[ITAL]Chandra X-Ray Observatory[/ITAL] Arcsecond Imaging of the Young, Oxygen-rich Supernova Remnant 1E 0102.2−7219

Abstract

We present observations of the young, oxygen-rich supernova remnant 1E 0102.2-7219 taken by the Chandra X-Ray Observatory during its orbital activation and checkout phase. The boundary of the blast-wave shock is clearly seen for the first time, allowing the diameter of the remnant and the mean blast-wave velocity to be determined accurately. The prominent X-ray bright ring of material may be the result of the reverse shock encountering ejecta; the radial variation of O vii versus O viii emission indicates an ionizing shock propagating inward, possibly through a strong density gradient in the ejecta. We compare the X-ray emission with Australia Telescope Compact Array 6 cm radio observations (Amy & Ball) and with archival Hubble Space Telescope [O iii] observations. The ring of radio emission is predominantly inward of the outer blast wave, which is consistent with an interpretation of synchrotron radiation originating behind the blast wave but outward of the bright X-ray ring of emission. Many (but not all) of the prominent optical filaments are seen to correspond to X-ray bright regions. We obtain an upper limit of approximately 9x1033 ergs s-1 (3 sigma) on any potential pulsar X-ray emission from the central region.

SNR 1E 0102.2-7219 as an X-ray calibration standard in the 0.5−1.0 keV bandpass and its application to the CCD instruments aboardChandra,Suzaku,SwiftandXMM-Newton

“…It is the brightest SNR in X-rays in the Small Magellanic Cloud (SMC). E0102 has been extensively imaged by Chandra (Gaetz et al 2000;Hughes et al 2000) and XMM-Newton (Sasaki et al 2001). Figures 1 and 2 show images of E0102 with the relevant spectral extraction regions for each of the instruments included in this analysis.…”

“…Since our objective is calibration, we decided against using any of the available plasma emission models for several reasons. First, the Chandra results on E0102 (Flanagan et al 2004;Gaetz et al 2000;Hughes et al 2000) have shown there are significant spectral variations within the SNR, implying that the plasma conditions are varying throughout the remnant. Since the other missions considered Suzaku XIS 6' 50.7" Fig.…”

“…Figure 21 shows the temporal behavior of the line normalizations for the Swift-XRT WT data, with representative spectra (from 2009, 2011, 2013) This discrepant behavior appears to occur when the main emitting ring of the remnant (radius 10−18 ) falls on the CCD bad-column gaps. Gaetz et al (2000) and Flanagan et al (2004) show that the line components have different spatial origins, with O vii Heα r arising predominantly from the south-east quadrant of the ring, while Ne x Lyα r is more symmetrically formed in the ring. Individual snapshots are quite frequently placed with parts of the remnant on the CCD bad columns.…”

Spitzer Space Telescope Detection of the Young Supernova Remnant 1E 0102.2-7219

“…E0102 is not obviously detected at 70 mm, although there is a small bump present in the low-level IR contours exactly at the remnant's position. The measured flux density of the whole rem- Gaetz et al (2000). The X-ray image was smoothed to match the resolution of the IR image.…”

Kinematics of Supernova Remnants: Status of X-Ray Observations

“…Additionally, the X-ray ejecta are observed in Cas A with a range of ionization states and densities (Lazendic et al 2006), these values have implications for the further plasma evolution of the features and we may be able to directly measure the plasma-state changes in future observations. (Figure 3, right-most) clearly shows the outer blast wave and bright inner rings of H-and He-like O and Ne emission (Gaetz et al 2000). A proper motion measurement in the X-ray was made using ROSAT, Einstein, and Chandra data (Hughes et al 2000b), giving 0.10 % ±0.025% yr −1 and the FS velocity in Table 2.…”