NGC 3673 is a barred spiral galaxy in the constellation Hydra. The galaxy lies about 75 million light years away from Earth, which means, given its apparent dimensions, that NGC 3673 is approximately 75,000 light years across.[1] It was discovered by John Herschel on March 22, 1836.[3]

The galaxy has a small, bright nucleus embedded in a bar,[4] with distinctly blue color.[5] The bar is weak and some darker areas are visible in it.[4] The bar has X-shaped features.[6] The bulge is weakly boxy.[5] At the end of the bar a nearly complete ring is formed,[7] measuring 1.5 by 0.7 arcminutes. From the ring emerge faint filamentary arms.[4] The spiral pattern resembles more that of a grand design galaxy than a flocculent pattern.[7] The star formation rate of the galaxy is estimated to be about 0.7 M☉ per year.[8] In the centre of the galaxy lies a supermassive black hole, whose mass is estimated to be 107.01 ± 0.37 (4.4 - 24 millions) M☉, based on the pitch angle of the spiral arms.[9]

NGC 3673 is a relatively isolated galaxy. It belongs to the same galaxy cloud as NGC 3923, NGC 3717, NGC 3885, NGC 3904, and NGC 4105 and their groups.[10]

References

  1. ^ a b c d e f g h i j "Results for object NGC 3673". NASA/IPAC Extragalactic Database. NASA and Caltech. Retrieved 24 February 2025.
  2. ^ "Revised NGC Data for NGC 3673". spider.seds.org. Retrieved 30 March 2024.
  3. ^ Seligman, Courtney. "NGC 3673 (= PGC 35097)". Celestial Atlas. Retrieved 19 November 2018.
  4. ^ a b c de Vaucouleurs, Gerard Henri; de Vaucouleurs, Antoinette; Shapley, Harlow (1964). Reference catalogue of bright galaxies. Austin: University of Texas Press. Bibcode:1964rcbg.book.....D.
  5. ^ a b Gao 高, Hua 桦; Ho, Luis C.; Barth, Aaron J.; Li, Zhao-Yu (1 October 2019). "The Carnegie-Irvine Galaxy Survey. VIII. Demographics of Bulges along the Hubble Sequence". The Astrophysical Journal Supplement Series. 244 (2): 34. arXiv:1901.03195. Bibcode:2019ApJS..244...34G. doi:10.3847/1538-4365/ab3c6a.
  6. ^ Laurikainen, E.; Salo, H. (February 2017). "Barlenses and X-shaped features compared: two manifestations of boxy/peanut bulges". Astronomy & Astrophysics. 598: A10. arXiv:1609.01936. Bibcode:2017A&A...598A..10L. doi:10.1051/0004-6361/201628936.
  7. ^ a b Sandage, A., Bedke, J. (1994), The Carnegie Atlas of Galaxies. Volume I, Carnegie Institution of Washington
  8. ^ 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.
  9. ^ Davis, Benjamin L.; Berrier, Joel C.; Johns, Lucas; Shields, Douglas W.; Hartley, Matthew T.; Kennefick, Daniel; Kennefick, Julia; Seigar, Marc S.; Lacy, Claud H. S. (20 June 2014). "The Black Hole Mass Function Derived from Local Spiral Galaxies". The Astrophysical Journal. 789 (2): 124. arXiv:1405.5876. Bibcode:2014ApJ...789..124D. doi:10.1088/0004-637X/789/2/124. S2CID 119302157.
  10. ^ 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.
Allikas: https://en.wikipedia.org/wiki/NGC_3673
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