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<ri:Resource created="2008-11-27T21:57:06Z" status="active" updated="2025-05-19T09:50:00Z" version="1.2" xmlns:cs="http://www.ivoa.net/xml/ConeSearch/v1.0" xmlns:ri="http://www.ivoa.net/xml/RegistryInterface/v1.0" xmlns:vr="http://www.ivoa.net/xml/VOResource/v1.0" xmlns:vs="http://www.ivoa.net/xml/VODataService/v1.1" xmlns:xsi="http://www.w3.org/2001/XMLSchema-instance" xsi:schemaLocation="http://www.ivoa.net/xml/ConeSearch/v1.0 http://vo.ari.uni-heidelberg.de/docs/schemata/ConeSearch.xsd http://www.ivoa.net/xml/VOResource/v1.0 http://vo.ari.uni-heidelberg.de/docs/schemata/VOResource.xsd http://www.ivoa.net/xml/VODataService/v1.1 http://vo.ari.uni-heidelberg.de/docs/schemata/VODataService.xsd" xsi:type="vs:CatalogService"><title>Bulge field stars from FLAMES-GIRAFFE spectra</title><shortName>J/A+A/486/177</shortName><identifier>ivo://CDS.VizieR/J/A+A/486/177</identifier><altIdentifier>doi:10.26093/cds/vizier.34860177</altIdentifier><curation><publisher ivo-id="ivo://CDS">CDS</publisher><creator><name>Zoccali M.</name></creator><creator><name>Hill V.</name></creator><creator><name>Lecureur A.</name></creator><creator><name>Barbuy B.</name></creator><creator><name>Renzini A.</name></creator><creator><name>Minniti D.,Gomez A.</name></creator><creator><name>Ortolani S.</name></creator><date role="Updated">2019-12-03T10:07:39Z</date><date role="Created">2008-11-27T21:57:06Z</date><contact><name>CDS support team</name><address>CDS, Observatoire de Strasbourg, 11 rue de l'Universite, F-67000 Strasbourg, France</address><email>cds-question@unistra.fr</email></contact></curation><content><subject>giant-stars</subject><subject>k-stars</subject><subject>chemical-abundances</subject><description>We determine the iron distribution function (IDF) for bulge field stars, in three different fields along the Galactic minor axis and at latitudes b=-4{deg}, b=-6{deg}, and b=-12{deg}. A fourth field including NGC 6553 is also included in the discussion. About 800 bulge field K giants were observed with the GIRAFFE spectrograph of FLAMES@VLT at spectral resolution R~20000. Several of them were observed again with UVES at R~45000 to insure the accuracy of the measurements. The LTE abundance analysis yielded stellar parameters and iron abundances that allowed us to construct an IDF for the bulge that, for the first time, is based on high-resolution spectroscopy for each individual star.</description><source format="bibcode">2008A&amp;A...486..177Z</source><referenceURL>https://cdsarc.cds.unistra.fr/viz-bin/cat/J/A+A/486/177</referenceURL><type>Catalog</type><contentLevel>Research</contentLevel><relationship><relationshipType>IsServedBy</relationshipType><relatedResource ivo-id="ivo://CDS.VizieR/TAP">TAP VizieR generic service</relatedResource></relationship><relationship><relationshipType>IsServedBy</relationshipType><relatedResource>Conesearch service</relatedResource></relationship><relationship><relationshipType>related-to</relationshipType><relatedResource ivo-id="ivo://CDS.VizieR/II/213">II/213 : OGLE Galactic Bulge periodic variables (Udalski+ 1996)</relatedResource><relatedResource ivo-id="ivo://CDS.VizieR/I/244">I/244 : OGLE General Catalog of Stars. 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