Table 2: Emission lines of the integrated spectrum (ejecta and circumstellar ring combined corresponding to the central 281 spaxels) in the J band. The spectral resolution is 150 km s-1 in the J band. Errors for the values listed in the table are given either in the text or in Table 1.
$\lambda_{\rm obs}$ $v_{\rm obs}$ $\sigma_{\rm obs}$ $\sigma_{\rm deconv}$ Flux Identification $\lambda_{\rm air}$
($\mu $m) (km s-1) (km s-1) (km s-1) (10-16 erg s-1 cm-2)   ($\mu $m)
1.253885 408 431 404 14 *[Fe II] a6D3/2-a4D1/2 1.2521
1.25385 261 431 404 14 *He I 1s3s-1s4p(3S-3P) 1.2528
Blend? The line transition probability for [Fe II] does not support this large flux. Furthermore large $\sigma_{\rm deconv}$.
1.25787 277 200 132 69 $\dagger$[Fe II] a6D9/2-a4D7/2 1.2567
1.27169 315 236 182 7 $\dagger$[Fe II] a6D1/2-a4D1/2 1.2703
1.27983 245 305 266 43 $\dagger$[Fe II] a6D3/2-a4D3/2 1.2788
1.27983 310 305 266 43 * He I 1s3d-1s5f(3D-3F) 1.2785
Blend? The line transition probability for [Fe II] does not support this large flux. Furthermore large $\sigma_{\rm deconv}$.
1.28300 277 281 238 367 $\dagger$Pa$\beta $ 1.2818
1.29562 311 190 117 18 $\dagger$[Fe II] a6D5/2-a4D5/2 1.2943
1.30651 302 253 204 12 *N I 1.3052
1.32178 277 166 71 23 $\dagger$[Fe II] a6D7/2-a4D7/2 1.3206
1.32901 226 339 304 10 $\dagger$[Fe II] a6D3/2-a4D5/2 1.3278
The lines marked with $\dagger$ have been observed previously for this object in Meikle et al. (1993).
The lines marked with * are new for this object or have a new identification.

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