{"status":"ok","message-type":"work","message-version":"1.0.0","message":{"indexed":{"date-parts":[[2026,2,3]],"date-time":"2026-02-03T16:17:48Z","timestamp":1770135468213,"version":"3.49.0"},"reference-count":91,"publisher":"American Astronomical Society","issue":"2","license":[{"start":{"date-parts":[[2017,12,21]],"date-time":"2017-12-21T00:00:00Z","timestamp":1513814400000},"content-version":"vor","delay-in-days":1,"URL":"https:\/\/iopscience.iop.org\/page\/copyright"},{"start":{"date-parts":[[2017,12,21]],"date-time":"2017-12-21T00:00:00Z","timestamp":1513814400000},"content-version":"tdm","delay-in-days":1,"URL":"https:\/\/iopscience.iop.org\/info\/page\/text-and-data-mining"}],"content-domain":{"domain":["iopscience.iop.org"],"crossmark-restriction":false},"short-container-title":["ApJ"],"published-print":{"date-parts":[[2017,12,20]]},"abstract":"<jats:title>Abstract<\/jats:title>\n               <jats:p>We present spectroscopic follow-up observations of CR7 with ALMA, targeted at constraining the infrared (IR) continuum and [C <jats:sc>ii<\/jats:sc>]<jats:inline-formula>\n                     <jats:tex-math>\n\n<\/jats:tex-math>\n                     <jats:inline-graphic xmlns:xlink=\"http:\/\/www.w3.org\/1999\/xlink\" xlink:href=\"apjaa9931ieqn1.gif\" xlink:type=\"simple\"\/>\n                  <\/jats:inline-formula> line-emission at high spatial resolution matched to the <jats:italic>HST<\/jats:italic>\/WFC3 imaging. CR7 is a luminous Ly<jats:italic>\u03b1<\/jats:italic> emitting galaxy at <jats:italic>z<\/jats:italic>\u00a0=\u00a06.6 that consists of three separated UV-continuum components. Our observations reveal several well-separated components of [C <jats:sc>ii<\/jats:sc>] emission. The two most luminous components in [C <jats:sc>ii<\/jats:sc>] coincide with the brightest UV components (A and B), blueshifted by <jats:inline-formula>\n                     <jats:tex-math>\n\n<\/jats:tex-math>\n                     <jats:inline-graphic xmlns:xlink=\"http:\/\/www.w3.org\/1999\/xlink\" xlink:href=\"apjaa9931ieqn2.gif\" xlink:type=\"simple\"\/>\n                  <\/jats:inline-formula> km s<jats:sup>\u22121<\/jats:sup> with respect to the peak of Ly<jats:italic>\u03b1<\/jats:italic> emission. Other [C <jats:sc>ii<\/jats:sc>] components are observed close to UV clumps B and C and are blueshifted by <jats:inline-formula>\n                     <jats:tex-math>\n\n<\/jats:tex-math>\n                     <jats:inline-graphic xmlns:xlink=\"http:\/\/www.w3.org\/1999\/xlink\" xlink:href=\"apjaa9931ieqn3.gif\" xlink:type=\"simple\"\/>\n                  <\/jats:inline-formula> and \u224880 km s<jats:sup>\u22121<\/jats:sup> with respect to the systemic redshift. We do not detect FIR continuum emission due to dust with a 3<jats:italic>\u03c3<\/jats:italic> limiting luminosity <jats:inline-formula>\n                     <jats:tex-math>\n\n<\/jats:tex-math>\n                     <jats:inline-graphic xmlns:xlink=\"http:\/\/www.w3.org\/1999\/xlink\" xlink:href=\"apjaa9931ieqn4.gif\" xlink:type=\"simple\"\/>\n                  <\/jats:inline-formula>. This allows us to mitigate uncertainties in the dust-corrected SFR and derive SFRs for the three UV clumps A, B, and C of 28, 5, and 7 <jats:inline-formula>\n                     <jats:tex-math>\n\n<\/jats:tex-math>\n                     <jats:inline-graphic xmlns:xlink=\"http:\/\/www.w3.org\/1999\/xlink\" xlink:href=\"apjaa9931ieqn5.gif\" xlink:type=\"simple\"\/>\n                  <\/jats:inline-formula> yr<jats:sup>\u22121<\/jats:sup>. All clumps have [C <jats:sc>ii<\/jats:sc>] luminosities consistent within the scatter observed in the local relation between SFR and <jats:inline-formula>\n                     <jats:tex-math>\n\n<\/jats:tex-math>\n                     <jats:inline-graphic xmlns:xlink=\"http:\/\/www.w3.org\/1999\/xlink\" xlink:href=\"apjaa9931ieqn6.gif\" xlink:type=\"simple\"\/>\n                  <\/jats:inline-formula>, implying that strong Ly<jats:italic>\u03b1<\/jats:italic> emission does not necessarily anti-correlate with [C <jats:sc>ii<\/jats:sc>] luminosity. Combining our measurements with the literature, we show that galaxies with blue UV slopes have weaker [C <jats:sc>ii<\/jats:sc>] emission at fixed SFR, potentially due to their lower metallicities and\/or higher photoionization. Comparison with hydrodynamical simulations suggests that CR7's clumps have metallicities of <jats:inline-formula>\n                     <jats:tex-math>\n\n<\/jats:tex-math>\n                     <jats:inline-graphic xmlns:xlink=\"http:\/\/www.w3.org\/1999\/xlink\" xlink:href=\"apjaa9931ieqn7.gif\" xlink:type=\"simple\"\/>\n                  <\/jats:inline-formula>. The observed ISM structure of CR7 indicates that we are likely witnessing the build up of a central galaxy in the early universe through complex accretion of satellites.<\/jats:p>","DOI":"10.3847\/1538-4357\/aa9931","type":"journal-article","created":{"date-parts":[[2017,12,21]],"date-time":"2017-12-21T16:22:45Z","timestamp":1513873365000},"page":"145","update-policy":"https:\/\/doi.org\/10.1088\/crossmark-policy","source":"Crossref","is-referenced-by-count":89,"title":["ALMA Reveals Metals yet No Dust within Multiple Components in 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