NGC 3367

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NGC 3367
NGC 3367 - Sn1992c a.jpg
NGC 3367 with SN 1992C by ESO
Observation data (J2000 epoch)
Constellation Leo
Right ascension 10h 46m 35.0s [1]
Declination +13° 45′ 03″ [1]
Redshift 0.010142 +/- 0.000024 [1]
Helio radial velocity 3040 ± 7 km/s [1]
Distance 113 ± 22 Mly (34.8 ± 6.7 Mpc) [1]
Apparent magnitude  (V)11.4 [2]
Characteristics
Type SB(rs)c [1]
Apparent size  (V)2.5′ × 2.4′ [2]
Other designations
UGC 5880, CGCG 066-011, MCG +02-28-005, PGC 32178 [1]

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. [3]

Contents

Characteristics

NGC 3367 is a barred spiral galaxy with an asymmetric shape seen nearly face-on, with an inclination of 25 degrees. [4] The inner arms begin at the ends of the bar, forming a ring with a major axis of 0.9 arcseconds, [5] and after half of a revolution start to branch, creating a multiple-arm structure. They are studded with many bright HII regions. [6] The star formation rate in NGC 3367 is nearly 3 M☉ per year. The outer arms form a semi-circular arch towards the south, at a distance of 50 arcseconds from the centre, more visible in the ultraviolet. [4]

Usually, asymmetry in a galaxy is caused by interaction with other galaxies, but no large satellite has been detected near NGC 3367. The cause of the asymmetry is assumed to be a minor merger or mass accretion that took place in the last billion years. Because no low surface brightness structures, like plumes and star streams, have been detected near NGC 3367, and nor is gas seen in HI imaging near the galaxy, it is believed that the galaxy accreted cold gas in the past million years. This gas accretion resulted in increased star formation and nuclear activity. [4]

NGC 3367 features a strong bar. The bar pattern speed was estimated to be 43 ± 6 km s−1 kpc−1 using the Tremaine-Weinberg method. [7] The bar of the galaxy is more prominent in the near infrared, suggesting the dominance of an old population of stars in that region. There is also a knot at the eastern end of the bar, where there is a non-negligible population of red giants and asymptotic giant branch stars. [4]

Nucleus

NGC 3367 has been categorised as a HII region or a type 2 Seyfert galaxy. However, optically there is no hint of an active galactic nucleus (AGN). The spectrum of NGC 3367 features unusually broad lines (FWHM of 490 m/s for Hβ) and a blue asymmetry. The spectrum looks like one produced from Wolf-Rayet stars. [8] There is no clear evidence of H-alpha emission. [9] The spectrum is also dominated by starburst features like low [Fe II] 1.2567 μm/Paβ line ratio. [10] The galaxy was observed by the Spitzer Space Telescope and [Ne v] 14.3 and 24.3 μm lines, consistent with the existence of a weak AGN were detected. [11] Observed by the XMM-Newton telescope, the galaxy's X-ray luminosity in 2-10 keV was 2.0 × 1040 erg s−1 dominated by a power law. This value is consistent with low-luminosity AGNs. [12]

When observed in radio waves, the galaxy features two radio lobes extending from a nuclear source, a feature common to Seyfert 2 galaxies. The emission of the southwest lobe is polarised, indicating it is above the plain of the disk, while the northeast is depolarised. The southwest lobe extends 26" from the nucleus and the northeast 33". The total extent of the source is approximately 12 kpc at the distance of the galaxy. [13] More detailed observations by the Very Large Array revealed a radio jet connecting the nucleus with the southwest lobe and a circumnuclear structure with a radius of nearly 300 pc. [14]

In the centre of the galaxy lies a supermassive black hole whose mass is estimated to be 15×106 (107.2) M☉ based on Ks bulge luminosity. [15] The X-ray spectra of the galaxy suggested the mass of the supermassive black hole to be in the range of 105 to 107M☉. [12]

Around the nucleus, at a radius of circa 2 arcseconds, has been detected using CO(1-0) emission a significant amount of molecular gas. The total mass of molecular gas in that region is estimated to be 3×108M☉ and in the central 5 arcseconds the mass of molecular gas is 5.9×108M☉. The presence of such a large mass could obscure the optical emission lines from an active galactic nucleus. The CO emission has an elongated shape, maybe due to the forces created by the stellar bar. [16]

Supernovae

Six supernovae have been observed in NGC 3367: SN 1986A (type Ia, mag 14.0), SN 1992C (type II, mag. 16.5), SN 2003aa (type Ic, mag. 17.6), SN 2007am (type II, mag. 17.8), SN 2018kp (type Ia, mag. 19.9) and SN 2022ewj (type II, mag. 16.3). [17] [18] SN 1992c was discovered by ESO astronomer Hans van Winckel on January 28, 1992. He found it on a photographic plate obtained by Guido Pizarro during a search programme carried out with the ESO 1-metre Schmidt telescope at La Silla. Spectra of the supernova, obtained by Della Valle and Christoffel Waelkens (Astronomical Institute of Leuven, Belgium), with the 2.2-metre telescope at La Silla, showed it to be of type II and that the explosion must have happened between 10 and 20 days earlier. The expansion velocity was measured at about 7000 km/sec. SN 1992c was located southeast of the centre of the galaxy, at the tip of a spiral arm. SN 1986A was found on February 4, 1986 near the condensations in the spiral arms east of the centre of the galaxy. [19]

Nearby galaxies

NGC 3367 is the foremost member in a galaxy group known as the NGC 3367 group. Other members of the group include NGC 3391, and NGC 3419. A bit further away lie the galaxies NGC 3300, and NGC 3306. [20] NGC 3367 lies in the same region of the sky as the Leo Group, whose redshift is about a third of NGC 3367. NGC 3377, a member of the Leo Group, lies 22 arcminutes to the north of NGC 3367. [21]

Related Research Articles

<span class="mw-page-title-main">Seyfert galaxy</span> Class of active galaxies with very bright nuclei

Seyfert galaxies are one of the two largest groups of active galaxies, along with quasars. They have quasar-like nuclei with very high surface brightnesses whose spectra reveal strong, high-ionisation emission lines, but unlike quasars, their host galaxies are clearly detectable.

<span class="mw-page-title-main">NGC 2841</span> Galaxy in the constellation Ursa Major

NGC 2841 is an unbarred spiral galaxy in the northern circumpolar constellation of Ursa Major. It was discovered on 9 March 1788 by German-born astronomer William Herschel. J. L. E. Dreyer, the author of the New General Catalogue, described it as, "very bright, large, very much extended 151°, very suddenly much brighter middle equal to 10th magnitude star". Initially thought to be about 30 million light-years distant, a 2001 Hubble Space Telescope survey of the galaxy's Cepheid variables determined its distance to be approximately 14.1 megaparsecs or 46 million light-years. The optical size of the galaxy is 8.′1 × 3.′5.

<span class="mw-page-title-main">NGC 3227</span> Galaxy in the constellation Leo

NGC 3227 is an intermediate spiral galaxy that is interacting with the dwarf elliptical galaxy NGC 3226. The two galaxies are one of several examples of a spiral with a dwarf elliptical companion that are listed in the Atlas of Peculiar Galaxies. Both galaxies may be found in the constellation Leo. It is a member of the NGC 3227 Group of galaxies, which is a member of the Leo II Groups, a series of galaxies and galaxy clusters strung out from the right edge of the Virgo Supercluster.

<span class="mw-page-title-main">NGC 3226</span> Dwarf elliptical galaxy in the constellation Leo

NGC 3226 is a dwarf elliptical galaxy that is interacting with the spiral galaxy NGC 3227. The two galaxies are one of several examples of a spiral with a dwarf elliptical companion that are listed in the Atlas of Peculiar Galaxies. Both galaxies may be found in the constellation Leo. It is a member of the NGC 3227 Group of galaxies, which is a member of the Leo II Groups, a series of galaxies and galaxy clusters strung out from the right edge of the Virgo Supercluster.

<span class="mw-page-title-main">NGC 5548</span> Type I Seyfert galaxy in the constellation Boötes

NGC 5548 is a Type I Seyfert galaxy with a bright, active nucleus. This activity is caused by matter flowing onto a 65 million solar mass (M☉) supermassive black hole at the core. Morphologically, this is an unbarred lenticular galaxy with tightly-wound spiral arms, while shell and tidal tail features suggest that it has undergone a cosmologically-recent merger or interaction event. NGC 5548 is approximately 245 million light years away and appears in the constellation Boötes. The apparent visual magnitude of NGC 5548 is approximately 13.3 in the V band.

<span class="mw-page-title-main">NGC 5033</span> Galaxy in the constellation Canes Venatici

NGC 5033 is an inclined spiral galaxy located in the constellation Canes Venatici. Distance estimates vary from between 38 and 60 million light years from the Milky Way. The galaxy has a very bright nucleus and a relatively faint disk. Significant warping is visible in the southern half of the disk. The galaxy's relatively large angular size and relatively high surface brightness make it an object that can be viewed and imaged by amateur astronomers. The galaxy's location relatively near Earth and its active galactic nucleus make it a commonly studied object for professional astronomers.

<span class="mw-page-title-main">NGC 5005</span> Galaxy in the constellation Canes Venatici

NGC 5005, also known as Caldwell 29, is an inclined spiral galaxy in the constellation Canes Venatici. The galaxy has a relatively bright nucleus and a bright disk that contains multiple dust lanes. The galaxy's high surface brightness makes it an object that is visible to amateur astronomers using large amateur telescopes.

<span class="mw-page-title-main">NGC 4536</span> Spiral galaxy in the constellation Virgo

NGC 4536 is an intermediate spiral galaxy in the constellation Virgo located about 10° south of the midpoint of the Virgo cluster. However, it is not considered a member of the cluster. Rather, it is a member of the M61 Group of galaxies, which is a member of the Virgo II Groups, a series of galaxies and galaxy clusters strung out from the southern edge of the Virgo Supercluster. The morphological classification in the De Vaucouleurs system is SAB(rs)bc, which indicates it is a weakly barred spiral galaxy with a hint of an inner ring structure plus moderate to loosely wound arms. It does not have a classical bulge around the nucleus.

<span class="mw-page-title-main">NGC 1672</span> Galaxy in the constellation Dorado

NGC 1672 is a barred spiral galaxy located in the constellation Dorado. It was discovered by the astronomer James Dunlop on November 5, 1826. It was originally unclear whether it was a member of the Dorado Group, with some sources finding it to be a member and other sources rejecting its membership. However, recent tip of the red-giant branch (TRGB) measurements indicate that NGC 1672 is located at the same distance as other members, suggesting it is indeed a member of the Dorado Group.

<span class="mw-page-title-main">NGC 7319</span> Galaxy in the constellation Pegasus

NGC 7319 is a highly distorted barred spiral galaxy that is a member of the compact Stephan's Quintet group located in the constellation Pegasus, some 311 megalight-years distant from the Milky Way. The galaxy's arms, dust and gas have been highly disturbed as a result of the interaction with the other members of the Quintet. Nearly all of the neutral hydrogen has been stripped from this galaxy, most likely as a result of a collision with NGC 7320c some 100 million years ago. A pair of long, parallel tidal tails extend southward from NGC 7319 in the direction of NGC 7320c, and is undergoing star formation.

<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 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 7674</span> Galaxy located in the constellation Pegasus

NGC 7674 is a spiral galaxy located in the constellation Pegasus. It is located at a distance of circa 350 million light years from Earth, which, given its apparent dimensions, means that NGC 7674 is about 125,000 light years across. It was discovered by John Herschel on August 16, 1830.

<span class="mw-page-title-main">NGC 985</span> Ring galaxy in the constellation Cetus

NGC 985 is a ring galaxy in the constellation of Cetus. It is located about 550 million light years away from Earth, which means, given its apparent dimensions, that NGC 985 is approximately 160,000 light years across. It was discovered by Francis Leavenworth in 1886. It is a type 1 Seyfert galaxy.

<span class="mw-page-title-main">NGC 6951</span> Galaxy in the constellation Cepheus

NGC 6951 is a barred spiral galaxy located in the constellation Cepheus. It is located at a distance of about 75 million light-years from Earth, which, given its apparent dimensions, means that NGC 6951 is about 100,000 light-years across. It was discovered by Jérôme Eugène Coggia in 1877 and independently by Lewis Swift in 1878.

<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 5363</span> Galaxy in the constellation Virgo

NGC 5363 is a lenticular galaxy located in the constellation Virgo. It is located at a distance of circa 65 million light years from Earth, which, given its apparent dimensions, means that NGC 5363 is about 100,000 light years across. It was discovered by William Herschel on January 19, 1784. It is a member of the NGC 5364 Group of galaxies, itself one of the Virgo III Groups strung out to the east of the Virgo Supercluster of galaxies.

<span class="mw-page-title-main">NGC 2273</span> Galaxy in the constellation Lynx

NGC 2273 is a barred spiral galaxy located in the constellation Lynx. It is located at a distance of circa 95 million light years from Earth, which, given its apparent dimensions, means that NGC 2273 is about 100,000 light years across. It was discovered by Nils Dunér on September 15, 1867.

<span class="mw-page-title-main">NGC 1142</span> Interacting and distorted spiral galaxy in the constellation Cetus

NGC 1142 is a distorted spiral galaxy in the constellation of Cetus. It is located about 370 million light years away from Earth, which means, given its apparent dimensions, that NGC 1142 is approximately 170,000 light years across. It is a type 2 Seyfert galaxy. It interacts with the elliptical galaxy NGC 1141.

<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.

References

  1. 1 2 3 4 5 6 7 "NASA/IPAC Extragalactic Database". Results for NGC 3367. Retrieved 2016-01-18.
  2. 1 2 "Revised NGC Data for NGC 3367". spider.seds.org. Retrieved 25 November 2018.
  3. ↑ Seligman, Courtney. "NGC 3367". Celestial Atlas. Retrieved 19 November 2018.
  4. 1 2 3 4 Hernández-Toledo, H. M.; Cano-Díaz, M.; Valenzuela, O.; Puerari, I.; García-Barreto, J. A; Moreno-Díaz, E.; Bravo-Alfaro, H. (1 December 2011). "The Bulgeless Seyfert/Liner Galaxy NGC 3367: Disk, Bar, Lopsidedness, and Environment". The Astronomical Journal. 142 (6): 182. arXiv: 1104.3622 . Bibcode:2011AJ....142..182H. doi:10.1088/0004-6256/142/6/182. S2CID   119111771.
  5. ↑ Uppsala General Catalogue of Galaxies, 1973, Acta Universitatis Upsalienis, Nova Regiae Societatis Upsaliensis, Series V: A Vol. 1
  6. ↑ Sandage, A., Bedke, J. (1994), The Carnegie Atlas of Galaxies. Volume I, Carnegie Institution of Washington, p. 15
  7. ↑ Gabbasov, R. F.; Repetto, P.; Rosado, M. (1 September 2009). "On the Bar Pattern Speed Determination of NGC 3367". The Astrophysical Journal. 702 (1): 392–402. arXiv: 0908.0718 . Bibcode:2009ApJ...702..392G. doi:10.1088/0004-637X/702/1/392. S2CID   15734407.
  8. ↑ Ho, L. C.; Filippenko, A. V.; Sargent, W. L. (June 1995). "A search for 'dwarf' Seyfert nuclei. 2: an optical spectral atlas of the nuclei of nearby galaxies". The Astrophysical Journal Supplement Series. 98: 477. Bibcode:1995ApJS...98..477H. doi:10.1086/192170.
  9. ↑ Ho, Luis C.; Filippenko, Alexei V.; Sargent, Wallace L. W.; Peng, Chien Y. (October 1997). "A Search for "Dwarf" Seyfert Nuclei. IV. Nuclei with Broad Hα Emission". The Astrophysical Journal Supplement Series. 112 (2): 391–414. arXiv: astro-ph/9704099 . Bibcode:1997ApJS..112..391H. doi:10.1086/313042. S2CID   15256980.
  10. ↑ Alonso-Herrero, Almudena; Rieke, Marcia J.; Rieke, George H.; Shields, Joseph C. (20 February 2000). "The Nature of LINERs". The Astrophysical Journal. 530 (2): 688–703. arXiv: astro-ph/9909316 . Bibcode:2000ApJ...530..688A. doi:10.1086/308388. S2CID   119478156.
  11. ↑ Satyapal, S.; Vega, D.; Dudik, R. P.; Abel, N. P.; Heckman, T. (20 April 2008). "Spitzer Uncovers Active Galactic Nuclei Missed by Optical Surveys in Seven Late-Type Galaxies". The Astrophysical Journal. 677 (2): 926–942. arXiv: 0801.2759 . Bibcode:2008ApJ...677..926S. doi:10.1086/529014. S2CID   16050838.
  12. 1 2 McAlpine, W.; Satyapal, S.; Gliozzi, M.; Cheung, C. C.; Sambruna, R. M.; Eracleous, Michael (10 February 2011). "Black Holes in Bulgeless Galaxies: Anxmm-Newtoninvestigation of NGC 3367 and NGC 4536". The Astrophysical Journal. 728 (1): 25. arXiv: 1012.0834 . Bibcode:2011ApJ...728...25M. doi:10.1088/0004-637X/728/1/25. S2CID   118885784.
  13. ↑ García-Barreto, J. A.; Rudnick, L.; Franco, J.; Martos, M. (July 1998). "Central Activity in the Barred Galaxy NGC 3367". The Astronomical Journal. 116 (1): 111–118. arXiv: astro-ph/9805107 . Bibcode:1998AJ....116..111G. doi:10.1086/300436. S2CID   6880853.
  14. ↑ García-Barreto, J. Antonio; Franco, José; Rudnick, Lawrence (April 2002). "VLA High-Resolution 1.4 and 8.4 GH[CLC]z[/CLC] Mapping of the Barred Galaxy NGC 3367". The Astronomical Journal. 123 (4): 1913–1921. arXiv: astro-ph/0201138 . doi: 10.1086/339559 .
  15. ↑ Dong, X. Y.; De Robertis, M. M. (March 2006). "Low-Luminosity Active Galaxies and Their Central Black Holes". The Astronomical Journal. 131 (3): 1236–1252. arXiv: astro-ph/0510694 . Bibcode:2006AJ....131.1236D. doi:10.1086/499334. S2CID   17630682.
  16. ↑ García-Barreto, J. A.; Scoville, N. Z.; Koda, J.; Sheth, K. (January 2005). "CO in the Bipolar Radio Continuum Galaxy NGC 3367". The Astronomical Journal. 129 (1): 125–135. arXiv: astro-ph/0409486 . Bibcode:2005AJ....129..125G. doi:10.1086/426321. S2CID   6526596.
  17. ↑ List of Supernovae IAU Central Bureau for Astronomical Telegrams. Retrieved 29 December 2015.
  18. ↑ "Bright Supernova pages - Most prolific galaxies". www.rochesterastronomy.org.
  19. ↑ "Supernova 1992C". www.eso.org. 10 November 2010.
  20. ↑ Makarov, Dmitry; Karachentsev, Igor (21 April 2011). "Galaxy groups and clouds in the local (z~ 0.01) Universe". Monthly Notices of the Royal Astronomical Society. 412 (4): 2498–2520. arXiv: 1011.6277 . Bibcode:2011MNRAS.412.2498M. doi:10.1111/j.1365-2966.2010.18071.x. S2CID   119194025. Archived from the original on 31 January 2016. Retrieved 15 December 2018.
  21. ↑ de Vaucouleurs, Gerard Henri; de Vaucouleurs, Antoinette; Shapley, Harlow (1964). Reference catalogue of bright galaxies. Austin: University of Texas Press. Bibcode:1964rcbg.book.....D.


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