Kinematics of the Galactic Supernova Remnant G109.1-1.0 (CTB 109)
| العنوان: | Kinematics of the Galactic Supernova Remnant G109.1-1.0 (CTB 109) |
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| المؤلفون: | Margarita Rosado, Mónica Sánchez-Cruces, I. Fuentes-Carrera, P. Ambrocio-Cruz |
| المصدر: | Monthly Notices of the Royal Astronomical Society. 473:1705-1717 |
| بيانات النشر: | Oxford University Press (OUP), 2017. |
| سنة النشر: | 2017 |
| مصطلحات موضوعية: | Physics, Astrophysics::High Energy Astrophysical Phenomena, Perseus Arm, Astronomy, Astronomy and Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, Lambda, Magnetar, 01 natural sciences, Supernova, Pulsar, Space and Planetary Science, 0103 physical sciences, Radiative transfer, 010306 general physics, Supernova remnant, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, Energy (signal processing) |
| الوصف: | We present direct images in the H$\alpha$ and [SII]$\lambda \lambda$6717,6731 $\textA$ 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. |
| تدمد: | 1365-2966 0035-8711 |
| DOI: | 10.1093/mnras/stx2460 |
| URL الوصول: | https://explore.openaire.eu/search/publication?articleId=doi_________::68bca70b4431215c6e8ef94eeb39e19f https://doi.org/10.1093/mnras/stx2460 |
| Rights: | OPEN |
| رقم الانضمام: | edsair.doi...........68bca70b4431215c6e8ef94eeb39e19f |
| قاعدة البيانات: | OpenAIRE |
| تدمد: | 13652966 00358711 |
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| DOI: | 10.1093/mnras/stx2460 |