NGC 5085 is a barred spiral galaxy in the constellation Hydra. The galaxy lies about 90 million light years away from Earth, which means, given its apparent dimensions, that NGC 5085 is approximately 130,000 light years across.[1] It was discovered by William Herschel on March 26, 1789.[3]

The galaxy has a small but bright bulge with elliptical shape. Two prominent low-surface brightness spiral arms emerge from the bulge in a grand design pattern. After about half a revolution the arms begin to branch. They can be traced for about a full revolution before fading.[4] The kinematics of the galaxy indicate that the arms start about 14 arcseconds from the nucleus while the symmetrical pattern ends a bit further away than the 42 arcseconds radius from the centre of the galaxy.[5] Dust lanes are visible running inside each of the two principal arms for the first half of their length. The outer disk has a flocculent pattern with many dust lanes and spiral fragments.[6] There are many HII regions along both the inner and outer arms.[4] The star formation rate of the galaxy is estimated to be 3.4 M☉ per year.[7]

NGC 5085 is a member of the NGC 5078 Group, also known as LGG 341.[8] Other members of the group include NGC 5061, IC 879, NGC 5078, IC 874, IC 4231, and NGC 5101.[9] It lies in the same galaxy cloud as NGC 5084.[8]

References

  1. ^ a b c d e f g h i j "Results for object NGC 5085". NASA/IPAC Extragalactic Database. NASA and Caltech. Retrieved 25 February 2025.
  2. ^ "Revised NGC Data for NGC 5085". spider.seds.org. Retrieved 30 March 2024.
  3. ^ Seligman, Courtney. "NGC 5085 (= PGC 46531)". Celestial Atlas. Retrieved 19 November 2018.
  4. ^ a b Eskridge, Paul B.; Frogel, Jay A.; Pogge, Richard W.; Quillen, Alice C.; Berlind, Andreas A.; Davies, Roger L.; DePoy, D. L.; Gilbert, Karoline M.; Houdashelt, Mark L.; Kuchinski, Leslie E.; Ramirez, Solange V.; Sellgren, K.; Stutz, Amelia; Terndrup, Donald M.; Tiede, Glenn P. (November 2002). "Near-Infrared and Optical Morphology of Spiral Galaxies". The Astrophysical Journal Supplement Series. 143 (1): 73–111. arXiv:astro-ph/0206320. Bibcode:2002ApJS..143...73E. doi:10.1086/342340.
  5. ^ J., Grosbol, P.; A., Patsis, P. (August 1998). "Stellar disks of optically flocculent and grand design spirals. Decoupling of stellar and gaseous disks". Astronomy and Astrophysics. 336: 840. Bibcode:1998A&A...336..840G. ISSN 0004-6361.{{cite journal}}: CS1 maint: multiple names: authors list (link)
  6. ^ Sandage, A., Bedke, J. (1994), The Carnegie Atlas of Galaxies. Volume I, Carnegie Institution of Washington
  7. ^ Parkash, Vaishali; Brown, Michael J. I.; Jarrett, T. H.; Bonne, Nicolas J. (1 September 2018). "Relationships between Hi Gas Mass, Stellar Mass, and the Star Formation Rate of HICAT+WISE (H i-WISE) Galaxies". The Astrophysical Journal. 864 (1): 40. arXiv:1807.06246. Bibcode:2018ApJ...864...40P. doi:10.3847/1538-4357/aad3b9.
  8. ^ a b Makarov, Dmitry; Karachentsev, Igor (21 April 2011). "Galaxy groups and clouds in the local (z~ 0.01) Universe". Monthly Notices of the Royal Astronomical Society. 412 (4): 2498–2520. arXiv:1011.6277. Bibcode:2011MNRAS.412.2498M. doi:10.1111/j.1365-2966.2010.18071.x. S2CID 119194025. Retrieved 1 February 2025.
  9. ^ Garcia, A. M. (1 July 1993). "General study of group membership. II. Determination of nearby groups". Astronomy and Astrophysics Supplement Series. 100: 47–90. Bibcode:1993A&AS..100...47G. ISSN 0365-0138.
Allikas: https://en.wikipedia.org/wiki/NGC_5085
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