Phoenix Cluster

[[File:Phoenix Cluster center, artist's depiction.jpg|thumb|left|200px|Artist's depiction of the center of the Phoenix Cluster, showing the central black hole and its accretion disc that fuels two powerful jets emanating from the nucleus
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[[File:Phoenix Cluster center, artist's depiction.jpg|thumb|left|200px|Artist's depiction of the center of the Phoenix Cluster, showing the central black hole and its accretion disc that fuels two powerful jets emanating from the nucleus
]]

Owing to its extreme properties, the Phoenix Cluster has been extensively studied and is considered one of the most important class of objects of its type. A multi-wavelength observational study by M. McDonald and colleagues show that it has an extremely strong [[cooling flow]] rate (roughly 3,280 {{solar mass}} per annum), described as a runaway cooling flow. This measurement is one of the highest ever seen in the middle of a galaxy cluster. The very strong cooling flow, in contrast to other galaxy clusters, has been a suggested result of the feedback mechanism to prevent a runaway cooling flow which may not be established yet in the Phoenix Cluster; the heating mechanism expected to be produced by the central black hole being inadequate to create a feedback (in contrast to the [[Perseus Cluster|Perseus]] and [[Virgo Cluster|Virgo]] clusters). This is further supported by the high starburst activity of the central galaxy Phoenix A, where stars are formed at 740 {{solar mass}} per annum (compared to the [[Milky Way]]'s 1 {{solar mass}} per annum of star production); the central active galactic nucleus attested to not have been producing sufficient energy to ionize the galaxy's gas and prevent starburst activity.{{Cite journal |last1=McDonald |first1=Michael |last2=Benson |first2=Bradford |last3=Veilleux |first3=Sylvain |last4=Bautz |first4=Marshall W. |last5=Reichardt |first5=Christian L. |date=22 February 2013 |title=An HST/WFC3-UVIS View of the Starburst in the Cool Core of the Phoenix Cluster |journal=[[The Astrophysical Journal]] |volume=765 |issue=2 |pages=L37 |arxiv=1211.7058 |bibcode=2013ApJ...765L..37M |doi=10.1088/2041-8205/765/2/L37 |issn=2041-8205}}

Owing to its extreme properties, the Phoenix Cluster has been extensively studied and is considered one of the most important class of objects of its type. A multiwavelength observational study by M. McDonald and colleagues show that it has an extremely strong [[cooling flow]] rate (roughly 3,280 {{solar mass}} per annum), described as a runaway cooling flow. This measurement is one of the highest ever seen in the middle of a galaxy cluster. The very strong cooling flow, in contrast to other galaxy clusters, has been a suggested result of the feedback mechanism to prevent a runaway cooling flow which may not be established yet in the Phoenix Cluster; the heating mechanism expected to be produced by the central black hole being inadequate to create a feedback (in contrast to the [[Perseus Cluster|Perseus]] and [[Virgo Cluster|Virgo]] clusters). This is further supported by the high starburst activity of the central galaxy Phoenix A, where stars are formed at 740 {{solar mass}} per annum (compared to the [[Milky Way]]'s 1 {{solar mass}} per annum of star production); the central active galactic nucleus attested to not have been producing sufficient energy to ionize the galaxy's gas and prevent starburst activity.{{Cite journal |last1=McDonald |first1=Michael |last2=Benson |first2=Bradford |last3=Veilleux |first3=Sylvain |last4=Bautz |first4=Marshall W. |last5=Reichardt |first5=Christian L. |date=22 February 2013 |title=An HST/WFC3-UVIS View of the Starburst in the Cool Core of the Phoenix Cluster |journal=[[The Astrophysical Journal]] |volume=765 |issue=2 |pages=L37 |arxiv=1211.7058 |bibcode=2013ApJ...765L..37M |doi=10.1088/2041-8205/765/2/L37 |issn=2041-8205}}

The cluster has the highest X-ray luminosity compared to other clusters.{{Cite journal |last=Talcott |first=Richard |title=A Galaxy Cluster Conundrum |journal=[[Astronomy (magazine)|Astronomy]] |volume=53 |issue=8 |pages=36}}

The cluster has the highest X-ray luminosity compared to other clusters.{{Cite journal |last=Talcott |first=Richard |title=A Galaxy Cluster Conundrum |journal=[[Astronomy (magazine)|Astronomy]] |volume=53 |issue=8 |pages=36}}

* A circumference that would take 71 days and 14 hours to travel at [[Speed of light|light speed]].

* A circumference that would take 71 days and 14 hours to travel at [[Speed of light|light speed]].

Such a high mass may place it into a proposed category of [[Ultramassive black holes|Ultramassive Black Holes]] or [[stupendously large black hole|Stupendously Large Black Hole]]s (SLABs), black holes that may have been seeded by [[primordial black hole]]s with masses that may reach {{solar mass|100 billion}} or more, larger than the upper maximum limit for at least luminous accreting [[supermassive black hole|black hole]]s hosted by disc galaxies of about {{solar mass|50 billion}}.{{Cite journal |last1=Carr |first1=Bernard |last2=Kühnel |first2=Florian |last3=Visinelli |first3=Luca |display-authors=1 |date=2 January 2021 |title=Constraints on stupendously large black holes |journal=[[Monthly Notices of the Royal Astronomical Society]] |volume=501 |issue=2 |pages=2029–2043 |arxiv=2008.08077 |bibcode=2021MNRAS.501.2029C |doi=10.1093/mnras/staa3651 |issn=0035-8711 |doi-access=free}}

Such a high mass may place it into a proposed category of [[stupendously large black hole]]s (SLABs), black holes that may have been seeded by [[primordial black hole]]s with masses that may reach {{solar mass|100 billion}} or more, larger than the upper maximum limit for at least luminous accreting [[supermassive black hole|black hole]]s hosted by disc galaxies of about {{solar mass|50 billion}}.{{Cite journal |last1=Carr |first1=Bernard |last2=Kühnel |first2=Florian |last3=Visinelli |first3=Luca |display-authors=1 |date=2 January 2021 |title=Constraints on stupendously large black holes |journal=[[Monthly Notices of the Royal Astronomical Society]] |volume=501 |issue=2 |pages=2029–2043 |arxiv=2008.08077 |bibcode=2021MNRAS.501.2029C |doi=10.1093/mnras/staa3651 |issn=0035-8711 |doi-access=free}}

Now, the {{solar mass|100 billion}} estimates aren't fully set in stone, and it's not for just one reason. Unlike other titanic black holes such as [[TON 618|TON-618]], Phoenix A* wasn't estimated using direct methods. Rather, it used thermodynamics and a [[Colorimetry (chemical method)|calorimetric]] method to calculate the cooling rate of gas from the surrounding cluster. Additionally, Phoenix A*'s primary source of pushback originates from the rate of star formation within its host galaxy. A typical black hole of above {{solar mass|50 billion}} would result in it heating up and blowing away surrounding gas, nullifying star formation. The issue lies within the fact that Phoenix A* lies within a hyperactive [[galaxy cluster]], churning new stars at a rate on the order of ~{{solar mass|740}} per year, indicative of a black hole of lower estimates—some even going as low as 40-{{solar mass|50 billion}}.{{Cite web |title=Reddit - Please wait for verification |url=https://www.reddit.com/r/Astronomy/comments/1gk9o2r/why_does_everyone_still_claim_ton_618_to_be_the/#:~:text=Phoenix%20A's%20mass%20&%20size%20has,%E2%80%A2%201y%20ago |access-date=2026-04-19 |website=www.reddit.com}}

== JWST observations ==

== JWST observations ==