NGC 957 (also Cr 28 and OCl 362) is a magnitude +7.6 open star cluster located 5920 light-years away in the constellation Perseus.
The cluster was discovered by British astronomer John Herschel using a 47.5 cm (18.7 inch) reflecting telescope at Windsor Road, Slough, on the 9th December 1831.
NGC 957 is sparsely populated, and its distance is estimated at about 1815 parsecs (5920 light years) away in the inner edge of the Perseus Arm. Its diameter is about 4.4 parsecs. In the same region are the IC 1805 and IC 1848 nebulae, the Double Cluster, and many bright young stars belonging to some OB associations. All studies indicate that the cluster is at a very young age, forming about 4-11 million years ago. It contains several massive blue stars, among which there are two Be stars, about to leave the main sequence stage and evolve to the giant stage. Research carried out in order to identify variable stars in the direction of this cluster have uncovered 10 eclipsing binaries, 3 pulsating and 1 semiregular variable. The cluster is located in the north-western part of the constellation, about 1.5° towards the east of the famous Double Cluster in Perseus, lying in a stellar field heavily obscured by interstellar dust. Through a pair of 10x50 binoculars, two stars of magnitude 8 surrounded by a slight haziness can be seen; a 100mm telescope can resolved fifteen stars of magnitude 12, located mainly to the north of the two brightest stars. With a 200mm telescope it is possible to identify additional components. The declination of this cluster favours observers in the northern hemisphere. The cluster is circumpolar at mid latitudes. The best time to observation is in the evening is between October and March.
Right Ascension 02h 33m 21.0s, Declination +57° 33' 36"
