IC 184

IC 184
SDSS image of IC 184
Observation data (J2000 epoch)
ConstellationCetus
Right ascension01h 59m 51.25s
Declination−06° 50′ 24.36″
Redshift0.017952
Heliocentric radial velocity5,382 km/s ± 26
Distance243 Mly
Apparent magnitude (V)13.8
Characteristics
TypeSB(r)a:;Sy2 HII
Size~93,000 ly (28.4 kpc) (estimated)
Other designations
6dF J0159512-065025, 2MASX J01595121-0650253, NSA 130927, PGC 7554, IRAS F01573-0704, MCG -01-06-021

IC 184 is a spiral galaxy located in the constellation of Cetus. The redshift of the galaxy is (z) 0.0179 and it was first discovered by the American astronomer Ormond Stone in October 1887 who gave the description of the object as both faint and small. It has also been classified as a Type 2 Seyfert galaxy.

Description

IC 184 is classified as an early-type spiral galaxy of type SB(r)a based on Calar Alto CCD imaging and is a member of small galaxy group comprising three other galaxies, MCG -01-06-09, MCG -01-06-020 and MCG -01-06-022. When observed, it is shown to have an outer bar feature that is clearly resolved into multiple spiral arms, depicted as having a bright appearance. The central region of the galaxy is found to have isophotal twisting and also the rotation of its position angle (PA). There is a presence of an inner bar that has a region shown as visible as a thick curved elongated feature that begins at the end. The northern spiral arm of the galaxy is found to be much more brighter compared to the southern spiral arm. There are also traces of both inner and outer shell features based on imaging made with Hubble Space Telescope (HST).

Evidence has found IC 184 is an isolated galaxy. When observed, it has a galaxy rotation curve that is orientated along the major axis position angle of 7° and 97°, with the rotation of both the gas and stars being described as decoupled with 4 arcseconds of its own galactic center. A further observation also found the presence of a structure within the innermost region of nine arcseconds, depicted as having a wavy central shape appearance. A water megamaser source has been detected in the galaxy. The luminosity of the megamaser emission is estimated to be 1.0 L☉.

References

  1. 1 2 3 4 5 6 7 8 "NED Search results for IC 184". NASA/IPAC Extragalactic Database. Retrieved 2026-01-31.
  2. ↑ "Revised IC Data for IC 184". spider.seds.org. Retrieved 30 March 2024.
  3. ↑ "Index Catalog Objects: IC 150 - 199". cseligman.com. Retrieved 2026-01-31.
  4. 1 2 Kollatschny, W.; Fricke, K. J. (September 1987). "The Seyfert 2 galaxy IC 184 and its surrounding group". Astronomy and Astrophysics. 183: 9–12. Bibcode:1987A&A...183....9K.
  5. ↑ Zhang, J. S.; Henkel, C.; Guo, Q.; Wang, H. G.; Fan, J. H. (2009-12-11). "ON THE NUCLEAR OBSCURATION OF H2O MASER GALAXIES". The Astrophysical Journal. 708 (2): 1528–1536. arXiv:0912.2159. doi:10.1088/0004-637X/708/2/1528.
  6. ↑ Zhang, J. S.; Henkel, C.; Guo, Q.; Wang, J. (2012-02-01). "Radio properties of H2O maser host galaxies". Astronomy & Astrophysics. 538: A152. arXiv:1201.2075. doi:10.1051/0004-6361/201117946. ISSN 0004-6361.
  7. ↑ Wozniak, Hervé; Champavert, Nicolas (2006-05-08). "Lifetime of nuclear velocity dispersion drops in barred galaxies". Monthly Notices of the Royal Astronomical Society. 369 (2): 853–859. arXiv:astro-ph/0603784. Bibcode:2006MNRAS.369..853W. doi:10.1111/j.1365-2966.2006.10359.x. ISSN 0035-8711.
  8. ↑ Erwin, Peter (2004-02-13). "Double-barred galaxies. I. A catalog of barred galaxies with stellar secondary bars and inner disks". Astronomy & Astrophysics. 415 (3): 941–957. arXiv:astro-ph/0310806. Bibcode:2004A&A...415..941E. doi:10.1051/0004-6361:20034408. ISSN 0004-6361.
  9. ↑ Marquez, I.; Durret, F.; Delgado, R. M. Gonzalez; Marrero, I.; Masegosa, J.; Maza, J.; Moles, M.; Perez, E.; Roth, M. (1999-09-21). "Near-infrared photometry of isolated spirals with and without an AGN". Astronomy and Astrophysics Supplement Series. 140: 1–14. arXiv:astro-ph/9909351. doi:10.1051/aas:1999516.
  10. ↑ Malkan, M. A.; Gorjian, V.; Tam, R. (1998-03-11). "A Hubble Space Telescope Imaging Survey of Nearby Active Galactic Nuclei". The Astrophysical Journal Supplement Series. 117 (1): 25–88. arXiv:astro-ph/9803123. Bibcode:1998ApJS..117...25M. doi:10.1086/313110.
  11. ↑ Márquez, I.; Masegosa, J.; Durret, F.; Delgado, R. M. González; Moles, M.; Maza, J.; Pérez, E.; Roth, M. (2003-10-01). "The detection of stellar velocity dispersion drops in the central regions of five isolated Seyfert spirals" (PDF). Astronomy & Astrophysics. 409 (2): 459–467. arXiv:astro-ph/0306497. Bibcode:2003A&A...409..459M. doi:10.1051/0004-6361:20031059. ISSN 0004-6361.
  12. ↑ Kondratko, P. T.; Greenhill, L. J.; Moran, J. M.; Lovell, J. E. J.; Kuiper, T. B. H.; Jauncey, D. L.; Cameron, L. B.; Gomez, J. F.; Garcia-Miro, C.; Moll, E.; de Gregorio-Monsalvo, I.; Jimenez-Bailon, E. (2006-02-10). "Discovery of Water Maser Emission in Eight AGNs with 70 m Antennas of NASA's Deep Space Network". The Astrophysical Journal. 638 (1): 100–105. arXiv:astro-ph/0510851. Bibcode:2006ApJ...638..100K. doi:10.1086/498641. ISSN 0004-637X.
  13. ↑ Liu, Z. W.; Zhang, J. S.; Henkel, C.; Liu, J.; Müller, P.; Guo, J. Z. Wang Q.; Wang, J.; Li, J. (2016-12-16). "A systematic observational study of radio properties of H2O megamaser Seyfert-2 galaxies". Monthly Notices of the Royal Astronomical Society. 466 (2): 1608–1624. arXiv:1612.05315. doi:10.1093/mnras/stw3158.