{"status":"ok","message-type":"work","message-version":"1.0.0","message":{"indexed":{"date-parts":[[2022,3,31]],"date-time":"2022-03-31T19:54:40Z","timestamp":1648756480395},"reference-count":2,"publisher":"Cambridge University Press (CUP)","issue":"S262","license":[{"start":{"date-parts":[[2010,4,13]],"date-time":"2010-04-13T00:00:00Z","timestamp":1271116800000},"content-version":"unspecified","delay-in-days":255,"URL":"https:\/\/www.cambridge.org\/core\/terms"}],"content-domain":{"domain":[],"crossmark-restriction":false},"short-container-title":["Proc. IAU"],"published-print":{"date-parts":[[2009,8]]},"abstract":"<jats:title>Abstract<\/jats:title><jats:p>During the last three decades, many papers have reported the existence of a luminosity metallicity or mass metallicity (<jats:italic>M<\/jats:italic>\u2013<jats:italic>Z<\/jats:italic>) relation for all kinds of galaxies: The more massive galaxies are also the ones with more metal-rich interstellar medium. We have obtained the mass-metallicity relation at different lookback times for the same set of galaxies from the Sloan Digital Sky Survey (SDSS), using the stellar metallicities estimated with our spectral synthesis code <jats:sc>starlight<\/jats:sc>. Using stellar metallicities has several advantages: We are free of the biases that affect the calibration of nebular metallicities; we can include in our study objects for which the nebular metallicity cannot be measured, such as AGN hosts and passive galaxies; we can probe metallicities at different epochs of a galaxy evolution.<\/jats:p><jats:p>We have found that the <jats:italic>M<\/jats:italic>\u2013<jats:italic>Z<\/jats:italic> relation steepens and spans a wider range in both mass and metallicity at higher redshifts for SDSS galaxies. We also have modeled the time evolution of stellar metallicity with a closed-box chemical evolution model, for galaxies of different types and masses. Our results suggest that the <jats:italic>M<\/jats:italic>\u2013<jats:italic>Z<\/jats:italic> relation for galaxies with present-day stellar masses down to 10<jats:sup>10<\/jats:sup><jats:italic>M<\/jats:italic><jats:sub>\u2299<\/jats:sub> is mainly driven by the star formation history and not by inflows or outflows.<\/jats:p>","DOI":"10.1017\/s1743921310003625","type":"journal-article","created":{"date-parts":[[2010,4,13]],"date-time":"2010-04-13T08:50:38Z","timestamp":1271148638000},"page":"442-443","source":"Crossref","is-referenced-by-count":0,"title":["What stellar populations can tell us about the evolution of the mass\u2013metallicity relation in SDSS galaxies"],"prefix":"10.1017","volume":"5","author":[{"given":"N.","family":"Vale Asari","sequence":"first","affiliation":[]},{"given":"G.","family":"Stasi\u0144ska","sequence":"additional","affiliation":[]},{"given":"R.","family":"Cid Fernandes","sequence":"additional","affiliation":[]},{"given":"J. M.","family":"Gomes","sequence":"additional","affiliation":[]},{"given":"M.","family":"Schlickmann","sequence":"additional","affiliation":[]},{"given":"A.","family":"Mateus","sequence":"additional","affiliation":[]},{"given":"W.","family":"Schoenell","sequence":"additional","affiliation":[]}],"member":"56","published-online":{"date-parts":[[2010,4,13]]},"reference":[{"key":"S1743921310003625_ref1","doi-asserted-by":"publisher","DOI":"10.1111\/j.1365-2966.2005.08752.x"},{"key":"S1743921310003625_ref2","doi-asserted-by":"publisher","DOI":"10.1111\/j.1745-3933.2009.00664.x"}],"container-title":["Proceedings of the International Astronomical Union"],"original-title":[],"language":"en","link":[{"URL":"https:\/\/www.cambridge.org\/core\/services\/aop-cambridge-core\/content\/view\/S1743921310003625","content-type":"unspecified","content-version":"vor","intended-application":"similarity-checking"}],"deposited":{"date-parts":[[2019,4,30]],"date-time":"2019-04-30T12:22:42Z","timestamp":1556626962000},"score":1,"resource":{"primary":{"URL":"https:\/\/www.cambridge.org\/core\/product\/identifier\/S1743921310003625\/type\/journal_article"}},"subtitle":[],"short-title":[],"issued":{"date-parts":[[2009,8]]},"references-count":2,"journal-issue":{"issue":"S262","published-print":{"date-parts":[[2009,8]]}},"alternative-id":["S1743921310003625"],"URL":"https:\/\/doi.org\/10.1017\/s1743921310003625","relation":{},"ISSN":["1743-9213","1743-9221"],"issn-type":[{"value":"1743-9213","type":"print"},{"value":"1743-9221","type":"electronic"}],"subject":[],"published":{"date-parts":[[2009,8]]}}}