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Start Over Author "Bosch Ramon, V." Journal astronomy and astrophysics
35 results on '"Bosch Ramon, V."'

1. MAGIC TeV gamma-ray observations of Markarian 421 during multiwavelength campaigns in 2006

Author

Aleksić, J., primary, Anderhub, H., additional, Antonelli, L. A., additional, Antoranz, P., additional, Backes, M., additional, Baixeras, C., additional, Balestra, S., additional, Barrio, J. A., additional, Bastieri, D., additional, Becerra González, J., additional, Becker, J. K., additional, Bednarek, W., additional, Berdyugin, A., additional, Berger, K., additional, Bernardini, E., additional, Biland, A., additional, Bock, R. K., additional, Bonnoli, G., additional, Bordas, P., additional, Borla Tridon, D., additional, Bosch-Ramon, V., additional, Bose, D., additional, Braun, I., additional, Bretz, T., additional, Britzger, D., additional, Camara, M., additional, Carmona, E., additional, Carosi, A., additional, Colin, P., additional, Commichau, S., additional, Contreras, J. L., additional, Cortina, J., additional, Costado, M. T., additional, Covino, S., additional, Dazzi, F., additional, De Angelis, A., additional, de Cea del Pozo, E., additional, De los Reyes, R., additional, De Lotto, B., additional, De Maria, M., additional, De Sabata, F., additional, Delgado Mendez, C., additional, Doert, M., additional, Domínguez, A., additional, Dominis Prester, D., additional, Dorner, D., additional, Doro, M., additional, Elsaesser, D., additional, Errando, M., additional, Ferenc, D., additional, Fonseca, M. V., additional, Font, L., additional, García López, R. J., additional, Garczarczyk, M., additional, Gaug, M., additional, Godinovic, N., additional, Hadasch, D., additional, Herrero, A., additional, Hildebrand, D., additional, Höhne-Mönch, D., additional, Hose, J., additional, Hrupec, D., additional, Hsu, C. C., additional, Jogler, T., additional, Klepser, S., additional, Krähenbühl, T., additional, Kranich, D., additional, La Barbera, A., additional, Laille, A., additional, Leonardo, E., additional, Lindfors, E., additional, Lombardi, S., additional, Longo, F., additional, López, M., additional, Lorenz, E., additional, Majumdar, P., additional, Maneva, G., additional, Mankuzhiyil, N., additional, Mannheim, K., additional, Maraschi, L., additional, Mariotti, M., additional, Martínez, M., additional, Mazin, D., additional, Meucci, M., additional, Miranda, J. M., additional, Mirzoyan, R., additional, Miyamoto, H., additional, Moldón, J., additional, Moles, M., additional, Moralejo, A., additional, Nieto, D., additional, Nilsson, K., additional, Ninkovic, J., additional, Orito, R., additional, Oya, I., additional, Paoletti, R., additional, Paredes, J. M., additional, Partini, S., additional, Pasanen, M., additional, Pascoli, D., additional, Pauss, F., additional, Pegna, R. G., additional, Perez-Torres, M. A., additional, Persic, M., additional, Peruzzo, L., additional, Prada, F., additional, Prandini, E., additional, Puchades, N., additional, Puljak, I., additional, Reichardt, I., additional, Rhode, W., additional, Ribó, M., additional, Rico, J., additional, Rissi, M., additional, Rügamer, S., additional, Saggion, A., additional, Saito, T. Y., additional, Salvati, M., additional, Sánchez-Conde, M., additional, Satalecka, K., additional, Scalzotto, V., additional, Scapin, V., additional, Schweizer, T., additional, Shayduk, M., additional, Shore, S. N., additional, Sierpowska-Bartosik, A., additional, Sillanpää, A., additional, Sitarek, J., additional, Sobczynska, D., additional, Spanier, F., additional, Spiro, S., additional, Stamerra, A., additional, Steinke, B., additional, Strah, N., additional, Struebig, J. C., additional, Suric, T., additional, Takalo, L., additional, Tavecchio, F., additional, Temnikov, P., additional, Tescaro, D., additional, Teshima, M., additional, Torres, D. F., additional, Vankov, H., additional, Wagner, R. M., additional, Zabalza, V., additional, Zandanel, F., additional, and Zanin, R., additional

Published
2010
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2. MAGIC observation of the GRB 080430 afterglow

Author

Aleksić, J., primary, Anderhub, H., additional, Antonelli, L. A., additional, Antoranz, P., additional, Backes, M., additional, Baixeras, C., additional, Balestra, S., additional, Barrio, J. A., additional, Bastieri, D., additional, Becerra González, J., additional, Becker, J. K., additional, Bednarek, W., additional, Berdyugin, A., additional, Berger, K., additional, Bernardini, E., additional, Biland, A., additional, Bock, R. K., additional, Bonnoli, G., additional, Bordas, P., additional, Borla Tridon, D., additional, Bosch-Ramon, V., additional, Bose, D., additional, Braun, I., additional, Bretz, T., additional, Britzger, D., additional, Camara, M., additional, Carmona, E., additional, Carosi, A., additional, Colin, P., additional, Commichau, S., additional, Contreras, J. L., additional, Cortina, J., additional, Costado, M. T., additional, Covino, S., additional, Dazzi, F., additional, De Angelis, A., additional, de Cea del Pozo, E., additional, De los Reyes, R., additional, De Lotto, B., additional, De Maria, M., additional, De Sabata, F., additional, Delgado Mendez, C., additional, Doert, M., additional, Domínguez, A., additional, Dominis Prester, D., additional, Dorner, D., additional, Doro, M., additional, Elsaesser, D., additional, Errando, M., additional, Ferenc, D., additional, Fernández, E., additional, Firpo, R., additional, Fonseca, M. V., additional, Font, L., additional, Galante, N., additional, García López, R. J., additional, Garczarczyk, M., additional, Gaug, M., additional, Godinovic, N., additional, Goebel, F., additional, Hadasch, D., additional, Herrero, A., additional, Hildebrand, D., additional, Höhne-Mönch, D., additional, Hose, J., additional, Hrupec, D., additional, Hsu, C. C., additional, Jogler, T., additional, Klepser, S., additional, Krähenbühl, T., additional, Kranich, D., additional, La Barbera, A., additional, Laille, A., additional, Leonardo, E., additional, Lindfors, E., additional, Lombardi, S., additional, Longo, F., additional, López, M., additional, Lorenz, E., additional, Majumdar, P., additional, Maneva, G., additional, Mankuzhiyil, N., additional, Mannheim, K., additional, Maraschi, L., additional, Mariotti, M., additional, Martínez, M., additional, Mazin, D., additional, Meucci, M., additional, Miranda, J. M., additional, Mirzoyan, R., additional, Miyamoto, H., additional, Moldón, J., additional, Moles, M., additional, Moralejo, A., additional, Nieto, D., additional, Nilsson, K., additional, Ninkovic, J., additional, Orito, R., additional, Oya, I., additional, Paoletti, R., additional, Paredes, J. M., additional, Pasanen, M., additional, Pascoli, D., additional, Pauss, F., additional, Pegna, R. G., additional, Perez-Torres, M. A., additional, Persic, M., additional, Peruzzo, L., additional, Prada, F., additional, Prandini, E., additional, Puchades, N., additional, Puljak, I., additional, Reichardt, I., additional, Rhode, W., additional, Ribó, M., additional, Rico, J., additional, Rissi, M., additional, Rügamer, S., additional, Saggion, A., additional, Saito, T. Y., additional, Salvati, M., additional, Sánchez-Conde, M., additional, Satalecka, K., additional, Scalzotto, V., additional, Scapin, V., additional, Schweizer, T., additional, Shayduk, M., additional, Shore, S. N., additional, Sierpowska-Bartosik, A., additional, Sillanpää, A., additional, Sitarek, J., additional, Sobczynska, D., additional, Spanier, F., additional, Spiro, S., additional, Stamerra, A., additional, Steinke, B., additional, Strah, N., additional, Struebig, J. C., additional, Suric, T., additional, Takalo, L., additional, Tavecchio, F., additional, Temnikov, P., additional, Tescaro, D., additional, Teshima, M., additional, Torres, D. F., additional, Turini, N., additional, Vankov, H., additional, Wagner, R. M., additional, Zabalza, V., additional, Zandanel, F., additional, Zanin, R., additional, Zapatero, J., additional, and de Ugarte-Postigo, A., additional

Published
2010
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5. Radio continuum and near-infrared study of the MGRO J2019+37region***

Author

Paredes, J. M., Martí, J., Ishwara-Chandra, C. H., Sánchez-Sutil, J. R., Muñoz-Arjonilla, A. J., Moldón, J., Peracaula, M., Luque-Escamilla, P. L., Zabalza, V., Bosch-Ramon, V., Bordas, P., Romero, G. E., Ribó, M., Paredes, J. M., Martí, J., Ishwara-Chandra, C. H., Sánchez-Sutil, J. R., Muñoz-Arjonilla, A. J., Moldón, J., Peracaula, M., Luque-Escamilla, P. L., Zabalza, V., Bosch-Ramon, V., Bordas, P., Romero, G. E., and Ribó, M.

Abstract

Context. MGRO J2019+37is an unidentified extended source of very high energy gamma-rays originally reported by the Milagro Collaboration as the brightest TeV source in the Cygnus region. Its extended emission could be powered by either a single or several sources. The GeV pulsar AGL J2020.5+3653, discovered by AGILE and associated with PSR J2021+3651, could contribute to the emission from MGRO J2019+37.

Published
2009
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6. Non-thermal emission from microquasar/ISM interaction

Author

Bordas, P., Bosch-Ramon, V., Paredes, J. M., Perucho, M., Bordas, P., Bosch-Ramon, V., Paredes, J. M., and Perucho, M.

Abstract

Context. The interaction of microquasar jets with their environment can produce non-thermal radiation as in the case of extragalactic outflows impacting on their surroundings. Significant observational evidence of jet/medium interaction in galactic microquasars has been collected in the past few years, although little theoretical work has been done regarding the resulting non-thermal emission.

Published
2009
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7. MAGIC upper limits to the VHE gamma-ray flux of 3C 454.3 in high emission state

Author

Anderhub, H., Antonelli, L. A., Antoranz, P., Backes, M., Baixeras, C., Balestra, S., Barrio, J. A., Bartko, H., Bastieri, D., Becerra González, J., Becker, J. K., Bednarek, W., Berger, K., Bernardini, E., Biland, A., Bock, R. K., Bonnoli, G., Bordas, P., Borla Tridon, D., Bosch-Ramon, V., Bretz, T., Britvitch, I., Camara, M., Carmona, E., Commichau, S., Contreras, J. L., Cortina, J., Costado, M. T., Covino, S., Curtef, V., Dazzi, F., De Angelis, A., De Cea del Pozo, E., de los Reyes, R., De Lotto, B., De Maria, M., De Sabata, F., Delgado Mendez, C., Dominguez, A., Dorner, D., Doro, M., Elsaesser, D., Errando, M., Ferenc, D., Fernández, E., Firpo, R., Fonseca, M. V., Font, L., Galante, N., García López, R. J., Garczarczyk, M., Gaug, M., Goebel, F., Hadasch, D., Hayashida, M., Herrero, A., Höhne-Mönch, D., Hose, J., Hsu, C. C., Huber, S., Jogler, T., Kranich, D., La Barbera, A., Laille, A., Leonardo, E., Lindfors, E., Lombardi, S., Longo, F., López, M., Lorenz, E., Majumdar, P., Maneva, G., Mankuzhiyil, N., Mannheim, K., Maraschi, L., Mariotti, M., Martínez, M., Mazin, D., Meucci, M., Meyer, M., Miranda, J. M., Mirzoyan, R., Moldón, J., Moles, M., Moralejo, A., Nieto, D., Nilsson, K., Ninkovic, J., Otte, N., Oya, I., Paoletti, R., Paredes, J. M., Pasanen, M., Pascoli, D., Pauss, F., Pegna, R. G., Perez-Torres, M. A., Persic, M., Peruzzo, L., Prada, F., Prandini, E., Puchades, N., Rhode, W., Ribó, M., Rico, J., Rissi, M., Robert, A., Rügamer, S., Saggion, A., Saito, T. Y., Salvati, M., Sanchez-Conde, M., Sartori, P., Satalecka, K., Scalzotto, V., Scapin, V., Schweizer, T., Shayduk, M., Shinozaki, K., Shore, S. N., Sidro, N., Sierpowska-Bartosik, A., Sillanpää, A., Sitarek, J., Sobczynska, D., Spanier, F., Stamerra, A., Stark, L. S., Takalo, L., Tavecchio, F., Temnikov, P., Tescaro, D., Teshima, M., Tluczykont, M., Torres, D. F., Turini, N., Vankov, H., Venturini, A., Vitale, V., Wagner, R. M., Wittek, W., Zabalza, V., Zandanel, F., Zanin, R., Zapatero, J., Vercellone, S., Donnarumma, I., D'Ammando, F., Tavani, M., Anderhub, H., Antonelli, L. A., Antoranz, P., Backes, M., Baixeras, C., Balestra, S., Barrio, J. A., Bartko, H., Bastieri, D., Becerra González, J., Becker, J. K., Bednarek, W., Berger, K., Bernardini, E., Biland, A., Bock, R. K., Bonnoli, G., Bordas, P., Borla Tridon, D., Bosch-Ramon, V., Bretz, T., Britvitch, I., Camara, M., Carmona, E., Commichau, S., Contreras, J. L., Cortina, J., Costado, M. T., Covino, S., Curtef, V., Dazzi, F., De Angelis, A., De Cea del Pozo, E., de los Reyes, R., De Lotto, B., De Maria, M., De Sabata, F., Delgado Mendez, C., Dominguez, A., Dorner, D., Doro, M., Elsaesser, D., Errando, M., Ferenc, D., Fernández, E., Firpo, R., Fonseca, M. V., Font, L., Galante, N., García López, R. J., Garczarczyk, M., Gaug, M., Goebel, F., Hadasch, D., Hayashida, M., Herrero, A., Höhne-Mönch, D., Hose, J., Hsu, C. C., Huber, S., Jogler, T., Kranich, D., La Barbera, A., Laille, A., Leonardo, E., Lindfors, E., Lombardi, S., Longo, F., López, M., Lorenz, E., Majumdar, P., Maneva, G., Mankuzhiyil, N., Mannheim, K., Maraschi, L., Mariotti, M., Martínez, M., Mazin, D., Meucci, M., Meyer, M., Miranda, J. M., Mirzoyan, R., Moldón, J., Moles, M., Moralejo, A., Nieto, D., Nilsson, K., Ninkovic, J., Otte, N., Oya, I., Paoletti, R., Paredes, J. M., Pasanen, M., Pascoli, D., Pauss, F., Pegna, R. G., Perez-Torres, M. A., Persic, M., Peruzzo, L., Prada, F., Prandini, E., Puchades, N., Rhode, W., Ribó, M., Rico, J., Rissi, M., Robert, A., Rügamer, S., Saggion, A., Saito, T. Y., Salvati, M., Sanchez-Conde, M., Sartori, P., Satalecka, K., Scalzotto, V., Scapin, V., Schweizer, T., Shayduk, M., Shinozaki, K., Shore, S. N., Sidro, N., Sierpowska-Bartosik, A., Sillanpää, A., Sitarek, J., Sobczynska, D., Spanier, F., Stamerra, A., Stark, L. S., Takalo, L., Tavecchio, F., Temnikov, P., Tescaro, D., Teshima, M., Tluczykont, M., Torres, D. F., Turini, N., Vankov, H., Venturini, A., Vitale, V., Wagner, R. M., Wittek, W., Zabalza, V., Zandanel, F., Zanin, R., Zapatero, J., Vercellone, S., Donnarumma, I., D'Ammando, F., and Tavani, M.

Abstract

Aims. We report upper limits to the very high energy flux ($E>100$GeV) of the flat spectrum radio quasar 3C 454.3 ($z=0.859$) derived by the Cherenkov telescope MAGIC during the high states of July/August and November/December 2007. We compare the upper limits derived in both time slots with the available quasi-simultaneous MeV-GeV data from the AGILE γ-ray satellite and interpret the observational results in the context of leptonic emission models.

Published
2009
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9. Leptonic secondary emission in a hadronic microquasar model

Author

Orellana, M., Bordas, P., Bosch-Ramon, V., Romero, G. E., Paredes, J. M., Orellana, M., Bordas, P., Bosch-Ramon, V., Romero, G. E., and Paredes, J. M.

Abstract

Context.It has been proposed that the origin of the very high-energy photons emitted from high-mass X-ray binaries with jet-like features, so-called microquasars (MQs), is related to hadronic interactions between relativistic protons in the jet and cold protons of the stellar wind. Leptonic secondary emission should be calculated in a complete hadronic model that includes the effects of pairs from charged pion decays inside the jets and the emission from pairs generated by gamma-ray absorption in the photosphere of the system.

Published
2007
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10. Gamma-ray emission from massive young stellar objects

Author

Araudo, A. T., Romero, G. E., Bosch-Ramon, V., Paredes, J. M., Araudo, A. T., Romero, G. E., Bosch-Ramon, V., and Paredes, J. M.

Abstract

Context.Massive stars form in dense and massive molecular cores. The exact formation mechanism is unclear, but it is possible that some massive stars are formed by processes similar to those that produce the low-mass stars, with accretion/ejection phenomena occurring at some point of the evolution of the protostar. This picture seems to be supported by the detection of a collimated stellar wind emanating from the massive protostar IRAS 16547-4247. A triple radio source is associated with the protostar: a compact core and two radio lobes. The emission of the southern lobe is clearly non-thermal. Such emission is interpreted as synchrotron radiation produced by relativistic electrons locally accelerated at the termination point of a thermal jet. Since the ambient medium is determined by the properties of the molecular cloud in which the whole system is embedded, we can expect high densities of particles and infrared photons. Because of the confirmed presence of relativistic electrons, inverse Compton and relativistic Bremsstrahlung interactions are unavoidable.

Published
2007
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11. Observation of VHE γ-rays from Cassiopeia A with the MAGIC telescope

Author

Albert, J., Aliu, E., Anderhub, H., Antoranz, P., Armada, A., Baixeras, C., Barrio, J. A., Bartko, H., Bastieri, D., Becker, J. K., Bednarek, W., Berger, K., Bigongiari, C., Biland, A., Bock, R. K., Bordas, P., Bosch-Ramon, V., Bretz, T., Britvitch, I., Camara, M., Carmona, E., Chilingarian, A., Coarasa, J. A., Commichau, S., Contreras, J. L., Cortina, J., Costado, M. T., Curtef, V., Danielyan, V., Dazzi, F., Angelis, A. De, Delgado, C., de los Reyes, R., De Lotto, B., Domingo-Santamaría, E., Dorner, D., Doro, M., Errando, M., Fagiolini, M., Ferenc, D., Fernández, E., Firpo, R., Flix, J., Fonseca, M. V., Font, L., Fuchs, M., Galante, N., García-López, R., Garczarczyk, M., Gaug, M., Giller, M., Goebel, F., Hakobyan, D., Hayashida, M., Hengstebeck, T., Herrero, A., Höhne, D., Hose, J., Hsu, C. C., Jacon, P., Jogler, T., Kosyra, R., Kranich, D., Kritzer, R., Laille, A., Lindfors, E., Lombardi, S., Longo, F., López, J., López, M., Lorenz, E., Majumdar, P., Maneva, G., Mannheim, K., Mansutti, O., Mariotti, M., Martínez, M., Mazin, D., Merck, C., Meucci, M., Meyer, M., Miranda, J. M., Mirzoyan, R., Mizobuchi, S., Moralejo, A., Nilsson, K., Ninkovic, J., Oña-Wilhelmi, E., Otte, N., Oya, I., Paneque, D., Panniello, M., Paoletti, R., Paredes, J. M., Pasanen, M., Pascoli, D., Pauss, F., Pegna, R., Persic, M., Peruzzo, L., Piccioli, A., Poller, M., Puchades, N., Prandini, E., Raymers, A., Rhode, W., Ribó, M., Rico, J., Rissi, M., Robert, A., Rügamer, S., Saggion, A., Sánchez, A., Sartori, P., Scalzotto, V., Scapin, V., Schmitt, R., Schweizer, T., Shayduk, M., Shinozaki, K., Shore, S. N., Sidro, N., Sillanpää, A., Sobczynska, D., Stamerra, A., Stark, L. S., Takalo, L., Temnikov, P., Tescaro, D., Teshima, M., Tonello, N., Torres, D. F., Turini, N., Vankov, H., Vitale, V., Wagner, R. M., Wibig, T., Wittek, W., Zandanel, F., Zanin, R., Zapatero, J., Albert, J., Aliu, E., Anderhub, H., Antoranz, P., Armada, A., Baixeras, C., Barrio, J. A., Bartko, H., Bastieri, D., Becker, J. K., Bednarek, W., Berger, K., Bigongiari, C., Biland, A., Bock, R. K., Bordas, P., Bosch-Ramon, V., Bretz, T., Britvitch, I., Camara, M., Carmona, E., Chilingarian, A., Coarasa, J. A., Commichau, S., Contreras, J. L., Cortina, J., Costado, M. T., Curtef, V., Danielyan, V., Dazzi, F., Angelis, A. De, Delgado, C., de los Reyes, R., De Lotto, B., Domingo-Santamaría, E., Dorner, D., Doro, M., Errando, M., Fagiolini, M., Ferenc, D., Fernández, E., Firpo, R., Flix, J., Fonseca, M. V., Font, L., Fuchs, M., Galante, N., García-López, R., Garczarczyk, M., Gaug, M., Giller, M., Goebel, F., Hakobyan, D., Hayashida, M., Hengstebeck, T., Herrero, A., Höhne, D., Hose, J., Hsu, C. C., Jacon, P., Jogler, T., Kosyra, R., Kranich, D., Kritzer, R., Laille, A., Lindfors, E., Lombardi, S., Longo, F., López, J., López, M., Lorenz, E., Majumdar, P., Maneva, G., Mannheim, K., Mansutti, O., Mariotti, M., Martínez, M., Mazin, D., Merck, C., Meucci, M., Meyer, M., Miranda, J. M., Mirzoyan, R., Mizobuchi, S., Moralejo, A., Nilsson, K., Ninkovic, J., Oña-Wilhelmi, E., Otte, N., Oya, I., Paneque, D., Panniello, M., Paoletti, R., Paredes, J. M., Pasanen, M., Pascoli, D., Pauss, F., Pegna, R., Persic, M., Peruzzo, L., Piccioli, A., Poller, M., Puchades, N., Prandini, E., Raymers, A., Rhode, W., Ribó, M., Rico, J., Rissi, M., Robert, A., Rügamer, S., Saggion, A., Sánchez, A., Sartori, P., Scalzotto, V., Scapin, V., Schmitt, R., Schweizer, T., Shayduk, M., Shinozaki, K., Shore, S. N., Sidro, N., Sillanpää, A., Sobczynska, D., Stamerra, A., Stark, L. S., Takalo, L., Temnikov, P., Tescaro, D., Teshima, M., Tonello, N., Torres, D. F., Turini, N., Vankov, H., Vitale, V., Wagner, R. M., Wibig, T., Wittek, W., Zandanel, F., Zanin, R., and Zapatero, J.

Abstract

Aims.We searched for very high energy (VHE) γ-ray emission from the supernova remnant Cassiopeia A

Published
2007
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12. Exploring the connection between the stellar wind and the non-thermal emission in LS 5039 ***

Author

Bosch-Ramon, V., Motch, C., Ribó, M., Lopes de Oliveira, R., Janot-Pacheco, E., Negueruela, I., Paredes, J. M., Martocchia, A., Bosch-Ramon, V., Motch, C., Ribó, M., Lopes de Oliveira, R., Janot-Pacheco, E., Negueruela, I., Paredes, J. M., and Martocchia, A.

Abstract

Context.LS 5039 has been observed with several X-ray instruments so far showing quite steady emission in the long term and no signatures of accretion disk. The source also presents X-ray variability at orbital timescales in flux and photon index. The system harbors an O-type main sequence star with moderate mass-loss. At present, the link between the X-rays and the stellar wind is unclear.

Published
2007
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13. Deep radio images of the HEGRA and Whipple TeV sources in the Cygnus OB2 region*

Author

Martí, J., Paredes, J. M., Ishwara Chandra, C. H., Bosch-Ramon, V., Martí, J., Paredes, J. M., Ishwara Chandra, C. H., and Bosch-Ramon, V.

Abstract

Context.The modern generation of Cherenkov telescopes has revealed a new population of gamma-ray sources in the Galaxy. Some of them have been identified with previously known X-ray binary systems while other remain without clear counterparts a lower energies. Our initial goal here was reporting on extensive radio observations of the first extended and yet unidentified source, namely TeV J2032+4130. This object was originally detected by the HEGRA telescope in the direction of the Cygnus OB2 region and its nature has been a matter of debate during the latest years. The situation has become more complex with the Whipple and MILAGRO telescopes new TeV detections in the same field which could be consistent with the historic HEGRA source, although a different origin cannot be ruled out.

Published
2007
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14. The radio to TeV orbital variability of the microquasar LS I +61 303

Author

Bosch-Ramon, V., Paredes, J. M., Romero, G. E., Ribó, M., Bosch-Ramon, V., Paredes, J. M., Romero, G. E., and Ribó, M.

Abstract

Context.The microquasar LS I +61 303 has recently been detected at TeV energies by the Cherenkov telescope MAGIC, presenting variability on timescales similar to its orbital period. This system has been intensively observed at different wavelengths during the last three decades, showing a very complex behavior along the orbit.

Published
2006
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15. INTEGRAL and XMM-Newton observations towards the unidentified MeV source GRO J1411-64

Author

Torres, D. F., Zhang, S., Reimer, O., Barcons, X., Corral, A., Bosch-Ramon, V., Paredes, J. M., Romero, G. E., Qu, J.-L., Collmar, W., Schönfelder, V., Butt, Y., Torres, D. F., Zhang, S., Reimer, O., Barcons, X., Corral, A., Bosch-Ramon, V., Paredes, J. M., Romero, G. E., Qu, J.-L., Collmar, W., Schönfelder, V., and Butt, Y.

Abstract

Aims.We investigate the nature of the COMPTEL unidentified source GRO J1411-64.

Published
2006
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16. On the multiwavelength spectrum of the microquasar 1E 1740.7-2942

Author

Bosch-Ramon, V., Romero, G. E., Paredes, J. M., Bazzano, A., Del Santo, M., Bassani, L., Bosch-Ramon, V., Romero, G. E., Paredes, J. M., Bazzano, A., Del Santo, M., and Bassani, L.

Abstract

Context.The microquasar 1E 1740.7-2942 is a source located in the direction of the Galactic Center. It has been detected at X-rays, soft gamma-rays, and in the radio band, showing an extended radio component in the form of a double-sided jet. Although no optical counterpart has been found so far for 1E 1740.7-2942, its X-ray activity strongly points to a galactic nature.

Published
2006
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17. Spectral energy distribution of the γ-ray microquasar LS 5039

Author

Paredes, J. M., Bosch-Ramon, V., Romero, G. E., Paredes, J. M., Bosch-Ramon, V., and Romero, G. E.

Abstract

The microquasar LS 5039 has recently been detected as a source of very high energy (VHE) γ-rays. This detection, that confirms the previously proposed association of LS 5039 with the EGRET source 3EG J1824-1514, makes of LS 5039 a special system with observational data covering nearly all the electromagnetic spectrum. In order to reproduce the observed spectrum of LS 5039, from radio to VHE γ-rays, we have applied a cold matter dominated jet model that takes into account accretion variability, the jet magnetic field, particle acceleration, adiabatic and radiative losses, microscopic energy conservation in the jet, and pair creation and absorption due to the external photon fields, as well as the emission from the first generation of secondaries. The radiative processes taken into account are synchrotron, relativistic Bremsstrahlung and inverse Compton (IC). The model is based on a scenario that has been characterized with recent observational results, concerning the orbital parameters, the orbital variability at X-rays and the nature of the compact object. The computed spectral energy distribution (SED) shows a good agreement with the available observational data.

Published
2006
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18. A microquasar model applied to unidentified gamma-ray sources

Author

Bosch-Ramon, V., Paredes, J. M., Romero, G. E., Torres, D. F., Bosch-Ramon, V., Paredes, J. M., Romero, G. E., and Torres, D. F.

Abstract

Among unidentified gamma-ray sources in the galactic plane, there are some that present significant variability and have been proposed to be high-mass microquasars. To deepen the study of the possible association between variable low galactic latitude gamma-ray sources and microquasars, we have applied a leptonic jet model based on the microquasar scenario that reproduces the gamma-ray spectrum of three unidentified gamma-ray sources, 3EG J1735-1500, 3EG J1828+0142  and GRO J1411-64, and is consistent with the observational constraints at lower energies. We conclude that if these sources were generated by microquasars, the particle acceleration processes could not be as efficient as in other objects of this type that present harder gamma-ray spectra. Moreover, the dominant mechanism of high-energy emission should be synchrotron self-Compton (SSC) scattering, and the radio jets may only be observed at low frequencies. For each particular case, further predictions of jet physical conditions and variability generation mechanisms have been made in the context of the model. Although there might be other candidates able to explain the emission coming from these sources, microquasars cannot be excluded as counterparts. Observations performed by the next generation of gamma-ray instruments, like GLAST, are required to test the proposed model.

Published
2006
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19. A broadband leptonic model for gamma-ray emitting microquasars

Author

Bosch-Ramon, V., Romero, G. E., Paredes, J. M., Bosch-Ramon, V., Romero, G. E., and Paredes, J. M.

Abstract

Observational and theoretical studies point to microquasars (MQs) as possible counterparts of a significant fraction of the unidentifiedgamma-ray sources detected so far. At present, a proper scenario to explain the emission beyond soft X-rays from these objects is not known, nor what the precise connection is between the radio and the high-energy radiation. We develop a new model where the MQ jet is dynamically dominated by cold protons and radiatively dominated by relativistic leptons. The matter content and power of the jet are both related with the accretion process. The magnetic field is assumed to be close to equipartition, although it is attached to and dominated by the jet matter. For the relativistic particles in the jet, their maximum energy depends on both the acceleration efficiency and the energy losses. The model takes into account the interaction of the relativistic jet particles with the magnetic field and all the photon and matter fields. Such interaction produces significant amounts of radiation from radio to very high energies through synchrotron, relativistic Bremsstrahlung, and inverse Compton (IC) processes. Variability of the emission produced by changes in the accretion process (e.g. via orbital eccentricity) is also expected. The effects of the gamma-ray absorption by the external photon fields on the gamma-ray spectrum have been taken into account, revealing clear spectral features that might be observed. This model is consistent to the accretion scenario, energy conservation laws, and current observational knowledge, and can provide deeper physical information of the source when tested against multiwavelength data.

Published
2006
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20. Electromagnetic radiation initiated by hadronic jets from microquasars in the ISM

Author

Bosch-Ramon, V., Aharonian, F. A., Paredes, J. M., Bosch-Ramon, V., Aharonian, F. A., and Paredes, J. M.

Abstract

Microquasars are potential candidates to produce a non-negligible fraction of the observed galactic cosmic rays. The protons accelerated at the jet termination shock interact with the interstellar medium and may produce detectable fluxes of extended emission at different energy bands: high-energy and very high-energy γ-rays produced by neutral pion-decay, synchrotron and bremsstrahlung emission in a wide energy range generated by the secondary electrons produced by charged pion-decay. We discuss the association between this scenario and some of the unidentified EGRET sources in the galactic plane.

Published
2005
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21. High-mass microquasars and low-latitude gamma-ray sources

Author

Bosch-Ramon, V., Romero, G. E., Paredes, J. M., Bosch-Ramon, V., Romero, G. E., and Paredes, J. M.

Abstract

Population studies of unidentified EGRET sources suggest that there exist at least three different populations of galactic gamma-ray sources. One of these populations is formed by young objects distributed along the galactic plane with a strong concentration toward the inner spiral arms of the Galaxy. Variability, spectral and correlation analysis indicate that this population is not homogeneous. In particular, there is a subgroup of sources that display clear variability in their gamma-ray fluxes on timescales from days to months. Following the proposal by Kaufman Bernadó et al. (2002), we suggest that this group of sources might be high-mass microquasars, i.e. accreting black holes or neutron stars with relativistic jets and early-type stellar companions. We present detailed inhomogeneous models for the gamma-ray emission of these systems that include both external and synchrotron self-Compton interactions. We have included effects of interactions between the jet and all external photon fields to which it is exposed: companion star, accretion disk, and hot corona. We make broadband calculations to predict the spectral energy distribution of the emission produced in the inner jet of these objects up to GeV energies. The results and predictions can be tested by present and future gamma-ray instruments like INTEGRAL, AGILE, and GLAST.

Published
2005
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22. γ-ray emission from microquasars: A numerical model for LSI +61°303

Author

Bosch-Ramon, V., Paredes, J. M., Bosch-Ramon, V., and Paredes, J. M.

Abstract

We explore the possible association between the microquasar LSI +61°303 and the EGRET source 2CG 135+01/3EG J0241+6103 by studying, with a detailed numerical model, whether this system can produce the emission and the variability detected by EGRET (>100 MeV) through inverse Compton (IC) scattering. Our numerical approach considers a population of relativistic electrons entrained in a cylindrical inhomogeneous jet, interacting with both the radiation and the magnetic fields, taking into account the Thomson and Klein-Nishina regimes of interaction. Our results reproduce the observed spectral characteristics and variability at γ-rays, thus strengthening the identification of LSI +61°303 as a high-energy γ-ray source.

Published
2004
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23. A numerical model for the γ-ray emission of the microquasar LS 5039

Author

Bosch-Ramon, V., Paredes, J. M., Bosch-Ramon, V., and Paredes, J. M.

Abstract

The possible association between the microquasar LS 5039 and the EGRET source 3EG J1824-1514 suggests that microquasars could also be sources of high-energy γ-rays. In this paper, we explore, with a detailed numerical model, if this system can produce the emission detected by EGRET (>100 MeV) through inverse Compton (IC) scattering. Our numerical approach considers a population of relativistic electrons entrained in a cylindrical inhomogeneous jet, interacting with both the radiation and the magnetic fields, taking into account the Thomson and Klein-Nishina regimes of interaction. The computed spectrum reproduces the observed spectral characteristics at very high energy.

Published
2004
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24. High-energy emission from jet-clump interactions in microquasars

Author

Araudo, A., Bosch-Ramon, V., and Romero, G.

Abstract

Context. High-mass microquasars are binary systems consisting of a massive star and an accreting compact object from which relativistic jets are launched. There is considerable observational evidence that winds of massive stars are clumpy. Individual clumps may interact with the jets in high-mass microquasars to produce outbursts of high-energy emission. Gamma-ray flares have been detected in some high-mass X-ray binaries, such as Cygnus X-1, and probably in LS 5039 and LS I+61 303.Aims. We predict the high-energy emission produced by the interaction between a jet and a clump of the stellar wind in a high-mass microquasar.Methods. Assuming a hydrodynamic scenario for the jet-clump interaction, we calculate the spectral energy distributions produced by the dominant non-thermal processes: relativistic bremsstrahlung, synchrotron and inverse Compton radiation, for leptons, and for hadrons, proton-proton collisions.Results. Significant levels of emission in X-rays (synchrotron), high-energy gamma rays (inverse Compton), and very high-energy gamma rays (from the decay of neutral pions) are predicted, with luminosities in the different domains in the range ~1032-1035?erg?s-1. The spectral energy distributions vary strongly depending on the specific conditions.Conclusions. Jet-clump interactions may be detectable at high and very high energies, and provide an explanation for the fast TeV variability found in some high-mass X-ray binary systems. Our model can help to infer information about the properties of jets and clumpy winds by means of high-sensitivity gamma-ray astronomy.

Published
2009

25. Studying the properties of the radio emitter in LS?5039

Author

Bosch-Ramon, V.

Abstract

Context. LS?5039 is an X-ray binary that presents non-thermal radio emission. The radiation at ~5?GHz is quite steady and optically thin, consisting of a dominant core plus an extended jet-like structure. There is a spectral turnover around 1?GHz, and evidence of variability on timescales of 1?yr at 234?MHz.Aims. We investigate the radio emitter properties using the available broadband radio data, and assuming two possible scenarios to explain the turnover: free-free absorption in the stellar wind, or synchrotron self-absorption.Methods. We use the relationships between the turnover frequency, the stellar wind density, the emitter location, size and magnetic field, and the Lorentz factor of the emitting electrons, as well as a reasonable assumption regarding the energy budget, to infer the properties of the low-frequency radio emitter. Also, we put this information in context with the broadband radio data.Results. The location and size of the low-frequency radio emitter can be restricted to ?few?AU from the primary star, its magnetic field to ~3?? 10-3?1?G, and the electron Lorentz factors to ~10-100. The observed variability of the extended structures seen with VLBA would point to electron bulk velocities ?3?? 108?cm?s-1, whereas much less variable radiation at 5?GHz would indicate velocities for the VLBA core ?108?cm?s-1. The emission at 234?MHz in the high state would mostly come from a region larger than the dominant broadband radio emitter.Conclusions. We suggest a scenario in which secondary pairs, created via gamma-ray absorption and moving in the stellar wind, are behind the steady broadband radio core, whereas the resolved jet-like radio emission would come from a collimated, faster, outflow.

Published
2009

26. The magnetic field and the location of the TeV emitter in Cygnus?X-1 and LS?5039

Author

Bosch-Ramon, V., Khangulyan, D., and Aharonian, F.

Abstract

Context. Cygnus?X-1 and LS?5039 are two X-ray binaries observed at TeV energies. Both sources are compact systems, contain jet-like (radio) structures, and harbor very luminous O stars. A TeV signal has been found around the superior conjunction of the compact object in both objects, when the highest gamma-ray opacities are expected.Aims. We investigate the implications of finding TeV emission from Cygnus?X-1 and LS?5039 around the superior conjunction, since this can give information on the system magnetic field and the location of the TeV emitter.Methods. Using the very high-energy spectra and fluxes observed around the superior conjunction in Cygnus?X-1 and LS?5039, we compute the absorbed luminosity that is caused by pair creation in the stellar photon field for different emitter positions with respect to the star and the observer line of sight. The role of the magnetic field and electromagnetic cascading are discussed. For the case of inefficient electromagnetic cascading, the expected secondary synchrotron fluxes are compared with the observed ones at X-ray energies.Results. We find that, in Cygnus?X-1 and LS?5039, either the magnetic field in the star surroundings is much smaller than the one expected for O stars or the TeV emitter is located at a distance >1012?cm from the compact object.Conclusions. Our results strongly suggest that the TeV emitters in Cygnus?X-1 and LS?5039 are located at the borders of the binary system and well above the orbital plane. This would not agree with those models for which the emitter is well inside the system, like the innermost-jet region (Cygnus?X-1 and LS?5039; microquasar scenario) or the region between the pulsar and the primary star (LS?5039; standard pulsar scenario).

Published
2008

27. Non-thermal emission from secondary pairs in close TeV binary systems

Author

Bosch-Ramon, V., Khangulyan, D., and Aharonian, F.

Abstract

Context. Massive hot stars produce dense ultraviolet (UV) photon fields in their surroundings. If a very high-energy (VHE) gamma ray emitter is located close to the star, then gamma rays are absorbed in the stellar photon field, creating secondary (electron-positron) pairs.Aims. We study the broadband emission of these secondary pairs in the stellar photon and magnetic fields.Methods. Under certain assumptions regarding the stellar wind and the magnetic field in the surroundings of a massive hot star, we calculate the steady state energy distribution of secondary pairs created in the system and its radiation from radio to gamma rays.Results. Under the ambient magnetic field, possibly high enough to suppress electromagnetic (EM) cascading, the energy of secondary pairs is radiated via synchrotron and single IC scattering producing radio-to-gamma ray radiation. The synchrotron spectral energy distribution (SED) is hard, peaks around X-ray energies, and becomes softer. The IC SED is hard as well and peaks around 10?GeV, also becoming softer at higher energies due to synchrotron loss dominance.Conclusions. The radio emission from secondary pairs is moderate and detectable as a point-like and/or extended source. In X-rays, the secondary pair synchrotron component may be dominant. At energies ?10?GeV, the secondary pair IC radiation may be dominant over the primary gamma ray emission, and possibly detectable by the next generation of instruments.

Published
2008

28. Radio detections towards unidentified variable EGRET sources

Author

Paredes, J., Mart?, J., Ishwara-Chandra, C., Torres, D., Romero, G., Combi, J., Bosch-Ramon, V., Mu?oz-Arjonilla, A., and S?nchez-Sutil, J.

Abstract

Context. A considerable fraction of the ?-ray sources discovered with the Energetic Gamma-Ray Experiment Telescope (EGRET) remain unidentified. The EGRET sources that have been properly identified are either pulsars or variable sources at both radio and gamma-ray wavelengths. Most of the variable sources are strong radio blazars. However, some low galactic-latitude EGRET sources, with highly variable ?-ray?emission, lack any evident counterpart according to the radio data available until now.Aims. The primary goal of this paper is to identify and characterise the potential radio counterparts of four highly variable ?-ray sources in the galactic plane through mapping the radio surroundings of the EGRET?confidence contours and determining the variable radio sources in the field whenever possible.Methods. We have carried out a radio exploration of the fields of the selected EGRET sources using the Giant Metrewave Radio Telescope (GMRT) interferometer at 21?cm wavelength, with pointings being separated by months.Results. We detected a total of 151 radio sources. Among them, we identified a few radio sources whose flux density has apparently changed on timescales of months. Despite the limitations of our search, their possible variability makes these objects a top-priority target for multiwavelength studies of the potential counterparts of highly variable, unidentified gamma-ray sources.

Published
2008

29. MAGIC observations of PG?1553+113 during a multiwavelength campaign in July 2006

Author

Albert, J., Aliu, E., Anderhub, H., Antoranz, P., Baixeras, C., Barrio, J., Bartko, H., Bastieri, D., Becker, J., Bednarek, W., Berdyugin, A., Berger, K., Bigongiari, C., Biland, A., Bock, R., Bordas, P., Bosch-Ramon, V., Bretz, T., Britvitch, I., Camara, M., Carmona, E., Chilingarian, A., Commichau, S., Contreras, J., Cortina, J., Costado, M., Curtef, V., Danielyan, V., Dazzi, F., De Angelis, A., Delgado, C., de los Reyes, R., De Lotto, B., Dorner, D., Doro, M., Errando, M., Fagiolini, M., Ferenc, D., Fern?ndez, E., Firpo, R., Fonseca, M., Font, L., Fuchs, M., Galante, N., Garc?a-L?pez, R., Garczarczyk, M., Gaug, M., Goebel, F., Hakobyan, D., Hayashida, M., Hengstebeck, T., Herrero, A., H?hne, D., Hose, J., Hsu, C., Huber, S., Jacon, P., Jogler, T., Kosyra, R., Kranich, D., Kritzer, R., Laille, A., Lindfors, E., Lombardi, S., Longo, F., L?pez, M., Lorenz, E., Majumdar, P., Maneva, G., Mannheim, K., Mariotti, M., Mart?nez, M., Mazin, D., Merck, C., Meucci, M., Meyer, M., Miranda, J., Mirzoyan, R., Mizobuchi, S., Moralejo, A., Nieto, D., Nilsson, K., Ninkovic, J., O?a-Wilhelmi, E., Otte, N., Oya, I., Panniello, M., Paoletti, R., Pasanen, M., Pascoli, D., Pauss, F., Pegna, R., Persic, M., Peruzzo, L., Piccioli, A., Prandini, E., Puchades, N., Raymers, A., Rico, J., Rhode, W., Rico, J., Rissi, M., Robert, A., R?gamer, S., Saggion, A., Saito, T., S?nchez, A., Sartori, P., Scalzotto, V., Scapin, V., Schmitt, R., Schweizer, T., Shayduk, M., Shinozaki, K., Shore, S., Sidro, N., Sillanp??, A., Sobczynska, D., Spanier, F., Stamerra, A., Stark, L., Takalo, L., Temnikov, P., Tescaro, D., Teshima, M., Torres, D., Turini, N., Vankov, H., Venturini, A., Vitale, V., Wagner, R., Wibig, T., Wittek, W., Zandanel, F., Zanin, R., and Zapatero, J.

Abstract

The active galactic nucleus PG?1553+113 was observed by the MAGIC telescope in July?2006 during a multiwavelength campaign, in which telescopes in the optical, X-ray, and very high energies participated. Although the MAGIC data were affected by strong atmospheric absorption (calima), they were analyzed after applying a correction. In 8.5?h, a signal was detected with a significance of 5.0?. The integral flux above 150?GeV was (2.6?0.9)?10-7?phs-1m-2. By fitting the differential energy spectrum with a power law, a spectral index of -4.1?0.3 was obtained.

Published
2009

30. Large-scale flow dynamics and radiation in pulsar γ-ray binaries

Author

Bosch-Ramon, V. and Barkov, M. V.

Abstract

Context.Several gamma-ray binaries show extended X-ray emission that may be associated to interactions of an outflow with the medium. Some of these systems are, or may be, high-mass binaries harboring young nonaccreting pulsars, in which the stellar and the pulsar winds collide, generating a powerful outflow that should terminate at some point in the ambient medium.

Published
2011
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32. On the origin of correlated X-ray/VHE emission from LS I +61 303

Author

Zabalza, V., Paredes, J. M., and Bosch-Ramon, V.

Abstract

Context.The MAGIC collaboration recently reported correlated X-ray and very high-energy (VHE) gamma-ray emission from the gamma-ray binary LS I +61 303 during  ~60% of one orbit. These observations suggest that the emission in these two bands has its origin in a single particle population.

Published
2011
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33. Search for an extended VHE γ-ray emission from Mrk 421 and Mrk 501 with the MAGIC Telescope

Author

Aleksić, J., Antonelli, L. A., Antoranz, P., Backes, M., Baixeras, C., Barrio, J. A., Bastieri, D., Becerra González, J., Bednarek, W., Berdyugin, A., Berger, K., Bernardini, E., Biland, A., Blanch, O., Bock, R. K., Bonnoli, G., Bordas, P., Borla Tridon, D., Bosch-Ramon, V., Bose, D., Braun, I., Bretz, T., Britzger, D., Camara, M., Carmona, E., Carosi, A., Colin, P., Commichau, S., Contreras, J. L., Cortina, J., Costado, M. T., Covino, S., Dazzi, F., De Angelis, A., De Cea del Pozo, E., De los Reyes, R., De Lotto, B., De Maria, M., De Sabata, F., Delgado Mendez, C., Doert, M., Domínguez, A., Dominis Prester, D., Dorner, D., Doro, M., Elsaesser, D., Errando, M., Ferenc, D., Fonseca, M. V., Font, L., García López, R. J., Garczarczyk, M., Gaug, M., Godinovic, N., Hadasch, D., Herrero, A., Hildebrand, D., Höhne-Mönch, D., Hose, J., Hrupec, D., Hsu, C. C., Jogler, T., Klepser, S., Krähenbühl, T., Kranich, D., La Barbera, A., Laille, A., Leonardo, E., Lindfors, E., Lombardi, S., Longo, F., López, M., Lorenz, E., Majumdar, P., Maneva, G., Mankuzhiyil, N., Mannheim, K., Maraschi, L., Mariotti, M., Martínez, M., Mazin, D., Meucci, M., Miranda, J. M., Mirzoyan, R., Miyamoto, H., Moldón, J., Moles, M., Moralejo, A., Nieto, D., Nilsson, K., Ninkovic, J., Orito, R., Oya, I., Paiano, S., Paoletti, R., Paredes, J. M., Partini, S., Pasanen, M., Pascoli, D., Pauss, F., Pegna, R. G., Perez-Torres, M. A., Persic, M., Peruzzo, L., Prada, F., Prandini, E., Puchades, N., Puljak, I., Reichardt, I., Rhode, W., Ribó, M., Rico, J., Rissi, M., Rügamer, S., Saggion, A., Saito, T. Y., Salvati, M., Sánchez-Conde, M., Satalecka, K., Scalzotto, V., Scapin, V., Schultz, C., Schweizer, T., Shayduk, M., Shore, S. N., Sierpowska-Bartosik, A., Sillanpää, A., Sitarek, J., Sobczynska, D., Spanier, F., Spiro, S., Stamerra, A., Steinke, B., Struebig, J. C., Suric, T., Takalo, L., Tavecchio, F., Temnikov, P., Terzic, T., Tescaro, D., Teshima, M., Torres, D. F., Vankov, H., Wagner, R. M., Weitzel, Q., Zabalza, V., Zandanel, F., Zanin, R., Neronov, A., and Semikoz, D. V.

Abstract

Context.Part of the very high energy γ-ray radiation coming from extragalactic sources is absorbed through the pair production process on the extragalactic background light photons. Extragalactic magnetic fields alter the trajectories of these cascade pairs and, in turn, convert cosmic background photons to γ-ray energies by inverse Compton scattering. These secondary photons can form an extended halo around bright VHE sources.

Published
2010
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34. Gamma rays from cloud penetration at the base of AGN jets

Author

Araudo, A. T., Bosch-Ramon, V., and Romero, G. E.

Abstract

Context.Dense and cold clouds seem to populate the broad line region surrounding the central black hole in AGNs. These clouds may interact with the AGN jet base which could have observational consequences.

Published
2010
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35. Simultaneous multi-frequency observation of the unknown redshift blazar PG 1553+113 in March-April 2008

Author

Aleksić, J., Anderhub, H., Antonelli, L. A., Antoranz, P., Backes, M., Baixeras, C., Balestra, S., Barrio, J. A., Bastieri, D., Becerra González, J., Becker, J. K., Bednarek, W., Berdyugin, A., Berger, K., Bernardini, E., Biland, A., Bock, R. K., Bonnoli, G., Bordas, P., Borla Tridon, D., Bosch-Ramon, V., Bose, D., Braun, I., Bretz, T., Britzger, D., Camara, M., Carmona, E., Carosi, A., Colin, P., Commichau, S., Contreras, J. L., Cortina, J., Costado, M. T., Covino, S., Dazzi, F., De Angelis, A., de Cea del Pozo, E., De los Reyes, R., De Lotto, B., De Maria, M., De Sabata, F., Delgado Mendez, C., Domínguez, A., Dominis Prester, D., Dorner, D., Doro, M., Elsaesser, D., Errando, M., Ferenc, D., Fernández, E., Firpo, R., Fonseca, M. V., Font, L., Galante, N., García López, R. J., Garczarczyk, M., Gaug, M., Godinovic, N., Goebel, F., Hadasch, D., Herrero, A., Hildebrand, D., Höhne-Mönch, D., Hose, J., Hrupec, D., Hsu, C. C., Jogler, T., Klepser, S., Krähenbühl, T., Kranich, D., La Barbera, A., Laille, A., Leonardo, E., Lindfors, E., Lombardi, S., Longo, F., López, M., Lorenz, E., Majumdar, P., Maneva, G., Mankuzhiyil, N., Mannheim, K., Maraschi, L., Mariotti, M., Martínez, M., Mazin, D., Meucci, M., Miranda, J. M., Mirzoyan, R., Miyamoto, H., Moldón, J., Moles, M., Moralejo, A., Nieto, D., Nilsson, K., Ninkovic, J., Orito, R., Oya, I., Paoletti, R., Paredes, J. M., Pasanen, M., Pascoli, D., Pauss, F., Pegna, R. G., Perez-Torres, M. A., Persic, M., Peruzzo, L., Prada, F., Prandini, E., Puchades, N., Puljak, I., Reichardt, I., Rhode, W., Ribó, M., Rico, J., Rissi, M., Rügamer, S., Saggion, A., Saito, T. Y., Salvati, M., Sánchez-Conde, M., Satalecka, K., Scalzotto, V., Scapin, V., Schweizer, T., Shayduk, M., Shore, S. N., Sierpowska-Bartosik, A., Sillanpää, A., Sitarek, J., Sobczynska, D., Spanier, F., Spiro, S., Stamerra, A., Steinke, B., Strah, N., Struebig, J. C., Suric, T., Takalo, L., Tavecchio, F., Temnikov, P., Tescaro, D., Teshima, M., Torres, D. F., Turini, N., Vankov, H., Wagner, R. M., Zabalza, V., Zandanel, F., Zanin, R., Zapatero, J., Pian, E., Bianchin, V., D'Ammando, F., Di Cocco, G., Fugazza, D., Ghisellini, G., Kurtanidze, O. M., Raiteri, C. M., Tosti, G., Treves, A., Vercellone, S., and Villata, M.

Abstract

The blazar PG 1553+113 is a well known TeV γ-ray emitter. In this paper we determine its spectral energy distribution through simultaneous multi-frequency data to study its emission processes. An extensive campaign was carried out between March and April 2008, where optical, X-ray, high-energy (HE) γ-ray, and very-high-energy (VHE) γ-ray data were obtained with the KVA, Abastumani, REM, RossiXTE/ASM, AGILE and MAGIC telescopes, respectively. We combine the data to derive the source's spectral energy distribution and interpret its double-peaked shape within the framework of a synchrotron self-Compton model.

Published
2010

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