2023A&A...670A...8M

Query : 2023A&A...670A...8M

2023A&A...670A...8M - Astronomy and Astrophysics, volume 670A8 (2023/2-1)

Study of the GeV to TeV morphology of the γ Cygni SNR (G 78.2+2.1) with MAGIC and Fermi-LAT Evidence for cosmic ray escape.

MAGIC COLLABORATION, ACCIARI V.A., ANSOLDI S., ANTONELLI L.A., ARBET ENGELS A., BAACK D., BABIC A., BANERJEE B., BARRES DE ALMEIDA U., BARRIO J.A., BECERRA GONZALEZ J., BEDNAREK W., BELLIZZI L., BERNARDINI E., BERTI A., BESENRIEDER J., BHATTACHARYYA W., BIGONGIARI C., BILAND A., BLANCH O., BONNOLI G., BOSNJAK Z., BUSETTO G., CAROSI R., CERIBELLA G., CERRUTI M., CHAI Y., CHILINGARIAN A., CIKOTA S., COLAK S.M., COLIN U., COLOMBO E., CONTRERAS J.L., CORTINA J., COVINO S., D'ELIA V., DA VELA P., DAZZI F., DE ANGELIS A., DE LOTTO B., DELFINO M., DELGADO J., DEPAOLI D., DI PIERRO F., DI VENERE L., DO SOUTO ESPINEIRA E., DOMINIS PRESTER D., DONINI A., DORNER D., DORO M., ELSAESSER D., FALLAH RAMAZANI V., FATTORINI A., FERRARA G., FOFFANO L., FONSECA M.V., FONT L., FRUCK C., FUKAMI S., GARCIA LOPEZ R.J., GARCZARCZYK M., GASPARYAN S., GAUG M., GIGLIETTO N., GIORDANO F., GLIWNY P., GODINOVIC N., GREEN D., HADASCH D., HAHN A., HERRERA J., HOANG J., HRUPEC D., HUTTEN M., INADA T., INOUE S., ISHIO K., IWAMURA Y., JOUVIN L., KAJIWARA Y., KARJALAINEN M., KERSZBERG D., KOBAYASHI Y., KUBO H., KUSHIDA J., LAMASTRA A., LELAS D., LEONE F., LINDFORS E., LOMBARDI S., LONGO F., LOPEZ M., LOPEZ-COTO R., LOPEZ-ORAMAS A., LOPORCHIO S., MACHADO DE OLIVEIRA FRAGA B., MASUDA S., MAGGIO C., MAJUMDAR P., MAKARIEV M., MALLAMACI M., MANEVA G., MANGANARO M., MANNHEIM K., MARASCHI L., MARIOTTI M., MARTINEZ M., MAZIN D., MENDER S., MICANOVIC S., MICELI D., MIENER T., MINEV M., MIRANDA J.M., MIRZOYAN R., MOLINA E., MORALEJO A., MORCUENDE D., MORENO V., MORETTI E., MUNAR-ADROVER P., NEUSTROEV V., NIGRO C., NILSSON K., NINCI D., NISHIJIMA K., NODA K., NOGUES L., NOZAKI S., OHTANI Y., OKA T., OTERO-SANTOS J., PALATIELLO M., PANEQUE D., PAOLETTI R., PAREDES J.M., PAVLETIC L., PENIL P., PERESANO M., PERSIC M., PRADA MORONI P.G., PRANDINI E., PULJAK I., RHODE W., RIBO M., RICO J., RIGHI C., RUGLIANCICH A., SAHA L., SAHAKYAN N., SAITO T., SAKURAI S., SATALECKA K., SCHLEICHER B., SCHMIDT K., SCHWEIZER T., SITAREK J., SNIDARIC I., SOBCZYNSKA D., SPOLON A., STAMERRA A., STROM D., STRZYS M., SUDA Y., SURIC T., TAKAHASHI M., TAVECCHIO F., TEMNIKOV P., TERZIC T., TESHIMA M., TORRES-ALBA N., TOSTI L., VAN SCHERPENBERG J., VANZO G., VAZQUEZ ACOSTA M., VENTURA S., VERGUILOV V., VIGORITO C.F., VITALE V., VOVK I., WILL M., ZARIC D., CELLI S. and MORLINO G.

Abstract (from CDS):


Context. Diffusive shock acceleration (DSA) is the most promising mechanism that accelerates Galactic cosmic rays (CRs) in the shocks of supernova remnants (SNRs). It is based on particles scattering caused by turbulence ahead and behind the shock. The turbulence upstream is supposedly generated by the CRs, but this process is not well understood. The dominant mechanism may depend on the evolutionary state of the shock and can be studied via the CRs escaping upstream into the interstellar medium (ISM).
Aims . Previous observations of the γ Cygni SNR showed a difference in morphology between GeV and TeV energies. Since this SNR has the right age and is at the evolutionary stage for a significant fraction of CRs to escape, our aim is to understand γ-ray emission in the vicinity of the γ Cygni SNR.
Methods. We observed the region of the γ Cygni SNR with the MAGIC Imaging Atmospheric Cherenkov telescopes between 2015 May and 2017 September recording 87 h of good-quality data. Additionally, we analysed Fermi-LAT data to study the energy dependence of the morphology as well as the energy spectrum in the GeV to TeV range. The energy spectra and morphology were compared against theoretical predictions, which include a detailed derivation of the CR escape process and their γ-ray generation.
Results. The MAGIC and Fermi-LAT data allowed us to identify three emission regions that can be associated with the SNR and that dominate at different energies. Our hadronic emission model accounts well for the morphology and energy spectrum of all source components. It constrains the time-dependence of the maximum energy of the CRs at the shock, the time-dependence of the level of turbulence, and the diffusion coefficient immediately outside the SNR shock. While in agreement with the standard picture of DSA, the time-dependence of the maximum energy was found to be steeper than predicted, and the level of turbulence was found to change over the lifetime of the SNR.

Abstract Copyright: © ESO 2023

Journal keyword(s): acceleration of particles - cosmic rays - gamma rays: general - gamma rays: ISM - ISM: clouds - ISM: supernova remnants

Simbad objects: 19

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Number of rows : 19
N Identifier Otype ICRS (J2000)
RA 		ICRS (J2000)
DEC 		Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2026 		#notes
1 M 1 SNR 05 34 31.8 +22 01 03           ~ 6516 1
2 IC 443 SNR 06 17 00.0000000 +22 34 11.998901           ~ 1314 1
3 SNR G347.3-00.5 SNR 17 12 27 -39 41.2     12.27     ~ 761 1
4 SNR G006.4-00.1 SNR 18 00 31.2011719 -23 25 48.001099           ~ 782 1
5 SNR G034.6-00.5 SNR 18 56 10.650 +01 13 21.30           ~ 1034 2
6 SNR G049.1-00.1 SNR 19 23 19.300 +14 09 21.00           ~ 309 0
7 4FGL J2016.2+3712 gam 20 16 13.7 +37 12 47           ~ 12 0
8 ARGO J2021+4038 gam 20 19 00.0 +40 42 00           ~ 33 1
9 MAGIC J2019+408 ? 20 19.5 +55 00           ~ 2 0
10 HD 193576 WR* 20 19 32.4229160448 +38 43 53.959035756 8.15 8.53 8.00     WN5+O6II-V 721 0
11 [UTA2002] C2 X 20 20 00.0 +40 40 03           ~ 3 0
12 NAME gam Cyg SNR SNR 20 20 17.100 +40 26 09.00           ~ 247 2
13 2HWC J2020+403 gam 20 20.6 +40 22           ~ 7 0
14 FL8Y J2021.0+4031e gam 20 21.0 +40 31           ~ 1 0
15 [UTA2002] C1 X 20 21 12.0 +40 47 55           ~ 3 0
16 PSR J2021+4026 Psr 20 21 30.496 +40 26 53.56           ~ 300 2
17 * gam Cyg V* 20 22 13.7018357 +40 15 24.044963 3.44 2.90 2.23 1.74 1.40 F8Ib 607 0
18 NAME Cyg X Cld 20 30 04.7973633 +40 51 36.002197           ~ 962 1
19 NAME Cyg Complex reg 20 32 +45.0           ~ 667 0

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