NGC 1106

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NGC 1106
NGC 1106 PanS.jpg
Observation data (J2000 epoch)
Right ascension 02h 50m 40.51s [1]
Declination +41° 40′ 17.4″ [1]
Redshift 0.014467 ± 0.000063 [1]
Heliocentric radial velocity 4337 ± 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 brightness 12.7 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]

Contents

Characteristics

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

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

Other Seyfert galaxies include:

Related Research Articles

An active galactic nucleus (AGN) is a compact region at the center of a galaxy that emits a significant amount of energy across the electromagnetic spectrum, with characteristics indicating that the luminosity is not produced by stars. Such excess, non-stellar emissions have been observed in the radio, microwave, infrared, optical, ultra-violet, X-ray and gamma ray wavebands. A galaxy hosting an AGN is called an active galaxy. The non-stellar radiation from an AGN is theorized to result from the accretion of matter by a supermassive black hole at the center of its host galaxy.

<span class="mw-page-title-main">Messier 77</span> Barred spiral galaxy in the constellation Cetus

Messier 77 (M77), also known as NGC 1068 or the Squid Galaxy, is a barred spiral galaxy in the constellation Cetus. It is about 47 million light-years (14 Mpc) away from Earth. Messier 77 was discovered by Pierre Méchain in 1780, who originally described it as a nebula. Méchain then communicated his discovery to Charles Messier, who subsequently listed the object in his catalog. Both Messier and William Herschel described this galaxy as a star cluster. Today, however, the object is known to be a galaxy.

<span class="mw-page-title-main">NGC 6946</span> Galaxy in the constellations Cepheus & Cygnus

NGC 6946, sometimes referred to as the Fireworks Galaxy, is a face-on intermediate spiral galaxy with a small bright nucleus, whose location in the sky straddles the boundary between the northern constellations of Cepheus and Cygnus. Its distance from Earth is about 25.2 million light-years or 7.72 megaparsecs, similar to the distance of M101 in the constellation Ursa Major. Both were once considered to be part of the Local Group, but are now known to be among the dozen bright spiral galaxies near the Milky Way but beyond the confines of the Local Group. NGC 6946 lies within the Virgo Supercluster.

<span class="mw-page-title-main">NGC 520</span> Pair of colliding spiral galaxies in the constellation Pisces

NGC 520 is a pair of colliding spiral galaxies about 105 million light-years away in the constellation Pisces. They were discovered by astronomer William Herschel on 13 December 1784.

<span class="mw-page-title-main">Low-ionization nuclear emission-line region</span> Type of galactic nucleus

A low-ionization nuclear emission-line region (LINER) is a type of galactic nucleus that is defined by its spectral line emission. The spectra typically include line emission from weakly ionized or neutral atoms, such as O, O+, N+, and S+. Conversely, the spectral line emission from strongly ionized atoms, such as O++, Ne++, and He+, is relatively weak. The class of galactic nuclei was first identified by Timothy Heckman in the third of a series of papers on the spectra of galactic nuclei that were published in 1980.

<span class="mw-page-title-main">Ionization cone</span> Astronomical phenomenon

Ionization cones are cones of ionized material extending from active galactic nuclei, predominantly observed in type II Seyfert galaxies. They are detected through their emission of electromagnetic radiation in the visible and infrared parts of the spectrum. The main method of observation is through spectroscopy, using spectral line analysis to measure the shape of the ionized region and the condition of the material such as temperature, density, composition, and degree of ionization.

<span class="mw-page-title-main">NGC 2623</span> Interacting galaxy in the constellation Cancer

NGC 2623/Arp 243 is an interacting galaxy located in the constellation Cancer. NGC 2623 is the result of two spiral galaxies that have merged. Scientists believe that this situation is similar to what will occur to the Milky Way, which contains the Solar System, and the neighboring galaxy, the Andromeda Galaxy in four billion years. Studying this galaxy and its properties have provided scientists with a better idea of the coming collision of the Milky Way and the Andromeda. Due to NGC 2623 being in the late stage of merging, the compression of the gas within the galaxy has led to a large amount of star formation, and to its unique structure of a bright core with two extending tidal tails.

<span class="mw-page-title-main">NGC 6810</span> Galaxy in the constellation of Pavo

NGC 6810 is a spiral galaxy approximately 87 million light-years away from Earth in the constellation of Pavo.

<span class="mw-page-title-main">NGC 3860</span> Spiral galaxy in the constellation Leo

NGC 3860 is a spiral galaxy located about 340 million light-years away in the constellation Leo. NGC 3860 was discovered by astronomer William Herschel on April 27, 1785. The galaxy is a member of the Leo Cluster and is a low-luminosity AGN (LLAGN). Gavazzi et al. however classified NGC 3860 as a strong AGN which may have been triggered by a supermassive black hole in the center of the galaxy.

<span class="mw-page-title-main">NGC 3883</span> Galaxy in the constellation Leo

NGC 3883 is a large low surface brightness spiral galaxy located about 330 million light-years away in the constellation Leo. NGC 3883 has a prominent bulge but does not host an AGN. The galaxy also has flocculent spiral arms in its disk. It was discovered by astronomer William Herschel on April 13, 1785 and is a member of the Leo Cluster.

<span class="mw-page-title-main">NGC 3884</span> Spiral galaxy in the constellation Leo

NGC 3884 is a spiral galaxy located about 330 million light-years away in the constellation Leo. The galaxy was discovered by astronomer William Herschel on April 27, 1785 and is a member of the Leo Cluster.

<span class="mw-page-title-main">NGC 708</span> Galaxy in the constellation Andromeda

NGC 708 is an elliptical galaxy located 240 million light-years away in the constellation Andromeda and was discovered by astronomer William Herschel on September 21, 1786. It is classified as a cD galaxy and is the brightest member of Abell 262. NGC 708 is a weak FR I radio galaxy and is also classified as a type 2 Seyfert galaxy.

<span class="mw-page-title-main">NGC 7469</span> Galaxy located in the constellation Pegasus

NGC 7469 is an intermediate spiral galaxy in the constellation of Pegasus. NGC 7469 is located about 200 million light-years away from Earth, which means, given its apparent dimensions, that NGC 7469 is approximately 90,000 light-years across. It was discovered by William Herschel on November 12, 1784.

<span class="mw-page-title-main">NGC 3367</span> Spiral galaxy in the constellation Leo

NGC 3367 is a barred spiral galaxy located in the constellation Leo. It is located at a distance of about 120 million light years from Earth, which, given its apparent dimensions, means that NGC 3367 is about 85,000 light years across. It was discovered by William Herschel on March 19, 1784.

<span class="mw-page-title-main">NGC 4939</span> Spiral galaxy in the constellation Virgo

NGC 4939 is a spiral galaxy located in the constellation Virgo. It is located at a distance of about 120 million light years from Earth, which, given its apparent dimensions, means that NGC 4939 is about 190,000 light years across. It was discovered by William Herschel on March 25, 1786.

<span class="mw-page-title-main">NGC 7130</span> Galaxy in the constellation Piscis Austrinus

NGC 7130 is a spiral galaxy located in the constellation Piscis Austrinus. It is located at a distance of about 220 million light years from Earth, which, given its apparent dimensions, means that NGC 7130 is about 100,000 light years across. It was discovered by John Herschel on September 25, 1834, and discovered independently by Lewis Swift on September 17, 1897. The location of the galaxy given in the New General Catalogue was off by 30 arcminutes in declination from the location of the galaxy.

<span class="mw-page-title-main">NGC 1386</span> Galaxy in the constellation Eridanus

NGC 1386 is a spiral galaxy located in the constellation Eridanus. It is located at a distance of circa 53 million light years from Earth, which, given its apparent dimensions, means that NGC 1386 is about 50,000 light years across. It is a Seyfert galaxy, the only one in Fornax Cluster.

<span class="mw-page-title-main">NGC 4074</span> Galaxy in the constellation Coma Berenices

NGC 4074 is a peculiar lenticular galaxy located 310 million light-years away in the constellation Coma Berenices. It was discovered by astronomer William Herschel on April 27, 1785 and is a member of the NGC 4065 Group.

<span class="mw-page-title-main">NGC 7592</span> Interacting galaxy system in the constellation Aquarius

NGC 7592 is an interacting galaxy system located 300 million light years away in the constellation Aquarius. It was discovered by William Herschel on September 20, 1784. The total infrared luminosity is 1011.33 L☉, and thus it is categorised as a luminous infrared galaxy. One of the galaxies hosts a type 2 Seyfert nucleus.

<span class="mw-page-title-main">NGC 5135</span>

NGC 5135 is a barred spiral galaxy located in the constellation Hydra. It is located at a distance of about 200 million light years from Earth. It was discovered by John Herschel on May 8, 1834. It is a Seyfert galaxy.

References

  1. 1 2 3 4 5 6 7 8 9 10 "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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