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<ri:Resource created="2016-07-15T17:01:44Z" 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>Halo red giants reddening</title><shortName>J/AJ/107/1577</shortName><identifier>ivo://CDS.VizieR/J/AJ/107/1577</identifier><altIdentifier>doi:10.26093/cds/vizier.51071577</altIdentifier><curation><publisher ivo-id="ivo://CDS">CDS</publisher><creator><name>Anthony-Twarog B.J.</name></creator><creator><name>Twarog B.A.</name></creator><date role="Updated">2023-04-06T16:50:06Z</date><date role="Created">2016-07-15T17:01:44Z</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>visible-astronomy</subject><subject>medium-band-photometry</subject><subject>chemically-peculiar-stars</subject><description>Updated uvby observations for a larger sample of metal-deficient red giants are presented and combined with a select sample of data from the literature transformed to a common system. Using the reddening maps of Burstein &amp; Heiles [AJ, 87, 1165 (1982)], new absolute magnitudes, distances, metallicities, and reddenings are derived for each star. The metallicities are determined with a revised calibration of the m1, (b-y) diagram based upon comparison to a compilation of recent spectroscopic abundances transformed to a common system. The photometric abundances agree very well with the spectroscopic; the dispersion among the residuals for 58 giants is +/-0.16dex. The dereddened indices are used to show that for red giants with [Fe/H]&lt;-1.5, there is a well-defined relation in the c0, (b-y)0 diagram which exhibits only a weak dependence upon metallicity. Use of the standard relations allows one to obtain reddening estimates for normal halo field giants and globular clusters in the appropriate metallicity range.</description><source format="bibcode">1994AJ....107.1577A</source><referenceURL>https://cdsarc.cds.unistra.fr/viz-bin/cat/J/AJ/107/1577</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/J/AJ/109/2828">J/AJ/109/2828 : CaII H and K filter photometry II. 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Note flag (1)</description><ucd>meta.note</ucd><dataType xsi:type="vs:VOTableType">int</dataType><flag>nullable</flag></column><column><name>Vmag</name><description>[6.7/14.2] Visual magnitude</description><unit>mag</unit><ucd>phot.mag;em.opt.V</ucd><dataType xsi:type="vs:VOTableType">float</dataType></column><column><name>e_Vmag</name><description>Standard deviation in V (2)</description><unit>mag</unit><ucd>stat.error;phot.mag;em.opt.V</ucd><dataType xsi:type="vs:VOTableType">float</dataType></column><column><name>b-y</name><description>b-y color index on the Stromgren system</description><unit>mag</unit><ucd>phot.color;em.opt.B;em.opt.V</ucd><dataType xsi:type="vs:VOTableType">float</dataType></column><column><name>e_b-y</name><description>Standard deviation in b-y (2)</description><unit>mag</unit><ucd>stat.error;phot.color;em.opt.B</ucd><dataType xsi:type="vs:VOTableType">float</dataType></column><column><name>o_b-y</name><description>Number of observations for V and b-y (3)</description><ucd>meta.number</ucd><dataType xsi:type="vs:VOTableType">int</dataType></column><column><name>m1</name><description>m_1_ index</description><unit>mag</unit><ucd>phot.color</ucd><dataType xsi:type="vs:VOTableType">float</dataType></column><column><name>e_m1</name><description>Standard deviation in m1 (2)</description><unit>mag</unit><ucd>stat.error</ucd><dataType xsi:type="vs:VOTableType">float</dataType></column><column><name>c1</name><description>c_1_ index</description><unit>mag</unit><ucd>phot.color</ucd><dataType xsi:type="vs:VOTableType">float</dataType></column><column><name>e_c1</name><description>Standard deviation in c1 (2)</description><unit>mag</unit><ucd>stat.error</ucd><dataType xsi:type="vs:VOTableType">float</dataType></column><column><name>o_c1</name><description>Number of observations for m1 and c1 (3)</description><ucd>meta.number</ucd><dataType xsi:type="vs:VOTableType">int</dataType></column><column><name>n_E(b-y)</name><description>[ *] Note for derived reddening (4)</description><ucd>meta.note</ucd><dataType xsi:type="vs:VOTableType" arraysize="1*">char</dataType></column><column><name>E(b-y)</name><description>? 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