Dominic Pang, Ethan O. Nadler, Andrew Benson, Vera Gluscevic

Astrophysics of Galaxies

On Cross-Correlating Line Intensity Maps from SPHEREx during Reionization

Abigail E. Ambrose, Eli Visbal and Matthew McQuinn

We have simulated Ly{\alpha}, H{\alpha}, H{\beta}, [OII], and [OIII] intensity maps which are observable by SPHEREx during cosmic reionization. We simulate these intensity maps including all significant sources of emission for each line, and include radiative transfer for the Ly{\alpha} intensity maps. We also include a simple model of dust extinction based on observations of galaxies at z<5. One of the main challenges of intensity mapping is interloping lines from galaxies at lower redshifts, which makes producing an auto-power spectrum challenging. We focus on cross-correlations between different lines, as this eliminates such foreground contamination of the signal. We have cross-correlated the simulated SPHEREx intensity maps to find the most observable cases. This includes modeling of interloping lines and masking bright interloping galaxies. Testing a range of cases motivated by observations, we find total signal-to-noise values up to 99 for the highest case of H{\alpha} cross-correlated with [OIII] at z=5 assuming no dust extinction. We also find cases which will not be detectable. We find that the dominant noise source in these intensity maps on most scales is from the instrument, except for Ly{\alpha} and [OII] and then only on the largest scales the interlopers are the dominant source. We find through intensity mapping we can probe galaxies with masses $M<4x10^{10}~M_{\odot}$ which are below the necessary luminosity for a 3{\sigma} signal-to-noise direct detection of galaxies by SPHEREx. However, the majority of our observable signal is dominated by large, directly detectable galaxies, rather than the smaller, fainter galaxies. We find marginal detections of the clustering portion of the power spectrum at z=5 for H{\alpha}x[OIII]. Detections of the clustering signal from other lines or at z>6 will require more sensitive instruments, such as the Cosmic Dawn Intensity Mapper.
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Quantum Physics

Wave packets from the spectrum

ChunJun Cao, Oliver Friedrich, Marin Girard et al. (+2 more)

The freedom to change Fock basis seems to ensure a minimum amount of locality in lattice theories in the following sense: If $\lbrace (\hat a_i^\dagger\,,\,\hat a_i)\rbrace$ for $i=1,\dots,n$ is a lattice of creation and annihilation operators and if a given Hamiltonian $\hat H$ induces highly non-local dynamics on that lattice, then it will usually be possible to change to a new set of operators $\lbrace (\hat b_i^\dagger\,,\,\hat b_i)\rbrace$ in terms of which the dynamics appear less non-local. We demonstrate this by turning a highly non-local random matrix model into a local, 1D lattice theory where particles can propagate in localized wave packets. More generally, we show that any Hamiltonian can be made to look like such a theory, with the lattice dispersion relation and the non-integrability of the theory depending on the spectrum of $\hat H$. We argue that our results are a step towards quantum mereology for fields.
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All authors ChunJun Cao, Oliver Friedrich, Marin Girard, Nicolas Loizeau, Ashmeet Singh

Strongly Correlated Electrons

Exactly solvable non-planar $\mathbb{Z}_{2}$ dimer liquids on checkerboard and ruby lattices

Julia Wildeboer, Zohar Nussinov, Thomas Iadecola et al. (+1 more)

We generalize an influential framework for exactly solvable quantum dimer models with dual Ising gauge theory descriptions realizing the $\mathbb{Z}_{2}$ topological phase from trivalent to tetravalent parent lattices. The resulting quantum dimer models live on crossed-medial lattices and possess the remarkable feature of having crossed plaquettes, leading to transition graphs with generically intersecting loops. This non-planar structure runs counter to established templates for analytically tractable dimer liquids. As the simplest realization of the construction, we introduce an exactly solvable quantum dimer model on the checkerboard lattice that allows an exact mapping to the toric code, thus providing a particularly direct connection between the latter and Anderson's short range resonating valence bond paradigm. We further show that a corresponding crossed ruby lattice construction, dual to an Ising gauge theory on the kagome lattice, naturally falls within the same framework. More generally, the construction gives rise to a broad class of exactly solvable crossed-medial quantum dimer models and admits natural iteration, generating cascades of solvable $\mathbb{Z}_{2}$ topological dimer liquids beyond the standard planar setting. We furthermore extend Kasteleyn methods to the relevant non-planar graphs, enabling controlled wave-function deformations away from the commuting-projector points while retaining efficient evaluation of correlation functions.
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All authors Julia Wildeboer, Zohar Nussinov, Thomas Iadecola, Alexander Seidel

High Energy Astrophysical Phenomena

Failed jet breakout in the metal-poor broad-lined type Ic supernova 2026gzf

Antonio Martin-Carrillo, Christina C. Thöne, James K. Leung et al. (+103 more)

A long-standing question in the death of massive stars is the role of relativistic jets. While many gamma-ray bursts and some fast X-ray transients seem to be associated with broad-lined type Ic supernovae, the opposite is not true. The lack of observable jet emission in those Ic-BL SNe can be explained by invoking off-axis jets, choked jets that inject all their energy into the stellar envelope, baryon-loaded jets for which the prompt high-energy emission is strongly suppressed, or non-jetted SNe. The lack of exact explosion time in the majority of SNe presents an obstacle to distinguish between these scenarios. Here we report the properties of SN 2026gzf associated with the X-ray thermal Einstein Probe shock-breakout EP260321a at z=0.0343. The absence of compelling shocked cocoon and radio emission up to 54 days, combined with initial expansion velocities of ~30,000 km/s and a circumstellar shell of ~0.07 M$_\odot$, favour a scenario for SN 2026gzf in which a jet was choked in the circumstellar shell. Our high-spatial resolution images of the SN environment show that the progenitor was located between two highly star-forming regions with a metallicity lower than any previously known Ic-BL SN. As the first case of a Ic-BL SN associated with high-energy prompt emission without the signature of a jet, SN 2026gzf provides a unique perspective to understand the successful launch of relativistic jets during the deaths of massive stars.
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All authors Antonio Martin-Carrillo, Christina C. Thöne, James K. Leung, Gregory Corcoran, Antonio de Ugarte Postigo, Peter G. Jonker, Luca Izzo, Andrew J. Levan, Benjamin P. Gompertz, Stéphane Basa, Nikhil Sarin, Jonathan Quirola-Vásquez, Rob A. J. Eyles-Ferris, Riccardo Brivio, Alan M. Watson, Laura Cotter, Jennifer Alexandra Chacón, Andrea Rossi, Andrea Melandri, Piramon Kumnurdmanee, Nial R. Tanvir, Anshika Gupta, Franz E. Bauer, Jean-Grégoire Ducoin, Andrea Reguitti, Kuntal Misra, Dong Xu, Susanna D. Vergani, Wen-fai Fong, Kendall Ackley, Edilberto Aguilar-Ruiz, Dalya Akl, Miguel Ángel Aloy, Jie An, Camila Angulo-Valdez, Sarah Antier, Jean-Luc Atteia, Rosa L. Becerra, Rene P. Breton, Nathaniel R. Butler, Sergio Campana, Francesco Carotenuto, Jorge Casares Velázquez, Ashley A. Chrimes, Valerio D'Elia, Joyce N. D. van Dalen, Fabio De Colle, Massimiliano De Pasquale, Vik S. Dhillon, Damien Dornic, Martin J. Dyer, Matteo Ferro, Morgan Fraser, Andrew S. Fruchter, Francis Fortin, Duncan K. Galloway, Leonardo García-García, Stefan Geier, Ramandeep Gill, Noémie Globus, Roberto Gualandi, Marion Guelfand, Francesco Guidolin, Dieter H. Hartmann, Agnes P. C. van Hoof, Pall Jakobsson, Divyanshu Janghel, Tom L. Killestein, Sylvio Klose, Shiho Kobayashi, Rubina Kotak, Amit Kumar, Asuka Kuwata, Tanmoy Laskar, William H. Lee, Massimiliano Lincetto, Gianluca Lombardi, Diego López-Cámara, Joseph D. Lyman, Elisabetta Maiorano, Keiichi Maeda, Nikos Mandarakas, Francesco Magnani, Jirong Mao, Enrique Moreno Méndez, Ana María Nicuesa Guelbenzu, Kanthanakorn Noysena, Laura K. Nuttall, Paul T. O'Brien, David O'Neill, Paolo Ochner, Margarita Pereyra, Giovanna Pugliese, Gavin Ramsay, Lauren Rhodes, Andrea Saccardi, Ruben Salvaterra, Fredd Sánchez Álvarez, Benjamin Schneider, Steve Schulze, Rhaana L. C. Starling, Danny Steeghs, Kzrysztof Ulaczyk, Chiara Ventura, Tayyaba Zafar, Zi-Pei Zhu

Mesoscale and Nanoscale Physics

Fabry-Perot Interference, g-factor Anisotropy, and Gate-Tunable Quantum dot in Chiral Tellurium Nanowires

Suresh Ghimire, Mohammad Hafijur Rahaman, Nathan Tanner Sawyers et al. (+8 more)

Chiral materials with strong spin-orbit coupling offer a unique platform for exploring the interplay between topology, chirality, and quantum transport yet the quantum coherent regime in elemental tellurium nanostructures remains largely unexplored. Here we demonstrate phase-coherent quasi-ballistic transport, anisotropic Zeeman spectroscopy, and gate-tunable quantum dot formation in hydrothermally grown t-tellurium nanowires. Single nanowire field-effect transistors exhibit p-type transport with hole mobilities rising from approx. 80 cm2 V-1 s-1 at 210 K to approx. 190 cm2 V-1 s-1 at 1 K, consistent with a crossover from phonon-limited to Coulomb scattering dominated regimes near 50 K. Notably, devices segregate into two distinct regimes based on their room temperature two-terminal resistance : low-resistance devices (< 30 kOhm) exhibit Fabry-Perot interference, whereas high resistance devices (> 30 kOhm) display Coulomb-blockade behavior revealing a two-terminal resistance-driven transition between quasi-ballistic and strongly localized transport regimes. Zeeman spectroscopy in in-plane and out-of-plane magnetic fields yields highly anisotropic Lande g-factors (an in-plane gparallel = 1.18 and an out-of-plane gperp = 18.41) and directly resolves a spin-orbit energy gap DeltaSO = 0.864 meV from an avoided crossing. These results establish chiral tellurium nanowires as a versatile platform for gate-defined spin qubits exploiting large, tunable g-factors and for hybrid tellurium-superconductor architectures targeting Majorana zero modes in an elemental vdW system.
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All authors Suresh Ghimire, Mohammad Hafijur Rahaman, Nathan Tanner Sawyers, Madan Mohan Bhandari, Gokul Acharya, Syed Zulfiqar Hussain Shah, Iris Nandhakumar, Pawan Kumar, Zainul Aabdin Khan, Hugh O. H. Churchill, Dharmraj Kotekar-Patil

Astrophysics of Galaxies

From Dense Gas Clouds to Supermassive Black Hole Seeds: Hybrid Hydro/Direct $N$-body Simulations of Runaway Collision-driven Intermediate-mass Black Hole Formation

Eunwoo Chung, Yongseok Jo, Ji-hoon Kim et al. (+2 more)

A population of dense stellar systems at high redshift has recently been uncovered by the JWST. To investigate the formation of supermassive black hole (SMBH) seeds in these dense environments without invoking any ad hoc seeding mechanisms, we present star cluster-scale simulations performed with an updated version of the hydrodynamics code Enzo-Abyss, which self-consistently integrates the gravity using a direct $N$-body method coupled with stellar evolution. By modeling initially dense, metal-poor gas clouds with varying turbulence, we consistently find the formation of dense clusters resembling early-stage nuclear star clusters (NSCs), as well as the formation of very massive stars (VMSs) ranging from $343\;\mathrm{M_\odot}$ to $5108\;\mathrm{M_\odot}$ via runaway collisions, irrespective of stellar wind feedback strength. Following the direct collapse of these VMSs, the resulting intermediate-mass black holes (IMBHs) grow through Eddington-limited gas accretion and tidal disruption events (TDEs). In our most optimistic model, we find a mass accretion rate of $1.64\times10^{-4}\;\mathrm{M_\odot\;yr^{-1}}$, with TDEs contributing $23\%$ of the total accretion over $\sim10\;\mathrm{Myr}$. Assuming a steady gas supply into the NSC driven by rapid structural assembly in the high-redshift environment, together with a constant TDE rate, we project that an IMBH with an initial mass of $6747\;\mathrm{M_\odot}$ at the center of the NSC can grow to $\sim62000\;\mathrm{M_\odot}$ within $100\;\mathrm{Myr}$ of its formation. Our numerical study, conducted within a single self-consistent framework that incorporates the essential physical processes, suggests that VMSs can form in dense gas clouds, collapse into IMBHs, and subsequently provide viable seeds for the SMBHs observed at high redshift.
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All authors Eunwoo Chung, Yongseok Jo, Ji-hoon Kim, Minyong Jung, Oh-kyoung Kwon

Astrophysics of Galaxies

Individual Star Sampling in Star Formation Simulations: A Semi-Deterministic Model

Yunwei Deng, Hui Li, Zhiqiang Yan et al. (+2 more)

In modern simulations that include star formation, it is common to use a universal and invariant initial mass function (IMF) to represent star populations or sample individual stars. However, stellar masses are determined by local and environmental processes that operate over a wide dynamical range and remain unresolved in simulations. We introduce a semi-deterministic (SDT) scheme for sampling individual stars from star-forming gas in numerical simulations. We represent unresolved molecular cores and protostellar disks with reservoir particles (RsvPs) and employ an on-the-fly friends-of-friends algorithm to identify star clusters. The instantaneous IMF for newly formed stars is then derived from the current cluster mass. We test the performance of this method in simulations of isolated molecular clouds and a major merger between two dwarf galaxies. Compared to existing IMF sampling methods, our SDT scheme naturally reproduces the observed $m_{\star,\text{max}}$-$M_\text{ecl}$ relation and yields numbers of massive stars consistent with optimal sampling theory. It also exhibits the smallest run-to-run variation among simulations with different random seeds. The regulated star formation results in a small ($\sim0.15$ Myr) but coherent time delay in the emergence of massive stars, reduces the large scatter arising from Poisson noise, and produces initial mass segregation within the clusters. On galactic scales, the SDT method predicts a steeper high-mass IMF slope at low star formation rates (SFRs), with the slope negatively correlated with the SFR. As the specific abundance of massive stars declines, our model naturally explains the systematically low H$\alpha$-based SFRs, where the H$\alpha$ indicator for Milky Way-like galaxies underestimate the intrinsic SFR owing to the reduced population of massive stars.
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All authors Yunwei Deng, Hui Li, Zhiqiang Yan, Chuizheng Kong, Zhi-Yu Zhang

High Energy Physics (Phenomenology)

Constraints and Projections for Millicharged Dark Matter in the Sun with Water Cherenkov Neutrino Detectors

Thong T.Q. Nguyen

Millicharged particles are well-motivated dark matter candidates that have been extensively investigated in terrestrial experiments. Recent studies proposed using the IceCube Neutrino Observatory to search for high-energy neutrinos produced by the capture and annihilation of millicharged dark matter in the Sun, deriving new constraints in the strong interaction regime where the millicharge is $q_\chi \sim 10^{-3}$-$10^{-2}$, which extend to small fractional abundances where all existing constraints lose sensitivity. In this work, I point out that the lower energy threshold of water Cherenkov detectors makes Super-Kamiokande and the future Hyper-Kamiokande sensitive to neutrinos from the annihilation of lighter millicharged dark matter, complementing the high-mass reach of IceCube. I find that Super-Kamiokande can constrain previously unexplored parameter space at $m_{\chi}=5$-28 GeV for dark matter fraction of $f_{\chi}=10^{-4.5}$, while Hyper-Kamiokande can improve these constraints and will be sensitive to fractional abundances as small as $f_{\chi}\simeq 5\times 10^{-6}$, nearly an order of magnitude below current IceCube limits.
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Cosmology and Nongalactic Astrophysics

A universal model for the accretion rates and formation times of dark matter halos

Ankita Bera and Benedikt Diemer

The formation histories of halos set the baseline rate at which galaxies accrete gas over cosmic time. While a number of models describe these histories and their derivative, the mass accretion rate (MAR), a simple and universal formula has remained elusive. Here we measure the median MARs and half-mass formation times of halos in dark matter-only and hydrodynamical simulations, in extremely different cosmologies ($\Lambda$CDM and Einstein-de Sitter), and across a wide range of redshifts ($z = 0$-$14$). We confirm that MARs increase with mass and redshift, and that they are virtually identical in hydrodynamical and dark matter-only simulations. We show that MARs are accurately described by a universal six-parameter function of three physical variables: the peak height $\nu$, the slope of the linear power spectrum $n_{\rm eff}$, and the effective linear growth rate $\alpha_{\rm eff}$. A complementary two-parameter fit for the formation redshift improves on the function of Lacey & Cole by fixing one parameter to its physical value and adding a dependence on $n_{\rm eff}$. Our model is broadly consistent with some prescriptions from the literature but provides a larger range and higher accuracy at high redshifts and low masses. Our fitting functions are implemented in the publicly available Colossus toolkit.
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High Energy Physics (Theory)

On BPS Branes

Cumrun Vafa, David H. Wu and Kai Xu

We study supersymmetric BPS branes (BPS-B) in supergravity theories. Some of these states are anticipated by BPS black-brane (BPS-BB) solutions of supergravity. In particular, we define and distinguish the cone generated by BPS branes from the subcone of charges that admit BPS black-brane attractor solutions in the infrared limit of the supergravity effective field theory. We denote these cones by $C_{\rm BPS-B}$ and $C_{\rm BPS-BB}$, respectively. We conjecture that, in any supersymmetric theory of quantum gravity, every integrally charged state lying in $C_{\rm BPS-BB}$ is realized by a BPS state in the spectrum. Furthermore, we conjecture and present evidence that when $C_{\rm BPS-B}$ is moduli independent, it can be determined as the cone dual to the $C_{\rm BPS-BB}$ under the electric-magnetic pairing.
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Quantum Physics

Quantum resources in non-stoquastic quantum annealing

Chiara Capecci, Sebastian Nagies, Naga Dileep Varikuti et al. (+1 more)

Quantum annealing promises to solve combinatorial optimization problems by preparing the ground state of a target Hamiltonian. Standard annealing protocols are, however, stoquastic and can thus be simulated by sign-problem-free quantum Monte-Carlo methods. To obtain a true quantum advantage, it has been proposed to use non-stoquastic catalyst Hamiltonians. Active only at intermediate stages of the protocol, these can, for certain problems, convert first-order into second-order quantum phase transitions and thus permit an exponential speedup over the stoquastic protocol. At the same time, the non-stoquastic catalyst renders quantum Monte-Carlo methods inefficient. It remains, however, an open question how other classical computation methods are affected by the non-stoquastic terms. We address this question by computing quantum resources – entanglement entropy and stabilizer Rényi entropy – whose presence makes classical computations based on tensor networks and stabilizer-tableau methods exponentially hard. We compare these with the spectral gap along the annealing path for two paradigmatic benchmark models, the fully connected $p$-spin model and a geometrically local Ising model. While the exact behavior shows a subtle dependency on the underlying model and the annealing path, our numerics suggest consistently that the scaling of entanglement and non-stabilizerness is at least maintained in the deeply non-stoquastic regime and in some cases even significantly enhanced. Our results thus suggest that improvements of quantum performance in non-stoquastic annealing coincide with significant presence of quantum computational resources.
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All authors Chiara Capecci, Sebastian Nagies, Naga Dileep Varikuti, Philipp Hauke

Cosmology and Nongalactic Astrophysics

On the potential of pseudo-scalar dark energy

Andrea Minotti, Yunzhi Wu and Marco Regis

A cosmological pseudo-scalar field provides a compelling realization of dynamical dark energy (DE). If its coupling to photons is non-negligible, the cosmic microwave background acquires a rotation of its polarization plane, known as cosmic birefringence (CB). We present an extended analysis of several pseudo-scalar DE models and derive constraints on the parameters of their potentials by combining observations of the background expansion history with measurements of CB. We find that the axion-like potential constitutes a viable model only for large values of the anomaly coefficient. Scenarios in which the pseudo-scalar field rolls down a potential with quadratic, linear, or Ratra-Peebles forms can successfully explain DE and CB, with a symmetry-breaking scale close to the GUT scale.
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High Energy Physics (Phenomenology)

Probing lepton number violation at FCC-ee

Praveen Bharadwaj, Sanjoy Mandal, Rojalin Padhan et al. (+1 more)

We propose high-multiplicity final-state signatures, such as $e^+e^-\to N\overline{N}\to \ell^+\ell^+ 4j$ with $\ell$ denoting $e,~\mu$, $\tau$, as probes of lepton number violation (LNV) at FCC-ee, featuring negligible Standard Model background. In contrast to conventional searches such as $pp\to \ell^+ N \to \ell^+ \ell^+ jj$ or the process $e^+e^-\to\nu N$, which are suppressed by the small neutrino masses in conventional seesaw scenarios, the minimal linear seesaw picture avoids this suppression. This enables a direct LNV probe from final-state topology, with over $\mathcal{O}(10^3)$ events expected at FCC-ee. Besides probing the Majorana nature of neutrinos, this offers a novel avenue to test the neutrino mass ordering established by oscillation experiments in a high-energy collider setting.
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All authors Praveen Bharadwaj, Sanjoy Mandal, Rojalin Padhan, José W. F. Valle

High Energy Astrophysical Phenomena

EP260321a/SN 2026gzf: The Faintest Shock Breakout Associated with a Broad-Lined Supernova

Brendan O'Connor, Xander J. Hall, Malte Busmann et al. (+33 more)

The explosion of a star is first marked by the shock wave breaking out of the stellar surface, producing a burst of ultraviolet and X-ray radiation. These events are observationally rare, despite likely accompanying the majority of supernovae. Here, we report on our multi-wavelength observing campaign of the closest Einstein Probe fast X-ray transient EP260321a at $z=0.0344$. The thermal ($kT=130$ eV) X-ray emission with peak luminosity $1.0\times10^{45}$ erg s$^{-1}$ points to a shock breakout origin. We demonstrate that EP260321a is accompanied by a broad-lined Type Ic supernova, SN 2026gzf. The supernova properties, including its spectral evolution, lightcurve evolution, and expansion velocities, are all typical of the energetic stripped-envelope supernovae associated with gamma-ray bursts. However, deep X-ray upper limits obtained with the Chandra X-ray Observatory do not detect an X-ray afterglow, and instead exclude the afterglow of known gamma-ray bursts or fast X-ray transients. If the stellar explosion launched a successful relativistic jet, we require that it had both a low Lorentz factor $\Gamma_0$\,$<$\,$30$ and a kinetic energy $E_\textrm{kin}$\,$<$\,$10^{49}$ erg for a stellar wind density of $A_*$\,$\gtrsim$\,$1$. We propose that EP260321a originated from a mildly relativistic, weak outflow that was choked by the progenitor star. This scenario is capable of naturally explaining its low X-ray luminosity and lack of prompt gamma-ray emission. EP260321a bridges the gap between SN 2008D and low-luminosity GRBs, suggesting a greater diversity in the physical parameters of stripped stars as they undergo terminal collapse.
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All authors Brendan O'Connor, Xander J. Hall, Malte Busmann, Daniel Gruen, Alberto Floris, Tomas Cabrera, Ziyuan Zhu, Antonella Palmese, Dylan Green, John Banovetz, Julius Gassert, Christopher L. Fryer, Roberto Ricci, Eleonora Troja, Surya Shivaprasad, Gregory R. Zeimann, Ariel J. Amsellem, Stephen Bailey, Segev BenZvi, Simone Dichiara, Hendrik van Eerten, Jeremy Hare, Lei Hu, Christopher M. Irwin, Keerthi Kunnumkai, Konstantin Malanchev, Mitra Maleki, Michael J. Moss, Adam D. Myers, Dheeraj Pasham, Christoph Ries, Geoffrey Ryan, David Schlegel, Michael Schmidt, Silona Wilke, Yu-Han Yang

Quantum Physics

Graviton-mediated entanglement due to light bending from a quantum rotor

Dripto Biswas, Sougato Bose, Anupam Mazumdar et al. (+1 more)

One of the key tests of the quantum nature of gravity is to test whether the virtual mediator of gravity between matter and photon gives rise to the quantum light-bending phenomenon. The off-shell degrees of freedom, involving the spin-2 and spin-0 components of graviton, reproduce the classical deviation of light rays, as well as have been predicted to generate entanglement between matter and photon. This paper explores the generation of entanglement due to the quantum gravitational interaction in an optomechanical setup with a quantum rotor and photon. The virtual exchange of a graviton provides entanglement between the photon degrees of freedom and the spatial position of the quantum rotor, with the rotational state affecting its magnitude. We analyze the case of a high spinning rotor, in an approximately classical state of angular momentum, and quantify its effect on the gravitationally induced entanglement between the photon and the position of the quantum rotor. We show that the difference in the linear entanglement entropies, of prograde-and-retrograde motion of the photon with respect to the quantum rotor, provide tangible observable consequences.
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All authors Dripto Biswas, Sougato Bose, Anupam Mazumdar, Marko Toroš

High Energy Physics (Theory)

Ramond from Random: Weil-Petersson Volumes for Super-Riemann surfaces with NS Boundaries and R Punctures

Clifford V. Johnson

The Weil-Petersson (WP) volumes of the (compactified) moduli space of ${N}=1$ supersymmetric Riemann surfaces with Neveu-Schwarz (NS) boundaries are frequently discussed in the literature. Such surfaces can also have marked points called Ramond (R) punctures, where the superconformal structure degenerates. Computing the volumes when these R punctures are included is more challenging for the usual differential and algebraic geometry approaches, and they are therefore less well explored. In particular, the spectral curve describing the inclusion of R punctures is apparently unknown, so far. However, the right random matrix model approach can handle the NS and~R sectors on an equal footing. Such a construction is presented, showing how to use a recently developed technique to readily compute many closed-form formulae for $V^{(2m)}_{g,n}(\{b_i\})$, the WP volumes for genus $g$ with $n$ NS-boundaries of geodesic lengths $b_i$ ($i{=}1,\ldots,n$), and $2m$ R-punctures. Several striking relations between volumes (and subsectors thereof) emerge naturally in this approach. Moreover, the hitherto missing spectral curve is presented, and its use for (re-)deriving the $V^{(2m)}_{g,n}(\{b_i\})$ is demonstrated by using topological recursion.
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Superconductivity

Quantum-geometric origin of superfluid weight in quasicrystals with critical states

Kazuma Saito, Ryo Okugawa, Yusuke Kato et al. (+1 more)

A distinctive feature of many quasiperiodic systems is the presence of critical states that are neither extended nor exponentially localized. We investigate the geometric effect on the superfluid weight in quasiperiodic systems with critical states at zero temperature. We employ both real-space and momentum-space approaches to superfluid weight in quasicrystals, which allows us to separate the conventional and quantum geometric contributions. We find that the superfluid weight is dominated by the geometric contribution in quasiperiodic systems with critical states. This finding reveals a fundamental interplay between superconductivity and critical states in quasicrystals.
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All authors Kazuma Saito, Ryo Okugawa, Yusuke Kato, Takami Tohyama

Quantum Physics

Absence of poor local minima in matrix product states

Hao-Kai Zhang, Chenghong Zhu, Shuo Liu et al. (+2 more)

Quantum circuits suffer from severe trainability issues: even shallow circuits are swamped with poor local minima. Yet matrix product states (MPS), which can be prepared by sequential circuits, are remarkably trainable in practice – as demonstrated by decades of successful density matrix renormalization group calculations. In this work, we resolve this apparent paradox by proving that the energy landscapes of MPS are free from poor local minima, under the same setting where brickwork circuits are not. The key insight is that the gauge freedom of MPS creates an effective local overparametrization that causes local minima to concentrate near the global minimum, analogous to overparametrized classical neural networks. We rigorously prove that the local minimum distribution is invariant under moves of the orthogonality center of MPS representations. Numerical experiments further confirm that the optimization of sequential circuits converges to near-optimal solutions even for random Hamiltonians, in stark contrast to brickwork circuits. Our findings establish a theoretical understanding of the trainability of MPS, providing a valuable guide for designing variational quantum circuits and algorithms with better trainability in the future.
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All authors Hao-Kai Zhang, Chenghong Zhu, Shuo Liu, Shi-Xin Zhang, Tao Xiang

Solar and Stellar Astrophysics

Mode Instability and a Massive, Isolated Outburst in the Pulsating White Dwarf GD 1212

J. J. Hermes, Keaton J. Bell, Andrew H. Dublin et al. (+8 more)

We analyze a large brightening event that lasted for roughly half a day in the pulsating hydrogen-atmosphere white dwarf GD 1212 during K2 Campaign 12 of the extended Kepler mission. For the other 80 days of K2 observations, GD 1212 exhibited a rich spectrum of long-period (~1100 s) pulsations that underwent rapid variations in frequency and amplitude but did not exhibit any additional outbursts. We refine previous attempts at mode identification and find a likely sequence of dipole and quadrupole splittings that reveal an overall rotation rate of roughly 17.0 hr. The outburst at Day 61 is fully resolved by the 60-second-cadence K2 data, with the entire white dwarf becoming up to 17.5% brighter overall, from an approximately 850 K increase in effective temperature, with pulsational variability during the outburst showing shorter periods and higher amplitudes. Outbursts are believed to be the result of nonlinear mode coupling via parametric instability, whereby energy stored in linearly excited parent modes is rapidly transferred to damped child modes that dissipate near the surface. Additionally, we characterize a "failed" outburst that caused correlated pulsation frequency changes, an approximately 5 microHz increase, with a small approximately 0.35% corresponding brightness increase. GD 1212 is now the eighth pulsating hydrogen-atmosphere DAV white dwarf to show outburst behavior, although it exhibited the largest outburst yet and has the longest inferred recurrence timescale. This high-signal-to-noise record tracing pulsations through both large and small temperature excursions in GD 1212 provides unique insights into parametric resonance and nonlinear mode coupling in white dwarf pulsations.
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All authors J. J. Hermes, Keaton J. Bell, Andrew H. Dublin, M. H. Montgomery, Steven D. Kawaler, Ian Clark, Zachary P. Vanderbosch, Bart H. Dunlap, P.-E. Tremblay, Paul Chote, Boris T. Gaensicke

High Energy Physics (Experiment)

Testing Heavy Dark Matter Decay as the Origin of KM3-230213A

KM3NeT Collaboration: O. Adriani, J. A. Aguilar, A. Albert et al. (+286 more)

This work explores the hypothesis that the ultra-high-energy neutrino event KM3-230213A originates from the decay of a heavy dark matter particle with a mass above PeV scale. The analysis exploits the deposited energy and arrival direction of the event as well as a complete detector Monte Carlo simulation to compute the expected signal distributions for different decay channels and assesses the relative contributions from Galactic and extragalactic dark matter. Assuming a dark matter origin of the event, we find that the preferred mass at 95% C.L. is larger than about 100 PeV in all scenarios considered, with best-fit lifetimes in the range $10^{26}$-$10^{27}$ s. These preferred regions are in tension with existing bounds from other neutrino telescopes and gamma-ray observations.
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All authors KM3NeT Collaboration: O. Adriani, J. A. Aguilar, A. Albert, A. R. Alhebsi, S. Alshalloudi, F. Ameli, M. Andre, L. Aphecetche, M. Ardid, S. Ardid, J. Aublin, F. Badaracco, B. Baret, A. Bariego-Quintana, L. Barigione, M. Barnard, Y. Becherini, M. Bendahman, F. Benfenati Gualandi, M. Benhassi, D. M. Benoit, Z. Beňušová, E. Berbee, C. van Bergen, E. Berti, V. Bertin, P. Betti, S. Biagi, M. Boettcher, D. Bonanno, M. Bondì, M. Bongi, S. Bottai, J. Boumaaza, M. Bouta, C. Bozza, R. M. Bozza, F. Bretaudeau, M. Breuhaus, R. Bruijn, J. Brunner, R. Bruno, E. Buis, R. Buompane, B. Caiffi, D. Calvo, E.G.J. van Campenhout, A. Capone, F. Carenini, V. Carretero, T. Cartraud, P. Castaldi, V. Cecchini, S. Celli, M. Chabab, A. Chen, S. Cherubini, M. Chianese, T. Chiarusi, W. Chung, M. Circella, R. Clark, R. Cocimano, J. A. B. Coelho, A. Coleiro, A. Condorelli, R. Coniglione, P. Coyle, A. Creusot, G. Cuttone, R. Dallier, A. De Benedittis, G. De Wasseige, V. Decoene, P. Deguire, I. Del Rosso, L. S. Di Mauro, I. Di Palma, A. F. Díaz, D. Diego-Tortosa, C. Distefano, A. Domi, C. Donzaud, D. Dornic, E. Drakopoulou, D. Drouhin, J.-G. Ducoin, P. Duverne, R. Dvornický, T. Eberl, E. Eckerová, A. Eddymaoui, M. Eff, D. van Eijk, I. El Bojaddaini, S. El Hedri, S. El Mentawi, V. Ellajosyula, A. Enzenhöfer, M. Farino, A. Ferrara, G. Ferrara, M. D. Filipović, F. Filippini, A. Foisseau, D. Franciotti, C. Frosin, L. A. Fusco, T. Gal, J. García Méndez, A. Garcia Soto, C. Gatius Oliver, N. Geißelbrecht, H. Ghaddari, L. Gialanella, B. K. Gibson, E. Giorgio, I. Goos, P. Goswami, S. R. Gozzini, R. Gracia, M. Guelfand, B. Guillon, C. Hanna, H. van Haren, E. Hazelton, A. Heijboer, L. Hennig, J. J. Hernández-Rey, A. Idrissi, W. Idrissi Ibnsalih, G. Illuminati, R. Jaimes, O. Janik, D. Joly, M. de Jong, P. de Jong, B. J. Jung, P. Kalaczyński, G. Kalaitzidakis, C. Karagiannis, U. F. Katz, J. Keegans, T. Khvichia, G. Kistauri, C. Kopper, A. Kouchner, Y. Y. Kovalev, L. Krupa, V. Kueviakoe, V. Kulikovskiy, R. Kvatadze, M. Labalme, R. Lahmann, M. Lamoureux, A. Langella, G. Larosa, C. Lastoria, J. Lazar, G. Lehaut, V. Lemaître, E. Leonora, N. Lessing, G. Levi, I. Lhenry-Yvon, M. Lincetto, M. Lindsey Clark, F. Longhitano, M. Loup, A. Luashvili, S. Madarapu, F. Magnani, V. A. Makeev, L. Malerba, F. Mamedov, P. Mánek, A. Manfreda, A. Manousakis, M. Marconi, A. Margiotta, A. Marinelli, C. Markou, L. Martin, M. Mastrodicasa, S. Mastroianni, J. Mauro, K. C. K. Mehta, G. Miele, P. Migliozzi, E. Migneco, M. L. Mitsou, C. M. Mollo, L. Morales-Gallegos, N. Mori, A. Mosbrugger, A. Moussa, I. Mozun Mateo, S. Mugnier, R. Muller, M. R. Musone, M. Musumeci, S. Navas, C. A. Nicolau, B. Nkosi, B. Ó Fearraigh, V. Oliviero, A. Orlando, E. Oukacha, L. Pacini, D. Paesani, P. Papini, V. Parisi, G. Pascua, B. Pascual-Estrugo, A. M. Păun, G. E. Păvălaš, S. Peña Martínez, M. Perrin-Terrin, V. Pestel, M. Petropavlova, L. Pfeiffer, P. Piattelli, A. Plavin, C. Poirè, V. Poireau, T. Pradier, J. Prado, S. Pulvirenti, N. Randazzo, A. Ratnani, S. Razzaque, I. C. Rea, D. Real, G. Riccobene, J. Robinson, A. Romanov, E. Ros, F. Salesa Greus, D. F. E. Samtleben, A. Sánchez Losa, S. Sanfilippo, M. Sanguineti, D. Santonocito, P. Sapienza, M. Scaringella, M. Scarnera, J. Schnabel, J. Schumann, M. Senniappan, P. A. Sevle Myhr, I. Sgura, R. Shanidze, Y. Shitov, F. Šimkovic, A. Simonelli, A. Sinopoulou, C. Sironneau, M. Spurio, O. Starodubtsev, I. Štekl, D. Stocco, M. Taiuti, Y. Tayalati, J. Tena, H. Thiersen, S. Thoudam, I. Tosta e Melo, B. Trocmé, V. Tsourapis, C. Tully, E. Tzamariudaki, A. Ukleja, A. Vacheret, V. Valsecchi, V. Van Elewyck, G. Vannoye, E. Vannuccini, G. Vasileiadis, F. Vazquez de Sola, A. Veutro, S. Viola, D. Vivolo, A. van Vliet, L. Voorend, E. de Wolf, S. Zavatarelli, D. Zito, J. D. Zornoza, J. Zúñiga

High Energy Physics (Theory)

Bootstrap Cone of the Multicritical Deconfined Quantum Critical Point

Zhijin Li and Tinhong Shen

The deconfined quantum critical point (DQCP) provides a prominent example of the unconventional phase transitions beyond the Landau-Ginzburg-Wilson paradigm and its nature has been controversial for decades. The DQCP has been extensively studied and the results lead to two opposite scenarios with pseudo-criticality or multicriticality. The pseudo-criticality is a prevailing scenario of DQCP which interprets the approximately scale invariant numerical results with the walking behavior near complex fixed points. In contrast, the multicriticality scenario conjectures the DQCP is a unitary fixed point with a relevant $SO(5)$ singlet scalar. In this work we provide substantial evidence for the multicriticality scenario using conformal bootstrap. We start with the observation that the large scale Quantum Monte Carlo (QMC) results nearly saturate the bootstrap bounds. After imposing suitable sparseness condition the bootstrap bound forms a sharp cone in the three-dimensional parameter space. The bootstrap cone is close to the QMC data. We use the navigator algorithm to locate the apex of the cone and extract the extremal solutions. We find striking consistencies between the bootstrap solutions and the fuzzy sphere data of DQCP, including the coefficients in the operator product expansions (OPEs) and the higher spectrum! The bootstrap cone unifies the QMC and the fuzzy sphere data into a unitary conformal field theory with a relevant $SO(5)$ singlet scalar, thus strongly supporting the multicriticality scenario of DQCP. The agreement between the conformal bootstrap, QMC and fuzzy sphere results is a surprise towards solving DQCP and decoding the profound phase diagram of the two-dimensional quantum magnets.
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Lattice Field Theory

Tame the Umklapp Processes in Real-Time Lattice Simulation for Hydrodynamics: An Ising Field Theory Study

Xiaojun Yao

We calculate the real-time symmetric correlation function of the stress-energy tensor for a near-integrable Ising field theory consisting of three stable scalar particles via lattice Hamiltonian simulation. Using classical exact diagonalization and the matrix product state tensor network methods, we find that in the scaling region of the lattice theory, Umklapp processes that break continuum momentum conservation are suppressed and the sound modes of relativistic hydrodynamics emerge at long wavelength and late time in non-equilibrium dynamics. The extracted ratio of bulk viscosity to entropy density is $\zeta/s=3.06\pm 0.68$ and the speed of sound is $c_s/c=0.76 \pm 0.02$ at the temperature $T\approx 7.14$ in units of the lowest stable particle's mass. Our study demonstrates the utility of real-time lattice Hamiltonian simulation for describing hydrodynamization and calculating transport coefficients nonperturbatively.
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