Observations of the Blazar 3c 66a With the Magic Telescopes in Stereoscopic Mode

Aleksić, J.; Antonelli, L. A.; Antoranz, P.; Backes, Michael; Barrio, J. A.; Bastieri, D.; González, J. Becerra; Bednarek, W.; Berdyugin, A.; Berger, K.; Bernardini, E.; Biland, A.; Blanch, O.; Böck, R.; Boller, A.; Bonnoli, G.; Bordas, P.; Tridon, D. Borla; Bosch‐Ramon, V.; Bose, D.; Braun, I.; Bretz, T.; Cámara, Miguel; Cañellas, A.; Carmona, E.; Carosi, A.; Colin, P.; Colombo, E.; Contreras, J. L.; Cortina, J.; Cossio, L.; Covino, S.; Dazzi, F.; Angelis, A. De; Pozo, E. De Cea del; Lotto, B. De; María, Mónica; Sabata, F. De; Mendez, C. Delgado; Ortega, A. Diago; Doert, M.; Domínguez, A.; Prester, D. Dominis; Dorner, D.; Doro, M.; Elsäesser, D.; Errando, M.; Ferenc, D.; Fonseca, M. V.; Font, L.; López, R. J. García; Garczarczyk, M.; Garrido, Daniel; Giavitto, G.; Godinović, N.; Hadasch, D.; Herrero, A.; Hildebrand, D.; Höhne-Mönch, D.; Hose, J.; Hrupec, Dario; Huber, Bernhard A.; Jogler, T.; Klepser, S.; Krähenbühl, T.; Kranich, D.; Krause, J.; Barbera, A. La; Lelas, D.; Leonardo, E.; Lindfors, E.; Lombardi, S.; Longo, F.; López, M.; Lorenz, E.; Majumdar, P.; Makariev, M.; Maneva, G.; Mankuzhiyil, N.; Mannheim, K.; Maraschi, L.; Mariotti, M.; Martı́nez, M.; Mazin, D.; Meucci, M.; Miranda, J. M.; Mirzoyan, R.; Miyamoto, H.; Moldón, J.; Moralejo, A.; Nieto, D.; Nilsson, K.; Orito, R.; Oya, I.; Paoletti, R.; Pardo, Sharon; Paredes, J. M.; Partini, S.; Pasanen, M.; Pauß, F.; Pegna, R.; Pérez-Torres, M. A.; Peršić, M.; Peruzzo, L.; Pochon, J.; Prada, Francisco; Moroni, P. G. Prada; Prandini, E.; Puchades, N.; Puljak, I.; Reichardt, I.; Reinthal, R.; Rhode, W.; Ribó, M.; Rico, J.; Rügamer, S.; Saggion, A.; Saito, Koji; Saito, T.; Salvati, M.; Sánchez‐Conde, Miguel A.; Satalecka, K.; Scalzotto, V.; Scapin, V.; Schultz, C.; Schweizer, T.; Shayduk, M.; Shore, Steven N.; Sierpowska-Bartosik, A.; Sillanpää, A.; Sitarek, J.; Sobczyńska, D.; Spanier, F.; Spiro, S.; Stamerra, A.; Steinke, B.; Storz, J.; Strah, N.; Struebig, J. C.; Surić, T.; Takalo, L. O.; Tavecchio, F.; Temnikov, P.; Terzić, T.; Tescaro, D.; Teshima, M.; Thom, M.; Torres, D. F.; Vankov, H.; Vogler, P.; Wagner, R. M.; Weitzel, Q.; Zabalza, V.; Zandanel, F.; Zanin, R.

doi:10.1088/0004-637x/726/2/58

Cited by 34 publications

(17 citation statements)

References 39 publications

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“…Furthermore, discoveries of γ-ray from distant blazars (e.g., [26,27,28]) support the EBL specific intensity level derived from galaxy count and recent EBL models [7,9,12]. As discussed the VHE recovered spectra of blazars up to ∼ 10 TeV are dominated by statistical and systematic uncertainties in the observations rather than EBL modelling.…”

Section: Discussionmentioning

confidence: 62%

“…[12]) satisfy the condition that the intrinsic spectrum corrected by the attenuation derived with our EBL model 4 has Γ int ≥ 1.5. We consider the following blazars: 3C 66A at z = 0.444 observed by MAGIC [26], 3C 279 at z = 0.536 observed by MAGIC in the 2007 observational campaign [27], and the discovery of PKS 1222+216 in the VHE regime [28], the second most distant flat-spectrum radio quasar known (z = 0.432). These three blazars are plotted in Fig.…”

Section: Pos(texas 2010)228mentioning

confidence: 99%

“…3. Figure 3: VHE spectra observed (blue) and EBL corrected (red) from the attenuation calculated with our EBL model of three high-redshift blazars measured by MAGIC [26,27,28]. The straight-red line is the best-fitting power law for every blazar with index Γ int .…”

Section: Pos(texas 2010)228mentioning

confidence: 99%

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Extragalactic Background Light Inferred from AEGIS Galaxy SED-type Fractions

Domínguez¹,

Primack²,

Rosario³

et al. 2011

Proceedings of 25th Texas Symposium on Relativistic Astrophysics — PoS(Texas 2010)

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The extragalactic background light (EBL) is of fundamental importance both for understanding the entire process of galaxy evolution and for γ-ray astronomy. However, the overall spectrum of the EBL between 0.1 and 1000 µm has never been determined directly neither from observed luminosity functions (LFs), over a wide redshift range, nor from any multiwavelength observation of galaxy spectral energy distributions (SEDs). The evolving, overall spectrum of the EBL is derived here utilizing a novel method based on observations only. The changing fractions of quiescent galaxies, star-forming galaxies, starburst galaxies and active galactic nucleus (AGN) galaxies from redshift 0.2 to 1 are estimated, and two alternative extrapolations of SED types to higher redshifts are considered. This allows calculation of the evolving EBL. The EBL uncertainties in our modelling based directly on the data are quantified, and their consequences for attenuation of very-high-energy γ-rays due to pair production on the EBL are discussed. It is concluded that the EBL seems well constrained from the UV to the mid-IR at an intensity level roughly matching galaxy count data. Independent efforts from IR and γ-ray astronomy are needed in order to reduce the uncertainties in the far-IR.

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Section: Discussionmentioning

confidence: 62%

Section: Pos(texas 2010)228mentioning

confidence: 99%

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Extragalactic Background Light Inferred from AEGIS Galaxy SED-type Fractions

Domínguez¹,

Primack²,

Rosario³

et al. 2011

Proceedings of 25th Texas Symposium on Relativistic Astrophysics — PoS(Texas 2010)

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show abstract

“…In discussing photon/ALP conversion in IGMFs, it is also necessary to consider the important role of the Extragalactic Background Light (EBL), its main effect being an additional attenuation of the photon flux (especially at energies above about 100 GeV). Recent gamma-ray observations already pose substantial challenges to the conventional models that explain the observed source spectra in terms of EBL attenuation [144,145,146,147,148].…”

Section: Search Of Axion-like Particles With Ctamentioning

confidence: 99%

Dark matter and fundamental physics with the Cherenkov Telescope Array

Doro

Conrad

Emmanoulopoulos

et al. 2013

Astroparticle Physics

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143

198

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The Cherenkov Telescope Array (CTA) is a project for a next-generation observatory for very high energy (GeV–TeV) ground-based gamma-ray astronomy, currently in its design phase, and foreseen to be operative a few years from now. Several tens of telescopes of 2–3 different sizes, distributed over a large area, will allow for a sensitivity about a factor 10 better than current instruments such as H.E.S.S, MAGIC and VERITAS, an energy coverage from a few tens of GeV to several tens of TeV, and a field of view of up to 10°. In the following study, we investigate the prospects for CTA to study several science questions that can profoundly influence our current knowledge of fundamental physics. Based on conservative assumptions for the performance of the different CTA telescope configurations currently under discussion, we employ a Monte Carlo based approach to evaluate the prospects for detection and characterisation of new physics with the array. First, we discuss CTA prospects for cold dark matter searches, following different observational strategies: in dwarf satellite galaxies of the Milky Way, which are virtually void of astrophysical background and have a relatively well known dark matter density; in the region close to the Galactic Centre, where the dark matter density is expected to be large while the astrophysical background due to the Galactic Centre can be excluded; and in clusters of galaxies, where the intrinsic flux may be boosted significantly by the large number of halo substructures. The possible search for spatial signatures, facilitated by the larger field of view of CTA, is also discussed. Next we consider searches for axion-like particles which, besides being possible candidates for dark matter may also explain the unexpectedly low absorption by extragalactic background light of gamma-rays from very distant blazars. We establish the axion mass range CTA could probe through observation of long-lasting flares in distant sources. Simulated light-curves of flaring sources are also used to determine the sensitivity to violations of Lorentz invariance by detection of the possible delay between the arrival times of photons at different energies. Finally, we mention searches for other exotic physics with CTA

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“…The details of MAGIC data analysis can be found in Moralejo et al (2009) and Aleksić et al (2010). 4C 21.35 was observed on June 17 th for 30 minutes under moderate moonlight conditions.…”

Section: Magic Observations Data Analysis and Resultsmentioning

confidence: 99%