Study of the GeV to TeV morphology of the <i>γ</i> Cygni SNR (G 78.2+2.1) with MAGIC and <i>Fermi-LAT</i>

Acciari, V. A.; Ansoldi, S.; Antonelli, L. A.; Engels, A. Arbet; Baack, Dominik; Babić, Ana; Banerjee, B.; Almeida, U. Barres de; Barrio, J. A.; González, J. Becerra; Bednarek, W.; Bellizzi, Lorenzo; Bernardini, E.; Berti, Alessio; Besenrieder, Jürgen; Bhattacharyya, W.; Bigongiari, C.; Biland, A.; Blanch, O.; Bonnoli, Giacomo; Bošnjak, Željka; Busetto, G.; Carosi, R.; Ceribella, Giovanni; Cerruti, M.; Chai, Yating; Chilingarian, A.; Cikota, Stefan; Colak, S. M.; Colin, U.; Colombo, E.; Contreras, J. L.; Cortina, J.; Covino, S.; D’Elia, V.; Vela, P. Da; Dazzi, F.; Angelis, A. De; Lotto, B. De; Delfino, Manuel; Delgado, Jordi; Depaoli, Davide; Pierro, F. Di; Venere, L. Di; Espiñeira, E. Do Souto; Prester, D. Dominis; Donini, Alice; Dorner, D.; Doro, M.; Elsäesser, D.; Ramazani, Vandad Fallah; Fattorini, Alicia; Ferrara, G.; Foffano, Luca; Fonseca, M. V.; Font, L.; Fruck, C.; Fukami, Satoshi; López, R. J. García; Garczarczyk, M.; Gasparyan, Sargis; Gaug, M.; Giglietto, N.; Giordano, F.; Gliwny, Paweł; Godinović, N.; Green, D.; Hadasch, D.; Hahn, Alexander; Herrera, J.; Hoang, J.; Hrupec, Dario; Hütten, Moritz; Inada, Tomohiro; Inoue, Susumu; Ishio, Kazuma; Iwamura, Y.; Jouvin, L.; Kajiwara, Y.; Karjalainen, Marie; Kerszberg, Daniel; Kobayashi, Yukiho; Kubo, H.; Kushida, J.; Lamastra, Alessandra; Lelas, D.; Leone, F.; Lindfors, E.; Lombardi, S.; Longo, F.; López, M.; López-Coto, R.; López-Oramas, Alicia; Loporchio, Serena; Fraga, Bernardo Machado de Oliveira; Masuda, S.; Maggio, C.; Majumdar, P.; Makariev, M.; Mallamaci, M.; Maneva, G.; Manganaro, M.; Mannheim, K.; Maraschi, L.; Mariotti, M.; Martı́nez, M.; Mazin, D.; Mender, Simone; Mićanović, Saša; Miceli, Davide; Miener, Tjark; Minev, M.; Miranda, Jose Miguel; Mirzoyan, R.; Molina, Edgar; Moralejo, A.; Morcuende, Daniel; Moreno, V.; Moretti, E.; Munar-Adrover, P.; Neustroev, V.; Nigro, Cosimo; Nilsson, K.; Ninci, D.; Nishijima, K.; Noda, K.; Nogués, L.; Nozaki, S.; Ohtani, Y.; Oka, Tomohiko; Otero-Santos, Jorge; Palatiello, M.; Paneque, D.; Paoletti, R.; Paredes, J. M.; Pavletić, Lovro; Peñil, Pablo; Peresano, M.; Peršić, M.; Moroni, Pier Giorgio Prada; Prandini, E.; Puljak, I.; Rhode, W.; Ribó, M.; Rico, J.; Righi, Chiara; Rugliancich, A.; Saha, L.; Sahakyan, N.; Saito, Tatsuhiko; Sakurai, S.; Satalecka, K.; Schleicher, Bernd; Schmidt, K.; Schweizer, T.; Sitarek, J.; Šnidarić, Iva; Sobczyńska, Dorota; Spolon, Alessia; Stamerra, A.; Strom, D.; Strzys, M.; Suda, Y.; Surić, T.; Takahashi, Mitsunari; Tavecchio, F.; Temnikov, P.; Terzić, T.; Teshima, M.; Torres-Albà, N.; Tosti, Luca; Scherpenberg, Juliane van; Vanzo, G.; Acosta, Mónica Vázquez; Ventura, Sofia; Verguilov, V.; Vigorito, C.; Vitale, V.; Vovk, Ievgen; Will, Martin; Zarić, Darko; Celli, S.; Morlino, G.

doi:10.1051/0004-6361/202038748

Cited by 7 publications

(4 citation statements)

References 88 publications

Supporting

Mentioning

Contrasting

Order By: Relevance

“…From VERITAS and Fermi/LAT analysis, [6] pointed out that the VHE 𝛾-rays can be explained with a non-thermal bremsstrahlung model from the SNR shell, i.e., a leptonic model. Recently, MAGIC also observed this SNR and discovered the VHE 𝛾-ray emission, MAGIC J2019+408, over the SNR shell and outward from the northern part of it [7]. However, in contrast to [6], the observed VHE 𝛾-ray spectrum can be explained by pion decay, i.e., a hadronic model.…”

Section: Introductionmentioning

confidence: 94%

See 1 more Smart Citation

X-ray Observation of Possible Cosmic-Ray Escaping Region of SNR G78.2+2.1

Tateishi¹

2023

Proceedings of 38th International Cosmic Ray Conference — PoS(ICRC2023)

View full text Add to dashboard Cite

The observation of non-thermal radiation of SNRs are essential for elucidating the mechanism of particle acceleration. MAGIC and Fermi discovered very high energy (VHE) 𝛾-ray radiation from the northern part of SNR G78.2+2.1 (MAGIC Collaboration. 2020). This radiation is suggested to be originated from cosmic rays escaping from the SNR. However, it is inconclusive since the electron energy distribution is not well estimated. To solve this problem, we analyzed data from the X-ray astronomy satellite Suzaku to evaluate the contribution of the leptonic emission of the broadband spectrum of MAGIC J2019+408. Our analysis revealed a hard X-ray component in the northern region of SNR G78.2+2.1 with a flux several times larger than the X-ray background radiation. The emission extending outside the SNR was represented in the X-ray image in 2-5 keV, but is not associated with the SNR. X-rays above 2 keV could be explained either by an absorbed thermal-emission model with a temperature of 1.6 +0.4 −0.2 keV and low-solar (0.3 ± 0.2 𝑍 ⊙ ) abundances or by an absorbed synchrotron (Γ = 3.7 ± 0.5) radiation model with no statistically significant difference. From SED analysis of radio to VHE 𝛾-ray, X-ray and 𝛾-ray spectra can be reproduced by the synchrotron model with the magnetic field strength of 50 𝜇G, but requires more-than one order-of-magnitude brighter radio flux than the observation result of the SNR shell. Alternatively, a magnetic intensity of 4 𝜇G will also satisfy radio and VHE 𝛾-ray flux, but this magnetic strength was significantly lower than what we expected for the diffusive shock acceleration. These results suggest that the observed X-rays have a different origin from nonthermal emission of MAGIC J2019+408, and some of the VHE 𝛾-rays originated from escaped cosmic rays.

show abstract

Section: Introductionmentioning

confidence: 94%

“…a leptonic model. The orange lines, red lines, and green dot represent the X-ray spectrum detected by XIS, the 𝛾-ray spectrum detected by Fermi/LAT and MAGIC[7], and 325 MHz radio flux in region R2 observed by GMRT[17], respectively. The dot line and black line represent the synchrotron and inverse Compton model of scenario 1 (black) and scenario 2 (blue).…”

mentioning

confidence: 99%

X-ray Observation of Possible Cosmic-Ray Escaping Region of SNR G78.2+2.1

Tateishi¹

2023

Proceedings of 38th International Cosmic Ray Conference — PoS(ICRC2023)

View full text Add to dashboard Cite

show abstract

“…Between May and November 2015, as well as between April and September 2017, MAGIC conducted observations on the 𝛾 Cygni SNR, G78.2+2.1, accumulating an effective observation time of 85 hours [6]. This SNR is believed to be the remnant of a core-collapse supernova with an age estimated of ∼ 7000 years, placing it in the Sedov-Taylor phase.…”

Section: Supernova Remnantsmentioning

confidence: 99%

Highlights of Galactic Science with the MAGIC telescopes

Strzys¹,

Abe²,

Abe³

et al. 2023

Proceedings of 38th International Cosmic Ray Conference — PoS(ICRC2023)

View full text Add to dashboard Cite

There are several types of Galactic sources that can potentially accelerate charged particles up to GeV and TeV energies. These accelerated particles can produce Very High Energy (E>100 GeV) gamma-ray emission through different non-thermal processes such as inverse Compton scattering of ambient photon fields by accelerated electrons or pion decay after proton-proton collisions.Here we present highlight results of observations with the MAGIC telescopes on Galactic sources: millisecond pulsars, supernova remnants (SNRs), pulsar wind nebulae (PWNe), novae and binary systems. In particular, we present the promising PeVatron candidate SNR G106.3+2.7 containing an energetic PWN named Boomerang. Also, in the ongoing search for new source classes we looked for very-high-energy emission from the millisecond pulsar PSR J0218+4232 that has long been considered as one of the best candidates. Furthermore, we present the observations during an exceptionally bright X-ray outburst from the low mass X-ray binary MAXI J1820+070. Finally, we highlight the MAGIC results of the first nova detected at VHEs: RS Ophiuchi, a recurrent symbiotic nova located in the Milky Way. The detection with the MAGIC telescopes proves a hadronic origin of the the gamma-ray emission, and helps in understanding the contribution of novae to the cosmic-ray budget.

show abstract

“…For example, angular resolution is a key element in increasing the sensitivity of instruments because the signal/background ratio is proportional to the square of the angular resolution times the rejection efficiency for cosmic rays for the point source, and angular resolution is also critical for the morphology study of the gamma-ray source; the detection of fine structures in morphologies would help to identify the origin of the gamma rays. The inverse Compton scattering of electrons should show narrow structures, which are governed by the rapid cooling of the radiating electrons [9,10], whereas hadronic interactions are expected to generate much smoother structures [11,12].…”

Section: Introductionmentioning

confidence: 99%

Study of Angular Resolution Using Imaging Atmospheric Cherenkov Technique

Liu,

Wu,

Liu

et al. 2024

Universe

View full text Add to dashboard Cite

Angular resolution is crucial for the detailed study of gamma-ray sources and current Cherenkov telescopes (e.g., HESS, MAGIC, and VERITAS) that operate below tens of TeV. Several gamma-ray sources with a photon energy larger than 100 TeV have been revealed by the LHAASO in recent years; the angular resolution of the LHAASO is around 0.3∘. A gamma-ray detector with an angular resolution of less than 0.1∘ operating beyond 100 TeV is needed to study the detailed morphology of ultra-high-energy gamma-ray sources further. The cost-effectiveness is crucial for such large-area detectors. In this paper, the impact of telescope aperture, field of view, pixel size, optical point spread function, and signal integration time window on angular resolution is studied. These results can provide essential elements for the design of telescope arrays.

show abstract

Study of the GeV to TeV morphology of the γ Cygni SNR (G 78.2+2.1) with MAGIC and Fermi-LAT

Cited by 7 publications

References 88 publications

X-ray Observation of Possible Cosmic-Ray Escaping Region of SNR G78.2+2.1

X-ray Observation of Possible Cosmic-Ray Escaping Region of SNR G78.2+2.1

Highlights of Galactic Science with the MAGIC telescopes

Study of Angular Resolution Using Imaging Atmospheric Cherenkov Technique

Contact Info

Product

Resources

About