Stephanův kvintet
| Stephanův kvintet | |
|---|---|
 Stephanův kvintet, Hubbleův dalekohled 2009 | |
| Pozorovací údaje (Ekvinokcium J2000,0) | |
| Rektascenze | 22h 35m 59,1s[1] |
| Deklinace | +33°57′31″[1] |
| Souhvězdí | Pegas (Peg) |
| Vzdálenost | 300 M [1] ly |
| Fyzikální charakteristiky | |
| Počet galaxií | 5 |
| Hmotnost | (1,03 ± 0,17) ×1012 |
| Označení v katalozích | |
| Arp 319,[2], APG 319,[1], HCG 92[3] | |
Stephanův kvintet je skupina pěti galaxií v souhvězdí Pegase. Čtyři galaxie Stephanova kvintetu, NGC 7317, NGC 7318a, NGC 7318b a NGC 7319, tvoří gravitačně vázanou kompaktní skupinu HCG 92 vzdálenou od Země přibližně 300 milionů světelných let. Tvary galaxií kompaktní skupiny jsou výrazně deformovány vzájemným gravitačním působením.[4] NGC 7319 má Seyfertovo jádro typu 2.[5]
Nejjasnější z pětice galaxií NGC 7320 leží ve vzdálenosti 39 milionů světelných let a na obloze se promítá na vzdálenější galaxie v pozadí. Vykazuje shodný rudý posuv jako galaxie NGC 7331 a její sousedé, takže pravděpodobně náleží ke skupině galaxii NGC 7331.
Stephanův kvintet objevil Édouard Stephan v roce 1877[4] jako první objevenou kompaktní skupinu galaxií.
| Jméno | Typ | Rektascenze (J2000) | Deklinace (J2000) | Rudý posuv (km/s) | Magnituda |
|---|---|---|---|---|---|
| NGC 7317 | E4 | 22h 35m 51.9s | +33°56′42″ | 6599 ± 26 | +14.6 |
| NGC 7318a (UGC 12099) | E2 pec | 22h 35m 56.7s | +33°57′56″ | 6630 ± 23 | +14.3 |
| NGC 7318b (UGC 12100) | SB(s)bc pec | 22h 35m 58.4s | +33°57′57″ | 5774 ± 24 | +13.9 |
| NGC 7319 | SB(s)bc pec | 22h 36m 03.5s | +33°58′33″ | 6747 ± 7 | +14.1 |
| NGC 7320c | (R)SAB(s)0/a | 22h 36m 20.4s | +33°59′06″ | 5985 ± 9 | +16.7 |
| Jméno | Typ | Rektascenze (J2000) | Deklinace (J2000) | Rudý posuv (km/s) | Magnituda |
|---|---|---|---|---|---|
| NGC 7320 | Scd | 22h 36m 03,5s | +33°56′54″ | 786 ± 20 | +12,5 |
Galerie
Stephanův kvintet spolu s galaxií NGC 7320C pravděpodobně náležející k HCG 92 (bílý obdélník označuje rozsah podrobného snímku Hubbleova dalekohledu z roku 1998-99)
Detail Stephanova kvintetu, který pořídil Hubbleův vesmírný dalekohled v letech 1998–99 (autor: NASA/ESA)
Stephanův kvintet na hvězdné mapě
Reference
- ↑ a b c d NASA/IPAC Extragalactic Database: Results for ARP 319 [online]. [cit. 2019-11-26]. Dostupné online. (anglicky)
- ↑ ARP, Halton. Atlas of Peculiar Galaxies. S. 1. Astrophysical Journal Supplement [online]. Listopad 1966 [cit. 2019-11-26]. Roč. 14, s. 1. Dostupné online. DOI 10.1086/190147. Bibcode 1966ApJS...14....1A. (anglicky)
- ↑ SIMBAD Astronomical Database: Results for HCG 92 [online]. [cit. 2019-11-26]. Dostupné online. (anglicky)
- ↑ a b KODRIŠ, Michal. Průvodce hvězdnou oblohou: Pegas [online]. [cit. 2019-11-26]. Dostupné online.
- ↑ AOKI, Kentaro; KOSUGI, George; WILSON, Andrew S.; YOSHIDA, Michitoshi. The Radio Emission of the Seyfert Galaxy NGC 7319. S. 565–571. Astrophysical Journal [online]. Srpen 1999 [cit. 2019-11-27]. Roč. 521, čís. 2, s. 565–571. Dostupné online. arXiv astro-ph/9812365. DOI 10.1086/307559. Bibcode 1999ApJ...521..565A. (anglicky)
Externí odkazy
Obrázky, zvuky či videa k tématu Stephanův kvintet na Wikimedia Commons - KODRIŠ, Michal. Průvodce hvězdnou oblohou: Pegas [online]. [cit. 2019-11-26]. Dostupné online.
Média použitá na této stránce
Stephan's Quintet, NGC7317, NGC7318A, NGC7318B, NGC7319, NGC7320, NGC 7320C
This close-up view of Stephan's Quintet, a group of five galaxies, reveals a string of bright star clusters that sparkles like a diamond necklace. The clusters, each harboring up to millions of stars, were born from the violent interactions between some members of the group. The rude encounters also have distorted the galaxies' shapes, creating elongated spiral arms and long, gaseous streamers.
The NASA Hubble Space Telescope photo showcases three regions of star birth: the long, sweeping tail and spiral arms of NGC 7319 [near center]; the gaseous debris of two galaxies, NGC 7318B and NGC 7318A [top right]; and the area north of those galaxies, dubbed the northern starburst region [top left].
The clusters' bluish color indicates that they're relatively young. Their ages span from about 2 million to more than 1 billion years old.
The brilliant star clusters in NGC 7318B's spiral arm (about 30,000 light-years long) and the northern starburst region are between 2 million and more than 100 million years old. NGC 7318B instigated the starburst by barreling through the region. The bully galaxy is just below NGC 7318A at top right. Although NGC 7318B appears dangerously close to NGC 7318A, it's traveling too fast to merge with its close neighbor. The partial galaxy on the far right is NGC 7320, a foreground galaxy not physically bound to the other galaxies in the picture.
About 20 to 50 of the clusters in the northern starburst region reside far from the coziness of galaxies. The clusters were born about 150,000 light-years from the nearest galaxy.
A galaxy that is no longer part of the group triggered another collision that wreaked havoc. NGC 7320C [not in the photo] plowed through the quintet several hundred million years ago, pulling out the 100,000 light-year-long tail of gaseous debris from NGC 7319. The clusters in NGC 7319's streaming tail are 10 million to 500 million years old and may have formed at the time of the violent collision. The faint bluish object at the tip of the tail is a young dwarf galaxy, which formed in the gaseous debris.
The quintet is in the constellation Pegasus, 270 million light-years from Earth. Spied by Edouard M. Stephan in 1877, Stephan's Quintet is the first compact group ever discovered.
The mosaic picture was taken by Hubble's Wide Field and Planetary Camera 2 on Dec. 30, 1998 and June 17, 1999.Galactic Wreckage in Stephan's Quintet.
A clash among members of a famous galaxy quintet reveals an assortment of stars across a wide color range, from young, blue stars to aging, red stars.
This portrait of Stephan's Quintet, also known as Hickson Compact Group 92, was taken by the new Wide Field Camera 3 (WFC3) aboard NASA's Hubble Space Telescope. Stephan's Quintet, as the name implies, is a group of five galaxies. The name, however, is a bit of a misnomer. Studies have shown that group member NGC 7320, at upper left, is actually a foreground galaxy about seven times closer to Earth than the rest of the group.
Three of the galaxies have distorted shapes, elongated spiral arms, and long, gaseous tidal tails containing myriad star clusters, proof of their close encounters. These interactions have sparked a frenzy of star birth in the central pair of galaxies. This drama is being played out against a rich backdrop of faraway galaxies.
The image, taken in visible and near-infrared light, showcases WFC3's broad wavelength range.
The colors trace the ages of the stellar populations, showing that star birth occurred at different epochs, stretching over hundreds of millions of years. The camera's infrared vision also peers through curtains of dust to see groupings of stars that cannot be seen in visible light.
NGC 7319, at top right, is a barred spiral with distinct spiral arms that follow nearly 180 degrees back to the bar. The blue specks in the spiral arm at the top of NGC 7319 and the red dots just above and to the right of the core are clusters of many thousands of stars. Most of the quintet is too far away even for Hubble to resolve individual stars.
Continuing clockwise, the next galaxy appears to have two cores, but it is actually two galaxies, NGC 7318A and NGC 7318B. Encircling the galaxies are young, bright blue star clusters and pinkish clouds of glowing hydrogen where infant stars are being born. These stars are less than 10 million years old and have not yet blown away their natal cloud. Far away from the galaxies, at right, is a patch of intergalactic space where many star clusters are forming.
NGC 7317, at bottom left, is a normal-looking elliptical galaxy that is less affected by the interactions.
Sharply contrasting with these galaxies is the dwarf galaxy NGC 7320 at upper left. Bursts of star formation are occurring in the galaxy's disk, as seen by the blue and pink dots. In this galaxy, Hubble can resolve individual stars, evidence that NGC 7320 is closer to Earth.
NGC 7320 is 40 million light-years from Earth. The other members of the quintet reside 290 million light-years away in the constellation Pegasus.
These farther members are markedly redder than the foreground galaxy, suggesting that older stars reside in their cores. The stars' light also may be further reddened by dust stirred up in the encounters.
Spied by Edouard M. Stephan in 1877, Stephan's Quintet is the first compact group ever discovered.
WFC3 observed the quintet in July and August 2009. The composite image was made by using filters that isolate light from the blue, green, and infrared portions of the spectrum, as well as emission from ionized hydrogen.
These Hubble observations are part of the Hubble Servicing Mission 4 Early Release Observations. NASA astronauts installed the WFC3 camera during a servicing mission in May to upgrade and repair the 19-year-old Hubble telescope.
Denoised by uploader.