Astronomy:NGC 5135

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NGC 5135
NGC 5135 legacy dr10.jpg
NGC 5135 by legacy surveys
Observation data (J2000 epoch)
ConstellationHydra
Right ascension 13h 25m 44.1s[1]
Declination−29° 50′ 01″[1]
Redshift0.013693 ± 0.000020 [1]
Helio radial velocity4,105 ± 6 km/s[1]
Distance194 Mly[1]
Apparent magnitude (V)12.9
Characteristics
TypeSB(l)ab [1]
Apparent size (V)2.6′ × 1.8′[1]
Notable featuresSeyfert galaxy
Other designations
ESO 444-G032, MCG -05-32-013, PGC 46974[1]

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.[2] It is a Seyfert galaxy.[1]

Characteristics

NGC 5135 has well defined spiral arms and is considered a grand design spiral galaxy. There is star formation along the leading edges of the arms.[3] There are dust lanes along the bar that curve towards the centre of galaxy.[4] Spiral arms become less well structured in the central regions.[3]

Near infrared image of the central region of NGC 5135 by Hubble Space Telescope.

NGC 5135 is a bright source in infrared light and with total infrared luminosity of 1011.16−1011.23 L☉ is considered a luminous infrared galaxy.[5][6] Also strong ultraviolet emission was detected in the central 2 arcseconds of the galaxy, with a dozen of prominent knots, indicative of a recent starburst.[7] The total star formation rate in the galaxy is estimated to be 15.61 ± 1.87 M☉ per year.[6] Knots of gas measuring 45–180 parsecs across are detected along the inner spiral arms in CO(6-5) imaging and some of them are associated with starburst regions.[8]

The nucleus of NGC 5135 has been found to be active and it has been categorised as a type II Seyfert galaxy.[9] The most accepted theory for the energy source of active galactic nuclei is the presence of an accretion disk around a supermassive black hole. The mass of the black hole in the centre of NGC 5135 is estimated to be 107.29 (19 million) M☉.[10]

The active nucleus is obscured in X-rays by Compton-thick material with a column density of 6.7+16.6
−2.8×1024/cm2.[11] An ionization cone has been detected in [Si vi] emission that extends for 600 parsec from the nucleus. To the ionization of the gas apart from the active nucleus also contribute supernova remnant shocks and young stars.[12]

One supernova has been observed in NGC 5135: SN 2023dpj (type II, mag. 17).[13]

Nearby galaxies

NGC 5135 belongs to a galaxy group known as LGG 351 or NGC 5135 group. Other members of the group include ESO 444- 12, NGC 5124, IC 4248, NGC 5150, NGC 5152, NGC 5153, IC 4275, NGC 5182, ESO 444- 47, ESO 444- 15, ESO 444- 21 and IC 4251,[14] along with NGC 5126. IC 4248, which lies 13.5 arcminutes from NGC 5135 and form a pair,[15] looks distorted and asymmetrical.[16]

See also

References

  1. ↑ 1.0 1.1 1.2 1.3 1.4 1.5 1.6 1.7 1.8 "NASA/IPAC Extragalactic Database". Results for NGC 5135. http://ned.ipac.caltech.edu/cgi-bin/nph-objsearch?objname=NGC+5135. 
  2. ↑ Seligman, Courtney. "NGC 5135". https://cseligman.com/text/atlas/ngc51.htm#5135. 
  3. ↑ 3.0 3.1 Martini, Paul; Regan, Michael W.; Mulchaey, John S.; Pogge, Richard W. (June 2003). "Circumnuclear Dust in Nearby Active and Inactive Galaxies. I. Data". The Astrophysical Journal Supplement Series 146 (2): 353–406. doi:10.1086/367817. Bibcode: 2003ApJS..146..353M. 
  4. ↑ Sandage, A., Bedke, J. (1994), The Carnegie Atlas of Galaxies. Volume I, Carnegie Institution of Washington
  5. ↑ Sanders, D. B.; Mazzarella, J. M.; Kim, D.-C.; Surace, J. A.; Soifer, B. T. (October 2003). "The IRAS Revised Bright Galaxy Sample". The Astronomical Journal 126 (4): 1607–1664. doi:10.1086/376841. Bibcode: 2003AJ....126.1607S. 
  6. ↑ 6.0 6.1 Gruppioni, C.; Berta, S.; Spinoglio, L.; Pereira-Santaella, M.; Pozzi, F.; Andreani, P.; Bonato, M.; De Zotti, G. et al. (1 June 2016). "Tracing black hole accretion with SED decomposition and IR lines: from local galaxies to the high- z Universe". Monthly Notices of the Royal Astronomical Society 458 (4): 4297–4320. doi:10.1093/mnras/stw577. 
  7. ↑ Gonzalez Delgado, Rosa M.; Heckman, Timothy; Leitherer, Claus; Meurer, Gerhardt; Krolik, Julian; Wilson, Andrew S.; Kinney, Anne; Koratkar, Anuradha (20 September 1998). "Ultraviolet-Optical Observations of the Seyfert 2 Galaxies NGC 7130, NGC 5135, and IC 3639: Implications for the Starburst–Active Galactic Nucleus Connection". The Astrophysical Journal 505 (1): 174–198. doi:10.1086/306154. Bibcode: 1998ApJ...505..174G. 
  8. ↑ Cao, Tianwen; Lu, Nanyao; Xu, C. Kevin; Zhao, Yinghe; Kalari, Venu Madhav; Gao, Yu; Charmandaris, Vassilis; Santos, Tanio Diaz et al. (18 October 2018). "ALMA Observation of NGC 5135: The Circumnuclear CO (6–5) and Dust Continuum Emission at 45 pc Resolution". The Astrophysical Journal 866 (2): 117. doi:10.3847/1538-4357/aae1f4. Bibcode: 2018ApJ...866..117C. 
  9. ↑ Levenson, N. A.; Weaver, K. A.; Heckman, T. M.; Awaki, H.; Terashima, Y. (10 February 2004). "Accretion and Outflow in the Active Galactic Nucleus and Starburst of NGC 5135". The Astrophysical Journal 602 (1): 135–147. doi:10.1086/380836. Bibcode: 2004ApJ...602..135L. 
  10. ↑ Marinucci, Andrea; Bianchi, Stefano; Nicastro, Fabrizio; Matt, Giorgio; Goulding, Andy D. (1 April 2012). "The Link Between the Hidden Broad Line Region and the Accretion Rate in Seyfert 2 Galaxies". The Astrophysical Journal 748 (2): 130. doi:10.1088/0004-637X/748/2/130. Bibcode: 2012ApJ...748..130M. 
  11. ↑ Yamada, Satoshi; Ueda, Yoshihiro; Tanimoto, Atsushi; Oda, Saeko; Imanishi, Masatoshi; Toba, Yoshiki; Ricci, Claudio (7 July 2020). "Nature of Compton-thick Active Galactic Nuclei in "Nonmerging" Luminous Infrared Galaxies UGC 2608 and NGC 5135 Revealed with Broadband X-Ray Spectroscopy". The Astrophysical Journal 897 (1): 107. doi:10.3847/1538-4357/ab94b1. Bibcode: 2020ApJ...897..107Y. 
  12. ↑ Bedregal, Alejandro G.; Colina, Luis; Alonso-Herrero, Almudena; Arribas, Santiago (20 June 2009). "Near-Ir Integral Field Spectroscopy Study of the Star Formation and Agn of the Lirg NGC 5135". The Astrophysical Journal 698 (2): 1852–1871. doi:10.1088/0004-637X/698/2/1852. Bibcode: 2009ApJ...698.1852B. 
  13. ↑ Transient Name Server entry for SN 2023dpj. Retrieved 25 October 2023.
  14. ↑ Garcia, A. M. (1 July 1993). "General study of group membership. II. Determination of nearby groups.". Astronomy and Astrophysics Supplement Series 100: 47–90. ISSN 0365-0138. Bibcode: 1993A&AS..100...47G. https://cdsarc.cds.unistra.fr/ftp/J/A+AS/100/47/table2.dat. 
  15. ↑ de Vaucouleurs, G.; de Vaucouleurs, A.; Corwin, J. R. (1 January 1976). "Second reference catalogue of bright galaxies". Second Reference Catalogue of Bright Galaxies 1976. Bibcode: 1976RC2...C......0D. https://ui.adsabs.harvard.edu/abs/1976RC2...C......0D/abstract. 
  16. ↑ For, B-Q; Staveley-Smith, L; Westmeier, T; Whiting, M; Oh, S-H; Koribalski, B; Wang, J; Wong, O I et al. (11 November 2019). "WALLABY early science − V. ASKAP H i imaging of the Lyon Group of Galaxies 351". Monthly Notices of the Royal Astronomical Society 489 (4): 5723–5741. doi:10.1093/mnras/stz2501. 

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