Descriptor: "pulsar" / Database: OpenAIRE - Searchworks@Jio Institute Digital Library Search Results

Your search keyword '"pulsar"' showing total 16,823 results

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16,823 results on '"pulsar"'

1. Practical approaches to analyzing PTA data: Cosmic strings with six pulsars

Author: Leclere, Hippolyte Quelquejay, Auclair, Pierre, Babak, Stanislav, Chalumeau, Aurélien, Steer, Danièle A., Antoniadis, J., Nielsen, A. -S. Bak, Bassa, C. G., Berthereau, A., Bonetti, M., Bortolas, E., Brook, P. R., Burgay, M., Caballero, R. N., Champion, D. J., Chanlaridis, S., Chen, S., Cognard, I., Desvignes, G., Falxa, M., Ferdman, R. D., Franchini, A., Gair, J. R., Goncharov, B., Graikou, E., Grießmeier, J. -M., Guillemot, L., Guo, Y. J., Hu, H., Iraci, F., Izquierdo-Villalba, D., Jang, J., Jawor, J., Janssen, G. H., Jessner, A., Karuppusamy, R., Keane, E. F., Keith, M. J., Kramer, M., Krishnakumar, M. A., Lackeos, K., Lee, K. J., Liu, K., Liu, Y., Lyne, A. G., McKee, J. W., Main, R. A., Mickaliger, M. B., Niţu, I. C., Parthasarathy, A., Perera, B. B. P., Perrodin, D., Petiteau, A., Porayko, N. K., Possenti, A., Samajdar, A., Sanidas, S. A., Sesana, A., Shaifullah, G., Speri, L., Spiewak, R., Stappers, B. W., Susarla, S. C., Theureau, G., Tiburzi, C., van der Wateren, E., Vecchio, A., Krishnan, V. Venkatraman, Verbiest, J. P. W., Wang, J., Wang, L., Wu, Z., AstroParticule et Cosmologie (APC (UMR_7164)), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité), Laboratoire de Physique et Chimie de l'Environnement et de l'Espace (LPC2E), Observatoire des Sciences de l'Univers en région Centre (OSUC), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université d'Orléans (UO)-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université d'Orléans (UO)-Centre National de la Recherche Scientifique (CNRS)-Centre National d’Études Spatiales [Paris] (CNES), Unité Scientifique de la Station de Nançay (USN), Université Paris sciences et lettres (PSL)-Université d'Orléans (UO)-Centre National de la Recherche Scientifique (CNRS), Institut de Recherches sur les lois Fondamentales de l'Univers (IRFU), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay, Laboratoire Univers et Théories (LUTH (UMR_8102)), and EPTA
Subjects: High Energy Physics - Theory, kink, binary: mass, noise, data analysis method, Cosmology and Nongalactic Astrophysics (astro-ph.CO), gravitational radiation: stochastic, string tension, gravitational radiation: background, FOS: Physical sciences, statistical analysis: Bayesian, General Relativity and Quantum Cosmology (gr-qc), parametric, General Relativity and Quantum Cosmology, High Energy Physics - Theory (hep-th), black hole: binary, [PHYS.GRQC]Physics [physics]/General Relativity and Quantum Cosmology [gr-qc], string: closed, string model, simplex, Astrophysics - Cosmology and Nongalactic Astrophysics, cosmic string: network, pulsar
Abstract: We search for a stochastic gravitational wave background (SGWB) generated by a network of cosmic strings using six millisecond pulsars from Data Release 2 (DR2) of the European Pulsar Timing Array (EPTA). We perform a Bayesian analysis considering two models for the network of cosmic string loops, and compare it to a simple power-law model which is expected from the population of supermassive black hole binaries. Our main strong assumption is that the previously reported common red noise process is a SGWB. We find that the one-parameter cosmic string model is slightly favored over a power-law model thanks to its simplicity. If we assume a two-component stochastic signal in the data (supermassive black hole binary population and the signal from cosmic strings), we get a $95\%$ upper limit on the string tension of $\log_{10}(Gμ) < -9.9$ ($-10.5$) for the two cosmic string models we consider. In extended two-parameter string models, we were unable to constrain the number of kinks. We test two approximate and fast Bayesian data analysis methods against the most rigorous analysis and find consistent results. These two fast and efficient methods are applicable to all SGWBs, independent of their source, and will be crucial for analysis of extended data sets., 13 pages, 5 figures
Published: 2023

2. Observations of the Crab Nebula and Pulsar with the Large-Sized Telescope Prototype of the Cherenkov Telescope Array

Author: Project, CTA-LST, Abe, H., Abe, K., Abe, S., Aguasca-Cabot, A., Agudo, I., Crespo, N. Alvarez, Antonelli, L. A., Aramo, C., Arbet-Engels, A., Arcaro, C., Artero, M., Asano, K., Aubert, P., Baktash, A., Bamba, A., Larriva, A. Baquero, Baroncelli, L., de Almeida, U. Barres, Barrio, J. A., Batkovic, I., Baxter, J., González, J. Becerra, Bernardini, E., Bernardos, M. I., Medrano, J. Bernete, Berti, A., Bhattacharjee, P., Biederbeck, N., Bigongiari, C., Bissaldi, E., Blanch, O., Bonnoli, G., Bordas, P., Borghese, A., Bulgarelli, A., Burelli, I., Buscemi, M., Cardillo, M., Caroff, S., Carosi, A., Cassol, F., Cauz, D., Ceribella, G., Chai, Y., Cheng, K., Chiavassa, A., Chikawa, M., Chytka, L., Cifuentes, A., Contreras, J. L., Cortina, J., Costantini, H., D'Amico, G., Dalchenko, M., De Angelis, A., de Lavergne, M. de Bony, De Lotto, B., de Menezes, R., Deleglise, G., Delgado, C., Mengual, J. Delgado, della Volpe, D., Dellaiera, M., Depaoli, D., Di Piano, A., Di Pierro, F., Di Tria, R., Di Venere, L., Díaz, C., Dominik, R. M., Prester, D. Dominis, Donini, A., Dorner, D., Doro, M., Elsässer, D., Emery, G., Escudero, J., Ramazani, V. Fallah, Ferrara, G., Ferrarotto, F., Fiasson, A., Coromina, L. Freixas, Fröse, S., Fukami, S., Fukazawa, Y., Garcia, E., López, R. Garcia, Gasbarra, C., Gasparrini, D., Geyer, F., Paiva, J. Giesbrecht, Giglietto, N., Giordano, F., Giro, E., Gliwny, P., Godinovic, N., Grau, R., Green, D., Green, J., Gunji, S., Hackfeld, J., Hadasch, D., Hahn, A., Hashiyama, K., Hassan, T., Hayashi, K., Heckmann, L., Heller, M., Llorente, J. Herrera, Hirotani, K., Hoffmann, D., Horns, D., Houles, J., Hrabovsky, M., Hrupec, D., Hui, D., Hütten, M., Iarlori, M., Imazawa, R., Inada, T., Inome, Y., Ioka, K., Iori, M., Ishio, K., Iwamura, Y., Jacquemont, M., Martinez, I. Jimenez, Jurysek, J., Kagaya, M., Karas, V., Katagiri, H., Kataoka, J., Kerszberg, D., Kobayashi, Y., Kong, A., Kubo, H., Kushida, J., Lainez, M., Lamanna, G., Lamastra, A., Flour, T. Le, Linhoff, M., Longo, F., López-Coto, R., López-Moya, M., López-Oramas, A., Loporchio, S., Lorini, A., Luque-Escamilla, P. L., Majumdar, P., Makariev, M., Mandat, D., Manganaro, M., Manicò, G., Mannheim, K., Mariotti, M., Marquez, P., Marsella, G., Martí, J., Martinez, O., Martínez, G., Martínez, M., Marusevec, P., Mas-Aguilar, A., Maurin, G., Mazin, D., Guillen, E. Mestre, Micanovic, S., Miceli, D., Miener, T., Miranda, J. M., Mirzoyan, R., Mizuno, T., Gonzalez, M. Molero, Molina, E., Montaruli, T., Monteiro, I., Moralejo, A., Morcuende, D., Morselli, A., Mrakovcic, K., Murase, K., Nagai, A., Nagataki, S., Nakamori, T., Nickel, L., Nievas, M., Nishijima, K., Noda, K., Nosek, D., Nozaki, S., Ohishi, M., Ohtani, Y., Oka, T., Okazaki, N., Okumura, A., Orito, R., Otero-Santos, J., Palatiello, M., Paneque, D., Pantaleo, F. R., Paoletti, R., Paredes, J. M., Pech, M., Pecimotika, M., Peresano, M., Pérez, A., Pietropaolo, E., Pirola, G., Plard, C., Podobnik, F., Poireau, V., Polo, M., Pons, E., Prandini, E., Prast, J., Principe, G., Priyadarshi, C., Prouza, M., Rando, R., Rhode, W., Ribó, M., Rizi, V., Fernandez, G. Rodriguez, Ruiz, J. E., Saito, T., Sakurai, S., Sanchez, D. A., Šarić, T., Sato, Y., Saturni, F. G., Schleicher, B., Schmuckermaier, F., Schubert, J. L., Schussler, F., Schweizer, T., Arroyo, M. Seglar, Silvia, R., Sitarek, J., Sliusar, V., Spolon, A., Strišković, J., Strzys, M., Suda, Y., Sunada, Y., Tajima, H., Takahashi, H., Takahashi, M., Takata, J., Takeishi, R., Tam, P. H. T., Tanaka, S. J., Tateishi, D., Tejedor, L. A., Temnikov, P., Terada, Y., Terauchi, K., Terzic, T., Teshima, M., Tluczykont, M., Tokanai, F., Torres, D. F., Travnicek, P., Truzzi, S., Tutone, A., Uhlrich, G., Vacula, M., Vallania, P., van Scherpenberg, J., Acosta, M. Vázquez, Verguilov, V., Viale, I., Vigliano, A., Vigorito, C. F., Vitale, V., Voutsinas, G., Vovk, I., Vuillaume, T., Walter, R., Will, M., Yamamoto, T., Yamazaki, R., Yoshida, T., Yoshikoshi, T., Zywucka, N., Bernloehr, K., Gueta, O., Kosack, K., Maier, G., Watson, J., Rijeka, University of, Physics, Department of, Rijeka, Croatia, Physics, Institute for Theoretical, Astrophysics, Würzburg, Universität, Nord, Campus Hubland, Würzburg, Germany, Physik, Institut für Theoretische, IV, Lehrstuhl, Plasma-Astroteilchenphysik, Bochum, Ruhr-Universität, Bochum, La Sapienza, INFN Sezione di Roma, Rome, Italy, ILANCE, Laboratory, CNRS - University of Tokyo International Research, Kashiwa, Chiba, Japan, Program, Physics, Science, Graduate School of Advanced, Engineering, University, Hiroshima, Hiroshima, Vergata, INFN Sezione di Roma Tor, Physics, Faculty of, Informatics, Applied, Lodz, University of, Lodz, Poland, Split, University of, FESB, Split, University, Yamagata, Yamagata, University, Tohoku, Institute, Astronomical, Aobaku, Sendai, Osijek, Josip Juraj Strossmayer University of, Osijek, dell'Aquila, INFN Dipartimento di Scienze Fisiche e Chimiche - Università degli Studi, Institute, Gran Sasso Science, L'Aquila, Oiwakecho, Kitashirakawa, Kyoto, Astronomy, Department of, Geneva, University of, Versoix, Switzerland, Sciences, Astronomical Institute of the Czech Academy of, Prague, Republic, Czech, Science, Faculty of, University, Ibaraki, Mito, Ibaraki, University, Waseda, Shinjuku, Tokyo, di Trieste, INFN Sezione, di Trieste, Università degli Studi, Trieste, INFN, di Siena, Università degli Studi, Fisiche, Dipartimento di Scienze, dell'Ambiente, della Terra e, di Fisica, Sezione, Siena, de Jaén, Escuela Politécnica Superior, de Jaén, Universidad, Lagunillas, Campus Las, Jaén, Spain, Physics, Saha Institute of Nuclear, Bidhannagar, Kolkata, India, Research, Institute for Nuclear, Energy, Nuclear, Sciences, Bulgarian Academy of, Sofia, Bulgaria, Sciences, FZU - Institute of Physics of the Czech Academy of, Praha, di Palermo, Dipartimento di Fisica e Chimica 'E. Segrè' Università degli Studi, Scienze, via delle, Palermo, de Electronica, Grupo, de Madrid, Universidad Complutense, Complutense, Av., Madrid, Physics, Department of Applied, Zagreb, University of, Zagreb, Center, Hiroshima Astrophysical Science, Higashi-Hiroshima, RIKEN, Physical, Institute of, Research, Chemical, Wako, Saitama, University, Charles, Particle, Institute of, Physics, Nuclear, Physics, Division of, Astronomy, Science, Graduate School of, University, Kyoto, Sakyo-ku, Research, Institute for Space-Earth Environmental, University, Nagoya, Chikusa-ku, Nagoya, Institute, Kobayashi-Maskawa, Particles, for the Origin of, Universe, the, Technology, Graduate School of, Industrial, Sciences, Social, University, Tokushima, Tokushima, Sciences, Department of Physical, University, Aoyama Gakuin, Fuchinobe, Sagamihara, Kanagawa, IRFU, CEA, Paris-Saclay, Université, Gif-sur-Yvette, France, University, Saitama, Sakura-ku, city, Saitama, di Torino, Dipartimento di Fisica - Universitá degli Studi, Torino, University, Konan, Kobe, Hyogo, Japan), Heidelberg, Zeuthen, Saclay, CEA, Merisiers, Orme des, France), Laboratoire d'Annecy de Physique des Particules (LAPP), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS), Centre de Physique des Particules de Marseille (CPPM), Aix Marseille Université (AMU)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Institut de Recherches sur les lois Fondamentales de l'Univers (IRFU), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay, Département d'Astrophysique (ex SAP) (DAP), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay, and CTA-LST Project
Subjects: Cherenkov Telescope Array, energy resolution, FOS: Physical sciences, GeV, gamma ray: energy spectrum, energy: threshold, muon, site, TeV, pulsar wind nebula, [PHYS.PHYS.PHYS-INS-DET]Physics [physics]/Physics [physics]/Instrumentation and Detectors [physics.ins-det], numerical calculations, Instrumentation and Methods for Astrophysics (astro-ph.IM), Monte Carlo, pulsar, High Energy Astrophysical Phenomena (astro-ph.HE), trigger, sensitivity, optics, flux, observatory, gamma ray: VHE, angular resolution, Astrophysics - High Energy Astrophysical Phenomena, Astrophysics - Instrumentation and Methods for Astrophysics, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], statistical, performance, spectral energy distribution
Abstract: CTA (Cherenkov Telescope Array) is the next generation ground-based observatory for gamma-ray astronomy at very-high energies. The Large-Sized Telescope prototype (LST-1) is located at the Northern site of CTA, on the Canary Island of La Palma. LSTs are designed to provide optimal performance in the lowest part of the energy range covered by CTA, down to $\simeq 20$ GeV. LST-1 started performing astronomical observations in November 2019, during its commissioning phase, and it has been taking data since then. We present the first LST-1 observations of the Crab Nebula, the standard candle of very-high energy gamma-ray astronomy, and use them, together with simulations, to assess the basic performance parameters of the telescope. The data sample consists of around 36 hours of observations at low zenith angles collected between November 2020 and March 2022. LST-1 has reached the expected performance during its commissioning period - only a minor adjustment of the preexisting simulations was needed to match the telescope behavior. The energy threshold at trigger level is estimated to be around 20 GeV, rising to $\simeq 30$ GeV after data analysis. Performance parameters depend strongly on energy, and on the strength of the gamma-ray selection cuts in the analysis: angular resolution ranges from 0.12 to 0.40 degrees, and energy resolution from 15 to 50%. Flux sensitivity is around 1.1% of the Crab Nebula flux above 250 GeV for a 50-h observation (12% for 30 minutes). The spectral energy distribution (in the 0.03 - 30 TeV range) and the light curve obtained for the Crab Nebula agree with previous measurements, considering statistical and systematic uncertainties. A clear periodic signal is also detected from the pulsar at the center of the Nebula., Accepted in ApJ. v3: updated author list and acknowledgements, fixed typos and other minor issues
Published: 2023

3. Uncovering stochastic gravitational-wave backgrounds with LISA

Author: Baghi, Quentin, Karnesis, Nikolaos, Bayle, Jean-Baptiste, Besançon, Marc, Inchauspé, Henri, Département de Physique des Particules (ex SPP) (DPhP), Institut de Recherches sur les lois Fondamentales de l'Univers (IRFU), and Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay
Subjects: observatory, density, spectral, noise, LISA, gravitational radiation, stochastic, [PHYS.GRQC]Physics [physics]/General Relativity and Quantum Cosmology [gr-qc], FOS: Physical sciences, General Relativity and Quantum Cosmology (gr-qc), Bayesian, detector, network, General Relativity and Quantum Cosmology, gravitational radiation, background, pulsar
Abstract: Finding a stochastic gravitational-wave background (SGWB) of astrophysical or primordial origin is one of the quests of current and future gravitational-wave observatories. While detector networks such as LIGO-Virgo-Kagra or pulsar timing arrays can use cross-correlations to tell instrumental noise and SGWB apart, LISA is likely to be the only flying detector of its kind in 2035. This particularity poses a challenge for data analysis. To tackle it, we present a strategy based on Bayesian model selection. We use a flexible noise power spectral density~(PSD) model and the knowledge of noise and signal transfer functions to allow SGWBs detection when the noise PSD is unknown. With this technique, we then probe the parameter space accessible by LISA for power-law SGWB shapes., 5 pages, 1 figure, contribution to the 2023 Gravitation session of the 57th Rencontres de Moriond
Published: 2023

4. Study of Magnetic Dipole Moment of the Pulsars

Author: Aakash Narayan and Ibrahim Mirza
Subjects: Pulsar, Neutron star
Abstract: Preprint version
Published: 2023
Full Text: View/download PDF

5. The second data release from the European Pulsar Timing Array: VI. Challenging the ultralight dark matter paradigm

Author: Smarra, Clemente, Goncharov, Boris, Barausse, Enrico, Antoniadis, J., Babak, S., Nielsen, A. -S. Bak, Bassa, C. G., Berthereau, A., Bonetti, M., Bortolas, E., Brook, P. R., Burgay, M., Caballero, R. N., Chalumeau, A., Champion, D. J., Chanlaridis, S., Chen, S., Cognard, I., Desvignes, G., Falxa, M., Ferdman, R. D., Franchini, A., Gair, J. R., Graikou, E., Grie, J. -M., Guillemot, L., Guo, Y. J., Hu, H., Iraci, F., Izquierdo-Villalba, D., Jang, J., Jawor, J., Janssen, G. H., Jessner, A., Karuppusamy, R., Keane, E. F., Keith, M. J., Kramer, M., Krishnakumar, M. A., Lackeos, K., Lee, K. J., Liu, K., Liu, Y., Lyne, A. G., McKee, J. W., Main, R. A., Mickaliger, M. B., Niţu, I. C., Parthasarathy, A., Perera, B. B. P., Perrodin, D., Petiteau, A., Porayko, N. K., Possenti, A., Leclere, H. Quelquejay, Samajdar, A., Sanidas, S. A., Sesana, A., Shaifullah, G., Speri, L., Spiewak, R., Stappers, B. W., Susarla, S. C., Theureau, G., Tiburzi, C., van der Wateren, E., Vecchio, A., Krishnan, V. Venkatraman, Wang, J., Wang, L., Wu, Z., AstroParticule et Cosmologie (APC (UMR_7164)), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité), Laboratoire de Physique et Chimie de l'Environnement et de l'Espace (LPC2E), Observatoire des Sciences de l'Univers en région Centre (OSUC), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université d'Orléans (UO)-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université d'Orléans (UO)-Centre National de la Recherche Scientifique (CNRS)-Centre National d’Études Spatiales [Paris] (CNES), Unité Scientifique de la Station de Nançay (USN), Université Paris sciences et lettres (PSL)-Université d'Orléans (UO)-Centre National de la Recherche Scientifique (CNRS), Institut de Recherches sur les lois Fondamentales de l'Univers (IRFU), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay, Laboratoire Univers et Théories (LUTH (UMR_8102)), and European Pulsar Timing Array
Subjects: High Energy Astrophysical Phenomena (astro-ph.HE), Cosmology and Nongalactic Astrophysics (astro-ph.CO), dark matter, interaction, density, local, FOS: Physical sciences, General Relativity and Quantum Cosmology (gr-qc), GeV, Astrophysics - Astrophysics of Galaxies, General Relativity and Quantum Cosmology, High Energy Physics - Phenomenology, High Energy Physics - Phenomenology (hep-ph), gravitation, Astrophysics of Galaxies (astro-ph.GA), [PHYS.HPHE]Physics [physics]/High Energy Physics - Phenomenology [hep-ph], [PHYS.GRQC]Physics [physics]/General Relativity and Quantum Cosmology [gr-qc], galaxy, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Astrophysics - High Energy Astrophysical Phenomena, pseudoscalar, dark matter, density, pulsar, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: Pulsar Timing Array experiments probe the presence of possible scalar/pseudoscalar ultralight dark matter particles through decade-long timing of an ensemble of galactic millisecond radio pulsars. With the second data release of the European Pulsar Timing Array, we focus on the most robust scenario, in which dark matter interacts only gravitationally with ordinary baryonic matter. Our results show that ultralight particles with masses $10^{-24.0}~\text{eV} \lesssim m \lesssim 10^{-23.2}~\text{eV}$ cannot constitute $100\%$ of the measured local dark matter density, but can have at most local density $\rho\lesssim 0.15$ GeV/cm$^3$., Comment: 5 pages + acknowledgements + refs, 2 figures
Published: 2023

6. Searching for continuous Gravitational Waves in the second data release of the International Pulsar Timing Array

Author: Falxa, M, Babak, S, Baker, P T, Bécsy, B, Chalumeau, A, Chen, S, Chen, Z, Cornish, N J, Guillemot, L, Hazboun, J S, Mingarelli, C M F, Parthasarathy, A, Petiteau, A, Pol, N S, Sesana, A, Spolaor, S B, Taylor, S R, Theureau, G, Vallisneri, M, Vigeland, S J, Witt, C A, Zhu, X, Antoniadis, J, Arzoumanian, Z, Bailes, M, Bhat, N D R, Blecha, L, Brazier, A, Brook, P R, Caballero, N, Cameron, A D, Casey-Clyde, J A, Champion, D, Charisi, M, Chatterjee, S, Cognard, I, Cordes, J M, Crawford, F, Cromartie, H T, Crowter, K, Dai, S, DeCesar, M E, Demorest, P B, Desvignes, G, Dolch, T, Drachler, B, Feng, Y, Ferrara, E C, Fiore, W, Fonseca, E, Garver-Daniels, N, Glaser, J, Goncharov, B, Good, D C, Griessmeier, J, Guo, Y J, Gültekin, K, Hobbs, G, Hu, H, Islo, K, Jang, J, Jennings, R J, Johnson, A D, Jones, M L, Kaczmarek, J, Kaiser, A R, Kaplan, D L, Keith, M, Kelley, L Z, Kerr, M, Key, J S, Laal, N, Lam, M T, Lamb, W G, Lazio, T J W, Liu, K, Liu, T, Luo, J, Lynch, R S, Madison, D R, Main, R, Manchester, R, McEwen, A, McKee, J, McLaughlin, M A, Ng, C, Nice, D J, Ocker, S, Olum, K D, Osłowski, S, Pennucci, T T, Perera, B B P, Perrodin, D, Porayko, N, Possenti, A, Quelquejay-Leclere, H, Ransom, S M, Ray, P S, Reardon, D J, Russell, C J, Samajdar, A, Sarkissian, J, Schult, L, Shaifullah, G, Shannon, R M, Shapiro-Albert, B J, Siemens, X, Simon, J J, Siwek, M, Smith, T L, Speri, L, Spiewak, R, Stairs, I H, Stappers, B, Stinebring, D R, Swiggum, J K, Tiburzi, C, Turner, J, Vecchio, A, Verbiest, Joris, Wahl, H, Wang, S Q, Wang, J, Wang, Jun, Wu, Ziwei, Zhang, L, Zhang, S, AstroParticule et Cosmologie (APC (UMR_7164)), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité), Unité Scientifique de la Station de Nançay (USN), Observatoire des Sciences de l'Univers en région Centre (OSUC), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université d'Orléans (UO)-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université d'Orléans (UO)-Centre National de la Recherche Scientifique (CNRS), Laboratoire de Physique et Chimie de l'Environnement et de l'Espace (LPC2E), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université d'Orléans (UO)-Centre National de la Recherche Scientifique (CNRS)-Centre National d’Études Spatiales [Paris] (CNES), Institut de Recherches sur les lois Fondamentales de l'Univers (IRFU), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay, Laboratoire Univers et Théories (LUTH (UMR_8102)), and IPTA
Subjects: noise, data analysis method, gravitational radiation, orbit: circle, FOS: Physical sciences, General Relativity and Quantum Cosmology (gr-qc), sensitivity, frequency: high, General Relativity and Quantum Cosmology, confidence limit, frequency: low, black hole: binary, [PHYS.GRQC]Physics [physics]/General Relativity and Quantum Cosmology [gr-qc], [PHYS.PHYS.PHYS-INS-DET]Physics [physics]/Physics [physics]/Instrumentation and Detectors [physics.ins-det], Astrophysics - Instrumentation and Methods for Astrophysics, Instrumentation and Methods for Astrophysics (astro-ph.IM), pulsar
Abstract: The International Pulsar Timing Array 2nd data release is the combination ofdatasets from worldwide collaborations. In this study, we search for continuouswaves: gravitational wave signals produced by individual supermassive blackhole binaries in the local universe. We consider binaries on circular orbitsand neglect the evolution of orbital frequency over the observational span. Wefind no evidence for such signals and set sky averaged 95% upper limits ontheir amplitude h 95 . The most sensitive frequency is 10nHz with h 95 = 9.110-15 . We achieved the best upper limit to date at low and high frequencies ofthe PTA band thanks to improved effective cadence of observations. In ouranalysis, we have taken into account the recently discovered common red noiseprocess, which has an impact at low frequencies. We also find that the peculiarnoise features present in some pulsars data must be taken into account toreduce the false alarm. We show that using custom noise models is essential insearching for continuous gravitational wave signals and setting the upperlimit.
Published: 2023

7. Detection of extended gamma-ray emission around the Geminga pulsar with H.E.S.S

Author: Collaboration, H. E. S. S., Aharonian, F., Benkhali, F. Ait, Aschersleben, J., Ashkar, H., Backes, M., Martins, V. Barbosa, Batzofin, R., Becherini, Y., Berge, D., Bernlöhr, K., Bi, B., Böttcher, M., Boisson, C., Bolmont, J., Borowska, J., Bouyahiaoui, M., Bradascio, F., Brose, R., Brun, F., Bruno, B., Bulik, T., Scheidlin, C. Burger, Cangemi, F., Caroff, S., Casanova, S., Celic, J., Cerruti, M., Chambery, P., Chand, T., Chandra, S., Chen, A., Chibueze, J., Chibueze, O., Cotter, G., Mbarubucyeye, J. Damascene, Devin, J., Djannati-Ataï, A., Dmytriiev, A., Egberts, K., Einecke, S., Ernenwein, J. P., Feijen, K., de Clairfontaine, G. Fichet, Filipovic, M., Fontaine, G., Füssling, M., Funk, S., Gabici, S., Gallant, Y. A., Ghafourizadeh, S., Giavitto, G., Giunti, L., Glawion, D., Glicenstein, J. F., Goswami, P., Grolleron, G., Grondin, M. -H., Haerer, L., Haupt, M., Hermann, G., Hinton, J. A., Hofmann, W., Holch, T. L., Holler, M., Horns, D., Huang, Zhiqiu, Jamrozy, M., Jankowsky, F., Joshi, V., Jung-Richardt, I., Kasai, E., Katarzyński, K., Khélifi, B., Kluźniak, W., Komin, Nu., Kosack, K., Kostunin, D., Lang, R. G., Stum, S. Le, Leitl, F., Lemière, A., Lemoine-Goumard, M., Lenain, J. -P., Leuschner, F., Lohse, T., Luashvili, A., Lypova, I., Mackey, J., Malyshev, D., Marandon, V., Marchegiani, P., Marcowith, A., Marinos, P., Martí-Devesa, G., Marx, R., Maurin, G., Meintjes, P. J., Meyer, M., Mitchell, A., Moderski, R., Mohrmann, L., Montanari, A., Moulin, E., Muller, J., Nakashima, K., de Naurois, M., Niemiec, J., Noel, A. Priyana, O'Brien, P., Ohm, S., Olivera-Nieto, L., Wilhelmi, E. de Ona, Ostrowski, M., Panny, S., Panter, M., Parsons, R. D., Peron, G., Prokhorov, D. A., Pühlhofer, G., Quirrenbach, A., Reimer, A., Reimer, O., Renaud, M., Reville, B., Rieger, F., Rowell, G., Rudak, B., Ricarte, H. Rueda, Ruiz-Velasco, E., Sahakian, V., Salzmann, H., Santangelo, A., Sasaki, M., Schüssler, F., Schutte, H. M., Schwanke, U., Shapopi, J. N. S., Sinha, A., Sol, H., Specovius, A., Spencer, S., Stawarz, Ł., Steinmassl, S., Sushch, I., Suzuki, H., Takahashi, T., Tanaka, T., Tavernier, T., Taylor, A. M., Terrier, R., Thorpe-Morgan, C., Tsirou, M., Tsuji, N., Vecchi, M., Venter, C., Vink, J., Wagner, S. J., White, R., Wierzcholska, A., Wong, Yu Wun, Zacharias, M., Zargaryan, D., Zdziarski, A. A., Zech, A., Zouari, S., Żywucka, N., Laboratoire Leprince-Ringuet (LLR), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-École polytechnique (X)-Centre National de la Recherche Scientifique (CNRS), AstroParticule et Cosmologie (APC (UMR_7164)), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité), Laboratoire Univers et Théories (LUTH (UMR_8102)), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Laboratoire de Physique Nucléaire et de Hautes Énergies (LPNHE (UMR_7585)), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Institut de Recherches sur les lois Fondamentales de l'Univers (IRFU), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay, Laboratoire d'Annecy de Physique des Particules (LAPP), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS), Laboratoire de Physique des Deux Infinis Bordeaux (LP2I - Bordeaux), Université de Bordeaux (UB)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Laboratoire Univers et Particules de Montpellier (LUPM), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Université de Montpellier (UM), Centre de Physique des Particules de Marseille (CPPM), Aix Marseille Université (AMU)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), and H.E.S.S.
Subjects: High Energy Astrophysical Phenomena (astro-ph.HE), electron: energy, lepton, background, water, halo, FOS: Physical sciences, imaging, Cherenkov counter: atmosphere, energy dependence, flux, gamma ray: emission, gamma ray: VHE, diffusion: model, HESS, TeV, Cherenkov, pulsar wind nebula, galaxy, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Astrophysics - High Energy Astrophysical Phenomena, HAWC, asymmetry, electron: diffusion, pulsar
Abstract: Geminga is an enigmatic radio-quiet gamma-ray pulsar located at a mere 250 pc distance from Earth. Extended very-high-energy gamma-ray emission around the pulsar was discovered by Milagro and later confirmed by HAWC, which are both water Cherenkov detector-based experiments. However, evidence for the Geminga pulsar wind nebula in gamma rays has long evaded detection by imaging atmospheric Cherenkov telescopes (IACTs) despite targeted observations. The detection of gamma-ray emission on angular scales > 2 deg poses a considerable challenge for the background estimation in IACT data analysis. With recent developments in understanding the complementary background estimation techniques of water Cherenkov and atmospheric Cherenkov instruments, the H.E.S.S. IACT array can now confirm the detection of highly extended gamma-ray emission around the Geminga pulsar with a radius of at least 3 deg in the energy range 0.5-40 TeV. We find no indications for statistically significant asymmetries or energy-dependent morphology. A flux normalisation of $(2.8\pm0.7)\times10^{-12}$ cm$^{-2}$s$^{-1}$TeV$^{-1}$ at 1 TeV is obtained within a 1 deg radius region around the pulsar. To investigate the particle transport within the halo of energetic leptons around the pulsar, we fitted an electron diffusion model to the data. The normalisation of the diffusion coefficient obtained of $D_0 = 7.6^{+1.5}_{-1.2} \times 10^{27}$ cm$^2$s$^{-1}$, at an electron energy of 100 TeV, is compatible with values previously reported for the pulsar halo around Geminga, which is considerably below the Galactic average., 16 pages, 15 figures, 7 tables. Accepted for publication in Astronomy & Astrophysics
Published: 2023

8. The second decametre pulsar census at the UTR-2

Author: I. P. Kravtsov, O. O. Konovalenko, A. I. Shevtsova, O. M. Ulyanov, V. V. Zakharenko, and Serge Yerin
Subjects: Radio telescope, Physics, Rotation period, Pulsar, Space and Planetary Science, Astrophysics::High Energy Astrophysical Phenomena, Dispersion (optics), Astronomy, Flux, Astronomy and Astrophysics
Abstract: In this paper, we present the results of the second census of pulsars in the decametre wave range at the Ukrainian T-shaped Radio telescope, second modification (UTR-2). Over the past 10 yr, the worldwide number of discovered nearby pulsars has doubled, which means that there is some urgency to search for a low-frequency radio emission from these newly discovered sources. To increase the sensitivity of this census, the integration time was doubled compared with the first census of 2010–2013. As a result, the decametre radio emission of 20 pulsars was detected, and their flux densities and the shape of their pulses were obtained. The dispersion measures for 10 pulsars and the rotation periods for eight pulsars were refined. For several pulsars, the scattering time constant and FWHM were estimated in the decametre wave range. The upper limits of flux densities for 102 pulsars that have not yet been detected were also estimated.
Published: 2022

9. Pulsar-Calibrated Timing Source for Synchronized Sampling

Author: Lin Zhu, He Yin, Xiqian Luo, Liang Zhang, Wenxuan Yao, Wei Qiu, and Yilu Liu
Subjects: General Computer Science, Pulsar, Environmental science, Sampling (statistics), Remote sensing
Published: 2022

10. Pulsar identification method based on adaptive grey wolf optimization algorithm in X-ray pulsar-based navigations

Author: Yu Jiang, Jing Jin, Hongyang Zhao, Bingjie Shan, and Yi Shen
Subjects: Atmospheric Science, education.field_of_study, Computer science, Stochastic resonance, Astrophysics::High Energy Astrophysical Phenomena, Fast Fourier transform, Population, Aerospace Engineering, Astronomy and Astrophysics, Filter (signal processing), Geophysics, Pulsar, Space and Planetary Science, Singular value decomposition, General Earth and Planetary Sciences, Detection theory, education, Algorithm, X-ray pulsar
Abstract: Fast and accurate identification of pulsar signals is important for X-ray pulsar-based navigation (XNAV). Traditional pulsar signal detection technology based on FFT search and epoch folding (EF) requires a very long time to obtain an appropriate signal-to-noise ratio (SNR) gain, especially for weak pulsar signals with low photon fluxes. This paper proposes an adaptive stochastic resonance (SR) method based on the grey wolf optimizer (GWO) algorithm for fast pulsar identification. The GWO algorithm can optimize the SR parameters to obtain the optimal SR output that matches the input signal. Meanwhile, the initial population of GWO is generated by Chebyshev chaotic maps, which guarantees the diversity of the initial population and enhances the global search capability of GWO. To further improve the performance of SR, we add an extra denoising process, including a high-pass filter and singular value decomposition (SVD) that determines the effective singular components through dispersion entropy (DE), to suppress the noise to a great extent. We use simulation data and Rossi X-ray Timing Explorer (RXTE) observation data to verify the proposed method. The output SNR is greatly improved, and the method can identify pulsars in a short time. The results indicated that the proposed method has great practical value in engineering. Further experiments reveal the importance of SVD, DE and the Chebyshev chaotic map for the algorithm.
Published: 2022

11. Two years of pulsar observations with the ultra-wide-band receiver on the Parkes radio telescope

Author: Michael Keith, Charlotte Sobey, Simon Johnston, Aditya Parthasarathy, Ryan Shannon, R. N. Manchester, Matthew Kerr, Shi Dai, L. S. Oswald, and Patrick Weltevrede
Subjects: High Energy Astrophysical Phenomena (astro-ph.HE), Physics, Astrophysics::High Energy Astrophysical Phenomena, FOS: Physical sciences, Ultra-wideband, Astronomy and Astrophysics, Astrophysics, law.invention, Radio telescope, Telescope, symbols.namesake, Pulsar, Space and Planetary Science, law, Dispersion (optics), Faraday effect, symbols, Astrophysics - High Energy Astrophysical Phenomena, Astrophysics - Instrumentation and Methods for Astrophysics, Supernova remnant, Instrumentation and Methods for Astrophysics (astro-ph.IM), Astrophysics::Galaxy Astrophysics
Abstract: The major programme for observing young, non-recycled pulsars with the Parkes telescope has transitioned from a narrow-band system to an ultra-wideband system capable of observing between 704 and 4032 MHz. We report here on the initial two years of observations with this receiver. Results include dispersion measure (DM) and Faraday rotation measure (RM) variability with time, determined with higher precision than hitherto, flux density measurements and the discovery of several nulling and mode changing pulsars. PSR J1703-4851 is shown to be one of a small subclass of pulsars that has a weak and a strong mode which alternate rapidly in time. PSR J1114-6100 has the fourth highest |RM| of any known pulsar despite its location far from the Galactic Centre. PSR J1825-1446 shows variations in both DM and RM likely due to its motion behind a foreground supernova remnant., Comment: Accepted for publication in MNRAS. This version fixes transcription errors in Table 4
Published: 2023

12. A polarization census of bright pulsars using the ultrawideband receiver on the Parkes radio telescope

Author: Simon Johnston, Patrick Weltevrede, Ryan Shannon, Shi Dai, L. S. Oswald, Charlotte Sobey, Matthew Kerr, Aditya Parthasarathy, and R. N. Manchester
Subjects: Astrophysics::High Energy Astrophysical Phenomena, FOS: Physical sciences, Astrophysics, 01 natural sciences, law.invention, Radio telescope, symbols.namesake, Pulsar, law, 0103 physical sciences, Faraday effect, Faraday cage, Instrumentation and Methods for Astrophysics (astro-ph.IM), 010303 astronomy & astrophysics, Circular polarization, High Energy Astrophysical Phenomena (astro-ph.HE), Physics, 010308 nuclear & particles physics, Linear polarization, Astronomy and Astrophysics, Polarization (waves), Astrophysics - Astrophysics of Galaxies, Interstellar medium, 13. Climate action, Space and Planetary Science, Astrophysics of Galaxies (astro-ph.GA), symbols, Astrophysics - High Energy Astrophysical Phenomena, Astrophysics - Instrumentation and Methods for Astrophysics
Abstract: We present high signal-to-noise, full polarization pulse profiles for 40 bright, 'slowly'-rotating (non-recycled) pulsars using the new Ultra-Wideband Low-frequency (UWL; 704-4032 MHz) receiver on the Parkes radio telescope. We obtain updated and accurate interstellar medium parameters towards these pulsars (dispersion measures and Faraday rotation measures), and reveal Faraday dispersion towards PSR J1721-3532 caused by interstellar scattering. We find general trends in the pulse profiles including decreasing fractional linear polarization and increasing degree of circular polarization with increasing frequency, consistent with previous studies, while also revealing new features and frequency evolution. This demonstrates results that can be obtained using UWL monitoring observations of slow pulsars, which are valuable for improving our understanding of pulsar emission and the intervening interstellar medium. The calibrated data products are publicly available., 20 pages, 5 figures, 2 tables, 25 pages of supporting information with 2 figures. Accepted for publication in MNRAS. doi:10.1093/mnras/stab861
Published: 2023

13. The impact of glitches on young pulsar rotational evolution

Author: Andrew Melatos, Patrick Weltevrede, Richard N. Manchester, S. Johnston, Marcus E. Lower, Matthew Bailes, Aditya Parthasarathy, Shi Dai, Charlotte Sobey, Liam Dunn, Ryan Shannon, L. S. Oswald, and Matthew Kerr
Subjects: High Energy Astrophysical Phenomena (astro-ph.HE), Physics, 010308 nuclear & particles physics, Astrophysics::High Energy Astrophysical Phenomena, Astrophysics::Instrumentation and Methods for Astrophysics, FOS: Physical sciences, Astronomy and Astrophysics, Context (language use), Interval (mathematics), Astrophysics, Approx, 01 natural sciences, Measure (mathematics), Glitch, Radio telescope, Pulsar, Space and Planetary Science, 0103 physical sciences, Range (statistics), Astrophysics::Solar and Stellar Astrophysics, Astrophysics - High Energy Astrophysical Phenomena, 010303 astronomy & astrophysics
Abstract: We report on a timing programme of 74 young pulsars that have been observed by the Parkes 64-m radio telescope over the past decade. Using modern Bayesian timing techniques, we have measured the properties of 124 glitches in 52 of these pulsars, of which 74 are new. We demonstrate that the glitch sample is complete to fractional increases in spin-frequency greater than $\Delta\nu^{90\%}_{g}/\nu \approx 8.1 \times 10^{-9}$. We measure values of the braking index, $n$, in 33 pulsars. In most of these pulsars, their rotational evolution is dominated by episodes of spin-down with $n > 10$, punctuated by step changes in the spin-down rate at the time of a large glitch. The step changes are such that, averaged over the glitches, the long-term $n$ is small. We find a near one-to-one relationship between the inter-glitch value of $n$ and the change in spin-down of the previous glitch divided by the inter-glitch time interval. We discuss the results in the context of a range of physical models., Comment: 24 pages, 9 figures and 9 tables. Published in MNRAS. (Fixed typo in the abstract and conclusion)
Published: 2023

14. Validation of heliospheric modeling algorithms through pulsar observations I: Interplanetary scintillation-based tomography

Author: C. Tiburzi, B.V. Jackson, L. Cota, G.M. Shaifullah, R.A. Fallows, M. Tokumaru, P. Zucca, Tiburzi, C, Jackson, B, Cota, L, Shaifullah, G, Fallows, R, Tokumaru, M, and Zucca, P
Subjects: High Energy Astrophysical Phenomena (astro-ph.HE), Atmospheric Science, Interplanetary Scintillation, Solar wind, Aerospace Engineering, FOS: Physical sciences, Astronomy and Astrophysics, Space Physics (physics.space-ph), Geophysics, Astrophysics - Solar and Stellar Astrophysics, Physics - Space Physics, Space and Planetary Science, General Earth and Planetary Sciences, Pulsar, Astrophysics - High Energy Astrophysical Phenomena, Solar and Stellar Astrophysics (astro-ph.SR)
Abstract: Solar-wind 3-D reconstruction tomography based on interplanetary scintillation (IPS) studies provides fundamental information for space-weather forecasting models, and gives the possibility to determine heliospheric column densities. Here we compare the time series of Solar-wind column densities derived from long-term observations of pulsars, and the Solar-wind reconstruction provided by the UCSD IPS tomography. This work represents a completely independent comparison and validation of these techniques to provide this measurement, and it strengthens confidence in the use of both in space-weather analyses applications., Comment: Published in Journal of Advances in Space Research
Published: 2023
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15. Constraining Post-Inflationary Axions with Pulsar Timing Arrays

Author: Servant, Géraldine and Simakachorn, Peera
Subjects: Cosmology and Nongalactic Astrophysics (astro-ph.CO), gravitational radiation, emission, background, stochastic, axion, mass, FOS: Physical sciences, axion, string, domain wall, NANOGrav, gravitational radiation, spectrum, GeV, U(1), symmetry breaking, dark matter, High Energy Physics - Phenomenology, High Energy Physics - Phenomenology (hep-ph), cosmic string, network, axion, decay constant, axion-like particles, history, inflation, Astrophysics - Cosmology and Nongalactic Astrophysics, gravitational radiation, background, pulsar
Abstract: Models that produce Axion-Like-Particles (ALP) after cosmological inflation due to spontaneous $U(1)$ symmetry breaking also produce cosmic string networks. Those axionic strings lose energy through gravitational wave emission during the whole cosmological history, generating a stochastic background of gravitational waves that spans many decades in frequency. We can therefore constrain the axion decay constant and axion mass from limits on the gravitational wave spectrum and compatibility with dark matter abundance as well as dark radiation. We derive such limits from analyzing the most recent NANOGrav data from Pulsar Timing Arrays (PTA). The limits are compatible with the slightly stronger $N_{\rm eff}$ bounds on dark radiation for ALP masses $m_a \lesssim 10^{-10}$ eV. On the other hand, for heavy ALPs with $m_a\gtrsim 0.1$ GeV and $N_{\rm DW}\neq 1$, new regions of parameter space can be probed by PTA data due to the dominant Domain-Wall contribution to the gravitational wave background., Comment: 8 pages, 4 figures + supplemental material (2 pages, 2 figures)
Published: 2023
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16. Do pulsar timing arrays observe merging primordial black holes?

Author: Depta, Paul Frederik, Schmidt-Hoberg, Kai, and Tasillo, Carlo
Subjects: black hole, primordial, black hole, binary, gravitational radiation, background, pulsar
Abstract: In this letter we evaluate whether the gravitational wave background recently observed by a number of different pulsar timing arrays could be due to merging primordial supermassive black hole binaries. We find that for homogeneously distributed primordial black holes this possibility is inconsistent with the strong cosmological and astrophysical constraints on their total abundance. If the distribution exhibits some clustering, however, the merger rate will in general be enhanced, opening the window for a consistent interpretation of the PTA data in terms of merging primordial black holes.
Published: 2023
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17. MeerKAT discovery of 13 new pulsars in Omega Centauri

Author: W Chen, P C C Freire, A Ridolfi, E D Barr, B Stappers, M Kramer, A Possenti, S M Ransom, L Levin, R P Breton, M Burgay, F Camilo, S Buchner, D J Champion, F Abbate, V Venkatraman Krishnan, P V Padmanabh, T Gautam, L Vleeschower, M Geyer, J-M Grießmeier, Y P Men, V Balakrishnan, and M C Bezuidenhout
Subjects: High Energy Astrophysical Phenomena (astro-ph.HE), Space and Planetary Science, FOS: Physical sciences, ddc:520, Binary, Pulsar, Astronomy and Astrophysics, Globular cluster, Astrophysics - High Energy Astrophysical Phenomena, Dewey Decimal Classification::500 | Naturwissenschaften::520 | Astronomie, Kartographie
Abstract: The most massive globular cluster in our Galaxy, Omega Centauri, is an interesting target for pulsar searches, because of its multiple stellar populations and the intriguing possibility that it was once the nucleus of a galaxy that was absorbed into the Milky Way. The recent discoveries of pulsars in this globular cluster and their association with known X-ray sources was a hint that, given the large number of known X-ray sources, there is a much larger undiscovered pulsar population. We used the superior sensitivity of the MeerKAT radio telescope to search for pulsars in Omega Centauri. In this paper, we present some of the first results of this survey, including the discovery of 13 new pulsars; the total number of known pulsars in this cluster currently stands at 18. At least half of them are in binary systems and preliminary orbital constraints suggest that most of the binaries have light companions. We also discuss the ratio between isolated and binaries pulsars, and how they were formed in this cluster.
Published: 2023
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18. Do pulsar timing arrays observe merging primordial black holes?

Author: Depta, Paul Frederik, Schmidt-Hoberg, Kai, and Tasillo, Carlo
Subjects: High Energy Physics - Phenomenology, Cosmology and Nongalactic Astrophysics (astro-ph.CO), High Energy Physics - Phenomenology (hep-ph), FOS: Physical sciences, black hole, primordial, black hole, binary, Astrophysics - Cosmology and Nongalactic Astrophysics, gravitational radiation, background, pulsar
Abstract: In this letter we evaluate whether the gravitational wave background recently observed by a number of different pulsar timing arrays could be due to merging primordial supermassive black hole binaries. We find that for homogeneously distributed primordial black holes this possibility is inconsistent with the strong cosmological and astrophysical constraints on their total abundance. If the distribution exhibits some clustering, however, the merger rate will in general be enhanced, opening the window for a consistent interpretation of the PTA data in terms of merging primordial black holes., Comment: 15 pages, 3 figures
Published: 2023
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19. Multi-scale Constraints on Scalar-Field couplings to Matter: The Geodetic and Frame-Dragging Effects

Author: Benisty, David, Brax, Philippe, Davis, Anne-Christine, Institut de Physique Théorique - UMR CNRS 3681 (IPHT), and Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay-Centre National de la Recherche Scientifique (CNRS)
Subjects: Astrophysics and Astronomy, Cosmology and Nongalactic Astrophysics (astro-ph.CO), gravitation: model, astro-ph.GA, gr-qc, satellite, FOS: Physical sciences, coupling: scalar, General Relativity and Quantum Cosmology (gr-qc), field theory: scalar: massive, frequency: high, General Relativity and Quantum Cosmology, Lense-Thirring effect, High Energy Physics - Phenomenology (hep-ph), de Sitter, precession, Particle Physics - Phenomenology, pulsar, Earth and Planetary Astrophysics (astro-ph.EP), General Relativity and Cosmology, hep-ph, coupling: conformal, star: orbit, Astrophysics - Astrophysics of Galaxies, dark energy: interaction, High Energy Physics - Phenomenology, [PHYS.HPHE]Physics [physics]/High Energy Physics - Phenomenology [hep-ph], Astrophysics of Galaxies (astro-ph.GA), astro-ph.EP, astro-ph.CO, [PHYS.GRQC]Physics [physics]/General Relativity and Quantum Cosmology [gr-qc], galaxy, proposed experiment, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Sagnac effect, geodesic, Astrophysics - Cosmology and Nongalactic Astrophysics, Astrophysics - Earth and Planetary Astrophysics
Abstract: The impact of light scalars coupled conformally and disformally to matter on the geodetic and frame-dragging (FD) precessions is calculated. For larger frequencies the disformal interaction becomes increasingly relevant. We use several satellite experiments and Pulsar time of arrival (ToA) measurements to derive bounds on the couplings, combining the Gravity Probe B, LARES, LAGEOS and GRACE results with pulsar timings. Forecasts for future constraints on the conformal and the disformal couplings based on the GINGER experiment, i.e. a future measurement of the Sagnac effect on Earth, the motion of $S$-stars around the galactic centre and future pulsar timing observations are presented., Comment: 14 pages
Published: 2023
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20. HAWC Detection of a TeV Halo Candidate Surrounding a Radio-quiet pulsar

Author: A. Albert, R. Alfaro, J. C. Arteaga-Velázquez, H. A. Ayala Solares, E. Belmont-Moreno, T. Capistrán, A. Carramiñana, S. Casanova, J. Cotzomi, S. Coutiño De León, E. De la Fuente, C. de León, R. Diaz Hernandez, M. A. DuVernois, J. C. Díaz-Vélez, C. Espinoza, K. L. Fan, N. Fraija, K. Fang, J. A. García-González, F. Garfias, A. Jardin-Blicq, M. M. González, J. A. Goodman, J. P. Harding, S. Hernandez, D. Huang, F. Hueyotl-Zahuantitla, P. Hüntemeyer, A. Iriarte, V. Joshi, A. Lara, J. Lee, H. León Vargas, J. T. Linnemann, A. L. Longinotti, G. Luis-Raya, K. Malone, O. Martinez, J. Martínez-Castro, J. A. Matthews, J. A. Morales-Soto, E. Moreno, M. Mostafá, A. Nayerhoda, L. Nellen, M. Newbold, M. U. Nisa, Y. Pérez Araujo, Y. Son, E. G. Pérez-Pérez, C. D. Rho, D. Rosa-González, A. Sandoval, M. Schneider, J. Serna-Franco, A. J. Smith, R. W. Springer, K. Tollefson, I. Torres, R. Torres-Escobedo, X. Wang, K. Whitaker, E. Willox, H. Zhou, and HEP, INSPIRE
Subjects: High Energy Astrophysical Phenomena (astro-ph.HE), formation, water, halo, FOS: Physical sciences, Astronomy and Astrophysics, VHE, observatory, Space and Planetary Science, gamma ray, TeV, spectral, Cherenkov, galaxy, Astrophysics - High Energy Astrophysical Phenomena, [PHYS.ASTR] Physics [physics]/Astrophysics [astro-ph], HAWC, pulsar
Abstract: Extended very-high-energy (VHE; 0.1–100 TeV) γ-ray emission has been observed around several middle-aged pulsars and referred to as “TeV halos.” Their formation mechanism remains under debate. It is also unknown whether they are ubiquitous or related to a certain subgroup of pulsars. With 2321 days of observation, the High Altitude Water Cherenkov (HAWC) Gamma-Ray Observatory detected VHE γ-ray emission at the location of the radio-quiet pulsar PSR J0359+5414 with >6σ significance. By performing likelihood tests with different spectral and spatial models and comparing the TeV spectrum with multiwavelength observations of nearby sources, we show that this excess is consistent with a TeV halo associated with PSR J0359+5414, though future observation of HAWC and multiwavelength follow-ups are needed to confirm this nature. This new halo candidate is located in a noncrowded region in the outer galaxy. It shares similar properties to the other halos but its pulsar is younger and radio-quiet. Our observation implies that TeV halos could commonly exist around pulsars and their formation does not depend on the configuration of the pulsar magnetosphere.
Published: 2023

21. Modified propagation of gravitational waves from the early radiation era

Author: He, Yutong, Pol, Alberto Roper, Brandenburg, Axel, AstroParticule et Cosmologie (APC (UMR_7164)), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité), and HEP, INSPIRE
Subjects: Cosmology and Nongalactic Astrophysics (astro-ph.CO), gravitation: model, energy spectrum, FOS: Physical sciences, General Relativity and Quantum Cosmology (gr-qc), General Relativity and Quantum Cosmology, Einstein Telescope, gravitational radiation: propagation, general relativity, gravitational radiation: spectrum, energy: density, WKB approximation, LIGO, numerical calculations, pulsar, LISA, [PHYS.GRQC] Physics [physics]/General Relativity and Quantum Cosmology [gr-qc], gravitational radiation: background, scale: Planck, VIRGO, frequency: low, slope, [PHYS.GRQC]Physics [physics]/General Relativity and Quantum Cosmology [gr-qc], spectral, [PHYS.ASTR] Physics [physics]/Astrophysics [astro-ph], [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: We study the propagation of cosmological gravitational wave (GW) backgrounds from the early radiation era until the present day in modified theories of gravity. Comparing to general relativity (GR), we study the effects that modified gravity parameters, such as the GW friction $\alpha_{\rm M}$ and the tensor speed excess $\alpha_{\rm T}$, have on the present-day GW spectrum. We use both the WKB estimate, which provides an analytical description but fails at superhorizon scales, and numerical simulations that allow us to go beyond the WKB approximation. We show that a constant $\alpha_{\rm T}$ makes relatively insignificant changes to the GR solution, especially taking into account the constraints on its value from GW observations by the LIGO--Virgo collaboration, while $\alpha_{\rm M}$ can introduce modifications to the spectral slopes of the GW energy spectrum in the low-frequency regime depending on the considered time evolution of $\alpha_{\rm M}$. The latter effect is additional to the damping or growth occurring equally at all scales that can be predicted by the WKB approximation. In light of the recent observations by pulsar timing array (PTA) collaborations, and the potential observations by future detectors such as SKA, LISA, DECIGO, BBO, or ET, we show that, in most of the cases, constraints cannot be placed on the effects of $\alpha_{\rm M}$ and the initial GW energy density $\mathcal{E}_{\rm GW}^*$ separately, but only on the combined effects of the two, unless the signal is observed at different frequency ranges. In particular, we provide some constraints on the combined effects from the reported PTA observations., Comment: 36 pages, 11 figures, 2 tables
Published: 2023

22. Constraining Post-Inflationary Axions with Pulsar Timing Arrays

Author: Servant, Géraldine and Simakachorn, Peera
Subjects: gravitational radiation, emission, background, stochastic, axion, mass, axion, string, domain wall, NANOGrav, gravitational radiation, spectrum, GeV, U(1), symmetry breaking, dark matter, cosmic string, network, axion, decay constant, axion-like particles, history, inflation, gravitational radiation, background, pulsar
Abstract: Models that produce Axion-Like-Particles (ALP) after cosmological inflation due to spontaneous $U(1)$ symmetry breaking also produce cosmic string networks. Those axionic strings lose energy through gravitational wave emission during the whole cosmological history, generating a stochastic background of gravitational waves that spans many decades in frequency. We can therefore constrain the axion decay constant and axion mass from limits on the gravitational wave spectrum and compatibility with dark matter abundance as well as dark radiation. We derive such limits from analyzing the most recent NANOGrav data from Pulsar Timing Arrays (PTA). The limits are compatible with the slightly stronger $N_{\rm eff}$ bounds on dark radiation for ALP masses $m_a \lesssim 10^{-10}$ eV. On the other hand, for heavy ALPs with $m_a\gtrsim 0.1$ GeV and $N_{\rm DW}\neq 1$, new regions of parameter space can be probed by PTA data due to the dominant Domain-Wall contribution to the gravitational wave background.
Published: 2023
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23. Detecting and characterizing pulsar haloes with the Cherenkov Telescope Array

Author: Christopher Eckner, Veronika Vodeb, Pierrick Martin, Gabrijela Zaharijas, Francesca Calore, and HEP, INSPIRE
Subjects: High Energy Astrophysical Phenomena (astro-ph.HE), model, Cherenkov Telescope Array, diffusion, halo, FOS: Physical sciences, Astronomy and Astrophysics, suppression, energy dependence, Space and Planetary Science, TeV, galaxy, Astrophysics - High Energy Astrophysical Phenomena, [PHYS.ASTR] Physics [physics]/Astrophysics [astro-ph], pulsar
Abstract: The recently identified source class of pulsar haloes may be numerous and bright enough in the TeV range to constitute a large fraction of the sources that will be observed with the Cherenkov Telescope Array (CTA). In this work, we quantify the prospects for detecting and characterizing pulsar haloes in observations of the projected Galactic Plane Survey (GPS), using a simple phenomenological diffusion model for individual pulsar haloes and their population in the Milky Way. Our ability to uncover pulsar haloes and constrain their main physical parameters in the CTA GPS is assessed in the framework of a full spatial-spectral likelihood analysis of simulated survey observations, using the most recent estimates for the instrument response function and prototypes for the science tools. For a model setup representative of the halo around Geminga, we find that about three hundred objects could give rise to detectable emission in the GPS survey. Yet, only a third of them could be identified through their energy-dependent morphology, and only one-tenth of them would allow the derivation of strong constraints on key physical parameters like the magnitude or extent of suppressed diffusion around the pulsar. We also provide a list of known pulsars that could be hosting a detectable (Geminga-like) halo in the GPS and assess the robustness of our findings against several systematic uncertainties., Comment: 20 pages, 9 figures (6 in the main text, 3 in appendices); submitted to MNRAS; comments welcome!
Published: 2023

24. HESS J1809$-$193: a halo of escaped electrons around a pulsar wind nebula?

Author: Aharonian, F., Benkhali, F. Ait, Aschersleben, J., Ashkar, H., Backes, M., Barbosa Martins, V., Batzofin, R., Becherini, Y., Berge, D., Böttcher, M., Boisson, C., Bolmont, J., Borowska, J., Bouyahiaoui, M., Bradascio, F., Breuhaus, M., Brose, R., Brun, F., Bruno, B., Bulik, T., Burger-Scheidlin, C., Bylund, T., Caroff, S., Casanova, S., Celic, J., Cerruti, M., Chambery, P., Chand, T., Chen, A., Chibueze, J., Chibueze, O., Mbarubucyeye, J. Damascene, Djannati-Ataï, A., Dmytriiev, A., Einecke, S., Ernenwein, J.-P., Feijen, K., Filipovic, M., Fontaine, G., Füßling, M., Funk, S., Gabici, S., Gallant, Y. A., Ghafourizadeh, S., Giavitto, G., Giunti, L., Glawion, D., Goswami, P., Grolleron, G., Grondin, M.-H., Haerer, L., Hinton, J. A., Hofmann, W., Holch, T. L., Holler, M., Horns, D., Huang, Zhiqiu, Jamrozy, M., Jankowsky, F., Joshi, V., Jung-Richardt, I., Kasai, E., Katarzynski, K., Khélifi, B., Klúzniak, W., Komin, Nu., Kosack, K., Kostunin, D., Lang, R. G., Le Stum, S., Leitl, F., Lemière, A., Lemoine-Goumard, M., Lenain, J.-P., Leuschner, F., Lohse, T., Luashvili, A., Lypova, I., Mackey, J., Malyshev, D., Marandon, V., Marchegiani, P., Marcowith, A., Marinos, P., Martí-Devesa, G., Marx, R., Mitchell, A., Moderski, R., Mohrmann, L., Montanari, A., Moulin, E., Muller, J., Nakashima, K., de Naurois, M., Niemiec, J., Noel, A. Priyana, Ohm, S., Olivera-Nieto, L., de Ona Wilhelmi, E., Ostrowski, M., Panny, S., Panter, M., Parsons, R. D., Prokhorov, D. A., Pühlhofer, G., Punch, M., Quirrenbach, A., Reichherzer, P., Reimer, A., Reimer, O., Renaud, M., Reville, B., Rieger, F., Rowell, G., Rudak, B., Sahakian, V., Santangelo, A., Sasaki, M., Schutte, H. M., Schwanke, U., Shapopi, J. N. S., Sol, H., Specovius, A., Spencer, S., Stawarz, Ł., Steenkamp, R., Steinmassl, S., Sushch, I., Suzuki, H., Takahashi, T., Tanaka, T., Terrier, R., Thorpe-Morgan, C., Tsirou, M., Tsuji, N., Uchiyama, Y., van Eldik, C., Vecchi, M., Veh, J., Venter, C., Vink, J., Wach, T., Wagner, S. J., White, R., Wierzcholska, A., Wong, Yu Wun, Zacharias, M., Zargaryan, D., Zdziarski, A. A., Zech, A., Zouari, S., Żywucka, N., H. E. S. S. Collaboration, Laboratoire Leprince-Ringuet (LLR), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-École polytechnique (X)-Centre National de la Recherche Scientifique (CNRS), AstroParticule et Cosmologie (APC (UMR_7164)), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité), Laboratoire Univers et Théories (LUTH (UMR_8102)), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Laboratoire de Physique Nucléaire et de Hautes Énergies (LPNHE (UMR_7585)), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Institut de Recherches sur les lois Fondamentales de l'Univers (IRFU), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay, Laboratoire d'Annecy de Physique des Particules (LAPP), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS), Laboratoire de Physique des Deux Infinis Bordeaux (LP2I - Bordeaux), Université de Bordeaux (UB)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Centre de Physique des Particules de Marseille (CPPM), Aix Marseille Université (AMU)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Laboratoire Univers et Particules de Montpellier (LUPM), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Université de Montpellier (UM), and H.E.S.S.
Subjects: electron, dimension: 3, halo, FOS: Physical sciences, GeV, GLAST, VHE, dimension, HESS, supernova, TeV, cloud, pulsar, High Energy Astrophysical Phenomena (astro-ph.HE), energy: high, high, observatory, 3 [dimension], ddc:520, high [energy], spectral, time dependence, galaxy, Astrophysics - High Energy Astrophysical Phenomena, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], HAWC, energy
Abstract: Astronomy and astrophysics 672, A103 (2023). doi:10.1051/0004-6361/202245459, Context. HESS J1809−193 is an unassociated very-high-energy γ-ray source located on the Galactic plane. While it has been connected to the nebula of the energetic pulsar PSR J1809−1917, supernova remnants and molecular clouds present in the vicinity also constitute possible associations. Recently, the detection of γ-ray emission up to energies of ∼100 TeV with the HAWC observatory has led to renewed interest in HESS J1809−193.Aims. We aim to understand the origin of the γ-ray emission of HESS J1809−193.Methods. We analysed 93.2 h of data taken on HESS J1809−193 above 0.27 TeV with the High Energy Stereoscopic System (H.E.S.S.), using a multi-component, three-dimensional likelihood analysis. In addition, we provide a new analysis of 12.5 yr of Fermi-LAT data above 1 GeV within the region of HESS J1809−193. The obtained results are interpreted in a time-dependent modelling framework.Results. For the first time, we were able to resolve the emission detected with H.E.S.S. into two components: an extended component (modelled as an elongated Gaussian with a 1-σ semi-major and semi-minor axis of ∼0.62° and ∼0.35°, respectively) that exhibits a spectral cutoff at ∼13 TeV, and a compact component (modelled as a symmetric Gaussian with a 1-σ radius of ∼0.1°) that is located close to PSR J1809−1917 and shows no clear spectral cutoff. The Fermi-LAT analysis also revealed extended γ-ray emission, on scales similar to that of the extended H.E.S.S. component.Conclusions. Our modelling indicates that based on its spectrum and spatial extent, the extended H.E.S.S. component is likely caused by inverse Compton emission from old electrons that form a halo around the pulsar wind nebula. The compact component could be connected to either the pulsar wind nebula or the supernova remnant and molecular clouds. Due to its comparatively steep spectrum, modelling the Fermi-LAT emission together with the H.E.S.S. components is not straightforward.Key words: acceleration of particles / radiation mechanisms: non-thermal / pulsars: individual: PSR J1809-1917 / gamma rays: general⋆ Corresponding authors; e-mail: contact.hess@hess-experiment.eu, Published by EDP Sciences, Les Ulis
Published: 2023
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25. HESS J1809$-$193: a halo of escaped electrons around a pulsar wind nebula?

Author: Aharonian, F., Benkhali, F. Ait, Aschersleben, J., Ashkar, H., Backes, M., Barbosa Martins, V., Batzofin, R., Becherini, Y., Berge, D., Böttcher, M., Boisson, C., Bolmont, J., Borowska, J., Bouyahiaoui, M., Bradascio, F., Breuhaus, M., Brose, R., Brun, F., Bruno, B., Bulik, T., Burger-Scheidlin, C., Bylund, T., Caroff, S., Casanova, S., Celic, J., Cerruti, M., Chambery, P., Chand, T., Chen, A., Chibueze, J., Chibueze, O., Mbarubucyeye, J. Damascene, Djannati-Ataï, A., Dmytriiev, A., Einecke, S., Ernenwein, J.-P., Feijen, K., Filipovic, M., Fontaine, G., Füßling, M., Funk, S., Gabici, S., Gallant, Y. A., Ghafourizadeh, S., Giavitto, G., Giunti, L., Glawion, D., Goswami, P., Grolleron, G., Grondin, M.-H., Haerer, L., Hinton, J. A., Hofmann, W., Holch, T. L., Holler, M., Horns, D., Huang, Zhiqiu, Jamrozy, M., Jankowsky, F., Joshi, V., Jung-Richardt, I., Kasai, E., Katarzynski, K., Khélifi, B., Klúzniak, W., Komin, Nu., Kosack, K., Kostunin, D., Lang, R. G., Le Stum, S., Leitl, F., Lemière, A., Lemoine-Goumard, M., Lenain, J.-P., Leuschner, F., Lohse, T., Luashvili, A., Lypova, I., Mackey, J., Malyshev, D., Marandon, V., Marchegiani, P., Marcowith, A., Marinos, P., Martí-Devesa, G., Marx, R., Mitchell, A., Moderski, R., Mohrmann, L., Montanari, A., Moulin, E., Muller, J., Nakashima, K., de Naurois, M., Niemiec, J., Noel, A. Priyana, Ohm, S., Olivera-Nieto, L., de Ona Wilhelmi, E., Ostrowski, M., Panny, S., Panter, M., Parsons, R. D., Prokhorov, D. A., Pühlhofer, G., Punch, M., Quirrenbach, A., Reichherzer, P., Reimer, A., Reimer, O., Renaud, M., Reville, B., Rieger, F., Rowell, G., Rudak, B., Sahakian, V., Santangelo, A., Sasaki, M., Schutte, H. M., Schwanke, U., Shapopi, J. N. S., Sol, H., Specovius, A., Spencer, S., Stawarz, Ł., Steenkamp, R., Steinmassl, S., Sushch, I., Suzuki, H., Takahashi, T., Tanaka, T., Terrier, R., Thorpe-Morgan, C., Tsirou, M., Tsuji, N., Uchiyama, Y., van Eldik, C., Vecchi, M., Veh, J., Venter, C., Vink, J., Wach, T., Wagner, S. J., White, R., Wierzcholska, A., Wong, Yu Wun, Zacharias, M., Zargaryan, D., Zdziarski, A. A., Zech, A., Zouari, S., Zywuck, N., and H. E. S. S. Collaboration
Subjects: electron, energy: high, dimension: 3, halo, GeV, GLAST, VHE, observatory, HESS, supernova, TeV, spectral, cloud, time dependence, galaxy, HAWC, pulsar
Abstract: Context. HESS J1809$-$193 is an unassociated very-high-energy $\gamma$-ray source located on the Galactic plane. While it has been connected to the nebula of the energetic pulsar PSR J1809$-$1917, supernova remnants and molecular clouds present in the vicinity also constitute possible associations. Recently, the detection of $\gamma$-ray emission up to energies of $\sim$100 TeV with the HAWC observatory has led to renewed interest in HESS J1809$-$193. Aims. We aim to understand the origin of the $\gamma$-ray emission of HESS J1809$-$193. Methods. We analysed 93.2 h of data taken on HESS J1809$-$193 above 0.27 TeV with the High Energy Stereoscopic System (H.E.S.S.), using a multi-component, three-dimensional likelihood analysis. In addition, we provide a new analysis of 12.5 yr of Fermi-LAT data above 1 GeV within the region of HESS J1809$-$193. The obtained results are interpreted in a time-dependent modelling framework. Results. For the first time, we were able to resolve the emission detected with H.E.S.S. into two components: an extended component that exhibits a spectral cut-off at $\sim$13 TeV, and a compact component that is located close to PSR J1809$-$1917 and shows no clear spectral cut-off. The Fermi-LAT analysis also revealed extended $\gamma$-ray emission, on scales similar to that of the extended H.E.S.S. component. Conclusions. Our modelling indicates that based on its spectrum and spatial extent, the extended H.E.S.S. component is likely caused by inverse Compton emission from old electrons that form a halo around the pulsar wind nebula. The compact component could be connected to either the pulsar wind nebula or the supernova remnant and molecular clouds. Due to its comparatively steep spectrum, modelling the Fermi-LAT emission together with the H.E.S.S. components is not straightforward. (abridged)
Published: 2023
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26. Combined analysis of neutron star natal kicks using proper motions and parallax measurements for radio pulsars and Be X-ray binaries

Author: Silvia Toonen, Andris Dorozsmai, Martyna Chruslinska, Andrei P. Igoshev, API Other Research (FNWI), and Low Energy Astrophysics (API, FNWI)
Subjects: High Energy Astrophysical Phenomena (astro-ph.HE), Physics, Proper motion, Accretion (meteorology), Gravitational wave, Astronomy, Astrophysics::High Energy Astrophysical Phenomena, FOS: Physical sciences, Binary number, Astronomy and Astrophysics, Astrophysics, Supernova, Neutron star, Astrophysics - Solar and Stellar Astrophysics, Pulsar, Space and Planetary Science, Astrophysics::Solar and Stellar Astrophysics, Astrophysics::Earth and Planetary Astrophysics, Astrophysics - High Energy Astrophysical Phenomena, Parallax, Astrophysics::Galaxy Astrophysics, Solar and Stellar Astrophysics (astro-ph.SR)
Abstract: Supernova explosion and the associated neutron star natal kicks are important events on a pathway of a binary to become a gravitational wave source, an X-ray binary or a millisecond radio pulsar. Weak natal kicks often lead to binary survival, while strong kicks frequently disrupt the binary. In this article, we aim to further constrain neutron star natal kicks in binaries. We explore binary population synthesis models by varying prescription for natal kick, remnant mass and mass accretion efficiency. We introduce a robust statistical technique to analyse combined observations of different nature. Using this technique, we further test different models using parallax and proper motion measurements for young isolated radio pulsars and similar measurements for Galactic Be X-ray binaries. Our best model for natal kicks is consistent with both measurements and contains a fraction of $w=0.2\pm 0.1$ weak natal kicks with $\sigma_1 = 45^{+25}_{-15}$ km/s, the remaining natal kicks are drawn from the high-velocity component, same as in previous works: $\sigma_2 = 336$ km/s. We found that currently used models for natal kicks of neutron stars produced by electron capture supernova (combination of maxwellian $\sigma=265$ km/s and $\sigma = 30$ km/s for electron capture) are inconsistent or marginally consistent with parallaxes and proper motions measured for isolated radio pulsars. We suggest a new model for natal kicks of ecSN, which satisfy both observations of isolated radio pulsars and Be X-ray binaries., Comment: 21 page, 36 figures, accepted to MNRAS on September 21
Published: 2021

27. Stringent Pulsar Timing Bounds on Light Scalar Couplings to Matter

Author: David Benisty, Brax, Philippe, Davis, Anne-Christine, Institut de Physique Théorique - UMR CNRS 3681 (IPHT), and Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay-Centre National de la Recherche Scientifique (CNRS)
Subjects: scalar, High Energy Physics - Theory, Astrophysics and Astronomy, astro-ph.SR, gr-qc, scalar tensor, FOS: Physical sciences, anomaly, General Relativity and Quantum Cosmology (gr-qc), General Relativity and Quantum Cosmology, High Energy Physics - Phenomenology (hep-ph), conformal, black hole, coupling, Solar and Stellar Astrophysics (astro-ph.SR), Particle Physics - Phenomenology, pulsar, astro-ph.HE, High Energy Astrophysical Phenomena (astro-ph.HE), General Relativity and Cosmology, [PHYS.HTHE]Physics [physics]/High Energy Physics - Theory [hep-th], hep-th, parametrization, hep-ph, high, solar system, radiation, High Energy Physics - Phenomenology, High Energy Physics - Theory (hep-th), Astrophysics - Solar and Stellar Astrophysics, frequency, [PHYS.HPHE]Physics [physics]/High Energy Physics - Phenomenology [hep-ph], [PHYS.GRQC]Physics [physics]/General Relativity and Quantum Cosmology [gr-qc], [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Astrophysics - High Energy Astrophysical Phenomena, Particle Physics - Theory
Abstract: Pulsar Timing constraints on scalar-tensor theories with conformal and disformal couplings to matter are discussed. Reducing the dynamics to the motion in the centre of mass frame and using the mean anomaly parametrisation, we find the first post-Newtonian corrections induced by the conformal and disformal interactions in the form of a generalized quasi-Keplerian solution. We also derive the radiation reaction force due to scalar radiation and the corresponding Post-Keplerian Parameters (PKP). We use different pulsar time of arrival (TOA) data sets to probe the scalar corrections to the PKP. In particular, we focus on systems with large orbital frequencies as the contributions to the PKP terms induced by the disformal coupling are sensitive to higher frequencies. We find that the most constraining { {pulsar timings}} are PSR B1913+16 and the double pulsar PSR J0737-3039A/B, being {{of the order of}} the Cassini bound on the conformal coupling obtained from the Shapiro effect in the solar system. { {The combined constraints using other pulsar timings give an upper bound on the conformal coupling $\beta^2 < 2.33 \cdot 10^{-5}$ and a lower bound on the disformal coupling scale of $\Lambda \geq 1.12 \ {\rm MeV}$ which is comparable to the Cassini bound and to the GW-170817 constraints respectively}}. Future measurements for pulsar timing with black hole companions are also discussed., Comment: 17 pages, 9 figures, Accepted in Phys. Rev. D
Published: 2022

28. Radio and X-ray spectral properties of gamma-ray bursts and pulsar wind nebulae

Author: Li Zhang, Fang-Wu Lu, J. Fang, Bing Zhou, and Bo-Tao Zhu
Subjects: Physics, Pulsar, Space and Planetary Science, Astrophysics::High Energy Astrophysical Phenomena, Spectral properties, X-ray, Astronomy and Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, Gamma-ray burst
Abstract: Both gamma-ray bursts (GRBs) and pulsar wind nebula (PWNe) are energetic outflows that are produced in powerful high-energy astrophysical environments. Based on the correlations between the radio luminosity LR and X-ray luminosity LX as well as between the multiband spectral slope αRX and radio flux FR for compiled GRB and PWN samples, the radio and X-ray spectral properties are statistically investigated. The results show that (1) the correlations between LR and LX are consistent for GRBs and PWNe, within the uncertainties; and (2) for the whole sample, FR is related to αRX, and GRBs have lower αRX than PWNe. It may be concluded that GRBs and PWNe have the same or similar particle acceleration mechanisms and radiation processes, i.e. synchrotron radiation, to produce the radio-to-X-ray band emission.
Published: 2021

29. Scintillation time-scale measurement of the highly active FRB20201124A

Author: Robert Wharton, Hsiu-Hsien Lin, D. Z. Li, R. A. Main, Suryarao Bethapudi, G. H. Hilmarsson, Laura Spitler, and Viswesh Marthi
Subjects: High Energy Astrophysical Phenomena (astro-ph.HE), Physics, Giant Metrewave Radio Telescope, Scintillation, Physics::Instrumentation and Detectors, Scattering, Astrophysics::High Energy Astrophysical Phenomena, FOS: Physical sciences, Astronomy and Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, Spectral line, Galactic halo, Radio telescope, Pulsar, Space and Planetary Science, Very-long-baseline interferometry, Astrophysics - High Energy Astrophysical Phenomena, Astrophysics::Galaxy Astrophysics
Abstract: Scintillation of compact radio sources results from the interference between images caused by multipath propagation, and probes the intervening scattering plasma and the velocities of the emitting source and scattering screen. In FRB20201124A, a repeating fast radio burst (FRB) which entered a period of extreme activity, we obtained many burst detections in observations at the upgraded Giant Metrewave Radio Telescope (uGMRT) and the Effelsberg 100\,m Radio Telescope. Bursts nearby in time show similar scintillation patterns, and we measure a scintillation timescale of $14.3\pm1.2$\,min and $7\pm2$\,min at Effelsberg (1370\,MHz) and uGMRT (650\,MHz), respectively, by correlating burst pair spectra. The scintillation bandwidth scaled to 1\,GHz is $0.5\pm0.1$\,MHz, and the inferred scintillation velocity at Effelsberg is $V_{\mathrm{ISS}}\approx (59\pm7) \sqrt{d_{l}/2\,\rm{kpc}}~{\rm km~s}^{-1}$, higher than Earth's velocity for any screen beyond a lens distance of $d_{l} \gtrsim 400\,$pc. From the measured scintillation bandwidth, FRB20201124A has comparatively lower scattering than nearby pulsars, and is underscattered by a factor of $\sim 30$ or $\sim 1200$ compared to the NE2001 and YMW16 model predictions respectively. This underscattering, together with the measured scintillation velocity are consistent with a scattering screen more nearby the Earth at $d_{l} \sim 400\,$pc, rather than at the 2\,kpc spiral arm which NE2001 predicts to be the dominant source of scattering. With future measurements, the distance, geometry, and velocity of the scattering screen could be obtained through modelling of the annual variation in $V_{\rm ISS}$, or through inter-station time delays or interferometric observations. Scintillation/scattering measurements of FRBs could help improve Galactic electron density models, particularly in the Galactic halo or at high Galactic latitudes., 9 pages, 9 figures, Accepted for publication in MNRAS
Published: 2021

30. The B-type binaries characterization programme I

Author: S. E. de Mink, J. I. Villaseñor, O. H. Ramirez-Agudelo, Chris Evans, Norbert Langer, W. D. Taylor, Hugues Sana, Leonardo A. Almeida, Philip Dufton, and Low Energy Astrophysics (API, FNWI)
Subjects: ULTRAVIOLET, Population, ECLIPSING BINARY, FOS: Physical sciences, Binary number, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Astronomy & Astrophysics, spectroscopic [binaries], early-type [stars], massive [stars], individual: 30 Doradus [open clusters and associations], Magellanic Clouds, Astrophysics::Solar and Stellar Astrophysics, education, Large Magellanic Cloud, Solar and Stellar Astrophysics (astro-ph.SR), Astrophysics::Galaxy Astrophysics, Physics, education.field_of_study, Science & Technology, FLAMES TARANTULA SURVEY, MULTIPLICITY, OBSERVATIONAL CAMPAIGN, Astronomy and Astrophysics, PULSAR, stars: early-type, ROTATIONAL VELOCITIES, galaxies: Magellanic Clouds, Galaxy, stars: massive, Black hole, VARIABILITY, Stars, Supernova, open clusters and associations: individual: 30 Doradus, Astrophysics - Solar and Stellar Astrophysics, Space and Planetary Science, Physical Sciences, BLACK-HOLE, Probability distribution, binaries: spectroscopic, MASSIVE STARS
Abstract: We present results from the B-type Binaries Characterisation (BBC) programme, a multi-epoch spectroscopic study of 88 early B-type binary candidates in the 30 Doradus region of the Large Magellanic Cloud (LMC). From radial-velocity analysis of 29 observational epochs we confirm the binary status of 64 of our targets, comprising 50 SB1 and 14 SB2 B-type binaries. A further 20 systems (classified as SB1*) show clear signs of periodicity but with more tentative periods. Orbital solutions are presented for these 84 systems, providing the largest homogeneous sample to date of the binary properties of early B-type stars. Our derived orbital-period distribution is generally similar to those for samples of more massive (O-type) binaries in both the LMC and the Galaxy. This similarity with the properties of the more massive O-type binaries is important as early B-type stars are expected to account for the majority of core-collapse supernovae. Differences in the period distributions of the different samples start to increase above 4 d, and are also present between the earliest (B0-0.7) and later-type (B1-2.5) systems within the BBC sample, although further study is required to understand if this is an observational bias or a real physical effect. We have examined the semi-amplitude velocities and orbital periods of our sample to identify potential candidates that could hide compact companions. Comparing with probability distributions of finding black hole companions to OB-type stars from a recent theoretical study, we have found 16 binaries in the higher probability region that warrant further study., 42 pages (main body: 28 pages, supplementary material: 14 pages), 20 figures. Accepted for publication in MNRAS
Published: 2021

31. Searches for continuous gravitational waves from young supernova remnants in the early third observing run of advanced LIGO and Virgo

Author: Abbott R.a, Abbott T.D.b, Abraham S.c, Acernese F.d, e, Ackley K.f, Adams A.g, Adams C.h, Adhikari R.X.a, Adya V.B.i, Affeldt C.j, k, Agarwal D.c, Agathos M.l, m, Agatsuma K.n, Aggarwal N.o, Aguiar O.D.p, Aiello L.q, r, s, Ain A.t, u, Ajith P.v, Akutsu T.w, x, Aleman K.M.y, Allen G.z, Allocca A.e, Altin P.A.i, Amato A.ab, Anand S.a, Ananyeva A.a, Anderson S.B.a, Anderson W.G.ac, Ando M.ad, Angelova S.V.af, Ansoldi S.ag, Antelis J.M.ai, Antier S.aj, Appert S.a, Arai K.ak, Arai K.a, Arai Y.ak, Araki S.al, Araya A.am, Araya M.C.a, Areeda J.S.y, Arène M.aj, Aritomi N.ad, Arnaud N.an, Aronson S.M.ap, Arun K.G.aq, Asada H.ar, Asali Y.as, Ashton G.f, Aso Y.at, Aston S.M.h, Astone P.av, Aubin F.aw, Aufmuth P.j, AultONeal K.ai, Austin C.b, Babak S.aj, Badaracco F.r, Bader M.K.M.ax, Bae S.ay, Bae Y.az, Baer A.M.g, Bagnasco S.ba, Bai Y.a, Baiotti L.bb, Baird J.aj, Bajpai R.bc, Ball M.bd, Ballardin G.ao, Ballmer S.W.be, Bals M.ai, Balsamo A.g, Baltus G.bf, Banagiri S.bg, Bankar D.c, Bankar R.S.c, Barayoga J.C.a, Barbieri C.bh, Barish B.C.a, Barker D.bk, Barneo P.bl, Barone F.e, Barr B.bn, Barsotti L.bo, Barsuglia M.aj, Barta D.bp, Bartlett J.bk, Barton M.A.w, Bartos I.ap, Bassiri R.bq, Basti A.t, Bawaj M.br, Bayley J.C.bn, Baylor A.C.ac, Bazzan M.bt, Bécsy B.bv, Bedakihale V.M.bw, Bejger M.bx, Belahcene I.an, Benedetto V.by, Beniwal D.bz, Benjamin M.G.ai, Bennett T.F.ca, Bentley J.D.n, BenYaala M.af, Bergamin F.j, Berger B.K.bq, Bernuzzi S.m, Bersanetti D.cb, Bertolini A.ax, Betzwieser J.h, Bhandare R.cc, Bhandari A.V.c, Bhattacharjee D.cd, Bhaumik S.ap, Bidler J.y, Bilenko I.A.ce, Billingsley G.a, Birney R.cf, Birnholtz O.cg, Biscans S.a, Bischi M.ch, Biscoveanu S.bo, Bisht A.j, Biswas B.c, Bitossi M.t, Bizouard M.-A.cj, Blackburn J.K.a, Blackman J.ck, Blair C.D.h, Blair D.G.cl, Blair R.M.bk, Bobba F.cm, Bode N.j, Boer M.cj, Bogaert G.cj, Boldrini M.av, Bondu F.cp, Bonilla E.bq, Bonnand R.aw, Booker P.j, Boom B.A.ax, Bork R.a, Boschi V.t, Bose N.cq, Bose S.c, Bossilkov V.cl, Boudart V.bf, Bouffanais Y.bt, Bozzi A.ao, Bradaschia C.t, Brady P.R.ac, Bramley A.h, Branch A.h, Branchesi M.r, Brau J.E.bd, Breschi M.m, Briant T.cr, Briggs J.H.bn, Brillet A.cj, Brinkmann M.j, Brockill P.ac, Brooks A.F.a, Brooks J.ao, Brown D.D.bz, Brunett S.a, Bruno G.cs, Bruntz R.g, Bryant J.n, Buikema A.bo, Bulik T.ct, Bulten H.J.ax, Buonanno A.cv, Buscicchio R.n, Buskulic D.aw, Byer R.L.bq, Cadonati L.cx, Caesar M.cy, Cagnoli G.ab, Cahillane C.a, Cain H.W., IIIb, Bustillo J.C.cz, Callaghan J.D.bn, Callister T.A.da, Calloni E.e, Camp J.B.dc, Canepa M.cb, Cannavacciuolo M.cm, Cannon K.C.ae, Cao H.bz, Cao J.de, Cao Z.df, Capocasa E.w, Capote E.y, Carapella G.cm, Carbognani F.ao, Carlin J.B.dg, Carney M.F.o, Carpinelli M.dh, Carullo G.t, Carver T.L.q, Diaz J.C.ao, Casentini C.dj, Castaldi G.dl, Caudill S.ax, Cavaglià M.cd, Cavalier F.an, Cavalieri R.ao, Cella G.t, Cerdá-Durán P.do, Cesarini E.dk, Chaibi W.cj, Chakravarti K.c, Champion B.dp, Chan C.-H.dq, Chan C.ae, Chan C.L.cz, Chan M.dr, Chandra K.cq, Chanial P.ao, Chao S.dq, Charlton P.ds, Chase E.A.o, Chassande-Mottin E.aj, Chatterjee D.ac, Chaturvedi M.cc, Chen A.cz, Chen C.dt, Chen H.Y.dv, Chen J.dq, Chen K.dw, Chen X.cl, Chen Y.-B.ck, Chen Y.-R.du, Chen Z.q, Cheng H.ap, Cheong C.K.cz, Cheung H.Y.cz, Chia H.Y.ap, Chiadini F.cn, Chiang C.-Y.dy, Chierici R.dz, Chincarini A.cb, Chiofalo M.L.t, Chiummo A.ao, Cho G.ea, Cho H.S.eb, Choate S.cy, Choudhary R.K.cl, Choudhary S.c, Christensen N.cj, Chu H.dw, Chu Q.cl, Chu Y.-K.dy, Chua S.cr, Chung K.W.ec, Ciani G.bt, Ciecielag P.bx, Cie?lar M.bx, Cifaldi M.dj, Ciobanu A.A.bz, Ciolfi R.bu, Cipriano F.cj, Cirone A.cb, Clara F.bk, Clark E.N.ee, Clark J.A.cx, Clarke L.ef, Clearwater P.dg, Clesse S.eg, Cleva F.cj, Coccia E.r, Cohadon P.-F.cr, Cohen D.E.an, Cohen L.b, Colleoni M.eh, Collette C.G.ei, Colpi M.bh, Compton C.M.bk, Constancio M., Jr.p, Conti L.bu, Cooper S.J.n, Corban P.h, Corbitt T.R.b, Cordero-Carrión I.ej, Corezzi S.br, Corley K.R.as, Cornish N.bv, Corre D.an, Corsi A.ek, Cortese S.ao, Costa C.A.p, Cotesta R.cw, Coughlin M.W.bg, Coughlin S.B.o, q, Coulon J.-P.cj, Countryman S.T.as, Cousins B.el, Couvares P.a, Covas P.B.eh, Coward D.M.cl, Cowart M.J.h, Coyne D.C.a, Coyne R.em, Creighton J.D.E.ac, Creighton T.D.en, Criswell A.W.bg, Croquette M.cr, Crowder S.G.eo, Cudell J.R.bf, Cullen T.J.b, Cumming A.bn, Cummings R.bn, Cuoco E.t, Cury?o M.ct, Dal Canton T.an, Dálya G.eq, Dana A.bq, DaneshgaranBajastani L.M.ca, D'Angelo B.cb, Danilishin S.L.er, D'Antonio S.dk, Danzmann K.j, Darsow-Fromm C.es, Dasgupta A.bw, Datrier L.E.H.bn, Dattilo V.ao, Dave I.cc, Davier M.an, Davies G.S.et, Davis D.a, Daw E.J.ev, Dean R.cy, DeBra D.bq, Deenadayalan M.c, Degallaix J.ew, De Laurentis M.e, Deléglise S.cr, Del Favero V.dp, De Lillo F.cs, De Lillo N.bn, Del Pozzo W.t, DeMarchi L.M.o, De Matteis F.dj, D'Emilio V.q, Demos N.bo, Dent T.et, Depasse A.cs, De Pietri R.ex, De Rosa R.e, De Rossi C.ao, DeSalvo R.dl, De Simone R.dx, Dhurandhar S.c, Díaz M.C.en, Diaz-Ortiz M., Jr.ap, Didio N.A.be, Dietrich T.cw, Di Fiore L.e, Di Fronzo C.n, Di Giorgio C.cm, Di Giovanni F.do, Di Girolamo T.e, Di Lieto A.t, Ding B.ei, Di Pace S.av, Di Palma I.av, Di Renzo F.t, Divakarla A.K.ap, Dmitriev A.n, Doctor Z.bd, D'Onofrio L.e, Donovan F.bo, Dooley K.L.q, Doravari S.c, Dorrington I.q, Drago M.r, Driggers J.C.bk, Drori Y.a, Du Z.de, Ducoin J.-G.an, Dupej P.bn, Durante O.cm, D'Urso D.dh, Duverne P.-A.an, Dwyer S.E.bk, Easter P.J.f, Ebersold M.ez, Eddolls G.bn, Edelman B.bd, Edo T.B.a, Edy O.eu, Effler A.h, Eguchi S.dr, Eichholz J.i, Eikenberry S.S.ap, Eisenmann M.aw, Eisenstein R.A.bo, Ejlli A.q, Enomoto Y.ad, Errico L.e, Essick R.C.dv, Estellés H.eh, Estevez D.fa, Etienne Z.fb, Etzel T.a, Evans M.bo, Evans T.M.h, Ewing B.E.el, Fafone V.r, Fair H.be, Fairhurst S.q, Fan X.de, Farah A.M.dv, Farinon S.cb, Farr B.bd, Farr W.M.da, Farrow N.W.f, Fauchon-Jones E.J.q, Favata M.fc, Fays M.bf, Fazio M.fd, Feicht J.a, Fejer M.M.bq, Feng F.aj, Fenyvesi E.bp, Ferguson D.L.cx, Fernandez-Galiana A.bo, Ferrante I.t, Ferreira T.A.p, Fidecaro F.t, Figura P.ct, Fiori I.ao, Fishbach M.o, Fisher R.P.g, Fittipaldi R.cn, Fiumara V.cn, Flaminio R.w, Floden E.bg, Flynn E.y, Fong H.ae, Font J.A.do, Fornal B.fi, Forsyth P.W.F.i, Franke A.es, Frasca S.av, Frasconi F.t, Frederick C.fj, Frei Z.eq, Freise A.fk, Frey R.bd, Fritschel P.bo, Frolov V.V.h, Fronzé G.G.ba, Fujii Y.fl, Fujikawa Y.fm, Fukunaga M.ak, Fukushima M.x, Fulda P.ap, Fyffe M.h, Gabbard H.A.bn, Gadre B.U.cw, Gaebel S.M.n, Gair J.R.cw, Gais J.cz, Galaudage S.f, Gamba R.m, Ganapathy D.bo, Ganguly A.v, Gao D.fn, Gaonkar S.G.c, Garaventa B.cb, García-Núñez C.cf, García-Quirós C.eh, Garufi F.e, Gateley B.bk, Gaudio S.ai, Gayathri V.ap, Ge G.fn, Gemme G.cb, Gennai A.t, George J.cc, Gergely L.fo, Gewecke P.es, Ghonge S.cx, Ghosh A.cw, Ghosh A.fp, Ghosh S.ac, Ghosh S.q, Ghosh S.ap, Giacomazzo B.bh, Giacoppo L.av, Giaime J.A.b, h, Giardina K.D.h, Gibson D.R.cf, Gier C.af, Giesler M.ck, Giri P.t, Gissi F.by, Glanzer J.b, Gleckl A.E.y, Godwin P.el, Goetz E.fq, Goetz R.ap, Gohlke N.j, Goncharov B.f, González G.b, Gopakumar A.fr, Gosselin M.ao, Gouaty R.aw, Grace B.i, Grado A.e, Granata M.ew, Granata V.cm, Grant A.bn, Gras S.bo, Grassia P.a, Gray C.bk, Gray R.bn, Greco G.br, Green A.C.ap, Green R.q, Gretarsson A.M.ai, Gretarsson E.M.ai, Griffith D.a, Griffiths W.q, Griggs H.L.cx, Grignani G.br, Grimaldi A.ft, Grimes E.ai, Grimm S.J.r, Grote H.q, Grunewald S.cw, Gruning P.an, Guerrero J.G.y, Guidi G.M.ch, Guimaraes A.R.b, Guixé G.bl, Gulati H.K.bw, Guo H.-K.fi, Guo Y.ax, Gupta A.a, Gupta A.fv, Gupta P.ax, Gustafson E.K.a, Gustafson R.fw, Guzman F.ee, Ha S.fx, Haegel L.aj, Hagiwara A.ak, Haino S.dy, Halim O.ah, Hall E.D.bo, Hamilton E.Z.q, Hammond G.bn, Han W.-B.ga, Haney M.ez, Hanks J.bk, Hanna C.el, Hannam M.D.q, Hannuksela O.A.ax, Hansen H.bk, Hansen T.J.ai, Hanson J.h, Harder T.cj, Hardwick T.b, Haris K.v, Harms J.r, Harry G.M.gb, Harry I.W.eu, Hartwig D.es, Hasegawa K.ak, Haskell B.bx, Hasskew R.K.h, Haster C.-J.bo, Hattori K.gc, Haughian K.bn, Hayakawa H.gd, Hayama K.dr, Hayes F.J.bn, Healy J.dp, Heidmann A.cr, Heintze M.C.h, Heinze J.j, Heinzel J.ge, Heitmann H.cj, Hellman F.gf, Hello P.an, Helmling-Cornell A.F.bd, Hemming G.ao, Hendry M.bn, Heng I.S.bn, Hennes E.ax, Hennig J.j, Hennig M.H.j, Vivanco F.H.f, Heurs M.j, Hild S.ax, Hill P.af, Himemoto Y.gg, Hines A.S.ee, Hiranuma Y.gh, Hirata N.w, Hirose E.ak, Hochheim S.j, Hofman D.ew, Hohmann J.N.es, Holgado A.M.z, Holland N.A.i, Hollows I.J.ev, Holmes Z.J.bz, Holt K.h, Holz D.E.dv, Hong Z.gi, Hopkins P.q, Hough J.bn, Howell E.J.cl, Hoy C.G.q, Hoyland D.n, Hreibi A.j, Hsieh B.-H.ak, Hsu Y.dq, Huang G.-Z.gi, Huang H.-Y.dy, Huang P.fn, Huang Y.-C.du, Huang Y.-J.dy, Huang Y.-W.bo, Hübner M.T.f, Huddart A.D.ef, Huerta E.A.z, Hughey B.ai, Hui D.C.Y.gj, Hui V.aw, Husa S.eh, Huttner S.H.bn, Huxford R.el, Huynh-Dinh T.h, Ide S.gk, Idzkowski B.ct, Iess A.dj, Ikenoue B.x, Imam S.gi, Inayoshi K.gl, Inchauspe H.ap, Ingram C.bz, Inoue Y.dw, Intini G.av, Ioka K.gm, Isi M.bo, Isleif K.es, Ito K.gn, Itoh Y.go, Iyer B.R.v, Izumi K.gq, JaberianHamedan V.cl, Jacqmin T.cr, Jadhav S.J.gr, Jadhav S.P.c, James A.L.q, Jan A.Z.dp, Jani K.cx, Janssens K.gs, Janthalur N.N.gr, Jaranowski P.gt, Jariwala D.ap, Jaume R.eh, Jenkins A.C.ec, Jeon C.gu, Jeunon M.bg, Jia W.bo, Jiang J.ap, Jin H.-B.gv, Johns G.R.g, Jones A.W.cl, Jones D.I.gx, Jones J.D.bk, Jones P.n, Jones R.bn, Jonker R.J.G.ax, Ju L.cl, Jung K.fx, Jung P.gd, Junker J.j, Kaihotsu K.gn, Kajita T.gy, Kakizaki M.gc, Kalaghatgi C.V.q, Kalogera V.o, Kamai B.a, Kamiizumi M.gd, Kanda N.go, Kandhasamy S.c, Kang G.ay, Kanner J.B.a, Kao Y.dq, Kapadia S.J.v, Kapasi D.P.i, Karat S.a, Karathanasis C.gz, Karki S.cd, Kashyap R.el, Kasprzack M.a, Kastaun W.j, Katsanevas S.ao, Katsavounidis E.bo, Katzman W.h, Kaur T.cl, Kawabe K.bk, Kawaguchi K.ak, Kawai N.ha, Kawasaki T.ad, Kéfélian F.cj, Keitel D.eh, Key J.S.hb, Khadka S.bq, Khalili F.Y.ce, Khan I.r, Khan S.q, Khazanov E.A.hc, Khetan N.r, Khursheed M.cc, Kijbunchoo N.i, Kim C.gu, Kim J.C.he, Kim J.hf, Kim K.hg, Kim W.S.az, Kim Y.-M.fx, Kimball C.o, Kimura N.fy, King P.J.bk, Kinley-Hanlon M.bn, Kirchhoff R.j, Kissel J.S.bk, Kita N.ad, Kitazawa H.gn, Kleybolte L.es, Klimenko S.ap, Knee A.M.fq, Knowles T.D.fb, Knyazev E.bo, Koch P.j, Koekoek G.ax, Kojima Y.hh, Kokeyama K.gd, Koley S.ax, Kolitsidou P.q, Kolstein M.gz, Komori K.ad, Kondrashov V.a, Kong A.K.H.du, Kontos A.hi, Koper N.j, Korobko M.es, Kotake K.dr, Kovalam M.cl, Kozak D.B.a, Kozakai C.at, Kozu R.hj, Kringel V.j, Krishnendu N.V.j, Królak A.hk, Kuehn G.j, Kuei F.dq, Kumar A.gr, Kumar P.hm, Kumar R.bk, Kumar R.bw, Kume J.ae, Kuns K.bo, Kuo C.dw, Kuo H.-S.gi, Kuromiya Y.gn, Kuroyanagi S.hn, Kusayanagi K.ha, Kwak K.fx, Kwang S.ac, Laghi D.t, Lalande E.ho, Lam T.L.cz, Lamberts A.cj, Landry M.bk, Lane B.B.bo, Lang R.N.bo, Lange J.dp, Lantz B.bq, la Rosa I.aw, Lartaux-Vollard A.an, Lasky P.D.f, Laxen M.h, Lazzarini A.a, Lazzaro C.bt, Leaci P.av, Leavey S.j, Lecoeuche Y.K.bk, Lee H.K.hr, Lee H.M.hg, Lee H.W.he, Lee J.ea, Lee K.bq, Lee R.du, Lehmann J.j, Lemaître A.hs, Leon E.y, Leonardi M.w, Leroy N.an, Letendre N.aw, Levin Y.f, Leviton J.N.fw, Li A.K.Y.a, Li B.dq, Li J.o, Li K.L.du, Li T.G.F.cz, Li X.ck, Lin C.-Y.ht, Lin F.-K.dy, Lin F.-L.gi, Lin H.L.dw, Lin L.C.-C.fx, Linde F.ax, Linker S.D.ca, Linley J.N.bn, Littenberg T.B.hv, Liu G.C.dt, Liu J.j, Liu K.dq, Liu X.ac, Llorens-Monteagudo M.do, Lo R.K.L.a, Lockwood A.hw, Lollie M.L.b, London L.T.bo, Longo A.hx, Lopez D.ez, Lorenzini M.dj, Loriette V.hz, Lormand M.h, Losurdo G.t, Lough J.D.j, Lousto C.O.dp, Lovelace G.y, Lück H.j, Lumaca D.dj, Lundgren A.P.eu, Luo L.-W.dy, Macas R.q, MacInnis M.bo, Macleod D.M.q, MacMillan I.A.O.a, Macquet A.cj, Hernandez I.M.ac, Magaña-Sandoval F.ap, Magazzù C.t, Magee R.M.el, Maggiore R.n, Majorana E.av, Makarem C.a, Maksimovic I.hz, Maliakal S.a, Malik A.cc, Man N.cj, Mandic V.bg, Mangano V.av, Mango J.L.ia, Mansell G.L.bk, Manske M.ac, 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J., Soni, K., Soni, S., Sorazu, B., Sordini, V., Sorrentino, F., Sorrentino, N., Sotani, H., Soulard, R., Souradeep, T., Sowell, E., Spagnuolo, V., Spencer, A. P., Spera, M., Srivastava, A. K., Srivastava, V., Staats, K., Stachie, C., Steer, D. A., Steinlechner, J., Steinlechner, S., Stops, D. J., Stover, M., Strain, K. A., Strang, L. C., Stratta, G., Strunk, A., Sturani, R., Stuver, A. L., Sudbeck, J., Sudhagar, S., Sudhir, V., Sugimoto, R., Suh, H. G., Summerscales, T. Z., Sun, H., Sun, L., Sunil, S., Sur, A., Suresh, J., Sutton, P. J., Suzuki, T., Swinkels, B. L., Szczepanczyk, M. J., Szewczyk, P., Tacca, M., Tagoshi, H., Tait, S. C., Takahashi, H., Takahashi, R., Takamori, A., Takano, S., Takeda, H., Takeda, M., Talbot, C., Tanaka, H., Tanaka, K., Tanaka, T., Tanasijczuk, A. J., Tanioka, S., Tanner, D. B., Tao, D., Tapia, A., Martin, E. N. T. S., Tasson, J. D., Telada, S., Tenorio, R., Terkowski, L., Test, M., Thirugnanasambandam, M. P., Thomas, M., Thomas, P., Thompson, J. 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M., Vardaro, M., Vargas, A. F., Varma, V., Vasuth, M., Vecchio, A., Vedovato, G., Veitch, J., Veitch, P. J., Venkateswara, K., Venneberg, J., Venugopalan, G., Verkindt, D., Verma, Y., Veske, D., Vetrano, F., Vicere, A., Viets, A. D., Villa-Ortega, V., Vinet, J. -Y., Vitale, S., Vo, T., Vocca, H., von Reis, E. R. G., von Wrangel, J., Vorvick, C., Vyatchanin, S. P., Wade, L. E., Wade, M., Wagner, K. J., Walet, R. C., Walker, M., Wallace, G. S., Wallace, L., Walsh, S., Wang, J., Wang, J. Z., Wang, W. H., Ward, R. L., Warner, J., Was, M., Washimi, T., Washington, N. Y., Watchi, J., Weaver, B., Wei, L., Weinert, M., Weinstein, A. J., Weiss, R., Weller, C. M., Wellmann, F., Wen, L., Wessels, P., Westhouse, J. W., Wette, K., Whelan, J. T., White, D. D., Whiting, B. F., Whittle, C., Wilken, D., Williams, D., Williams, M. J., Williamson, A. R., Willis, J. L., Willke, B., Wilson, D. J., Winkler, W., Wipf, C. C., Wlodarczyk, T., Woan, G., Woehler, J., Wofford, J. K., Wong, I. C. F., Wu, C., Wu, D. S., Wu, H., Wu, S., Wysocki, D. M., Xiao, L., Xu, W. -R., Yamada, T., Yamamoto, H., Yamamoto, K., Yamamoto, T., Yamashita, K., Yamazaki, R., Yang, F. W., Yang, L., Yang, Y., Yang, Z., Yap, M. J., Yeeles, D. W., Yelikar, A. B., Ying, M., Yokogawa, K., Yokoyama, J., Yokozawa, T., Yoon, A., Yoshioka, T., Yu, H., Yuzurihara, H., Zadrozny, A., Zanolin, M., Zeidler, S., Zelenova, T., Zendri, J. -P., Zevin, M., Zhan, M., Zhang, H., Zhang, J., Zhang, L., Zhang, R., Zhang, T., Zhao, C., Zhao, G., Zhao, Y., Zhou, Z., Zhu, X. J., Zhu, Z. -H., Zucker, M. 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Jeunon, M, Jia, W, Jiang, J, Jin, H, Johns, G, Jones, A, Jones, D, Jones, J, Jones, P, Jones, R, Jonker, R, Ju, L, Jung, K, Jung, P, Junker, J, Kaihotsu, K, Kajita, T, Kakizaki, M, Kalaghatgi, C, Kalogera, V, Kamai, B, Kamiizumi, M, Kanda, N, Kandhasamy, S, Kang, G, Kanner, J, Kao, Y, Kapadia, S, Kapasi, D, Karat, S, Karathanasis, C, Karki, S, Kashyap, R, Kasprzack, M, Kastaun, W, Katsanevas, S, Katsavounidis, E, Katzman, W, Kaur, T, Kawabe, K, Kawaguchi, K, Kawai, N, Kawasaki, T, Kefelian, F, Keitel, D, Key, J, Khadka, S, Khalili, F, Khan, I, Khan, S, Khazanov, E, Khetan, N, Khursheed, M, Kijbunchoo, N, Kim, C, Kim, J, Kim, K, Kim, W, Kim, Y, Kimball, C, Kimura, N, King, P, Kinley-Hanlon, M, Kirchhoff, R, Kissel, J, Kita, N, Kitazawa, H, Kleybolte, L, Klimenko, S, Knee, A, Knowles, T, Knyazev, E, Koch, P, Koekoek, G, Kojima, Y, Kokeyama, K, Koley, S, Kolitsidou, P, Kolstein, M, Komori, K, Kondrashov, V, Kong, A, Kontos, A, Koper, N, Korobko, M, Kotake, K, Kovalam, M, Kozak, D, Kozakai, C, Kozu, R, Kringel, V, Krishnendu, N, Krolak, A, Kuehn, G, Kuei, F, Kumar, A, Kumar, P, Kumar, R, Kume, J, Kuns, K, Kuo, C, Kuo, H, Kuromiya, Y, Kuroyanagi, S, Kusayanagi, K, Kwak, K, Kwang, S, Laghi, D, Lalande, E, Lam, T, Lamberts, A, Landry, M, Lane, B, Lang, R, Lange, J, Lantz, B, la Rosa, I, Lartaux-Vollard, A, Lasky, P, Laxen, M, Lazzarini, A, Lazzaro, C, Leaci, P, Leavey, S, Lecoeuche, Y, Lee, H, Lee, J, Lee, K, Lee, R, Lehmann, J, Lemaitre, A, Leon, E, Leonardi, M, Leroy, N, Letendre, N, Levin, Y, Leviton, J, Li, A, Li, B, Li, J, Li, K, Li, T, Li, X, Lin, C, Lin, F, Lin, H, Lin, L, Linde, F, Linker, S, Linley, J, Littenberg, T, Liu, G, Liu, J, Liu, K, Liu, X, Llorens-Monteagudo, M, Lo, R, Lockwood, A, Lollie, M, London, L, Longo, A, Lopez, D, Lorenzini, M, Loriette, V, Lormand, M, Losurdo, G, Lough, J, Lousto, C, Lovelace, G, Luck, H, Lumaca, D, Lundgren, A, Luo, L, Macas, R, Macinnis, M, Macleod, D, Macmillan, I, Macquet, A, Hernandez, I, Magana-Sandoval, F, Magazzu, 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Szewczyk, P, Tacca, M, Tagoshi, H, Tait, S, Takahashi, H, Takahashi, R, Takamori, A, Takano, S, Takeda, H, Takeda, M, Talbot, C, Tanaka, H, Tanaka, K, Tanaka, T, Tanasijczuk, A, Tanioka, S, Tanner, D, Tao, D, Tapia, A, Martin, E, Tasson, J, Telada, S, Tenorio, R, Terkowski, L, Test, M, Thirugnanasambandam, M, Thomas, M, Thomas, P, Thompson, J, Thondapu, S, Thorne, K, Thrane, E, Tiwari, S, Tiwari, V, Toland, K, Tolley, A, Tomaru, T, Tomigami, Y, Tomura, T, Tonelli, M, Torres-Forne, A, Torrie, C, Tosta e Melo, I, Toyra, D, Trapananti, A, Travasso, F, Traylor, G, Tringali, M, Tripathee, A, Troiano, L, Trovato, A, Trozzo, L, Trudeau, R, Tsai, D, Tsang, K, Tsang, T, Tsao, J, Tse, M, Tso, R, Tsubono, K, Tsuchida, S, Tsukada, L, Tsuna, D, Tsutsui, T, Tsuzuki, T, Turconi, M, Tuyenbayev, D, Ubhi, A, Uchikata, N, Uchiyama, T, Udall, R, Ueda, A, Uehara, T, Ueno, K, Ueshima, G, Ugolini, D, Unnikrishnan, C, Uraguchi, F, Urban, A, Ushiba, T, Usman, S, Utina, A, Vahlbruch, H, Vajente, G, Vajpeyi, A, Valdes, G, Valentini, M, Valsan, V, van Bakel, N, van Beuzekom, M, van den Brand, J, van Den Broeck, C, Vander-Hyde, D, van der Schaaf, L, van Heijningen, J, Vanosky, J, van Putten, M, Vardaro, M, Vargas, A, Varma, V, Vasuth, M, Vecchio, A, Vedovato, G, Veitch, J, Veitch, P, Venkateswara, K, Venneberg, J, Venugopalan, G, Verkindt, D, Verma, Y, Veske, D, Vetrano, F, Vicere, A, Viets, A, Villa-Ortega, V, Vinet, J, Vitale, S, Vo, T, Vocca, H, von Reis, E, von Wrangel, J, Vorvick, C, Vyatchanin, S, Wade, L, Wade, M, Wagner, K, Walet, R, Walker, M, Wallace, G, Wallace, L, Walsh, S, Wang, J, Wang, W, Ward, R, Warner, J, Was, M, Washimi, T, Washington, N, Watchi, J, Weaver, B, Wei, L, Weinert, M, Weinstein, A, Weiss, R, Weller, C, Wellmann, F, Wen, L, Wessels, P, Westhouse, J, Wette, K, Whelan, J, White, D, Whiting, B, Whittle, C, Wilken, D, Williams, D, Williams, M, Williamson, A, Willis, J, Willke, B, Wilson, D, Winkler, W, Wipf, C, Wlodarczyk, T, Woan, G, Woehler, J, Wofford, J, Wong, I, Wu, C, Wu, D, Wu, H, Wu, S, Wysocki, D, Xiao, L, Xu, W, Yamada, T, Yamamoto, H, Yamamoto, K, Yamamoto, T, Yamashita, K, Yamazaki, R, Yang, F, Yang, L, Yang, Y, Yang, Z, Yap, M, Yeeles, D, Yelikar, A, Ying, M, Yokogawa, K, Yokoyama, J, Yokozawa, T, Yoon, A, Yoshioka, T, Yu, H, Yuzurihara, H, Zadrozny, A, Zanolin, M, Zeidler, S, Zelenova, T, Zendri, J, Zevin, M, Zhan, M, Zhang, H, Zhang, J, Zhang, L, Zhang, R, Zhang, T, Zhao, C, Zhao, G, Zhao, Y, Zhou, Z, Zhu, X, Zhu, Z, Zucker, M, Zweizig, J, The LIGO Scientific Collaboration, The Virgo Collaboration, The KAGRA Collaboration, Arai, Koya, Arai, Koji, Arène, M., Bécsy, B., Cain III, H. W., Calderón Bustillo, J., Casanueva Diaz, J., Cavaglià, M., Cerdá-Durán, P., Chiang, C-Y., Chu, Y-K., Cieślar, M., Constancio Jr., M., Cordero-Carrión, I., Curyło, M., Dálya, G., D’Angelo, B., D’Antonio, S., Deléglise, S., D’Emilio, V., Díaz, M. C., Diaz-Ortiz Jr., M., D’Onofrio, L., D’Urso, D., Estellés, H., Fronzé, G. G., García-Núñez, C., García-Quirós, C., Ghosh, Abhirup., Ghosh, Archisman, Ghosh, Shaon, Ghosh, Shrobana, Ghosh, Sourath, González, G., Guixé, G., Gupta, Anchal, Gupta, Anuradha, Hernandez Vivanco, F., Hsieh, B-H., Huang, G-Z., Huang, H-Y., Huang, Y-C., Hübner, M. T., Kéfélian, F., Królak, A., Kumar, Rahul, Kumar, Rakesh, Kuo, H-S., La Rosa, I., Lemaître, A., Lin, C-Y., Lin, F-K., Lin, F-L., Lück, H., Magaña Hernandez, I., Magaña-Sandoval, F., Magazzù, C., Márka, S., Márka, Z., Mo, Geoffrey, Mukherjee, Arunava, Mukherjee, Soma, Mukherjee, Subroto, Muñiz, E. A., Nguyen Quynh, L., O’Brien, B. D., O’Dell, J., O’Reilly, B., O’Shaughnessy, R., O’Shea, E., Peña Arellano, F. E., Périgois, C., Perriès, S., Pürrer, M., Rosińska, D., Roy, Santosh, Roy, Soumen, Schönbeck, A., Südbeck, J., Suzuki, Takamasa, Suzuki, Toshikazu, Szczepańczyk, M. J., Tanaka, Kazuyuki, Tanaka, Kenta, Tanaka, Taiki, Tanaka, Takahiro, Tapia San Martin, E. N., Tiwari, Shubhanshu, Tiwari, Srishti, Torres-Forné, A., Töyrä, D., Tsao, J-S., Van Den Broeck, C., Vasúth, M., Viceré, A., Weßels, P., Xu, W-R., Yamamoto, Kazuhiro, Yamamoto, Kohei, Yang, Yang, Yang, Yi, Yu, Hang, Yu, Haocun, Zadrożny, A., Zhao, Yue, and Zhao, Yuhang
Subjects: TIMING NOISE, Astronomy, Supernova remnants (1667), FOS: Physical sciences, Gravitational wave astronomy (675), Gravitational waves (678), Neutron stars (1108), Astrophysics, Astronomy & Astrophysics, Vela, 01 natural sciences, CHANDRA, Pulsar, 0103 physical sciences, Gravitational wave astronomy, Gravitational waves, Neutron stars, Supernova remnants, Supernova remnant, 010303 astronomy & astrophysics, QC, QB, High Energy Astrophysical Phenomena (astro-ph.HE), Physics, Science & Technology, OBJECT, Settore FIS/05, 010308 nuclear & particles physics, Gravitational wave, CONSTRAINTS, Astronomy and Astrophysics, PULSAR, LIGO, G291.0-0.1, CASSIOPEIA, Neutron star, Supernova, DA 495, Amplitude, Space and Planetary Science, Physical Sciences, X-RAY, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Astrophysics - High Energy Astrophysical Phenomena, EMISSION
Abstract: We present results of three wide-band directed searches for continuous gravitational waves from 15 young supernova remnants in the first half of the third Advanced LIGO and Virgo observing run. We use three search pipelines with distinct signal models and methods of identifying noise artifacts. Without ephemerides of these sources, the searches are conducted over a frequency band spanning from 10~Hz to 2~kHz. We find no evidence of continuous gravitational radiation from these sources. We set upper limits on the intrinsic signal strain at 95\% confidence level in sample sub-bands, estimate the sensitivity in the full band, and derive the corresponding constraints on the fiducial neutron star ellipticity and $r$-mode amplitude. The best 95\% confidence constraints placed on the signal strain are $7.7\times 10^{-26}$ and $7.8\times 10^{-26}$ near 200~Hz for the supernova remnants G39.2--0.3 and G65.7+1.2, respectively. The most stringent constraints on the ellipticity and $r$-mode amplitude reach $\lesssim 10^{-7}$ and $ \lesssim 10^{-5}$, respectively, at frequencies above $\sim 400$~Hz for the closest supernova remnant G266.2--1.2/Vela Jr., https://dcc.ligo.org/P2000479
Published: 2021

32. Modeling pulsed radio and gamma-ray emissions from PSRs J2302+4442 and J0659+1414

Author: S. J. Dang, X. Xu, R. S. Zhao, Q. W. Lin, J. T. Bai, Guojun Qiao, Ai-Jun Dong, Y.J. Du, Q. J. Zhi, and L. H. Shang
Subjects: Physics, Millisecond, Astrophysics::High Energy Astrophysical Phenomena, Astrophysics::Instrumentation and Methods for Astrophysics, Gamma ray, Magnetic dip, Astronomy and Astrophysics, Astrophysics, Radiation, Light curve, Viewing angle, Pulsar, Space and Planetary Science, Millisecond pulsar
Abstract: The multi-band observation, from radio to gamma-ray, plays a crucial role in constraining the emission physics and geometrical magnetospheric models of the pulsars. In this paper, We use three-dimensional magnetospheric model, with the joint of the annular gap (AG) and core gap (CG) model, to simulate the radio and gamma-ray light curves for two representative pulsars, a millisecond pulsar J2302+4442 and a young pulsar J0659+1414. It is found that for PSR J2302 + 4442, the simulated magnetic inclination angle α and viewing angle ζ are 34 ∘ and 46 ∘ , and for PSR J0659 + 1414 are 45 ∘ and 33 ∘ . This implies that the radio and gamma-ray pulse emission originates from different magnetospheric regions and the radiation geometry for millisecond and young pulsar is different. The studies show that the joint of the AG and CG model can describe the light curves not only for millisecond pulsars but also for young pulsars, and hence it can be used to explain the multi-wavelength observations of pulsars.
Published: 2021

33. A broad-band radio study of PSR J0250+5854

Author: Chun-sheng Zhang, C.H. Agar, A. Loh, V. I. Kondratiev, J. Künsemöller, Benjamin Stappers, J.N. Girard, Jason W. T. Hessels, Aris Karastergiou, L. Bondonneau, Baptiste Cecconi, Jean-Mathias Grießmeier, Charlotte Sobey, C.M. Tan, Di Li, Patrick Weltevrede, B. Peng, Michael Keith, H.G. Wang, Gilles Theureau, W.J. Huang, Philippe Zarka, Laboratoire de Physique et Chimie de l'Environnement et de l'Espace (LPC2E), Observatoire des Sciences de l'Univers en région Centre (OSUC), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université d'Orléans (UO)-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université d'Orléans (UO)-Centre National de la Recherche Scientifique (CNRS)-Centre National d’Études Spatiales [Paris] (CNES), Laboratoire d'études spatiales et d'instrumentation en astrophysique (LESIA (UMR_8109)), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Unité Scientifique de la Station de Nançay (USN), Centre National de la Recherche Scientifique (CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire des Sciences de l'Univers en région Centre (OSUC), Université Paris sciences et lettres (PSL)-Université d'Orléans (UO)-Centre National de la Recherche Scientifique (CNRS)-Université d'Orléans (UO), Laboratoire Univers et Théories (LUTH (UMR_8102)), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Diderot - Paris 7 (UPD7), Astrophysique Interprétation Modélisation (AIM (UMR_7158 / UMR_E_9005 / UM_112)), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris Diderot - Paris 7 (UPD7), High Energy Astrophys. & Astropart. Phys (API, FNWI), Université Paris sciences et lettres (PSL)-Université d'Orléans (UO)-Centre National de la Recherche Scientifique (CNRS), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Astrophysique Interprétation Modélisation (AIM (UMR7158 / UMR_E_9005 / UM_112)), and Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS)
Subjects: Astrophysics::High Energy Astrophysical Phenomena, Population, Polarimetry, FOS: Physical sciences, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, polarisation, magnetars, Magnetar, 01 natural sciences, neutron stars, stars: neutron, stars: magnetars, Pulsar, 0103 physical sciences, education, 010303 astronomy & astrophysics, High Energy Astrophysical Phenomena (astro-ph.HE), Physics, polarization, pulsars: individual: PSR J0250+5854, education.field_of_study, Spectral index, 010308 nuclear & particles physics, Conjunction (astronomy), Astrophysics::Instrumentation and Methods for Astrophysics, Astronomy and Astrophysics, LOFAR, Polarization (waves), PSR J0250+5854, [SDU]Sciences of the Universe [physics], Space and Planetary Science, pulsars, broadband, Astrophysics - High Energy Astrophysical Phenomena, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph]
Abstract: We present radio observations of the most slowly rotating known radio pulsar PSR J0250+5854. With a 23.5 s period, it is close, or even beyond, the $P$-$\dot{P}$ diagram region thought to be occupied by active pulsars. The simultaneous observations with FAST, the Chilbolton and Effelsberg LOFAR international stations, and NenuFAR represent a five-fold increase in the spectral coverage of this object, with the detections at 1250 MHz (FAST) and 57 MHz (NenuFAR) being the highest- and lowest-frequency published respectively to date. We measure a flux density of $4\pm2$ $\mu$Jy at 1250 MHz and an exceptionally steep spectral index of $-3.5^{+0.2}_{-1.5}$, with a turnover below $\sim$95 MHz. In conjunction with observations of this pulsar with the GBT and the LOFAR Core, we show that the intrinsic profile width increases drastically towards higher frequencies, contrary to the predictions of conventional radius-to-frequency mapping. We examine polarimetric data from FAST and the LOFAR Core and conclude that its polar cap radio emission is produced at an absolute height of several hundreds of kilometres around 1.5 GHz, similar to other rotation-powered pulsars across the population. Its beam is significantly underfilled at lower frequencies, or it narrows because of the disappearance of conal outriders. Finally, the results for PSR J0250+5854 and other slowly spinning rotation-powered pulsars are contrasted with the radio-detected magnetars. We conclude that magnetars have intrinsically wider radio beams than the slow rotation-powered pulsars, and that consequently the latter's lower beaming fraction is what makes objects such as PSR J0250+5854 so scarce., Comment: 14 pages, 6 figures
Published: 2021

34. The observations of the gigahertz‐peaked spectra pulsars

Author: Karolina Rożko
Subjects: Physics, Interstellar medium, Pulsar, Space and Planetary Science, Astronomy and Astrophysics, Astrophysics, Spectral line
Published: 2021

35. The Spectrum Power of Interstellar Plasma Inhomogeneities in the Direction of Eleven Radio Pulsars

Author: T. V. Smirnova and M. V. Popov
Subjects: Physics, Pulsar, Space and Planetary Science, High Energy Physics::Phenomenology, Spectrum (functional analysis), Computer Science::Programming Languages, Computer Science::Symbolic Computation, Astronomy and Astrophysics, Plasma, Astrophysics, Computer Science::Digital Libraries, Power (physics)
Abstract: Abstract We have analyzed two-dimensional correlation functions from the dynamic spectra of 11 pulsars using the archival data of the “Radioastron” project. The time-sections of these functions were approximated by exponential functions with a power $$\alpha $$. It is shown that this approximation describes the shape of the correlation function much better than the Gaussian. The temporal structure function $$D(\Delta t)$$ for small values of the delay $$\Delta t$$is a power law with an index $$\alpha $$. The spectrum power of spatial inhomogeneities of the interstellar plasma is related to the power of the structure function as $$n = \alpha + 2$$. We have determined the characteristic scintillation time and the power $$n$$ in the direction of 11 pulsars. In the direction of three pulsars (B0329+54, B0823+26, and B1929+10), the spectrum power of spatial inhomogeneities of the interstellar plasma turned out to be very close to the value for the Kolmogorov spectrum ($$n = 3.67$$). For other pulsars, it ranges from 3.18 to 3.86. It is shown that the measured scintillation parameters are significantly influenced by the duration of the observation session, expressed by its ratio to the characteristic scintillation time. If this parameter is less than 10, the parameter estimates may be biased: the values of $$\alpha $$ and the characteristic scintillation time $${{t}_{{{\text{scint}}}}}$$ may decrease.
Published: 2021

36. Comparison of Terrestrial and Lunar Time Scales by Giant Pulsar Impulses

Author: Alexander E. Rodin, V. A. Fedorova, and V. V. Oreshko
Subjects: Physics, Pulsar, Space and Planetary Science, Astronomy, Astronomy and Astrophysics, Astrophysics::Earth and Planetary Astrophysics
Abstract: Abstract We have developed a model for the time delay of pulse arrival between stations on the Moon and Earth. Comparison of the lunar and terrestrial time scales is proposed to be carried out by comparing the arrival time moments of giant pulses from pulsars. A method for such a comparison has been developed based on the cross-correlation analysis of the received pulses. Using the example of giant pulses from the pulsar PSR 0531+21, we showed that the error of comparing scales in the case of a high signal-to-noise ratio reaches a sub-discrete level and, thus, is determined by the reception band of the recording equipment.
Published: 2021

37. Neutron Stars and the Nuclear Matter Equation of State

Author: James M. Lattimer
Subjects: Physics, Nuclear and High Energy Physics, Neutron star, Equation of state, Pulsar, Gravitational wave, Astrophysics::High Energy Astrophysical Phenomena, Nuclear Theory, Astrophysics::Earth and Planetary Astrophysics, Astrophysics, Nuclear Experiment, Nuclear matter, Astrophysics::Galaxy Astrophysics
Abstract: Neutron stars provide a window into the properties of dense nuclear matter. Several recent observational and theoretical developments provide powerful constraints on their structure and internal composition. Among these are the first observed binary neutron star merger, GW170817, whose gravitational radiation was accompanied by electromagnetic radiation from a short γ-ray burst and an optical afterglow believed to be due to the radioactive decay of newly minted heavy r-process nuclei. These observations give important constraints on the radii of typical neutron stars and on the upper limit to the neutron star maximum mass and complement recent pulsar observations that established a lower limit. Pulse-profile observations by the Neutron Star Interior Composition Explorer (NICER) X-ray telescope provide an independent, consistent measure of the neutron star radius. Theoretical many-body studies of neutron matter reinforce these estimates of neutron star radii. Studies using parameterized dense matter equations of state (EOSs) reveal several EOS-independent relations connecting global neutron star properties.
Published: 2021

38. Modelling spin-up episodes in accreting millisecond X-ray pulsars

Author: Arthur G. Suvorov and Kostas Glampedakis
Subjects: High Energy Astrophysical Phenomena (astro-ph.HE), Physics, Millisecond, Accretion (meteorology), Astrophysics::High Energy Astrophysical Phenomena, Stellar magnetic field, FOS: Physical sciences, Astronomy and Astrophysics, General Relativity and Quantum Cosmology (gr-qc), Astrophysics, Radius, Approx, General Relativity and Quantum Cosmology, Magnetic field, Pulsar, Space and Planetary Science, Astrophysics::Earth and Planetary Astrophysics, Spin-up, Astrophysics - High Energy Astrophysical Phenomena
Abstract: Accreting millisecond X-ray pulsars are known to provide a wealth of physical information during their successive states of outburst and quiescence. Based on the observed spin-up and spin-down rates of these objects it is possible, among other things, to infer the stellar magnetic field strength and test models of accretion disc flow. In this paper we consider the three accreting X-ray pulsars (XTE J1751-305, IGR J00291+5934, and SAX J1808.4-3658) with the best available timing data, and model their observed spin-up rates with the help of a collection of standard torque models that describe a magnetically-threaded accretion disc truncated at the magnetospheric radius. Whilst none of these models are able to explain the observational data, we find that the inclusion of the physically motivated phenomenological parameter $\xi$, which controls the uncertainty in the location of the magnetospheric radius, leads to an enhanced disc-integrated accretion torque. These 'new' torque models are compatible with the observed spin-up rates as well as the inferred magnetic fields of these objects provided that $\xi \approx 0.1-0.5$. Our results are supplemented with a discussion of the relevance of additional physics effects that include the presence of a multipolar magnetic field and general-relativistic gravity., Comment: 15 pages, 9 figures. Accepted for publication in MNRAS
Published: 2021

39. Resolving dichotomy in compact objects through continuous gravitational waves observation

Author: Tomasz Bulik, Christopher A. Tout, Tushar Mondal, Banibrata Mukhopadhyay, Surajit Kalita, Tout, Christopher [0000-0002-1556-9449], and Apollo - University of Cambridge Repository
Subjects: Gravitational-wave observatory, Astrophysics::High Energy Astrophysical Phenomena, FOS: Physical sciences, radiation mechanisms: general, General Relativity and Quantum Cosmology (gr-qc), Astrophysics, General Relativity and Quantum Cosmology, stars: neutron, Pulsar, stars: rotation, Solar and Stellar Astrophysics (astro-ph.SR), white dwarfs, High Energy Astrophysical Phenomena (astro-ph.HE), Physics, Gravitational wave, stars: magnetic field, White dwarf, Astronomy and Astrophysics, Interferometry, Supernova, Neutron star, gravitational waves, Astrophysics - Solar and Stellar Astrophysics, Space and Planetary Science, Big Bang Observer, Astrophysics - High Energy Astrophysical Phenomena
Abstract: More than two dozen soft gamma-ray repeaters (SGRs) and anomalous X-ray pulsars (AXPs) have been detected so far. These are isolated compact objects. Many of them are either found to be associated with supernova remnants or their surface magnetic fields are directly measured, confirming that they are neutron stars (NSs). However, it has been argued that some SGRs and AXPs are highly magnetized white dwarfs (WDs). Meanwhile, the existence of super-Chandrasekhar WDs has remained to be a puzzle. However, not even a single such massive WD has been observed directly. Moreover, some WD pulsars are detected in electromagnetic surveys and some of their masses are still not confirmed. Here we calculate the signal-to-noise ratio for all these objects, considering different magnetic field configurations and thereby estimate the required time for their detection by various gravitational wave (GW) detectors. For SGRs and AXPs, we show that, if these are NSs, they can hardly be detected by any of the GW detectors, while if they are WDs, Big Bang Observer (BBO), DECi-hertz Interferometer Gravitational wave Observatory (DECIGO) and Advanced Laser Interferometer Antenna (ALIA) would be able to detect them within a few days to a year of integration, depending on the magnetic field strength and its configuration. Similarly, if a super-Chandrasekhar WD has a dominant toroidal field, we show that even Laser Interferometer Space Antenna (LISA) and TianQin would be able to detect it within one year of integration. We also discuss how GWs can confirm the masses of the WD pulsars., 10 pages including 12 figures and 2 tables; Accepted for publication in MNRAS
Published: 2021

40. FAST early pulsar discoveries: Effelsberg follow-up

Author: Luxi Qian, Di Li, Y T Chen, Michael Kramer, Xiao-Yao Xie, Paulo C. C. Freire, Mengyao Xue, K Lackeos, Wenbai Zhu, D. J. Champion, Jiarui Niu, George Hobbs, N.K. Porayko, R. A. Main, M Cruces, A. D. Cameron, Zhizheng Pan, J Wongphecauxon, Yu-Xuan Zhu, S P You, Zhijie Liu, Mao Yuan, X H Yu, Youling Yue, P. J. Wang, Chenchen Miao, E. Graikou, and M Krco
Subjects: High Energy Astrophysical Phenomena (astro-ph.HE), Physics, Electron density, education.field_of_study, Linear polarization, Astrophysics::High Energy Astrophysical Phenomena, media_common.quotation_subject, Population, Astrophysics::Instrumentation and Methods for Astrophysics, FOS: Physical sciences, White dwarf, Astronomy and Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, Orbit, Astrophysics - Solar and Stellar Astrophysics, Pulsar, Space and Planetary Science, Sky, Astrophysics - High Energy Astrophysical Phenomena, education, Solar and Stellar Astrophysics (astro-ph.SR), Astrophysics::Galaxy Astrophysics, media_common, Radio astronomy
Abstract: We report the follow-up of 10 pulsars discovered by the Five-hundred-metre Aperture Spherical radio-Telescope (FAST) during its commissioning. The pulsars were discovered at a frequency of 500-MHz using the ultrawide-band (UWB) receiver in drift-scan mode, as part of the Commensal Radio Astronomy FAST Survey (CRAFTS). We carried out the timing campaign with the 100-m Effelsberg radio-telescope at L-band around 1.36 GHz. Along with 11 FAST pulsars previously reported, FAST seems to be uncovering a population of older pulsars, bordering and/or even across the pulsar death-lines. We report here two sources with notable characteristics. PSR J1951+4724 is a young and energetic pulsar with nearly 100 per cent of linearly polarized flux density and visible up to an observing frequency of 8 GHz. PSR J2338+4818, a mildly recycled pulsar in a 95.2-d orbit with a Carbon–Oxygen white dwarf (WD) companion of $\gtrsim 1\, \rm {M}_{\odot }$, based on estimates from the mass function. This system is the widest WD binary with the most massive companion known to-date. Conspicuous discrepancy was found between estimations based on NE2001 and YMW16 electron density models, which can be attributed to underrepresentation of pulsars in the sky region between Galactic longitudes 70° < l < 100°. This work represents one of the early CRAFTS results, which start to show potential to substantially enrich the pulsar sample and refine the Galactic electron density model.
Published: 2021

41. Profile changes associated with dispersion measure events in PSR J1713+0747

Author: Ue-Li Pen, Robert Main, Jing Luo, Fang Xi Lin, Hsiu-Hsien Lin, Marten H. van Kerkwijk, James Mckee, and D. Simard
Subjects: Physics, 010308 nuclear & particles physics, Astrophysics::High Energy Astrophysical Phenomena, Astronomy and Astrophysics, Astrophysics, Interference (wave propagation), 01 natural sciences, Measure (mathematics), law.invention, Pulse (physics), Amplitude, Pulsar, 13. Climate action, Space and Planetary Science, Achromatic lens, law, 0103 physical sciences, Dispersion (optics), Baseband, 010303 astronomy & astrophysics
Abstract: Propagation effects in the interstellar medium and intrinsic profile changes can cause variability in the timing of pulsars, which limits the accuracy of fundamental science done via pulsar timing. One of the best timing pulsars, PSR J1713+0747, has gone through two ‘dip’ events in its dispersion measure (DM) time series. If these events reflect real changes in electron column density, they should lead to multiple imaging. We show that the events are well fitted by an underdense corrugated sheet model, and look for associated variability in the pulse profile using principal component analysis. We find that there are transient pulse profile variations, but they vary in concert with the DM, unlike what is expected from lensing due to a corrugated sheet. The change is consistent in shape across profiles from both the Green Bank and Arecibo radio observatories, and its amplitude appears to be achromatic across the 820-MHz, 1.4-GHz, and 2.3-GHz bands, again unlike expected from interference between lensed images. This result is puzzling. We note that some of the predicted lensing effects would need higher time and frequency resolution data than used in this analysis. Future events appear likely, and storing baseband data or keeping multiple time–frequency resolutions will allow more in-depth study of propagation effects and hence improvements to pulsar timing accuracy.
Published: 2021

42. The main challenges of Public Sector Accounting reforms and World Bank's Public Sector Accounting and Reporting (PULSAR) Program

Author: Dmitri Gourfinkel
Subjects: Public sector accounting, Public Administration, Pulsar, business.industry, Strategy and Management, Accounting, Business
Abstract: PurposeThe purpose of this article is to contribute to a dialogue between practitioners and academics. The article discusses the relevance of Public Sector Accounting (PSA) reforms, including their key approaches and challenges, and the role of the World Bank's Public Sector Accounting and Reporting (PULSAR) Program.Design/methodology/approachThis is a practitioner's viewpoint, which reflects World Bank and PULSAR Program's publicly available documents and the opinions of a practitioner involved in the implementation of PSA reforms.FindingsImplementation of PSA reforms, based on the good international standards and practices, such as International Public Sector Accounting Standards (IPSAS), represents an opportunity for governments to significantly improve (1) the quality, reliability and comparability of their financial information; (2) decision-making process of the high-level public officials; and (3) the overall levels of fiscal transparency and public sector accountability and performance. There are several main approaches of the PSA reform implementation that could be observed across the globe. In practice, many countries and different jurisdictions face multiple challenges associated with PSA reform implementation. The World Bank and PULSAR Program in particular represent a valuable source of knowledge generation and sharing, and also acts as a catalyst for promoting PSA reforms in beneficiary countries.Research limitations/implicationsThe limitations of this article (which are also its strength in terms of fitness for purpose) are that as a practitioner's viewpoint, it provides a brief overview and personal judgements rather than an empirical analysis of developments applying a theoretical framework.Social implicationsA practitioner's engagement with academic supports increased understanding of the respective views leading to better outcomes for practitioners and academics working in the area of public sector accounting.Originality/valueThe article provides a practitioner's input on the relevance of PSA reforms and their key challenges.
Published: 2021

43. ALMA and NOEMA constraints on synchrotron nebular emission from embryonic superluminous supernova remnants and radio–gamma-ray connection

Author: Geoffrey C. Bower, Conor Omand, D. B. Fox, R. Margutti, Kohta Murase, Ryan Chornock, Hiroshi Nagai, Deanne L. Coppejans, Casey J. Law, Peter Mészáros, and Kazumi Kashiyama
Subjects: High Energy Astrophysical Phenomena (astro-ph.HE), Physics, Astrophysics::High Energy Astrophysical Phenomena, Gamma ray, FOS: Physical sciences, Astronomy and Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, Magnetar, Synchrotron, law.invention, Synchrotron emission, Supernova, Crab Nebula, Astrophysics - Solar and Stellar Astrophysics, Noema, Pulsar, Space and Planetary Science, law, Astrophysics - High Energy Astrophysical Phenomena, Solar and Stellar Astrophysics (astro-ph.SR), Astrophysics::Galaxy Astrophysics
Abstract: Fast-rotating pulsars and magnetars have been suggested as the central engines of super-luminous supernovae (SLSNe) and fast radio bursts, and this scenario naturally predicts non-thermal synchrotron emission from their nascent pulsar wind nebulae (PWNe). We report results of high-frequency radio observations with ALMA and NOEMA for three SLSNe (SN 2015bn, SN 2016ard, and SN 2017egm), and present a detailed theoretical model to calculate non-thermal emission from PWNe with an age of about 1-3 yr. We find that the ALMA data disfavors a PWN model motivated by the Crab nebula for SN 2015bn and SN 2017egm, and argue that this tension can be resolved if the nebular magnetization is very high or very low. Such models can be tested by future MeV-GeV gamma-ray telescopes such as AMEGO., Comment: 7 pages, 4 figures, 2 tables
Published: 2021

44. Variation in Radiation Intensity of 26 Radio Pulsars at 111 MHz

Author: A. N. Kazantsev
Subjects: Physics, Pulsar, Space and Planetary Science, Phased array, Astrophysics::High Energy Astrophysical Phenomena, Log-normal distribution, Astrophysics::Instrumentation and Methods for Astrophysics, Northern Hemisphere, Astronomy and Astrophysics, Astrophysics, Variation (astronomy), Radio astronomy observatory, Radiant intensity
Abstract: This article presents the results of processing observations of 26 radio pulsars of the Northern Hemisphere, obtained as part of the search and study of giant pulses at the Large Phased Array of the Pushchino Radio Astronomy Observatory at 111 MHz. Individual pulses with peak flux density 30 and more times higher than the peak flux density of dynamic average profile were found from the pulsars B0011+47, B0450+55, B0525+21, B0751+32, B0823+26, and B0917+63. Pulsars B0450+55, B0525+21, and B0751+32 generate individual pulses that meet the main criteria for giant pulses of pulsars. The analysis of the distributions of individual pulses of pulsars by the peak flux density relative to the average flux density in the session is carried out. From the analyzed sample, for 5 pulsars the distribution is lognormal, for 10 it is a combination of log-normal and power-law distributions. In other cases, it cannot be unambiguously approximated only by the lognormal distribution or by a combination of the lognormal and power-law distributions.
Published: 2021

45. Quality over Quantity: Optimizing pulsar timing array analysis for stochastic and continuous gravitational wave signals

Author: Lorenzo Speri, Nataliya K Porayko, Mikel Falxa, Siyuan Chen, Jonathan R Gair, Alberto Sesana, Stephen R Taylor, AstroParticule et Cosmologie (APC (UMR_7164)), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité), and HEP, INSPIRE
Subjects: High Energy Astrophysical Phenomena (astro-ph.HE), noise, [PHYS.GRQC] Physics [physics]/General Relativity and Quantum Cosmology [gr-qc], background, gravitational radiation, FOS: Physical sciences, Astronomy and Astrophysics, General Relativity and Quantum Cosmology (gr-qc), Bayesian, General Relativity and Quantum Cosmology, quality, Space and Planetary Science, correlation, frequentist, [PHYS.GRQC]Physics [physics]/General Relativity and Quantum Cosmology [gr-qc], stochastic, [PHYS.ASTR] Physics [physics]/Astrophysics [astro-ph], [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Astrophysics - High Energy Astrophysical Phenomena, signature, pulsar
Abstract: The search for gravitational waves using Pulsar Timing Arrays (PTAs) is a computationally expensive complex analysis that involves source-specific noise studies. As more pulsars are added to the arrays, this stage of PTA analysis will become increasingly challenging. Therefore, optimizing the number of included pulsars is crucial to reduce the computational burden of data analysis. Here, we present a suite of methods to rank pulsars for use within the scope of PTA analysis. First, we use the maximization of the signal-to-noise ratio as a proxy to select pulsars. With this method, we target the detection of stochastic and continuous gravitational wave signals. Next, we present a ranking that minimizes the coupling between spatial correlation signatures, namely monopolar, dipolar, and Hellings & Downs correlations. Finally, we also explore how to combine these two methods. We test these approaches against mock data using frequentist and Bayesian hypothesis testing. For equal-noise pulsars, we find that an optimal selection leads to an increase in the log-Bayes factor two times steeper than a random selection for the hypothesis test of a gravitational wave background versus a common uncorrelated red noise process. For the same test but for a realistic European PTA (EPTA) data set, a subset of 25 pulsars selected out of 40 can provide a log-likelihood ratio that is 89 % of the total, implying that an optimally selected subset of pulsars can yield results comparable to those obtained from the whole array. We expect these selection methods to play a crucial role in future PTA data combinations.
Published: 2022

46. Multi-wavelength study of the galactic PeVatron candidate LHAASO J2108+5157

Author: Abe, S., Aguasca-Cabot, A., Agudo, I., Crespo, N. Alvarez, Antonelli, L. A., Aramo, C., Arbet-Engels, A., Artero, M., Asano, K., Aubert, P., Baktash, A., Bamba, A., Larriva, A. Baquero, Baroncelli, L., Almeida, U. Barres, Barrio, J. A., Batkovic, I., Baxter, J., González, J. Becerra, Bernardini, E., Bernardos, M. I., Medrano, J. Bernete, Berti, A., Bhattacharjee, P., Biederbeck, N., Bigongiari, C., Bissaldi, E., Blanch, O., Bordas, P., Buisson, C., Bulgarelli, A., Burelli, I., Buscemi, M., Cardillo, M., Caroff, S., Carosi, A., Cassol, F., Cauz, D., Ceribella, G., Chai, Y., Cheng, K., Chiavassa, A., Chikawa, M., Chytka, L., Cifuentes, A., Contreras, J. L., Cortina, J., Costantini, H., D Amico, G., Dalchenko, M., Angelis, A., Lavergne, M. Bony, Lotto, B., Menezes, R., Deleglise, G., Delgado, C., Mengual, J. Delgado, Della Volpe, D., Dellaiera, M., Di Piano, A., Di Pierro, F., Di Tria, R., Di Venere, L., Díaz, C., Dominik, R. M., Dominis Prester, D., Donini, A., Dorner, D., Doro, M., Elsässer, D., Emery, G., Escudero, J., Fallah Ramazani, V., Ferrara, G., Fiasson, A., Coromina, L. Freixas, Fröse, S., Fukami, S., Fukazawa, Y., Garcia, E., López, R. Garcia, Gasparrini, D., Geyer, D., Paiva, J. Giesbrecht, Giglietto, N., Giordano, F., Giro, E., Gliwny, P., Godinovic, N., Grau, R., Green, D., Green, J., Gunji, S., Hackfeld, J., Hadasch, D., Hahn, A., Hashiyama, K., Hassan, T., Hayashi, K., Heckmann, L., Heller, M., Llorente, J. Herrera, Hirotani, K., Hoffmann, D., Horns, D., Houles, J., Hrabovsky, M., Hrupec, D., Hui, D., Hütten, M., Imazawa, R., Tomohiro Inada, Inome, Y., Ioka, K., Iori, M., Ishio, K., Iwamura, Y., Jacquemont, M., Martinez, I. Jimenez, Jurysek, J., Kagaya, M., Karas, V., Katagiri, H., Kataoka, J., Kerszberg, D., Kobayashi, Y., Kong, A., Kubo, H., Kushida, J., Lainez, M., Lamanna, G., Lamastra, A., Flour, T. Le, Linhoff, M., Longo, F., López-Coto, R., López-Moya, M., López-Oramas, A., Loporchio, S., Lorini, A., Luque-Escamilla, P. L., Majumdar, P., Makariev, M., Mandat, D., Manganaro, M., Manicò, G., Mannheim, K., Mariotti, M., Marquez, P., Marsella, G., Martí, J., Martinez, O., Martínez, G., Martínez, M., Marusevec, P., Mas-Aguilar, A., Maurin, G., Mazin, D., Guillen, E. Mestre, Micanovic, S., Miceli, D., Miener, T., Miranda, J. M., Mirzoyan, R., Mizuno, T., Gonzalez, M. Molero, Molina, E., Montaruli, T., Monteiro, I., Moralejo, A., Morcuende, D., Morselli, A., Mrakovcic, K., Murase, K., Nagai, A., Nakamori, T., Nickel, L., Nievas, M., Nishijima, K., Noda, K., Nosek, D., Nozaki, S., Ohishi, M., Ohtani, Y., Okazaki, N., Okumura, A., Orito, R., Otero-Santos, J., Palatiello, M., Paneque, D., Pantaleo, F. R., Paoletti, R., Paredes, J. M., Pavletić, L., Pech, M., Pecimotika, M., Pietropaolo, E., Pirola, G., Podobnik, F., Poireau, V., Polo, M., Pons, E., Prandini, E., Prast, J., Priyadarshi, C., Prouza, M., Rando, R., Rhode, W., Ribó, M., Rizi, V., Fernandez, G. Rodriguez, Saito, T., Sakurai, S., Sanchez, D. A., Šarić, T., Saturni, F. G., Scherpenberg, J., Schleicher, B., Schmuckermaier, F., Schubert, J. L., Schussler, F., Schweizer, T., Arroyo, M. Seglar, Sitarek, J., Sliusar, V., Spolon, A., Strišković, J., Strzys, M., Suda, Y., Sunada, Y., Tajima, H., Takahashi, M., Takahashi, H., Takata, J., Takeishi, R., Tam, P. H. T., Tanaka, S. J., Tateishi, D., Temnikov, P., Terada, Y., Terauchi, K., Terzic, T., Teshima, M., Tluczykont, M., Tokanai, F., Torres, D. F., Travnicek, P., Truzzi, S., Tutone, A., Uhlrich, G., Vacula, M., Vázquez Acosta, M., Verguilov, V., Viale, I., Vigliano, A., Vigorito, C. F., Vitale, V., Voutsinas, G., Vovk, I., Vuillaume, T., Walter, R., Will, M., Yamamoto, T., Yamazaki, R., Yoshida, T., Yoshikoshi, T., Zywucka, N., Balbo, M., Eckert, D., Tramacere, A., Laboratoire d'Annecy de Physique des Particules (LAPP), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS), Centre de Physique des Particules de Marseille (CPPM), Aix Marseille Université (AMU)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Institut de Recherches sur les lois Fondamentales de l'Univers (IRFU), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay, and CTA-LST
Subjects: halo, FOS: Physical sciences, electron: relativistic, power spectrum, UHE, GLAST, VHE, ISM: individual objects: LHAASO J2108+5157, X-ray, pulsars: general, synchrotron, supernova, TeV, cloud, High Energy Astrophysical Phenomena, pulsar, High Energy Astrophysical Phenomena (astro-ph.HE), magnetic field: low, photon, Astronomy and Astrophysics, gamma rays: general, acceleration, radiation mechanisms: non-thermal, p: interaction, Large-Sized Telescope, LHAASO J2108+5157, Space and Planetary Science, quality, gamma ray, spectral, galaxy, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Astrophysics - High Energy Astrophysical Phenomena
Abstract: LHAASO J2108+5157 is one of the few known unidentified Ultra-High-Energy (UHE) gamma-ray sources with no Very-High-Energy (VHE) counterpart, recently discovered by the LHAASO collaboration. We observed LHAASO J2108+5157 in the X-ray band with XMM-Newton in 2021 for a total of 3.8 hours and at TeV energies with the Large-Sized Telescope prototype (LST-1), yielding 49 hours of good quality data. In addition, we analyzed 12 years of Fermi-LAT data, to better constrain emission of its High-Energy (HE) counterpart 4FGL J2108.0+5155. We found an excess (3.7 sigma) in the LST-1 data at energies E > 3 TeV. Further analysis in the whole LST-1 energy range assuming a point-like source, resulted in a hint (2.2 sigma) of hard emission which can be described with a single power law with photon index Gamma = 1.6 +- 0.2 between 0.3 - 100 TeV. We did not find any significant extended emission which could be related to a Supernova Remnant (SNR) or Pulsar Wind Nebula (PWN) in the XMM-Newton data, which puts strong constraints on possible synchrotron emission of relativistic electrons. The LST-1 and LHAASO observations can be explained as inverse Compton-dominated leptonic emission of relativistic electrons with a cutoff energy of $100^{+70}_{-30}$ TeV. The low magnetic field in the source imposed by the X-ray upper limits on synchrotron emission is compatible with a hypothesis of a PWN or a TeV halo. The lack of a pulsar in the neighborhood of the UHE source is a challenge to the PWN/TeV-halo scenario. The UHE gamma rays can also be explained as $π^0$ decay-dominated hadronic emission due to interaction of relativistic protons with one of the two known molecular clouds in the direction of the source. The hard spectrum in the LST-1 band is compatible with protons escaping a shock around a middle-aged SNR because of their high low-energy cut-off., 26 pages, 9 figures, 5 tables; Astronomy and Astrophysics (accepted on 6 March 2023)
Published: 2022

47. Statistical Analysis of Radio Frequency Interference (RFI) Caused by Solar Radiation During Wet and Dry

Author: Marhamah Mohd Shafie, Roslan Umar, and Nor Hazmin Sabri
Subjects: General Mathematics, General Physics and Astronomy, General Chemistry, General Biochemistry, Genetics and Molecular Biology, Electromagnetic interference, Weather station, Jupiter, Solar observation, Solar wind, Pulsar, Ultra high frequency, Very-long-baseline interferometry, Environmental science, General Agricultural and Biological Sciences, Remote sensing
Abstract: This paper describes a effect of solar radiation and radio signal within ultra-high frequency (UHF), which statistically deduced using Spearman correlation method. The observation was done in several location including Balai Cerap KUSZA (BCK) during dry and wet season. Solar radiation one of meteoparameters that measured simultaneously using a weather station. This data was analysed and compared to power level (radio signal) in dBm during wet and dry seasons. Findings show that telecommunication services occupy the UHF band. Hence, it can be concluded that, there are still some frequencies available for radio astronomical sources including that below 400 MHz. This allocation is suitable for solar observation, Jupiter observation, continuum observation, solar wind observation, as well as pulsar and deuterium observation and VLBI application. Statistical analysis indicate that solar radiation was significantly prominent during peaks of 382.5 MHz, 1800.0 MHz and 2160.0 MHz. It is largely related with a correlation of 0.6252, 0.6769, 0.5965 during the wet season and only small and moderate correlation at all peaks during the dry season. This important information could be a significant contribution for radio astronomers when trying to identify the best allocation for observing radio astronomical sources in the future.
Published: 2021

48. Coherent curvature radiation: maximum luminosity and high-energy emission

Author: Ralph A. M. J. Wijers, A. J. Cooper, and High Energy Astrophys. & Astropart. Phys (API, FNWI)
Subjects: High Energy Astrophysical Phenomena (astro-ph.HE), Physics, Crab Pulsar, Astrophysics::High Energy Astrophysical Phenomena, FOS: Physical sciences, Astronomy and Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, Radiation, Curvature, Charged particle, Magnetic field, Luminosity, Neutron star, Pulsar, Space and Planetary Science, Astrophysics - High Energy Astrophysical Phenomena
Abstract: High brightness temperature radio transients such as pulsars and fast radio bursts require the coherent radiation of particles. The antenna class of coherent radiation models require a large number of charged particles radiating in phase, therefore the particles must be spatially confined and have well-aligned velocities. Given these necessary conditions, we look at the magnetic field induced by the currents associated with coherently emitting accelerated particles and consider the interaction between the radiating particles and the induced magnetic field. We find a maximum luminosity of coherent curvature radiation that depends on source parameters such as surface magnetic field and neutron star spin period. We find that coherent radio emission across all luminosities can be explained by coherent curvature radiation and suggest it could be universally responsible for both FRBs and extreme galactic sources. Using the Crab Pulsar as an example, we constrain the emission parameters and origin of the most extreme nanoshots to within 60km of the pulsar surface assuming coherent curvature radiation. In agreement with recent observations, we also predict simultaneous X-ray emission from small-scale particle gyration due to the induced field., Comment: Accepted to MNRAS Letters
Published: 2021

49. On the angular momentum extraction from the rotation powered pulsars

Author: Shota Kisaka and Shinpei Shibata
Subjects: High Energy Astrophysical Phenomena (astro-ph.HE), Physics, Angular momentum, Astrophysics::High Energy Astrophysical Phenomena, FOS: Physical sciences, Energy flux, Astronomy and Astrophysics, Angular velocity, Rotation, Computational physics, Relativistic particle, Pulsar, Space and Planetary Science, Torque, Cylinder, Astrophysics - High Energy Astrophysical Phenomena
Abstract: The rotation powered pulsar loses angular momentum at a rate of the rotation power divided by the angular velocity $\Omega_*$. This means that the length of the lever arm of the angular momentum extracted by the photons, relativistic particles and wind must be on average $c/\Omega_*$, which is known as the light cylinder radius. Therefore, any deposition of the rotation power within the light cylinder causes insufficient loss of angular momentum. In this paper, we investigate two cases of this type of energy release: polar cap acceleration and Ohmic heating in the magnetospheric current inside the star. As for the first case, the outer magnetosphere beyond the light cylinder is found to compensate the insufficient loss of the angular momentum. We argue that the energy flux coming from the sub-rotating magnetic field lines must be larger than the solid-angle average value, and as a result, an enhanced energy flux emanating beyond the light cylinder is observed in different phases in the light curve from those of emission inside the light cylinder. As for the second case, the stellar surface rotates more slowly than the stellar interior. We find that the way the magnetospheric current closes inside the star is linked to how the angular momentum is transferred inside the star. We obtain numerical solutions which show that the magnetospheric current inside the star spreads over the polar cap magnetic flux embedded in the star in such a way that electromotive force is gained efficiently., Comment: Accepted for publication in MNRAS, 9 pages, 16 figures
Published: 2021

50. Estimator for Deep-Space Position and Attitude Using X-ray Pulsars

Author: Joel T. Runnels and Demoz Gebre-Egziabher
Subjects: Physics, Stars, Pulsar, Filter (video), Astrophysics::High Energy Astrophysical Phenomena, Angle of arrival, Detector, Rate gyro, Aerospace Engineering, Joint Probabilistic Data Association Filter, NASA Deep Space Network, Electrical and Electronic Engineering, Computational physics
Abstract: In this article, we develop an algorithm for the estimation of a full six degree of freedom position, navigation, and timing solution in deep space by measuring the time and angle of arrival of x-rays photons from pulsars and other bright stars. We show that for pulsar navigation, the position and attitude determination problems are coupled. This is due in part to the small signal-to-noise ratio of pulsar signals and the fact that x-ray photons emanating from various pulsars and bright stars have no unique identifier that can be used to associate them with their source. To address this challenge, a joint probabilistic data association filter is developed. The filter fuses angular rate measurements from a three-axis rate gyro with time-of-arrival and angle-of-arrival measurements from an x-ray detector. The performance of the filter is validated in simulation, and the tradeoffs associated with detector size and initial conditions are evaluated. Additional validation of the algorithm is performed by playback of data from x-ray detectors on the Chandra spacecraft. The results show that positioning accuracy on the order of 1000 km and attitude accuracies on the order of 5 arcseconds can be achieved.
Published: 2021

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