Astronomy:Markarian 382

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Markarian 382
SDSS image of Markarian 382
Observation data (J2000 epoch)
ConstellationLynx
Right ascension 07h 55m 25.29s[1]
Declination+39° 11′ 09.90″[1]
Redshift0.033165[1]
Helio radial velocity9,943 km/s ± 14[1]
Distance474 Mly
Apparent magnitude (V)16.11
Apparent magnitude (B)16.45
Characteristics
TypeSc(r);Sy1 Sbrst [1]
Size~142,200 ly (43.61 kpc) (estimated)[1]
Other designations
CGCG 207-005, KIG 0214, PGC 22190, MCG +07-17-001, SIG 0319, UNAM-KIAS 0045, KUG 0752+393, IRAS F07520+3918, MRK 382[1]

Markarian 382 is a Type 1 Seyfert galaxy[2] with an active galactic nucleus, located in the constellation of Lynx. The redshift of the galaxy is (z) 0.0331[1] and it was first discovered in the 1415 GHz survey by A.G. de Bruyn and A.S. Wilson in November 1976.[3] This galaxy has been classified as radio-quiet.[2]

Description

Markarian 382 has been specifically categorized as a narrow-line Seyfert galaxy.[4] It is known to be X-ray variable with two flux states shown on high and low levels. When it underwent a high flux state, its optical spectrum has a soft appearance, which is mainly characterized by a low fractional variability state displayed in X-ray bands. When reaching a low flux state, the spectrum is the opposite.[5]

The host galaxy of Markarian 382 is a barred spiral galaxy of type SBa based on imaging made with Hubble Space Telescope (HST), modeled by a single bulge and disk showing presence of spiral arms.[6][7] When imaged, it is found to display a bar surrounded by a ring feature, with its spiral structure forming a pseudo-ring on its outer side.[8] There is also a presence of a dust lane found to be curved and located northwest from the central bright nucleus, and also along the edge of a stellar bar.[9]

The central supermassive black hole of Markarian 382 is estimated to be 0.90 ± 0.12 x 107 Mʘ.[10] A study published in December 2022, has estimated the black hole as 6.50+0.19-0.29 Mʘ instead with an Eddington luminosity of 0.81 LEdd. When observed in energy band, the X-ray spectrum contains two warm absorbing components with turbulent velocities of 100 and 100 kilometers per seconds.[11]

An absorption system is found around Markarian 382. When observed, it is found to be made up of at least four velocity components. Upon further observations, there are two H I components classified as weak with measured column densities of around 1012.8 and 1013.3 cm−2 and blueshifted velocities of -62 and -228 kilometer per seconds. Doubly ionized silicon absorption has also been detected in additional.[12]

References

  1. ↑ 1.0 1.1 1.2 1.3 1.4 1.5 1.6 1.7 "NED Search results for Markarian 382". https://ned.ipac.caltech.edu/byname?objname=Markarian+382&hconst=67.8&omegam=0.308&omegav=0.692&wmap=4&corr_z=1. 
  2. ↑ 2.0 2.1 P., Singh, K.; R., Rao, A.; N., Vahia, M. (August 1992). "EXOSAT measurement of the spectrum of Markarian 382." (in en). Astronomy and Astrophysics 262: 49. ISSN 0004-6361. Bibcode: 1992A&A...262...49S. https://articles.adsabs.harvard.edu/full/1992A%26A...262...49S. 
  3. ↑ de Bruyn, A. G.; Wilson, A. S. (November 1976). "A 1415 MHz Survey of Seyfert and Related Galaxies" (in en). Astronomy and Astrophysics 53: 93. ISSN 0004-6361. Bibcode: 1976A&A....53...93D. https://articles.adsabs.harvard.edu/pdf/1976A%26A....53...93D. 
  4. ↑ Véron-Cetty, M.-P.; Véron, P.; Gonçalves, A. C. (June 2001). "A spectrophotometric atlas of Narrow-Line Seyfert 1 galaxies" (in en). Astronomy and Astrophysics 372 (3): 730–754. doi:10.1051/0004-6361:20010489. ISSN 0004-6361. Bibcode: 2001A&A...372..730V. https://ui.adsabs.harvard.edu/abs/2001A&A...372..730V/abstract. 
  5. ↑ Xu, Xinpeng; Ding, Nan; Gu, Qiusheng (2025-10-06). "The analysis of the soft X-ray excess in the narrow-line Seyfert 1 galaxy Mrk 382". Monthly Notices of the Royal Astronomical Society 543 (4): 3981–3992. doi:10.1093/mnras/staf1682. ISSN 0035-8711. 
  6. ↑ Malkan, Matthew A.; Gorjian, Varoujan; Tam, Raymond (July 1998). "A Hubble Space Telescope Imaging Survey of Nearby Active Galactic Nuclei" (in en). The Astrophysical Journal Supplement Series 117 (1): 25–88. doi:10.1086/313110. ISSN 0067-0049. Bibcode: 1998ApJS..117...25M. 
  7. ↑ Kim, Minjin; Ho, Luis C.; Peng, Chien Y.; Barth, Aaron J.; Im, Myungshin (October 2017). "Stellar Photometric Structures of the Host Galaxies of Nearby Type 1 Active Galactic Nuclei" (in en). The Astrophysical Journal Supplement Series 232 (2): 21. doi:10.3847/1538-4365/aa8a75. ISSN 0067-0049. Bibcode: 2017ApJS..232...21K. 
  8. ↑ Slavcheva-Mihova, L.; Mihov, B. (February 2011). "Optical multiband surface photometry of a sample of Seyfert galaxies. I. Large-scale morphology and local environment analysis of matched Seyfert and inactive galaxy samples" (in en). Astronomy and Astrophysics 526: A43. doi:10.1051/0004-6361/200913243. ISSN 0004-6361. Bibcode: 2011A&A...526A..43S. 
  9. ↑ Deo, R. P.; Crenshaw, D. M.; Kraemer, S. B. (July 2006). "The Host Galaxies of Narrow-Line Seyfert 1 Galaxies: Nuclear Dust Morphology and Starburst Rings" (in en). The Astronomical Journal 132 (1): 321–346. doi:10.1086/504894. ISSN 0004-6256. Bibcode: 2006AJ....132..321D. 
  10. ↑ Botte, V.; Ciroi, S.; Rafanelli, P.; Mille, F. Di (2004-02-26), "Exploring Narrow-Line Seyfert 1 Galaxies through the Physical Properties of Their Hosts", The Astronomical Journal 127 (6): 3168–3179, doi:10.1086/420803, Bibcode: 2004AJ....127.3168B 
  11. ↑ Tortosa, Alessia; Ricci, Claudio; Ho, Luis C; Tombesi, Francesco; Du, Pu; Inayoshi, Kohei; Wang, Jian-Min; Shangguan, Jinyi et al. (2022-12-08). "Systematic broad-band X-ray study of super-Eddington accretion on to supermassive black holes – I. X-ray continuum". Monthly Notices of the Royal Astronomical Society 519 (4): 6267–6283. doi:10.1093/mnras/stac3590. ISSN 0035-8711. 
  12. ↑ Klimenko, Viacheslav V.; Kulkarni, Varsha; Wake, David A.; Poudel, Suraj; Bershady, Matthew A.; Péroux, Celine; Lundgren, Britt (2023-08-28). "The Baryonic Content of Galaxies Mapped by MaNGA and the Gas Around Them". The Astrophysical Journal 954 (2): 115. doi:10.3847/1538-4357/ace329. ISSN 0004-637X. Bibcode: 2023ApJ...954..115K. 



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