{"status":"ok","message-type":"work","message-version":"1.0.0","message":{"indexed":{"date-parts":[[2026,5,9]],"date-time":"2026-05-09T21:53:47Z","timestamp":1778363627624,"version":"3.51.4"},"reference-count":57,"publisher":"American Astronomical Society","issue":"1","license":[{"start":{"date-parts":[[2021,3,25]],"date-time":"2021-03-25T00:00:00Z","timestamp":1616630400000},"content-version":"vor","delay-in-days":24,"URL":"https:\/\/iopscience.iop.org\/page\/copyright"},{"start":{"date-parts":[[2021,3,25]],"date-time":"2021-03-25T00:00:00Z","timestamp":1616630400000},"content-version":"tdm","delay-in-days":24,"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":[[2021,3,1]]},"abstract":"<jats:title>Abstract<\/jats:title>\n               <jats:p>We study the mass\u2013metallicity relation for 19 members of a spectroscopically confirmed protocluster in the COSMOS field at <jats:italic>z<\/jats:italic> = 2.2 (CC2.2), and compare it with that of 24 similarly selected field galaxies at the same redshift. Both samples are H<jats:italic>\u03b1<\/jats:italic> emitting sources, chosen from the HiZELS narrowband survey, with metallicities derived from the <jats:inline-formula>\n                     <jats:tex-math>\n\n<\/jats:tex-math>\n                     <mml:math xmlns:mml=\"http:\/\/www.w3.org\/1998\/Math\/MathML\" overflow=\"scroll\">\n                        <mml:mi mathvariant=\"normal\">N<\/mml:mi>\n                        <mml:mn>2<\/mml:mn>\n                        <mml:mspace width=\"0.33em\"\/>\n                        <mml:mfenced close=\")\" open=\"(\">\n                           <mml:mrow>\n                              <mml:mstyle displaystyle=\"false\">\n                                 <mml:mfrac>\n                                    <mml:mrow>\n                                       <mml:mo stretchy=\"false\">[<\/mml:mo>\n                                       <mml:mi>NII<\/mml:mi>\n                                       <mml:mo stretchy=\"false\">]<\/mml:mo>\n                                       <mml:mi>\u03bb<\/mml:mi>\n                                       <mml:mn>6584<\/mml:mn>\n                                    <\/mml:mrow>\n                                    <mml:mrow>\n                                       <mml:mi mathvariant=\"normal\">H<\/mml:mi>\n                                       <mml:mi>\u03b1<\/mml:mi>\n                                    <\/mml:mrow>\n                                 <\/mml:mfrac>\n                              <\/mml:mstyle>\n                           <\/mml:mrow>\n                        <\/mml:mfenced>\n                     <\/mml:math>\n                     <jats:inline-graphic xmlns:xlink=\"http:\/\/www.w3.org\/1999\/xlink\" xlink:href=\"apjabe5a3ieqn1.gif\" xlink:type=\"simple\"\/>\n                  <\/jats:inline-formula> line ratio. For the mass-matched samples of protocluster and field galaxies, we find that protocluster galaxies with 10<jats:sup>9.9<\/jats:sup>\n                  <jats:italic>M<\/jats:italic>\n                  <jats:sub>\u2299<\/jats:sub> \u2264 <jats:italic>M<\/jats:italic>\n                  <jats:sub>*<\/jats:sub> \u2264 10<jats:sup>10.9<\/jats:sup>\n                  <jats:italic>M<\/jats:italic>\n                  <jats:sub>\u2299<\/jats:sub> are metal deficient by 0.10 \u00b1 0.04 dex (2.5<jats:italic>\u03c3<\/jats:italic> significance) compared to their coeval field galaxies. This metal deficiency is absent for low-mass galaxies, <jats:italic>M<\/jats:italic>\n                  <jats:sub>*<\/jats:sub> &lt; 10<jats:sup>9.9<\/jats:sup>\n                  <jats:italic>M<\/jats:italic>\n                  <jats:sub>\u2299<\/jats:sub>. Moreover, relying on both spectral energy distribution derived and H<jats:italic>\u03b1<\/jats:italic> (corrected for dust extinction based on M<jats:sub>*<\/jats:sub>) star formation rates (SFRs), we find no strong environmental dependence of the SFR\u2013<jats:italic>M<\/jats:italic>\n                  <jats:sub>*<\/jats:sub> relation; however, we are not able to rule out the existence of small dependence due to inherent uncertainties in both SFR estimators. The existence of 2.5<jats:italic>\u03c3<\/jats:italic> significant metal deficiency for massive protocluster galaxies favors a model in which funneling of the primordial cold gas through filaments dilutes the metal content of protoclusters at high redshifts (<jats:italic>z<\/jats:italic> \u2273 2). At these redshifts, gas reservoirs in filaments are dense enough to cool down rapidly and fall into the potential well of the protocluster to lower the gas-phase metallicity of galaxies. Moreover, part of this metal deficiency could be originated from galaxy interactions that are more prevalent in dense environments.<\/jats:p>","DOI":"10.3847\/1538-4357\/abe5a3","type":"journal-article","created":{"date-parts":[[2021,3,25]],"date-time":"2021-03-25T12:49:51Z","timestamp":1616676591000},"page":"57","update-policy":"https:\/\/doi.org\/10.1088\/crossmark-policy","source":"Crossref","is-referenced-by-count":16,"title":["Evidence for Gas-phase Metal Deficiency in Massive Protocluster Galaxies at z 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