NGC 121
| Kugelsternhaufen NGC 121 | |
|---|---|
 | |
| Aufnahme des Kugelsternhaufen mit dem Hubble-Weltraumteleskop. | |
| AladinLite | |
| Sternbild | Tukan |
| Position Äquinoktium: J2000.0, Epoche: J2000.0 | |
| Rektaszension | 00h 26m 49,0s [1] |
| Deklination | −71° 32′ 10″ [1] |
| Erscheinungsbild | |
| Helligkeit (visuell) | 11,24 mag |
| Helligkeit (B-Band) | 11,2 mag |
| Winkelausdehnung | 3/2 [2] |
| Farbexzess E(B-V) (Rötung) | 0,037 mag [3] |
| Physikalische Daten | |
| Zugehörigkeit | Kleine Magellansche Wolke |
| Entfernung | ca. 210.000 Lj |
| Masse | ca. 350.000 M☉ |
| Durchmesser | 175 Lj |
| Kernradius | 9,61″ ± 0,35″ |
| Alter | (10,6 ± 0,5) Mrd. Jahre |
| Metallizität [Fe/H] | −1,71 ± 0,10 |
| Geschichte | |
| Entdeckung | John Herschel |
| Entdeckungsdatum | 20. September 1835 |
| Katalogbezeichnungen | |
| NGC 121 • ESO 50-12 • GC 58 • Lindsay 10 • Kron 2 | |
NGC 121 ist die Bezeichnung für einen Kugelsternhaufen nahe der Kleinen Magellanschen Wolke im Sternbild Tukan. NGC 121 ist im Unterschied zu 47 Tucanae ein Mitglied derselben. Er hat einen Durchmesser von 3′ und eine scheinbare Helligkeit von 11,2 mag. Der Kugelsternhaufen ist etwa 200.000 Lichtjahre vom Sonnensystem entfernt und hat einen Durchmesser von etwa 175 Lichtjahren. Er ist mit einem geschätzten Alter von etwa 11 Milliarden Jahren der älteste Kugelhaufen in der Kleinen Magellanschen Wolke[4].
NGC 121 wurde am 20. September 1835 von dem britischen Astronomen John Frederick William Herschel entdeckt.
Weblinks
Einzelnachweise
- ↑ SIMBAD database, operated at CDS, Strasbourg, France. Abgerufen am 9. März 2008 (englisch).
- ↑ Students for the Exploration and Development of Space. Abgerufen am 9. März 2008 (englisch).
- ↑ NASA/IPAC EXTRAGALACTIC DATABASE
- ↑ http://cseligman.com/text/atlas/ngc1.htm#121
Auf dieser Seite verwendete Medien
Autor/Urheber: Credit: ESA/Hubble & NASA Acknowlegement: Stefano Campani, Lizenz: CC BY 3.0
The oldest cluster in its cloud
This image shows NGC 121, a globular cluster in the constellation of Tucana (The Toucan). Globular clusters are big balls of old stars that orbit the centres of their galaxies like satellites — the Milky Way, for example, has around 150.
NGC 121 belongs to one of our neighbouring galaxies, the Small Magellanic Cloud (SMC). It was discovered in 1835 by English astronomer John Herschel, and in recent years it has been studied in detail by astronomers wishing to learn more about how stars form and evolve.
Stars do not live forever — they develop differently depending on their original mass. In many clusters, all the stars seem to have formed at the same time, although in others we see distinct populations of stars that are different ages. By studying old stellar populations in globular clusters, astronomers can effectively use them as tracers for the stellar population of their host galaxies. With an object like NGC 121, which lies close to the Milky Way, Hubble is able to resolve individual stars and get a very detailed insight.
NGC 121 is around 10 billion years old, making it the oldest cluster in its galaxy; all of the SMC's other globular clusters are 8 billion years old or younger. However, NGC 121 is still several billions of years younger than its counterparts in the Milky Way and in other nearby galaxies like the Large Magellanic Cloud. The reason for this age gap is not completely clear, but it could indicate that cluster formation was initially delayed for some reason in the SMC, or that NGC 121 is the sole survivor of an older group of star clusters.
This image was taken using Hubble’s Advanced Camera for Surveys (ACS). A version of this image was submitted to the Hubble’s Hidden Treasures image processing competition by contestant Stefano Campani.
Credit:
ESA/Hubble & NASA Acknowlegement: Stefano Campani
About the Object
Name: NGC 121
Type: • Milky Way : Star : Grouping : Cluster : Globular
• X - Stars Images/Videos
Distance: 200000 light years
Colours & filters Band Wavelength Telescope
Optical V 555 nm Hubble Space Telescope ACS Infrared I 814 nm Hubble Space Telescope ACS.