Located in the constellation Cygnus, the emission nebula Sh2-115 stretches across a rich region of the Milky Way filled with glowing gas, dark filaments, and young stars. This vast cloud of ionized hydrogen lies about 7,500 light-years away and is energized by the ultraviolet radiation from nearby hot, massive stars. Complex pillars and wisps of interstellar material sculpted by stellar winds give this nebula a distinctly textured appearance, revealing the dynamic processes at play within star-forming regions of our galaxy.

This detailed narrowband image combines 100×10-minute exposures in H-alpha (7nm), 70×10-minute in OIII (3nm), and 38×10-minute in SII (3nm). The resulting SHO composition highlights subtle differences in chemical composition and temperature, mapping hydrogen in red, oxygen in blue, and sulfur in gold. Together they unveil the intricate cosmic structures hidden within Sh2-115.

This bi-color image of the California Nebula is produced by combining data from two specific wavelengths: Hydrogen Alpha (Ha) and doubly ionized Oxygen (OIII). The red hues represent areas rich in ionized hydrogen (Ha emissions), indicative of regions with active star formation. The bluish-green tones correspond to OIII emissions, revealing areas with doubly ionized oxygen. This data aids astronomers in studying the nebula's chemical composition, ionization processes, and the influence of massive stars on its structure. The application of Ha and OIII imaging allows for a more detailed understanding of the dynamic astrophysical processes at play within this interstellar cloud located in the Perseus Arm of our Milky Way galaxy.