Astrophys. J., 851, 37-37 (2017/December-2)
A study of Fermi-LAT GeV γ-ray emission toward the magnetar-harboring supernova remnant Kesteven 73 and its molecular environment.
LIU B., CHEN Y., ZHANG X., LIU Q.-C., HE T.-L., ZHOU X., ZHOU P. and SU Y.
Abstract (from CDS):
We report our independent GeV γ-ray study of the young shell-type supernova remnant (SNR) Kes 73, which harbors a central magnetar, and CO-line millimeter observations toward the SNR. Using 7.6 years of Fermi-LAT observation data, we detected an extended γ-ray source ("source A") with centroid on the west of the SNR, with a significance of 21σ in 0.1-300 GeV and an error circle of 5.'4 in angular radius. The γ-ray spectrum cannot be reproduced by a pure leptonic emission or a pure emission from the magnetar, and thus a hadronic emission component is needed. The CO-line observations reveal a molecular cloud (MC) at VLSR ∼ 90 km s–1, which demonstrates morphological correspondence with the western boundary of the SNR brightened in multiwavelength. The 12CO (J = 2 - 1)/12CO (J = 1 - 0) ratio in the left (blue) wing 85-88 km s–1 is prominently elevated to ∼1.1 along the northwestern boundary, providing kinematic evidence of the SNR-MC interaction. This SNR-MC association yields a kinematic distance 9 kpc to Kes 73. The MC is shown to be capable of accounting for the hadronic γ-ray emission component. The γ-ray spectrum can be interpreted with a pure hadronic emission or a magnetar+hadronic hybrid emission. In the case of pure hadronic emission, the spectral index of the protons is 2.4, very similar to that of the radio-emitting electrons, essentially consistent with the diffusive shock acceleration theory. In the case of magnetar+hadronic hybrid emission, a magnetic field decay rate >=1036 erg s–1 is needed to power the magnetar's curvature radiation.
© 2017. The American Astronomical Society. All rights reserved.
acceleration of particles - gamma rays: ISM - ISM: individual objects: G27.4+0.0 , Kes 73 - ISM: molecules - ISM: supernova remnants - stars: magnetars, 1E 1841-045 - stars: magnetars, 1E 1841-045
Figure 1: Sources A and B are not in SIMBAD.
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