IC 1954

In this article, we are going to thoroughly explore the topic of IC 1954 and its impact on modern society. For decades, IC 1954 has been the subject of debate, research and development, influencing multiple aspects of daily life. Over the years, IC 1954 has evolved and adapted to new trends and technologies, becoming a relevant topic of interest to a wide spectrum of people. In this sense, it is crucial to understand the role that IC 1954 plays in our current society, as well as analyze its implications at a social, political, economic and cultural level. Throughout this article, we will address various perspectives and opinions about IC 1954, with the aim of offering a global and complete vision of this topic that is so relevant today.

IC 1954
IC 1954 imaged by the Hubble Space Telescope
Observation data (J2000 epoch)
ConstellationHorologium
Right ascension03h 31m 31.2844s[1]
Declination−51° 54′ 17.100″[1]
Redshift0.003542 ± 0.000007 [1]
Heliocentric radial velocity1,062 ± 2 km/s[1]
Distance47.4 ± 7.4 Mly (14.5 ± 2.3 Mpc)[1]
Group or clusterIC 1954 group (LGG 93)
Apparent magnitude (V)11.4[2]
Characteristics
TypeSA(s)c [1]
Size~44,100 ly (13.51 kpc) (estimated)[1]
Apparent size (V)3.2′ × 1.5′[1]
Other designations
ESO 200- G 036, IRAS 03300-5204, PGC 13090[1]

IC 1954 is a spiral galaxy in the constellation Horologium. The galaxy lies about 45 million light years away from Earth, which means, given its apparent dimensions, that IC 1954 is approximately 45,000 light years across.[1] It was discovered independently by Robert T. A. Innes in 1898 and DeLisle Stewart and October 14, 1898.[3]

The galaxy has two large, curling arms that extend from the centre and wrap around. The arms are followed by thick strands of dark reddish dust. The arms and rest of the galaxy’s disc are speckled with glowing patches; some are blue in colour, others are pink. The pink spots are star forming regions emitting H-alpha light. There are also many star clusters. In the center of the galaxy lies a bar, which could be a region of intense star formation.[4] The bar is short, 6 arcseconds long, and with several knots. A large cluster or OB association is visible at its western end.[5] Hydrogen line mapping shows a central compact disk with bright emission with a radius of 5 kpc surrounded by fainter emission.[6] The total star formation rate of the galaxy is estimated to be 0.36 M☉ per year. The galaxy is seen at an angle of 57°.[7]

IC 1954 is a member of the IC 1954 group, also known as LGG 93. Other members of the group include IC 1933, IC 1959, NGC 1249, and NGC 1311.[8] It belongs in the same galaxy cloud as the Dorado Group.[9]

References

  1. ^ a b c d e f g h i j "Results for IC 1954". NASA/IPAC Extragalactic Database. NASA and Caltech. Retrieved 2 February 2025.
  2. ^ "Revised NGC Data for IC 1954". spider.seds.org. Retrieved 30 March 2024.
  3. ^ Seligman, Courtney. "IC 1954 (= PGC 13090 = ESO 200-036)". Celestial Atlas. Retrieved 19 November 2018.
  4. ^ Public Domain This article incorporates text from this source, which is in the public domain. "The new and improved IC 1954". www.esahubble.org. Retrieved 2 February 2025.
  5. ^ Phillips, Andrew C.; Illingworth, Garth D.; MacKenty, John W.; Franx, Marijn (April 1996). "Nuclei of Nearby Disk Galaxies.I.A Hubble Space Telescope Imaging Survey". The Astronomical Journal. 111: 1566. doi:10.1086/117896.
  6. ^ Eibensteiner, Cosima; et al. (November 2024). "PHANGS-MeerKAT and MHONGOOSE HI observations of nearby spiral galaxies: Physical drivers of the molecular gas fraction, R mol". Astronomy & Astrophysics. 691: A163. arXiv:2407.01716. doi:10.1051/0004-6361/202449944.
  7. ^ Lee, Janice C.; et al. (1 January 2022). "The PHANGS-HST Survey: Physics at High Angular Resolution in Nearby Galaxies with the Hubble Space Telescope". The Astrophysical Journal Supplement Series. 258 (1): 10. arXiv:2101.02855. Bibcode:2022ApJS..258...10L. doi:10.3847/1538-4365/ac1fe5.
  8. ^ 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.
  9. ^ 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.
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