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== Features ==
== Features ==
IRAS 09104+4109 has an [[active galactic nucleus]] (AGN). It is a [[Seyfert galaxy|Seyfert type 2 galaxy]]<ref>{{Cite journal |last=Rowan-Robinson |first=M. |date=2000-08-01 |title=Hyperluminous infrared galaxies |url=https://ui.adsabs.harvard.edu/abs/2000MNRAS.316..885R |journal=Monthly Notices of the Royal Astronomical Society |volume=316 |issue=4 |pages=885–900 |doi=10.1046/j.1365-8711.2000.03588.x |arxiv=astro-ph/9912286 |bibcode=2000MNRAS.316..885R |issn=0035-8711}}</ref> with a strong [[Spectral line|emission-line]] [[spectrum]] (z = 0.442), with a range of [[Excitation spectrum|excitations]] and very large equivalent widths but shows no broad lines. Moreover, IRAS 09104+4109 is classified a [[Type-cD galaxy|cD galaxy]] located inside a cool rich [[Galaxy cluster|cluster of galaxies]],<ref>{{Cite web |last1=Vignali |first1=C. |last2=Piconcelli |first2=E. |last3=Lanzuisi |first3=G. C. Feruglio, R. Maiolino, F. Fiore, J. Fritz, V. La Parola, M. Mignoli, F. Pozzi |last4=Feltre |first4=A. |last5=Feruglio |first5=C. |last6=Maiolino |first6=R. |last7=Fiore |first7=F. |last8=Fritz |first8=J. |last9=La Parola |first9=V. |title=On the nature of the absorber in IRAS 09104+4109: the X-ray and mid-infrared view |url=https://academic.oup.com/mnras/article/416/3/2068/962044?login=false |access-date=2024-05-21 |website=academic.oup.com}}</ref><ref name=":0">{{Cite journal |last1=Kleinmann |first1=S. G. |last2=Hamilton |first2=Donald |last3=Keel |first3=W. C. |last4=Wynn-Williams |first4=C. G. |last5=Eales |first5=S. A. |last6=Becklin |first6=E. E. |last7=Kuntz |first7=K. D. |date=1988-05-01 |title=The Properties and Environment of the Giant, Infrared-Luminous Galaxy IRAS 09104+4109 |url=https://ui.adsabs.harvard.edu/abs/1988ApJ...328..161K |journal=The Astrophysical Journal |volume=328 |pages=161 |doi=10.1086/166276 |bibcode=1988ApJ...328..161K |issn=0004-637X}}</ref> experiencing a [[cooling flow]].<ref>{{Cite journal |last1=Fabian |first1=A. C. |last2=Crawford |first2=C. S. |date=1995-06-01 |title=ROSAT HRI observations of IRAS P09104+4109: a massive cooling flow |url=https://ui.adsabs.harvard.edu/abs/1995MNRAS.274L..63F |journal=Monthly Notices of the Royal Astronomical Society |volume=274 |issue=4 |pages=L63–L66 |doi=10.1093/mnras/274.1.L63 |arxiv=astro-ph/9505052 |bibcode=1995MNRAS.274L..63F |issn=0035-8711}}</ref> The galaxy is the most [[Luminous efficiency function|luminous]] object to be discovered by [[IRAS]] survey, emitting 6 x 10^12^ L_sun_ h^-2^, which 99% of the energy emerges at infrared [[wavelength]]s. The high luminosity of IRAS 09104+4109 might be related to an interaction with one or more members of the rich cluster in which it lies.<ref name=":0"/> It is selected by its strong 60 m emission (>0.5 Jy), yet faint [[Apparent magnitude|optical magnitude]] (''V''>18).<ref name=":0" />
IRAS 09104+4109 has an [[active galactic nucleus]] (AGN). It is a [[Seyfert galaxy|Seyfert type 2 galaxy]]<ref>{{Cite journal |last=Rowan-Robinson |first=M. |date=2000-08-01 |title=Hyperluminous infrared galaxies |journal=Monthly Notices of the Royal Astronomical Society |volume=316 |issue=4 |pages=885–900 |doi=10.1046/j.1365-8711.2000.03588.x |doi-access=free |arxiv=astro-ph/9912286 |bibcode=2000MNRAS.316..885R |issn=0035-8711}}</ref> with a strong [[Spectral line|emission-line]] [[spectrum]] (z = 0.442), with a range of [[Excitation spectrum|excitations]] and very large equivalent widths but shows no broad lines. Moreover, IRAS 09104+4109 is classified a [[Type-cD galaxy|cD galaxy]] located inside a cool rich [[Galaxy cluster|cluster of galaxies]],<ref>{{Cite web |last1=Vignali |first1=C. |last2=Piconcelli |first2=E. |last3=Lanzuisi |first3=G. C. Feruglio, R. Maiolino, F. Fiore, J. Fritz, V. La Parola, M. Mignoli, F. Pozzi |last4=Feltre |first4=A. |last5=Feruglio |first5=C. |last6=Maiolino |first6=R. |last7=Fiore |first7=F. |last8=Fritz |first8=J. |last9=La Parola |first9=V. |title=On the nature of the absorber in IRAS 09104+4109: the X-ray and mid-infrared view |url=https://academic.oup.com/mnras/article/416/3/2068/962044?login=false |access-date=2024-05-21 |website=academic.oup.com}}</ref><ref name=":0">{{Cite journal |last1=Kleinmann |first1=S. G. |last2=Hamilton |first2=Donald |last3=Keel |first3=W. C. |last4=Wynn-Williams |first4=C. G. |last5=Eales |first5=S. A. |last6=Becklin |first6=E. E. |last7=Kuntz |first7=K. D. |date=1988-05-01 |title=The Properties and Environment of the Giant, Infrared-Luminous Galaxy IRAS 09104+4109 |url=https://ui.adsabs.harvard.edu/abs/1988ApJ...328..161K |journal=The Astrophysical Journal |volume=328 |pages=161 |doi=10.1086/166276 |bibcode=1988ApJ...328..161K |issn=0004-637X}}</ref> experiencing a [[cooling flow]].<ref>{{Cite journal |last1=Fabian |first1=A. C. |last2=Crawford |first2=C. S. |date=1995-06-01 |title=ROSAT HRI observations of IRAS P09104+4109: a massive cooling flow |journal=Monthly Notices of the Royal Astronomical Society |volume=274 |issue=4 |pages=L63–L66 |doi=10.1093/mnras/274.1.L63 |doi-access=free |arxiv=astro-ph/9505052 |bibcode=1995MNRAS.274L..63F |issn=0035-8711}}</ref> The galaxy is the most [[Luminous efficiency function|luminous]] object to be discovered by [[IRAS]] survey, emitting 6 x 10^12^ L_sun_ h^-2^, which 99% of the energy emerges at infrared [[wavelength]]s. The high luminosity of IRAS 09104+4109 might be related to an interaction with one or more members of the rich cluster in which it lies.<ref name=":0"/> It is selected by its strong 60 m emission (>0.5 Jy), yet faint [[Apparent magnitude|optical magnitude]] (''V''>18).<ref name=":0" />


The galaxy shows a "warm" far-[[Infrared|IR color]] ''F''(25 m)/''F''(60 m) of 0.3, similar to of luminous optically selected quasars and suggests that much of the far-IR emission is emitted from dust heated by the central [[ultraviolet]] (UV) continuum source.<ref>{{Cite journal |last1=de Grijp |first1=M. H. K. |last2=Miley |first2=G. K. |last3=Lub |first3=J. |last4=de Jong |first4=T. |date=1985-03-01 |title=Infrared Seyferts: a new population of active galaxies? |url=https://ui.adsabs.harvard.edu/abs/1985Natur.314..240D |journal=Nature |volume=314 |issue=6008 |pages=240–242 |doi=10.1038/314240a0 |bibcode=1985Natur.314..240D |issn=0028-0836}}</ref><ref>{{Cite journal |last1=Neugebauer |first1=G. |last2=Miley |first2=G. K. |last3=Soifer |first3=B. T. |last4=Clegg |first4=P. E. |date=1986-09-01 |title=Quasars Measured by the Infrared Astronomical Satellite |url=https://ui.adsabs.harvard.edu/abs/1986ApJ...308..815N |journal=The Astrophysical Journal |volume=308 |pages=815 |doi=10.1086/164553 |bibcode=1986ApJ...308..815N |hdl=1887/6519 |issn=0004-637X}}</ref> The [[rest frame]] of UV/optical spectrum of the nucleus shows a type 2 spectrum with strong, narrow emission lines covering a range of [[ionization]]s. This implies [[photoionization]] by a strong UV nonthermal continuum.<ref>{{Cite journal |last1=Soifer |first1=B. T. |last2=Neugebauer |first2=G. |last3=Armus |first3=L. |last4=Shupe |first4=D. L. |date=1996-02-01 |title=Near Infrared Observations of IRAS 09104+4109 |url=https://ui.adsabs.harvard.edu/abs/1996AJ....111..649S |journal=The Astronomical Journal |volume=111 |pages=649 |doi=10.1086/117814 |bibcode=1996AJ....111..649S |issn=0004-6256}}</ref><ref>{{Cite journal |last1=Evans |first1=A. S. |last2=Sanders |first2=D. B. |last3=Cutri |first3=R. M. |last4=Radford |first4=S. J. E. |last5=Surace |first5=J. A. |last6=Solomon |first6=P. M. |last7=Downes |first7=D. |last8=Kramer |first8=C. |date=1998-10-01 |title=Near-Infrared Spectroscopy and a Search for CO Emission in Three Extremely Luminous IRAS Sources: IRAS F09105+4108, IRAS F15307+3252, and PG 1634+706 |url=https://ui.adsabs.harvard.edu/abs/1998ApJ...506..205E |journal=The Astrophysical Journal |volume=506 |issue=1 |pages=205–221 |doi=10.1086/306234 |arxiv=astro-ph/9806091 |bibcode=1998ApJ...506..205E |issn=0004-637X}}</ref>
The galaxy shows a "warm" far-[[Infrared|IR color]] ''F''(25 m)/''F''(60 m) of 0.3, similar to of luminous optically selected quasars and suggests that much of the far-IR emission is emitted from dust heated by the central [[ultraviolet]] (UV) continuum source.<ref>{{Cite journal |last1=de Grijp |first1=M. H. K. |last2=Miley |first2=G. K. |last3=Lub |first3=J. |last4=de Jong |first4=T. |date=1985-03-01 |title=Infrared Seyferts: a new population of active galaxies? |url=https://ui.adsabs.harvard.edu/abs/1985Natur.314..240D |journal=Nature |volume=314 |issue=6008 |pages=240–242 |doi=10.1038/314240a0 |bibcode=1985Natur.314..240D |issn=0028-0836}}</ref><ref>{{Cite journal |last1=Neugebauer |first1=G. |last2=Miley |first2=G. K. |last3=Soifer |first3=B. T. |last4=Clegg |first4=P. E. |date=1986-09-01 |title=Quasars Measured by the Infrared Astronomical Satellite |url=https://ui.adsabs.harvard.edu/abs/1986ApJ...308..815N |journal=The Astrophysical Journal |volume=308 |pages=815 |doi=10.1086/164553 |bibcode=1986ApJ...308..815N |hdl=1887/6519 |issn=0004-637X}}</ref> The [[rest frame]] of UV/optical spectrum of the nucleus shows a type 2 spectrum with strong, narrow emission lines covering a range of [[ionization]]s. This implies [[photoionization]] by a strong UV nonthermal continuum.<ref>{{Cite journal |last1=Soifer |first1=B. T. |last2=Neugebauer |first2=G. |last3=Armus |first3=L. |last4=Shupe |first4=D. L. |date=1996-02-01 |title=Near Infrared Observations of IRAS 09104+4109 |url=https://ui.adsabs.harvard.edu/abs/1996AJ....111..649S |journal=The Astronomical Journal |volume=111 |pages=649 |doi=10.1086/117814 |bibcode=1996AJ....111..649S |issn=0004-6256}}</ref><ref>{{Cite journal |last1=Evans |first1=A. S. |last2=Sanders |first2=D. B. |last3=Cutri |first3=R. M. |last4=Radford |first4=S. J. E. |last5=Surace |first5=J. A. |last6=Solomon |first6=P. M. |last7=Downes |first7=D. |last8=Kramer |first8=C. |date=1998-10-01 |title=Near-Infrared Spectroscopy and a Search for CO Emission in Three Extremely Luminous IRAS Sources: IRAS F09105+4108, IRAS F15307+3252, and PG 1634+706 |url=https://ui.adsabs.harvard.edu/abs/1998ApJ...506..205E |journal=The Astrophysical Journal |volume=506 |issue=1 |pages=205–221 |doi=10.1086/306234 |arxiv=astro-ph/9806091 |bibcode=1998ApJ...506..205E |issn=0004-637X}}</ref>
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A study conducted in 2007, proves IRAS 09104+4109 as the first "changing-look quasar". This was done by having researchers to analyze the [[Spectroscopy|spectroscopic data]] from the ''PN'' and the ''MOS'' [[camera]]s in the 0.4–10 [[keV]] band. They also used an archival ''BeppoSAX'' 1–50 keV observation of to investigate the possible variations of the quasar emission and found that the [[X-ray]] emission in the ''EPIC'' band is dominated by the [[Intracluster medium|intra-cluster medium]] [[Thermal radiation|thermal]] emission, which the quasar contributes ~35% of the total flux in the 2–10 keV band.<ref>{{Cite journal |last1=Piconcelli |first1=E. |last2=Fiore |first2=F. |last3=Nicastro |first3=F. |last4=Mathur |first4=S. |last5=Brusa |first5=M. |last6=Comastri |first6=A. |last7=Puccetti |first7=S. |date=2007-10-01 |title=The XMM-Newton view of IRAS 09104+4109: evidence for a changing-look Type 2 quasar? |url=https://www.aanda.org/articles/aa/abs/2007/37/aa7630-07/aa7630-07.html |journal=Astronomy & Astrophysics |language=en |volume=473 |issue=1 |pages=85–89 |doi=10.1051/0004-6361:20077630 |arxiv=0707.2465 |bibcode=2007A&A...473...85P |issn=0004-6361}}</ref>
A study conducted in 2007, proves IRAS 09104+4109 as the first "changing-look quasar". This was done by having researchers to analyze the [[Spectroscopy|spectroscopic data]] from the ''PN'' and the ''MOS'' [[camera]]s in the 0.4–10 [[keV]] band. They also used an archival ''BeppoSAX'' 1–50 keV observation of to investigate the possible variations of the quasar emission and found that the [[X-ray]] emission in the ''EPIC'' band is dominated by the [[Intracluster medium|intra-cluster medium]] [[Thermal radiation|thermal]] emission, which the quasar contributes ~35% of the total flux in the 2–10 keV band.<ref>{{Cite journal |last1=Piconcelli |first1=E. |last2=Fiore |first2=F. |last3=Nicastro |first3=F. |last4=Mathur |first4=S. |last5=Brusa |first5=M. |last6=Comastri |first6=A. |last7=Puccetti |first7=S. |date=2007-10-01 |title=The XMM-Newton view of IRAS 09104+4109: evidence for a changing-look Type 2 quasar? |url=https://www.aanda.org/articles/aa/abs/2007/37/aa7630-07/aa7630-07.html |journal=Astronomy & Astrophysics |language=en |volume=473 |issue=1 |pages=85–89 |doi=10.1051/0004-6361:20077630 |arxiv=0707.2465 |bibcode=2007A&A...473...85P |issn=0004-6361}}</ref>


Further studies in 2012, showed that IRAS 09104+4109 is a rare example of a [[Cosmic dust|dust enshrouded]] quasar which also associated with a double-lobed [[Astronomical radio source|radio source]] at the [[position angle]] of =333° (probably an [[Fanaroff–Riley classification|FR II]] radio source).<ref>{{Cite web |last1=Fanaroff |first1=B. L. |last2=Riley |first2=J. M. |title=The Morphology of Extragalactic Radio Sources of High and Low Luminosity |url=https://academic.oup.com/mnras/article/167/1/31P/2604898?login=false |access-date=2024-05-21 |website=academic.oup.com}}</ref> However, the steep radio [[spectral index]] and [[Misalignment mechanism|misalignment]] between the jets and ionized [[Optical Emission Spectrometer|optical emission]] suggested that the orientation of the quasar in IRAS 09104+4109 had recently changed. To prove this [[hypothesis]], researchers used a combination of new, multiband [[Giant Metrewave Radio Telescope]] [[observation]]s and archival [[Radio data communication|radio data]] and confirmed that the jets in IRAS 09104+ 4109, estimated to 20-160 Myr, are no longer actively fed by energetic particles.<ref name=":1" /> This results suggested that the realignment of the quasar, the cessation of jet activity and the onset of rapid [[star formation]] in IRAS 09104+4109, may have been caused by a gas-rich [[galaxy merger]].<ref>{{Cite journal |last1=O'Sullivan |first1=Ewan |last2=Giacintucci |first2=Simona |last3=Babul |first3=Arif |last4=Raychaudhury |first4=Somak |last5=Venturi |first5=Tiziana |last6=Bildfell |first6=Chris |last7=Mahdavi |first7=Andisheh |last8=Oonk |first8=J. B. R. |last9=Murray |first9=Norman |last10=Hoekstra |first10=Henk |last11=Donahue |first11=Megan |date=2012-08-01 |title=A Giant Metrewave Radio Telescope/Chandra view of IRAS 09104+4109: a type 2 QSO in a cooling flow |url=https://ui.adsabs.harvard.edu/abs/2012MNRAS.424.2971O |journal=Monthly Notices of the Royal Astronomical Society |volume=424 |issue=4 |pages=2971–2993 |doi=10.1111/j.1365-2966.2012.21459.x |arxiv=1206.1525 |bibcode=2012MNRAS.424.2971O |issn=0035-8711}}</ref>
Further studies in 2012, showed that IRAS 09104+4109 is a rare example of a [[Cosmic dust|dust enshrouded]] quasar which also associated with a double-lobed [[Astronomical radio source|radio source]] at the [[position angle]] of =333° (probably an [[Fanaroff–Riley classification|FR II]] radio source).<ref>{{Cite web |last1=Fanaroff |first1=B. L. |last2=Riley |first2=J. M. |title=The Morphology of Extragalactic Radio Sources of High and Low Luminosity |url=https://academic.oup.com/mnras/article/167/1/31P/2604898?login=false |access-date=2024-05-21 |website=academic.oup.com}}</ref> However, the steep radio [[spectral index]] and [[Misalignment mechanism|misalignment]] between the jets and ionized [[Optical Emission Spectrometer|optical emission]] suggested that the orientation of the quasar in IRAS 09104+4109 had recently changed. To prove this [[hypothesis]], researchers used a combination of new, multiband [[Giant Metrewave Radio Telescope]] [[observation]]s and archival [[Radio data communication|radio data]] and confirmed that the jets in IRAS 09104+ 4109, estimated to 20-160 Myr, are no longer actively fed by energetic particles.<ref name=":1" /> This results suggested that the realignment of the quasar, the cessation of jet activity and the onset of rapid [[star formation]] in IRAS 09104+4109, may have been caused by a gas-rich [[galaxy merger]].<ref>{{Cite journal |last1=O'Sullivan |first1=Ewan |last2=Giacintucci |first2=Simona |last3=Babul |first3=Arif |last4=Raychaudhury |first4=Somak |last5=Venturi |first5=Tiziana |last6=Bildfell |first6=Chris |last7=Mahdavi |first7=Andisheh |last8=Oonk |first8=J. B. R. |last9=Murray |first9=Norman |last10=Hoekstra |first10=Henk |last11=Donahue |first11=Megan |date=2012-08-01 |title=A Giant Metrewave Radio Telescope/Chandra view of IRAS 09104+4109: a type 2 QSO in a cooling flow |journal=Monthly Notices of the Royal Astronomical Society |volume=424 |issue=4 |pages=2971–2993 |doi=10.1111/j.1365-2966.2012.21459.x |doi-access=free |arxiv=1206.1525 |bibcode=2012MNRAS.424.2971O |issn=0035-8711}}</ref>


A [[Northern Extended Millimeter Array]] (NOEMA) found there are traces of [[Oxocarbon|carbon oxide]] (2–1) in the z=0.4418 cluster-central IRAS 09104+4109, which ~4.5x10^10 M sol of [[Atomic and molecular astrophysics|molecular gas]] is found, in and around the galaxy. As in many low redshift cool core clusters, the gas is located in a series of clumps extending along the old [[Astrophysical jet|radio jets]] and [[Radio lobe|lobes]]. It has a relatively low [[velocity dispersion]] of (336 [+39,-35] km/s [[Full width at half maximum|FWHM]]) and shows no [[velocity gradient]]s indicative of outflow or infall. Roughly, half its gas is located in a central clump on the northeast side of the galaxy, overlapping a bright ionized [[Galaxy filament|gas filament]] and a spur of excess X-ray [[Emission spectrum|emission]], suggesting that this is a location of rapid cooling.<ref name=":2">{{Cite journal |last1=O'Sullivan |first1=Ewan |last2=Combes |first2=Françoise |last3=Babul |first3=Arif |last4=Chapman |first4=Scott |last5=Phadke |first5=Kedar A. |last6=Schellenberger |first6=Gerrit |last7=Salomé |first7=Philippe |date=2021-10-20 |title=Molecular gas along the old radio jets of the cluster-central type 2 quasar IRAS 09104+4109 |journal=Monthly Notices of the Royal Astronomical Society |volume=508 |issue=3 |pages=3796–3811 |doi=10.1093/mnras/stab2825 |arxiv=2109.13756 |issn=0035-8711}}</ref> The molecular gas is unusually extended, outwards to ~55 kpc radius, which is comparable to the scale of the filamentary [[nebula]] in the [[Perseus Cluster|Perseus cluster]], the higher redshift of this system. The extent falls within the [[Convective instability|thermal instability]] radius of the intracluster medium (ICM), with t cool/t_ff<25 and t_cool}/t_eddy~1 within ~70 kpc. [[Continuum (measurement)|Continuum measurements]] at 159.9 [[Hertz|GHz]] from NOEMA and 850 [[micron]] from the JCMT SCUBA-2 show excess far infrared emission, which we interpret as free-free emission arising from the ongoing [[Starburst galaxy|starburst]]. These observations suggest that the ICM cooling is not strongly affected by its buried quasar, and that cooling from the ICM can build [[Petroleum reservoir|gas reservoirs]] sufficient enough, to fuel the quasar-mode activity and drive the reorientation of its central AGN.<ref name=":2" />
A [[Northern Extended Millimeter Array]] (NOEMA) found there are traces of [[Oxocarbon|carbon oxide]] (2–1) in the z=0.4418 cluster-central IRAS 09104+4109, which ~4.5x10^10 M sol of [[Atomic and molecular astrophysics|molecular gas]] is found, in and around the galaxy. As in many low redshift cool core clusters, the gas is located in a series of clumps extending along the old [[Astrophysical jet|radio jets]] and [[Radio lobe|lobes]]. It has a relatively low [[velocity dispersion]] of (336 [+39,-35] km/s [[Full width at half maximum|FWHM]]) and shows no [[velocity gradient]]s indicative of outflow or infall. Roughly, half its gas is located in a central clump on the northeast side of the galaxy, overlapping a bright ionized [[Galaxy filament|gas filament]] and a spur of excess X-ray [[Emission spectrum|emission]], suggesting that this is a location of rapid cooling.<ref name=":2">{{Cite journal |last1=O'Sullivan |first1=Ewan |last2=Combes |first2=Françoise |last3=Babul |first3=Arif |last4=Chapman |first4=Scott |last5=Phadke |first5=Kedar A. |last6=Schellenberger |first6=Gerrit |last7=Salomé |first7=Philippe |date=2021-10-20 |title=Molecular gas along the old radio jets of the cluster-central type 2 quasar IRAS 09104+4109 |journal=Monthly Notices of the Royal Astronomical Society |volume=508 |issue=3 |pages=3796–3811 |doi=10.1093/mnras/stab2825 |doi-access=free |arxiv=2109.13756 |issn=0035-8711}}</ref> The molecular gas is unusually extended, outwards to ~55 kpc radius, which is comparable to the scale of the filamentary [[nebula]] in the [[Perseus Cluster|Perseus cluster]], the higher redshift of this system. The extent falls within the [[Convective instability|thermal instability]] radius of the intracluster medium (ICM), with t cool/t_ff<25 and t_cool}/t_eddy~1 within ~70 kpc. [[Continuum (measurement)|Continuum measurements]] at 159.9 [[Hertz|GHz]] from NOEMA and 850 [[micron]] from the JCMT SCUBA-2 show excess far infrared emission, which we interpret as free-free emission arising from the ongoing [[Starburst galaxy|starburst]]. These observations suggest that the ICM cooling is not strongly affected by its buried quasar, and that cooling from the ICM can build [[Petroleum reservoir|gas reservoirs]] sufficient enough, to fuel the quasar-mode activity and drive the reorientation of its central AGN.<ref name=":2" />


== References ==
== References ==

Revision as of 21:08, 16 July 2024

IRAS 09104+4109
IRAS 09104+4109 captured by SDSS
Observation data (J2000 epoch)
ConstellationLynx
Right ascension09h 13m 45.49s
Declination+40d 56m 28.22s
Redshift0.440797
Heliocentric radial velocity132,148 km/s
Distance4.885 Gly (1497.7 Mpc)
Group or clusterCDGS 25
Apparent magnitude (V)0.54
Apparent magnitude (B)0.43
Surface brightness18.8
Characteristics
TypeQSO2, HyLIRG
Apparent size (V)0.14' x 0.09'
Notable featuresLuminous infrared galaxy containing a quasar
Other designations
WN B0910+4108, PGC 97525, NVSS J091345+405630, IRAS F09105+4108, RX J0913.7+4056, 2XMM J091345.5+405629, 2CXO J091345.5+405628

IRAS 09104+4109 is a galaxy located in the constellation Lynx. With a redshift of 0.440797, the light travel time for this galaxy, corresponds to 4.8 billion light-years from Earth.[1] It is the brightest cluster galaxy in CDGS 25, also known as WHL J091345.5+405628[2] and a notable, unique ultraluminous infrared galaxy.[3][4]

Features

IRAS 09104+4109 has an active galactic nucleus (AGN). It is a Seyfert type 2 galaxy[5] with a strong emission-line spectrum (z = 0.442), with a range of excitations and very large equivalent widths but shows no broad lines. Moreover, IRAS 09104+4109 is classified a cD galaxy located inside a cool rich cluster of galaxies,[6][7] experiencing a cooling flow.[8] The galaxy is the most luminous object to be discovered by IRAS survey, emitting 6 x 10^12^ L_sun_ h^-2^, which 99% of the energy emerges at infrared wavelengths. The high luminosity of IRAS 09104+4109 might be related to an interaction with one or more members of the rich cluster in which it lies.[7] It is selected by its strong 60 m emission (>0.5 Jy), yet faint optical magnitude (V>18).[7]

The galaxy shows a "warm" far-IR color F(25 m)/F(60 m) of 0.3, similar to of luminous optically selected quasars and suggests that much of the far-IR emission is emitted from dust heated by the central ultraviolet (UV) continuum source.[9][10] The rest frame of UV/optical spectrum of the nucleus shows a type 2 spectrum with strong, narrow emission lines covering a range of ionizations. This implies photoionization by a strong UV nonthermal continuum.[11][12]

IRAS 09104+4109 has a luminosity bolometer of ~ 1012.6 h-2 L sun, which its optical spectrum is characterized by the presence of narrow emission lines, although broad Balmer and Mg II lines were observed in polarized light.[13][14] These findings, found there is a quasar inside IRAS 09104+4109, ionizing the narrow-line region and heats dust within ~130 pc of its central engine.[13] Furthermore, IRAS 09104+4109 produces a radio jet.[15]

A study conducted in 2007, proves IRAS 09104+4109 as the first "changing-look quasar". This was done by having researchers to analyze the spectroscopic data from the PN and the MOS cameras in the 0.4–10 keV band. They also used an archival BeppoSAX 1–50 keV observation of to investigate the possible variations of the quasar emission and found that the X-ray emission in the EPIC band is dominated by the intra-cluster medium thermal emission, which the quasar contributes ~35% of the total flux in the 2–10 keV band.[16]

Further studies in 2012, showed that IRAS 09104+4109 is a rare example of a dust enshrouded quasar which also associated with a double-lobed radio source at the position angle of =333° (probably an FR II radio source).[17] However, the steep radio spectral index and misalignment between the jets and ionized optical emission suggested that the orientation of the quasar in IRAS 09104+4109 had recently changed. To prove this hypothesis, researchers used a combination of new, multiband Giant Metrewave Radio Telescope observations and archival radio data and confirmed that the jets in IRAS 09104+ 4109, estimated to 20-160 Myr, are no longer actively fed by energetic particles.[13] This results suggested that the realignment of the quasar, the cessation of jet activity and the onset of rapid star formation in IRAS 09104+4109, may have been caused by a gas-rich galaxy merger.[18]

A Northern Extended Millimeter Array (NOEMA) found there are traces of carbon oxide (2–1) in the z=0.4418 cluster-central IRAS 09104+4109, which ~4.5x10^10 M sol of molecular gas is found, in and around the galaxy. As in many low redshift cool core clusters, the gas is located in a series of clumps extending along the old radio jets and lobes. It has a relatively low velocity dispersion of (336 [+39,-35] km/s FWHM) and shows no velocity gradients indicative of outflow or infall. Roughly, half its gas is located in a central clump on the northeast side of the galaxy, overlapping a bright ionized gas filament and a spur of excess X-ray emission, suggesting that this is a location of rapid cooling.[19] The molecular gas is unusually extended, outwards to ~55 kpc radius, which is comparable to the scale of the filamentary nebula in the Perseus cluster, the higher redshift of this system. The extent falls within the thermal instability radius of the intracluster medium (ICM), with t cool/t_ff<25 and t_cool}/t_eddy~1 within ~70 kpc. Continuum measurements at 159.9 GHz from NOEMA and 850 micron from the JCMT SCUBA-2 show excess far infrared emission, which we interpret as free-free emission arising from the ongoing starburst. These observations suggest that the ICM cooling is not strongly affected by its buried quasar, and that cooling from the ICM can build gas reservoirs sufficient enough, to fuel the quasar-mode activity and drive the reorientation of its central AGN.[19]

References

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  16. ^ Piconcelli, E.; Fiore, F.; Nicastro, F.; Mathur, S.; Brusa, M.; Comastri, A.; Puccetti, S. (2007-10-01). "The XMM-Newton view of IRAS 09104+4109: evidence for a changing-look Type 2 quasar?". Astronomy & Astrophysics. 473 (1): 85–89. arXiv:0707.2465. Bibcode:2007A&A...473...85P. doi:10.1051/0004-6361:20077630. ISSN 0004-6361.
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  18. ^ O'Sullivan, Ewan; Giacintucci, Simona; Babul, Arif; Raychaudhury, Somak; Venturi, Tiziana; Bildfell, Chris; Mahdavi, Andisheh; Oonk, J. B. R.; Murray, Norman; Hoekstra, Henk; Donahue, Megan (2012-08-01). "A Giant Metrewave Radio Telescope/Chandra view of IRAS 09104+4109: a type 2 QSO in a cooling flow". Monthly Notices of the Royal Astronomical Society. 424 (4): 2971–2993. arXiv:1206.1525. Bibcode:2012MNRAS.424.2971O. doi:10.1111/j.1365-2966.2012.21459.x. ISSN 0035-8711.
  19. ^ a b O'Sullivan, Ewan; Combes, Françoise; Babul, Arif; Chapman, Scott; Phadke, Kedar A.; Schellenberger, Gerrit; Salomé, Philippe (2021-10-20). "Molecular gas along the old radio jets of the cluster-central type 2 quasar IRAS 09104+4109". Monthly Notices of the Royal Astronomical Society. 508 (3): 3796–3811. arXiv:2109.13756. doi:10.1093/mnras/stab2825. ISSN 0035-8711.
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