{{Short description|Galaxy in the constellation of Boötes}} {{Infobox galaxy|name=[[IRAS]] 14394+5332|epoch=[[J2000.0]]|constellation name=[[Boötes]]|ra={{RA|14|41|04.42}}<ref name="ned" />|dec={{DEC|+53|20|09.04}}<ref name="ned" />|z=0.105024<ref name="ned" />|h_radial_v=31,485 [[kilometer per second|km/s]]<ref name="ned" />|dist_ly=1.410 [[light year|Gly]]|appmag_v=17.77|type=ULIRG Sy2<ref name="ned" />|size=~{{convert|50.26|kpc|ly|abbr=on|lk=on|order=flip}} (estimated){{r|ned}}|names=[[2MASX]] J14410437+5320088, [[Lyon-Meudon Extragalactic Database|LEDA]] 84264, [[IRAS]] F14394+5332, IRAS F14394+5332E, [[Sloan Digital Sky Survey|SDSS]] J144104.38+532008.6, AKARI J1441041+532010<ref name="ned" />|image=File:Image of IRAS 14394+5332.png|caption=[[Sloan Digital Sky Survey|SDSS]] image of IRAS 14394+5332. The galaxy on the right of the image is LEDA 2438180.}}
'''IRAS 14394+5332''' is an [[Luminous infrared galaxy|ultraluminous infrared galaxy]] and a [[galaxy merger]] located in the constellation of [[Boötes]]. It has a [[redshift]] of (z) 0.105, estimating the distance to be 1.4 billion light-years from Earth.<ref name="ned">{{Cite web |title=NED Search results for IRAS 14394+5332 |url=https://ned.ipac.caltech.edu/byname?objname=IRAS+14394+5332&hconst=67.8&omegam=0.308&omegav=0.692&wmap=4&corr_z=1 |access-date=2025-08-17 |website=NASA/IPAC Extragalactic Database}}</ref> The galaxy was first discovered by astronomers in 1996 who found it having a total infrared [[luminosity]] of {{val|1.10|e=12}} L<sub>☉</sub>.<ref>{{Cite journal |last1=Murphy |first1=T. W. |last2=Armus |first2=L. |last3=Matthews |first3=K. |last4=Soifer |first4=B. T. |last5=Mazzarella |first5=J. M. |last6=Shupe |first6=D. L. |last7=Strauss |first7=M. A. |last8=Neugebauer |first8=G. |date= 1996|title=Visual and Near-Infrared Imaging of Ultraluminous Infrared Galaxies: The IRAS 2 Jy Sample |url=https://articles.adsabs.harvard.edu/pdf/1996AJ....111.1025M |journal=The Astronomical Journal |language=en |volume=111 |pages=1025 |doi=10.1086/117849 |bibcode=1996AJ....111.1025M |issn=0004-6256}}</ref>{{efn|Given as a log(L<sub>IR</sub>/{{solar luminosity}}) of 12.04.}}
== Description == IRAS 14394+5332 is described as a triple [[interacting galaxy]] system<ref name=":0">{{Cite journal |last1=Dey |first1=Subhrata |last2=Goyal |first2=Arti |last3=Małek |first3=Katarzyna |last4=Díaz-Santos |first4=Tanio |date=2024-04-25 |title=Radio-only and Radio-to-far-ultraviolet Spectral Energy Distribution Modeling of 14 ULIRGs: Insights into the Global Properties of Infrared Bright Galaxies |journal=The Astrophysical Journal |volume=966 |issue=1 |pages=61 |doi=10.3847/1538-4357/ad2c93 |arxiv=2402.10786 |bibcode=2024ApJ...966...61D |doi-access=free |issn=0004-637X}}</ref> consisting of a [[spiral galaxy]] located in western direction and a final-stage double nucleus galaxy merger located in the eastern direction with two closely spaced nuclei, only separating by 2.6 [[Parsec|kiloparsecs]] from each other.<ref name=":1">{{Cite journal |last1=Tadhunter |first1=C |last2=Rodríguez Zaurín |first2=J |last3=Rose |first3=M |last4=Spence |first4=R A W |last5=Batcheldor |first5=D |last6=Berg |first6=M A |last7=Ramos Almeida |first7=C |last8=Spoon |first8=H W W |last9=Sparks |first9=W |last10=Chiaberge |first10=M |date=2018-05-05 |title=Quantifying the AGN-driven outflows in ULIRGs (QUADROS) – II. Evidence for compact outflow regions from HST [O III] imaging observations |journal=Monthly Notices of the Royal Astronomical Society |volume=478 |issue=2 |pages=1558–1569 |doi=10.1093/mnras/sty1064 |doi-access=free |issn=0035-8711|arxiv=1805.00514 }}</ref><ref>{{Cite journal |last1=Rodríguez Zaurín |first1=J. |last2=Tadhunter |first2=C. N. |last3=Delgado |first3=R. M. González |date=2010-04-11 |title=The properties of the stellar populations in ULIRGs - II. Star formation histories and evolution |journal=Monthly Notices of the Royal Astronomical Society |volume=403 |issue=3 |pages=1317–1330 |doi=10.1111/j.1365-2966.2009.16075.x |arxiv=0911.4052 |bibcode=2010MNRAS.403.1317R |doi-access=free |issn=0035-8711}}</ref><ref>{{Cite journal |last1=Meusinger |first1=H. |last2=Stecklum |first2=B. |last3=Theis |first3=C. |last4=Brunzendorf |first4=J. |date=2001-12-01 |title=The merger stage of the ultra-luminous infrared galaxy IRAS 03158+4227 |url=https://www.aanda.org/articles/aa/pdf/2001/45/aa1671.pdf |journal=Astronomy & Astrophysics |language=en |volume=379 |issue=3 |pages=845–854 |doi=10.1051/0004-6361:20011371 |arxiv=astro-ph/0111521 |bibcode=2001A&A...379..845M |issn=0004-6361}}</ref><ref>{{Cite journal |last1=Veilleux |first1=S. |last2=Kim |first2=D.-C. |last3=Sanders |first3=D. B. |date=December 2002 |title=Optical and Near-Infrared Imaging of the''IRAS''1 Jy Sample of Ultraluminous Infrared Galaxies. II. The Analysis |url=https://iopscience.iop.org/article/10.1086/343844/fulltext/ |journal=The Astrophysical Journal Supplement Series |volume=143 |issue=2 |pages=315–376 |doi=10.1086/343844 |arxiv=astro-ph/0207401 |bibcode=2002ApJS..143..315V |issn=0067-0049}}</ref> A long [[tidal tail]] made up diffused [[Radio wave|radio emission]] is seen extending by 35 kiloparsecs between the galaxies.<ref name=":2">{{Cite journal |last1=Dinh-V-Trung |last2=Lo |first2=K. Y. |last3=Kim |first3=D.-C. |last4=Gao |first4=Yu |last5=Gruendl |first5=R. A. |date=July 2001 |title=Nature of Widely Separated Ultraluminous Infrared Galaxies |journal=The Astrophysical Journal |language=en |volume=556 |issue=1 |pages=141–149 |doi=10.1086/321578 |arxiv=astro-ph/0103285 |bibcode=2001ApJ...556..141D |issn=0004-637X}}</ref><ref name=":3">{{Cite journal |last1=Spence |first1=R A W |last2=Tadhunter |first2=C N |last3=Rose |first3=M |last4=Rodríguez Zaurín |first4=J |date=2018-05-07 |title=Quantifying the AGN-driven outflows in ULIRGs (QUADROS) III: measurements of the radii and kinetic powers of eight near-nuclear outflows |journal=Monthly Notices of the Royal Astronomical Society |volume=478 |issue=2 |pages=2438–2460 |doi=10.1093/mnras/sty1046 |doi-access=free |issn=0035-8711|arxiv=1805.02647 }}</ref>
The nucleus on the eastern side of the double nucleus galaxy in the IRAS 14394+5332 system, is found to be [[Active galactic nucleus|active]]. It is described as a [[Seyfert galaxy|Seyfert type 2 galaxy]] based on [[Wavelength|optical wavelength]] observations and is bright at [[Infrared|near-infrared]] wavelengths compared to the faint western nucleus, with it displaying [[Spectral line|emission lines]] in its [[spectrum]].<ref>{{Cite journal |last1=Nandi |first1=S |last2=Das |first2=M |last3=Dwarakanath |first3=K S |date=2021-04-14 |title=Tracing the evolution of ultraluminous infrared galaxies into radio galaxies with low frequency radio observations |journal=Monthly Notices of the Royal Astronomical Society |volume=503 |issue=4 |pages=5746–5762 |doi=10.1093/mnras/stab275 |doi-access=free |issn=0035-8711|arxiv=2102.10600 }}</ref><ref name=":2" /> Furthermore, the morphology of the double nucleus galaxy is complex according to [[Hubble Space Telescope]] optical imaging, who described it having two condensation components that seems to be divided by a [[dust lane]].<ref name=":1" /> HST imaging also found the structure is irregular with the higher [[surface brightness]] feature centering more on the northern condensation component connected with the eastern nucleus.<ref name=":1" />
Observations found the eastern nucleus of the galaxy has detections of nuclear outflows. Based on results, it shows a [[doubly ionized oxygen]] emission-line [[Kinematics|kinematic]] feature best described by three narrow components; mainly a redmost component and two other components described having [[Redshift|blueshift]] measurements of –700 and –1360 kilometers per second. Data also showed these profiles of doubly ionized oxygen emission lines are noticed as different when compared to the other emission lines.<ref>{{Cite journal |last1=Rodríguez Zaurín |first1=J. |last2=Tadhunter |first2=C. N. |last3=Rose |first3=M. |last4=Holt |first4=J. |date=June 2013 |title=The importance of warm, AGN-driven outflows in the nuclear regions of nearby ULIRGs |journal=Monthly Notices of the Royal Astronomical Society |language=en |volume=432 |issue=1 |pages=138–166 |doi=10.1093/mnras/stt423 |arxiv=1303.1400 |doi-access=free |issn=0035-8711}}</ref>
There are also evidence of [[Ionization|ionized]] outflows in the eastern nucleus of the galaxy within a 0.75 ± 0.12 kiloparsec region, with a mass outflow rate of {{val|3.4|13.8|3.0}} [[Solar mass|M<sub>☉</sub>]] per year and a kinetic power measuring {{val|0.66|3.12|0.60}} percent in energy levels.<ref name=":3" /> A total [[Star formation|star formation rate]] of 2.26 ± 0.03 M<sub>☉</sub> per year and a stellar mass of 10.50 ± 0.06 M<sub>☉</sub> has been estimated for the system.<ref name=":0" />
== Notes == {{noteslist}}
== References == <references />
== External links == *[http://simbad.u-strasbg.fr/simbad/sim-id?Ident=2MASX%20J14410437%2B5320088&NbIdent=1 IRAS 14394+5332 on SIMBAD]
{{Boötes}} {{DEFAULTSORT:IRAS 14394 5332}} [[Category:Luminous infrared galaxies]] [[Category:Galaxy mergers]] [[Category:Boötes]] [[Category:IRAS catalogue objects]] [[Category:Interacting galaxies]] [[Category:Seyfert galaxies]] [[Category:Active galaxies]] [[Category:LEDA objects|084264]] [[Category:SDSS objects]] [[Category:Astronomical objects discovered in 1996]]