Credit: Aldo Zanetti
Astronomical and Imaging Data
| RA: | 19h 18m 02.10s |
| DEC: | +18° 34′ 18.0″ |
| MAG: | 13.22 |
| Diameter: | 4′ |
| Const: | Sge |
| OTA | Celestron 9.25 Edge HD |
| Focal Length | 2350 |
| Camera | ASI1600MM |
| Site | Po Plain, Italy |
| Sky Quality | Bortle 7 |
Useful Informations
Palomar 10 is a faint and sparse globular cluster in the constellation Sagitta. It’s one of the Palomar globular clusters, a group of very faint clusters discovered in the 1950s that are heavily obscured by dust in the Milky Way’s galactic plane.
Key Physical Properties
Palomar 10 is located approximately 19,200 light-years from Earth, but it’s situated very close to the galactic plane, at a galactic latitude of only 2.72 degrees. This proximity to the Milky Way’s disk means its light is heavily reddened and obscured by interstellar dust, making it difficult to observe. For this reason, it was only discovered in 1955.
It’s a relatively sparse cluster, containing fewer stars and being less centrally concentrated than more typical globular clusters. Its classification as a globular cluster was uncertain for a time, with some considering it a very old open cluster due to its diffuse nature. However, its age and low metallicity have since confirmed its status as a globular cluster.
Stellar and Chemical Composition
Palomar 10 is considered a metal-poor stellar system, a common trait of globular clusters formed in the early universe. Its metallicity, while low, is not as low as some of the oldest globular clusters. This, combined with its location near the galactic disk, suggests it may have a slightly different formation history.
Due to its faintness and the obscuring dust, detailed studies of its stellar populations and chemical abundances are challenging. However, the existing research confirms its classification as a true globular cluster.