NGC 2439 | |
---|---|
![]() NGC 2439 (taken from Stellarium) | |
Observation data ( J2000 epoch) | |
Right ascension | 07h 40m 45.0s [1] |
Declination | −31° 41′ 36″ [1] |
Distance | 3.855 kpc (12.57 kly) [2] |
Apparent magnitude (V) | 6.9 [3] |
Apparent dimensions (V) | 10 ″ [4] |
Physical characteristics | |
Radius | 82 ± 23 ly (tidal) |
Other designations | Cr 158, C 0738-315 [3] |
Associations | |
Constellation | Puppis |
NGC 2439 is a sparse [5] open cluster of stars in the constellation Puppis. It has an apparent visual magnitude of 6.9, an angular size of 10 arcminutes, and is visible using a small telescope. [4] This is a young cluster with age estimates in the range of 20–300 million years. [6] [7] It has a tidal radius of approximately 82 light years. [2] No chemically peculiar stars have been found. [6]
Distance estimates to this cluster vary widely. [5] Piskunov and associates (2008) gave an estimate of 3,855 kpc. [2] A value in the range 3–4 kpc means the cluster lies well below the Galactic Plane. It is positioned in a hole in the Milky Way's gas and dust, with the reduced absorption resulting in a lower than expected extinction of 1.27 in visual magnitude. This result raises the question of whether this cluster actually exists. [5] It is positioned along the same line of sight as two groups of B-type supergiant stars. The nearer group is located at a distance of 1.03 kpc, while the second group is at 3.2 kpc. [8]
NGC 2439 | |
---|---|
![]() NGC 2439 (taken from Stellarium) | |
Observation data ( J2000 epoch) | |
Right ascension | 07h 40m 45.0s [1] |
Declination | −31° 41′ 36″ [1] |
Distance | 3.855 kpc (12.57 kly) [2] |
Apparent magnitude (V) | 6.9 [3] |
Apparent dimensions (V) | 10 ″ [4] |
Physical characteristics | |
Radius | 82 ± 23 ly (tidal) |
Other designations | Cr 158, C 0738-315 [3] |
Associations | |
Constellation | Puppis |
NGC 2439 is a sparse [5] open cluster of stars in the constellation Puppis. It has an apparent visual magnitude of 6.9, an angular size of 10 arcminutes, and is visible using a small telescope. [4] This is a young cluster with age estimates in the range of 20–300 million years. [6] [7] It has a tidal radius of approximately 82 light years. [2] No chemically peculiar stars have been found. [6]
Distance estimates to this cluster vary widely. [5] Piskunov and associates (2008) gave an estimate of 3,855 kpc. [2] A value in the range 3–4 kpc means the cluster lies well below the Galactic Plane. It is positioned in a hole in the Milky Way's gas and dust, with the reduced absorption resulting in a lower than expected extinction of 1.27 in visual magnitude. This result raises the question of whether this cluster actually exists. [5] It is positioned along the same line of sight as two groups of B-type supergiant stars. The nearer group is located at a distance of 1.03 kpc, while the second group is at 3.2 kpc. [8]