NGC 871

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NGC 871
NGC 870 71 PanS.jpg
Observation data
Constellation Aries [1]
Right ascension 02h 17m 10,7s [1]
Declination +14° 32′ 52″ [1]
Redshift +0012475±0.000003 [1]
Heliocentric radial velocity 3740 ± 1 km/s [1]
Distance 52,2 ± 3,7
(170 ± 12)×106 ly) [1]
Apparent magnitude  (V)13,4 mag [1]
Apparent magnitude  (B)14,1 mag [1]
Other designations
NGC 0871 • UGC 1759 • PGC 8722 • CGCG 438-046 • MCG -02-06-053 • IRAS 02144+1419 • 2MASX J02171073+1432521 • CN 513

NGC 871 is a barred spiral galaxy in the Aries constellation. [1] Its discovery and first description was realized by William Herschel on October 14, 1784 [2] and the findings made public through his Catalogue of Nebulae and Clusters of Stars in 1786.

Contents

By using the galaxies' radial velocities and distances as a grouping factor, astronomers assign this galaxy to LGG (Lyon Groups of Galaxies) 53 along with 8 other members (UGC 1693, UGC 1761, NGC 876, NGC 877, UGC 1817, IC 1791 and UGC 1773). [3] [4]

Galaxy group NGC 871/6/7

At the current epoch, most galaxies can be found in medium-density group environments, where tidal interactions play an important role in galactic evolution. Several nearby, gas-rich groups exhibit clear signs of these interactions, giving the opportunity for scientists to study how galaxies are formed and interact with each other. [5]

In 2012 astronomers conducted an extensive survey to measure the Hl emissions from NGC 871 and other galaxies in LGG 53, using the Giant Metrewave Radio Telescope and Canada–France–Hawaii Telescope. This galaxy group first attracted attention due to its gas-rich interaction as well as harboring AGC (Arecibo General Catalog) 749170, a galaxy with a mass of ~×109.3 M☉. This group resides in a common HI distribution with a total HI mass of Mhl 6 x 10×1010 M☉. Such a massive structure is very rare in the local Universe (galaxies with a Mhl > ×1010 M☉ represents less 2 per cent of cases) and each large spiral in NGC 871/6/7 seems to exceeds this value. [5]

The study suggests seven of the eight gas-rich detections (three spirals and four dwarfs) contain stellar components and appear to be standard dark-matter dominated galaxies that were built during the epoch of galaxy assembly. AGC 749170 however is probably the result of major mergers and very active tidal interaction, resulting in the massive structure we can observe today. [5]

See also

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<span class="mw-page-title-main">NGC 2293</span> Galaxy in the constellation Canis Major

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<span class="mw-page-title-main">NGC 4324</span> Galaxy in the constellation of Virgo

NGC 4324 is a lenticular galaxy located about 85 million light-years away in the constellation Virgo. It was discovered by astronomer Heinrich d'Arrest on March 4, 1862. NGC 4324 has a stellar mass of 5.62 × 1010M☉, and a baryonic mass of 5.88 × 1010M☉. The galaxy's total mass is around 5.25 × 1011M☉. NGC 4324 is notable for having a ring of star formation surrounding its nucleus. It was considered a member of the Virgo II Groups until 1999, when its distance was recalculated and it was placed in the Virgo W Group.

References

  1. 1 2 3 4 5 6 7 8 9 "NED results for object NGC 0871". ned.ipac.caltech.edu. Retrieved 2023-11-07.
  2. ↑ "Herschel Catalog". www.messier.seds.org. Retrieved 2023-11-06.
  3. ↑ Garcia, A. M. (1993-07-01). "General study of group membership. II. Determination of nearby groups". Astronomy and Astrophysics Supplement Series. 100: 47–90. ISSN   0365-0138.
  4. ↑ Mahtessian, A. P. (1998-07-01). "Groups of galaxies. III. Some empirical characteristics". Astrophysics. 41: 308–321. doi:10.1007/BF03036100. ISSN   0571-7256.
  5. 1 2 3 Lee-Waddell, K.; Spekkens, K.; Cuillandre, J.-C.; Cannon, J.; Haynes, M. P.; Sick, J.; Chandra, P.; Patra, N.; Stierwalt, S.; Giovanelli, R. (2014-10-01). "An extremely optically dim tidal feature in the gas-rich interacting galaxy group NGC 871/NGC 876/NGC 877". Monthly Notices of the Royal Astronomical Society. 443 (4): 3601–3611. arXiv: 1407.1732 . doi: 10.1093/mnras/stu1345 . ISSN   1365-2966.
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