Astronomy:IC 184

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IC 184
SDSS image of IC 184
Observation data (J2000 epoch)
ConstellationCetus
Right ascension 01h 59m 51.25s[1]
Declination−06° 50′ 24.36″[1]
Redshift0.017952[1]
Helio radial velocity5,382 km/s ± 26[1]
Distance243 Mly
Apparent magnitude (V)13.8[2]
Characteristics
TypeSB(r)a:;Sy2 HII[1]
Size~93,000 ly (28.4 kpc) (estimated)[1]
Other designations
6dF J0159512-065025, 2MASX J01595121-0650253, NSA 130927, PGC 7554, IRAS F01573-0704, MCG -01-06-021[1]

IC 184 is a spiral galaxy located in the constellation of Cetus. The redshift of the galaxy is (z) 0.0179[1] 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.[3] It has also been classified as a Type 2 Seyfert galaxy.[4][5][6]

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.[7][4] 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.[8] 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.[9] There are also traces of both inner and outer shell features based on imaging made with Hubble Space Telescope (HST).[10]

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.[11] A water megamaser source has been detected in the galaxy.[12] The luminosity of the megamaser emission is estimated to be 1.0 Lʘ.[13]

References

  1. ↑ 1.0 1.1 1.2 1.3 1.4 1.5 1.6 1.7 "NED Search results for IC 184". https://ned.ipac.caltech.edu/byname?objname=IC+184&hconst=67.8&omegam=0.308&omegav=0.692&wmap=4&corr_z=1. 
  2. ↑ "Revised IC Data for IC 184". https://spider.seds.org/ngc/revngcic.cgi?IC184. 
  3. ↑ "Index Catalog Objects: IC 150 - 199". https://cseligman.com/text/atlas/ic1a.htm#ic184. 
  4. ↑ 4.0 4.1 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. https://ui.adsabs.harvard.edu/abs/1987A%26A...183....9K/abstract. 
  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. 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" (in en). Astronomy & Astrophysics 538: A152. doi:10.1051/0004-6361/201117946. ISSN 0004-6361. https://www.aanda.org/articles/aa/abs/2012/02/aa17946-11/aa17946-11.html. 
  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. doi:10.1111/j.1365-2966.2006.10359.x. ISSN 0035-8711. Bibcode: 2006MNRAS.369..853W. 
  8. ↑ Erwin, Peter (2004-02-13). "Double-barred galaxies. I. A catalog of barred galaxies with stellar secondary bars and inner disks" (in en). Astronomy & Astrophysics 415 (3): 941–957. doi:10.1051/0004-6361:20034408. ISSN 0004-6361. Bibcode: 2004A&A...415..941E. 
  9. ↑ Marquez, I.; Durret, F.; Delgado, R. M. Gonzalez; Marrero, I.; Masegosa, J.; Maza, J.; Moles, M.; Perez, E. et al. (1999-09-21). "Near-infrared photometry of isolated spirals with and without an AGN". Astronomy and Astrophysics Supplement Series 140: 1–14. 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. doi:10.1086/313110. Bibcode: 1998ApJS..117...25M. 
  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" (in en). Astronomy & Astrophysics 409 (2): 459–467. doi:10.1051/0004-6361:20031059. ISSN 0004-6361. Bibcode: 2003A&A...409..459M. https://www.aanda.org/articles/aa/pdf/2003/38/aa3705.pdf. 
  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. et al. (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. doi:10.1086/498641. ISSN 0004-637X. Bibcode: 2006ApJ...638..100K. https://iopscience.iop.org/article/10.1086/498641/fulltext/. 
  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. doi:10.1093/mnras/stw3158. 



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