IC 4141
| Galaxie IC 4141 | |
|---|---|
 (c) ESA/Hubble, CC BY 4.0 | |
| Aufnahme von IC 4141 mithilfe des Hubble-Weltraumteleskops | |
| AladinLite | |
| Sternbild | Haar der Berenike |
| Position Äquinoktium: J2000.0, Epoche: J2000.0 | |
| Rektaszension | 13h 04m 07,731s [1] |
| Deklination | +19° 12′ 38,33″ [1] |
| Erscheinungsbild | |
| Morphologischer Typ | SR/b / LINER[2] |
| Helligkeit (visuell) | 16,2 mag[3] |
| Helligkeit (B-Band) | 17,0 mag[3] |
| Winkelausdehnung | 0.70 × 0.60[3] |
| Flächenhelligkeit | 15,1 mag/arcmin²[3] |
| Physikalische Daten | |
| Zugehörigkeit | Abell 1668[1] |
| Rotverschiebung | 0.066341 ± 0.000015[1] |
| Radialgeschwindigkeit | 19.889 ± 4 km/s[1] |
| Hubbledistanz H0 = 73 km/(s • Mpc) | (888 ± 62) · 106 Lj (272,3 ± 19,1) Mpc [1] |
| Durchmesser | 255.000 Lj[4] |
| Geschichte | |
| Entdeckung | Max Wolf |
| Entdeckungsdatum | 27. Januar 1904 |
| Katalogbezeichnungen | |
| IC 4141 • PGC 45147 • MCG +03-33-027 • 2MASX J13040769+1912384 • GALEXASC J130407.76+191236.7 • NVSS J130407+191238 • WISEA J130407.73+191238.4 | |
IC 4141 ist eine ringförmige Spiralgalaxie vom Hubble-Typ Sb mit aktivem Galaxienkern im Sternbild Coma Berenices am Nordsternhimmel. Sie ist schätzungsweise 888 Millionen Lichtjahre von der Milchstraße entfernt und hat einen Durchmesser von etwa 255.000 Lichtjahren. Vom Sonnensystem aus entfernt sich daie Galaxie mit einer errechneten Radialgeschwindigkeit von näherungsweise 19.900 Kilometern pro Sekunde.
Diese Ranken aus hellem Gas entstehen durch einen Prozess, der als Staudruck-Stripping bezeichnet wird, und ihre Ähnlichkeit mit baumelnden Tentakeln hat die Astronomen dazu veranlasst, die Galaxie als eine „Quallen-Galaxie“ zu bezeichnen.[5]
Das Objekt wurde am 27. Januar 1904 von Max Wolf entdeckt.[6]
Galaktisches Umfeld
| Nr. | Galaxie | Alternativname | Rek | Dek | Distanz/asec |
|---|---|---|---|---|---|
| →[7] | IC 4141 | LEDA/PGC 45147 | 13h04m07.731s | +19d12m38.33s | 0 |
| 1 | IC 4148 | 2MASX J13041066+1915323 | 13h04m10.685s | +19d15m32.95s | 179.54 |
| 2 | IC 4146 | 2MASX J13041038+1916423 | 13h04m10.379s | +19d16m41.75s | 246.26 |
| 3 | 2MASX J13040028+1908474 | WISEA J130400.35+190848.0 | 13h04m00.358s | +19d08m47.90s | 252.94 |
| 4 | 2MASX J13042066+1915535 | WISEA J130420.61+191553.3 | 13h04m20.619s | +19d15m53.17s | 267.00 |
| 5 | 2MASX J13034962+1914233 | WISEA J130349.61+191422.7 | 13h03m49.618s | +19d14m22.71s | 277.00 |
| 6 | 2MASX J13042490+1909406 | WISEA J130424.81+190941.0 | 13h04m24.875s | +19d09m40.95s | 300.79 |
| 7 | IC 4139 | LEDA/PGC 3090109 | 13h04m04.149s | +19d17m41.91s | 307.73 |
| 8 | IC 4130 | LEDA/PGC 45103 | 13h03m46.594s | +19d16m17.54 | 370.89 |
| 9 | 2MASX J13035109+1918483 | WISEA J130351.08+191848.7 | 13h03m51.080s | +19d18m48.72s | 438.96 |
| 10 | LEDA/PGC 1589252 | 2MASX J13035173+1921003 | 13h03m51.725s | +19d21m00.16s | 550.58 |
| 11 | 2MASX J13033224+1917140 | WISEA J130332.28+191713.7 | 13h03m32.285s | +19d17m13.76s | 572.46 |
| 12 | LEDA/PGC 3090107 | 2MASX J13032794+1907590 | 13h03m27.971s | +19d07m58.93s | 628.79 |
| 13 | 2MASX J13043034+1922336 | WISEA J130430.36+192233.7 | 13h04m30.369s | +19d22m33.57s | 676.05 |
| 14 | IC 4119 | 2MASX J13031513+1913578 | 13h03m15.170s | +19d13m57.95s | 748.73 |
| 15 | 2MASX J13033966+1901210 | WISEA J130339.70+190121.2 | 13h03m39.709s | +19d01m20.93s | 785.27 |
Weblinks
Einzelnachweise
- ↑ a b c d NASA/IPAC EXTRAGALACTIC DATABASE
- ↑ Simbad
- ↑ a b c d e SEDS: IC 4141
- ↑ NASA/IPAC
- ↑ M. Gullieuszik, E. Giunchi. B. M. Poggianti, A. Moretti, C. Scarlata, D. Calzetti, A. Werle, A. Zanella, M. Radovich, C. Bellhouse, Daniela Bettoni, A. Franchetto, J. Fritz, Y. L. Jaff e, S. L. McGee, M. Mingozzi,A. Omizzolo, S. Tonnesen, M. Verheijen, and B. Vulcani: UV and Hα HST observations of 6 GASP jellyfish galaxies. In: The Astrophysical Journal. 945. Jahrgang, 2023, S. 1–13, doi:10.3847/1538-4357/acb59b (englisch).
- ↑ Seligman
- ↑ SIMBAD
Auf dieser Seite verwendete Medien
A jellyfish galaxy adrift (potw2321a).tiff
(c) ESA/Hubble, CC BY 4.0
The jellyfish galaxy JW39 hangs serenely in this image from the NASA/ESA Hubble Space Telescope. This galaxy lies over 900 million light-years away in the constellation Coma Berenices, and is one of several jellyfish galaxies that Hubble has been studying over the past two years.Despite this jellyfish galaxy’s serene appearance, it is adrift in a ferociously hostile environment; a galaxy cluster. Compared to their more isolated counterparts, the galaxies in galaxy clusters are often distorted by the gravitational pull of larger neighbours, which can twist galaxies into a variety of weird and wonderful shapes. If that was not enough, the space between galaxies in a cluster is also pervaded with a searingly hot plasma known as the intracluster medium. While this plasma is extremely tenuous, galaxies moving through it experience it almost like swimmers fighting against a current, and this interaction can strip galaxies of their star-forming gas.This interaction between the intracluster medium and the galaxies is called ram-pressure stripping, and is the process responsible for the trailing tendrils of this jellyfish galaxy. As JW39 has moved through the cluster the pressure of the intracluster medium has stripped away gas and dust into long trailing ribbons of star formation that now stretch away from the disc of the galaxy.Astronomers using Hubble’s Wide Field Camera 3 studied these trailing tendrils in detail, as they are a particularly extreme environment for star formation. Surprisingly, they found that star formation in the ‘tentacles’ of jellyfish galaxies was not noticeably different from star formation in the galaxy disc.[Image Description: A spiral galaxy. It is large in the centre with a lot of detail visible. The core glows brightly and is surrounded by concentric rings of dark and light dust. The spiral arms are thick and puffy with grey dust and glowing blue areas of star formation. They wrap around the galaxy to form a ring. Part of the arm is drawn out into a dark thread above the galaxy, and dust from the arm trails off to the right.]
(c) ESA/Hubble, CC BY 4.0
The jellyfish galaxy JW39 hangs serenely in this image from the NASA/ESA Hubble Space Telescope. This galaxy lies over 900 million light-years away in the constellation Coma Berenices, and is one of several jellyfish galaxies that Hubble has been studying over the past two years.Despite this jellyfish galaxy’s serene appearance, it is adrift in a ferociously hostile environment; a galaxy cluster. Compared to their more isolated counterparts, the galaxies in galaxy clusters are often distorted by the gravitational pull of larger neighbours, which can twist galaxies into a variety of weird and wonderful shapes. If that was not enough, the space between galaxies in a cluster is also pervaded with a searingly hot plasma known as the intracluster medium. While this plasma is extremely tenuous, galaxies moving through it experience it almost like swimmers fighting against a current, and this interaction can strip galaxies of their star-forming gas.This interaction between the intracluster medium and the galaxies is called ram-pressure stripping, and is the process responsible for the trailing tendrils of this jellyfish galaxy. As JW39 has moved through the cluster the pressure of the intracluster medium has stripped away gas and dust into long trailing ribbons of star formation that now stretch away from the disc of the galaxy.Astronomers using Hubble’s Wide Field Camera 3 studied these trailing tendrils in detail, as they are a particularly extreme environment for star formation. Surprisingly, they found that star formation in the ‘tentacles’ of jellyfish galaxies was not noticeably different from star formation in the galaxy disc.[Image Description: A spiral galaxy. It is large in the centre with a lot of detail visible. The core glows brightly and is surrounded by concentric rings of dark and light dust. The spiral arms are thick and puffy with grey dust and glowing blue areas of star formation. They wrap around the galaxy to form a ring. Part of the arm is drawn out into a dark thread above the galaxy, and dust from the arm trails off to the right.]