NGC 7592
{{Short description|Interacting galaxy system in the constellation Aquarius}}
{{Infobox Galaxy
| name = NGC 7592
| image = NGC 7592 hst 08669 R814B555.png
| image_size = 250px
| caption = Hubble Space Telescope (HST) image of the galaxy
| epoch = J2000
| type = S0+ pec{{cite web
| title=NASA/IPAC Extragalactic Database
| work=Results for NGC 7592
| url=http://ned.ipac.caltech.edu/cgi-bin/nph-objsearch?objname=NGC+7592
| access-date=2020-11-03}}
| z = 0.024444 ± 0.000113
| h_radial_v = 7,328 ± 34 km/s
| size_v = 1.2{{prime}} × 0.9{{prime}}
| constellation name = Aquarius
| notes = mergering galaxy pair
| names = MCG -01-59-017, VV 731, PGC 70999, 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.{{cite web |last1=Seligman |first1=Courtney |title=NGC 7592 (= PGC 70999) |url= http://cseligman.com/text/atlas/ngc75a.htm#7592 |website=Celestial Atlas |access-date=19 November 2018}} The total infrared luminosity is {{val|e=11.33|ul=L_solar}}, and thus it is categorised as a luminous infrared galaxy.{{cite journal |last1=Sanders |first1=D. B. |last2=Mazzarella |first2=J. M. |last3=Kim |first3=D.-C. |last4=Surace |first4=J. A. |last5=Soifer |first5=B. T. |title=The IRAS Revised Bright Galaxy Sample |journal=The Astronomical Journal |date=October 2003 |volume=126 |issue=4 |pages=1607–1664 |doi=10.1086/376841|bibcode=2003AJ....126.1607S |arxiv=astro-ph/0306263 |s2cid=14825701 }} One of the galaxies hosts a type 2 Seyfert nucleus.{{cite journal |last1=Maia |first1=Marcio A. G. |last2=Machado |first2=Rodolfo S. |last3=Willmer |first3=Christopher N. A. |title=The Seyfert Population in the Local Universe |journal=The Astronomical Journal |date=October 2003 |volume=126 |issue=4 |pages=1750–1762 |doi=10.1086/378360|arxiv=astro-ph/0307180 |bibcode=2003AJ....126.1750M |s2cid=12785006 }}
Characteristics
File:NGC 7592 legacy dr10.jpg]]
NGC 7592 is an interacting galaxy system and ongoing galaxy merger between an early type galaxy and a late type spiral galaxy. The system has at least two faint diffuse tidal tails, with the longer one extending about 2 arcminutes towards the south. Based on the total infrared luminosity of the galaxy ({{val|e=11.33|ul=L_solar}}), NGC 7592 is categorised as a luminous infrared galaxy. Luminous infrared galaxies are characterised by increased star formation. The star formation rate of NGC 7592 is estimated to be 26 {{solar mass}} per year.
= Nuclei =
The two galactic nuclei, whose projected separation is 14 arcseconds, have nearly equal luminance in near infrared imaging. 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.{{cite journal |last1=Rafanelli |first1=Piero |last2=Marziani |first2=Paolo |title=The complex nature of the interacting system NGC 7592 |journal=The Astronomical Journal |date=March 1992 |volume=103 |pages=743 |doi=10.1086/116098|bibcode=1992AJ....103..743R }} 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.{{cite journal |last1=Hattori |first1=Takashi |last2=Yoshida |first2=Michitoshi |last3=Ohtani |first3=Hiroshi |last4=Ishigaki |first4=Tsuyoshi |last5=Sugai |first5=Hajime |last6=Hayashi |first6=Tadashi |last7=Ozaki |first7=Shinobu |last8=Ishii |first8=Motomi |title=Tridimensional Spectroscopic Observation of the Interacting System NGC 7592 |journal=Publications of the Astronomical Society of Japan |date=25 June 2002 |volume=54 |issue=3 |pages=393–404 |doi=10.1093/pasj/54.3.393|doi-access=free }} There is diffuse X-ray emission around both nuclei.
At the end of one tidal tail lies a bright source in visual light that is identified as NGC 7592C. It is located about 12 arcseconds south from the mid-distance of the two other nuclei.{{cite journal |last1=Haan |first1=S. |last2=Armus |first2=L. |last3=Laine |first3=S. |last4=Charmandaris |first4=V. |last5=Smith |first5=J. D. |last6=Schweizer |first6=F. |last7=Brandl |first7=B. |last8=Evans |first8=A. S. |last9=Surace |first9=J. A. |last10=Diaz-Santos |first10=T. |last11=Beirão |first11=P. |last12=Murphy |first12=E. J. |last13=Stierwalt |first13=S. |last14=Hibbard |first14=J. E. |last15=Yun |first15=M. |last16=Jarrett |first16=T. H. |title=Spitzer IRS spectral mapping of the Toomre sequence: spatial variations of PAH, gas, and dust properties in nearby major mergers |journal=The Astrophysical Journal Supplement Series |date=1 December 2011 |volume=197 |issue=2 |pages=27 |doi=10.1088/0067-0049/197/2/27|arxiv=1110.3046 |bibcode=2011ApJS..197...27H |s2cid=35762225 }} 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.{{cite journal |last1=Torres-Albà |first1=N. |last2=Iwasawa |first2=K. |last3=Díaz-Santos |first3=T. |last4=Charmandaris |first4=V. |last5=Ricci |first5=C. |last6=Chu |first6=J. K. |last7=Sanders |first7=D. B. |last8=Armus |first8=L. |last9=Barcos-Muñoz |first9=L. |last10=Evans |first10=A. S. |last11=Howell |first11=J. H. |last12=Inami |first12=H. |last13=Linden |first13=S. T. |last14=Medling |first14=A. M. |last15=Privon |first15=G. C. |last16=U |first16=V. |last17=Yoon |first17=I. |title=C-GOALS - II. Chandra observations of the lower luminosity sample of nearby luminous infrared galaxies in GOALS |journal=Astronomy & Astrophysics |date=1 December 2018 |volume=620 |pages=A140 |doi=10.1051/0004-6361/201834105|arxiv=1810.02371 |bibcode=2018A&A...620A.140T |doi-access=free }} Its spectrum, both optical and infrared, suggests it is an extranuclear star formation region.{{cite journal |last1=Smith |first1=Beverly J. |last2=Campbell |first2=Kristen |last3=Struck |first3=Curtis |last4=Soria |first4=Roberto |last5=Swartz |first5=Douglas |last6=Magno |first6=Macon |last7=Dunn |first7=Brianne |last8=Giroux |first8=Mark L. |title=Diffuse X-Ray-emitting Gas in Major Mergers |journal=The Astronomical Journal |date=23 January 2018 |volume=155 |issue=2 |pages=81 |doi=10.3847/1538-3881/aaa1a6|arxiv=1712.04049 |bibcode=2018AJ....155...81S |hdl=20.500.11937/66900 |s2cid=119360716 |hdl-access=free |doi-access=free }} Based on its kinematics, the south condensation is part of the spiral galaxy.
See also
- NGC 5256 - a similar interacting galactic pair
References
{{reflist}}
External links
- {{commons category-inline}}
{{wikiSky}}
{{Ngc80}}
{{Aquarius (constellation)}}
Category:Luminous infrared galaxies