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Intracluster medium - Wikipedia
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data-mw-ve-target-container> <div class="vector-body-before-content"> <div class="mw-indicators"> </div> <div id="siteSub" class="noprint">From Wikipedia, the free encyclopedia</div> </div> <div id="contentSub"><div id="mw-content-subtitle"></div></div> <div id="mw-content-text" class="mw-body-content"><div class="mw-content-ltr mw-parser-output" lang="en" dir="ltr"><div class="shortdescription nomobile noexcerpt noprint searchaux" style="display:none">Superheated plasma that permeates a galaxy cluster</div> <figure class="mw-halign-right" typeof="mw:File/Thumb"><a href="/wiki/File:The_Sunyaev-Zeldovich_effect_in_the_Spiderweb_protocluster_(eso2304a).jpg" class="mw-file-description"><img src="//upload.wikimedia.org/wikipedia/commons/thumb/7/7c/The_Sunyaev-Zeldovich_effect_in_the_Spiderweb_protocluster_%28eso2304a%29.jpg/320px-The_Sunyaev-Zeldovich_effect_in_the_Spiderweb_protocluster_%28eso2304a%29.jpg" decoding="async" width="320" height="320" class="mw-file-element" srcset="//upload.wikimedia.org/wikipedia/commons/thumb/7/7c/The_Sunyaev-Zeldovich_effect_in_the_Spiderweb_protocluster_%28eso2304a%29.jpg/480px-The_Sunyaev-Zeldovich_effect_in_the_Spiderweb_protocluster_%28eso2304a%29.jpg 1.5x, //upload.wikimedia.org/wikipedia/commons/thumb/7/7c/The_Sunyaev-Zeldovich_effect_in_the_Spiderweb_protocluster_%28eso2304a%29.jpg/640px-The_Sunyaev-Zeldovich_effect_in_the_Spiderweb_protocluster_%28eso2304a%29.jpg 2x" data-file-width="1500" data-file-height="1500" /></a><figcaption>The overlaid blue cloud illustrates the intracluster medium around the <a href="/wiki/Spiderweb_Galaxy" class="mw-redirect" title="Spiderweb Galaxy">Spiderweb Galaxy</a>, as seen when the universe was 3 billion years old</figcaption></figure> <p>In <a href="/wiki/Astronomy" title="Astronomy">astronomy</a>, the <b>intracluster medium</b> (<b>ICM</b>) is the superheated <a href="/wiki/Plasma_(physics)" title="Plasma (physics)">plasma</a> that permeates a <a href="/wiki/Galaxy_cluster" title="Galaxy cluster">galaxy cluster</a>. The gas consists mainly of <a href="/wiki/Ionized_hydrogen" class="mw-redirect" title="Ionized hydrogen">ionized hydrogen</a> and <a href="/wiki/Helium" title="Helium">helium</a> and accounts for most of the <a href="/wiki/Baryon" title="Baryon">baryonic</a> material in galaxy clusters. The ICM is heated to temperatures on the order of 10 to 100 <a href="/wiki/Orders_of_magnitude_(temperature)" title="Orders of magnitude (temperature)">megakelvins</a>, emitting strong <a href="/wiki/X-ray" title="X-ray">X-ray</a> radiation. </p> <meta property="mw:PageProp/toc" /> <div class="mw-heading mw-heading2"><h2 id="Composition">Composition</h2><span class="mw-editsection"><span class="mw-editsection-bracket">[</span><a href="/w/index.php?title=Intracluster_medium&action=edit&section=1" title="Edit section: Composition"><span>edit</span></a><span class="mw-editsection-bracket">]</span></span></div> <p>The ICM is composed primarily of ordinary <a href="/wiki/Baryon" title="Baryon">baryons</a>, mainly ionised hydrogen and helium.<sup id="cite_ref-:0_1-0" class="reference"><a href="#cite_note-:0-1"><span class="cite-bracket">[</span>1<span class="cite-bracket">]</span></a></sup> This plasma is enriched with heavier elements, including <a href="/wiki/Iron" title="Iron">iron</a>. The average amount of heavier elements relative to hydrogen, known as <a href="/wiki/Metallicity" title="Metallicity">metallicity</a> in astronomy, ranges from a third to a half of the value in the <a href="/wiki/Sun" title="Sun">sun</a>.<sup id="cite_ref-:0_1-1" class="reference"><a href="#cite_note-:0-1"><span class="cite-bracket">[</span>1<span class="cite-bracket">]</span></a></sup><sup id="cite_ref-:4_2-0" class="reference"><a href="#cite_note-:4-2"><span class="cite-bracket">[</span>2<span class="cite-bracket">]</span></a></sup> Studying the chemical composition of the ICMs as a function of radius has shown that cores of the galaxy clusters are more metal-rich than at larger radii.<sup id="cite_ref-:4_2-1" class="reference"><a href="#cite_note-:4-2"><span class="cite-bracket">[</span>2<span class="cite-bracket">]</span></a></sup> In some clusters (e.g. the <a href="/wiki/Centaurus_cluster" class="mw-redirect" title="Centaurus cluster">Centaurus cluster</a>) the metallicity of the gas can rise to above that of the sun.<sup id="cite_ref-3" class="reference"><a href="#cite_note-3"><span class="cite-bracket">[</span>3<span class="cite-bracket">]</span></a></sup> Due to the gravitational field of clusters, metal-enriched gas ejected from <a href="/wiki/Supernova" title="Supernova">supernova</a> remains <a href="/wiki/Gravitational_binding_energy" title="Gravitational binding energy">gravitationally bound</a> to the cluster as part of the ICM.<sup id="cite_ref-:4_2-2" class="reference"><a href="#cite_note-:4-2"><span class="cite-bracket">[</span>2<span class="cite-bracket">]</span></a></sup> By looking at varying <a href="/wiki/Redshift" title="Redshift">redshift</a>, which corresponds to looking at different epochs of the evolution of the Universe, the ICM can provide a history record of element production in a galaxy.<sup id="cite_ref-4" class="reference"><a href="#cite_note-4"><span class="cite-bracket">[</span>4<span class="cite-bracket">]</span></a></sup> </p><p>Roughly 15% of a galaxy cluster's mass resides in the ICM. The stars and galaxies contribute only around 5% to the total mass. It is theorized that most of the mass in a galaxy cluster consists of <a href="/wiki/Dark_matter" title="Dark matter">dark matter</a> and not baryonic matter. For the Virgo Cluster, the ICM contains roughly 3 × 10<sup>14</sup> M<sub>☉</sub> while the total mass of the cluster is estimated to be 1.2 × 10<sup>15</sup> M<sub>☉</sub>.<sup id="cite_ref-:0_1-2" class="reference"><a href="#cite_note-:0-1"><span class="cite-bracket">[</span>1<span class="cite-bracket">]</span></a></sup><sup id="cite_ref-5" class="reference"><a href="#cite_note-5"><span class="cite-bracket">[</span>5<span class="cite-bracket">]</span></a></sup> </p><p>Although the ICM on the whole contains the bulk of a cluster's baryons, it is not very dense, with typical values of 10<sup>−3</sup> particles per cubic centimeter. The <a href="/wiki/Mean_free_path" title="Mean free path">mean free path</a> of the particles is roughly 10<sup>16</sup> m, or about one lightyear. The density of the ICM rises towards the centre of the cluster with a relatively strong peak. In addition, the temperature of the ICM typically drops to 1/2 or 1/3 of the outer value in the central regions. Once the density of the plasma reaches a critical value, enough interactions between the ions ensures cooling via X-ray radiation.<sup id="cite_ref-6" class="reference"><a href="#cite_note-6"><span class="cite-bracket">[</span>6<span class="cite-bracket">]</span></a></sup> </p> <div class="mw-heading mw-heading2"><h2 id="Observing_the_intracluster_medium">Observing the intracluster medium</h2><span class="mw-editsection"><span class="mw-editsection-bracket">[</span><a href="/w/index.php?title=Intracluster_medium&action=edit&section=2" title="Edit section: Observing the intracluster medium"><span>edit</span></a><span class="mw-editsection-bracket">]</span></span></div> <p>As the ICM is at such high temperatures, it emits <a href="/wiki/X-ray" title="X-ray">X-ray</a> radiation, mainly by the <a href="/wiki/Bremsstrahlung" title="Bremsstrahlung">bremsstrahlung</a> process and X-ray <a href="/wiki/Emission_lines" class="mw-redirect" title="Emission lines">emission lines</a> from the heavy elements.<sup id="cite_ref-:0_1-3" class="reference"><a href="#cite_note-:0-1"><span class="cite-bracket">[</span>1<span class="cite-bracket">]</span></a></sup> These X-rays can be observed using an <a href="/wiki/X-ray_telescope" title="X-ray telescope">X-ray telescope</a> and through analysis of this data, it is possible to determine the physical conditions, including the temperature, density, and metallicity of the plasma. </p><p>Measurements of the temperature and density profiles in galaxy clusters allow for a determination of the mass distribution profile of the ICM through <a href="/wiki/Hydrostatic_equilibrium" title="Hydrostatic equilibrium">hydrostatic equilibrium</a> modeling. The mass distributions determined from these methods reveal masses that far exceed the luminous mass seen and are thus a strong indication of dark matter in galaxy clusters.<sup id="cite_ref-7" class="reference"><a href="#cite_note-7"><span class="cite-bracket">[</span>7<span class="cite-bracket">]</span></a></sup> </p><p>Inverse <a href="/wiki/Compton_scattering" title="Compton scattering">Compton scattering</a> of low energy photons through interactions with the relativistic electrons in the ICM cause distortions in the spectrum of the <a href="/wiki/Cosmic_microwave_background" title="Cosmic microwave background">cosmic microwave background radiation (CMB)</a>, known as the <a href="/wiki/Sunyaev%E2%80%93Zel%27dovich_effect" class="mw-redirect" title="Sunyaev–Zel'dovich effect">Sunyaev–Zel'dovich effect</a>. These temperature distortions in the CMB can be used by telescopes such as the <a href="/wiki/South_Pole_Telescope" title="South Pole Telescope">South Pole Telescope</a> to detect dense clusters of galaxies at high redshifts.<sup id="cite_ref-8" class="reference"><a href="#cite_note-8"><span class="cite-bracket">[</span>8<span class="cite-bracket">]</span></a></sup> </p><p>In December 2022, the <a href="/wiki/James_Webb_Space_Telescope" title="James Webb Space Telescope">James Webb Space Telescope</a> is reported to be studying the faint light emitted in the intracluster medium.<sup id="cite_ref-SPC-20221209_9-0" class="reference"><a href="#cite_note-SPC-20221209-9"><span class="cite-bracket">[</span>9<span class="cite-bracket">]</span></a></sup> Which a 2018 study found to be an "accurate luminous tracer of dark matter".<sup id="cite_ref-10" class="reference"><a href="#cite_note-10"><span class="cite-bracket">[</span>10<span class="cite-bracket">]</span></a></sup> </p> <div class="mw-heading mw-heading2"><h2 id="Cooling_flows">Cooling flows</h2><span class="mw-editsection"><span class="mw-editsection-bracket">[</span><a href="/w/index.php?title=Intracluster_medium&action=edit&section=3" title="Edit section: Cooling flows"><span>edit</span></a><span class="mw-editsection-bracket">]</span></span></div> <p>Plasma in regions of the cluster, with a cooling time shorter than the age of the system, should be cooling due to strong X-ray radiation where emission is proportional to the density squared. Since the density of the ICM is highest towards the center of the cluster, the radiative cooling time drops a significant amount.<sup id="cite_ref-:3_11-0" class="reference"><a href="#cite_note-:3-11"><span class="cite-bracket">[</span>11<span class="cite-bracket">]</span></a></sup> The central cooled gas can no longer support the weight of the external hot gas and the pressure gradient drives what is known as a <a href="/wiki/Cooling_flow" title="Cooling flow">cooling flow</a> where the hot gas from the external regions flows slowly towards the center of the cluster. This inflow would result in regions of cold gas and thus regions of new star formation.<sup id="cite_ref-:2_12-0" class="reference"><a href="#cite_note-:2-12"><span class="cite-bracket">[</span>12<span class="cite-bracket">]</span></a></sup> Recently however, with the launch of new X-ray telescopes such as the <a href="/wiki/Chandra_X-ray_Observatory" title="Chandra X-ray Observatory">Chandra X-ray Observatory</a>, images of galaxy clusters with better spatial resolution have been taken. These new images do not indicate signs of new star formation on the order of what was historically predicted, motivating research into the mechanisms that would prevent the central ICM from cooling.<sup id="cite_ref-:3_11-1" class="reference"><a href="#cite_note-:3-11"><span class="cite-bracket">[</span>11<span class="cite-bracket">]</span></a></sup> </p> <div class="mw-heading mw-heading2"><h2 id="Heating">Heating</h2><span class="mw-editsection"><span class="mw-editsection-bracket">[</span><a href="/w/index.php?title=Intracluster_medium&action=edit&section=4" title="Edit section: Heating"><span>edit</span></a><span class="mw-editsection-bracket">]</span></span></div> <figure class="mw-default-size" typeof="mw:File/Thumb"><a href="/wiki/File:NASA-PerseusGalaxyCluster-ChandraXRayObservatory-20140624.jpg" class="mw-file-description"><img src="//upload.wikimedia.org/wikipedia/commons/thumb/2/23/NASA-PerseusGalaxyCluster-ChandraXRayObservatory-20140624.jpg/220px-NASA-PerseusGalaxyCluster-ChandraXRayObservatory-20140624.jpg" decoding="async" width="220" height="220" class="mw-file-element" srcset="//upload.wikimedia.org/wikipedia/commons/thumb/2/23/NASA-PerseusGalaxyCluster-ChandraXRayObservatory-20140624.jpg/330px-NASA-PerseusGalaxyCluster-ChandraXRayObservatory-20140624.jpg 1.5x, //upload.wikimedia.org/wikipedia/commons/thumb/2/23/NASA-PerseusGalaxyCluster-ChandraXRayObservatory-20140624.jpg/440px-NASA-PerseusGalaxyCluster-ChandraXRayObservatory-20140624.jpg 2x" data-file-width="3600" data-file-height="3600" /></a><figcaption><a href="/wiki/Chandra_X-ray_Observatory" title="Chandra X-ray Observatory">Chandra</a> image of the <a href="/wiki/Perseus_cluster" class="mw-redirect" title="Perseus cluster">Perseus Cluster</a>'s radio lobes. These relativistic jets of plasma emit <a href="/wiki/Radio_wave" title="Radio wave">radio waves</a>, are X-ray "cold", and appear as dark patches in stark contrast to the rest of the ICM. </figcaption></figure> <p>There are two popular explanations of the mechanisms that prevent the central ICM from cooling: feedback from <a href="/wiki/Active_galactic_nucleus" title="Active galactic nucleus">active galactic nuclei</a> through injection of <a href="/wiki/Astrophysical_jet" title="Astrophysical jet">relativistic jets</a> of plasma<sup id="cite_ref-:1_13-0" class="reference"><a href="#cite_note-:1-13"><span class="cite-bracket">[</span>13<span class="cite-bracket">]</span></a></sup> and sloshing of the ICM plasma during mergers with subclusters.<sup id="cite_ref-14" class="reference"><a href="#cite_note-14"><span class="cite-bracket">[</span>14<span class="cite-bracket">]</span></a></sup><sup id="cite_ref-15" class="reference"><a href="#cite_note-15"><span class="cite-bracket">[</span>15<span class="cite-bracket">]</span></a></sup> The relativistic jets of material from active galactic nuclei can be seen in images taken by telescopes with high angular resolution such as the <a href="/wiki/Chandra_X-ray_Observatory" title="Chandra X-ray Observatory">Chandra X-ray Observatory</a>. </p> <div class="mw-heading mw-heading2"><h2 id="See_also">See also</h2><span class="mw-editsection"><span class="mw-editsection-bracket">[</span><a href="/w/index.php?title=Intracluster_medium&action=edit&section=5" title="Edit section: See also"><span>edit</span></a><span class="mw-editsection-bracket">]</span></span></div> <ul><li><a href="/wiki/Interstellar_medium" title="Interstellar medium">Interstellar medium</a></li></ul> <div class="mw-heading mw-heading2"><h2 id="References">References</h2><span class="mw-editsection"><span class="mw-editsection-bracket">[</span><a href="/w/index.php?title=Intracluster_medium&action=edit&section=6" title="Edit section: References"><span>edit</span></a><span class="mw-editsection-bracket">]</span></span></div> <style data-mw-deduplicate="TemplateStyles:r1239543626">.mw-parser-output .reflist{margin-bottom:0.5em;list-style-type:decimal}@media screen{.mw-parser-output .reflist{font-size:90%}}.mw-parser-output .reflist .references{font-size:100%;margin-bottom:0;list-style-type:inherit}.mw-parser-output .reflist-columns-2{column-width:30em}.mw-parser-output .reflist-columns-3{column-width:25em}.mw-parser-output .reflist-columns{margin-top:0.3em}.mw-parser-output .reflist-columns ol{margin-top:0}.mw-parser-output .reflist-columns li{page-break-inside:avoid;break-inside:avoid-column}.mw-parser-output .reflist-upper-alpha{list-style-type:upper-alpha}.mw-parser-output .reflist-upper-roman{list-style-type:upper-roman}.mw-parser-output .reflist-lower-alpha{list-style-type:lower-alpha}.mw-parser-output .reflist-lower-greek{list-style-type:lower-greek}.mw-parser-output .reflist-lower-roman{list-style-type:lower-roman}</style><div class="reflist"> <div class="mw-references-wrap mw-references-columns"><ol class="references"> <li id="cite_note-:0-1"><span class="mw-cite-backlink">^ <a href="#cite_ref-:0_1-0"><sup><i><b>a</b></i></sup></a> <a href="#cite_ref-:0_1-1"><sup><i><b>b</b></i></sup></a> <a href="#cite_ref-:0_1-2"><sup><i><b>c</b></i></sup></a> <a href="#cite_ref-:0_1-3"><sup><i><b>d</b></i></sup></a></span> <span class="reference-text"><style data-mw-deduplicate="TemplateStyles:r1238218222">.mw-parser-output cite.citation{font-style:inherit;word-wrap:break-word}.mw-parser-output .citation q{quotes:"\"""\"""'""'"}.mw-parser-output .citation:target{background-color:rgba(0,127,255,0.133)}.mw-parser-output .id-lock-free.id-lock-free a{background:url("//upload.wikimedia.org/wikipedia/commons/6/65/Lock-green.svg")right 0.1em center/9px no-repeat}.mw-parser-output .id-lock-limited.id-lock-limited a,.mw-parser-output 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Vol. 1201. pp. 383–386. <a href="/wiki/ArXiv_(identifier)" class="mw-redirect" title="ArXiv (identifier)">arXiv</a>:<span class="id-lock-free" title="Freely accessible"><a rel="nofollow" class="external text" href="https://arxiv.org/abs/0909.0560">0909.0560</a></span>. <a href="/wiki/Bibcode_(identifier)" class="mw-redirect" title="Bibcode (identifier)">Bibcode</a>:<a rel="nofollow" class="external text" href="https://ui.adsabs.harvard.edu/abs/2009AIPC.1201..383Z">2009AIPC.1201..383Z</a>. <a href="/wiki/CiteSeerX_(identifier)" class="mw-redirect" title="CiteSeerX (identifier)">CiteSeerX</a> <span class="id-lock-free" title="Freely accessible"><a rel="nofollow" class="external text" href="https://citeseerx.ist.psu.edu/viewdoc/summary?doi=10.1.1.246.2787">10.1.1.246.2787</a></span>. <a href="/wiki/Doi_(identifier)" class="mw-redirect" title="Doi (identifier)">doi</a>:<a rel="nofollow" class="external text" href="https://doi.org/10.1063%2F1.3293082">10.1063/1.3293082</a>. <a href="/wiki/S2CID_(identifier)" class="mw-redirect" title="S2CID (identifier)">S2CID</a> <a rel="nofollow" class="external text" href="https://api.semanticscholar.org/CorpusID:119287922">119287922</a>.</cite><span title="ctx_ver=Z39.88-2004&rft_val_fmt=info%3Aofi%2Ffmt%3Akev%3Amtx%3Abook&rft.genre=conference&rft.btitle=Cluster+Core+Heating+from+Merging+Subclusters&rft.series=AIP+Conference+Proceedings&rft.pages=383-386&rft.date=2009-01-01&rft_id=https%3A%2F%2Fapi.semanticscholar.org%2FCorpusID%3A119287922%23id-name%3DS2CID&rft_id=info%3Abibcode%2F2009AIPC.1201..383Z&rft_id=https%3A%2F%2Fciteseerx.ist.psu.edu%2Fviewdoc%2Fsummary%3Fdoi%3D10.1.1.246.2787%23id-name%3DCiteSeerX&rft_id=info%3Adoi%2F10.1063%2F1.3293082&rft_id=info%3Aarxiv%2F0909.0560&rft.aulast=ZuHone&rft.aufirst=J.+A.&rft.au=Markevitch%2C+M.&rfr_id=info%3Asid%2Fen.wikipedia.org%3AIntracluster+medium" class="Z3988"></span></span> </li> <li id="cite_note-15"><span class="mw-cite-backlink"><b><a href="#cite_ref-15">^</a></b></span> <span class="reference-text"><link rel="mw-deduplicated-inline-style" href="mw-data:TemplateStyles:r1238218222"><cite id="CITEREFFabian2002" class="citation book cs1">Fabian, Andrew C. 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Springer, Berlin, Heidelberg. pp. 24–36. <a href="/wiki/ArXiv_(identifier)" class="mw-redirect" title="ArXiv (identifier)">arXiv</a>:<span class="id-lock-free" title="Freely accessible"><a rel="nofollow" class="external text" href="https://arxiv.org/abs/astro-ph/0201386">astro-ph/0201386</a></span>. <a href="/wiki/CiteSeerX_(identifier)" class="mw-redirect" title="CiteSeerX (identifier)">CiteSeerX</a> <span class="id-lock-free" title="Freely accessible"><a rel="nofollow" class="external text" href="https://citeseerx.ist.psu.edu/viewdoc/summary?doi=10.1.1.255.3254">10.1.1.255.3254</a></span>. <a href="/wiki/Doi_(identifier)" class="mw-redirect" title="Doi (identifier)">doi</a>:<a rel="nofollow" class="external text" href="https://doi.org/10.1007%2F10856495_3">10.1007/10856495_3</a>. <a href="/wiki/ISBN_(identifier)" class="mw-redirect" title="ISBN (identifier)">ISBN</a> <a href="/wiki/Special:BookSources/978-3-540-43769-7" title="Special:BookSources/978-3-540-43769-7"><bdi>978-3-540-43769-7</bdi></a>. <a href="/wiki/S2CID_(identifier)" class="mw-redirect" title="S2CID (identifier)">S2CID</a> <a rel="nofollow" class="external text" href="https://api.semanticscholar.org/CorpusID:118831315">118831315</a>.</cite><span title="ctx_ver=Z39.88-2004&rft_val_fmt=info%3Aofi%2Ffmt%3Akev%3Amtx%3Abook&rft.genre=bookitem&rft.atitle=Cooling+Flows+in+Clusters+of+Galaxies&rft.btitle=Lighthouses+of+the+Universe%3A+The+Most+Luminous+Celestial+Objects+and+Their+Use+for+Cosmology&rft.series=Eso+Astrophysics+Symposia&rft.pages=24-36&rft.pub=Springer%2C+Berlin%2C+Heidelberg&rft.date=2002&rft_id=https%3A%2F%2Fapi.semanticscholar.org%2FCorpusID%3A118831315%23id-name%3DS2CID&rft_id=info%3Adoi%2F10.1007%2F10856495_3&rft_id=https%3A%2F%2Fciteseerx.ist.psu.edu%2Fviewdoc%2Fsummary%3Fdoi%3D10.1.1.255.3254%23id-name%3DCiteSeerX&rft_id=info%3Aarxiv%2Fastro-ph%2F0201386&rft.isbn=978-3-540-43769-7&rft.aulast=Fabian&rft.aufirst=Andrew+C.&rfr_id=info%3Asid%2Fen.wikipedia.org%3AIntracluster+medium" class="Z3988"></span></span> </li> </ol></div></div> <!-- NewPP limit report Parsed by mw‐web.codfw.main‐5857dfdcd6‐w7flh Cached time: 20241203071738 Cache expiry: 2592000 Reduced expiry: false Complications: [vary‐revision‐sha1, show‐toc] CPU time usage: 0.282 seconds Real time usage: 0.370 seconds Preprocessor visited node count: 1135/1000000 Post‐expand include size: 42444/2097152 bytes Template argument size: 624/2097152 bytes Highest expansion depth: 8/100 Expensive parser function count: 1/500 Unstrip recursion depth: 1/20 Unstrip post‐expand size: 61600/5000000 bytes Lua time usage: 0.173/10.000 seconds Lua memory usage: 4897168/52428800 bytes Number of Wikibase entities loaded: 0/400 --> <!-- Transclusion expansion time report (%,ms,calls,template) 100.00% 321.490 1 -total 66.12% 212.567 1 Template:Reflist 30.02% 96.520 1 Template:Short_description 29.36% 94.377 2 Template:Cite_book 20.12% 64.698 9 Template:Cite_journal 13.75% 44.208 3 Template:Main_other 13.13% 42.223 1 Template:SDcat 12.53% 40.287 2 Template:Pagetype 4.52% 14.543 2 Template:Cite_news 2.20% 7.058 1 Template:Cite_conference --> <!-- Saved in parser cache with key enwiki:pcache:4217326:|#|:idhash:canonical and timestamp 20241203071738 and revision id 1258053716. 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