Chandra observation of the Galactic supernova remnant CTB 109 (G109.1-1.0)

Abstract

Context: We study the X-ray emission of the Galactic supernova remnant (SNR) CTB 109 (G109.1-1.0), which is well-known for its enigmatic half-shell morphology both in radio and in X-rays and is associated with the anomalous X-ray pulsar (AXP) 1E2259+586. Aims: We want to understand the origin of the X-ray bright feature inside the SNR called the Lobe and the details of the interaction of the SNR shock wave with the ambient interstellar medium (ISM). Methods: The Lobe and the northeastern part of the SNR were observed with Chandra ACIS-I. We analysed the spectrum of the X-ray emission by dividing the entire observed emission into small regions. The X-ray emission is best reproduced with one-component or two-component non-equilibrium ionisation models depending on the position. In the two-component model one emission component represents the shocked ISM and the other the shocked ejecta. Results: We detect enhanced element abundances, in particular for Si and Fe, in and around the Lobe. There is one particular region next to the Lobe with a high Si abundance of 3.3 (2.6 - 4.0) times the solar value. This is the first, unequivocal detection of ejecta in CTB 109. Conclusions: The new Chandra data confirm that the Lobe was created by the interaction of the SNR shock and the supernova ejecta with dense and inhomogeneous medium in the environment of SNR CTB 109. The newly calculated age of the SNR is t ~ 1.4 x 10^4 yr.

Accepted for publication in A&A. 9 pages, 10 figures

References in corpus (5)

• The strongest cosmic magnets: Soft Gamma-ray Repeaters and Anomalous X-ray Pulsars
• Fermi-LAT Observations and A Broadband Study of Supernova Remnant CTB 109
• Evidence for Shocked Molecular Gas in the Galactic SNR CTB 109 (G109.1-1.0)
• Physical and chemical inhomogeneities inside the Vela SNR shell. Indications of ejecta shrapnels
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Cited by in corpus (21)

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• Comparing supernova remnants around strongly magnetized and canonical pulsars
• Kinematics of the Galactic SNR G109.1-1.0 (CTB 109)
• Spatially resolved X-ray study of supernova remnants that host magnetars: Implication of their fossil field origin
• Suzaku Studies of the Supernova Remnant CTB~109 Hosting the Magnetar 1E~2259+586
• ALMA CO Observations of Gamma-Ray Supernova Remnant N132D in the Large Magellanic Cloud: Possible Evidence for Shocked Molecular Clouds Illuminated by Cosmic-Ray Protons
• A Complete Catalogue of Dusty Supernova Remnants
• The life cycle of magnetars: a novel approach to estimate their ages
• A systematic study of soft X-ray pulse profiles of magnetars in quiescence
• Observational constraints on the maximum energies of accelerated particles in supernova remnants: low maximum energies and a large variety
• Study on the escape timescale of high-energy particles from supernova remnants through thermal X-ray properties
• How do supernova remnants cool? -- I. Morphology, optical emission lines, and shocks
• 3D Hydrodynamic Simulations of the Galactic Supernova Remnant CTB 109
• Multipole Analysis of Radio Continuum Images of Supernova Remnants: Comparison of Type Ia and Core Collapse
• Statistical ages and the cooling rate of X-ray dim isolated neutron stars
• Anisotropic neutrino effect on magnetar spin: constraint on inner toroidal field
• 3D MHD simulations of the supernova remnant CTB 109
• Correlation of Burst Behaviour with Magnetar Age