{"id":19370,"date":"2019-05-31T13:53:29","date_gmt":"2019-05-31T17:53:29","guid":{"rendered":"https:\/\/www.astrofisicamas.cl\/?p=19370"},"modified":"2019-05-31T13:53:29","modified_gmt":"2019-05-31T17:53:29","slug":"sdss-iv-manga-dependence-of-global-and-spatially-resolved-sfr-m-%e2%88%97-relations-on-galaxy-properties","status":"publish","type":"post","link":"https:\/\/astrofisicamas.cl\/en\/sdss-iv-manga-dependence-of-global-and-spatially-resolved-sfr-m-%e2%88%97-relations-on-galaxy-properties\/","title":{"rendered":"SDSS IV MaNGA: Dependence of Global and Spatially Resolved SFR-M \u2217 Relations on Galaxy Properties"},"content":{"rendered":"<p>[:en]<em><strong>Hsi-An Pan, Lihwai Lin, Bau-Ching Hsieh, Sebasti\u00e1n F. S\u00e1nchez et al., 2018, ApJ 854, 159<\/strong><\/em><!--more--><\/p>\n<p>The galaxy integrated H<i>\u03b1<\/i>\u00a0star formation rate\u2013stellar mass relation, or SFR(global)\u2013<i>M<\/i>\u00a0<sub>*<\/sub>(global) relation, is crucial for understanding star formation history and evolution of galaxies. However, many studies have dealt with SFR using unresolved measurements, which makes it difficult to separate out the contamination from other ionizing sources, such as active galactic nuclei and evolved stars. Using the integral field spectroscopic observations from SDSS-IV MaNGA, we spatially disentangle the contribution from different H<i>\u03b1<\/i>\u00a0powering sources for ~1000 galaxies. We find that, when including regions dominated by all ionizing sources in galaxies, the spatially resolved relation between H<i>\u03b1<\/i>\u00a0surface density (\u03a3<sub>H<i>\u03b1<\/i>\u00a0<\/sub>(all)) and stellar mass surface density (\u03a3<sub>*<\/sub>(all)) progressively turns over at the high \u03a3<sub>*<\/sub>(all) end for increasing\u00a0<i>M<\/i>\u00a0<sub>*<\/sub>(global) and\/or bulge dominance (bulge-to-total light ratio, B\/T). This in turn leads to the flattening of the integrated H<i>\u03b1<\/i>(global)\u2013<i>M<\/i>\u00a0<sub>*<\/sub>(global) relation in the literature. By contrast, there is no noticeable flattening in both integrated H<i>\u03b1<\/i>(H\u00a0<span class=\"small-caps\">ii<\/span>)\u2013<i>M<\/i>\u00a0<sub>*<\/sub>(H\u00a0<span class=\"small-caps\">ii<\/span>) and spatially resolved \u03a3<sub>H<i>\u03b1<\/i>\u00a0<\/sub>(H\u00a0<span class=\"small-caps\">ii<\/span>)\u2013\u03a3<sub>*<\/sub>(H\u00a0<span class=\"small-caps\">ii<\/span>) relations when only regions where star formation dominates the ionization are considered. In other words, the flattening can be attributed to the increasing regions powered by non-star-formation sources, which generally have lower ionizing ability than star formation. An analysis of the fractional contribution of non-star-formation sources to total H<i>\u03b1<\/i>\u00a0luminosity of a galaxy suggests a decreasing role of star formation as an ionizing source toward high-mass, high-B\/T galaxies and bulge regions. This result indicates that the appearance of the galaxy integrated SFR\u2013<i>M<\/i>\u00a0<sub>*<\/sub>\u00a0relation critically depends on their global properties (<i>M<\/i>\u00a0<sub>*<\/sub>(global) and B\/T) and relative abundances of various ionizing sources within the galaxies.<\/p>\n<p><a href=\"https:\/\/iopscience.iop.org\/article\/10.3847\/1538-4357\/aaa9bc\">Read paper<\/a>[:es]<em><strong>Hsi-An Pan, Lihwai Lin, Bau-Ching Hsieh, Sebasti\u00e1n F. S\u00e1nchez et al., 2018, ApJ 854, 159<\/strong><\/em><!--more--><\/p>\n<p>The galaxy integrated H<i>\u03b1<\/i>\u00a0star formation rate\u2013stellar mass relation, or SFR(global)\u2013<i>M<\/i>\u00a0<sub>*<\/sub>(global) relation, is crucial for understanding star formation history and evolution of galaxies. However, many studies have dealt with SFR using unresolved measurements, which makes it difficult to separate out the contamination from other ionizing sources, such as active galactic nuclei and evolved stars. Using the integral field spectroscopic observations from SDSS-IV MaNGA, we spatially disentangle the contribution from different H<i>\u03b1<\/i>\u00a0powering sources for ~1000 galaxies. We find that, when including regions dominated by all ionizing sources in galaxies, the spatially resolved relation between H<i>\u03b1<\/i>\u00a0surface density (\u03a3<sub>H<i>\u03b1<\/i>\u00a0<\/sub>(all)) and stellar mass surface density (\u03a3<sub>*<\/sub>(all)) progressively turns over at the high \u03a3<sub>*<\/sub>(all) end for increasing\u00a0<i>M<\/i>\u00a0<sub>*<\/sub>(global) and\/or bulge dominance (bulge-to-total light ratio, B\/T). This in turn leads to the flattening of the integrated H<i>\u03b1<\/i>(global)\u2013<i>M<\/i>\u00a0<sub>*<\/sub>(global) relation in the literature. By contrast, there is no noticeable flattening in both integrated H<i>\u03b1<\/i>(H\u00a0<span class=\"small-caps\">ii<\/span>)\u2013<i>M<\/i>\u00a0<sub>*<\/sub>(H\u00a0<span class=\"small-caps\">ii<\/span>) and spatially resolved \u03a3<sub>H<i>\u03b1<\/i>\u00a0<\/sub>(H\u00a0<span class=\"small-caps\">ii<\/span>)\u2013\u03a3<sub>*<\/sub>(H\u00a0<span class=\"small-caps\">ii<\/span>) relations when only regions where star formation dominates the ionization are considered. In other words, the flattening can be attributed to the increasing regions powered by non-star-formation sources, which generally have lower ionizing ability than star formation. An analysis of the fractional contribution of non-star-formation sources to total H<i>\u03b1<\/i>\u00a0luminosity of a galaxy suggests a decreasing role of star formation as an ionizing source toward high-mass, high-B\/T galaxies and bulge regions. This result indicates that the appearance of the galaxy integrated SFR\u2013<i>M<\/i>\u00a0<sub>*<\/sub>\u00a0relation critically depends on their global properties (<i>M<\/i>\u00a0<sub>*<\/sub>(global) and B\/T) and relative abundances of various ionizing sources within the galaxies.<\/p>\n<p><a href=\"https:\/\/iopscience.iop.org\/article\/10.3847\/1538-4357\/aaa9bc\">Ver publicaci\u00f3n<\/a>[:]<\/p>","protected":false},"excerpt":{"rendered":"<p>[:en]Hsi-An Pan, Lihwai Lin, Bau-Ching Hsieh, Sebasti\u00e1n F. S\u00e1nchez et al., 2018, ApJ 854, 159<\/p>","protected":false},"author":4,"featured_media":0,"comment_status":"open","ping_status":"open","sticky":false,"template":"","format":"standard","meta":{"_coblocks_attr":"","_coblocks_dimensions":"","_coblocks_responsive_height":"","_coblocks_accordion_ie_support":"","_eb_attr":"","footnotes":""},"categories":[1],"tags":[],"class_list":["post-19370","post","type-post","status-publish","format-standard","hentry","category-uncategorized"],"yoast_head":"<!-- This site is optimized with the Yoast SEO plugin v27.2 - https:\/\/yoast.com\/product\/yoast-seo-wordpress\/ -->\n<title>SDSS IV MaNGA: Dependence of Global and Spatially Resolved SFR-M \u2217 Relations on Galaxy Properties - Instituto Milenio de Astrof\u00edsica MAS<\/title>\n<meta name=\"robots\" content=\"index, follow, max-snippet:-1, max-image-preview:large, max-video-preview:-1\" \/>\n<link rel=\"canonical\" href=\"https:\/\/astrofisicamas.cl\/en\/sdss-iv-manga-dependence-of-global-and-spatially-resolved-sfr-m-\u2217-relations-on-galaxy-properties\/\" \/>\n<meta property=\"og:locale\" content=\"en_US\" \/>\n<meta property=\"og:type\" content=\"article\" \/>\n<meta property=\"og:title\" content=\"SDSS IV MaNGA: Dependence of Global and Spatially Resolved SFR-M \u2217 Relations on Galaxy Properties - Instituto Milenio de Astrof\u00edsica MAS\" \/>\n<meta property=\"og:description\" content=\"[:en]Hsi-An Pan, Lihwai Lin, Bau-Ching Hsieh, Sebasti\u00e1n F. S\u00e1nchez et al., 2018, ApJ 854, 159\" \/>\n<meta property=\"og:url\" content=\"https:\/\/astrofisicamas.cl\/en\/sdss-iv-manga-dependence-of-global-and-spatially-resolved-sfr-m-\u2217-relations-on-galaxy-properties\/\" \/>\n<meta property=\"og:site_name\" content=\"Instituto Milenio de Astrof\u00edsica MAS\" \/>\n<meta property=\"article:published_time\" content=\"2019-05-31T17:53:29+00:00\" \/>\n<meta name=\"author\" content=\"Catalina Limari\" \/>\n<meta name=\"twitter:card\" content=\"summary_large_image\" \/>\n<meta name=\"twitter:label1\" content=\"Written by\" \/>\n\t<meta name=\"twitter:data1\" content=\"Catalina Limari\" \/>\n\t<meta name=\"twitter:label2\" content=\"Est. reading time\" \/>\n\t<meta name=\"twitter:data2\" content=\"3 minutes\" \/>\n<script type=\"application\/ld+json\" class=\"yoast-schema-graph\">{\"@context\":\"https:\/\/schema.org\",\"@graph\":[{\"@type\":\"Article\",\"@id\":\"https:\/\/astrofisicamas.cl\/sdss-iv-manga-dependence-of-global-and-spatially-resolved-sfr-m-%e2%88%97-relations-on-galaxy-properties\/#article\",\"isPartOf\":{\"@id\":\"https:\/\/astrofisicamas.cl\/sdss-iv-manga-dependence-of-global-and-spatially-resolved-sfr-m-%e2%88%97-relations-on-galaxy-properties\/\"},\"author\":{\"name\":\"Catalina Limari\",\"@id\":\"https:\/\/astrofisicamas.cl\/#\/schema\/person\/4641a979ab58f0203310a447e1179de3\"},\"headline\":\"SDSS IV MaNGA: Dependence of Global and Spatially Resolved SFR-M \u2217 Relations on Galaxy Properties\",\"datePublished\":\"2019-05-31T17:53:29+00:00\",\"mainEntityOfPage\":{\"@id\":\"https:\/\/astrofisicamas.cl\/sdss-iv-manga-dependence-of-global-and-spatially-resolved-sfr-m-%e2%88%97-relations-on-galaxy-properties\/\"},\"wordCount\":603,\"commentCount\":0,\"publisher\":{\"@id\":\"https:\/\/astrofisicamas.cl\/#organization\"},\"inLanguage\":\"en-US\"},{\"@type\":\"WebPage\",\"@id\":\"https:\/\/astrofisicamas.cl\/sdss-iv-manga-dependence-of-global-and-spatially-resolved-sfr-m-%e2%88%97-relations-on-galaxy-properties\/\",\"url\":\"https:\/\/astrofisicamas.cl\/sdss-iv-manga-dependence-of-global-and-spatially-resolved-sfr-m-%e2%88%97-relations-on-galaxy-properties\/\",\"name\":\"SDSS IV MaNGA: Dependence of Global and Spatially Resolved SFR-M \u2217 Relations on Galaxy Properties - 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