[{"data":1,"prerenderedAt":-1},["ShallowReactive",2],{"doc-detail-135432-en":3,"doc-seo-135432-105":31,"detail-sidebar-cat-0-en-105":93},{"code":4,"msg":5,"data":6},0,"success",{"doc_id":7,"user_id":8,"nickname":9,"user_avatar":10,"doc_module":4,"category_id":11,"category_name":12,"doc_title":13,"doc_description":14,"doc_content":15,"file_id":16,"file_url":17,"file_type":18,"file_size":19,"view_count":20,"is_deleted":4,"is_public":21,"is_downloadable":21,"audit_status":21,"page_count":22,"language":23,"language_code":24,"site_id":25,"html_lang":24,"table_of_contents":26,"faqs":27,"seo_title":28,"seo_description":14,"update_tm":29,"read_time":30},135432,1374402739827,"Nguyễn Văn Học","https://ap-avatar.wpscdn.com/avatar/14000c97e7351f1a627?x-image-process=image/resize,m_fixed,w_180,h_180&k=1787885694763230660",8,"Research & Report","3D modeling of the molecular gas kinematics in optically-selected jellyfish galaxies","Cluster galaxies are shaped by ram pressure from the intracluster medium, which can disturb or strip their gas while keeping the stellar component relatively intact. The study models star and molecular-gas distribution and kinematics in four late-type cluster systems (JO201, JO204, JO206, JW100) using MUSE@VLT and ALMA/CO data. Results indicate stellar bars in all but possibly JW100, ram-pressure signatures in JO201 and JO206, molecular-disk outskirts stripping in JO206, and rotation-dominated kinematics in JO204, with molecular gas turbulence enhanced and environment-insensitive mass-size behavior.","arXiv :2301 .03090v2 [ astro-ph .GA] 7 Apr 2023  \nDraft version April 10, 2023  \nTypeset using LATEX twocolumn style in AASTeX631  \n3D modeling of the molecular gas kinematics in optically-selected jelly􀀌sh galaxies  \nCecilia Bacchini  ,1 Matilde Mingozzi  ,2 Bianca M. Poggianti  ,1 Alessia Moretti  ,1 Marco Gullieuszik  ,1 Antonino Marasco  ,1 Bernardo Cervantes Sodi  ,3 Osbaldo Snchez-Garca  3  \n,  \nBenedetta Vulcani  ,1 Ariel Werle  ,1 Rosita Paladino  ,4 and Mario Radovich 1  \n1 INAF - Osservatorio Astronomico di Padova, vicolo dell'Osservatorio 5, IT-35122 Padova, Italy  \n2 Space Telescope Science Institute, 3700 San Martin Drive, Baltimore, MD 21218, USA  \n3 Istituto de Radioastronom􀀓􀀐a y Astrof􀀓􀀐sica, Universidad Nacional Aut􀀓onoma de M􀀓exico, Campus Morelia, A. P. 3-72, C. P. 58089, Michoac􀀓an, M􀀓exico  \n4 INAF - Istituto di Radioastronomia, via P. Gobetti 101, I-40129 Bologna, Italy  \nABSTRACT  \nCluster galaxies are subject to the ram pressure exerted by the intracluster medium, which can perturb or even strip away their gas while leaving the stars undisturbed. We model the distribution and kinematics of the stars and the molecular gas in four late-type cluster galaxies (JO201, JO204, JO206, and JW100), which show tails of atomic and ionized gas indicative of ongoing ram pressure stripping. We analyze MUSE@VLT data and CO data from ALMA searching for signatures of radial gas 􀀍ows, ram pressure stripping, and other perturbations. We 􀀌nd that all galaxies, with the possible exception of JW100, host stellar bars. Signatures of ram pressure are found in JO201 and JO206, which also shows clear indications of ongoing stripping in the molecular disk outskirts. The stripping a􀀋ects the whole molecular gas disk of JW100 . The molecular gas kinematics in JO204 is instead dominated by rotation rather than ram pressure. We also 􀀌nd indications of enhanced turbulence of the molecular gas compared to 􀀌eld galaxies. Large-scale radial 􀀍ows of molecular gas are present in JO204 and JW100, but more uncertain in JO201 and JO206 . We show that our sample follows the molecular gas mass-size relation, con􀀌rming that it is essentially independent of environment even for the most extreme cases of stripping. Our 􀀌ndings are consistent with the molecular gas being a􀀋ected by the ram pressure on di􀀋erent timescales and less severely than the atomic and ionized gas phases, likely because the molecular gas is denser and more gravitationally bound to the galaxy.  \n1. INTRODUCTION  \nIn dense environments, such as groups and clusters, galaxies are a􀀋ected by various physical mechanisms that can signi􀀌cantly in􀀍uence their properties and evolution (Nulsen 1982; Boselli & Gavazzi 2006; Corteseet al. 2021) . These processes are usually divided into gravitational and hydrodynamical interactions (Boselli et al. 2022a) . Gravitational perturbations can be induced by tidal forces due to the potential of other cluster/group members (Merritt 1983) or the large scale structure itself (Byrd & Valtonen 1990), but also by 􀀍yby encounters and mergers (Barnes & Hernquist 1992; Kronberger et al. 2006) . Gravitational interactions affect both the stellar and the gaseous components of galaxies. Instead, the hydrodynamical interactions be  \nCorresponding author: Cecilia Bacchini  \n[cecilia.bacchini@inaf.it](cecilia.bacchini@inaf.it)  \ntween the galactic interstellar medium (ISM) and the intracluster medium (ICM) are expected to in􀀍uence only the gaseous components of galaxies. These mechanisms are the thermal evaporation of the cold and warm (T . 104 K) ISM due to the interaction of the hot (T 􀀙 107 􀀀 108 K) ICM (Cowie & Songaila 1977), the removal of the outer ISM layer due to the viscosity momentum transfer with the ICM (viscous stripping) or instabilities (Nulsen 1982; Roediger & Hensler 2008), and the ram pressure stripping, that is the removal of the ISM due to the pressure exerted by the ICM while a galaxy is moving through the cluster (Gunn & Gott 1972) . In a","cbCaibT5lP9v7vQY","https://ap.wps.com/l/cbCaibT5lP9v7vQY","pdf",3678360,6,1,29,"English","en",105,"# Abstract\n# Introduction\n## Environmental mechanisms shaping cluster galaxies\n## Hydrodynamical interactions and ram pressure stripping\n## Expected ram-pressure effects on gas morphology and kinematics","[{\"question\":\"What environmental process drives the gas disturbance in cluster galaxies in this study?\",\"answer\":\"Ram pressure exerted by the intracluster medium perturbs or can strip gas from cluster galaxies while leaving stars relatively undisturbed.\"},{\"question\":\"Which observational data are used to study stars and molecular gas?\",\"answer\":\"The analysis uses MUSE@VLT data for the stellar and ionized components and ALMA CO data to trace molecular gas kinematics and distribution.\"},{\"question\":\"How do the galaxies in the sample differ in the role of ram pressure?\",\"answer\":\"Ram-pressure signatures are found in JO201 and JO206, where JO206 also shows clear ongoing stripping in molecular-disk outskirts. JO204 is dominated by rotation rather than ram pressure, and JW100 shows stripping effects mainly on the molecular gas disk.\"}]","3D modeling of the molecular gas kinematics in optically-selected jellyfish galaxies | PDF",1787312127,73,{"code":4,"msg":32,"data":33},"ok",{"site_id":25,"language":24,"slug":34,"title":13,"keywords":35,"description":14,"schema_data":36,"social_meta":88,"head_meta":90,"extra_data":92,"updated_unix":29},"3d-modeling-of-the-molecular-gas-kinematics-in-optically-selected-jellyfish-galaxies","",{"@graph":37,"@context":87},[38,55,70],{"@type":39,"itemListElement":40},"BreadcrumbList",[41,45,49,52],{"item":42,"name":43,"@type":44,"position":21},"https://docshare.wps.com","Home","ListItem",{"item":46,"name":47,"@type":44,"position":48},"https://docshare.wps.com/document/","Document",2,{"item":50,"name":12,"@type":44,"position":51},"https://docshare.wps.com/document/research-report/",3,{"item":53,"name":13,"@type":44,"position":54},"https://docshare.wps.com/document/3d-modeling-of-the-molecular-gas-kinematics-in-optically-selected-jellyfish-galaxies/135432/",4,{"url":53,"name":13,"@type":56,"author":57,"headline":13,"publisher":59,"fileFormat":62,"inLanguage":24,"description":14,"dateModified":63,"datePublished":64,"encodingFormat":62,"isAccessibleForFree":65,"interactionStatistic":66},"DigitalDocument",{"name":9,"@type":58},"Person",{"url":42,"name":60,"@type":61},"DocShare","Organization","application/pdf","2026-08-30","2026-08-21",true,{"@type":67,"interactionType":68,"userInteractionCount":20},"InteractionCounter",{"@type":69},"ViewAction",{"@type":71,"mainEntity":72},"FAQPage",[73,79,83],{"name":74,"@type":75,"acceptedAnswer":76},"What environmental process drives the gas disturbance in cluster galaxies in this study?","Question",{"text":77,"@type":78},"Ram pressure exerted by the intracluster medium perturbs or can strip gas from cluster galaxies while leaving stars relatively undisturbed.","Answer",{"name":80,"@type":75,"acceptedAnswer":81},"Which observational data are used to study stars and molecular gas?",{"text":82,"@type":78},"The analysis uses MUSE@VLT data for the stellar and ionized components and ALMA CO data to trace molecular gas kinematics and distribution.",{"name":84,"@type":75,"acceptedAnswer":85},"How do the galaxies in the sample differ in the role of ram pressure?",{"text":86,"@type":78},"Ram-pressure signatures are found in JO201 and JO206, where JO206 also shows clear ongoing stripping in molecular-disk outskirts. JO204 is dominated by rotation rather than ram pressure, and JW100 shows stripping effects mainly on the molecular gas disk.","https://schema.org",{"og:url":53,"og:type":89,"og:title":13,"og:site_name":60,"og:description":14},"article",{"robots":91,"canonical":53},"index,follow",{"doc_id":7,"site_id":25},{"code":4,"msg":5,"data":94},[95,99,103,107,112,116,121,124,129,132,136],{"id":21,"doc_module":4,"doc_module_name":47,"category_name":96,"show_sort_weight":97,"slug":98},"Story & Novel",90,"story-novel",{"id":48,"doc_module":4,"doc_module_name":47,"category_name":100,"show_sort_weight":101,"slug":102},"Literature",80,"literature",{"id":54,"doc_module":4,"doc_module_name":47,"category_name":104,"show_sort_weight":105,"slug":106},"Exam",70,"exam",{"id":108,"doc_module":4,"doc_module_name":47,"category_name":109,"show_sort_weight":110,"slug":111},5,"Comic",60,"comic",{"id":20,"doc_module":4,"doc_module_name":47,"category_name":113,"show_sort_weight":114,"slug":115},"Technology",50,"technology",{"id":117,"doc_module":4,"doc_module_name":47,"category_name":118,"show_sort_weight":119,"slug":120},7,"Healthcare",40,"healthcare",{"id":11,"doc_module":4,"doc_module_name":47,"category_name":12,"show_sort_weight":122,"slug":123},30,"research-report",{"id":125,"doc_module":4,"doc_module_name":47,"category_name":126,"show_sort_weight":127,"slug":128},9,"Religion & Spirituality",20,"religion-spirituality",{"id":127,"doc_module":4,"doc_module_name":47,"category_name":130,"show_sort_weight":127,"slug":131},"World Cup","world-cup",{"id":133,"doc_module":4,"doc_module_name":47,"category_name":134,"show_sort_weight":133,"slug":135},10,"Lifestyle","lifestyle",{"id":137,"doc_module":4,"doc_module_name":47,"category_name":138,"show_sort_weight":108,"slug":139},19,"General","general"]