Markarian 382
From Wikipedia, the free encyclopedia
| Markarian 382 | |
|---|---|
 SDSS image of Markarian 382 | |
| Observation data (J2000 epoch) | |
| Constellation | Lynx |
| Right ascension | 07h 55m 25.29s[1] |
| Declination | +39° 11′ 09.90″[1] |
| Redshift | 0.033165[1] |
| Heliocentric radial velocity | 9,943 km/s ± 14[1] |
| Distance | 474 Mly |
| Apparent magnitude (V) | 16.11 |
| Apparent magnitude (B) | 16.45 |
| Characteristics | |
| Type | Sc(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]
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 × 107 M☉.[10] A study published in December 2022, has estimated the black hole as 6.50+0.19-0.29 M☉ 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 2 3 4 5 6 7 8 "NED Search results for Markarian 382". NASA/IPAC Extragalactic Database. Retrieved 2025-12-21.
- 1 2 P., Singh, K.; R., Rao, A.; N., Vahia, M. (August 1992). "EXOSAT measurement of the spectrum of Markarian 382". Astronomy and Astrophysics. 262: 49. Bibcode:1992A&A...262...49S. ISSN 0004-6361.
{{cite journal}}: CS1 maint: multiple names: authors list (link) - ↑ de Bruyn, A. G.; Wilson, A. S. (November 1976). "A 1415 MHz Survey of Seyfert and Related Galaxies". Astronomy and Astrophysics. 53: 93. Bibcode:1976A&A....53...93D. ISSN 0004-6361.
- ↑ Véron-Cetty, M.-P.; Véron, P.; Gonçalves, A. C. (June 2001). "A spectrophotometric atlas of Narrow-Line Seyfert 1 galaxies". Astronomy and Astrophysics. 372 (3): 730–754. arXiv:astro-ph/0104151. Bibcode:2001A&A...372..730V. doi:10.1051/0004-6361:20010489. ISSN 0004-6361.
- ↑ 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.
- ↑ Malkan, Matthew A.; Gorjian, Varoujan; Tam, Raymond (July 1998). "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. ISSN 0067-0049.
- ↑ 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". The Astrophysical Journal Supplement Series. 232 (2): 21. arXiv:1710.02194. Bibcode:2017ApJS..232...21K. doi:10.3847/1538-4365/aa8a75. ISSN 0067-0049.
- ↑ 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". Astronomy and Astrophysics. 526: A43. arXiv:1011.1772. Bibcode:2011A&A...526A..43S. doi:10.1051/0004-6361/200913243. ISSN 0004-6361.
- ↑ 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". The Astronomical Journal. 132 (1): 321–346. arXiv:astro-ph/0603806. Bibcode:2006AJ....132..321D. doi:10.1086/504894. ISSN 0004-6256.
- ↑ 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, arXiv:astro-ph/0402627, Bibcode:2004AJ....127.3168B, doi:10.1086/420803
- ↑ Tortosa, Alessia; Ricci, Claudio; Ho, Luis C; Tombesi, Francesco; Du, Pu; Inayoshi, Kohei; Wang, Jian-Min; Shangguan, Jinyi; Li, Ruancun (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. arXiv:2212.06183. doi:10.1093/mnras/stac3590. ISSN 0035-8711.
- ↑ 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. arXiv:2308.10992. Bibcode:2023ApJ...954..115K. doi:10.3847/1538-4357/ace329. ISSN 0004-637X.
