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6 results on '"3C 58"'

1. Generation of cosmic rays in pulsar wind nebulae.

Author

Sinitsyna, Vera G. and Sinitsyna, Vera Y.

Subjects
*NEBULAE, *SPECTRAL energy distribution, *PULSARS, *CRAB Nebula, *COSMIC rays, *SUPERNOVA remnants
Abstract

The overall observations of plerions from radio to the very high energy gamma‐rays could provide information about the evolution of pulsar wind nebulae (PWN) from the young Crab‐like stage to the older plerion stages. Geminga is a nearby (250 pc) and middle‐aged pulsar of ∼3.4×105$$ \sim 3.4\times {10}^5 $$ years. The Geminga pulsar wind nebula was detected in X‐rays, and the detailed studies reveal the morphological and spectral variability, which may raise a high energy emission. The extended MeV‐TeV emission from Geminga in SHALON, Milagro, HAWC observations, and Fermi‐LAT detection and upper limits could arise from the PWN associated with the Geminga SNR. 3C58 is similar to the Crab Nebula (explosion of the 1054 year) on many parameters, but these two objects differ significantly in luminosity and size at X‐rays and radio‐emission. The 3C 58 estimated age varies from ∼800$$ \sim 800 $$ to (5−7)×103$$ \left(5-7\right)\times {10}^3 $$ years. MeV‐GeV gamma‐ray emission from the nebula has been detected by Fermi‐LAT. The γ‐ray source associated with the 3C 58 was detected above 800 GeV for the first time by SHALON in observations of 2011 year and systematically studied since then. The overall spectral energy distribution and information about the extension of PWN from radio to GeV‐TeV energies can contribute to particle transport models and also to the understanding of the mechanisms of PWN expanding, which is, in turn, can shed light on the age of 3C 58 and the history of progenitor SN explosion. [ABSTRACT FROM AUTHOR]

Published
2023
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2. Revealing hidden variability in PWNe with spectral index maps.

Author

Guest, Benson T and Safi-Harb, Samar

Subjects
*NEUTRON temperature, *SUPERNOVA remnants, *ALGORITHMS, *PULSARS
Abstract

Pulsar wind nebulae (PWNe) are the synchrotron bubbles inflated by the rotational energy of a neutron star. Observing variability within them has previously been limited to cases of significant brightening, or the few instances where transient features are interpreted in terms of intrinsic motion or associated with variability from the pulsar. Jet and torus morphology are also only visible in cases of differing brightness with respect to the surrounding nebula and favourable alignment with our line of sight. Spectral map analysis involves binning observations with an adaptive algorithm to meet a signal limit and colouring the results based on the desired model parameter fits. Minute changes in spectral index become therefore apparent even in cases where brightness images alone do not suggest any underlying changes. We present a Chandra X-ray study of the PWNe in G21.5–0.9, Kes 75, G54.1+0.3, G11.2–0.3, and 3C 58, using archival observations accumulated over the ∼20-yr lifetime of the mission. With the spectral map analysis technique, we discover evidence for previously unknown variability opening a new window into viewing PWNe. [ABSTRACT FROM AUTHOR]

Published
2020
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3. Search for very high energy gamma-ray emission from pulsar-pulsar wind nebula systems with the Magic telescope

Author

Antoranz Canales, Pedro, Barrio Uña, Juan Abel, Contreras González, José Luis, Fonseca González, Mª Victoria, Miranda Pantoja, José Miguel, Nieto, Daniel, Antoranz Canales, Pedro, Barrio Uña, Juan Abel, Contreras González, José Luis, Fonseca González, Mª Victoria, Miranda Pantoja, José Miguel, and Nieto, Daniel

Abstract

© The American Astronomical Society. We thank the Instituto de Astrofisica de Canarias for the excellent working conditions at the Observatorio del Roque de los Muchachos in La Palma. The support of the German BMBF and MPG, the Italian INFN, and the Spanish MICINN is gratefully acknowledged. This work was also supported by ETH Research Grant TH 34/043, by the Polish MNiSzW Grant NN203 390834, and by theYIP of the Helmholtz Gemeinschaft. We thank D.A. Smith and the Nancay Radio Observatory operated by the Paris Observatory (associated with the French CNRS) for the ephemerides of PSR J0218+4232, and also S. M. Ransom (NRAO) for the ephemerides of PSR J0205+6449., The MAGIC collaboration has searched for high-energy gamma-ray emission of some of the most promising pulsar candidates above an energy threshold of 50 GeV, an energy not reachable up to now by other ground-based instruments. Neither pulsed nor steady gamma-ray emission has been observed at energies of 100 GeV from the classical radio pulsars PSR J0205+6449 and PSR J2229+6114 (and their nebulae 3C58 and Boomerang, respectively) and the millisecond pulsar PSR J0218+4232. Here, we present the flux upper limits for these sources and discuss their implications in the context of current model predictions., German BMBF, German MPG, Italian INFN, Spanish MICINN, ETH Research Grant, Polish MNiSzW, YIP of the Helmholtz Gemeinschaft, Depto. de Estructura de la Materia, Física Térmica y Electrónica, Fac. de Ciencias Físicas, TRUE, pub

Published
2023

4. Search for very high energy gamma-ray emission from pulsar-pulsar wind nebula systems with the Magic telescope

Author

M. Camara, Valentí Bosch-Ramon, L. A. Antonelli, Pierre Colin, Pratik Majumdar, M. V. Fonseca, M. Rissi, E. De Cea del Pozo, V. Scapin, Ignasi Reichardt, Aaron Dominguez, S. Balestra, Felicitas Pauss, Fabio Zandanel, L. O. Takalo, R. Mirzoyan, M. Garczarczyk, Victor Zabalza, E. Carmona, Konstancja Satalecka, Michele Doro, Ismaël Cognard, Igor Oya, Denis Bastieri, I. Puljak, Roberta Zanin, A. De Angelis, D. Elsaesser, M. Salvati, Fabrizio Tavecchio, Manel Errando, J. M. Paredes, Antonio Stamerra, G. Maneva, B. De Lotto, Tihomir Surić, Daniel Kranich, D. Dominis Prester, Daniela Dorner, Thomas Bretz, S. N. Shore, Florian Goebel, A. Sillanpää, M. Shayduk, Elina Lindfors, Mosè Mariotti, Ll. Font, Saverio Lombardi, Kari Nilsson, A. Saggion, M. López, Daniel Mazin, Nijil Mankuzhiyil, D. Britzger, Nicola Galante, Adrian Biland, R. G. Pegna, A. Laille, Markus Gaug, Dorota Sobczyńska, Miguel A. Pérez-Torres, R. Firpo, C. Baixeras, Robert Wagner, Petar Temnikov, S. Rügamer, Wolfgang Rhode, Stefano Covino, Elisa Bernardini, Juan Abel Barrio, Daniel Nieto, F. De Sabata, Pol Bordas, D. Bose, R. de los Reyes, Nicola Turini, J. Zapatero, E. Prandini, Francisco Prada, R. K. Bock, T. Schweizer, Karl Mannheim, Hiroko Miyamoto, R. J. García López, D. Borla Tridon, Jose Luis Contreras, Stefan Klepser, L. S. Stark, Julia Becker, N. Puchades, S. Commichau, Artemio Herrero, Agnieszka Sierpowska-Bartosik, D. Tescaro, Wlodek Bednarek, Alessandro Carosi, Marc Ribó, A. Robert, Juan Cortina, Laura Maraschi, M. T. Costado, Diego F. Torres, A. La Barbera, C. Delgado Mendez, Giacomo Bonnoli, Masahiro Teshima, M. Pasanen, Massimo Persic, D. Hadasch, Riccardo Paoletti, V. Scalzotto, J. Becerra González, P. Antoranz, M. I. Martínez, Jose Miguel Miranda, Abelardo Moralejo, Mario Meucci, Takashi Saito, Mariano Moles, Reiko Orito, Javier Moldon, D. Pascoli, Julian Sitarek, Felix Spanier, S. Spiro, E. Lorenz, J. Hose, al K. Berger, J. Rico, Jelena Ninkovic, D. Hildebrand, L. Peruzzo, Francesco Dazzi, Miguel A. Sánchez-Conde, E. Leonardo, Daniel Ferenc, H. Vankov, Ilana M. Braun, T. Jogler, Francesco Longo, D. Höhne-Mönch, Dario Hrupec, H. Anderhub, Michael Backes, Enrique Fernández, C. C. Hsu, Nikola Godinovic, M. De Maria, H., Anderhub, L. A., Antonelli, P., Antoranz, M., Backe, C., Baixera, S., Balestra, J. A., Barrio, D., Bastieri, J. B., Gonzalez, J. K., Becker, W., Bednarek, A. K., Berger, E., Bernardini, A., Biland, R. K., Bock, G., Bonnoli, P., Borda, D. B., Tridon, V., Bosch Ramon, D., Bose, I., Braun, T., Bretz, D., Britzger, M., Camara, E., Carmona, A., Carosi, P., Colin, S., Commichau, J. L., Contrera, J., Cortina, M. T., Costado, S., Covino, F., Dazzi, A. D., Angeli, E. D., del Pozo, R. D., los Reye, B. D., Lotto, M. D., Maria, F. D., Sabata, C. D., Mendez, A., Dominguez, D. D., Prester, D., Dorner, M., Doro, D., Elsaesser, M., Errando, D., Ferenc, E., Fernandez, R., Firpo, M. V., Fonseca, L., Font, N., Galante, R. J. G., Lopez, M., Garczarczyk, M., Gaug, N., Godinovic, F., Goebel, D., Hadasch, A., Herrero, D., Hildebrand, D., Hohne Monch, J., Hose, D., Hrupec, C. C., Hsu, T., Jogler, S., Klepser, D., Kranich, A. L., Barbera, A., Laille, E., Leonardo, E., Lindfor, S., Lombardi, Longo, Francesco, M., Lopez, E., Lorenz, P., Majumdar, G., Maneva, N., Mankuzhiyil, K., Mannheim, L., Maraschi, M., Mariotti, M., Martinez, D., Mazin, M., Meucci, J. M., Miranda, R., Mirzoyan, H., Miyamoto, J., Moldon, M., Mole, A., Moralejo, D., Nieto, K., Nilsson, J., Ninkovic, R., Orito, I., Oya, R., Paoletti, J. M., Parede, M., Pasanen, D., Pascoli, F., Pau, R. G., Pegna, M. A., Perez Torre, M., Persic, L., Peruzzo, F., Prada, E., Prandini, N., Puchade, I., Puljak, I., Reichardt, W., Rhode, M., Ribo, J., Rico, M., Rissi, A., Robert, S., Rugamer, A., Saggion, T. Y., Saito, M., Salvati, M., Sanchez Conde, K., Satalecka, V., Scalzotto, V., Scapin, T., Schweizer, M., Shayduk, S. N., Shore, A., Sierpowska Bartosik, A., Sillanpaa, J., Sitarek, D., Sobczynska, F., Spanier, S., Spiro, A., Stamerra, L. S., Stark, T., Suric, L., Takalo, F., Tavecchio, P., Temnikov, D., Tescaro, M., Teshima, D. F., Torre, N., Turini, H., Vankov, R. M., Wagner, V., Zabalza, F., Zandanel, R., Zanin, J., Zapatero, I., Cognard, Eidgenössische Technische Hochschule - Swiss Federal Institute of Technology [Zürich] (ETH Zürich), Istituto Nazionale di Astrofisica (INAF), Universidad Complutense de Madrid = Complutense University of Madrid [Madrid] (UCM), Technische Universität Dortmund [Dortmund] (TU), Universitat Autònoma de Barcelona (UAB), Universita degli Studi di Padova, University of Lódź, 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)-Centre National de la Recherche Scientifique (CNRS)-Université d'Orléans (UO)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université d'Orléans (UO)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National d’Études Spatiales [Paris] (CNES), and Universitat de Barcelona

Subjects
Astrofísica, CRAB PULSAR, Astrophysics, 7. Clean energy, 01 natural sciences, Pulsar wind nebula, LARGE-AREA TELESCOPE, Pulsar Wind Nebulae, Millisecond pulsar, Gamma ray astronomy, Very High Energy Gamma-ray Astronomy, MAGIC telescope, MAGIC (telescope), MILLISECOND PULSAR, X-RAY, PSR J0218+4232, SOURCE LIST, 3C 58, DISCOVERY, EGRET, RADIATION, 010303 astronomy & astrophysics, Physics, Gamma ray, Threshold energy, Púlsars, Electrónica, Física nuclear, methods: observational, Electricidad, Telescopis espacials, Astrophysics::High Energy Astrophysical Phenomena, Pulsar planet, gamma rays: stars, Space telescopes, Nebulae, Pulsar, 0103 physical sciences, Astronomia de raigs gamma, Pulsars, Astrophysics::Galaxy Astrophysics, 010308 nuclear & particles physics, Astronomy, Astronomy and Astrophysics, telescopes, pulsars: individual (PSR J0205+6449 PSR J2229+6114 PSR J0218+4232), Stars, Space and Planetary Science, [SDU]Sciences of the Universe [physics], Nebuloses
Abstract

International audience; The MAGIC collaboration has searched for high-energy gamma-ray emission of some of the most promising pulsar candidates above an energy threshold of 50 GeV, an energy not reachable up to now by other ground-based instruments. Neither pulsed nor steady gamma-ray emission has been observed at energies of 100 GeV from the classical radio pulsars PSR J0205+6449 and PSR J2229+6114 (and their nebulae 3C58 and Boomerang, respectively) and the millisecond pulsar PSR J0218+4232. Here, we present the flux upper limits for these sources and discuss their implications in the context of current model predictions.

Published
2010
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5. Optical observations of psr j0205+6449

Author

Vitaly Neustroev and Andrew Shearer

Subjects
Physics, 3c 58, Nebula, Crab Pulsar, extinction, supernova remnant 3c-58, Astronomy and Astrophysics, Astrophysics, Pulsar wind nebula, Optical pulsar, Pulsar, Space and Planetary Science, pulsars: individual: psr j0205+6449, Magnitude (astronomy), William Herschel Telescope, pulsations, Supernova remnant, discovery
Abstract

PSR J0205+6449 is a X-ray and radio pulsar in supernova remnant 3C 58. We report on observations of the central region of 3C 58 using the 4.2-m William Herschel Telescope with the intention of identifying the optical counterpart of PSR J0205+6449 and characterising its pulsar wind nebula. Around the pulsar position we identified extended emission with a magnitude of $B = 23 \fm 97 \pm 0.10$, $V = 22 \fm 95 \pm 0.05$ and $R = 22 \fm 15 \pm 0.03$ consistent with a pulsar wind nebula. From the R-band image we identified three knots with $m_R$ = $24 \fm 08 \pm 0.07$ (o1), $24 \fm 15 \pm 0.07$ (o2) and $24 \fm 24 \pm 0.08$ (o3). We confirm the presence of an optical pulsar wind nebula around PSR J0205+6449 and give an upper limit of $m_R \approx$ 24 for the optical magnitude of the pulsar. Furthermore we make the tentative suggestion that our object o1, with an $m_R \approx$ 24.08 is the optical counterpart. If confirmed the pulsar would have an $L_R/L_x\approx 0.004$ and an optical efficiency of about 5% of the Crab pulsar. Such a low efficiency is more consistent with the characteristic age of the pulsar rather than that of SN 1181., Comment: The paper contains 3 figures and 3 tables, accepted for publication in MNRAS

Published
2008

6. Search for very high energy gamma-ray emission from pulsar-pulsar wind nebula systems with the Magic telescope

Author

Antoranz Canales, Pedro, Barrio Uña, Juan Abel, Contreras González, José Luis, Fonseca González, María Victoria, Miranda Pantoja, José Miguel, Nieto Castaño, Daniel, Antoranz Canales, Pedro, Barrio Uña, Juan Abel, Contreras González, José Luis, Fonseca González, María Victoria, Miranda Pantoja, José Miguel, and Nieto Castaño, Daniel

Abstract

© The American Astronomical Society. We thank the Instituto de Astrofisica de Canarias for the excellent working conditions at the Observatorio del Roque de los Muchachos in La Palma. The support of the German BMBF and MPG, the Italian INFN, and the Spanish MICINN is gratefully acknowledged. This work was also supported by ETH Research Grant TH 34/043, by the Polish MNiSzW Grant NN203 390834, and by theYIP of the Helmholtz Gemeinschaft. We thank D.A. Smith and the Nancay Radio Observatory operated by the Paris Observatory (associated with the French CNRS) for the ephemerides of PSR J0218+4232, and also S. M. Ransom (NRAO) for the ephemerides of PSR J0205+6449., The MAGIC collaboration has searched for high-energy gamma-ray emission of some of the most promising pulsar candidates above an energy threshold of 50 GeV, an energy not reachable up to now by other ground-based instruments. Neither pulsed nor steady gamma-ray emission has been observed at energies of 100 GeV from the classical radio pulsars PSR J0205+6449 and PSR J2229+6114 (and their nebulae 3C58 and Boomerang, respectively) and the millisecond pulsar PSR J0218+4232. Here, we present the flux upper limits for these sources and discuss their implications in the context of current model predictions., German BMBF, German MPG, Italian INFN, Spanish MICINN, ETH Research Grant, Polish MNiSzW, YIP of the Helmholtz Gemeinschaft, Depto. de Estructura de la Materia, Física Térmica y Electrónica, Fac. de Ciencias Físicas, TRUE, pub

Published
2010

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