English (United Kingdom)

https://curated-unify.zendy.io/wp-json/zendy-region/v1/featured_content/oa?rat=en

https://curated-unify.zendy.io/wp-json/zendy-region/v1/highlighted_journal/

Global: Zendy Plus annual

Presents the access of premium content as premium feature

Premium Content

Presents the keyphrase highlighting as premium feature

Keyphrase Highlighting

Presents the summarisation as premium feature

Summarisation

Insights

Presents the pdf analysis as premium feature

PDF Analysis

Presents the zaia usage as premium feature

ZAIA

Global: Zendy Plus monthly

Global: Zendy Tools annual

Global: Zendy Tools monthly

Global: Zendy Free Plan

We present new optical emission-line images of the young SNR 1E 0102-7219(E0102) in the SMC obtained with the HST Advanced Camera for Surveys (ACS).E0102 is a member of the oxygen-rich class of SNRs showing strong oxygen, neon, and other metal-line emissions in its optical and X-ray spectra, and anabsence of H and He. The progenitor of E0102 may have been a Wolf-Rayet starthat underwent considerable mass loss prior to exploding as a Type Ib/c orIIL/b SN. The ejecta in this SNR are fast-moving (V > 1000 km/s) and emit asthey are compressed and heated in the reverse shock. In 2003, we obtainedoptical [O III], H-alpha, and continuum images with the ACS Wide Field Camera.The [O III] image captures the full velocity range of the ejecta, and showsconsiderable high-velocity emission projected in the middle of the SNR that wasDoppler-shifted out of the narrow F502N bandpass of a previous Wide Field andPlanetary Camera 2 image from 1995. Using these two epochs separated by ~8.5years, we measure the transverse expansion of the ejecta around the outer rimin this SNR for the first time at visible wavelengths. From proper-motionmeasurements of 12 ejecta filaments, we estimate a mean expansion velocity forthe bright ejecta of ~2000 km/s and an inferred kinematic age for the SNR of\~2050 +/- 600 years. The age we derive from HST data is about twice thatinferred by Hughes et al.(2000) from X-ray data, though our 1-sigma error barsoverlap. Our proper-motion age is consistent with an independent opticalkinematic age derived by Eriksen et al.(2003) using spatially resolved [O III]radial-velocity data. We derive an expansion center that lies very close toX-ray and radio hotspots, which could indicate the presence of a compactremnant (neutron star or black hole).

Optical Structure and Proper‐Motion Age of the Oxygen‐rich Supernova Remnant 1E 0102−7219 in the Small Magellanic Cloud