NGC 5953

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NGC 5953
NGC 5953 in Arp 91 (HST potw2140a, cropped).jpg
NGC 5953 by Hubble Space Telescope
Observation data (J2000 epoch)
Constellation Serpens
Right ascension 15h 34m 32.4s [1]
Declination 15° 11′ 38″ [1]
Redshift 0.006555 ± 0.000020 [1]
Heliocentric radial velocity 1965 ± 6 km/s [1]
Distance 78 ± 15 Mly (26 ± 4.7 Mpc) [1]
Apparent magnitude  (V)13.0
Characteristics
Type SAa: pec [1]
Apparent size  (V)1.35′ × 1.16′ [1]
Notable featuresinteracting galaxy, Seyfert galaxy
Other designations
UGC 9903, Arp 91B, VV 244a, MRK 9031, MCG +03-40-005, PGC 55480 [1]

NGC 5953 is a peculiar spiral galaxy in the constellation Serpens. The galaxy lies about 80 million light years away from Earth, which means, given its apparent dimensions, that NGC 5953 is approximately 35,000 light years across. [1] It was discovered by William Herschel on April 17, 1784. [2] NGC 5953 interacts with NGC 5954 forming a pair known as Arp 91. [3]

Contents

Characteristics

NGC 5953 and NGC 5954 pair Arp91 - HST - SDSS - DECam - Potw2140a.jpg
NGC 5953 and NGC 5954 pair

NGC 5953 is an unbarred spiral galaxy seen face on with many dust lanes. Two tidal plumes are visible, one to the northwest and one to the south of the galaxy. [4] The spiral arms are flocculent and appear fragmented and are associated with star formation regions. [5]

The galaxy has recently undergone intense star formation in the circumnuclear region around the nucleus where there are huge HII regions, probably as a result of its interaction with NGC 5954. [6] The large HII region has been found to emit radio waves, appearing as a discrete source 5 arcseconds from the nucleus. [7] A circumnuclear star ring with a diameter of 10–14 arcseconds is visible, which coincides with a disk of CO gas. Based on near infrared observations the ring hosts a red giant but not hot gas. [8] The total star formation rate of the galaxy is estimated to be 2.56 ± 0.1 M☉ per year. [9]

Active nucleus

The nucleus of the galaxy has been found to be active and it is categorised as a type 2 Seyfert galaxy [7] or as a LINER. [10] 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 black hole in the nucleus of NGC 5953 is estimated to have a mass of 7×106  M☉ based on velocity dispersion. [11]

A jet is visible to the north of the nucleus in radio waves extending for 0.3 arcseconds, which corresponds to a projected distance of 40 parsecs in the distance of the galaxy. [12]

Nearby galaxies

NGC 5953 forms a pair with another spiral galaxy, NGC 5954, which lies 43 arcminutes away. [7] The interaction has distorted NGC 5954. [3] The pair is part of the NGC 5962 group or LGG 400. Other members of the group, apart from NGC 5962, include UGC 9925 and UGC 9951. A bit further away lie NGC 5951, NGC 5956, and NGC 5957. [13] [14]

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

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

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

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

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

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<span class="mw-page-title-main">NGC 1241</span> Galaxy in the constellation Eridanus

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<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.

<span class="mw-page-title-main">NGC 3516</span> Galaxy in the constellation of Ursa Major

NGC 3516 is a barred lenticular galaxy in the constellation of Ursa Major. NGC 3516 is located about 150 million light years away from Earth, which means, given its apparent dimensions, that NGC 3516 is approximately 100,000 light years across. It was discovered by William Herschel on April 3, 1785.

<span class="mw-page-title-main">NGC 5506</span> Galaxy in the constellation of Virgo

NGC 5506 is a spiral galaxy located in the constellation Virgo. It is located at a distance of about 75 million light years from Earth, which, given its apparent dimensions, means that NGC 5506 is about 80,000 light years across. It was discovered by William Herschel on April 15, 1787. It is a Seyfert galaxy.

<span class="mw-page-title-main">NGC 4593</span> Galaxy in the constellation of Virgo

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<span class="mw-page-title-main">NGC 2110</span>

NGC 2110 is a lenticular galaxy located in the constellation Orion. It is located at a distance of about 120 million light years from Earth, which, given its apparent dimensions, means that NGC 2110 is about 90,000 light years across. It was discovered by William Herschel on October 5, 1785. It is a Seyfert galaxy.

<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 "NASA/IPAC Extragalactic Database". Results for NGC 5953. Retrieved 2024-03-26.
  2. ↑ Seligman, Courtney. "NGC 5953 (with NGC 5954 = Arp 91) (= PGC 55480 = PGC 1477680 = UGC 9903 = CGCG 107-008: = MCG +03-40-005)". Celestial Atlas. Retrieved 19 November 2018.
  3. 1 2 "A Dangerous Dance". www.spacetelescope.org. 4 October 2021. Retrieved 27 March 2024.
  4. ↑ Iono, Daisuke; Yun, Min S.; Ho, Paul T. P. (May 2005). "Atomic and Molecular Gas in Colliding Galaxy Systems. I. The Data". The Astrophysical Journal Supplement Series. 158 (1): 1–37. doi:10.1086/429093.
  5. ↑ 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.
  6. ↑ Gonzalez Delgado, R. M.; Perez, E. (1 August 1996). "The circumnuclear region in the Seyfert 2 galaxy NGC 5953". Monthly Notices of the Royal Astronomical Society. 281 (3): 781–798. doi:10.1093/mnras/281.3.781.
  7. 1 2 3 Rafanelli, P.; Osterbrock, D. E.; Pogge, R. W. (January 1990). "The optical counterpart of the radio source close to the Seyfert 2 nucleus of NGC 5953 = ARP 91 B". The Astronomical Journal. 99: 53. doi:10.1086/115312.
  8. ↑ Casasola, V.; Hunt, L. K.; Combes, F.; García-Burillo, S.; Boone, F.; Eckart, A.; Neri, R.; Schinnerer, E. (February 2010). "Molecular gas in NUclei of GAlaxies (NUGA) XIII. The interacting Seyfert 2/LINER galaxy NGC 5953". Astronomy and Astrophysics. 510: A52. doi:10.1051/0004-6361/200913056.
  9. ↑ 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 (21 June 2018). "Erratum: 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. 477 (2): 2815–2816. doi:10.1093/mnras/sty772.
  10. ↑ Veilleux, S.; Kim, D.-C.; Sanders, D. B.; Mazzarella, J. M.; Soifer, B. T. (May 1995). "Optical Spectroscopy of Luminous Infrared Galaxies. II. Analysis of the Nuclear and Long-Slit Data". The Astrophysical Journal Supplement Series. 98: 171. doi:10.1086/192158.
  11. ↑ McElroy, Douglas B. (September 1995). "A Catalog of Stellar Velocity Dispersions. II. 1994 Update". The Astrophysical Journal Supplement Series. 100: 105. doi:10.1086/192209.
  12. ↑ Krips, M.; Eckart, A.; Krichbaum, T. P.; Pott, J.-U.; Leon, S.; Neri, R.; García-Burillo, S.; Combes, F.; Boone, F.; Baker, A. J.; Tacconi, L. J.; Schinnerer, E.; Hunt, L. K. (March 2007). "NUclei of GAlaxies: V. Radio emission in 7 NUGA sources". Astronomy & Astrophysics. 464 (2): 553–563. doi:10.1051/0004-6361:20065037.
  13. ↑ 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 20 March 2017.
  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. Bibcode:1993A&AS..100...47G. ISSN   0365-0138.
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