IC 1590
 | |
| Offener Sternhaufen im NCG 281 | |
| AladinLite | |
| Sternbild | Kassiopeia |
| Position Äquinoktium: J2000.0 | |
|---|---|
| Rektaszension | 00h 52m 50,2s [1] |
| Deklination | +56° 38′ 35″ [1] |
| Erscheinungsbild | |
| Physikalische Daten | |
| Zugehörigkeit | Milchstraße, evtl. eingebettet in NGC 281 |
| Geschichte | |
| Entdeckt von | Guillaume Bigourdan |
| Entdeckungszeit | 31. Oktober 1899 |
| Katalogbezeichnungen | |
| IC 1590 • ESO 51-SC17 • | |
IC 1590 ist ein offener Sternhaufen im Sternbild Kassiopeia, der sich in der Nebelzone von NGC 281 befindet. 279 Sterne mit Helligkeiten kleiner oder gleich 17 sind innerhalb oder in der Nähe des Haufens sichtbar. Das Alter des Haufens wird auf 3,5 Millionen Jahre geschätzt, womit er im Vergleich zu anderen Sternsystemen relativ jung ist. Im Inneren des Haufens befindet sich ein Mehrfachsternsystem, das Licht aussendet, das dazu beiträgt, dass der Staub in NGC 281 leuchtet.
Das Objekt wurde am 31. Oktober 1899 von Guillaume Bigourdan entdeckt.[2]
Einzelnachweise
Auf dieser Seite verwendete Medien
The Pacman Nebula.jpg
This composite image of NGC 281 contains X-ray data from Chandra, in purple, with infrared observations from Spitzer, in red, green, blue. NGC 281 is typically divided into two subregions: the region in the upper middle of the image, which is surrounded by the purple 10-million-degree gas, and a younger region in the lower part of the image. There is evidence that the formation of a cluster, appearing in a beige cloud to the lower right, was triggered by a previous generation of star formation. Also, astronomers have found some isolated star formation on the left side of the image that appears to have been occurring at the same time as star formation in other regions of the cluster. This supports the idea that something externally triggered the "baby boom" of stars in NGC 281.
This composite image of NGC 281 contains X-ray data from Chandra, in purple, with infrared observations from Spitzer, in red, green, blue. NGC 281 is typically divided into two subregions: the region in the upper middle of the image, which is surrounded by the purple 10-million-degree gas, and a younger region in the lower part of the image. There is evidence that the formation of a cluster, appearing in a beige cloud to the lower right, was triggered by a previous generation of star formation. Also, astronomers have found some isolated star formation on the left side of the image that appears to have been occurring at the same time as star formation in other regions of the cluster. This supports the idea that something externally triggered the "baby boom" of stars in NGC 281.