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<ri:Resource created="2025-03-05T09:19:54Z" status="active" updated="2025-05-21T20:12:45Z" 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>The Galactic bulge exploration. III. RRL FeH_CaT_</title><shortName>J/AJ/168/139</shortName><identifier>ivo://CDS.VizieR/J/AJ/168/139</identifier><altIdentifier>doi:10.26093/cds/vizier.51680139</altIdentifier><curation><publisher ivo-id="ivo://CDS">CDS</publisher><creator><name>Kunder A.</name></creator><creator><name>Prudil Z.</name></creator><creator><name>Skaggs C.</name></creator><creator><name>Reggiani H.</name></creator><creator><name>Nataf D.M.</name></creator><creator><name>Hughes J.,Covey K.R.</name></creator><creator><name>Devine K.</name></creator><date role="Updated">2025-05-21T20:12:45Z</date><date role="Created">2025-03-05T09:19:54Z</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>variable-stars</subject><subject>visible-astronomy</subject><subject>spectroscopy</subject><subject>infrared-astronomy</subject><subject>chemical-abundances</subject><subject>milky-way-galaxy</subject><subject>line-intensities</subject><description>RR Lyrae stars (RRLs) are excellent tracers of stellar populations for old, metal-poor components in the the Milky Way and the Local Group. Their luminosities have a metallicity dependence, but determining spectroscopic [Fe/H] metallicities for RRLs, especially at distances outside the solar neighborhood, is challenging. Using 40 RRLs with metallicities derived from both Fe(II) and Fe(I) abundances, we verify the calibration between the [Fe/H] of RRLs from the calcium triplet. Our calibration is applied to all RRLs with Gaia Radial Velocity Spectrometer (RVS) spectra in Gaia DR3 and to 80 stars in the inner Galaxy from the BRAVA-RR survey. The coadded Gaia RVS RRL spectra provide RRL metallicities with an uncertainty of 0.25 dex, which is a factor of two improvement over the Gaia photometric RRL metallicities. Within our Galactic bulge RRL sample, we find a dominant fraction with low energies without a prominent rotating component. Due to the large fraction of such stars, we interpret these stars as belonging to the in situ metal-poor Galactic bulge component, although we cannot rule out that a fraction of these belong to an ancient accretion event such as Kraken/Heracles.</description><source format="bibcode">2024AJ....168..139K</source><referenceURL>https://cdsarc.cds.unistra.fr/viz-bin/cat/J/AJ/168/139</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/III/283">III/283 : RAVE 6th data release (Steinmetz+, 2020)</relatedResource><relatedResource ivo-id="ivo://CDS.VizieR/I/355">I/355 : Gaia DR3 Part 1. 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