2012
DOI: 10.1088/0004-637x/757/2/126
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Nucleosynthetic Layers in the Shocked Ejecta of Cassiopeia A

Abstract: We present a 3-dimensional analysis of the supernova remnant Cassiopeia A using high resolution spectra from the Spitzer Space Telescope. We observe supernova ejecta both immediately before and during the shock-ejecta interaction. We determine that the reverse shock of the remnant is spherical to within 7%, although the center of this sphere is offset from the geometric center of the remnant by 810 km s −1 . We determine that the velocity width of the nucleosynthetic layers is ∼1000 km s −1 over 4000 square ar… Show more

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Cited by 26 publications
(27 citation statements)
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“…Figures 3(a) and (b) show that the velocity structure of the [Fe II]-lineemitting gas in Slit 4 is "arc"-like, suggesting that the slit crosses a portion of an expanding shell. This is consistent with the result of previous studies that the main ejecta shell is a thin shell expanding at 4000-5000 km s −1 (e.g., DeLaney et al 2010;Isensee et al 2012). In Slit 4, therefore, we have both blue and redshifted Fe knots along a given sight line, and the uncertainty due to different sight lines disappears.…”
Section: Note Insupporting
confidence: 92%
“…Figures 3(a) and (b) show that the velocity structure of the [Fe II]-lineemitting gas in Slit 4 is "arc"-like, suggesting that the slit crosses a portion of an expanding shell. This is consistent with the result of previous studies that the main ejecta shell is a thin shell expanding at 4000-5000 km s −1 (e.g., DeLaney et al 2010;Isensee et al 2012). In Slit 4, therefore, we have both blue and redshifted Fe knots along a given sight line, and the uncertainty due to different sight lines disappears.…”
Section: Note Insupporting
confidence: 92%
“…They find that silicates are the prevalent dust in regions dominated by Ar II and Ar III lines, while alumina dust best characterises the regions rich in Ne II emission lines. Because Cas A has kept some memory of the initial A132, page 8 of 16 chemical stratification of its SN progenitor (DeLaney et al 2010;Isensee et al 2012;Milisavljevic & Fesen 2013), this result is not surprising. As shown in BS14, alumina is the primary dust component in the Ne-rich zone 2, with a mass that is about eight times that of silicates in this zone.…”
Section: Current Sputtering In Cas Amentioning
confidence: 98%
“…However, it is worth pointing out a few drawbacks with the initial model and subsequent studies. Firstly, an SN ejecta is not fully-mixed but shows some stratification in its chemical composition, as indicated by atomic line emission in the remnant phase (Isensee et al 2012). The SN models with 18−20 M progenitors that were considered by Bianchi & Schneider produce a large dust mass (∼0.2−0.4 M ) because the ejecta is fully-mixed and CNT is used to model dust formation, for which the above caveats apply.…”
Section: Comparison With Existing Studiesmentioning
confidence: 99%
See 1 more Smart Citation
“…In this section, we derive Spitzer mid-infrared (MIR) line fluxes to be compared with the [Si I] 1.645 µm flux. The entire area of Cas A had been mapped by the Spitzer Space Telescope with two Infrared Spectrograph (IRS) low-resolution modules (R = 60-130) SL (5-15 µm) and LL (15-38 µm) (Smith et al 2009), while the central area surrounding the explosion center had been also mapped with two high-resolution (R ∼ 600) modules SH (10-20 µm) and LH (20-35 µm) (Isensee et al 2010(Isensee et al , 2012. The data were downloaded from the Spitzer Heritage Archive 2 .…”
Section: Spitzer Mid-infrared Line Fluxesmentioning
confidence: 99%