NGC 6441
| NGC 6441 | |
|---|---|
 |
|
| Observation data (J2000 epoch) | |
| Constellation | Scorpius |
| Right ascension | 17h 50m 13.06s |
| Declination | −37° 03′ 05.2″ |
| Distance | 44 kly (13.5 kpc) |
| Apparent magnitude (V) | 7.2 |
| Apparent dimensions (V) | 9.6′ |
| Physical characteristics | |
| Mass | 1.6×106 M☉ |
| Radius | 4.8 |
| Tidal radius | 88.8 ly (27.23 pc) |
| Metallicity | = −0.53dex |
| Estimated age | 13−13.7 Gyr |
![{\displaystyle {\begin{smallmatrix}\left[{\ce {Fe}}/{\ce {H}}\right]\end{smallmatrix}}}](https://wikimedia.org/api/rest_v1/media/math/render/svg/4c0821bd80891e071c08e7c7ee8e022baedf522c)
NGC 6441 is the New General Catalogue identifier for a globular cluster in the southern constellation of Scorpius. It was discovered by the Scottish astronomer James Dunlop on May 13, 1826, who described it as "a small, well-defined rather bright nebula, about 20″ in diameter". The cluster is located 5 arc minutes east-northeast of the star G Scorpii, and is some 44,000 light years from the Sun.
This is one of the most massive and luminous globular clusters in the Milky Way, with an estimated 1.6 million solar masses of stars. It is located in the bulge of the galaxy at a distance of 13 kilolight-years (3.9 kpc) from the core, and is considered metal "rich". That is, it has a relatively high abundance of elements with higher mass than helium. The core region of the cluster subtends an angle of 0.11 arc minutes, compared to the half-mass radius of 0.64 arc minutes. The density of stars in the core region is indicated by the luminosity density: 5.25 L⊙ pc−3. The cluster has a half-light radius of 7.1 ly (2.18 pc).
This cluster has an abnormally large number of RR Lyrae variables—68 candidates as of 2006, and their periods are longer than is typical for their respective metallicities. (The mean period for the cluster's RRab stars is 0.759 day.) There are also several type II Cepheid stars, which is unusual given the high metallicity of this cluster. Examination of the red giant branch section of the color-magnitude diagram suggests that there are at least two and possibly three distinct populations in the cluster. The brightest and higher temperature members of the red clump stars are more concentrated toward the center of the cluster. This group may be a helium-enriched second generation of stars.
...
Wikipedia