A Study of Fermi-LAT GeV γ-Ray Emission toward the Magnetar-harboring Supernova Remnant Kesteven 73 and Its Molecular Environment

Liu, Bing; Chen, Yang; Zhang, Xiao; Liu, Qian-Cheng; He, Ting-Lan; Zhou, Xin; Zhou, Ping; Su, Yang

doi:10.3847/1538-4357/aa97d9

Cited by 9 publications

(10 citation statements)

References 45 publications

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“…Observations of the diffusive TeV energy gamma-ray emission from the Galactic Center from H.E.S.S. [48,49] and MAGIC models [6] are presented along with a GeV gamma-ray flux emission source in Kes 73 and its molecular environment using Fermi-LAT [72] as a reference to determine the reasonable- ness of the parameters used and to test the model. The young SNR Kes 73 (G27.4+0.0) hosts 1E 1841-045.…”

Section: Resultsmentioning

confidence: 99%

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High-energy gamma-ray emission from SNR G57.2+0.8 hosting SGR J1935+2154

Anjos,

Coelho,

Pereira

et al. 2021

Preprint

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In recent years some efforts have been made to identify active sources capable of accelerating particles up to 10 15 eV, known as PeVatrons. Measurements of TeV (10 12 eV) gamma-rays from supernova remnants (SNRs) have shown that efficient particle acceleration can occur in SNR diffusive shocks. In this paper, we obtain the contribution to the high energy and very high-energy gamma-ray (VHE, E > 100 GeV) emission due to cosmic-ray acceleration from Supernova Remnant G57.2+0.8 hosting the Soft Gamma Repeater (SGR) J1935+2154 with the use of the GALPROP code. To do so, we take into account the SNR + SGR association as a single source close to the galactic center. We propose that the above setting can provide a more comprehensive scenario for the generation of GeV-TeV gammarays. We also discuss the contribution from the SNR G57.2+0.8 and SGR J1935+2154 region to the diffusive TeV energy gamma-ray emission from the galactic center.

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Section: Resultsmentioning

confidence: 99%

“…The young SNR Kes 73 (G27.4+0.0) hosts 1E 1841-045. The model in [72] also provides the GeV gamma-ray contribution from this source considering the interaction of the SNR Kes 73 and the surrounding MC. The gamma-ray spectrum obtained can be explained by either a pure hadronic or a hadronic plus a magnetar emission.…”

Section: Resultsmentioning

confidence: 99%

High-energy gamma-ray emission from SNR G57.2+0.8 hosting SGR J1935+2154

Anjos,

Coelho,

Pereira

et al. 2021

Preprint

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“…The masses of the X-ray-emitting gas are ∼ 46 M and ∼ 200 M in Kes 73 and N49, respectively, indicating that the gas is dominated by the ISM. Kes 73 is possibly interacting with molecular gas in the east (Liu et al 2017), and N49 is interacting with molecular clouds in the southeast (Banas et al 1997;Otsuka et al 2010;Yamane et al 2018). The inhomogeneous ambient medium significantly influences the Xray morphology of the SNRs.…”

Section: Environment and Clues About The Progenitormentioning

confidence: 99%

“…3). The distance of Kes 73 is suggested to be 7.5-9.8 kpc using the HI observation by Tian & Leahy (2008) and 9 kpc using CO observation (Liu et al 2017). Here we take the distance of 8.5 kpc for Kes 73.…”

Section: Introductionmentioning

confidence: 99%

Spatially resolved X-ray study of supernova remnants that host magnetars: Implication of their fossil field origin

Zhou

Vink

Safi‐Harb

et al. 2019

A&A

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Magnetars are regarded as the most magnetized neutron stars in the Universe. Aiming to unveil what kinds of stars and supernovae can create magnetars, we have performed a state-of-the-art spatially resolved spectroscopic X-ray study of the supernova remnants (SNRs) Kes 73, RCW 103, and N49, which host magnetars 1E 1841−045, 1E 161348−5055, and SGR 0526−66, respectively. The three SNRs are O-and Ne-enhanced and are evolving in the interstellar medium with densities of > 1-2 cm −3 . The metal composition and dense environment indicate that the progenitor stars are not very massive. The progenitor masses of the three magnetars are constrained to be < 20 M (11-15 M for Kes 73, 13 M for RCW 103, and ∼ 13-17 M for N49). Our study suggests that magnetars are not necessarily made from very massive stars, but originate from stars that span a large mass range. The explosion energies of the three SNRs range from 10 50 erg to ∼ 2 × 10 51 erg, further refuting that the SNRs are energized by rapidly rotating (millisecond) pulsars. We report that RCW 103 is produced by a weak supernova explosion with significant fallback, as such an explosion explains the low explosion energy (∼ 10 50 erg), small observed metal masses (M O ∼ 4 × 10 −2 M and M Ne ∼ 6 × 10 −3 M ), and sub-solar abundances of heavier elements such as Si and S. Our study supports the fossil field origin as an important channel to produce magnetars, given the normal mass range (M ZAMS < 20 M ) of the progenitor stars, the low-to-normal explosion energy of the SNRs, and the fact that the fraction of SNRs hosting magnetars is consistent with the magnetic OB stars with high fields.

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“…Recently observations of Tycho's supernova remnant (SNR) reveal that Type Ia SNR may be also associated with MC (Zhou et al 2016b;Chen et al 2017). There are about 80 Galactic SNRs which are confirmed or suggested to be in physical contact with MCs, among 294 Galactic SNRs, at present (Gaensler et al 2008;Jiang et al 2010;Tian et al 2010;Eger et al 2011;Jeong et al 2012;Frail et al 2013;Chen et al 2014;Fukuda et al 2014;Su et al 2014;Zhou et al 2014;Zhu et al 2014;Zhang et al 2015;Voisin et al 2016;Zhou et al 2016a,c;de Wilt et al 2017;Lau et al 2017;Liu et al 2017;Su et al 2017b;Liu et al 2018;Maxted et al 2018;Su et al 2018;Ma et al 2019;Yu et al 2019;Green 2019, and references therein). Based on associations between SNRs and MCs, we could determine the distances of SNRs, and accordingly, the evolutionary stages of SNRs (e.g.…”

Section: Introductionmentioning

confidence: 99%

Molecular Clouds Surrounding Supernova Remnant G43.9+1.6: Associated and Non-associated

Zhou¹,

Su²,

Yang³

et al. 2020

Preprint

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Many supernova remnants (SNRs) are considered to evolve in molecular environments, but the associations between SNRs and molecular clouds (MCs) are often unclear. Being aware of such ambiguous case, we report our study on the molecular environment towards the SNR G43.9+1.6 by CO line observations. We investigated the correlations between the SNR and MCs at different velocities, and found two velocity components, i.e. ∼5 km s −1 and ∼50 km s −1 velocity components, showing spatial correlations with the remnant. However, no dynamical evidence of disturbance was found for the ∼5 km s −1 velocity component. At the distance of the ∼5 km s −1 velocity component, either near or far distance, the derived physical parameters are unreasonable too. We conclude that the SNR is not associated with the ∼5 km s −1 velocity component, and their spatial correlation is just a chance correlation. For the ∼50 km s −1 velocity component, dynamical evidence of disturbances, as well as the spatial correlation, indicate that it is associated with the SNR. We found that all the CO spectra extracted from the molecular clumps distributed along the border of the remnant are with broadened components presented, which can be fitted by Gaussian functions. By further analysis, we suggest that the SNR is at a near kinematic distance of about 3.1 kpc.

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A Study of Fermi-LAT GeV γ-Ray Emission toward the Magnetar-harboring Supernova Remnant Kesteven 73 and Its Molecular Environment

Cited by 9 publications

References 45 publications

High-energy gamma-ray emission from SNR G57.2+0.8 hosting SGR J1935+2154

High-energy gamma-ray emission from SNR G57.2+0.8 hosting SGR J1935+2154

Spatially resolved X-ray study of supernova remnants that host magnetars: Implication of their fossil field origin

Molecular Clouds Surrounding Supernova Remnant G43.9+1.6: Associated and Non-associated

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