NGC 1703 is a spiral galaxy in the constellation Dorado. The galaxy lies about 60 million light years away from Earth, which means, given its apparent dimensions, that NGC 1703 is approximately 50,000 light years across.[2] It was discovered by John Herschel on December 4, 1834.[4]

The galaxy is characterised as SA(s)c meaning that it doesn't have a bar, however there may be a weak bar present.[5] There is no box-shaped bulge detected, a feature commonly associated with barred galaxies.[6] The galaxy is seen nearly face-on, at an inclination of about 27°.[5] It has a small nucleus and two well-defined spiral arms in a grand design pattern. The arms are smooth for about half a revolution but their outer regions are patchy. One arm can be traced for about a full revolution while the other fades after about three quarters of a revolution.[7] In the centre of the galaxy lies a supermassive black hole, whose mass is estimated to be 107.01 ± 0.40 (4 - 26 million) M☉, based on the pitch angle of the spiral arms.[8] The star formation rate based on the HI amount is estimated to be about 1.1 solar mass per year.[9]

NGC 1703 is located in the vicinity of the Dorado Group, lying in the same galaxy cloud as the rest of the members.[10] Garcia considers the galaxy a member of the LGG 119 group, which also includes NGC 1672 and NGC 1688.[11]

References

  1. ^ "A Dorado's Scale". www.noirlab.edu. 9 March 2022. Retrieved 17 February 2025.
  2. ^ a b c d e f g h "NASA/IPAC Extragalactic Database". Results for NGC 1703. Retrieved 1 February 2025.
  3. ^ "Revised NGC Data for NGC 1703". spider.seds.org. Retrieved 30 March 2024.
  4. ^ Seligman, Courtney. "NGC 1703 (= PGC 16234)". Celestial Atlas. Retrieved 19 November 2018.
  5. ^ a b Martínez-García, Eric E.; González-Lópezlira, Rosa A. (21 February 2013). "Signatures of Long-Lived Spiral Patterns". The Astrophysical Journal. 765 (2): 105. doi:10.1088/0004-637X/765/2/105.
  6. ^ Méndez-Abreu, J.; Corsini, E. M.; Debattista, Victor P.; De Rijcke, S.; Aguerri, J. A. L.; Pizzella, A. (1 June 2008). "Confirmation of a Kinematic Diagnostic for Face-On Box/Peanut-shaped Bulges". The Astrophysical Journal. 679 (2): L73 – L76. doi:10.1086/589541. hdl:11577/2447890.
  7. ^ 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. doi:10.1086/342340.
  8. ^ 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.
  9. ^ 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. doi:10.3847/1538-4357/aad3b9.
  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.
  11. ^ 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_1703
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