Table 4: Emission lines in the complete spectrum (ejecta and circumstellar ring combined corresponding to 281 spaxels) in K. The spectral resolution is 67 km s-1 in the K 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)
2.00855 275 239 229 5 $\dagger$[Fe II] a4P1/2-a2P1/2 2.0067
2.01696 272 327 317 8 * [Fe II] a2G9/2-a2H9/2 2.0151
2.04779 259 293 285 8 $\dagger$[Fe II] a4P5/2-a2P3/2 2.0460
2.06003 275 291 283 108 $\dagger$He I 2s1S-2p1P0 2.0581
2.11412 279 369 363 8 *He I 1s3p-1s4s 2.1121
2.13462 258 267 258 3 $\dagger$[Fe II] a4P3/2-a2P3/2 2.1328
2.16331   416 411 4 *  
Which could be part of a broad component of Br$\gamma $ (not seen on the red side of Br$\gamma $).
2.16754 277 291 283 58 $\dagger H {\sc i}$ Br$\gamma $ 2.1655
2.19052   575 571 3 *  
2.20659 255 381 375 2 *Na I $2\rm p^65p{-} 2p^69s$ 2.2047
2.20659 -58 381 375 2 or $\dagger$ Na I $4\rm s^2S{-}4p^2P^o$ 2.2070
2.22026   365 359 4 *  
2.22593 290 243 234 5 * [Fe II] a2G9/2-a2H11/2 2.2238
2.24580 286 534 530 4 $\dagger$[Fe II] a4P1/2-a2P3/2 2.2436
Blend? The line transition probability for [Fe II] does not support this large flux. Furthermore large $\sigma_{\rm deconv}$.
2.25525   452 447 3 *  
2.31030 304 403 397 3 *Ni II $\rm 3p^63d^8(^3F)4s{-}3p^63d^8(^3F)4s$ 2.3079
2.32381 291 284 276 5 *O I $\rm 2s^22p^3(^2D)3s{-}2s^22p^3(^4S)5f$ 2.3215
The lines marked with $\dagger$ have been observed previously for this object.
The lines marked with * are new for this object or have a new identification.
The lines 2.24-2.32 $\mu $m were observed in Meikle et al. (1993) as a blended unidentified feature.

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