NGC 1106

Coordinates: Sky map 02h 50m 40.51s, +41° 40′ 17.4″
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NGC 1106
Observation data (J2000 epoch)
Right ascension02h 50m 40.51s[1]
Declination+41° 40′ 17.4″[1]
Redshift0.014467 ± 0.000063[1]
Heliocentric radial velocity4337 ± 19 km/s[1]
Distance~199 ± 14 · 106 Mly[1] (61.0 ± 4.3 Mpc)
Apparent magnitude (V)12.5[1]
Apparent magnitude (B)13.5[1]
Surface brightness12.7 mag/arcmin2[1]
Characteristics
Apparent size (V)1.30 x 1.0 arcmin[1]
Other designations
UGC 2322, MCG 7-6-76, ZWG 539.112,
PGC 10792, IRAS 02474+4127

NGC 1106 is a lenticular, non-barred spiral galaxy with considerable structure (type SA0^+), located in the Perseus constellation.[1][2] It was first observed by astronomer John Herschel in 1828.[3]

Characteristics[edit]

In 2016, astronomers confirmed NGC 1106 contains a Compton-thick[4] active galactic nucleus, after extensive analysis of the galaxy's X-ray spectra.[5] Due to the AGN in its center, it's also classified as a type II Seyfert galaxy, meaning it has the characteristic bright core of a Seyfert galaxy, as well as appearing bright when viewed at infrared wavelengths.

Star formation[edit]

A study released in 2022 detected active star formation in NGC 1106.[6] The research involved the use of far-ultraviolet and mid-infrared analysis, both techniques are extensively used as star formation rate tracers.[7]

See also[edit]

Other Seyfert galaxies include:

References[edit]

  1. ^ a b c d e f g h i j "Revised NGC Data for NGC 1106". spider.seds.org. Retrieved 2023-12-02.
  2. ^ "NASA/IPAC Extragalactic Database's result for NGC 1106". ned.ipac.caltech.edu. Retrieved 2023-12-02.
  3. ^ "Dreyer". www.klima-luft.de. Retrieved 2023-12-02.
  4. ^ "Compton Thick AGN: The dark side of the X-ray background - A. Comastri". ned.ipac.caltech.edu. Retrieved 2023-12-03.
  5. ^ Tanimoto, Atsushi; Ueda, Yoshihiro; Kawamuro, Taiki; Ricci, Claudio (2016-06-01). "Suzaku follow-up of heavily obscured active galactic nuclei detected in Swift/BAT survey: NGC 1106, UGC 03752, and NGC 2788A". Publications of the Astronomical Society of Japan. 68: S26. arXiv:1601.05056. Bibcode:2016PASJ...68S..26T. doi:10.1093/pasj/psw008. ISSN 0004-6264.
  6. ^ Kolokythas, Konstantinos; Vaddi, Sravani; O'Sullivan, Ewan; Loubser, Ilani; Babul, Arif; Raychaudhury, Somak; Lagos, Patricio; Jarrett, Thomas H. (2022-03-01). "The Complete Local-Volume Groups Sample - IV. Star formation and gas content in group-dominant galaxies". Monthly Notices of the Royal Astronomical Society. 510 (3): 4191–4207. arXiv:2112.08498. Bibcode:2022MNRAS.510.4191K. doi:10.1093/mnras/stab3699. ISSN 0035-8711.
  7. ^ Brown, M. J. I.; Moustakas, J.; Jarrett, T. H.; Cluver, M. (2018). "The Ultraviolet–Infrared Color–Magnitude Relation of Star-forming Galaxies". Research Notes of the AAS. 2 (4): 217. arXiv:1811.05638. Bibcode:2018RNAAS...2..217B. doi:10.3847/2515-5172/aaf21c. ISSN 2515-5172.


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