| Credit: | Hubble Space Telescope |
| NGC 330 | |
| Constellation: | Tucana |
| Epoch: | J2000 |
| Ra: | [1] |
| Constellation Name: | Tucana |
| Dist Ly: | 182000 |
| Appmag V: | 9.60 |
| Size V: | 2.8′ × 2.5′[2] |
| Age: | Gyr |
| Names: | ESO 029-SC 024. |
NGC 330 is an open cluster in the Small Magellanic Cloud. It is located in the constellation Tucana. It was discovered on 1 August 1826 by James Dunlop. It was described by Dreyer as "a globular cluster, very bright, small, a little extended, stars from 13th to 15th magnitude."[3] At an aperture of 31.0 arcseconds, the apparent V-band magnitude is 9.60, but at this wavelength, it also has 0.36 magnitudes of interstellar extinction.
NGC 330 is quite young, at about 40 million years old, and has a large proportion of Be stars. Its estimated mass is, and its total luminosity is, leading to a mass-to-luminosity ratio of 0.06 /.[4] All else equal, older star clusters have higher mass-to-luminosity ratios; that is, they have lower luminosities for the same mass.[4] About 34% of the massive star population in NGC 330 is estimated to be in a close binary star system; this is lower than clusters in the Large Magellanic Cloud and the Milky Way, but it is unknown if this is because NGC 330 is metal-poor or is older than the compared clusters.[5]