{"id":991,"date":"2024-05-01T11:23:00","date_gmt":"2024-05-01T09:23:00","guid":{"rendered":"http:\/\/matlas.astro.unistra.fr\/WP\/?p=991"},"modified":"2024-08-22T11:32:38","modified_gmt":"2024-08-22T09:32:38","slug":"the-size-and-structure-of-globular-cluster-systems-and-their-connection-to-dark-matter-halos-2","status":"publish","type":"post","link":"https:\/\/matlas.astro.unistra.fr\/WP\/?p=991","title":{"rendered":"The Size and Structure of Globular Cluster Systems and Their Connection to Dark Matter Halos"},"content":{"rendered":"\n<figure class=\"wp-block-image size-large\"><img loading=\"lazy\" width=\"1024\" height=\"576\" src=\"http:\/\/matlas.astro.unistra.fr\/WP\/wp-content\/uploads\/2024\/08\/apjad3444f18_lr-1024x576.jpg\" alt=\"\" class=\"wp-image-992\" srcset=\"https:\/\/matlas.astro.unistra.fr\/WP\/wp-content\/uploads\/2024\/08\/apjad3444f18_lr-1024x576.jpg 1024w, https:\/\/matlas.astro.unistra.fr\/WP\/wp-content\/uploads\/2024\/08\/apjad3444f18_lr-300x169.jpg 300w, https:\/\/matlas.astro.unistra.fr\/WP\/wp-content\/uploads\/2024\/08\/apjad3444f18_lr-768x432.jpg 768w, https:\/\/matlas.astro.unistra.fr\/WP\/wp-content\/uploads\/2024\/08\/apjad3444f18_lr-1536x865.jpg 1536w, https:\/\/matlas.astro.unistra.fr\/WP\/wp-content\/uploads\/2024\/08\/apjad3444f18_lr.jpg 1997w\" sizes=\"(max-width: 767px) 89vw, (max-width: 1000px) 54vw, (max-width: 1071px) 543px, 580px\" \/><figcaption>The effective radii of GC systems plotted against the total number of GCs (Lim+2024)<\/figcaption><\/figure>\n\n\n\n<p>We study the size and structure of globular cluster (GC) systems of 118 early-type galaxies from the NGVS, MATLAS, and ACSVCS surveys. Fitting S\u00e9rsic profiles, we investigate the relationship between effective radii of GC systems (R\u00a0<sub>e,gc<\/sub>) and galaxy properties.<\/p>\n\n\n\n<!--more-->\n\n\n\n<p>GC systems are 2\u20134 times more extended than host galaxies across the entire stellar mass range of our sample (10<sup>8.3<\/sup>\u00a0M\u00a0<sub>\u2299<\/sub>\u00a0&lt; M\u00a0<sub>*<\/sub>\u00a0&lt; 10<sup>11.6<\/sup>\u00a0M\u00a0<sub>\u2299<\/sub>). The relationship between R\u00a0<sub>e,gc<\/sub>\u00a0and galaxy stellar mass exhibits a characteristic &#8220;knee&#8221; at a stellar mass of M\u00a0<sub>p\u00a0<\/sub>\u2243 10<sup>10.8<\/sup>, similar to the galaxy R\u00a0<sub>e\u00a0<\/sub>\u2013stellar mass relationship. We present a new characterization of the traditional blue and red GC color subpopulations, describing them with respect to host galaxy $(g^{\\prime} -i^{\\prime} )$ color (\u0394<sub>gi<\/sub>): GCs with similar colors to their hosts have a &#8220;red&#8221; \u0394<sub>gi<\/sub>, and those significantly bluer GCs have a &#8220;blue&#8221; \u0394<sub>gi<\/sub>. The GC populations with red \u0394<sub>gi<\/sub>, even in dwarf galaxies, are twice as extended as the stars, suggesting that formation or survival mechanisms favor the outer regions. We find a tight correlation between R\u00a0<sub>e,gc<\/sub>\u00a0and the total number of GCs, with intrinsic scatter \u22720.1 dex spanning two and three orders of magnitude in size and number, respectively. This holds for both red and blue subpopulations, albeit with different slopes. Assuming that N\u00a0<sub>GC,Total<\/sub>\u00a0correlates with M\u00a0<sub>200<\/sub>, we find that the red GC systems have effective radii of roughly 1%\u20135% R\u00a0<sub>200<\/sub>, while the blue GC systems in massive galaxies can have sizes as large as \u223c10% R\u00a0<sub>200<\/sub>. Environmental dependence on R\u00a0<sub>e,gc<\/sub>\u00a0is also found, with lower-density environments exhibiting more extended GC systems at fixed mass.<\/p>\n\n\n\n<p>Lim, S. et al., 2024, <a href=\"https:\/\/ui.adsabs.harvard.edu\/abs\/2024ApJ...966..168L\/abstract\" data-type=\"URL\" data-id=\"https:\/\/ui.adsabs.harvard.edu\/abs\/2024ApJ...966..168L\/abstract\">ApJ 966, 168<\/a><\/p>\n","protected":false},"excerpt":{"rendered":"<p>We study the size and structure of globular cluster (GC) systems of 118 early-type galaxies from the NGVS, MATLAS, and ACSVCS surveys. Fitting S\u00e9rsic profiles, we investigate the relationship between effective radii of GC systems (R\u00a0e,gc) and galaxy properties.<\/p>\n","protected":false},"author":1,"featured_media":0,"comment_status":"open","ping_status":"open","sticky":false,"template":"","format":"standard","meta":[],"categories":[4],"tags":[],"_links":{"self":[{"href":"https:\/\/matlas.astro.unistra.fr\/WP\/index.php?rest_route=\/wp\/v2\/posts\/991"}],"collection":[{"href":"https:\/\/matlas.astro.unistra.fr\/WP\/index.php?rest_route=\/wp\/v2\/posts"}],"about":[{"href":"https:\/\/matlas.astro.unistra.fr\/WP\/index.php?rest_route=\/wp\/v2\/types\/post"}],"author":[{"embeddable":true,"href":"https:\/\/matlas.astro.unistra.fr\/WP\/index.php?rest_route=\/wp\/v2\/users\/1"}],"replies":[{"embeddable":true,"href":"https:\/\/matlas.astro.unistra.fr\/WP\/index.php?rest_route=%2Fwp%2Fv2%2Fcomments&post=991"}],"version-history":[{"count":1,"href":"https:\/\/matlas.astro.unistra.fr\/WP\/index.php?rest_route=\/wp\/v2\/posts\/991\/revisions"}],"predecessor-version":[{"id":993,"href":"https:\/\/matlas.astro.unistra.fr\/WP\/index.php?rest_route=\/wp\/v2\/posts\/991\/revisions\/993"}],"wp:attachment":[{"href":"https:\/\/matlas.astro.unistra.fr\/WP\/index.php?rest_route=%2Fwp%2Fv2%2Fmedia&parent=991"}],"wp:term":[{"taxonomy":"category","embeddable":true,"href":"https:\/\/matlas.astro.unistra.fr\/WP\/index.php?rest_route=%2Fwp%2Fv2%2Fcategories&post=991"},{"taxonomy":"post_tag","embeddable":true,"href":"https:\/\/matlas.astro.unistra.fr\/WP\/index.php?rest_route=%2Fwp%2Fv2%2Ftags&post=991"}],"curies":[{"name":"wp","href":"https:\/\/api.w.org\/{rel}","templated":true}]}}