Three-dimensional Kinematic Reconstruction of the Optically Emitting, High-velocity, Oxygen-rich Ejecta of Supernova Remnant N132D
| Autor: | Judy Schmidt, Dan Milisavljevic, Daniel J. Patnaude, Salvatore Orlando, George Takahashi, Michael D. Gladders, Jordan M. McGraw, Hidetoshi Sano, Niharika Sravan, Paul P. Plucinsky, Charles J. Law, John Banovetz |
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| Přispěvatelé: | ITA, USA, JPN |
| Rok vydání: | 2020 |
| Předmět: |
010504 meteorology & atmospheric sciences
Astrophysics::High Energy Astrophysical Phenomena FOS: Physical sciences Astrophysics::Cosmology and Extragalactic Astrophysics Astrophysics 01 natural sciences 0103 physical sciences Astrophysics::Solar and Stellar Astrophysics Spectral resolution Large Magellanic Cloud Ejecta Supernova remnant 010303 astronomy & astrophysics Solar and Stellar Astrophysics (astro-ph.SR) Astrophysics::Galaxy Astrophysics 0105 earth and related environmental sciences High Energy Astrophysical Phenomena (astro-ph.HE) Physics Center (category theory) Astronomy and Astrophysics Astrophysics - Astrophysics of Galaxies Cassiopeia A Radial velocity Supernova Astrophysics - Solar and Stellar Astrophysics Space and Planetary Science Astrophysics of Galaxies (astro-ph.GA) Astrophysics - High Energy Astrophysical Phenomena |
| Zdroj: | The Astrophysical Journal. 894:73 |
| ISSN: | 1538-4357 |
| Popis: | We present a three-dimensional kinematic reconstruction of the optically-emitting, oxygen-rich ejecta of supernova remnant N132D in the Large Magellanic Cloud. Data were obtained with the 6.5 m Magellan telescope in combination with the IMACS+GISMO instrument and survey [O III] $\lambda\lambda$4959,5007 line emission in a ${\sim}$3$^{\prime}~\times$ 3$^{\prime}$ region centered on N132D. The spatial and spectral resolution of our data enable detailed examination of the optical ejecta structure. The majority of N132D's optically bright oxygen ejecta are arranged in a torus-like geometry tilted approximately 28$^{\circ}$ with respect to the plane of the sky. The torus has a radius of 4.4 pc ($D_{\rm LMC}$/50 kpc), exhibits a blue-shifted radial velocity asymmetry of $-3000$ to $+2300$ km s$^{-1}$, and has a conspicuous break in its circumference. Assuming homologous expansion from the geometric center of O-rich filaments, the average expansion velocity of 1745 km s$^{-1}$ translates to an age since explosion of 2450 $\pm$ 195 yr. A faint, spatially-separated "runaway knot" (RK) with total space velocity of 3650 km s$^{-1}$ is nearly perpendicular to the torus plane and coincident with X-ray emission that is substantially enhanced in Si relative to the LMC and N132D's bulk ejecta. These kinematic and chemical signatures suggest that the RK may have had its origin deep within the progenitor star. Overall, the main shell morphology and high-velocity, Si-enriched components of N132D have remarkable similarity with that of Cassiopeia A, which was the result of a Type IIb supernova explosion. Our results underscore the need for further observations and simulations that can robustly reconcile whether the observed morphology is dominated by explosion dynamics or shaped by interaction with the environment. Comment: 18 pages, 12 figures, accepted for publication in ApJ; 3D animation of N132D can found at: http://www.physics.purdue.edu/kaboom/n132d-anim.mp4 |
| Databáze: | OpenAIRE |
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