Kinematics of the Galactic SNR G109.1-1.0 (CTB 109)

Abstract

We present direct images in the H$\alpha$ and [SII]$\lambda \lambda$6717,6731 $\text{A˚}$ lines of the Galactic Supernova Remnant G109.1-1.0 (CTB 109). We confirm that the filaments detected are the optical counterpart of the X-ray and radio supernova remnant due to their high [SII]/H$\alpha$ line-ratios. We study for the first time the kinematics of the optical counterpart of SNR CTB 109 using the UNAM scanning Fabry-Perot interferometer PUMA. We estimate a systemic velocity of V${}_{LSR}$=-50$\pm$6 km s${}^{-1}$ for this remnant and an expansion velocity of V${}_{exp}$=230$\pm$5 km s${}^{-1}$. From this velocity value and taking into account previous studies about the kinematics of objects at that Galactic longitude we derive a distance to the SNR CTB 109 of 3.1$\pm$0.2 kpc, locating it in the Perseus arm. Using the [SII]$\lambda$6717/[SII]$\lambda$6731 line-ratio we find an electronic density value around n${}_e$= 580 cm${}^{-3}$. Considering that this remnant is evolving in a low density medium with higher density cloudlets responsible of the optical emission, we determine the age and energy deposited in the ISM by the supernova explosion (E${}_0$) in both the Sedov-Taylor phase and the radiative phase. For both cases the age is of thousands of years and the E${}_0$ is rather typical of SNRs containing simple pulsars so that, the energy released to the ISM cannot be used to distinguish between supernova remnants hosting typical pulsars from those hosting powerful magnetars as in the case of CTB 109.

arXiv comment14 pages, 8 Figures, Accepted for publication in MNRAS

References in corpus (20)

• A New Electron Density Model for Estimation of Pulsar and FRB Distances
• The McGill Magnetar Catalog
• The strongest cosmic magnets: Soft Gamma-ray Repeaters and Anomalous X-ray Pulsars
• NE2001.I. A New Model for the Galactic Distribution of Free Electrons and its Fluctuations
• The Distance to the Perseus Spiral Arm in the Milky Way
• Kinematic Distances to Molecular Clouds identified in the Galactic Ring Survey
• Changes in the X-ray Emission from the Magnetar Candidate 1E 2259+586 during its 2002 Outburst
• Population synthesis studies of isolated neutron stars with magnetic field decay
• Distances to Anomalous X-ray Pulsars using Red Clump Stars
• Constraining the Braking Indices of Magnetars
• A Self-Absorption Census of Cold HI Clouds in the Canadian Galactic Plane Survey
• XMM-Newton observations of the Galactic Supernova Remnant CTB 109 (G109.1-1.0)
• Pulsar Braking Indices, Glitches and Energy Dissipation In Neutron Stars
• The distance to the SNR CTB109 deduced from its environment
• Evidence for Shocked Molecular Gas in the Galactic SNR CTB 109 (G109.1-1.0)
• Supernova remnants with magnetars: clues to magnetar formation
• Chandra observation of the Galactic supernova remnant CTB 109 (G109.1-1.0)
• Kinematics of the ionized gas in the Local Group irregular galaxy IC 1613
• Distance to the SNR CTB 109/AXP 1E 2259+586 by HI absorption and self-absorption
• Suzaku Studies of the Supernova Remnant CTB~109 Hosting the Magnetar 1E~2259+586

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