Astronomy:NGC 7212

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NGC 7212
NGC 7212
NGC 7212 image by SDSS
Observation data (J2000 epoch)
ConstellationPegasus
Right ascension 22h 07m 02.0808s[1]
Declination+10° 14′ 03.154″[1]
Redshift0.026632[1]
Helio radial velocity7,984 km/s ± 21[1]
Distance369 Mly
Apparent magnitude (V)14.1[2]
Characteristics
TypeSab; Sy2[1]
Size~112,200 ly (34.40 kpc) (estimated)[1]
Other designations
CGCG 428-032, CGCG 2204.6+1000, MCG +02-56-011, IRAS 22045+0959, PGC 68065[1] UGC 11910

NGC 7212 is a spiral galaxy located in the constellation Pegasus. It is about 369 million light-years from Earth.[1] It was discovered on October 2, 1886, by the astronomer Lewis A. Swift.[3] It is also classified as a Seyfert galaxy[4] and such contains an extended emission-line region (EELR).[5]

Description

NGC 7212 is classified to be part of an interacting system of three galaxies, of which two are of them are found to be merging together.[6][4] The nucleus is found active and it has been categorized as a Seyfert galaxy of Type 2 based on the discovery of weak hydrogen beta emission lines.[7][6] A study published in February 1995, has found it has a presence of a jet-like feature being shown as both ionized and extended from the nucleus region by around 10 arcseconds, with an orientation of 170°.[8]

In 2020, X-ray emission was found in NGC 7212 by Chandra X-ray Observatory. When observed, the emission is described as extended on kiloparsec scales and diffused, with 20% of it being located outside of the central radius.[9] Imaging with Hubble Space Telescope (HST), also found there are also detections of doubly ionized oxygen emission mainly made up of several blob components located both north and south from the nucleus.[10]

Galaxy Triplet

NGC 7212 imaged by Hubble Space Telescope

NGC 7212 is part of a triplet of galaxies, at the center of which it lies. The galaxy to the northeast is PGC 6728403. The second, located to the southwest, is 2MASS J22070015+1013286. The first two galaxies show clear signs of gravitational interaction. As for the third, further south, its distance from Hubble remains unknown, and it may well be a background galaxy[11]

Supermassive black hole

A study conducted in 2007 with 90 Seyfert 2-type galaxies using velocity dispersion allowed scientists to estimate the mass of their central supermassive black holes. For NGC 7212, the mass of the black hole is equal to 30 × 10⁶ M☉.[12]

According to an article published in 2012, Several studies of velocity dispersion in the central region have allowed its mass to be estimated at 3.2 × 10⁷ M☉.[13]

References

  1. ↑ 1.0 1.1 1.2 1.3 1.4 1.5 1.6 1.7 "NED Search results for NGC 7212". https://ned.ipac.caltech.edu/byname?objname=NGC+7212&hconst=67.8&omegam=0.308&omegav=0.692&wmap=4&corr_z=1. 
  2. ↑ "Revised NGC Data for NGC 7212". http://spider.seds.org/ngc/revngcic.cgi?NGC7212. 
  3. ↑ "NGC Objects: NGC 7200 - 7249". https://cseligman.com/text/atlas/ngc72.htm#7212. 
  4. ↑ 4.0 4.1 Contini, M.; Cracco, V.; Ciroi, S.; Mura, G. La (2012-09-01). "Distribution of the heavy elements throughout the extended narrow-line region of the Seyfert galaxy NGC 7212" (in en). Astronomy & Astrophysics 545: A72. doi:10.1051/0004-6361/201219184. ISSN 0004-6361. Bibcode: 2012A&A...545A..72C. https://www.aanda.org/articles/aa/abs/2012/09/aa19184-12/aa19184-12.html. 
  5. ↑ Cracco, V.; Ciroi, S.; Di Mille, F.; Vaona, L.; Frassati, A.; Smirnova, A. A.; La Mura, G.; Moiseev, A. V. et al. (2011-10-24). "The origin of gas in extended narrow-line regions of nearby Seyfert galaxies - I. NGC 7212". Monthly Notices of the Royal Astronomical Society 418 (4): 2630–2641. doi:10.1111/j.1365-2966.2011.19654.x. ISSN 0035-8711. Bibcode: 2011MNRAS.418.2630C. 
  6. ↑ 6.0 6.1 Wasilewski, A. J. (October 1981). "A new Seyfert galaxy with asymmetric forbidden-line profiles in an interacting system". Publications of the Astronomical Society of the Pacific 93: 560. doi:10.1086/130887. ISSN 0004-6280. Bibcode: 1981PASP...93..560W. https://doi.org/10.1086/130887. 
  7. ↑ Congiu, E.; Contini, M.; Ciroi, S.; Cracco, V.; Berton, M.; Di Mille, F.; Frezzato, M.; La Mura, G. et al. (2017-06-29). "High-resolution spectroscopy of the extended narrow-line region of IC 5063 and NGC 7212". Monthly Notices of the Royal Astronomical Society 471 (1): 562–588. doi:10.1093/mnras/stx1628. ISSN 0035-8711. 
  8. ↑ Tran, Hien D. (February 1995). "The Nature of Seyfert 2 Galaxies with Obscured Broad-Line Regions. II. Individual Objects". The Astrophysical Journal 440: 578. doi:10.1086/175297. ISSN 0004-637X. Bibcode: 1995ApJ...440..578T. https://articles.adsabs.harvard.edu//full/1995ApJ...440..578T/0000587.000.html. 
  9. ↑ Jones, Mackenzie L.; Fabbiano, G.; Elvis, Martin; Paggi, A.; Karovska, M.; Maksym, W. P.; Siemiginowska, A.; Raymond, J. (2020-03-10). "Chandra Observations of NGC 7212: Large-scale Extended Hard X-Ray Emission". The Astrophysical Journal 891 (2): 133. doi:10.3847/1538-4357/ab76c8. ISSN 0004-637X. Bibcode: 2020ApJ...891..133J. 
  10. ↑ Schmitt, H. R.; Donley, J. L.; Antonucci, R. R. J.; Hutchings, J. B.; Kinney, A. L. (October 2003). "A Hubble Space Telescope Survey of Extended [Oiii] λ5007 Emission in a Far-Infrared Selected Sample of Seyfert Galaxies: Observations" (in en). The Astrophysical Journal Supplement Series 148 (2): 327–352. doi:10.1086/377440. ISSN 0067-0049. Bibcode: 2003ApJS..148..327S. 
  11. ↑ "NGC 7212 - Galaxy Triplet in Pegasus". https://theskylive.com/sky/deepsky/ngc7212-object. 
  12. ↑ Bian, W.; Gu, Q. (March 2007). "The Eddington Ratios in Seyfert 2 Galaxies with and without Hidden Broad-Line Regions" (in en). The Astrophysical Journal 657 (1): 159–166. doi:10.1086/510708. ISSN 0004-637X. Bibcode: 2007ApJ...657..159B. https://iopscience.iop.org/article/10.1086/510708. 
  13. ↑ Marinucci, Andrea; Bianchi, Stefano; Nicastro, Fabrizio; Matt, Giorgio; Goulding, Andy D. (2012-04-01). "The Link Between the Hidden Broad Line Region and the Accretion Rate in Seyfert 2 Galaxies". The Astrophysical Journal 748 (2): 130. doi:10.1088/0004-637X/748/2/130. ISSN 0004-637X. Bibcode: 2012ApJ...748..130M. https://iopscience.iop.org/article/10.1088/0004-637X/748/2/130. 



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