{"id":704,"date":"2025-06-23T15:27:05","date_gmt":"2025-06-23T15:27:05","guid":{"rendered":"https:\/\/bluemuse.univ-lyon1.fr\/?page_id=704"},"modified":"2025-07-21T11:56:52","modified_gmt":"2025-07-21T11:56:52","slug":"swg1-the-local-volume","status":"publish","type":"page","link":"https:\/\/bluemuse.univ-lyon1.fr\/index.php\/swg1-the-local-volume\/","title":{"rendered":"SWG1: The Local Volume"},"content":{"rendered":"<p><strong>Key Science Case: <a href=\"https:\/\/bluemuse.univ-lyon1.fr\/index.php\/swg1-key-science-case-massive-stars\/\">Massive Stars<\/a><\/strong><\/p>\n<p><strong>Additional science cases:<\/strong><\/p>\n<ul>\n<li>BlueMUSE will provide systematic <strong>maps of <\/strong><strong>stellar properties and chemical compositions for very massive clusters in the Milky Way and local group galaxies<\/strong>, such as NGC 2070 in the Large Magellanic Cloud. Its unique wavelength coverage in the blue range (4000 &#8211; 5000 \u00c5) is essential for accessing key diagnostic lines, such as [OII], [SiII\/III\/IV], and [NII]. Since hot stars are intrinsically blue, BlueMUSE\u2019s wavelength coverage aligns closely with the peak of their spectral energy distributions, offering significant advantages over MUSE. Additionally, the large spectral resolution of BlueMUSE will enable a more detailed exploration of the kinematics and the presence of binary within these environments.<\/li>\n<\/ul>\n<p><img loading=\"lazy\" decoding=\"async\" class=\" wp-image-709 alignleft\" src=\"https:\/\/bluemuse.univ-lyon1.fr\/wp-content\/myimages\/2025\/06\/SWG1_Fig1-293x300.png\" alt=\"\" width=\"397\" height=\"407\" srcset=\"https:\/\/bluemuse.univ-lyon1.fr\/wp-content\/myimages\/2025\/06\/SWG1_Fig1-293x300.png 293w, https:\/\/bluemuse.univ-lyon1.fr\/wp-content\/myimages\/2025\/06\/SWG1_Fig1-1001x1024.png 1001w, https:\/\/bluemuse.univ-lyon1.fr\/wp-content\/myimages\/2025\/06\/SWG1_Fig1-768x785.png 768w, https:\/\/bluemuse.univ-lyon1.fr\/wp-content\/myimages\/2025\/06\/SWG1_Fig1-1502x1536.png 1502w, https:\/\/bluemuse.univ-lyon1.fr\/wp-content\/myimages\/2025\/06\/SWG1_Fig1.png 1594w\" sizes=\"auto, (max-width: 397px) 100vw, 397px\" \/><\/p>\n<p><i><span lang=\"EN-US\">Figure 1. Three colour image of the star-forming region N180 in the Large Magellanic Cloud, imaged with MUSE as a 64-pointing mosaic (8<\/span><\/i><i><span dir=\"RTL\" lang=\"AR-SA\">\u2019<\/span><\/i><i><span lang=\"EN-US\">x8<\/span><\/i><i><span dir=\"RTL\" lang=\"AR-SA\">\u2019<\/span><\/i><i><span lang=\"EN-US\">). The red, green, and blue colours are [SII]6717, H\u03b1, and [OIII]5007, respectively. Image from <a href=\"https:\/\/ui.adsabs.harvard.edu\/abs\/2019MNRAS.486.5263M\/abstract\">McLeod et al. (2019)<\/a>.<\/span><\/i><\/p>\n<ul>\n<li>In our Galaxy and within the Local Group BlueMUSE will be able to map physical properties at the smallest physical scales (sub-parsec). The aim of these studies is to <strong>understand the interplay between stellar feedback and the immediate surrounding medium.<\/strong> At intermediate distances (2 and 10 Mpc), the panoramic BlueMUSE field of view will enable to map the diffuse ionised gas component, physical conditions, abundances, and kinematics of the ionised gas in large and diverse samples of resolved nebulae. The wavelength range covered by BlueMUSE will provide emission lines sensitive to gas densities (e.g., [OII] \u03bb\u03bb3729, 3726, [Cl III] \u03bb\u03bb5518, 5535, [ArIV] \u03bb\u03bb4740,4711), temperature ([OIII] \u03bb\u03bb4363, 4958, 5007; [NeIII] \u03bb\u03bb3343, 3968, 3869) and enable direct abundance measurements. These will be fundamental to study the mixing time scales across different galactic environments. The blue range will also cover the [NeV] \u03bb\u03bb3426 line, used as AGN diagnostic. The increased spectral resolution will enable a better derivation of the kinematics of the ionised gas and stellar components, important to understand the 3D structure of disk galaxies.<\/li>\n<li>The spatial information provided by an IFS is essential for <strong>disentangling individual spectra in dense stellar environments<\/strong>, such as globular clusters (GCs). MUSE allowed for the retrieval of tens of thousands of spectra per cluster, enabling detailed studies of their chemical compositions and dynamics. Access to the blue-visible and near-UV wavelength regions with BlueMUSE will uncover critical spectral features that are highly sensitive to subtle abundance differences among distinct stellar populations within GCs. Moreover, the increased spectral resolution will offer enhanced precision in measuring radial velocities, facilitating the detection of binary systems and probing stellar dynamics in the vicinity of intermediate-mass black holes.<\/li>\n<li>Due to their faintness, <strong>Ultra Faint <\/strong><strong>Dwarf<\/strong> galaxies (UFDs) are only found as satellites of the dominant galaxies in the Local Group, but their <strong>nature offers unique laboratories to study the properties of dark matter.<\/strong> As the amount of baryons in these galaxies is rather small, one expects their star formation histories to be simple and lacking strong stellar feedback episodes. A consequence is that the dark matter (density) profiles are expected to be closely related to those of dark-matter-only simulations, making UFDs systems where the difference between intrinsic properties of dark matter can be studied, as well as targets to potentially determine the nature of dark matter (e.g., is it \u201ccold\u201d, \u201cwarm\u201d or \u201cfuzzy\u201d) and whether it is collision-less or self-interacting.<\/li>\n<\/ul>\n<p><img loading=\"lazy\" decoding=\"async\" class=\"wp-image-711 aligncenter\" src=\"https:\/\/bluemuse.univ-lyon1.fr\/wp-content\/myimages\/2025\/06\/SWG1_Fig3-300x100.png\" alt=\"\" width=\"681\" height=\"227\" srcset=\"https:\/\/bluemuse.univ-lyon1.fr\/wp-content\/myimages\/2025\/06\/SWG1_Fig3-300x100.png 300w, https:\/\/bluemuse.univ-lyon1.fr\/wp-content\/myimages\/2025\/06\/SWG1_Fig3-1024x342.png 1024w, https:\/\/bluemuse.univ-lyon1.fr\/wp-content\/myimages\/2025\/06\/SWG1_Fig3-768x257.png 768w, https:\/\/bluemuse.univ-lyon1.fr\/wp-content\/myimages\/2025\/06\/SWG1_Fig3-1536x513.png 1536w, https:\/\/bluemuse.univ-lyon1.fr\/wp-content\/myimages\/2025\/06\/SWG1_Fig3.png 2048w\" sizes=\"auto, (max-width: 681px) 100vw, 681px\" \/><\/p>\n<div>\n<p class=\"ObjectCaption\"><em><span lang=\"EN-US\">Figure 2. A typical coma spectrum of comet 9P\/Tempel 1 (<a href=\"https:\/\/ui.adsabs.harvard.edu\/abs\/2011ApJ...734L...1M\/abstract\">Meech et al. 2011<\/a><\/span><span lang=\"EN-US\">). The BlueMUSE coverage (blue-shaded region) covers multiple radicals like CN, C2, and C3 and group transitions.<\/span><\/em><\/p>\n<\/div>\n<ul>\n<li>Large field of view IFS have proven extremely useful to detect faint activity levels in <strong>comets<\/strong>, helping us understand how their activity evolves with varying distances from the Sun. A number of radicals are observable in the blue part of the optical range (e.g., CN and C3). BlueMUSE will provide an in-depth insight into the production mechanisms of species in the coma of comets, as well as their activity. BlueMUSE will also offer <strong>unique opportunities for the observation of interstellar objects, which formed in other planetary systems and crossing pass through our own solar system.<\/strong><\/li>\n<\/ul>\n","protected":false},"excerpt":{"rendered":"<p>Key Science Case: Massive Stars Additional science cases: BlueMUSE will provide systematic maps of stellar properties and chemical compositions for very massive clusters in the Milky Way and local group galaxies, such as NGC 2070 in the Large Magellanic Cloud. Its unique wavelength coverage in the blue range (4000 &#8211; 5000 \u00c5) is essential for&hellip;&nbsp;<a href=\"https:\/\/bluemuse.univ-lyon1.fr\/index.php\/swg1-the-local-volume\/\" rel=\"bookmark\">Read More &raquo;<span class=\"screen-reader-text\">SWG1: The Local Volume<\/span><\/a><\/p>\n","protected":false},"author":8,"featured_media":0,"parent":0,"menu_order":0,"comment_status":"closed","ping_status":"closed","template":"","meta":{"neve_meta_sidebar":"","neve_meta_container":"","neve_meta_enable_content_width":"","neve_meta_content_width":0,"neve_meta_title_alignment":"","neve_meta_author_avatar":"","neve_post_elements_order":"","neve_meta_disable_header":"","neve_meta_disable_footer":"","neve_meta_disable_title":"","footnotes":""},"class_list":["post-704","page","type-page","status-publish","hentry"],"_links":{"self":[{"href":"https:\/\/bluemuse.univ-lyon1.fr\/index.php\/wp-json\/wp\/v2\/pages\/704","targetHints":{"allow":["GET"]}}],"collection":[{"href":"https:\/\/bluemuse.univ-lyon1.fr\/index.php\/wp-json\/wp\/v2\/pages"}],"about":[{"href":"https:\/\/bluemuse.univ-lyon1.fr\/index.php\/wp-json\/wp\/v2\/types\/page"}],"author":[{"embeddable":true,"href":"https:\/\/bluemuse.univ-lyon1.fr\/index.php\/wp-json\/wp\/v2\/users\/8"}],"replies":[{"embeddable":true,"href":"https:\/\/bluemuse.univ-lyon1.fr\/index.php\/wp-json\/wp\/v2\/comments?post=704"}],"version-history":[{"count":15,"href":"https:\/\/bluemuse.univ-lyon1.fr\/index.php\/wp-json\/wp\/v2\/pages\/704\/revisions"}],"predecessor-version":[{"id":796,"href":"https:\/\/bluemuse.univ-lyon1.fr\/index.php\/wp-json\/wp\/v2\/pages\/704\/revisions\/796"}],"wp:attachment":[{"href":"https:\/\/bluemuse.univ-lyon1.fr\/index.php\/wp-json\/wp\/v2\/media?parent=704"}],"curies":[{"name":"wp","href":"https:\/\/api.w.org\/{rel}","templated":true}]}}