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Prospects for Cherenkov Telescope Array Observations of the Young Supernova Remnant RX J1713.7-3946
(2017)
Acero, F. ; Aloisio, R. ; Amans, J. ; Amato, Elena ; Antonelli, L. A. ; Aramo, C. ; Armstrong, T. ; Arqueros, F. ; Asano, Katsuaki ; Ashley, M. ; Backes, M. ; Balazs, C. ; Balzer, A. ; Bamba, Aya ; Barkov, Maxim ; Barrio, J. A. ; Benbow, Wystan ; Bernloehr, K. ; Beshley, V. ; Bigongiari, C. ; Biland, A. ; Bilinsky, A. ; Bissaldi, Elisabetta ; Biteau, J. ; Blanch, O. ; Blasi, P. ; Blazek, J. ; Boisson, C. ; Bonanno, G. ; Bonardi, A. ; Bonavolonta, C. ; Bonnoli, G. ; Braiding, C. ; Brau-Nogue, S. ; Bregeon, J. ; Brown, A. M. ; Bugaev, V. ; Bulgarelli, A. ; Bulik, T. ; Burton, Michael ; Burtovoi, A. ; Busetto, G. ; Bottcher, M. ; Cameron, R. ; Capalbi, M. ; Caproni, Anderson ; Caraveo, P. ; Carosi, R. ; Cascone, E. ; Cerruti, M. ; Chaty, Sylvain ; Chen, A. ; Chen, X. ; Chernyakova, M. ; Chikawa, M. ; Chudoba, J. ; Cohen-Tanugi, J. ; Colafrancesco, S. ; Conforti, V. ; Contreras, J. L. ; Costa, A. ; Cotter, G. ; Covino, Stefano ; Covone, G. ; Cumani, P. ; Cusumano, G. ; Daniel, M. ; Dazzi, F. ; De Angelis, A. ; De Cesare, G. ; De Franco, A. ; De Frondat, F. ; Dal Pino, E. M. de Gouveia ; De Lisio, C. ; Lopez, R. de los Reyes ; De Lotto, B. ; de Naurois, M. ; De Palma, F. ; Del Santo, M. ; Delgado, C. ; della Volpe, D. ; Di Girolamo, T. ; Di Giulio, C. ; Di Pierro, F. ; Di Venere, L. ; Doro, M. ; Dournaux, J. ; Dumas, D. ; Dwarkadas, Vikram V. ; Diaz, C. ; Ebr, J. ; Egberts, Kathrin ; Einecke, S. ; Elsaesser, D. ; Eschbach, S. ; Falceta-Goncalves, D. ; Fasola, G. ; Fedorova, E. ; Fernandez-Barral, A. ; Ferrand, Gilles ; Fesquet, M. ; Fiandrini, E. ; Fiasson, A. ; Filipovic, Miroslav D. ; Fioretti, V. ; Font, L. ; Fontaine, Gilles ; Franco, F. J. ; Freixas Coromina, L. ; Fujita, Yutaka ; Fukui, Y. ; Funk, S. ; Forster, A. ; Gadola, A. ; Lopez, R. Garcia ; Garczarczyk, M. ; Giglietto, N. ; Giordano, F. ; Giuliani, A. ; Glicenstein, J. ; Gnatyk, R. ; Goldoni, P. ; Grabarczyk, T. ; Graciani, R. ; Graham, J. ; Grandi, P. ; Granot, Jonathan ; Green, A. J. ; Griffiths, S. ; Gunji, S. ; Hakobyan, H. ; Hara, S. ; Hassan, T. ; Hayashida, M. ; Heller, M. ; Helo, J. C. ; Hinton, J. ; Hnatyk, B. ; Huet, J. ; Huetten, M. ; Humensky, T. B. ; Hussein, M. ; Horandel, J. ; Ikeno, Y. ; Inada, T. ; Inome, Y. ; Inoue, S. ; Inoue, T. ; Inoue, Y. ; Ioka, K. ; Iori, Maurizio ; Jacquemier, J. ; Janecek, P. ; Jankowsky, D. ; Jung, I. ; Kaaret, P. ; Katagiri, H. ; Kimeswenger, S. ; Kimura, Shigeo S. ; Knodlseder, J. ; Koch, B. ; Kocot, J. ; Kohri, K. ; Komin, N. ; Konno, Y. ; Kosack, K. ; Koyama, S. ; Kraus, Michaela ; Kubo, Hidetoshi ; Mezek, G. Kukec ; Kushida, J. ; La Palombara, N. ; Lalik, K. ; Lamanna, G. ; Landt, H. ; Lapington, J. ; Laporte, P. ; Lee, S. ; Lees, J. ; Lefaucheur, J. ; Lenain, J. -P. ; Leto, Giuseppe ; Lindfors, E. ; Lohse, T. ; Lombardi, S. ; Longo, F. ; Lopez, M. ; Lucarelli, F. ; Luque-Escamilla, Pedro Luis ; Lopez-Coto, R. ; Maccarone, M. C. ; Maier, G. ; Malaguti, G. ; Mandat, D. ; Maneva, G. ; Mangano, S. ; Marcowith, Alexandre ; Marti, J. ; Martinez, M. ; Martinez, G. ; Masuda, S. ; Maurin, G. ; Maxted, N. ; Melioli, Claudio ; Mineo, T. ; Mirabal, N. ; Mizuno, T. ; Moderski, R. ; Mohammed, M. ; Montaruli, T. ; Moralejo, A. ; Mori, K. ; Morlino, G. ; Morselli, A. ; Moulin, Emmanuel ; Mukherjee, R. ; Mundell, C. ; Muraishi, H. ; Murase, Kohta ; Nagataki, Shigehiro ; Nagayoshi, T. ; Naito, T. ; Nakajima, D. ; Nakamori, T. ; Nemmen, R. ; Niemiec, Jacek ; Nieto, D. ; Nievas-Rosillo, M. ; Nikolajuk, M. ; Nishijima, K. ; Noda, K. ; Nogues, L. ; Nosek, D. ; Novosyadlyj, B. ; Nozaki, S. ; Ohira, Yutaka ; Ohishi, M. ; Ohm, S. ; Okumura, A. ; Ong, R. A. ; Orito, R. ; Orlati, A. ; Ostrowski, M. ; Oya, I. ; Padovani, Marco ; Palacio, J. ; Palatka, M. ; Paredes, Josep M. ; Pavy, S. ; Persic, M. ; Petrucci, P. ; Petruk, Oleh ; Pisarski, A. ; Pohl, Martin ; Porcelli, A. ; Prandini, E. ; Prast, J. ; Principe, G. ; Prouza, M. ; Pueschel, Elisa ; Puelhofer, G. ; Quirrenbach, A. ; Rameez, M. ; Reimer, O. ; Renaud, M. ; Ribo, M. ; Rico, J. ; Rizi, V. ; Rodriguez, J. ; Fernandez, G. Rodriguez ; Rodriguez Vazquez, J. J. ; Romano, Patrizia ; Romeo, G. ; Rosado, J. ; Rousselle, J. ; Rowell, G. ; Rudak, B. ; Sadeh, I. ; Safi-Harb, S. ; Saito, T. ; Sakaki, N. ; Sanchez, D. ; Sangiorgi, P. ; Sano, H. ; Santander, M. ; Sarkar, S. ; Sawada, M. ; Schioppa, E. J. ; Schoorlemmer, H. ; Schovanek, P. ; Schussler, F. ; Sergijenko, O. ; Servillat, M. ; Shalchi, A. ; Shellard, R. C. ; Siejkowski, H. ; Sillanpaa, A. ; Simone, D. ; Sliusar, V. ; Sol, H. ; Stanic, S. ; Starling, R. ; Stawarz, L. ; Stefanik, S. ; Stephan, M. ; Stolarczyk, T. ; Szanecki, M. ; Szepieniec, T. ; Tagliaferri, G. ; Tajima, H. ; Takahashi, M. ; Takeda, J. ; Tanaka, M. ; Tanaka, S. ; Tejedor, L. A. ; Telezhinsky, Igor O. ; Temnikov, P. ; Terada, Y. ; Tescaro, D. ; Teshima, M. ; Testa, V. ; Thoudam, S. ; Tokanai, F. ; Torres, D. F. ; Torresi, E. ; Tosti, G. ; Townsley, C. ; Travnicek, P. ; Trichard, C. ; Trifoglio, M. ; Tsujimoto, S. ; Vagelli, V. ; Vallania, P. ; Valore, L. ; van Driel, W. ; van Eldik, C. ; Vandenbroucke, Justin ; Vassiliev, V. ; Vecchi, M. ; Vercellone, Stefano ; Vergani, S. ; Vigorito, C. ; Vorobiov, S. ; Vrastil, M. ; Vazquez Acosta, M. L. ; Wagner, S. J. ; Wagner, R. ; Wakely, S. P. ; Walter, R. ; Ward, J. E. ; Watson, J. J. ; Weinstein, A. ; White, M. ; White, R. ; Wierzcholska, A. ; Wilcox, P. ; Williams, D. A. ; Wischnewski, R. ; Wojcik, P. ; Yamamoto, T. ; Yamamoto, H. ; Yamazaki, Ryo ; Yanagita, S. ; Yang, L. ; Yoshida, T. ; Yoshida, M. ; Yoshiike, S. ; Yoshikoshi, T. ; Zacharias, M. ; Zampieri, L. ; Zanin, R. ; Zavrtanik, M. ; Zavrtanik, D. ; Zdziarski, A. ; Zech, Alraune ; Zechlin, Hannes ; Zhdanov, V. ; Ziegler, A. ; Zorn, J.
We perform simulations for future Cherenkov Telescope Array (CTA) observations of RX J1713.7-3946, a young supernova remnant (SNR) and one of the brightest sources ever discovered in very high energy (VHE) gamma rays. Special attention is paid to exploring possible spatial (anti) correlations of gamma rays with emission at other wavelengths, in particular X-rays and CO/H I emission. We present a series of simulated images of RX J1713.7-3946 for CTA based on a set of observationally motivated models for the gamma-ray emission. In these models, VHE gamma rays produced by high-energy electrons are assumed to trace the nonthermal X-ray emission observed by XMM-Newton, whereas those originating from relativistic protons delineate the local gas distributions. The local atomic and molecular gas distributions are deduced by the NANTEN team from CO and H I observations. Our primary goal is to show how one can distinguish the emission mechanism(s) of the gamma rays (i.e., hadronic versus leptonic, or a mixture of the two) through information provided by their spatial distribution, spectra, and time variation. This work is the first attempt to quantitatively evaluate the capabilities of CTA to achieve various proposed scientific goals by observing this important cosmic particle accelerator.
Ahnen, M. L. ; Ansoldi, S. ; Antonelli, L. A. ; Antoranz, P. ; Babic, A. ; Banerjee, B. ; Bangale, P. ; de Almeida, U. Barres ; Barrio, J. A. ; Gonzalez, J. Becerra ; Bednarek, W. ; Bernardini, E. ; Berti, A. ; Biasuzzi, B. ; Biland, A. ; Blanch, O. ; Bonnefoy, S. ; Bonnoli, G. ; Borracci, F. ; Bretz, T. ; Buson, S. ; Carosi, A. ; Chatterjee, A. ; Clavero, R. ; Colin, P. ; Colombo, E. ; Contreras, J. L. ; Cortina, J. ; Covino, S. ; Da Vela, P. ; Dazzi, F. ; De Angelis, A. ; De Lotto, B. ; Wilhelmi, E. de Ona ; Di Pierro, F. ; Doert, M. ; Dominguez, A. ; Prester, D. Dominis ; Dorner, D. ; Doro, M. ; Einecke, S. ; Glawion, D. Eisenacher ; Elsaesser, D. ; Engelkemeier, M. ; Ramazani, V. Fallah ; Fernandez-Barral, A. ; Fidalgo, D. ; Fonseca, M. V. ; Font, L. ; Frantzen, K. ; Fruck, C. ; Galindo, D. ; Lopez, R. J. Garcia ; Garczarczyk, M. ; Terrats, D. Garrido ; Gaug, M. ; Giammaria, P. ; Godinovic, N. ; Gonzalez Munoz, A. ; Gora, D. ; Guberman, D. ; Hadasch, D. ; Hahn, A. ; Hanabata, Y. ; Hayashida, M. ; Herrera, J. ; Hose, J. ; Hrupec, D. ; Hughes, G. ; Idec, W. ; Kodani, K. ; Konno, Y. ; Kubo, H. ; Kushida, J. ; La Barbera, A. ; Lelas, D. ; Lindfors, E. ; Lombardi, S. ; Longo, F. ; Lopez, M. ; Lopez-Coto, R. ; Majumdar, P. ; Makariev, M. ; Mallot, K. ; Maneva, G. ; Manganaro, M. ; Mannheim, K. ; Maraschi, L. ; Marcote, B. ; Mariotti, M. ; Martinez, M. ; Mazin, D. ; Menzel, U. ; Miranda, J. M. ; Mirzoyan, R. ; Moralejo, A. ; Moretti, E. ; Nakajima, D. ; Neustroev, V. ; Niedzwiecki, A. ; Rosillo, M. Nievas ; Nilsson, K. ; Nishijima, K. ; Noda, K. ; Nogues, L. ; Overkemping, A. ; Paiano, S. ; Palacio, J. ; Palatiello, M. ; Paneque, D. ; Paoletti, R. ; Paredes, J. M. ; Paredes-Fortuny, X. ; Pedaletti, G. ; Peresano, M. ; Perri, L. ; Persic, M. ; Poutanen, J. ; Moroni, P. G. Prada ; Prandini, E. ; Puljak, I. ; Reichardt, I. ; Rhode, W. ; Ribo, M. ; Rico, J. ; Rodriguez Garcia, J. ; Saito, T. ; Satalecka, K. ; Schroder, S. ; Schultz, C. ; Schweizer, T. ; Shore, S. N. ; Sillanpaa, A. ; Sitarek, J. ; Snidaric, I. ; Sobczynska, D. ; Stamerra, A. ; Steinbring, T. ; Strzys, M. ; Suric, T. ; Takalo, L. ; Tavecchio, F. ; Temnikov, P. ; Terzic, T. ; Tescaro, D. ; Teshima, M. ; Thaele, J. ; Torres, D. F. ; Toyama, T. ; Treves, A. ; Vanzo, G. ; Verguilov, V. ; Vovk, I. ; Ward, J. E. ; Will, M. ; Wu, M. H. ; Zanin, R. ; Abeysekara, A. U. ; Archambault, S. ; Archer, A. ; Benbow, W. ; Bird, R. ; Buchovecky, M. ; Buckley, J. H. ; Bugaev, V. ; Connolly, M. P. ; Cui, W. ; Dickinson, H. J. ; Falcone, A. ; Feng, Q. ; Finley, J. P. ; Fleischhack, H. ; Flinders, A. ; Fortson, L. ; Gillanders, G. H. ; Griffin, S. ; Grube, J. ; Huetten, M. ; Hanna, D. ; Holder, J. ; Humensky, T. B. ; Kaaret, P. ; Kar, P. ; Kelley-Hoskins, N. ; Kertzman, M. ; Kieda, D. ; Krause, M. ; Krennrich, F. ; Lang, M. J. ; Maier, G. ; McCann, A. ; Moriarty, P. ; Mukherjee, R. ; Nieto, D. ; Ong, R. A. ; Otte, N. ; Park, N. ; Perkins, J. ; Pichel, A. ; Pohl, M. ; Popkow, A. ; Pueschel, Elisa ; Quinn, J. ; Ragan, K. ; Reynolds, P. T. ; Richards, G. T. ; Roache, E. ; Rovero, A. C. ; Rulten, C. ; Sadeh, I. ; Santander, M. ; Sembroski, G. H. ; Shahinyan, K. ; Telezhinsky, Igor O. ; Tucci, J. V. ; Tyler, J. ; Wakely, S. P. ; Weinstein, A. ; Wilcox, P. ; Wilhelm, Alina ; Williams, D. A. ; Zitzer, B. ; Razzaque, S. ; Villata, M. ; Raiteri, C. M. ; Aller, H. D. ; Aller, M. F. ; Larionov, V. M. ; Arkharov, A. A. ; Blinov, D. A. ; Efimova, N. V. ; Grishina, T. S. ; Hagen-Thorn, V. A. ; Kopatskaya, E. N. ; Larionova, L. V. ; Larionova, E. G. ; Morozova, D. A. ; Troitsky, I. S. ; Ligustri, R. ; Calcidese, P. ; Berdyugin, A. ; Kurtanidze, O. M. ; Nikolashvili, M. G. ; Kimeridze, G. N. ; Sigua, L. A. ; Kurtanidze, S. O. ; Chigladze, R. A. ; Chen, W. P. ; Koptelova, E. ; Sakamoto, T. ; Sadun, A. C. ; Moody, J. W. ; Pace, C. ; Pearson, R. ; Yatsu, Y. ; Mori, Y. ; Carraminyana, A. ; Carrasco, L. ; de la Fuente, E. ; Norris, J. P. ; Smith, P. S. ; Wehrle, A. ; Gurwell, M. A. ; Zook, A. ; Pagani, C. ; Perri, M. ; Capalbi, M. ; Cesarini, A. ; Krimm, H. A. ; Kovalev, Y. Y. ; Kovalev, Yu. A. ; Ros, E. ; Pushkarev, A. B. ; Lister, M. L. ; Sokolovsky, K. V. ; Kadler, M. ; Piner, G. ; Lahteenmaki, A. ; Tornikoski, M. ; Angelakis, E. ; Krichbaum, T. P. ; Nestoras, I. ; Fuhrmann, L. ; Zensus, J. A. ; Cassaro, P. ; Orlati, A. ; Maccaferri, G. ; Leto, P. ; Giroletti, M. ; Richards, J. L. ; Max-Moerbeck, W. ; Readhead, A. C. S.
Aims. We present an extensive study of the BL Lac object Mrk 501 based on a data set collected during the multi-instrument campaign spanning from 2009 March 15 to 2009 August 1, which includes, among other instruments, MAGIC, VERITAS, Whipple 10 m, and Fermi-LAT to cover the gamma-ray range from 0.1 GeV to 20 TeV; RXTE and Swift to cover wavelengths from UV to hard X-rays; and GASP-WEBT, which provides coverage of radio and optical wavelengths. Optical polarization measurements were provided for a fraction of the campaign by the Steward and St. Petersburg observatories. We evaluate the variability of the source and interband correlations, the gamma-ray flaring activity occurring in May 2009, and interpret the results within two synchrotron self-Compton (SSC) scenarios. Methods. The multiband variability observed during the full campaign is addressed in terms of the fractional variability, and the possible correlations are studied by calculating the discrete correlation function for each pair of energy bands where the significance was evaluated with dedicated Monte Carlo simulations. The space of SSC model parameters is probed following a dedicated grid-scan strategy, allowing for a wide range of models to be tested and offering a study of the degeneracy of model-to-data agreement in the individual model parameters, hence providing a less biased interpretation than the "single-curve SSC model adjustment" typically reported in the literature. Results. We find an increase in the fractional variability with energy, while no significant interband correlations of flux changes are found on the basis of the acquired data set. The SSC model grid-scan shows that the flaring activity around May 22 cannot be modeled adequately with a one-zone SSC scenario (using an electron energy distribution with two breaks), while it can be suitably described within a two (independent) zone SSC scenario. Here, one zone is responsible for the quiescent emission from the averaged 4.5-month observing period, while the other one, which is spatially separated from the first, dominates the flaring emission occurring at X-rays and very-high-energy (> 100 GeV, VHE) gamma-rays. The flaring activity from May 1, which coincides with a rotation of the electric vector polarization angle (EVPA), cannot be satisfactorily reproduced by either a one-zone or a two-independent-zone SSC model, yet this is partially affected by the lack of strictly simultaneous observations and the presence of large flux changes on sub-hour timescales (detected at VHE gamma rays). Conclusions. The higher variability in the VHE emission and lack of correlation with the X-ray emission indicate that, at least during the 4.5-month observing campaign in 2009, the highest energy (and most variable) electrons that are responsible for the VHE gamma rays do not make a dominant contribution to the similar to 1 keV emission. Alternatively, there could be a very variable component contributing to the VHE gamma-ray emission in addition to that coming from the SSC scenario. The studies with our dedicated SSC grid-scan show that there is some degeneracy in both the one-zone and the two-zone SSC scenarios probed, with several combinations of model parameters yielding a similar model-to-data agreement, and some parameters better constrained than others. The observed gamma-ray flaring activity, with the EVPA rotation coincident with the first gamma-ray flare, resembles those reported previously for low frequency peaked blazars, hence suggesting that there are many similarities in the flaring mechanisms of blazars with different jet properties.
De Angelis, A. ; Tatischeff, V. ; Tavani, M. ; Oberlack, U. ; Grenier, I. ; Hanloni, L. ; Walter, R. ; Argan, A. ; Von Ballmoos, P. ; Bulgarelli, A. ; Donnarumma, I. ; Hernanz, M. ; Kuvvetli, I. ; Pearce, M. ; Zdziarski, A. ; Aboudan, A. ; Ajello, M. ; Ambrosi, G. ; Bernard, D. ; Bernardini, E. ; Bonvicini, V. ; Brogna, A. ; Branchesi, M. ; Budtz-Jorgensen, C. ; Bykov, A. M. ; Campana, R. ; Cardillo, M. ; Coppi, P. ; De Martino, D. ; Diehl, R. ; Doro, M. ; Fioretti, V. ; Funk, S. ; Ghisellini, G. ; Grove, E. ; Hamadache, C. ; Hartmann, D. H. ; Hayashida, M. ; Isern, J. ; Kanbach, G. ; Kiener, J. ; Knodlseder, J. ; Labanti, C. ; Laurent, P. ; Limousin, O. ; Longo, F. ; Mannheim, K. ; Marisaldi, M. ; Martinez, M. ; Mazziotta, Mario Nicola ; McEnery, J. ; Mereghetti, S. ; Minervini, G. ; Moiseev, A. ; Morselli, A. ; Nakazawa, K. ; Orleanski, P. ; Paredes, J. M. ; Patricelli, B. ; Pevre, J. ; Piano, G. ; Pohl, Martin ; Ramarijaona, H. ; Rando, R. ; Reichardt, I. ; Roncadelli, M. ; Silva, R. ; Tavecchio, F. ; Thompson, D. J. ; Turolla, R. ; Ulyanov, A. ; Vacchi, A. ; Wu, X. ; Zoglauer, A.
e-ASTROGAM (‘enhanced ASTROGAM’) is a breakthrough Observatory space mission, with a detector composed by a Silicon tracker, a calorimeter, and an anticoincidence system, dedicated to the study of the non-thermal Universe in the photon energy range from 0.3 MeV to 3 GeV – the lower energy limit can be pushed to energies as low as 150 keV, albeit with rapidly degrading angular resolution, for the tracker, and to 30 keV for calorimetric detection. The mission is based on an advanced space-proven detector technology, with unprecedented sensitivity, angular and energy resolution, combined with polarimetric capability. Thanks to its performance in the MeV-GeV domain, substantially improving its predecessors, e-ASTROGAM will open a new window on the non-thermal Universe, making pioneering observations of the most powerful Galactic and extragalactic sources, elucidating the nature of their relativistic outflows and their effects on the surroundings. With a line sensitivity in the MeV energy range one to two orders of magnitude better than previous generation instruments, e-ASTROGAM will determine the origin of key isotopes fundamental for the understanding of supernova explosion and the chemical evolution of our Galaxy. The mission will provide unique data of significant interest to a broad astronomical community, complementary to powerful observatories such as LIGO-Virgo-GEO600-KAGRA, SKA, ALMA, E-ELT, TMT, LSST, JWST, Athena, CTA, IceCube, KM3NeT, and the promise of eLISA.
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