Highlights of Galactic Science with the MAGIC telescopes

Abstract

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.

ICRC 2023 Rapporteur: Status of the Gamma-ray Astronomy field

“…[111]. We could also see the VHE gamma-ray observations [112] and modeling [113] of Eta Carina, the MAGIC observation of HESS J0632+057 and MAXI J1820+070 [49], the LS 5039 modulation and source coincident with V4641 Sgr detected by HAWC [114] and the observation of the Be/X-ray binary LS V +44 17 by VERITAS during outburst [115].…”

“…Some already known sources for which we had some updates are W51C, measured by LHAASO up to 300 TeV [47] for which still hadronic models (with an energy cut-off at 400 TeV) are favored to explain the emission. Updates on the measurement of another claimed PeVatron SNR G106.3+2.7 (Boomerang) were shown by HAWC [48], MAGIC [49] and also VERITAS [50], showing a spectrum that extends up to 500 TeV (see Fig. 3).…”

“…3). The VHE observations of 𝛾 Cygni [49,51] favor a hadronic origin for the emission although also reaching lower than PeV energies. New sources like LHAASO J2002+3238 is spatially associated with SNR G69.7+1.0 [52] but the origin of the VHE 𝛾-ray emission is unclear whether it is leptonic or hadronic.…”

“…7. LHAASO observed gamma rays from the location of the millisecond pulsar J0218+4232 [106], but even though spatially coincident, it is difficult to associate it with the millisecond pulsar and MAGIC did not find any emission coming from the region [49]. Finally, a study of the X-ray and 𝛾-ray emission of the variable 𝛾-ray pulsar PSR J2021+4026 [107] observed in different wavelengths shows a gamma-to-X shift of 0.21 in phase related to mode change.…”