NGC 7130

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NGC 7130
NGC 7130 hst 05479 606.png
NGC 7130 by the Hubble Space Telescope
Observation data (J2000 epoch)
Constellation Piscis Austrinus
Right ascension 21h 48m 19.5s [1]
Declination −34° 57′ 04″ [1]
Redshift 0.016151 ± 0.000050 [1]
Helio radial velocity 4,842 ± 15 km/s [1]
Distance 221 Mly (68 Mpc) [1]
Apparent magnitude  (V)12.1
Characteristics
Type Sa pec [1]
Apparent size  (V)1.5′ × 1.4′ [1]
Notable featuresSeyfert and starburst galaxy
Other designations
IC 5135, ESO 403- G032, AM 2145-351, MCG -06-47-015, PGC 67387 [1]

NGC 7130 (also known as IC 5135) 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. [1] It was discovered by John Herschel on September 25, 1834, and discovered independently by Lewis Swift on September 17, 1897. [2] The location of the galaxy given in the New General Catalogue was off by 30 arcminutes in declination from the location of the galaxy. [3]

Contents

Characteristics

NGC 7130 is characterised as a peculiar galaxy based on its distorted shape. The galaxy has two faint arms towards the south, while north of the galaxy there is diffuse H-alpha emission. Two knots with H-alpha emission are observed southeast of the galaxy. [4] The galaxy has star streams and trailing tidal arms. [5] It has been suggested that the distorted shape of NGC 7130 is the result of the interaction with another galaxy. [4] [5] In the infrared K-band a bar is visible. [6] The total infrared luminosity of NGC 7130 is 2.2×1011  L☉ (1011.35L☉) and it is categorised as a luminous infrared galaxy. [7]

Nucleus

NGC 7130 has a bright nucleus which is characterised as active. The galaxy features optical emission lines typical of a type 2 Seyfert galaxy, with broad lines and strong emission lines from high ionisation elements, like [He II], however the ultraviolet spectrum is more consistent with the emission produced by young, massive O-type stars, suggesting an active starburst in the nucleus. [8] More detailed observations in ultraviolet reveal an asymmetric circumnuclear starburst ring with several knots. The total span of the ring is one arcsecond, which corresponds to 310 pc, in the north-south direction, and 0.7 arcseconds, which corresponds to 220 pc, in east-west direction. Ultraviolet emission is also observed at the inner part of the spiral arms at the leading edge of the bar. [9]

The galaxy emits also X-rays. Based on observations by Chandra X-ray Observatory it was found that the two thirds of the X-ray emission at 0.3–8 keV of the galaxy comes from the circumnuclear starburst activity and the galaxy disk, while the rest was attributed to an active galactic nucleus (AGN) hidden by a Compton-thick column with column density over 1024 cm−2. The percentage attributed to the AGN exceeds 50% at higher energies, over 2 keV. [10] The transition from the emission of the AGN to that of the starburst is smooth, as seen by the different ionisation states of the gas around the nucleus. The extended narrow-line region of NGC 7130 is estimated to have a radius of 1.8±0.8 kpc. There is also an outflowing wind, whose origin however cannot be determined accurately. [5]

In the centre of NGC 7130 lies a supermassive black hole whose mass is estimated to be 3.9×107  M☉ (107.59M☉) based on stellar velocity dispersion. [11] The star formation rate in the central kiloparsec of NGC 7130 is estimated to be 4.3 M☉ per year. [12] The total star formation rate of the galaxy is estimated to be 21 M☉ per year. [13]

Supernovae

Two supernovae have been observed in NGC 7130: SN 2010bt (type IIn, mag 15.9), [14] and SN 2017hgz (type Ia, mag 15.1). [15]

Nearby galaxies

NGC 7130 belongs in a galaxy group known as LGG 445. Other members of the galaxy group include NGC 7057, IC 5105, NGC 7087, NGC 7060, NGC 7072, NGC 7075, NGC 7110, IC 5128, and IC 5139. [16] Near NGC 7130 lie also the distorted NGC 7135, 18 arcminutes to the east, and IC 5131, 12 arcminutes to the west. [17] It has been suggested that the distortion of NGC 7130 was caused by an interaction with one of these two galaxies, [17] however, they have nearly half the redshift. [18]

See also

Related Research Articles

An active galactic nucleus (AGN) is a compact region at the center of a galaxy that has a much-higher-than-normal luminosity over at least some portion of the electromagnetic spectrum with characteristics indicating that the luminosity is not produced by stars. Such excess non-stellar emission has 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">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 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">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 1614</span> Galaxy in the constellation Eridanus

NGC 1614 is the New General Catalogue identifier for a spiral galaxy in the equatorial constellation of Eridanus. It was discovered on December 29, 1885 by American astronomer Lewis Swift, who described it in a shorthand notation as: pretty faint, small, round, a little brighter middle. The nebula was then catalogued by Danish-Irish astronomer J. L. E. Drayer in 1888. When direct photography became available, it was noted that this galaxy displayed some conspicuous peculiarities. American astronomer Halton Arp included it in his 1966 Atlas of Peculiar Galaxies. In 1971, Swiss astronomer Fritz Zwicky described it as a "blue post-eruptive galaxy, compact patchy core, spiral plumes, long blue jet SSW".

<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 7213</span> Galaxy in the constellation Grus

NGC 7213 is a lenticular galaxy located in the constellation Grus. It is located at a distance of circa 70 million light-years from Earth, which, given its apparent dimensions, means that NGC 7213 is about 75,000 light-years across. It was discovered by John Herschel on September 30, 1834. It is an active galaxy with characteristics between a type I Seyfert galaxy and LINER.

<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 4636</span> Galaxy in the constellation Virgo

NGC 4636 is an elliptical galaxy located in the constellation Virgo. It is a member of the NGC 4753 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. It is located at a distance of about 55 million light years from Earth, which, given its apparent dimensions, means that NGC 4636 is about 105,000 light years across.

<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">IC 1459</span> Elliptical galaxy in the constellation of Grus

IC 1459 is an elliptical galaxy located in the constellation Grus. It is located at a distance of circa 85 million light-years from Earth, which, given its apparent dimensions, means that IC 1459 is about 130,000 light-years across. It was discovered by Edward Emerson Barnard in 1892.

<span class="mw-page-title-main">NGC 4278</span> Galaxy in the constellation Coma Berenices

NGC 4278 is an elliptical galaxy located in the constellation Coma Berenices. It is located at a distance of circa 55 million light years from Earth, which, given its apparent dimensions, means that NGC 4278 is about 65,000 light years across. It was discovered by William Herschel on March 13, 1785. NGC 4278 is part of the Herschel 400 Catalogue and can be found about one and 3/4 of a degree northwest of Gamma Comae Berenices even with a small telescope.

<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 1241</span> Galaxy in the constellation Eridanus

NGC 1241 is a spiral galaxy located in the constellation Eridanus. It is located at a distance of circa 150 million light years from Earth, which, given its apparent dimensions, means that NGC 1241 is about 140,000 light years across. It was discovered by William Herschel on January 10, 1785. It is classified as a Seyfert galaxy.

<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 7679</span> Galaxy in the constellation Pisces

NGC 7679 is a lenticular galaxy with a peculiar morphology in the constellation Pisces. It is located at a distance of circa 200 million light years from Earth, which, given its apparent dimensions, means that NGC 7679 is about 60,000 light years across. It was discovered by Heinrich d'Arrest on September 23, 1864. The total infrared luminosity is 1011.05 L☉, and thus it is categorised as a luminous infrared galaxy. NGC 7679 is both a starburst galaxy and a Seyfert galaxy.

<span class="mw-page-title-main">NGC 2617</span> Galaxy in the constellation Hydra

NGC 2617 is a Seyfert galaxy in the equatorial constellation of Hydra. It was discovered on February 12, 1885, by French astronomer Édouard Stephan. In 1888, Danish astronomer J. L. E. Dreyer described it as "extremely faint, very small, 2 very faint stars involved". It is located at an estimated distance of 202 million light years. In the infrared, the galaxy has an angular size of 0.693 by 0.652 arcminutes.

References

  1. 1 2 3 4 5 6 7 8 9 "NASA/IPAC Extragalactic Database". Results for NGC 7130. Retrieved 2016-01-18.
  2. ↑ Seligman, Courtney. "NGC 7130 (= IC 5135 = PGC 67387)". Celestial Atlas. Retrieved 19 November 2018.
  3. ↑ de Vaucouleurs, Gerard Henri; de Vaucouleurs, Antoinette; Shapley, Harlow (1964). Reference catalogue of bright galaxies. Austin: University of Texas Press. Bibcode:1964rcbg.book.....D.
  4. 1 2 Eskridge, Paul B.; Frogel, Jay A.; Pogge, Richard W.; Quillen, Alice C.; Berlind, Andreas A.; Davies, Roger L.; DePoy, D. L.; Gilbert, Karoline M.; Houdashelt, Mark L.; Kuchinski, Leslie E.; Ramirez, Solange V.; Sellgren, K.; Stutz, Amelia; Terndrup, Donald M.; Tiede, Glenn P. (November 2002). "Near-Infrared and Optical Morphology of Spiral Galaxies". The Astrophysical Journal Supplement Series. 143 (1): 73–111. arXiv: astro-ph/0206320 . Bibcode:2002ApJS..143...73E. doi:10.1086/342340. S2CID   15491635.
  5. 1 2 3 Davies, Rebecca L.; Rich, Jeffrey A.; Kewley, Lisa J.; Dopita, Michael A. (21 April 2014). "Starburst–AGN mixing – I. NGC 7130". Monthly Notices of the Royal Astronomical Society. 439 (4): 3835–3846. arXiv: 1402.0493 . Bibcode:2014MNRAS.439.3835D. doi:10.1093/mnras/stu234. S2CID   55816252.
  6. ↑ Mulchaey, John S.; Regan, Michael W.; Kundu, Arunav (June 1997). "The Fueling of Nuclear Activity. I. A Near-Infrared Imaging Survey of Seyfert and Normal Galaxies". The Astrophysical Journal Supplement Series. 110 (2): 299–319. Bibcode:1997ApJS..110..299M. doi: 10.1086/313005 .
  7. ↑ 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. arXiv: astro-ph/0306263 . Bibcode:2003AJ....126.1607S. doi:10.1086/376841. S2CID   14825701.
  8. ↑ Thuan, T. X. (June 1984). "Ultraviolet observations of starburst and mini-Seyfert galactic nuclei". The Astrophysical Journal. 281: 126. Bibcode:1984ApJ...281..126T. doi:10.1086/162081.
  9. ↑ 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. arXiv: astro-ph/9806107 . Bibcode:1998ApJ...505..174G. doi:10.1086/306154. S2CID   119098033.
  10. ↑ Levenson, N. A.; Weaver, K. A.; Heckman, T. M.; Awaki, H.; Terashima, Y. (January 2005). "Deconstructing NGC 7130". The Astrophysical Journal. 618 (1): 167–177. arXiv: astro-ph/0411644 . Bibcode:2005ApJ...618..167L. doi:10.1086/425913. S2CID   15228036.
  11. ↑ 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. arXiv: 1201.5397 . Bibcode:2012ApJ...748..130M. doi:10.1088/0004-637X/748/2/130. S2CID   38183296.
  12. ↑ Diamond-Stanic, Aleksandar M.; Rieke, George H. (20 February 2012). "The Relationship between Black Hole Growth and Star Formation in Seyfert Galaxies". The Astrophysical Journal. 746 (2): 168. arXiv: 1106.3565 . Bibcode:2012ApJ...746..168D. doi:10.1088/0004-637X/746/2/168. S2CID   119277531.
  13. ↑ Gruppioni, C.; Berta, S.; Spinoglio, L.; Pereira-Santaella, M.; Pozzi, F.; Andreani, P.; Bonato, M.; De Zotti, G.; Malkan, M.; Negrello, M.; Vallini, L.; Vignali, C. (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. arXiv: 1603.02818 . Bibcode:2016MNRAS.458.4297G. doi:10.1093/mnras/stw577. S2CID   53417437.
  14. ↑ Transient Name Server entry for SN 2010bt. Retrieved 23 March 2023.
  15. ↑ "Bright Supernova pages - Most prolific galaxies". www.rochesterastronomy.org.
  16. ↑ Garcia, A. M. (1993). "General study of group membership. II - Determination of nearby groups". Astronomy and Astrophysics Supplement Series. 100 (1): 47–90. Bibcode:1993A&AS..100...47G. ISSN   0365-0138.
  17. 1 2 Allan Sandage (1994). The Carnegie atlas of galaxies. 1 (1994). p. 15.
  18. ↑ 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 23 December 2018.


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