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We have computed a grid of photoionization models with a substantial range in the slope of the ionizing power law (\u22121.5 &amp;lt; \u03b1 &amp;lt; \u22120.5), gas metallicity (0.01 &amp;lt; Z\/Z\u2299 &amp;lt; 3.0), gas density (1 &amp;lt; nH &amp;lt; 104 cm\u22123), and ionization parameter (10\u22125 &amp;lt; U &amp;lt; 1.0). We find the contribution from He\u2009ii \u03bb1215.1 to be negligible, i.e. &amp;lt;0.1 of Ly\u2009\u03b1 flux, across our entire model grid. The contribution from O\u2009v] \u03bb\u03bb1213.8,1218.3 is generally negligible when U is low (\u227210\u22123) and\/or when the gas metallicity is low (Z\/Z\u2299\u00a0\u2272\u00a00.1). However, at higher values of U and Z we find that O\u2009v] can significantly contaminate Ly\u2009\u03b1, in some circumstances accounting for more than half the total flux of the Ly\u2009\u03b1\u00a0+\u00a0He\u2009ii\u00a0+\u00a0O\u2009v] blend. We also provide means to estimate the fluxes of O\u2009v] \u03bb\u03bb1213.8,1218.3 and He\u2009ii \u03bb1215.1 by extrapolating from other lines. We estimate the fluxes of O\u2009v] and He\u2009ii for a sample of 107 Type 2 active galaxies at z &amp;gt; 2, and find evidence for significant (\u226510\u00a0per\u2009cent) contamination of Ly\u2009\u03b1 fluxes in the majority of cases (84\u00a0per\u2009cent). We also discuss prospects for using O\u2009v] \u03bb\u03bb1213.8,1218.3 as a diagnostic for the presence of AGN activity in high-z Ly\u2009\u03b1 emitters, and caution that the presence of significant O\u2009v] emission could impact the apparent kinematics of Ly\u2009\u03b1, potentially mimicking the presence of high-velocity gas outflows.<\/jats:p>","DOI":"10.1093\/mnras\/stz687","type":"journal-article","created":{"date-parts":[[2019,4,2]],"date-time":"2019-04-02T19:31:59Z","timestamp":1554233519000},"page":"2102-2115","source":"Crossref","is-referenced-by-count":9,"title":["O\u2009v] \u03bb\u03bb1213.8,1218.3 emission from extended nebulae around quasars: contamination of Ly\u2009\u03b1 and a new diagnostic for AGN activity in Ly\u2009\u03b1 emitters"],"prefix":"10.1093","volume":"486","author":[{"given":"A","family":"Humphrey","sequence":"first","affiliation":[{"name":"Instituto de Astrof\u00edsica e Ci\u00eancias do Espa\u00e7o, Universidade do Porto, CAUP, Rua das Estrelas, PT P-4150-762 Porto, Portugal"}]}],"member":"286","published-online":{"date-parts":[[2019,4,3]]},"reference":[{"key":"2020040220051918900_bib1","doi-asserted-by":"publisher","first-page":"3306","DOI":"10.1093\/mnras\/stt1500","volume":"435","author":"Alexandroff","year":"2013","journal-title":"MNRAS"},{"key":"2020040220051918900_bib2","doi-asserted-by":"publisher","first-page":"473","DOI":"10.1146\/annurev.aa.31.090193.002353","volume":"31","author":"Antonucci","year":"1993","journal-title":"ARA&A"},{"key":"2020040220051918900_bib3","doi-asserted-by":"crossref","first-page":"3162","DOI":"10.1093\/mnras\/sty2827","volume":"482","author":"Arrigoni\u00a0Battaia","year":"2019","journal-title":"MNRAS"},{"key":"2020040220051918900_bib4","doi-asserted-by":"publisher","first-page":"1","DOI":"10.1016\/j.nuclphysa.2005.06.010","volume":"777","author":"Asplund","year":"2006","journal-title":"Nucl. 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