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Year of publication
Language
- English (75)
Is part of the Bibliography
- yes (75)
Keywords
- gamma rays: galaxies (20)
- gamma rays: general (17)
- BL Lacertae objects: general (12)
- galaxies: active (12)
- acceleration of particles (8)
- astroparticle physics (8)
- radiation mechanisms: non-thermal (7)
- binaries: general (6)
- X-rays: binaries (4)
- galaxies: jets (4)
Institute
Unprecedented study of the broadband emission of Mrk 421 during flaring activity in March 2010
(2015)
Aleksic, J. ; Ansoldi, S. ; Antonelli, L. A. ; Antoranz, P. ; Babic, A. ; Bangale, P. ; de Almeida, U. Barres ; Barrio, J. A. ; Gonzalez, J. Becerra ; Bednarek, W. ; Bernardini, E. ; Biasuzzi, B. ; Biland, A. ; Blanch Bigas, O. ; Boller, A. ; Bonnefoy, S. ; Bonnoli, G. ; Borracci, F. ; Bretz, T. ; Carmona, E. ; Carosi, A. ; Colin, P. ; Colombo, E. ; Contreras, J. L. ; Cortina, J. ; Covino, S. ; Da Vela, P. ; Dazzi, F. ; De Angelis, A. ; De Caneva, G. ; De Lotto, B. ; Wilhelmi, E. de Ona ; Mendez, C. Delgado ; Prester, Dijana Dominis ; Dorner, D. ; Doro, M. ; Einecke, S. ; Eisenacher, D. ; Elsaesser, D. ; Fonseca, M. V. ; Font, L. ; Frantzen, K. ; Fruck, C. ; Galindo, D. ; Lopez, R. J. Garcia ; Garczarczyk, M. ; Terrats, D. Garrido ; Gaug, M. ; Godinovic, N. ; Munoz, A. Gonzalez ; Gozzini, S. R. ; Hadasch, D. ; Hanabata, Y. ; Hayashida, M. ; Herrera, J. ; Hildebrand, D. ; Hose, J. ; Hrupec, D. ; Hughes, G. ; Idec, W. ; Kadenius, V. ; Kellermann, H. ; Knoetig, M. L. ; Kodani, K. ; Konno, Y. ; Krause, J. ; Kubo, H. ; Kushida, J. ; La Barbera, A. ; Lelas, D. ; Lewandowska, N. ; Lindfors, E. ; Lombardi, S. ; Lopez, M. ; Lopez-Coto, R. ; Lopez-Oramas, A. ; Lorenz, E. ; Lozano, I. ; Makariev, M. ; Mallot, K. ; Maneva, G. ; Mankuzhiyil, N. ; Mannheim, K. ; Maraschi, L. ; Marcote, B. ; Mariotti, M. ; Martinez, M. ; Mazin, D. ; Menzel, U. ; Miranda, J. M. ; Mirzoyan, R. ; Moralejo, A. ; Munar-Adrover, P. ; Nakajima, D. ; Niedzwiecki, A. ; Nilsson, K. ; Nishijima, K. ; Noda, K. ; Orito, R. ; Overkemping, A. ; Paiano, S. ; Palatiello, M. ; Paneque, D. ; Paoletti, R. ; Paredes, J. M. ; Paredes-Fortuny, X. ; Persic, M. ; Moroni, P. G. Prada ; Prandini, E. ; Puljak, I. ; Reinthal, R. ; Rhode, W. ; Ribo, M. ; Rico, J. ; Garcia, J. Rodriguez ; Rugamer, S. ; Saito, T. ; Saito, K. ; Satalecka, K. ; Scalzotto, V. ; Scapin, V. ; Schultz, C. ; Schweizer, T. ; Sun, S. ; Shore, S. N. ; Sillanpaa, A. ; Sitarek, J. ; Snidaric, I. ; Sobczynska, D. ; Spanier, F. ; Stamatescu, V. ; Stamerra, A. ; Steinbring, T. ; Steinke, B. ; Storz, J. ; Strzys, M. ; Takalo, L. ; Takami, H. ; Tavecchio, F. ; Temnikov, P. ; Terzic, T. ; Tescaro, D. ; Teshima, M. ; Thaele, J. ; Tibolla, O. ; Torres, D. F. ; Toyama, T. ; Treves, A. ; Uellenbeck, M. ; Vogler, P. ; Zanin, R. ; Archambault, S. ; Archer, A. ; Beilicke, M. ; Benbow, W. ; Berger, K. ; Bird, R. ; Biteau, Jonathan ; Buckley, J. H. ; Bugaev, V. ; Cerruti, M. ; Chen, Xiaoming ; Ciupik, L. ; Collins-Hughes, E. ; Cui, W. ; Eisch, J. D. ; Falcone, A. ; Feng, Q. ; Finley, J. P. ; Fortin, P. ; Fortson, L. ; Furniss, A. ; Galante, N. ; Gillanders, G. H. ; Griffin, S. ; Gyuk, G. ; Hakansson, Nils ; Holder, J. ; Johnson, C. A. ; Kaaret, P. ; Kar, P. ; Kertzman, M. ; Kieda, D. ; Lang, M. J. ; McArthur, S. ; McCann, A. ; Meagher, K. ; Millis, J. ; Moriarty, P. ; Ong, R. A. ; Otte, A. N. ; Perkins, J. S. ; Pichel, A. ; Pohl, Manuela ; Popkow, A. ; Prokoph, H. ; Pueschel, Elisa ; Ragan, K. ; Reyes, L. C. ; Reynolds, P. T. ; Richards, G. T. ; Roache, E. ; Rovero, A. C. ; Sembroski, G. H. ; Shahinyan, K. ; Staszak, D. ; Telezhinsky, Igor O. ; Tucci, J. V. ; Tyler, J. ; Varlotta, A. ; Wakely, S. P. ; Welsing, R. ; Wilhelm, Alina ; Williams, D. A. ; Buson, S. ; Finke, J. ; Villata, M. ; Raiteri, C. ; Aller, H. D. ; Aller, M. F. ; Cesarini, A. ; Chen, W. P. ; Gurwell, M. A. ; Jorstad, S. G. ; Kimeridze, G. N. ; Koptelova, E. ; Kurtanidze, O. M. ; Kurtanidze, S. O. ; Lahteenmaki, A. ; Larionov, V. M. ; Larionova, E. G. ; Lin, H. C. ; McBreen, B. ; Moody, J. W. ; Morozova, D. A. ; Marscher, A. P. ; Max-Moerbeck, W. ; Nikolashvili, M. G. ; Perri, M. ; Readhead, A. C. S. ; Richards, J. L. ; Ros, J. A. ; Sadun, A. C. ; Sakamoto, T. ; Sigua, L. A. ; Smith, P. S. ; Tornikoski, M. ; Troitsky, I. S. ; Wehrle, A. E. ; Jordan, B.
Context. Because of its proximity, Mrk 421 is one of the best sources on which to study the nature of BL Lac objects. Its proximity allows us to characterize its broadband spectral energy distribution (SED).
Aims. The goal is to better understand the mechanisms responsible for the broadband emission and the temporal evolution of Mrk 421. These mechanisms may also apply to more distant blazars that cannot be studied with the same level of detail.
Methods. A flare occurring in March 2010 was observed for 13 consecutive days (from MJD 55 265 to MJD 55 277) with unprecedented wavelength coverage from radio to very high energy (VHE; E > 100 GeV) gamma-rays with MAGIC, VERITAS, Whipple, Fermi-LAT, MAXI, RXTE, Swift, GASP-WEBT, and several optical and radio telescopes. We modeled the day-scale SEDs with one-zone and two-zone synchrotron self-Compton (SSC) models, investigated the physical parameters, and evaluated whether the observed broadband SED variability can be associated with variations in the relativistic particle population.
Results. The activity of Mrk 421 initially was high and then slowly decreased during the 13-day period. The flux variability was remarkable at the X-ray and VHE bands, but it was minor or not significant at the other bands. The variability in optical polarization was also minor. These observations revealed an almost linear correlation between the X-ray flux at the 2-10 keV band and the VHE gamma-ray flux above 200 GeV, consistent with the gamma-rays being produced by inverse-Compton scattering in the Klein-Nishina regime in the framework of SSC models. The one-zone SSC model can describe the SED of each day for the 13 consecutive days reasonably well, which once more shows the success of this standard theoretical scenario to describe the SEDs of VHE BL Lacs such as Mrk 421. This flaring activity is also very well described by a two-zone SSC model, where one zone is responsible for the quiescent emission, while the other smaller zone, which is spatially separated from the first, contributes to the daily variable emission occurring at X-rays and VHE gamma-rays. The second blob is assumed to have a smaller volume and a narrow electron energy distribution with 3 x 10(4) < gamma < 6 x 10(5), where. is the Lorentz factor of the electrons. Such a two-zone scenario would naturally lead to the correlated variability at the X-ray and VHE bands without variability at the optical/UV band, as well as to shorter timescales for the variability at the X-ray and VHE bands with respect to the variability at the other bands.
Conclusions. Both the one-zone and the two-zone SSC models can describe the daily SEDs via the variation of only four or five model parameters, under the hypothesis that the variability is associated mostly with the underlying particle population. This shows that the particle acceleration and cooling mechanism that produces the radiating particles might be the main mechanism responsible for the broadband SED variations during the flaring episodes in blazars. The two-zone SSC model provides a better agreement with the observed SED at the narrow peaks of the low-and high-energy bumps during the highest activity, although the reported one-zone SSC model could be further improved by varying the parameters related to the emitting region itself (delta, B and R), in addition to the parameters related to the particle population.
Aleksic, J. ; Ansoldi, S. ; Antonelli, L. A. ; Antoranz, P. ; Babic, A. ; Bangale, P. ; de Almeida, U. Barres ; Barrio, J. A. ; Gonzalez, J. Becerra ; Bednarek, W. ; Berger, K. ; Bernardini, E. ; Bilandli, A. ; Bianch, O. ; Bock, R. K. ; Bonnefoy, S. ; Bonnoli, G. ; Borracci, F. ; Bretz, T. ; Carmona, E. ; Carosi, A. ; Fidalgo, D. Carreto ; Colin, P. ; Colombo, E. ; Contreras, J. L. ; Cortina, J. ; Covino, S. ; Da Vela, P. ; Dazzi, F. ; De Angelis, A. ; De Caneva, G. ; De Lotto, B. ; Delgado Mendez, C. ; Doert, M. ; Dominguez, A. ; Prester, Dijana Dominis ; Dorner, D. ; Doro, M. ; Einecke, S. ; Eisenacher, D. ; Elsaesser, D. ; Farina, E. ; Ferenc, D. ; Fonseca, M. V. ; Font, L. ; Frantzen, K. ; Fruck, C. ; Garcia Lopez, R. J. ; Garczarczyki, M. ; Garrido Terrats, D. ; Gaug, M. ; Giavitto, G. ; Godinovic, N. ; Gonzalez Munoz, A. ; Gozzini, S. R. ; Hadamek, A. ; Hadasch, D. ; Herrero, A. ; Hildebrand, D. ; Hose, J. ; Hrupec, D. ; Idec, W. ; Kadenius, V. ; Kellermann, H. ; Knoetig, M. L. ; Krause, J. ; Kushida, J. ; La Barbera, A. ; Lelas, D. ; Lewandowska, N. ; Lindfors, E. ; Longo, F. ; Lombardi, S. ; Lopez, M. ; Lopez-Coto, R. ; Lopez-Oramas, A. ; Lorenz, E. ; Lozano, I. ; Makariev, M. ; Mallot, K. ; Maneva, G. ; Mankuzhiyil, N. ; Mannheim, K. ; Maraschi, L. ; Marcote, B. ; Mariotti, M. ; Martinez, M. ; Mazin, D. ; Menzel, U. ; Meucci, M. ; Miranda, J. M. ; Mirzoyan, R. ; Moralejo, A. ; Munar-Adrover, P. ; Nakajima, D. ; Niedzwiecki, A. ; Nilsson, K. ; Nowak, N. ; Orito, R. ; Overkemping, A. ; Paiano, S. ; Palatiello, M. ; Paneque, D. ; Paoletti, R. ; Paredes, J. M. ; Paredes-Fortuny, X. ; Partini, S. ; Persic, M. ; Prada, F. ; Moroni, P. G. Prada ; Prandini, E. ; Preziuso, S. ; Puljak, I. ; Reinthal, R. ; Rhode, W. ; Ribo, M. ; Rico, J. ; Garcia, J. Rodriguez ; Ruegamer, S. ; Saggion, A. ; Saito, K. ; Salvati, M. ; Satalecka, K. ; Scalzotto, V. ; Scapin, V. ; Schuliz, C. ; Schweizer, T. ; Shore, S. N. ; Sillanpaa, A. ; Sitarek, J. ; Snidaric, I. ; Sobczynska, D. ; Spanier, F. ; Stamatescu, V. ; Stamerra, A. ; Steinbring, T. ; Storz, J. ; Sun, S. ; Suric, T. ; Takalo, L. ; Tavecchio, F. ; Temnikov, P. ; Terzic, T. ; Tescaro, D. ; Teshima, M. ; Thaele, J. ; Tibolla, O. ; Torres, D. F. ; Toyama, T. ; Treves, A. ; Uellenbeck, M. ; Vogler, P. ; Wagner, R. M. ; Zandanel, F. ; Zanin, R. ; Archambault, S. ; Behera, B. ; Beilicke, M. ; Benbow, W. ; Bird, R. ; Buckley, J. H. ; Bugaev, V. ; Cerruti, M. ; Chen, X. ; Ciupik, L. ; Collins-Hughes, E. ; Cui, W. ; Dumm, J. ; Eisch, J. D. ; Falcone, A. ; Federici, S. ; Feng, Q. ; Finley, J. P. ; Fleischhack, H. ; Fortin, P. ; Fortson, L. ; Furniss, A. ; Griffin, S. ; Griffiths, S. T. ; Grube, J. ; Gyuk, G. ; Hanna, D. ; Holder, J. ; Hughes, G. ; Humensky, T. B. ; Johnson, C. A. ; Kaaret, P. ; Kertzman, M. ; Khassen, Y. ; Kieda, D. ; Krawczynski, H. ; Krennrich, F. ; Kumar, S. ; Lang, M. J. ; Maier, G. ; McArthur, S. ; Meagher, K. ; Moriarty, P. ; Mukherjee, R. ; Ong, R. A. ; Otte, A. N. ; Park, N. ; Pichel, A. ; Pohl, M. ; Popkow, A. ; Prokoph, H. ; Quinn, M. J. ; Ragan, K. ; Rajotte, J. ; Reynolds, P. T. ; Richards, G. T. ; Roache, E. ; Rovero, A. C. ; Sembroski, G. H. ; Shahinyan, K. ; Staszak, D. ; Telezhinsky, Igor O. ; Theiling, M. ; Tucci, J. V. ; Tyler, J. ; Varlotta, A. ; Wakely, S. P. ; Weekes, T. C. ; Weinstein, A. ; Welsing, R. ; Wilhelm, Alina ; Williams, D. A. ; Zitzer, B. ; Villata, M. ; Raiteri, C. ; Aller, H. D. ; Aller, M. F. ; Chen, W. P. ; Jordan, B. ; Koptelova, E. ; Kurtanidze, O. M. ; Lahteenmaki, A. ; McBreen, B. ; Larionov, V. M. ; Lin, C. S. ; Nikolashvili, M. G. ; Angelakis, E. ; Capalbi, M. ; Carraminana, A. ; Carrasco, L. ; Cassaro, P. ; Cesarini, A. ; Fuhrmann, L. ; Giroletti, M. ; Hovatta, T. ; Krichbaum, T. P. ; Krimm, H. A. ; Max-Moerbeck, W. ; Moody, J. W. ; Maccaferri, G. ; Mori, Y. ; Nestoras, I. ; Orlati, A. ; Pace, C. ; Pearson, R. ; Perri, M. ; Readhead, A. C. S. ; Richards, J. L. ; Sadun, A. C. ; Sakamoto, T. ; Tammi, J. ; Tornikoski, M. ; Yatsu, Y. ; Zook, A.
Aims. We perform an extensive characterization of the broadband emission of Mrk 421, as well as its temporal evolution, during the non-flaring (low) state. The high brightness and nearby location (z = 0.031) of Mrk 421 make it an excellent laboratory to study blazar emission. The goal is to learn about the physical processes responsible for the typical emission of Mrk 421, which might also be extended to other blazars that are located farther away and hence are more difficult to study.
Methods. We performed a 4.5-month multi-instrument campaign on Mrk 421 between January 2009 and June 2009, which included VLBA, F-GAMMA, GASP-WEBT, Swift, RXTE, Fermi-LAT, MAGIC, and Whipple, among other instruments and collaborations. This extensive radio to very-high-energy (VHE; E > 100 GeV) gamma-ray dataset provides excellent temporal and energy coverage, which allows detailed studies of the evolution of the broadband spectral energy distribution.
Results. Mrk421 was found in its typical (non-flaring) activity state, with a VHE flux of about half that of the Crab Nebula, yet the light curves show significant variability at all wavelengths, the highest variability being in the X-rays. We determined the power spectral densities (PSD) at most wavelengths and found that all PSDs can be described by power-laws without a break, and with indices consistent with pink/red-noise behavior. We observed a harder-when-brighter behavior in the X-ray spectra and measured a positive correlation between VHE and X-ray fluxes with zero time lag. Such characteristics have been reported many times during flaring activity, but here they are reported for the first time in the non-flaring state. We also observed an overall anti-correlation between optical /UV and X-rays extending over the duration of the campaign.
Conclusions. The harder-when-brighter behavior in the X-ray spectra and the measured positive X-ray/VHE correlation during the 2009 multiwavelength campaign suggests that the physical processes dominating the emission during non-flaring states have similarities with those occurring during flaring activity. In particular, this observation supports leptonic scenarios as being responsible for the emission of Mrk 421 during non-flaring activity. Such a temporally extended X-ray /VHE correlation is not driven by any single flaring event, and hence is difficult to explain within the standard hadronic scenarios. The highest variability is observed in the X-ray band, which, within the one-zone synchrotron self-Compton scenario, indicates that the electron energy distribution is most variable at the highest energies.
Aleksic, J. ; Ansoldi, S. ; Antonelli, L. A. ; Antoranz, P. ; Babic, A. ; Bangale, P. ; de Almeida, U. Barres ; Barrio, J. A. ; Becerra Gonzalez, J. ; Bednarek, W. ; Berger, K. ; Bernardini, E. ; Biland, A. ; Blanch Bigas, O. ; Bock, R. K. ; Bonnefoy, S. ; Bonnoli, G. ; Borracci, F. ; Bretz, T. ; Carmona, E. ; Carosi, A. ; Fidalgo, D. Carreto ; Colin, P. ; Colombo, E. ; Contreras, J. L. ; Cortina, J. ; Covino, S. ; Da Vela, P. ; Dazzi, F. ; De Angelis, A. ; De Caneva, G. ; De Lotto, B. ; Delgado Mendez, C. ; Doert, M. ; Dominguez, A. ; Prester, Dijana Dominis ; Dorner, D. ; Doro, M. ; Einecke, S. ; Eisenacher, D. ; Elsaesser, D. ; Farina, E. ; Ferenc, D. ; Fonseca, M. V. ; Font, L. ; Frantzen, K. ; Fruck, C. ; Garcia Lopez, R. J. ; Garczarczyk, M. ; Garrido Terrats, D. ; Gaug, M. ; Giavitto, G. ; Godinovic, N. ; Gonzalez Munoz, A. ; Gozzini, S. R. ; Hadamek, A. ; Hadasch, D. ; Herrero, A. ; Hildebrand, D. ; Hose, J. ; Hrupec, D. ; Idec, W. ; Kadenius, V. ; Kellermann, H. ; Knoetig, M. L. ; Krause, J. ; Kushida, J. ; La Barbera, A. ; Lelas, D. ; Lewandowska, N. ; Lindfors, E. ; Lombardi, S. ; Lopez, M. ; Lopez-Coto, R. ; Lopez-Oramas, A. ; Lorenz, E. ; Lozano, I. ; Makariev, M. ; Mallot, K. ; Maneva, G. ; Mankuzhiyil, N. ; Mannheim, K. ; Maraschi, L. ; Marcote, B. ; Mariotti, M. ; Martinez, M. ; Mazin, D. ; Menzel, U. ; Meucci, M. ; Miranda, J. M. ; Mirzoyan, R. ; Moralejo, A. ; Munar-Adrover, P. ; Nakajima, D. ; Niedzwiecki, A. ; Nilsson, K. ; Nowak, N. ; Orito, R. ; Overkemping, A. ; Paiano, S. ; Palatiello, M. ; Paneque, D. ; Paoletti, R. ; Paredes, J. M. ; Paredes-Fortuny, X. ; Partini, S. ; Persic, M. ; Prada, F. ; Moroni, P. G. Prada ; Prandini, E. ; Preziuso, S. ; Puljak, I. ; Reinthal, R. ; Rhode, W. ; Ribo, M. ; Rico, J. ; Garcia, J. Rodriguez ; Ruegamer, S. ; Saggion, A. ; Saito, T. ; Saito, K. ; Salvati, M. ; Satalecka, K. ; Scalzotto, V. ; Scapin, V. ; Schultz, C. ; Schweizer, T. ; Shore, S. N. ; Sillanpaa, A. ; Sitarek, J. ; Snidaric, I. ; Sobczynska, D. ; Spanier, F. ; Stamatescu, V. ; Stamerra, A. ; Steinbring, T. ; Storz, J. ; Sun, S. ; Suric, T. ; Takalo, L. ; Tavecchio, F. ; Temnikov, P. ; Terzic, T. ; Tescaro, D. ; Teshima, M. ; Thaele, J. ; Tibolla, O. ; Torres, D. F. ; Toyama, T. ; Treves, A. ; Uellenbeck, M. ; Vogler, P. ; Wagner, R. M. ; Zandanel, F. ; Zanin, R. ; Behera, B. ; Beilicke, M. ; Benbow, W. ; Berger, K. ; Bird, R. ; Bouvier, A. ; Bugaev, V. ; Cerruti, M. ; Chen, Xuhui ; Ciupik, L. ; Collins-Hughes, E. ; Cui, W. ; Duke, C. ; Dumm, J. ; Falcone, A. ; Federici, Simone ; Feng, Q. ; Finley, J. P. ; Fortson, L. ; Furniss, A. ; Galante, N. ; Gillanders, G. H. ; Griffin, S. ; Griffiths, S. T. ; Grube, J. ; Gyuk, G. ; Hanna, D. ; Holder, J. ; Johnson, C. A. ; Kaaret, P. ; Kertzman, M. ; Kieda, D. ; Krawczynski, H. ; Lang, M. J. ; Madhavan, A. S. ; Maier, G. ; Majumdar, P. ; Meagher, K. ; Moriarty, P. ; Mukherjee, R. ; Nieto, D. ; Ong, R. A. ; Otte, A. N. ; Pichel, A. ; Pohl, Manula ; Popkow, A. ; Prokoph, H. ; Quinn, J. ; Rajotte, J. ; Ratliff, G. ; Reyes, L. C. ; Reynolds, P. T. ; Richards, G. T. ; Roache, E. ; Sembroski, G. H. ; Shahinyan, K. ; Sheidaei, F. ; Smith, A. W. ; Staszak, D. ; Telezhinsky, Igor O. ; Theiling, M. ; Tyler, J. ; Varlotta, A. ; Vincent, S. ; Wakely, S. P. ; Weekes, T. C. ; Welsing, R. ; Williams, D. A. ; Zajczyk, A. ; Zitzer, B. ; Villata, M. ; Raiteri, C. M. ; Ajello, M. ; Perri, M. ; Aller, H. D. ; Aller, M. F. ; Larionov, V. M. ; Efimova, N. V. ; Konstantinova, T. S. ; Kopatskaya, E. N. ; Chen, W. P. ; Koptelova, E. ; Hsiao, H. Y. ; Kurtanidze, O. M. ; Nikolashvili, M. G. ; Kimeridze, G. N. ; Jordan, B. ; Leto, Paolo ; Buemi, C. S. ; Trigilio, C. ; Umana, G. ; Lahteenmaki, A. ; Nieppola, E. ; Tornikoski, M. ; Sainio, J. ; Kadenius, V. ; Giroletti, M. ; Cesarini, A. ; Fuhrmann, L. ; Kovalev, Yu. A. ; Kovalev, Y. Y.
Context. Blazars are variable sources on various timescales over a broad energy range spanning from radio to very high energy (>100 GeV, hereafter VHE). Mrk 501 is one of the brightest blazars at TeV energies and has been extensively studied since its first VHE detection in 1996. However, most of the gamma-ray studies performed on Mrk 501 during the past years relate to flaring activity, when the source detection and characterization with the available gamma-ray instrumentation was easier to perform.
Aims. Our goal is to characterize the source gamma-ray emission in detail, together with the radio-to-X-ray emission, during the non-flaring (low) activity, which is less often studied than the occasional flaring (high) activity.
Methods. We organized a multiwavelength (MW) campaign on Mrk 501 between March and May 2008. This multi-instrument effort included the most sensitive VHE gamma-ray instruments in the northern hemisphere, namely the imaging atmospheric Cherenkov telescopes MAGIC and VERITAS, as well as Swift, RXTE, the F-GAMMA, GASP-WEBT, and other collaborations and instruments. This provided extensive energy and temporal coverage of Mrk 501 throughout the entire campaign.
Results. Mrk 501 was found to be in a low state of activity during the campaign, with a VHE flux in the range of 10%-20% of the Crab nebula flux. Nevertheless, significant flux variations were detected with various instruments, with a trend of increasing variability with energy and a tentative correlation between the X-ray and VHE fluxes. The broadband spectral energy distribution during the two different emission states of the campaign can be adequately described within the homogeneous one-zone synchrotron self-Compton model, with the (slightly) higher state described by an increase in the electron number density.
Conclusions. The one-zone SSC model can adequately describe the broadband spectral energy distribution of the source during the two months covered by the MW campaign. This agrees with previous studies of the broadband emission of this source during flaring and non-flaring states. We report for the first time a tentative X-ray-to-VHE correlation during such a low VHE activity. Although marginally significant, this positive correlation between X-ray and VHE, which has been reported many times during flaring activity, suggests that the mechanisms that dominate the X-ray/VHE emission during non-flaring-activity are not substantially different from those that are responsible for the emission during flaring activity.
Ahnen, M. L. ; Ansoldi, S. ; Antonelli, L. A. ; Arcaro, C. ; Babic, A. ; Banerjee, B. ; Bangale, P. ; Barres de Almeida, U. ; Barrio, J. A. ; Gonzalez, J. Becerra ; Bednarek, W. ; Bernardini, E. ; Berti, A. ; Bhattacharyya, W. ; Blanch, O. ; Bonnoli, G. ; Carosi, R. ; Carosi, A. ; Chatterjee, A. ; Colak, S. M. ; Colin, P. ; Colombo, E. ; Contreras, J. L. ; Cortina, J. ; Covino, S. ; Cumani, P. ; Da Vela, P. ; Dazzi, F. ; De Angelis, A. ; De Lotto, B. ; Delfino, M. ; Delgado, Jose Miguel Martins ; Di Pierro, F. ; Doert, M. ; Dominguez, A. ; Prester, D. Dominis ; Doro, M. ; Glawion, D. Eisenacher ; Engelkemeier, M. ; Ramazani, V. Fallah ; Fernandez-Barral, A. ; Fidalgo, D. ; Fonseca, M. V. ; Font, L. ; Fruck, C. ; Galindo, D. ; Lopez, R. J. Garcia ; Garczarczyk, M. ; Gaug, M. ; Giammaria, P. ; Godinovic, N. ; Gora, D. ; Guberman, D. ; Hadasch, D. ; Hahn, A. ; Hassan, T. ; Hayashida, M. ; Herrera, J. ; Hose, J. ; Hrupec, D. ; Ishio, K. ; Konno, Y. ; Kubo, H. ; Kushida, J. ; Kuvezdic, D. ; Lelas, D. ; Lindfors, E. ; Lombardi, S. ; Longo, F. ; Lopez, M. ; Maggio, C. ; Majumdar, P. ; Makariev, M. ; Maneva, G. ; Manganaro, M. ; Maraschi, L. ; Mariotti, M. ; Martinez, M. ; Mazin, D. ; Menzel, U. ; Minev, M. ; Miranda, J. M. ; Mirzoyan, R. ; Moralejo, A. ; Moreno, V. ; Moretti, E. ; Nagayoshi, T. ; Neustroev, V. ; Niedzwiecki, A. ; Nievas Rosillo, M. ; Nigro, C. ; Nilsson, K. ; Ninci, D. ; Nishijima, K. ; Noda, K. ; Nogues, L. ; Paiano, S. ; Palacio, J. ; Paneque, D. ; Paoletti, R. ; Paredes, J. M. ; Pedaletti, G. ; Peresano, M. ; Perri, L. ; Persic, M. ; Moroni, P. G. Prada ; Prandini, E. ; Puljak, I. ; Garcia, J. R. ; Reichardt, I. ; Ribo, M. ; Rico, J. ; Righi, C. ; Rugliancich, A. ; Saito, T. ; Satalecka, K. ; Schroeder, S. ; Schweizer, T. ; Shore, S. N. ; Sitarek, J. ; Snidaric, I. ; Sobczynska, D. ; Stamerra, A. ; Strzys, M. ; Suric, T. ; Takalo, L. ; Tavecchio, F. ; Temnikov, P. ; Terzic, T. ; Teshima, M. ; Torres-Alba, N. ; Treves, A. ; Tsujimoto, S. ; Vanzo, G. ; Vazquez Acosta, M. ; Vovk, I. ; Ward, J. E. ; Will, M. ; Zaric, D. ; Arbet-Engels, A. ; Baack, D. ; Balbo, M. ; Biland, A. ; Blank, M. ; Bretz, T. ; Bruegge, K. ; Bulinski, M. ; Buss, J. ; Dmytriiev, A. ; Dorner, D. ; Einecke, S. ; Elsaesser, D. ; Herbst, T. ; Hildebrand, D. ; Kortmann, L. ; Linhoff, L. ; Mahlke, M. ; Mannheim, K. ; Mueller, S. A. ; Neise, D. ; Neronov, A. ; Noethe, M. ; Oberkirch, J. ; Paravac, A. ; Rhode, W. ; Schleicher, B. ; Schulz, F. ; Sedlaczek, K. ; Shukla, A. ; Sliusar, V. ; Walter, R. ; Archer, A. ; Benbow, W. ; Bird, R. ; Brose, Robert ; Buckley, J. H. ; Bugaev, V. ; Christiansen, J. L. ; Cui, W. ; Daniel, M. K. ; Falcone, A. ; Feng, Q. ; Finley, J. P. ; Gillanders, G. H. ; Gueta, O. ; Hanna, D. ; Hervet, O. ; Holder, J. ; Hughes, G. ; Huetten, M. ; Humensky, T. B. ; Johnson, C. A. ; Kaaret, P. ; Kar, P. ; Kelley-Hoskins, N. ; Kertzman, M. ; Kieda, D. ; Krause, M. ; Krennrich, F. ; Kumar, S. ; Lang, M. J. ; Lin, T. T. Y. ; Maier, G. ; McArthur, S. ; Moriarty, P. ; Mukherjee, R. ; Ong, R. A. ; Otte, A. N. ; Park, N. ; Petrashyk, A. ; Pichel, A. ; Pohl, Martin ; 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. ; Sushch, Iurii ; Tyler, J. ; Wakely, S. P. ; Weinstein, A. ; Wells, R. M. ; Wilcox, P. ; Wilhel, A. ; Williams, D. A. ; Williamson, T. J. ; Zitzer, B. ; Perri, M. ; Verrecchia, F. ; Leto, C. ; Villata, M. ; Raiteri, C. M. ; Jorstad, S. G. ; Larionov, V. M. ; Blinov, D. A. ; Grishina, T. S. ; Kopatskaya, E. N. ; Larionova, E. G. ; Nikiforova, A. A. ; Morozova, D. A. ; Troitskaya, Yu. V. ; Troitsky, I. S. ; Kurtanidze, O. M. ; Nikolashvili, M. G. ; Kurtanidze, S. O. ; Kimeridze, G. N. ; Chigladze, R. A. ; Strigachev, A. ; Sadun, A. C.
Aims. We aim to characterize the multiwavelength emission from Markarian 501 (Mrk 501), quantify the energy-dependent variability, study the potential multiband correlations, and describe the temporal evolution of the broadband emission within leptonic theoretical scenarios. Methods. We organized a multiwavelength campaign to take place between March and July of 2012. Excellent temporal coverage was obtained with more than 25 instruments, including the MAGIC, FACT and VERITAS Cherenkov telescopes, the instruments on board the Swift and Fermi spacecraft, and the telescopes operated by the GASP-WEBT collaboration. Results. Mrk 501 showed a very high energy (VHE) gamma-ray flux above 0.2 TeV of similar to 0.5 times the Crab Nebula flux (CU) for most of the campaign. The highest activity occurred on 2012 June 9, when the VHE flux was similar to 3 CU, and the peak of the high-energy spectral component was found to be at similar to 2 TeV. Both the X-ray and VHE gamma-ray spectral slopes were measured to be extremely hard, with spectral indices <2 during most of the observing campaign, regardless of the X-ray and VHE flux. This study reports the hardest Mrk 501 VHE spectra measured to date. The fractional variability was found to increase with energy, with the highest variability occurring at VHE. Using the complete data set, we found correlation between the X-ray and VHE bands; however, if the June 9 flare is excluded, the correlation disappears (significance <3 sigma) despite the existence of substantial variability in the X-ray and VHE bands throughout the campaign. Conclusions. The unprecedentedly hard X-ray and VHE spectra measured imply that their low- and high-energy components peaked above 5 keV and 0.5 TeV, respectively, during a large fraction of the observing campaign, and hence that Mrk 501 behaved like an extreme high-frequency-peaked blazar (EHBL) throughout the 2012 observing season. This suggests that being an EHBL may not be a permanent characteristic of a blazar, but rather a state which may change over time. The data set acquired shows that the broadband spectral energy distribution (SED) of Mrk 501, and its transient evolution, is very complex, requiring, within the framework of synchrotron self-Compton (SSC) models, various emission regions for a satisfactory description. Nevertheless the one-zone SSC scenario can successfully describe the segments of the SED where most energy is emitted, with a significant correlation between the electron energy density and the VHE gamma-ray activity, suggesting that most of the variability may be explained by the injection of high-energy electrons. The one-zone SSC scenario used reproduces the behavior seen between the measured X-ray and VHE gamma-ray fluxes, and predicts that the correlation becomes stronger with increasing energy of the X-rays.
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.
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Ground-based gamma-ray astronomy has had a major breakthrough with the impressive results obtained using systems of imaging atmospheric Cherenkov telescopes. Ground-based gamma-ray astronomy has a huge potential in astrophysics, particle physics and cosmology. CTA is an international initiative to build the next generation instrument, with a factor of 5-10 improvement in sensitivity in the 100 GeV-10 TeV range and the extension to energies well below 100 GeV and above 100 TeV. CTA will consist of two arrays (one in the north, one in the south) for full sky coverage and will be operated as open observatory. The design of CTA is based on currently available technology. This document reports on the status and presents the major design concepts of CTA.
Introducing the CTA concept
(2013)
Acharya, B. S. ; Actis, M. ; Aghajani, T. ; Agnetta, G. ; Aguilar, J. ; Aharonian, Felix A. ; Ajello, M. ; Akhperjanian, A. G. ; Alcubierre, M. ; Aleksic, J. ; Alfaro, R. ; Aliu, E. ; Allafort, A. J. ; Allan, D. ; Allekotte, I. ; Amato, E. ; Anderson, J. ; Angüner, Ekrem Oǧuzhan ; Antonelli, L. A. ; Antoranz, P. ; Aravantinos, A. ; Arlen, T. ; Armstrong, T. ; Arnaldi, H. ; Arrabito, L. ; Asano, K. ; Ashton, T. ; Asorey, H. G. ; Awane, Y. ; Baba, H. ; Babic, A. ; Baby, N. ; Baehr, J. ; Bais, A. ; Baixeras, C. ; Bajtlik, S. ; Balbo, M. ; Balis, D. ; Balkowski, C. ; Bamba, A. ; Bandiera, R. ; Barber, A. ; Barbier, C. ; Barcelo, M. ; Barnacka, Anna ; Barnstedt, Jürgen ; Barres de Almeida, U. ; Barrio, J. A. ; Basili, A. ; Basso, S. ; Bastieri, D. ; Bauer, C. ; Baushev, Anton N. ; Becerra Gonzalez, J. ; Becherini, Yvonne ; Bechtol, K. C. ; Tjus, J. Becker ; Beckmann, Volker ; Bednarek, W. ; Behera, B. ; Belluso, M. ; Benbow, W. ; Berdugo, J. ; Berger, K. ; Bernard, F. ; Bernardino, T. ; Bernlöhr, K. ; Bhat, N. ; Bhattacharyya, S. ; Bigongiari, C. ; Biland, A. ; Billotta, S. ; Bird, T. ; Birsin, E. ; Bissaldi, E. ; Biteau, Jonathan ; Bitossi, M. ; Blake, S. ; Blanch Bigas, O. ; Blasi, P. ; Bobkov, A. A. ; Boccone, V. ; Boettcher, Markus ; Bogacz, L. ; Bogart, J. ; Bogdan, M. ; Boisson, Catherine ; Boix Gargallo, J. ; Bolmont, J. ; Bonanno, G. ; Bonardi, A. ; Bonev, T. ; Bonifacio, P. ; Bonnoli, G. ; Bordas, Pol ; Borgland, A. W. ; Borkowski, Janett ; Bose, R. ; Botner, O. ; Bottani, A. ; Bouchet, L. ; Bourgeat, M. ; Boutonnet, C. ; Bouvier, A. ; Brau-Nogue, S. ; Braun, I. ; Bretz, T. ; Briggs, M. S. ; Bringmann, T. ; Brook, P. ; Brun, Pierre ; Brunetti, L. ; Buanes, T. ; Buckley, J. H. ; Buehler, R. ; Bugaev, V. ; Bulgarelli, A. ; Bulik, Tomasz ; Busetto, G. ; Buson, S. ; Byrum, K. ; Cailles, M. ; Cameron, R. A. ; Camprecios, J. ; Canestrari, R. ; Cantu, S. ; Capalbi, M. ; Caraveo, P. A. ; Carmona, E. ; Carosi, A. ; Carr, John ; Carton, P. H. ; Casanova, Sabrina ; Casiraghi, M. ; Catalano, O. ; Cavazzani, S. ; Cazaux, S. ; Cerruti, M. ; Chabanne, E. ; Chadwick, Paula M. ; Champion, C. ; Chen, Andrew ; Chiang, J. ; Chiappetti, L. ; Chikawa, M. ; Chitnis, V. R. ; Chollet, F. ; Chudoba, J. ; Cieslar, M. ; Cillis, A. N. ; Cohen-Tanugi, J. ; Colafrancesco, Sergio ; Colin, P. ; Calome, J. ; Colonges, S. ; Compin, M. ; Conconi, P. ; Conforti, V. ; Connaughton, V. ; Conrad, Jan ; Contreras, J. L. ; Coppi, P. ; Corona, P. ; Corti, D. ; Cortina, J. ; Cossio, L. ; Costantini, H. ; Cotter, G. ; Courty, B. ; Couturier, S. ; Covino, S. ; Crimi, G. ; Criswell, S. J. ; Croston, J. ; Cusumano, G. ; Dafonseca, M. ; Dale, O. ; Daniel, M. ; Darling, J. ; Davids, I. ; Dazzi, F. ; De Angelis, A. ; De Caprio, V. ; De Frondat, F. ; de Gouveia Dal Pino, E. M. ; de la Calle, I. ; De La Vega, G. A. ; Lopez, R. de los Reyes ; De Lotto, B. ; De Luca, A. ; de Mello Neto, J. R. T. ; de Naurois, M. ; de Oliveira, Y. ; de Ona Wilhelmi, E. ; de Souza, V. ; Decerprit, G. ; Decock, G. ; Deil, C. ; Delagnes, E. ; Deleglise, G. ; Delgado, C. ; Della Volpe, D. ; Demange, P. ; Depaola, G. ; Dettlaff, A. ; Di Paola, A. ; Di Pierro, F. ; Diaz, C. ; Dick, J. ; Dickherber, R. ; Dickinson, H. ; Diez-Blanco, V. ; Digel, S. ; Dimitrov, D. ; Disset, G. ; Djannati-Ataï, A. ; Doert, M. ; Dohmke, M. ; Domainko, W. ; Prester, Dijana Dominis ; Donat, A. ; Dorner, D. ; Doro, M. ; Dournaux, J-L. ; Drake, G. ; Dravins, D. ; Drury, L. ; Dubois, F. ; Dubois, R. ; Dubus, G. ; Dufour, C. ; Dumas, D. ; Dumm, J. ; Durand, D. ; Dyks, J. ; Dyrda, M. ; Ebr, J. ; Edy, E. ; Egberts, Kathrin ; Eger, P. ; Einecke, S. ; Eleftheriadis, C. ; Elles, S. ; Emmanoulopoulos, D. ; Engelhaupt, D. ; Enomoto, R. ; Ernenwein, J-P ; Errando, M. ; Etchegoyen, A. ; Evans, P. ; Falcone, A. ; Fantinel, D. ; Farakos, K. ; Farnier, C. ; Fasola, G. ; Favill, B. ; Fede, E. ; Federici, S. ; Fegan, S. ; Feinstein, F. ; Ferenc, D. ; Ferrando, P. ; Fesquet, M. ; Fiasson, A. ; Fillin-Martino, E. ; Fink, D. ; Finley, C. ; Finley, J. P. ; Fiorini, M. ; Firpo Curcoll, R. ; Flores, H. ; Florin, D. ; Focke, W. ; Foehr, C. ; Fokitis, E. ; Font, L. ; Fontaine, G. ; Fornasa, M. ; Foerster, A. ; Fortson, L. ; Fouque, N. ; Franckowiak, A. ; Fransson, C. ; Fraser, G. ; Frei, R. ; Albuquerque, I. F. M. ; Fresnillo, L. ; Fruck, C. ; Fujita, Y. ; Fukazawa, Y. ; Fukui, Y. ; Funk, S. ; Gaebele, W. ; Gabici, S. ; Gabriele, R. ; Gadola, A. ; Galante, N. ; Gall, D. ; Gallant, Y. ; Gamez-Garcia, J. ; Garcia, B. ; Garcia Lopez, R. ; Gardiol, D. ; Garrido, D. ; Garrido, L. ; Gascon, D. ; Gaug, M. ; Gaweda, J. ; Gebremedhin, L. ; Geffroy, N. ; Gerard, L. ; Ghedina, A. ; Ghigo, M. ; Giannakaki, E. ; Gianotti, F. ; Giarrusso, S. ; Giavitto, G. ; Giebels, B. ; Gika, V. ; Giommi, P. ; Girard, N. ; Giro, E. ; Giuliani, A. ; Glanzman, T. ; Glicenstein, J. -F. ; Godinovic, N. ; Golev, V. ; Gomez Berisso, M. ; Gomez-Ortega, J. ; Gonzalez, M. M. ; Gonzalez, A. ; Gonzalez, F. ; Gonzalez Munoz, A. ; Gothe, K. S. ; Gougerot, M. ; Graciani, R. ; Grandi, P. ; Granena, F. ; Granot, J. ; Grasseau, G. ; Gredig, R. ; Green, A. ; Greenshaw, T. ; Gregoire, T. ; Grimm, O. ; Grube, J. ; Grudzinska, M. ; Gruev, V. ; Gruenewald, S. ; Grygorczuk, J. ; Guarino, V. ; Gunji, S. ; Gyuk, G. ; Hadasch, D. ; Hagiwara, R. ; Hahn, J. ; Hakansson, N. ; Hallgren, A. ; Hamer Heras, N. ; Hara, S. ; Hardcastle, M. J. ; Harris, J. ; Hassan, T. ; Hatanaka, K. ; Haubold, T. ; Haupt, A. ; Hayakawa, T. ; Hayashida, M. ; Heller, R. ; Henault, F. ; Henri, G. ; Hermann, G. ; Hermel, R. ; Herrero, A. ; Hidaka, N. ; Hinton, J. ; Hoffmann, D. ; Hofmann, W. ; Hofverberg, P. ; Holder, J. ; Horns, D. ; Horville, D. ; Houles, J. ; Hrabovsky, M. ; Hrupec, D. ; Huan, H. ; Huber, B. ; Huet, J. -M. ; Hughes, G. ; Humensky, T. B. ; Huovelin, J. ; Ibarra, A. ; Illa, J. M. ; Impiombato, D. ; Incorvaia, S. ; Inoue, S. ; Inoue, Y. ; Ioka, K. ; Ismailova, E. ; Jablonski, C. ; Jacholkowska, A. ; Jamrozy, M. ; Janiak, M. ; Jean, P. ; Jeanney, C. ; Jimenez, J. J. ; Jogler, T. ; Johnson, T. ; Journet, L. ; Juffroy, C. ; Jung, I. ; Kaaret, P. ; Kabuki, S. ; Kagaya, M. ; Kakuwa, J. ; Kalkuhl, C. ; Kankanyan, R. ; Karastergiou, A. ; Kaercher, K. ; Karczewski, M. ; Karkar, S. ; Kasperek, Aci. ; Kastana, D. ; Katagiri, H. ; Kataoka, J. ; Katarzynski, K. ; Katz, U. ; Kawanaka, N. ; Kellner-Leidel, B. ; Kelly, H. ; Kendziorra, E. ; Khelifi, B. ; Kieda, D. B. ; Kifune, T. ; Kihm, T. ; Kishimoto, T. ; Kitamoto, K. ; Kluzniak, W. ; Knapic, C. ; Knapp, J. w ; Knoedlseder, J. ; Koeck, F. ; Kocot, J. ; Kodani, K. ; Koehne, J. -H. ; Kohri, K. ; Kokkotas, K. ; Kolitzus, D. ; Komin, N. ; Kominis, I. ; Konno, Y. ; Koeppel, H. ; Korohoda, P. ; Kosack, K. ; Koss, G. ; Kossakowski, R. ; Kostka, P. ; Koul, R. ; Kowal, G. ; Koyama, S. ; Koziol, J. ; Kraehenbuehl, T. ; Krause, J. ; Krawzcynski, H. ; Krennrich, F. ; Krepps, A. ; Kretzschmann, A. ; Krobot, R. ; Krueger, P. ; Kubo, H. ; Kudryavtsev, V. A. ; Kushida, J. ; Kuznetsov, A. ; La Barbera, A. ; La Palombara, N. ; La Parola, V. ; La Rosa, G. ; Lacombe, K. ; Lamanna, G. ; Lande, J. ; Languignon, D. ; Lapington, J. ; Laporte, P. ; Lavalley, C. ; Le Flour, T. ; Le Padellec, A. ; Lee, S. -H. ; Lee, W. H. ; Leigui de Oliveira, M. A. ; Lelas, D. ; Lenain, J. -P. ; Leopold, D. J. ; Lerch, T. ; Lessio, L. ; Lieunard, B. ; Lindfors, E. ; Liolios, A. ; Lipniacka, A. ; Lockart, H. ; Lohse, T. ; Lombardi, S. ; Lopatin, A. ; Lopez, M. ; Lopez-Coto, R. ; Lopez-Oramas, A. ; Lorca, A. ; Lorenz, E. ; Lubinski, P. ; Lucarelli, F. ; Luedecke, H. ; Ludwin, J. ; Luque-Escamilla, P. L. ; Lustermann, W. ; Luz, O. ; Lyard, E. ; Maccarone, M. C. ; Maccarone, T. J. ; Madejski, G. M. ; Madhavan, A. ; Mahabir, M. ; Maier, G. ; Majumdar, P. ; Malaguti, G. ; Maltezos, S. ; Manalaysay, A. ; Mancilla, A. ; Mandat, D. ; Maneva, G. ; Mangano, A. ; Manigot, P. ; Mannheim, K. ; Manthos, I. ; Maragos, N. ; Marcowith, Alexandre ; Mariotti, M. ; Marisaldi, M. ; Markoff, S. ; Marszalek, A. ; Martens, C. ; Marti, J. ; Martin, J-M. ; Martin, P. ; Martinez, G. ; Martinez, F. ; Martinez, M. ; Masserot, A. ; Mastichiadis, A. ; Mathieu, A. ; Matsumoto, H. ; Mattana, F. ; Mattiazzo, S. ; Maurin, G. ; Maxfield, S. ; Maya, J. ; Mazin, D. ; Mc Comb, L. ; McCubbin, N. ; McHardy, I. ; McKay, R. ; Medina, C. ; Melioli, C. ; Melkumyan, D. ; Mereghetti, S. ; Mertsch, P. ; Meucci, M. ; Michalowski, J. ; Micolon, P. ; Mihailidis, A. ; Mineo, T. ; Minuti, M. ; Mirabal, N. ; Mirabel, F. ; Miranda, J. M. ; Mirzoyan, R. ; Mizuno, T. ; Moal, B. ; Moderski, R. ; Mognet, I. ; Molinari, E. ; Molinaro, M. ; Montaruli, T. ; Monteiro, I. ; Moore, P. ; Moralejo Olaizola, A. ; Mordalska, M. ; Morello, C. ; Mori, K. ; Mottez, F. ; Moudden, Y. ; Moulin, Emmanuel ; Mrusek, I. ; Mukherjee, R. ; Munar-Adrover, P. ; Muraishi, H. ; Murase, K. ; Murphy, A. ; Nagataki, S. ; Naito, T. ; Nakajima, D. ; Nakamori, T. ; Nakayama, K. ; Naumann, C. L. ; Naumann, D. ; Naumann-Godo, M. ; Nayman, P. ; Nedbal, D. ; Neise, D. ; Nellen, L. ; Neustroev, V. ; Neyroud, N. ; Nicastro, L. ; Nicolau-Kuklinski, J. ; Niedzwiecki, A. ; Niemiec, J. ; Nieto, D. ; Nikolaidis, A. ; Nishijima, K. ; Nolan, S. ; Northrop, R. ; Nosek, D. ; Nowak, N. ; Nozato, A. ; O'Brien, P. ; Ohira, Y. ; Ohishi, M. ; Ohm, S. ; Ohoka, H. ; Okuda, T. ; Okumura, A. ; Olive, J. -F. ; Ong, R. A. ; Orito, R. ; Orr, M. ; Osborne, J. ; Ostrowski, M. ; Otero, L. A. ; Otte, N. ; Ovcharov, E. ; Oya, I. ; Ozieblo, A. ; Padilla, L. ; Paiano, S. ; Paillot, D. ; Paizis, A. ; Palanque, S. ; Palatka, M. ; Pallota, J. ; Panagiotidis, K. ; Panazol, J. -L. ; Paneque, D. ; Panter, M. ; Paoletti, R. ; Papayannis, Alexandros ; Papyan, G. ; Paredes, J. M. ; Pareschi, G. ; Parks, G. ; Parraud, J. -M. ; Parsons, D. ; Arribas, M. Paz ; Pech, M. ; Pedaletti, G. ; Pelassa, V. ; Pelat, D. ; Perez, M. D. C. ; Persic, M. ; Petrucci, P-O ; Peyaud, B. ; Pichel, A. ; Pita, S. ; Pizzolato, F. ; Platos, L. ; Platzer, R. ; Pogosyan, L. ; Pohl, M. ; Pojmanski, G. ; Ponz, J. D. ; Potter, W. ; Poutanen, J. ; Prandini, E. ; Prast, J. ; Preece, R. ; Profeti, F. ; Prokoph, H. ; Prouza, M. ; Proyetti, M. ; Puerto-Gimenez, I. ; Puehlhofer, G. ; Puljak, I. ; Punch, M. ; Pyziol, R. ; Quel, E. J. ; Quinn, J. ; Quirrenbach, A. ; Racero, E. ; Rajda, P. J. ; Ramon, P. ; Rando, R. ; Rannot, R. C. ; Rataj, M. ; Raue, M. ; Reardon, P. ; Reimann, O. ; Reimer, A. ; Reimer, O. ; Reitberger, K. ; Renaud, M. ; Renner, S. ; Reville, B. ; Rhode, W. ; Ribo, M. ; Ribordy, M. ; Richer, M. G. ; Rico, J. ; Ridky, J. ; Rieger, F. ; Ringegni, P. ; Ripken, J. ; Ristori, P. R. ; Riviere, A. ; Rivoire, S. ; Rob, L. ; Roeser, U. ; Rohlfs, R. ; Rojas, G. ; Romano, Patrizia ; Romaszkan, W. ; Romero, G. E. ; Rosen, S. ; Lees, S. Rosier ; Ross, D. ; Rouaix, G. ; Rousselle, J. ; Rousselle, S. ; Rovero, A. C. ; Roy, F. ; Royer, S. ; Rudak, B. ; Rulten, C. ; Rupinski, M. ; Russo, F. ; Ryde, F. ; Sacco, B. ; Saemann, E. O. ; Saggion, A. ; Safiakian, V. ; Saito, K. ; Saito, T. ; Saito, Y. ; Sakaki, N. ; Sakonaka, R. ; Salini, A. ; Sanchez, F. ; Sanchez-Conde, M. ; Sandoval, A. ; Sandaker, H. ; Sant'Ambrogio, E. ; Santangelo, A. ; Santos, E. M. ; Sanuy, A. ; Sapozhnikov, L. ; Sarkar, S. ; Sartore, N. ; Sasaki, H. ; Satalecka, K. ; Sawada, M. ; Scalzotto, V. ; Scapin, V. ; Scarcioffolo, M. ; Schafer, J. ; Schanz, T. ; Schlenstedt, S. ; Schlickeiser, R. ; Schmidt, T. ; Schmoll, J. ; Schovanek, P. ; Schroedter, M. ; Schultz, C. ; Schultze, J. ; Schulz, A. ; Schure, K. ; Schwab, T. ; Schwanke, U. ; Schwarz, J. ; Schwarzburg, S. ; Schweizer, T. ; Schwemmer, S. ; Segreto, A. ; Seiradakis, J. -H. ; Sembroski, G. H. ; Seweryn, K. ; Sharma, M. ; Shayduk, M. ; Shellard, R. C. ; Shi, J. ; Shibata, T. ; Shibuya, A. ; Shum, E. ; Sidoli, L. ; Sidz, M. ; Sieiro, J. ; Sikora, M. ; Silk, J. ; Sillanpaa, A. ; Singh, B. B. ; Sitarek, J. ; Skole, C. ; Smareglia, R. ; Smith, A. ; Smith, D. ; Smith, J. ; Smith, N. ; Sobczynska, D. ; Sol, H. ; Sottile, G. ; Sowinski, M. ; Spanier, F. ; Spiga, D. ; Spyrou, S. ; Stamatescu, V. ; Stamerra, A. ; Starling, R. ; Stawarz, L. ; Steenkamp, R. ; Stegmann, Christian ; Steiner, S. ; Stergioulas, N. ; Sternberger, R. ; Sterzel, M. ; Stinzing, F. ; Stodulski, M. ; Straumann, U. ; Strazzeri, E. ; Stringhetti, L. ; Suarez, A. ; Suchenek, M. ; Sugawara, R. ; Sulanke, K. -H. ; Sun, S. ; Supanitsky, A. D. ; Suric, T. ; Sutcliffe, P. ; Sykes, J. ; Szanecki, M. ; Szepieniec, T. ; Szostek, A. ; Tagliaferri, G. ; Tajima, H. ; Takahashi, H. ; Takahashi, K. ; Takalo, L. ; Takami, H. ; Talbot, C. ; Tammi, J. ; Tanaka, M. ; Tanaka, S. ; Tasan, J. ; Tavani, M. ; Tavernet, J. -P. ; Tejedor, L. A. ; Telezhinsky, Igor O. ; Temnikov, P. ; Tenzer, C. ; Terada, Y. ; Terrier, R. ; Teshima, M. ; Testa, V. ; Tezier, D. ; Thuermann, D. ; Tibaldo, L. ; Tibolla, O. ; Tiengo, A. ; Tluczykont, M. ; Todero Peixoto, C. J. ; Tokanai, F. ; Tokarz, M. ; Toma, K. ; Torii, K. ; Tornikoski, M. ; Torres, D. F. ; Torres, M. ; Tosti, G. ; Totani, T. ; Toussenel, C. ; Tovmassian, G. ; Travnicek, P. ; Trifoglio, M. ; Troyano, I. ; Tsinganos, K. ; Ueno, H. ; Umehara, K. ; Upadhya, S. S. ; Usher, T. ; Uslenghi, M. ; Valdes-Galicia, J. F. ; Vallania, P. ; Vallejo, G. ; van Driel, W. ; van Eldik, C. ; Vandenbrouke, J. ; Vanderwalt, J. ; Vankov, H. ; Vasileiadis, G. ; Vassiliev, V. ; Veberic, D. ; Vegas, I. ; Vercellone, S. ; Vergani, S. ; Veyssiere, C. ; Vialle, J. P. ; Viana, A. ; Videla, M. ; Vincent, P. ; Vincent, S. ; Vink, J. ; Vlahakis, N. ; Vlahos, L. ; Vogler, P. ; Vollhardt, A. ; von Gunten, H. P. ; Vorobiov, S. ; Vuerli, C. ; Waegebaert, V. ; Wagner, R. ; Wagner, R. 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The Cherenkov Telescope Array (CTA) is a new observatory for very high-energy (VHE) gamma rays. CTA has ambitions science goals, for which it is necessary to achieve full-sky coverage, to improve the sensitivity by about an order of magnitude, to span about four decades of energy, from a few tens of GeV to above 100 TeV with enhanced angular and energy resolutions over existing VHE gamma-ray observatories. An international collaboration has formed with more than 1000 members from 27 countries in Europe, Asia, Africa and North and South America. In 2010 the CTA Consortium completed a Design Study and started a three-year Preparatory Phase which leads to production readiness of CTA in 2014. In this paper we introduce the science goals and the concept of CTA, and provide an overview of the project.
Acciari, V. A. ; Arlen, T. ; Aune, T. ; Benbow, W. ; Bird, R. ; Bouvier, A. ; Bradbury, S. M. ; Buckley, J. H. ; Bugaev, V. ; de la Calle Perez, I. ; Carter-Lewis, D. A. ; Cesarini, A. ; Ciupik, L. ; Collins-Hughes, E. ; Connolly, M. P. ; Cui, W. ; Duke, C. ; Dumm, J. ; Falcone, A. ; Federici, Simone ; Fegan, D. J. ; Fegan, S. J. ; Finley, J. P. ; Finnegan, G. ; Fortson, L. ; Gaidos, J. ; Galante, N. ; Gall, D. ; Gibbs, K. ; Gillanders, G. H. ; Griffin, S. ; Grube, J. ; Gyuk, G. ; Hanna, D. ; Horan, D. ; Humensky, T. B. ; Kaaret, P. ; Kertzman, M. ; Khassen, Y. ; Kieda, D. ; Krawczynski, H. ; Krennrich, F. ; Lang, M. J. ; McEnery, J. E. ; Madhavan, A. S. ; Moriarty, P. ; Nelson, T. ; Ong, R. A. ; Orr, M. ; Otte, A. N. ; Perkins, J. S. ; Petry, D. ; Pichel, A. ; Pohl, M. ; Quinn, J. ; Ragan, K. ; Reynolds, T. ; Roache, E. ; Rovero, A. ; Schroedter, M. ; Sembroski, G. H. ; Smith, A. ; Telezhinsky, Igor O. ; Theiling, M. ; Toner, J. ; Tyler, J. ; Varlotta, A. ; Vivier, M. ; Wakely, S. P. ; Ward, J. E. ; Weekes, T. C. ; Weinstein, A. ; Welsing, R. ; Williams, D. A. ; Wissel, S.
The variability of the blazar Markarian 421 in TeV gamma rays over a 14-year time period has been explored with the Whipple 10 m telescope. It is shown that the dynamic range of its flux variations is large and similar to that in X-rays. A correlation between the X-ray and TeV energy bands is observed during some bright flares and when the complete data sets are binned on long timescales. The main database consists of 878.4 h of observation with the Whipple telescope, spread over 783 nights. The peak energy response of the telescope was 400 GeV with 20% uncertainty. This is the largest database of any TeV-emitting active galactic nucleus (AGN) and hence was used to explore the variability profile of Markarian 421. The tithe-averaged flux from Markarian 421 over this period was 0.446 +/- 0.008 Crab flux units. The flux exceeded 10 Crab flux units on three separate occasions. For the 2000-2001 season the average flux reached 1.86 Crab units, while in the 1996-1997 season the average flux was only 0.23 Crab units.
Acciari, V. A. ; Aliu, E. ; Arlen, T. ; Aune, T. ; Beilicke, M. ; Benbow, W. ; Bradbury, S. M. ; Buckley, J. H. ; Bugaev, V. ; Byrum, K. ; Cannon, A. ; Cesarini, A. ; Ciupik, L. ; Collins-Hughes, E. ; Cui, W. ; Dickherber, R. ; Duke, C. ; Errando, M. ; Finley, J. P. ; Finnegan, G. ; Fortson, L. ; Furniss, A. ; Galante, N. ; Gall, D. ; Gillanders, G. H. ; Godambe, S. ; Griffin, S. ; Grube, J. ; Guenette, R. ; Gyuk, G. ; Hanna, D. ; Holder, J. ; Hughes, J. P. ; Hui, C. M. ; Humensky, T. B. ; Kaaret, P. ; Karlsson, N. ; Kertzman, M. ; Kieda, D. ; Krawczynski, H. ; Krennrich, F. ; Lang, M. J. ; LeBohec, S. ; Madhavan, A. S. ; Maier, G. ; Majumdar, P. ; McArthur, S. ; McCann, A. ; Moriarty, P. ; Mukherjee, R. ; Ong, R. A. ; Orr, M. ; Otte, A. N. ; Pandel, D. ; Park, N. H. ; Perkins, J. S. ; Pohl, Martin ; Quinn, J. ; Ragan, K. ; Reyes, L. C. ; Reynolds, P. T. ; Roache, E. ; Rose, H. J. ; Saxon, D. B. ; Schroedter, M. ; Sembroski, G. H. ; Senturk, G. Demet ; Slane, P. ; Smith, A. W. ; Tesic, G. ; Theiling, M. ; Thibadeau, S. ; Tsurusaki, K. ; Varlotta, A. ; Vassiliev, V. V. ; Vincent, S. ; Vivier, M. ; Wakely, S. P. ; Ward, J. E. ; Weekes, T. C. ; Weinstein, A. ; Weisgarber, T. ; Williams, D. A. ; Wood, M. ; Zitzer, B.
We report the discovery of TeV gamma-ray emission from the Type Ia supernova remnant (SNR) G120.1+1.4, known as Tycho's SNR. Observations performed in the period 2008-2010 with the VERITAS ground-based gamma-ray observatory reveal weak emission coming from the direction of the remnant, compatible with a point source located at 00(h)25(m)27(s).0, +64 degrees 10'50 '' (J2000). The TeV photon spectrum measured by VERITAS can be described with a power law dN/dE = C(E/3.42 TeV)(-Gamma) with Gamma = 1.95 +/- 0.51(stat) +/- 0.30(sys) and C = (1.55 +/- 0.43(stat) +/- 0.47(sys)) x 10(-14) cm(-2) s(-1) TeV-1. The integral flux above 1 TeV corresponds to similar to 0.9% of the steady Crab Nebula emission above the same energy, making it one of the weakest sources yet detected in TeV gamma rays. We present both leptonic and hadronic models that can describe the data. The lowest magnetic field allowed in these models is similar to 80 mu G, which may be interpreted as evidence for magnetic field amplification.
Acciari, V. A. ; Aliu, E. ; Arlen, T. ; Aune, T. ; Beilicke, M. ; Benbow, W. ; Bradbury, S. M. ; Buckley, J. H. ; Bugaev, V. ; Byrum, K. ; Cannon, A. ; Cesarini, A. ; Ciupik, L. ; Collins-Hughes, E. ; Connolly, M. P. ; Cui, W. ; Dickherber, R. ; Duke, C. ; Errando, M. ; Falcone, A. ; Finley, J. P. ; Finnegan, G. ; Fortson, L. ; Furniss, A. ; Galante, N. ; Gall, D. ; Gillanders, G. H. ; Godambe, S. ; Griffin, S. ; Grube, J. ; Guenette, R. ; Gyuk, G. ; Hanna, D. ; Holder, J. ; Hughes, G. ; Hui, C. M. ; Humensky, T. B. ; Kaaret, P. ; Karlsson, N. ; Kertzman, M. ; Kieda, D. ; Krawczynski, H. ; Krennrich, F. ; Lang, M. J. ; LeBohec, S. ; Maier, G. ; Majumdar, P. ; McArthur, S. ; McCann, A. ; Moriarty, P. ; Mukherjee, R. ; Ong, R. A. ; Orr, M. ; Otte, A. N. ; Park, N. ; Perkins, J. S. ; Pohl, Martin ; Prokoph, H. ; Quinn, J. ; Ragan, K. ; Reyes, L. C. ; Reynolds, P. T. ; Roache, E. ; Rose, H. J. ; Ruppel, J. ; Saxon, D. B. ; Schroedter, M. ; Sembroski, G. H. ; Senturk, G. D. ; Smith, A. W. ; Staszak, D. ; Tesic, G. ; Theiling, M. ; Thibadeau, S. ; Tsurusaki, K. ; Varlotta, A. ; Vassiliev, V. V. ; Vincent, S. ; Vivier, M. ; Wakely, S. P. ; Ward, J. E. ; Weekes, T. C. ; Weinstein, A. ; Weisgarber, T. ; Williams, D. A. ; Zitzer, B.
We present the results of observations of the TeV binary LS I + 61 degrees 303 with the VERITAS telescope array between 2008 and 2010, at energies above 300 GeV. In the past, both ground-based gamma-ray telescopes VERITAS and MAGIC have reported detections of TeV emission near the apastron phases of the binary orbit. The observations presented here show no strong evidence for TeV emission during these orbital phases; however, during observations taken in late 2010, significant emission was detected from the source close to the phase of superior conjunction (much closer to periastron passage) at a 5.6 standard deviation (5.6 sigma) post-trials significance. In total, between 2008 October and 2010 December a total exposure of 64.5 hr was accumulated with VERITAS on LS I + 61 degrees 303, resulting in an excess at the 3.3 sigma significance level for constant emission over the entire integrated data set. The flux upper limits derived for emission during the previously reliably active TeV phases (i.e., close to apastron) are less than 5% of the Crab Nebula flux in the same energy range. This result stands in apparent contrast to previous observations by both MAGIC and VERITAS which detected the source during these phases at 10% of the Crab Nebula flux. During the two year span of observations, a large amount of X-ray data were also accrued on LS I + 61 degrees 303 by the Swift X-ray Telescope and the Rossi X-ray Timing Explorer Proportional Counter Array. We find no evidence for a correlation between emission in the X-ray and TeV regimes during 20 directly overlapping observations. We also comment on data obtained contemporaneously by the Fermi Large Area Telescope.