GREAT [CII] and CO observations of the BD+40{\deg}4124 region

TL;DR

This study uses high-resolution observations of CO and [CII] lines in the BD+40°4124 region to analyze the emission sources, revealing details about the nebula, star, and outflows with implications for star formation processes.

Contribution

First high-resolution observations of CO J=13→12 and [CII] in the BD+40°4124 region, distinguishing emission sources and dynamics of the nebula and young stars.

Findings

[CII] emission is strong in the reflection nebula around BD+40°4124.

[CII] emission suggests ionized gas expansion near the B2 star.

Faint CO emission indicates possible accretion disk around BD+40°4124.

Abstract

The BD+40\degree4124 region was observed with high angular and spectral resolution with the German heterodyne instrument GREAT in CO J = 13 \rightarrow 12 and [CII] on SOFIA. These observations show that the [CII] emission is very strong in the reflection nebula surrounding the young Herbig Ae/Be star BD+40\degree4124. A strip map over the nebula shows that the [CII] emission approximately coincides with the optical nebulosity. The strongest [CII] emission is centered on the B2 star and a deep spectrum shows that it has faint wings, which suggests that the ionized gas is expanding. We also see faint CO J = 13 \rightarrow 12 at the position of BD+40\degree4124, which suggests that the star may still be surrounded by an accretion disk.We also detected [CII] emission and strong CO J = 13 \rightarrow 12 toward V1318 Cyg. Here the [CII] emission is fainter than in BD+40\degree4124 and appears to come from the outflow, since it shows red and blue wings with very little emission at the systemic velocity, where the CO emission is quite strong. It therefore appears that in the broad ISO beam the [CII] emission was dominated by the reflection nebula surrounding BD+40\degree4124, while the high J CO lines originated from the adjacent younger and more deeply embedded binary system V1318 Cyg.