Astronomy:NGC 7592

From HandWiki
Short description: Interacting galaxy system in the constellation Aquarius
NGC 7592
NGC 7592 hst 08669 R814B555.png
Hubble Space Telescope (HST) image of the galaxy
Observation data (J2000 epoch)
ConstellationAquarius
Right ascension 23h 18m 22.2s[1]
Declination−04° 25′ 01″[1]
Redshift0.024444 ± 0.000113
Helio radial velocity7,328 ± 34 km/s[1]
Distance306 Mly (95 Mpc)[1]
Apparent magnitude (V)13.5[2]
Characteristics
TypeS0+ pec[1]
Apparent size (V)1.2′ × 0.9′[1]
Notable featuresmergering galaxy pair
Other designations
MCG -01-59-017, VV 731, PGC 70999,[1] Mrk 928

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.[3] The total infrared luminosity is 1011.33 L☉, and thus it is categorised as a luminous infrared galaxy.[4] One of the galaxies hosts a type 2 Seyfert nucleus.[5]

Characteristics

Wide field view of NGC 7592 with the legacy surveys

NGC 7592 is an interacting galaxy system and ongoing galaxy merger between an early type galaxy and a late type spiral galaxy.[6] The system has at least two faint diffuse tidal tails, with the longer one extending about 2 arcminutes towards the south.[7] Based on the total infrared luminosity of the galaxy (1011.33 L☉), NGC 7592 is categorised as a luminous infrared galaxy.[4] Luminous infrared galaxies are characterised by increased star formation. The star formation rate of NGC 7592 is estimated to be 26 M☉ per year.[7]

Nuclei

The two galactic nuclei, whose projected separation is 14 arcseconds, have nearly equal luminance in near infrared imaging.[8] The west nucleus is known to be a Seyfert, a type of active galactic nucleus (AGN). Based on its spectral lines, it has been categorised as type 1.9 or type 2.[9] The most accepted theory for the energy source of AGNs is the presence of an accretion disk around a supermassive black hole. It has been suggested that around the Seyfert nucleus lies a rotating, star-forming knotty disk or ring with a diameter of about 1.5 kpc viewed nearly edge-on, and which is perpendicular to the galactic plane. It is possible that it is material accreted from the other galaxy. The east nucleus features a complex structure, probably due to extinction.[6] There is diffuse X-ray emission around both nuclei.[7]

At the end of one tidal tail lies a bright source in visual light that is identified as NGC 7592C.[7] It is located about 12 arcseconds south from the mid-distance of the two other nuclei.[8] It has been suggested that it is another galaxy taking part in the merger, however its infrared emission is fainter than the other two nuclei and it has not been detected in x-rays by Chandra X-ray Observatory.[10] Its spectrum, both optical and infrared, suggests it is an extranuclear star formation region.[7] Based on its kinematics, the south condensation is part of the spiral galaxy.[6]

See also

  • NGC 5256 - a similar interacting galactic pair

References

  1. ↑ 1.0 1.1 1.2 1.3 1.4 1.5 1.6 "NASA/IPAC Extragalactic Database". Results for NGC 7592. http://ned.ipac.caltech.edu/cgi-bin/nph-objsearch?objname=NGC+7592. 
  2. ↑ "Revised NGC Data for NGC 7592". http://spider.seds.org/ngc/revngcic.cgi?NGC7592. 
  3. ↑ Seligman, Courtney. "NGC 7592 (= PGC 70999)". http://cseligman.com/text/atlas/ngc75a.htm#7592. 
  4. ↑ 4.0 4.1 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. 
  5. ↑ Maia, Marcio A. G.; Machado, Rodolfo S.; Willmer, Christopher N. A. (October 2003). "The Seyfert Population in the Local Universe". The Astronomical Journal 126 (4): 1750–1762. doi:10.1086/378360. Bibcode: 2003AJ....126.1750M. 
  6. ↑ 6.0 6.1 6.2 Hattori, Takashi; Yoshida, Michitoshi; Ohtani, Hiroshi; Ishigaki, Tsuyoshi; Sugai, Hajime; Hayashi, Tadashi; Ozaki, Shinobu; Ishii, Motomi (25 June 2002). "Tridimensional Spectroscopic Observation of the Interacting System NGC 7592". Publications of the Astronomical Society of Japan 54 (3): 393–404. doi:10.1093/pasj/54.3.393. 
  7. ↑ 7.0 7.1 7.2 7.3 7.4 Smith, Beverly J.; Campbell, Kristen; Struck, Curtis; Soria, Roberto; Swartz, Douglas; Magno, Macon; Dunn, Brianne; Giroux, Mark L. (23 January 2018). "Diffuse X-Ray-emitting Gas in Major Mergers". The Astronomical Journal 155 (2): 81. doi:10.3847/1538-3881/aaa1a6. Bibcode: 2018AJ....155...81S. 
  8. ↑ 8.0 8.1 Haan, S.; Armus, L.; Laine, S.; Charmandaris, V.; Smith, J. D.; Schweizer, F.; Brandl, B.; Evans, A. S. et al. (1 December 2011). "Spitzer IRS spectral mapping of the Toomre sequence: spatial variations of PAH, gas, and dust properties in nearby major mergers". The Astrophysical Journal Supplement Series 197 (2): 27. doi:10.1088/0067-0049/197/2/27. Bibcode: 2011ApJS..197...27H. 
  9. ↑ Rafanelli, Piero; Marziani, Paolo (March 1992). "The complex nature of the interacting system NGC 7592". The Astronomical Journal 103: 743. doi:10.1086/116098. Bibcode: 1992AJ....103..743R. 
  10. ↑ Torres-Albà, N.; Iwasawa, K.; Díaz-Santos, T.; Charmandaris, V.; Ricci, C.; Chu, J. K.; Sanders, D. B.; Armus, L. et al. (1 December 2018). "C-GOALS - II. Chandra observations of the lower luminosity sample of nearby luminous infrared galaxies in GOALS". Astronomy & Astrophysics 620: A140. doi:10.1051/0004-6361/201834105. Bibcode: 2018A&A...620A.140T. 

External links



Retrieved from "https://handwiki.org/wiki/index.php?title=Astronomy:NGC_7592&oldid=3340572"