NGC 3059
| Galaxie NGC 3059 | |
|---|---|
.jpg) (c) ESA/Hubble, CC BY 4.0 | |
| Aufnahme des Hubble-Weltraumteleskops | |
| AladinLite | |
| Sternbild | Kiel des Schiffs |
| Position Äquinoktium: J2000.0, Epoche: J2000.0 | |
| Rektaszension | 09h 50m 08,1s[1] |
| Deklination | −73° 55′ 20″[1] |
| Erscheinungsbild | |
| Morphologischer Typ | SB(rs)c[1] |
| Helligkeit (visuell) | 10,8 mag[2] |
| Helligkeit (B-Band) | 11,6 mag[2] |
| Winkelausdehnung | 3,6′ × 3,2′[1] |
| Positionswinkel | 70°[2] |
| Flächenhelligkeit | 13,3 mag/arcmin²[2] |
| Physikalische Daten | |
| Rotverschiebung | 0.004193 ± 0.000010[1] |
| Radialgeschwindigkeit | (1257 ± 3) km/s[1] |
| Hubbledistanz H0 = 73 km/(s • Mpc) | (47 ± 3) · 106 Lj (14,4 ± 1,0) Mpc [1] |
| Durchmesser | 50.000 Lj[3] |
| Geschichte | |
| Entdeckung | John Herschel |
| Entdeckungsdatum | 23. März 1835 |
| Katalogbezeichnungen | |
| NGC 3059 • PGC 28298 • ESO 037-007 • IRAS 09496-7341 • 2MASX J09500818-7355199 • SGC 094938-7341.2 • GC 1967 • h 3205 • HIPASS J0950-73 | |
NGC 3059 ist eine Balken-Spiralgalaxie vom Hubble-Typ SBbc und liegt im Sternbild Carina am Südsternhimmel. Sie ist schätzungsweise 47 Millionen Lichtjahre von der Milchstraße entfernt und hat einen Durchmesser von etwa 55.000 Lichtjahren.
Das Objekt wurde am 23. März 1835 von John Herschel entdeckt.[4]
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A broad and narrow galactic view (potw2423a).jpg
(c) ESA/Hubble, CC BY 4.0
This Picture of the Week features the barred spiral galaxy NGC 3059, which lies about 57 million light-years from Earth. The data used to compose this image were collected by Hubble in May 2024, as part of an observing programme that studied a number of galaxies. All the observations were made using the same range of filters: partially transparent materials that allow only very specific wavelengths of light to pass through. Filters are used extensively in observational astronomy, and can be calibrated to allow either extremely narrow or somewhat broader ranges of light through. Narrow-band filters are invaluable from a scientific perspective because certain light wavelengths are associated with specific physical and chemical processes. For example, under particular conditions, hydrogen atoms are known to emit red light with wavelength value of 656.46 nanometres. Red light at this wavelength is known as H-alpha emission, or the ‘H-alpha line’. It is very useful to astronomers because its presence acts as an indicator of certain physical processes and conditions; it is often a tell-tale sign of new stars being formed, for example.Thus, narrow-band filters calibrated to allow H-alpha emission through can be used to identify regions of space where stars are forming. Such a filter was used for this image, the narrow-band filter called F657N or the H-alpha filter. The F stands for filter, and the N stands for narrow. The numerical value refers to the peak wavelength (in nanometres) that the filter lets through. The eagle-eyed amongst you may have noticed that 657 is very close to the 656.46 H-alpha line’s wavelength. Data collected using five other filters contributed to this image as well, all of which were wide-band filters; meaning that they allow a wider range of light wavelengths through. This is less useful for identifying extremely specific lines (such as the H-alpha line) but still enables astronomers to explore relatively specific parts of the electromagnetic spectrum. In addition, collectively the information from multiple filters can be used to make beautiful images such as this one.[Image Description: A spiral galaxy seen face-on, so that its many arms and its glowing, bar-shaped core can be easily seen. The arms are filled with bluish patches of older stars, pink patches where new stars are forming, and dark threads of dust. A few bright stars with cross-shaped diffraction spikes lie in the foreground.]
(c) ESA/Hubble, CC BY 4.0
This Picture of the Week features the barred spiral galaxy NGC 3059, which lies about 57 million light-years from Earth. The data used to compose this image were collected by Hubble in May 2024, as part of an observing programme that studied a number of galaxies. All the observations were made using the same range of filters: partially transparent materials that allow only very specific wavelengths of light to pass through. Filters are used extensively in observational astronomy, and can be calibrated to allow either extremely narrow or somewhat broader ranges of light through. Narrow-band filters are invaluable from a scientific perspective because certain light wavelengths are associated with specific physical and chemical processes. For example, under particular conditions, hydrogen atoms are known to emit red light with wavelength value of 656.46 nanometres. Red light at this wavelength is known as H-alpha emission, or the ‘H-alpha line’. It is very useful to astronomers because its presence acts as an indicator of certain physical processes and conditions; it is often a tell-tale sign of new stars being formed, for example.Thus, narrow-band filters calibrated to allow H-alpha emission through can be used to identify regions of space where stars are forming. Such a filter was used for this image, the narrow-band filter called F657N or the H-alpha filter. The F stands for filter, and the N stands for narrow. The numerical value refers to the peak wavelength (in nanometres) that the filter lets through. The eagle-eyed amongst you may have noticed that 657 is very close to the 656.46 H-alpha line’s wavelength. Data collected using five other filters contributed to this image as well, all of which were wide-band filters; meaning that they allow a wider range of light wavelengths through. This is less useful for identifying extremely specific lines (such as the H-alpha line) but still enables astronomers to explore relatively specific parts of the electromagnetic spectrum. In addition, collectively the information from multiple filters can be used to make beautiful images such as this one.[Image Description: A spiral galaxy seen face-on, so that its many arms and its glowing, bar-shaped core can be easily seen. The arms are filled with bluish patches of older stars, pink patches where new stars are forming, and dark threads of dust. A few bright stars with cross-shaped diffraction spikes lie in the foreground.]