Observed Spectral profile of CED211


Date & Time: Dec 10 2021, from 19:00 to 19:09 JST(+0900)
Composed 4 shots with 3 minutes exposed
Optical: Meade 25cm(10") Schmidt Cassegrain (f=2500mm, F10.0)
with SBIG DSS7 Spectrometer
Auto-guided with Meade LX200 Equatorial & Lacerta M-GEN
Cooled CCD Camera: SBIG ST-402ME (Temp.: -25°C)
Location: Ooizumi, Hokuto city, Yamanashi pref.

Upper strip: taken spectrogram, Lower strip: stretched 3-pixel-width & pseudo-colored image


This page shows a spectrogram of the CED211 and an intensity profile provided from it. The profile reveals characteristic emission lines commonly found in planetary nebulae, such as the Balmer series from Hα to Hδ originating from hydrogen atoms, two O III lines from ionized oxygen atoms, as well as weaker lines from ionized nitrogen (N II) and neutral helium (He I). Additionally, prominent broad absorption bands of titanium oxide (TiO) are observed, typical of M-type stars. It is suggested that these emission lines arise from interstellar gas expelled by the star, while the absorption bands are attributed to the star itself, with material expelled from its outer layers.

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