NGC 5643
| Galaxie Daten von NGC 5643 | |
|---|---|
 | |
| Aufnahme des Hubble-Weltraumteleskops | |
| AladinLite | |
| Sternbild | Wolf |
| Position Äquinoktium: J2000.0, Epoche: J2000.0 | |
| Rektaszension | 14h 32m 40,7s[1] |
| Deklination | −44° 10′ 28″[1] |
| Erscheinungsbild | |
| Morphologischer Typ | SAB(rs)c / Sy2[1] |
| Helligkeit (visuell) | 10,2 mag[2] |
| Helligkeit (B-Band) | 10,9 mag[2] |
| Winkelausdehnung | 4,7′ × 4,2′[2] |
| Positionswinkel | 153°[2] |
| Flächenhelligkeit | 13,3 mag/arcmin²[2] |
| Physikalische Daten | |
| Rotverschiebung | 0.003999 ± 0.000007[1] |
| Radialgeschwindigkeit | (1199 ± 2) km/s[1] |
| Hubbledistanz H0 = 73 km/(s • Mpc) | (48 ± 3) · 106 Lj (14,6 ± 1,0) Mpc [1] |
| Durchmesser | 65.000 Lj |
| Geschichte | |
| Entdeckung | John Herschel |
| Entdeckungsdatum | 1. Juni 1834 |
| Katalogbezeichnungen | |
| NGC 5643 • PGC 51969 • ESO 272-G016 • MCG -07-30-003 • IRAS 14294-4357 • 2MASX J14324077-4410285 • AM 1429-435 • GC 3909 • h 3572 • Dun 469? | |
NGC 5643 ist eine Balkenspiralgalaxie mit aktivem Galaxienkern vom Hubble-Typ SAB(rs)c im Sternbild Wolf am Südsternhimmel. Sie ist schätzungsweise 48 Millionen Lichtjahre von der Milchstraße entfernt, hat einen Scheibendurchmesser von etwa 65.000 Lj und ist als Seyfert-2-Galaxie klassifiziert.
Das Objekt wurde am 1. Juni 1834 von John Herschel entdeckt.[3]
Literatur
- König, Michael & Binnewies, Stefan (2019): Bildatlas der Galaxien: Die Astrophysik hinter den Astrofotografien, Stuttgart: Kosmos, S. 162
Weblinks
- Spirals Are In This Season
- SIMBAD Astronomical Database
- ESO: Verborgen im Staub 28. Mai 2018
Einzelnachweise
Auf dieser Seite verwendete Medien
Autor/Urheber: Judy Schmidt from USA, Lizenz: CC BY 2.0
Home to an another active nucleus, NGC 5643 is a picturesque barred spiral galaxy with spiral arms intertwined in such a way to make them difficult to count. It is similar in size to our own Milky Way, and one might surmise that it looks somewhat similar to our home galaxy, if not for the active nucleus. Older, yellowish colored stars gather in the center and along the bar, while younger stars and regions of star formation populate the periphery, giving rise to the variation in colors for the image. Dark streaks of umber trace dust in the galaxy's complicated arms. Even though this image is mostly near-infrared, the colors look similar to a traditional visible light image.
Due to the relative brightness of the core, it was necessary to create a second image of the galaxy detailing the nuclear region. That is available here: flickr/p/25mnGPD
Data from the following proposals were used to compose this image: The Hubble Constant to 1%: Physics beyond LambdaCDM The Fueling of Active Nuclei: Why are Active Galaxies Active?
Note there was a data gap just south of the nucleus where no WFC3 data were available. Some older WF/PC2 data were used to fill that in.
Red: WFC3/IR F160W Green: WFC3/UVIS F814W Blue: WFC3/UVIS F555W
North is NOT up. It is 31.91° counter-clockwise from up.