| NGC 2527 | |
|---|---|
 | |
| Observation data (J2000epoch) | |
| Right ascension | 08h 04m 58s[1] |
| Declination | −28° 08′ 48″[1] |
| Distance | 1,960ly (601pc[2]) |
| Apparent magnitude (V) | 6.5[1] |
| Apparent dimensions (V) | 20' |
| Physical characteristics | |
| Mass | 740[3] M☉ |
| Estimated age | 445 million years[2] 810 million years[4] |
| Other designations | NGC 2520,Cr 174 |
| Associations | |
| Constellation | Puppis |
| See also:Open cluster,List of open clusters | |
NGC 2527 (also catalogued asNGC 2520) is anopen cluster in the constellationPuppis. It was discovered byWilliam Herschel on December 9, 1784. The cluster was also observed byJohn Herschel on January 7, 1831. He also observed it on February 5, 1837, identifying it as a different object, which was catalogued as NGC 2520. It is a poor cluster and with no central concentration, withTrumpler class III1p.[5]
The core radius of the cluster is 1 parsec (3.3 light years), while the tidal radius is 5.1 parsecs (17 light years) and represents the average outer limit of NGC 2527, beyond which a star is unlikely to remain gravitationally bound to the cluster core.[4] 37 stars, probable members of the cluster, are located within the central part of the cluster and 96 probable members are located within the angular radius of the cluster.[4] The brightest star members areA-type stars, with the brightest being an A3 star with magnitude 9.38.[6] In the cluster has been detected onewhite dwarf, with mass0.77±0.03 M☉. Its age is estimated to be441±188 years and the progenitor star has initial mass circa 3.1M☉.[7] Theturn-off mass of the cluster is at 2.8M☉. Themetallicity of the cluster is -0.01, similar to the solar one.[8]
NGC 2527 lies 3.8 degrees south ofRho Puppis and can be seen with 50mmbinoculars as a moderately large, bright patch of haze, with no stars visible with direct vision.[9]
