IC 2144 is a small reflection nebula located in the zone of avoidance near the Galactic anticenter .
It has been investigated here largely on the basis of Keck/HIRES optical spectroscopy ( R \approx 48,000 ) and a SpeX spectrogram of the near-IR ( R = 2000 ) obtained at the NASA IRTF .
The only star in the nebula that is obvious in the optical or near-IR is the peculiar emission-line object MWC 778 ( V = 12.8 ) , which resembles a T Tauri star in some respects .
What appear to be F- or G-type absorption features are detectable in its optical region under the very complex emission line spectrum ; their radial velocity agrees with the CO velocity of the larger cloud in which IC 2144 is embedded .
There are significant differences between the spectrum of the brightest area of the nebula and of MWC 778 , the presumed illuminator , an issue discussed in some detail .
The distance of IC 2144 is inferred to be about 1.0 kpc by reference to other star-forming regions in the vicinity .
The extinction is large , as demonstrated by [ Fe ii ] emission line ratios in the near-IR and by the strength of the diffuse interstellar band spectrum ; a provisional value of A _ { V } of 3.0 mag was assumed .
The SED of MWC 778 rises steeply beyond about 1 \mu m , with a slope characteristic of a Class I source .
Integration of the flux distribution leads to an IR luminosity of about 510 L _ { \sun } .
If MWC 778 is indeed a F- or G-type pre–main-sequence star several magnitudes above the ZAMS , a population of faint emission H \alpha stars would be expected in the vicinity .
Such a search , like other investigations that are recommended in this paper , has yet to be carried out .