This is my first mono RGB image with new equipment purchased around Christmas 2025. It includes an ASI2600MM Pro, ZWO 7×36mm EFW and Antlia Edge 4.5nm LRGB and SII, Ha and OIII filters. This is only a RGB image. I did shoot several Ha 600 second subs but didn’t see any significant nebulosity. Processed with PixInsight. Nothing fancy. Imaged from my Bortle 8.5 backyard. C&C Welcome.

Messier 35 also known as NGC 2168 or the Shoe-Buckle Cluster, is a relatively close open cluster of stars in the west of Gemini. It was discovered by Philippe Loys de Chéseaux around 1745 and independently discovered by John Bevis before 1750. It’s scattered over part of the sky almost the size of the full moon and is 2,970 light-years away. The compact open cluster NGC 2158 lies directly southwest of it.

Leonard & Merritt (1989) computed the mass of M35 using a statistical technique based on proper motion velocities of its stars. The mass within the central 3.75 parsecs (12.2 ly) was found to be between 1600 and 3200 solar masses, consistent with the mass of a realistic stellar population within the same radius. Bouy et al. in 2015 found a mass of around 1,600 M☉ within the central 27.5' × 27.5′. There are 305 stars that can be intrinsically shown to be extremely likely to be members and up to 4,349 averaging the 50% membership probability, from the kinematic (such as parallax and proper motion) and spectral data published before 2015. The cluster's metallicity is [Fe/H] = −0.21±0.10, where −1 would be ten times less metallic than the sun.