High Energy Astrophysical Phenomena (astro-ph.HE)
Fri, 26 May 2023
1.Charge-Sign Dependent Cosmic-Ray Modulation Observed with the Calorimetric Electron Telescope on the International Space Station
Authors:O. Adriani, Y. Akaike, K. Asano, Y. Asaoka, E. Berti, G. Bigongiari, W. R. Binns, M. Bongi, P. Brogi, A. Bruno, J. H. Buckley, N. Cannady, G. Castellini, C. Checchia, M. L. Cherry, G. Collazuol, G. A. de Nolfo, K. Ebisawa, A. W. Ficklin, H. Fuke, S. Gonzi, T. G. Guzik, T. Hams, K. Hibino, M. Ichimura, K. Ioka, W. Ishizaki, M. H. Israel, K. Kasahara, J. Kataoka, R. Kataoka, Y. Katayose, C. Kato, N. Kawanaka, Y. Kawakubo, K. Kobayashi, K. Kohri, H. S. Krawczynski, J. F. Krizmanic, P. Maestro, P. S. Marrocchesi, A. M. Messineo, J. W. Mitchell, S. Miyake, A. A. Moiseev, M. Mori, N. Mori, H. M. Motz, K. Munakata, S. Nakahira, J. Nishimura, S. Okuno, J. F. Ormes, S. Ozawa, L. Pacini, P. Papini, B. F. Rauch, S. B. Ricciarini, K. Sakai, T. Sakamoto, M. Sasaki, Y. Shimizu, A. Shiomi, P. Spillantini, F. Stolzi, S. Sugita, A. Sulaj, M. Takita, T. Tamura, T. Terasawa, S. Torii, Y. Tsunesada, Y. Uchihori, E. Vannuccini, J. P. Wefel, K. Yamaoka, S. Yanagita, A. Yoshida, K. Yoshida, W. V. Zober
Abstract: We present the observation of a charge-sign dependent solar modulation of galactic cosmic rays (GCRs) with the CALorimetric Electron Telescope onboard the International Space Station over 6 yr, corresponding to the positive polarity of the solar magnetic field. The observed variation of proton count rate is consistent with the neutron monitor count rate, validating our methods for determining the proton count rate. It is observed by the CALorimetric Electron Telescope that both GCR electron and proton count rates at the same average rigidity vary in anticorrelation with the tilt angle of the heliospheric current sheet, while the amplitude of the variation is significantly larger in the electron count rate than in the proton count rate. We show that this observed charge-sign dependence is reproduced by a numerical ``drift model'' of the GCR transport in the heliosphere. This is a clear signature of the drift effect on the long-term solar modulation observed with a single detector.
2.Constraining models for the origin of ultra-high-energy cosmic rays with a novel combined analysis of arrival directions, spectrum, and composition data measured at the Pierre Auger Observatory
Authors:The Pierre Auger Collaboration, A. Abdul Halim, P. Abreu, M. Aglietta, I. Allekotte, K. Almeida Cheminant, A. Almela, R. Aloisio, J. Alvarez-Muñiz, J. Ammerman Yebra, G. A. Anastasi, L. Anchordoqui, B. Andrada, S. Andringa, C. Aramo, P. R. Araújo Ferreira, E. Arnone, J. C. Arteaga Velázquez, H. Asorey, P. Assis, G. Avila, E. Avocone, A. M. Badescu, A. Bakalova, A. Balaceanu, F. Barbato, A. Bartz Mocellin, J. A. Bellido, C. Berat, M. E. Bertaina, G. Bhatta, M. Bianciotto, P. L. Biermann, V. Binet, K. Bismark, T. Bister, J. Biteau, J. Blazek, C. Bleve, J. Blümer, M. Boháčová, D. Boncioli, C. Bonifazi, L. Bonneau Arbeletche, N. Borodai, J. Brack, P. G. Brichetto Orchera, F. L. Briechle, A. Bueno, S. Buitink, M. Buscemi, M. Büsken, A. Bwembya, K. S. Caballero-Mora, L. Caccianiga, I. Caracas, R. Caruso, A. Castellina, F. Catalani, G. Cataldi, L. Cazon, M. Cerda, J. A. Chinellato, J. Chudoba, L. Chytka, R. W. Clay, A. C. Cobos Cerutti, R. Colalillo, A. Coleman, M. R. Coluccia, R. Conceição, A. Condorelli, G. Consolati, M. Conte, F. Convenga, D. Correia dos Santos, P. J. Costa, C. E. Covault, M. Cristinziani, C. S. Cruz Sanchez, S. Dasso, K. Daumiller, B. R. Dawson, R. M. de Almeida, J. de Jesús, S. J. de Jong, J. R. T. de Mello Neto, I. De Mitri, J. de Oliveira, D. de Oliveira Franco, F. de Palma, V. de Souza, E. De Vito, A. Del Popolo, O. Deligny, L. Deval, A. di Matteo, M. Dobre, C. Dobrigkeit, J. C. D'Olivo, L. M. Domingues Mendes, J. C. dos Anjos, R. C. dos Anjos, J. Ebr, F. Ellwanger, M. Emam, R. Engel, I. Epicoco, M. Erdmann, A. Etchegoyen, C. Evoli, H. Falcke, J. Farmer, G. Farrar, A. C. Fauth, N. Fazzini, F. Feldbusch, F. Fenu, A. Fernandes, B. Fick, J. M. Figueira, A. Filipčič, T. Fitoussi, B. Flaggs, T. Fodran, T. Fujii, A. Fuster, C. Galea, C. Galelli, B. García, C. Gaudu, H. Gemmeke, F. Gesualdi, A. Gherghel-Lascu, P. L. Ghia, U. Giaccari, M. Giammarchi, J. Glombitza, F. Gobbi, F. Gollan, G. Golup, M. Gómez Berisso, P. F. Gómez Vitale, J. P. Gongora, J. M. González, N. González, I. Goos, D. Góra, A. Gorgi, M. Gottowik, T. D. Grubb, F. Guarino, G. P. Guedes, E. Guido, S. Hahn, P. Hamal, M. R. Hampel, P. Hansen, D. Harari, V. M. Harvey, A. Haungs, T. Hebbeker, C. Hojvat, J. R. Hörandel, P. Horvath, M. Hrabovský, T. Huege, A. Insolia, P. G. Isar, P. Janecek, J. A. Johnsen, J. Jurysek, A. Kääpä, K. H. Kampert, B. Keilhauer, A. Khakurdikar, V. V. Kizakke Covilakam, H. O. Klages, M. Kleifges, F. Knapp, N. Kunka, B. L. Lago, N. Langner, M. A. Leigui de Oliveira, Y Lema-Capeans, V. Lenok, A. Letessier-Selvon, I. Lhenry-Yvon, D. Lo Presti, L. Lopes, L. Lu, Q. Luce, J. P. Lundquist, A. Machado Payeras, M. Majercakova, D. Mandat, B. C. Manning, P. Mantsch, S. Marafico, F. M. Mariani, A. G. Mariazzi, I. C. Mariş, G. Marsella, D. Martello, S. Martinelli, O. Martínez Bravo, M. A. Martins, M. Mastrodicasa, H. J. Mathes, J. Matthews, G. Matthiae, E. Mayotte, S. Mayotte, P. O. Mazur, G. Medina-Tanco, J. Meinert, D. Melo, A. Menshikov, C. Merx, S. Michal, M. I. Micheletti, L. Miramonti, S. Mollerach, F. Montanet, L. Morejon, C. Morello, A. L. Müller, K. Mulrey, R. Mussa, M. Muzio, W. M. Namasaka, A. Nasr-Esfahani, L. Nellen, G. Nicora, M. Niculescu-Oglinzanu, M. Niechciol, D. Nitz, D. Nosek, V. Novotny, L. Nožka, A Nucita, L. A. Núñez, C. Oliveira, M. Palatka, J. Pallotta, G. Parente, J. Pawlowsky, M. Pech, J. Pękala, R. Pelayo, L. A. S. Pereira, E. E. Pereira Martins, J. Perez Armand, C. Pérez Bertolli, L. Perrone, S. Petrera, C. Petrucci, T. Pierog, M. Pimenta, M. Platino, B. Pont, M. Pothast, M. Pourmohammad Shahvar, P. Privitera, M. Prouza, A. Puyleart, S. Querchfeld, J. Rautenberg, D. Ravignani, M. Reininghaus, J. Ridky, F. Riehn, M. Risse, V. Rizi, W. Rodrigues de Carvalho, E. Rodriguez, J. Rodriguez Rojo, M. J. Roncoroni, S. Rossoni, M. Roth, A. C. Rovero, P. Ruehl, A. Saftoiu, M. Saharan, F. Salamida, H. Salazar, G. Salina, J. D. Sanabria Gomez, F. Sánchez, E. M. Santos, E. Santos, F. Sarazin, R. Sarmento, R. Sato, P. Savina, C. M. Schäfer, V. Scherini, H. Schieler, M. Schimassek, M. Schimp, F. Schlüter, D. Schmidt, O. Scholten, H. Schoorlemmer, P. Schovánek, F. G. Schröder, J. Schulte, T. Schulz, S. J. Sciutto, M. Scornavacche, A. Segreto, S. Sehgal, S. U. Shivashankara, G. Sigl, G. Silli, O. Sima, F. Simon, R. Smau, R. Šmída, P. Sommers, J. F. Soriano, R. Squartini, M. Stadelmaier, D. Stanca, S. Stanič, J. Stasielak, P. Stassi, M. Straub, A. Streich, M. Suárez-Durán, T. Suomijärvi, A. D. Supanitsky, Z. Svozilikova, Z. Szadkowski, A. Tapia, C. Taricco, C. Timmermans, O. Tkachenko, P. Tobiska, C. J. Todero Peixoto, B. Tomé, Z. Torrès, A. Travaini, P. Travnicek, C. Trimarelli, M. Tueros, M. Unger, L. Vaclavek, M. Vacula, J. F. Valdés Galicia, L. Valore, E. Varela, A. Vásquez-Ramírez, D. Veberič, C. Ventura, I. D. Vergara Quispe, V. Verzi, J. Vicha, J. Vink, J. Vlastimil, S. Vorobiov, C. Watanabe, A. A. Watson, A. Weindl, L. Wiencke, H. Wilczyński, D. Wittkowski, B. Wundheiler, B. Yue, A. Yushkov, O. Zapparrata, E. Zas, D. Zavrtanik, M. Zavrtanik
Abstract: The combined fit of the measured energy spectrum and shower maximum depth distributions of ultra-high-energy cosmic rays is known to constrain the parameters of astrophysical models with homogeneous source distributions. Studies of the distribution of the cosmic-ray arrival directions show a better agreement with models in which a fraction of the flux is non-isotropic and associated with the nearby radio galaxy Centaurus A or with catalogs such as that of starburst galaxies. Here, we present a novel combination of both analyses by a simultaneous fit of arrival directions, energy spectrum, and composition data measured at the Pierre Auger Observatory. We find that a model containing a flux contribution from the starburst galaxy catalog of around 20% at 40 EeV with a magnetic field blurring of around $20^\circ$ for a rigidity of 10 EV provides a fair simultaneous description of all three observables. The starburst galaxy model is favored with a significance of $4.5\sigma$ (considering experimental systematic effects) compared to a reference model with only homogeneously distributed background sources. By investigating a scenario with Centaurus A as a single source in combination with the homogeneous background, we confirm that this region of the sky provides the dominant contribution to the observed anisotropy signal. Models containing a catalog of jetted active galactic nuclei whose flux scales with the $\gamma$-ray emission are, however, disfavored as they cannot adequately describe the measured arrival directions.
3.Sensitivity of the Cherenkov Telescope Array to TeV photon emission from the Large Magellanic Cloud
Authors:The Cherenkov Telescope Array Consortium
Abstract: A deep survey of the Large Magellanic Cloud at ~0.1-100TeV photon energies with the Cherenkov Telescope Array is planned. We assess the detection prospects based on a model for the emission of the galaxy, comprising the four known TeV emitters, mock populations of sources, and interstellar emission on galactic scales. We also assess the detectability of 30 Doradus and SN 1987A, and the constraints that can be derived on the nature of dark matter. The survey will allow for fine spectral studies of N157B, N132D, LMC P3, and 30 Doradus C, and half a dozen other sources should be revealed, mainly pulsar-powered objects. The remnant from SN 1987A could be detected if it produces cosmic-ray nuclei with a flat power-law spectrum at high energies, or with a steeper index 2.3-2.4 pending a flux increase by a factor >3-4 over ~2015-2035. Large-scale interstellar emission remains mostly out of reach of the survey if its >10GeV spectrum has a soft photon index ~2.7, but degree-scale 0.1-10TeV pion-decay emission could be detected if the cosmic-ray spectrum hardens above >100GeV. The 30 Doradus star-forming region is detectable if acceleration efficiency is on the order of 1-10% of the mechanical luminosity and diffusion is suppressed by two orders of magnitude within <100pc. Finally, the survey could probe the canonical velocity-averaged cross section for self-annihilation of weakly interacting massive particles for cuspy Navarro-Frenk-White profiles.
4.A spectral-timing study of the inner flow geometry in MAXI J1535--571 with $Insight$-HXMT and NICER
Authors:Wei Yu, Qing-Cui Bu, He-Xin Liu, Yue Huang, Liang Zhang, Zi-Xu Yang, Jin-Lu Qu, Shu Zhang, Li-Ming Song, Shuang-Nan Zhang, Shu-Mei Jia, Xiang Ma, Lian Tao, Ming-Yu Ge, Qing-Zhong Liu, Jing-Zhi Yan, Xue-Lei Cao, Zhi Chang, Li Chen, Yong Chen, Yu-Peng Chen, Guo-Qiang Ding, Ju Guan, Jing Jin, Ling-Da Kong, Bing Li, Cheng-Kui Li, Ti-Pei Li, Xiao-Bo Li, Jin-Yuan Liao, Bai-Sheng Liu, Cong-Zhan Liu, Fang-Jun Lu, Rui-Can Ma, Jian-Yin Nie, Xiao-Qin Ren, Na Sai, Ying Tan, You-Li Tuo, Ling-Jun Wang, Peng-Ju Wang, Bai-Yang Wu, Guang-Cheng Xiao, Qian-Qing Yin, Yuan You, Juan Zhang, Peng Zhang, Wei Zhang, Yue-Xin Zhang, Hai-Sheng Zhao, Shi-Jie Zheng, Deng-Ke Zhou
Abstract: We have performed a spectral-timing analysis on the black hole X-ray binary MAXI J1535--571 during its 2017 outburst, with the aim of exploring the evolution of the inner accretion flow geometry. X-ray reverberation lags are observed in the hard-intermediate state (HIMS) and soft-intermediate state (SIMS) of the outburst. During the HIMS, the characteristic frequency of the reverberation lags $\nu_0$ (the frequency at which the soft lag turns to zero in the lag-frequency spectra) increases when the spectrum softens. This reflects a reduction of the spatial distance between the corona and accretion disc, when assuming the measured time lags are associated with the light travel time. We also find a strong correlation between $\nu_0$ and type-C Quasi Periodic Oscillation (QPO) centroid frequency $\nu_{QPO}$, which can be well explained by the Lense-Thirring (L-T) precession model under a truncated disk geometry. Despite the degeneracy in the spectral modellings, our results suggest that the accretion disc is largely truncated in the low hard state (LHS), and moves inward as the spectrum softens. Combine the spectral modelling results with the $\nu_0$ - $\nu_{QPO}$ evolution, we are inclined to believe that this source probably have a truncated disk geometry in the hard state.
5.The FAST Galactic Plane Pulsar Snapshot Survey: IV. Timing results of 30 FAST-GPPS discovered pulsars
Authors:W. Q. Su, J. L. Han, P. F. Wang, J. P. Yuan, Chen Wang, D. J. Zhou, Tao Wang, Yi Yan, W. C. Jing, Z. L. Yang, N. N. Cai, Xue Chen, Jun Xu, Lang Xie, H. G. Wang, R. X. Xu, X. P. You
Abstract: Timing observations are crucial for determining the physical properties of newly discovered pulsars. Using the L-band 19-beam receiver of the Five-hundred-meter Aperture Spherical radio Telescope (FAST), the FAST Galactic Plane Pulsar Snapshot (GPPS) survey has discovered many faint and weak pulsars, which are hardly detected using other radio telescopes in limited observation time. To obtain accurate position, spin parameters, dispersion measure, and to calculate derived parameters such as characteristic age and surface magnetic fields, we collect available FAST pulsar data obtained either through targeted following-up observations or coincidental survey observations with one of the 19 beams of the L-band 19-beam receiver. From these data we get the time of arrival (TOA) measurements for 30 newly discovered pulsars as well as 13 known pulsars. We demonstrate that TOA measurements from any beams of the L-band 19-beam receiver acquired through any FAST observation mode (e.g., the tracking mode or the snapshot mode) can be combined together for getting timing solutions. We update the ephemeris of 13 previously known pulsars and obtained the first phase-coherent timing results for 30 isolated pulsars discovered in the FAST GPPS survey. Notably, PSR J1904+0853 is an isolated millisecond pulsar, PSR J1906+0757 is a disrupted recycled pulsar, and PSR J1856+0211 is a long-period pulsar that can constrain pulsar death lines. Based on these timing solutions, all available FAST data can be added together to get the best pulse profiles.
6.Particle acceleration with Magnetic Reconnection in large scale RMHD simulations: I. Current sheet identification and characterization
Authors:Matteo Nurisso, Annalisa Celotti, Andrea Mignone, Gianluigi Bodo
Abstract: We present a new algorithm for the identification and physical characterization of current sheets and reconnection sites in 2D and 3D large scale relativisticmagnetohydrodynamic numerical simulations. This has been implemented in the PLUTO code and tested in the cases of a single current sheet, a 2D jet and a 3D unstable plasma column. Its main features are: a) a computational cost which allows its use in large scale simulations; b) the capability to deal with complex 2D and 3D structures of the reconnection sites. In the performed simulations, we identify the computational cells that are part of a current sheet by a measure of the gradient of the magnetic field along different directions. Lagrangian particles, which follow the fluid, are used to sample plasma parameters before entering the reconnection sites that form during the evolution of the different configurations considered. Specifically, we track the distributions of the magnetization parameter $\sigma$ and the thermal to magnetic pressure ratio $\beta$ that - according to particle-in-cell simulation results - control the properties of particle acceleration in magnetic reconnection regions. Despite the initial conditions of the simulations were not chosen "ad hoc", the 3D simulation returns results suitable for efficient particle acceleration and realistic non-thermal particle distributions.
7.QCD, Gravitational Waves, and Pulsars
Authors:Partha Bagchi, Oindrila Ganguly, Biswanath Layek, Anjishnu Sarkar, Ajit M. Srivastava
Abstract: Investigations of the phase diagram of quantum chromodynamics (QCD) have revealed that exotic new phases, the so called {\it color superconducting phases}, may arise at very high baryon densities. It is speculated that these exotic phases may arise in the cores of neutron stars. Focus on neutrons stars has tremendously intensified in recent years with the direct detection of gravitational waves (GW) by LIGO/Virgo from BNS merger events which has allowed the possibility of directly probing the properties of the interior of a neutron star. A remarkable phenomenon manifested by rapidly rotating neutron stars is in their {\it avatar} as {\it Pulsars}. The accuracy of pulsar timing can reach the level of one part in 10$^{15}$, comparable to that of atomic clocks. This suggests that even a tiny deformation of the pulsar can leave its imprints on the pulses by inducing tiny perturbations in the entire moment of inertia (MI) tensor affecting the pulse timings, as well as the pulse profile (from wobbling induced by off-diagonal MI components). This may allow a new probe of various phase transitions occurring inside a pulsar core through induced density fluctuations affecting the MI tensor. Such perturbations also naturally induce a rapidly changing quadrupole moment of the star, thereby providing a new source of gravitational wave emission. Another remarkable possibility arises when we consider the effect of an external GW on neutron star. With the possibility of detecting any minute changes in its configuration through pulse observations, the neutron star has the potential of performing as a Weber detector of gravitational wave. This brief review will focus on these specific aspects of a pulsar. Specifically, the focus will be on the type of physics which can be probed by utilizing the effect of changes in the MI tensor of the pulsar on pulse properties.
8.The First LHAASO Catalog of Gamma-Ray Sources
Authors:Zhen Cao The LHAASO Collaboration, F. Aharonian The LHAASO Collaboration, Q. An The LHAASO Collaboration, Axikegu The LHAASO Collaboration, Y. X. Bai The LHAASO Collaboration, Y. W. Bao The LHAASO Collaboration, D. Bastieri The LHAASO Collaboration, X. J. Bi The LHAASO Collaboration, Y. J. Bi The LHAASO Collaboration, J. T. Cai The LHAASO Collaboration, Q. Cao The LHAASO Collaboration, W. Y. Cao The LHAASO Collaboration, Zhe Cao The LHAASO Collaboration, J. Chang The LHAASO Collaboration, J. F. Chang The LHAASO Collaboration, A. M. Chen The LHAASO Collaboration, E. S. Chen The LHAASO Collaboration, Liang Chen The LHAASO Collaboration, Lin Chen The LHAASO Collaboration, Long Chen The LHAASO Collaboration, M. J. Chen The LHAASO Collaboration, M. L. Chen The LHAASO Collaboration, Q. H. Chen The LHAASO Collaboration, S. H. Chen The LHAASO Collaboration, S. Z. Chen The LHAASO Collaboration, T. L. Chen The LHAASO Collaboration, Y. Chen The LHAASO Collaboration, N. Cheng The LHAASO Collaboration, Y. D. Cheng The LHAASO Collaboration, M. Y. Cui The LHAASO Collaboration, S. W. Cui The LHAASO Collaboration, X. H. Cui The LHAASO Collaboration, Y. D. Cui The LHAASO Collaboration, B. Z. Dai The LHAASO Collaboration, H. L. Dai The LHAASO Collaboration, Z. G. Dai The LHAASO Collaboration, Danzengluobu The LHAASO Collaboration, D. della Volpe The LHAASO Collaboration, X. Q. Dong The LHAASO Collaboration, K. K. Duan The LHAASO Collaboration, J. H. Fan The LHAASO Collaboration, Y. Z. Fan The LHAASO Collaboration, J. Fang The LHAASO Collaboration, K. Fang The LHAASO Collaboration, C. F. Feng The LHAASO Collaboration, L. Feng The LHAASO Collaboration, S. H. Feng The LHAASO Collaboration, X. T. Feng The LHAASO Collaboration, Y. L. Feng The LHAASO Collaboration, S. Gabici The LHAASO Collaboration, B. Gao The LHAASO Collaboration, C. D. Gao The LHAASO Collaboration, L. Q. Gao The LHAASO Collaboration, Q. Gao The LHAASO Collaboration, W. Gao The LHAASO Collaboration, W. K. Gao The LHAASO Collaboration, M. M. Ge The LHAASO Collaboration, L. S. Geng The LHAASO Collaboration, G. Giacinti The LHAASO Collaboration, G. H. Gong The LHAASO Collaboration, Q. B. Gou The LHAASO Collaboration, M. H. Gu The LHAASO Collaboration, F. L. Guo The LHAASO Collaboration, X. L. Guo The LHAASO Collaboration, Y. Q. Guo The LHAASO Collaboration, Y. Y. Guo The LHAASO Collaboration, Y. A. Han The LHAASO Collaboration, H. H. He The LHAASO Collaboration, H. N. He The LHAASO Collaboration, J. Y. He The LHAASO Collaboration, X. B. He The LHAASO Collaboration, Y. He The LHAASO Collaboration, M. Heller The LHAASO Collaboration, Y. K. Hor The LHAASO Collaboration, B. W. Hou The LHAASO Collaboration, C. Hou The LHAASO Collaboration, X. Hou The LHAASO Collaboration, H. B. Hu The LHAASO Collaboration, Q. Hu The LHAASO Collaboration, S. C. Hu The LHAASO Collaboration, D. H. Huang The LHAASO Collaboration, T. Q. Huang The LHAASO Collaboration, W. J. Huang The LHAASO Collaboration, X. T. Huang The LHAASO Collaboration, X. Y. Huang The LHAASO Collaboration, Y. Huang The LHAASO Collaboration, Z. C. Huang The LHAASO Collaboration, X. L. Ji The LHAASO Collaboration, H. Y. Jia The LHAASO Collaboration, K. Jia The LHAASO Collaboration, K. Jiang The LHAASO Collaboration, X. W. Jiang The LHAASO Collaboration, Z. J. Jiang The LHAASO Collaboration, M. Jin The LHAASO Collaboration, M. M. Kang The LHAASO Collaboration, T. Ke The LHAASO Collaboration, D. Kuleshov The LHAASO Collaboration, K. Kurinov The LHAASO Collaboration, B. B. Li The LHAASO Collaboration, Cheng Li The LHAASO Collaboration, Cong Li The LHAASO Collaboration, D. Li The LHAASO Collaboration, F. Li The LHAASO Collaboration, H. B. Li The LHAASO Collaboration, H. C. Li The LHAASO Collaboration, H. Y. Li The LHAASO Collaboration, J. Li The LHAASO Collaboration, Jian Li The LHAASO Collaboration, Jie Li The LHAASO Collaboration, K. Li The LHAASO Collaboration, W. L. Li The LHAASO Collaboration, W. L. Li The LHAASO Collaboration, X. R. Li The LHAASO Collaboration, Xin Li The LHAASO Collaboration, Y. Z. Li The LHAASO Collaboration, Zhe Li The LHAASO Collaboration, Zhuo Li The LHAASO Collaboration, E. W. Liang The LHAASO Collaboration, Y. F. Liang The LHAASO Collaboration, S. J. Lin The LHAASO Collaboration, B. Liu The LHAASO Collaboration, C. Liu The LHAASO Collaboration, D. Liu The LHAASO Collaboration, H. Liu The LHAASO Collaboration, H. D. Liu The LHAASO Collaboration, J. Liu The LHAASO Collaboration, J. L. Liu The LHAASO Collaboration, J. Y. Liu The LHAASO Collaboration, M. Y. Liu The LHAASO Collaboration, R. Y. Liu The LHAASO Collaboration, S. M. Liu The LHAASO Collaboration, W. Liu The LHAASO Collaboration, Y. Liu The LHAASO Collaboration, Y. N. Liu The LHAASO Collaboration, R. Lu The LHAASO Collaboration, Q. Luo The LHAASO Collaboration, H. K. Lv The LHAASO Collaboration, B. Q. Ma The LHAASO Collaboration, L. L. Ma The LHAASO Collaboration, X. H. Ma The LHAASO Collaboration, J. R. Mao The LHAASO Collaboration, Z. Min The LHAASO Collaboration, W. Mitthumsiri The LHAASO Collaboration, H. J. Mu The LHAASO Collaboration, Y. C. Nan The LHAASO Collaboration, A. Neronov The LHAASO Collaboration, Z. W. Ou The LHAASO Collaboration, B. Y. Pang The LHAASO Collaboration, P. Pattarakijwanich The LHAASO Collaboration, Z. Y. Pei The LHAASO Collaboration, M. Y. Qi The LHAASO Collaboration, Y. Q. Qi The LHAASO Collaboration, B. Q. Qiao The LHAASO Collaboration, J. J. Qin The LHAASO Collaboration, D. Ruffolo The LHAASO Collaboration, A. Sáiz The LHAASO Collaboration, D. Semikoz The LHAASO Collaboration, C. Y. Shao The LHAASO Collaboration, L. Shao The LHAASO Collaboration, O. Shchegolev The LHAASO Collaboration, X. D. Sheng The LHAASO Collaboration, F. W. Shu The LHAASO Collaboration, H. C. Song The LHAASO Collaboration, Yu. V. Stenkin The LHAASO Collaboration, V. Stepanov The LHAASO Collaboration, Y. Su The LHAASO Collaboration, Q. N. Sun The LHAASO Collaboration, X. N. Sun The LHAASO Collaboration, Z. B. Sun The LHAASO Collaboration, P. H. T. Tam The LHAASO Collaboration, Q. W. Tang The LHAASO Collaboration, Z. B. Tang The LHAASO Collaboration, W. W. Tian The LHAASO Collaboration, C. Wang The LHAASO Collaboration, C. B. Wang The LHAASO Collaboration, G. W. Wang The LHAASO Collaboration, H. G. Wang The LHAASO Collaboration, H. H. Wang The LHAASO Collaboration, J. C. Wang The LHAASO Collaboration, K. Wang The LHAASO Collaboration, L. P. Wang The LHAASO Collaboration, L. Y. Wang The LHAASO Collaboration, P. H. Wang The LHAASO Collaboration, R. Wang The LHAASO Collaboration, W. Wang The LHAASO Collaboration, X. G. Wang The LHAASO Collaboration, X. Y. Wang The LHAASO Collaboration, Y. Wang The LHAASO Collaboration, Y. D. Wang The LHAASO Collaboration, Y. J. Wang The LHAASO Collaboration, Z. H. Wang The LHAASO Collaboration, Z. X. Wang The LHAASO Collaboration, Zhen Wang The LHAASO Collaboration, Zheng Wang The LHAASO Collaboration, D. M. Wei The LHAASO Collaboration, J. J. Wei The LHAASO Collaboration, Y. J. Wei The LHAASO Collaboration, T. Wen The LHAASO Collaboration, C. Y. Wu The LHAASO Collaboration, H. R. Wu The LHAASO Collaboration, S. Wu The LHAASO Collaboration, X. F. Wu The LHAASO Collaboration, Y. S. Wu The LHAASO Collaboration, S. Q. Xi The LHAASO Collaboration, J. Xia The LHAASO Collaboration, J. J. Xia The LHAASO Collaboration, G. M. Xiang The LHAASO Collaboration, D. X. Xiao The LHAASO Collaboration, G. Xiao The LHAASO Collaboration, G. G. Xin The LHAASO Collaboration, Y. L. Xin The LHAASO Collaboration, Y. Xing The LHAASO Collaboration, Z. Xiong The LHAASO Collaboration, D. L. Xu The LHAASO Collaboration, R. F. Xu The LHAASO Collaboration, R. X. Xu The LHAASO Collaboration, W. L. Xu The LHAASO Collaboration, L. Xue The LHAASO Collaboration, D. H. Yan The LHAASO Collaboration, J. Z. Yan The LHAASO Collaboration, T. Yan The LHAASO Collaboration, C. W. Yang The LHAASO Collaboration, F. Yang The LHAASO Collaboration, F. F. Yang The LHAASO Collaboration, H. W. Yang The LHAASO Collaboration, J. Y. Yang The LHAASO Collaboration, L. L. Yang The LHAASO Collaboration, M. J. Yang The LHAASO Collaboration, R. Z. Yang The LHAASO Collaboration, S. B. Yang The LHAASO Collaboration, Y. H. Yao The LHAASO Collaboration, Z. G. Yao The LHAASO Collaboration, Y. M. Ye The LHAASO Collaboration, L. Q. Yin The LHAASO Collaboration, N. Yin The LHAASO Collaboration, X. H. You The LHAASO Collaboration, Z. Y. You The LHAASO Collaboration, Y. H. Yu The LHAASO Collaboration, Q. Yuan The LHAASO Collaboration, H. Yue The LHAASO Collaboration, H. D. Zeng The LHAASO Collaboration, T. X. Zeng The LHAASO Collaboration, W. Zeng The LHAASO Collaboration, M. Zha The LHAASO Collaboration, B. B. Zhang The LHAASO Collaboration, F. Zhang The LHAASO Collaboration, H. M. Zhang The LHAASO Collaboration, H. Y. Zhang The LHAASO Collaboration, J. L. Zhang The LHAASO Collaboration, L. X. Zhang The LHAASO Collaboration, Li Zhang The LHAASO Collaboration, P. F. Zhang The LHAASO Collaboration, P. P. Zhang The LHAASO Collaboration, R. Zhang The LHAASO Collaboration, S. B. Zhang The LHAASO Collaboration, S. R. Zhang The LHAASO Collaboration, S. S. Zhang The LHAASO Collaboration, X. Zhang The LHAASO Collaboration, X. P. Zhang The LHAASO Collaboration, Y. F. Zhang The LHAASO Collaboration, Yi Zhang The LHAASO Collaboration, Yong Zhang The LHAASO Collaboration, B. Zhao The LHAASO Collaboration, J. Zhao The LHAASO Collaboration, L. Zhao The LHAASO Collaboration, L. Z. Zhao The LHAASO Collaboration, S. P. Zhao The LHAASO Collaboration, F. Zheng The LHAASO Collaboration, B. Zhou The LHAASO Collaboration, H. Zhou The LHAASO Collaboration, J. N. Zhou The LHAASO Collaboration, M. Zhou The LHAASO Collaboration, P. Zhou The LHAASO Collaboration, R. Zhou The LHAASO Collaboration, X. X. Zhou The LHAASO Collaboration, C. G. Zhu The LHAASO Collaboration, F. R. Zhu The LHAASO Collaboration, H. Zhu The LHAASO Collaboration, K. J. Zhu The LHAASO Collaboration, X. Zuo. The LHAASO Collaboration
Abstract: We present the first catalog of very-high energy and ultra-high energy $\gamma$-ray sources detected by the Large High Altitude Air Shower Observatory (LHAASO), using 508 days of data collected by the Water Cherenkov Detector Array (WCDA) from March 2021 to September 2022 and 933 days of data recorded by the Kilometer Squared Array (KM2A) from January 2020 to September 2022. This catalog represents the most sensitive $E > 1$ TeV gamma-ray survey of the sky covering declination from $-$20$^{\circ}$ to 80$^{\circ}$. In total, the catalog contains 90 sources with extended size smaller than $2^\circ$ and with significance of detection at $> 5\sigma$. For each source, we provide its position, extension and spectral characteristics. Furthermore, based on our source association criteria, 32 new TeV sources are proposed in this study. Additionally, 43 sources are detected with ultra-high energy ($E > 100$ TeV) emission at $> 4\sigma$ significance level.
9.K2 Optical Emission from OJ 287 and Other Gamma-Ray Blazars on Hours-to-Weeks Timescales from 2014-2018
Authors:Ann E. Wehrle Space Science Institute, Michael Carini Western Kentucky University, Paul J. Wiita The College of New Jersey, Joshua Pepper Lehigh University, B. Scott Gaudi The Ohio State University, Richard W. Pogge The Ohio State Univserity, Keivan G. Stassun Vanderbilt University, Steven Villaneuva, Jr. NASA Goddard Space Flight Center
Abstract: We present second observations by K2 of OJ~287 and 7 other $\gamma$-ray AGNs obtained in 2017-2018, second and third observations of the lobe-dominated, steep spectrum quasar 3C~207, and observations of 9 additional blazars not previously observed with K2. The AGN were observed simultaneously with K2 and the Fermi Large Area Telescope for 51-81 days. Our full sample, observed in 2014-2018, contained 16 BL Lac objects (BL Lacs), 9 Flat Spectrum Radio Quasars (FSRQs), and 4 other $\gamma$-ray AGNs. Twelve BL Lacs and 7 FSRQs exhibited fast, jagged light curves while 4 BL Lacs and 2 FSRQs had slow, smooth light curves. Some objects changed their red-noise character significantly between repeated K2 observations. The optical characteristics of OJ~287 derived from the short-cadence K2 light curves changed between observations made before and after the predicted passage of the suspected secondary supermassive black hole through the accretion disk of the primary supermassive black hole. The average slopes of the periodogram power spectral densities of the BL Lacs' and FSRQs' light curves differed significantly, by $\approx 12$\%, with the BL Lac slopes being steeper, and a KS test with a $p$-value of 0.039 indicates that these samples probably come from different populations; however, this result is not as strongly supported by PSRESP analyses. Differences in the origin of the jets from the ergosphere or accretion disk in these two classes could produce such a disparity, as could different sizes or locations of emission regions within the jets.
10.Sun is a cosmic ray TeVatron
Authors:Prabir Banik, Arunava Bhadra, Sanjay K. Ghosh
Abstract: Very recently, HAWC observatory discovered the high-energy gamma ray emission from the solar disk during the quiescent stage of the sun, extending the Fermi-LAT detection of intense, hard emission between 0.1 - 200 GeV to TeV energies. The flux of these observed gamma-rays is significantly higher than that theoretically expected from hadronic interactions of galactic cosmic rays with the solar atmosphere. More importantly, spectral slope of Fermi and HAWC observed gamma ray energy spectra differ significantly from that of galactic cosmic rays casting doubt on the prevailing galactic cosmic ray ancestry model of solar disk gamma rays. In this letter, we argue that the quiet sun can accelerate cosmic rays to TeV energies with an appropriate flux level in the solar chromosphere, as the solar chromosphere in its quiet state probably possesses the required characteristics to accelerate cosmic rays to TeV energies. Consequently, the mystery of the origin of observed gamma rays from the solar disc can be resolved consistently through the hadronic interaction of these cosmic rays with solar matter above the photosphere in a quiet state. The upcoming IceCube-Gen2 detector should be able to validate the proposed model in future through observation of TeV muon neutrino flux from the solar disk. The proposed idea should have major implications on the origin of galactic cosmic rays.
11.Monte Carlo Radiation Transport for Astrophysical Transients Powered by Circumstellar Interaction
Authors:Gururaj A. Wagle, Emmanouil Chatzopoulos, Ryan Wollaeger, Christopher J. Fontes
Abstract: In this paper, we introduce \texttt{SuperLite}, an open-source Monte Carlo radiation transport code designed to produce synthetic spectra for astrophysical transient phenomena affected by circumstellar interaction. \texttt{SuperLite} utilizes Monte Carlo methods for semi-implicit, semi-relativistic radiation transport in high-velocity shocked outflows, employing multi-group structured opacity calculations. The code enables rapid post-processing of hydrodynamic profiles to generate high-quality spectra that can be compared with observations of transient events, including superluminous supernovae, pulsational pair-instability supernovae, and other peculiar transients. We present the methods employed in \texttt{SuperLite} and compare the code's performance to that of other radiative transport codes, such as \texttt{SuperNu} and CMFGEN. We show that \texttt{SuperLite} has successfully passed standard Monte Carlo radiation transport tests and can reproduce spectra of typical supernovae of Type Ia, Type IIP and Type IIn.
12.Dynamical friction in dark matter spikes: corrections to Chandrasekhar's formula
Authors:Fani Dosopoulou
Abstract: We consider the intermediate mass-ratio inspiral of a stellar-mass compact object with an intermediate-mass black hole that is surrounded by a dark matter density spike. The interaction of the inspiraling black hole with the dark matter particles in the spike leads to dynamical friction. This can alter the dynamics of the black hole binary, leaving an imprint on the gravitational wave signal. Previous calculations did not include in the evaluation of the dynamical friction coefficient the contribution from particles that move faster than the black hole. This term is neglected in the standard Chandrasekhar's treatment where only slower moving particles contribute to the decelerating drag. Here, we demonstrate that dynamical friction produced by the fast moving particles has a significant effect on the evolution of a massive binary within a dark matter spike. For a density profile $\rho\propto r^{-\gamma}$ with $\gamma\lesssim 1$, the dephasing of the gravitational waveform can be several orders of magnitude larger than estimated using the standard treatment. As $\gamma$ approaches $0.5$ the error becomes arbitrarily large. Finally, we show that dynamical friction tends to make the orbit more eccentric for any $\gamma < 1.8$. However, energy loss by gravitational wave radiation is expected to dominate the inspiral, leading to orbital circularization in most cases.