Astronomy:IC 1816

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IC 1816
IC 1816 imaged by Dark Energy Survey.
Observation data (J2000 epoch)
ConstellationFornax
Right ascension 02h 31m 50.97s[1]
Declination−36° 40′ 19.64″[1]
Redshift0.016945 ± 0.000020[1]
Helio radial velocity5,080 km/s[1]
Distance245 Mly
Apparent magnitude (V)13.1[2]
Characteristics
TypeSB(r)ab pec?[1]
Size~136,000 ly (41.7 kpc) (estimated)[1]
Other designations
ESO 355-G025, MCG -06-06-011, AM 0229-365, IRAS 02297-3653, 6dF J0231510-364019, PGC 9634[1]

IC 1816 is a barred spiral galaxy located in the constellation of Fornax. The galaxy is located 245 million light-years from Earth and has a diameter of approximately 136,000 light-years across.[1] It was first discovered by Lewis Swift on 12 October 1896, who classified it as a small faint round object.[3]

Description

IC 1816 is an isolated face-on spiral galaxy.[4][5] It has three spiral arms with the northwest arm, the brightest and most detached.[5] Two of the arms are distinctive and seem to open up as its spiral structure travels inwards. The galaxy also shows a prominent curved dust lane.[6] There is a clearly resolved ring and a smaller elongated structure interpreted as a nuclear bar.[5] An inner bar might be present given the observation of a small counter-rotation located from its nucleus although a nuclear disk is suggested.[7] The star formation rate for IC 1816 is estimated to be 0.74 Mʘ per year.[8]

The nucleus of IC 1816 is active. It was originally classified as a type 1 Seyfert galaxy[9] but later reclassified as a type 2 Seyfert galaxy due to it lacking broad emission lines.[10] The Seyfert spectrum of the galaxy is found extending as far as 3.4 arcseconds east from the nucleus.[11] A hydrogen alpha component is seen broadening, likely caused by the blending of nitrogen lines.[12]

IC 1816 has an extended narrow line region showing highly ionized gas, indicated by the presence of coronal line emission, with the region mainly centering in its star-forming ring.[13] The gas located in its nuclear region is mainly blueshifted with a peak velocity dispersion of 320 kilometers per second, suggesting the active galactic nucleus of the galaxy is powered through outflows.[4]

References

  1. ↑ 1.0 1.1 1.2 1.3 1.4 1.5 1.6 1.7 "NED search results for IC 1816". https://ned.ipac.caltech.edu/byname?objname=IC+1816&hconst=67.8&omegam=0.308&omegav=0.692&wmap=4&corr_z=1. 
  2. ↑ "Revised NGC Data for IC 1816". http://spider.seds.org/ngc/revngcic.cgi?IC+1816. 
  3. ↑ "IC 1816 (= PGC 9634)". https://cseligman.com/text/atlas/ic18.htm#ic1816. 
  4. ↑ 4.0 4.1 Davies, Rebecca L.; Dopita, Michael A.; Kewley, Lisa; Groves, Brent; Sutherland, Ralph; Hampton, Elise J.; Shastri, Prajval; Kharb, Preeti et al. (2016-06-10). "The Role of Radiation Pressure in the Narrow Line Regions of Seyfert Host Galaxies". The Astrophysical Journal 824 (1): 50. doi:10.3847/0004-637x/824/1/50. ISSN 0004-637X. Bibcode: 2016ApJ...824...50D. 
  5. ↑ 5.0 5.1 5.2 Márquez, I.; Durret, F.; González Delgado, R. M.; Marrero, I.; Masegosa, J.; Maza, J.; Moles, M.; Pérez, E. et al. (November 1999). "Near-infrared photometry of isolated spirals with and without an AGN". Astronomy and Astrophysics Supplement Series 140 (1): 1–14. doi:10.1051/aas:1999516. ISSN 0365-0138. 
  6. ↑ Deo, R. P.; Crenshaw, D. M.; Kraemer, S. B. (2006-06-06). "The Host Galaxies of Narrow-Line Seyfert 1 Galaxies: Nuclear Dust Morphology and Starburst Rings". The Astronomical Journal 132 (1): 321–346. doi:10.1086/504894. ISSN 0004-6256. Bibcode: 2006AJ....132..321D. https://iopscience.iop.org/article/10.1086/504894/fulltext/. 
  7. ↑ Marquez, I.; Durret, F.; Masegosa, J.; Moles, M.; Varela, J.; Delgado, R. M. Gonzalez; Maza, J.; Perez, E. et al. (2003-11-28), "Long slit spectroscopy of a sample of isolated spirals with and without an AGN", Astronomy & Astrophysics 416 (2): 475–498, doi:10.1051/0004-6361:20034108, arXiv:astro-ph/0311616 
  8. ↑ Looze, Ilse De; Cormier, Diane; Lebouteiller, Vianney; Madden, Suzanne; Baes, Maarten; Bendo, George J.; Boquien, Médéric; Boselli, Alessandro et al. (2014-08-01). "The applicability of far-infrared fine-structure lines as star formation rate tracers over wide ranges of metallicities and galaxy types" (in en). Astronomy & Astrophysics 568: A62. doi:10.1051/0004-6361/201322489. ISSN 0004-6361. Bibcode: 2014A&A...568A..62D. https://www.aanda.org/articles/aa/pdf/2014/08/aa22489-13.pdf. 
  9. ↑ Maia, M. a. G.; da Costa, L. N.; Willmer, C.; Pellegrini, P. S.; Rite, C. (March 1987). "New Southern Galaxies with Active Nuclei" (in en). The Astronomical Journal 93: 546. doi:10.1086/114336. ISSN 0004-6256. Bibcode: 1987AJ.....93..546M. https://articles.adsabs.harvard.edu/pdf/1987AJ.....93..546M. 
  10. ↑ Cid Fernandes, Roberto; Storchi-Bergmann, Thaisa; Schmitt, Henrique R. (June 1998). "The Stellar Content of Active Galaxies" (in en). Monthly Notices of the Royal Astronomical Society 297 (2): 579–616. doi:10.1046/j.1365-8711.1998.01519.x. ISSN 0035-8711. Bibcode: 1998MNRAS.297..579C. 
  11. ↑ Fehmers, G. C.; de Grijp, M. H. K.; Miley, G. K.; Keel, W. C. (November 1994). "Warm IRAS sources from the point source catalog. IV. Extended optical line emission." (in en). Astronomy and Astrophysics Supplement Series 108: 61–67. ISSN 0365-0138. https://articles.adsabs.harvard.edu/pdf/1994A%26AS..108...61F. 
  12. ↑ Winkler, H. (August 1992). "Variability studies of Seyfert galaxies - II. Spectroscopy." (in en). Monthly Notices of the Royal Astronomical Society 257 (4): 677–688. doi:10.1093/mnras/257.4.677. ISSN 0035-8711. https://articles.adsabs.harvard.edu/pdf/1992MNRAS.257..677W. 
  13. ↑ Dopita, Michael A.; Shastri, Prajval; Davies, Rebecca; Kewley, Lisa; Hampton, Elise; Scharwächter, Julia; Sutherland, Ralph; Kharb, Preeti et al. (March 2015). "Probing the Physics of Narrow Line Regions in Active Galaxies. II. The Siding Spring Southern Seyfert Spectroscopic Snapshot Survey (S7)" (in en). The Astrophysical Journal Supplement Series 217 (1): 12. doi:10.1088/0067-0049/217/1/12. ISSN 0067-0049. Bibcode: 2015ApJS..217...12D. 



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