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<ri:Resource created="2017-01-05T08:45:46Z" status="active" updated="2025-06-13T15:25:00Z" 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>Abundances of late-type stars</title><shortName>J/ApJ/797/69</shortName><identifier>ivo://CDS.VizieR/J/ApJ/797/69</identifier><altIdentifier>doi:10.26093/cds/vizier.17970069</altIdentifier><curation><publisher ivo-id="ivo://CDS">CDS</publisher><creator><name>Roederer I.U.</name></creator><creator><name>Jacobson H.R.</name></creator><creator><name>Thanathibodee T.</name></creator><creator><name>Frebel A.</name></creator><creator><name>Toller E.</name></creator><date role="Updated">2017-11-29T11:48:53Z</date><date role="Created">2017-01-05T08:45:46Z</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>chemical-abundances</subject><subject>metallicity</subject><subject>line-intensities</subject><description>We report the detection of several absorption lines of neutral phosphorus (P, Z=15) in archival near-ultraviolet spectra obtained with the Space Telescope Imaging Spectrograph on board the Hubble Space Telescope. We derive phosphorus abundances or interesting upper limits in 14 late-type stars with metallicities spanning -3.8&lt;[Fe/H]&lt;-0.1. Previously, phosphorus had only been studied in Galactic stars with -1.0&lt;[Fe/H]&lt;+0.3. Iron lines reveal abundance offsets between the optical and ultraviolet regions, and we discuss and apply a correction factor to account for this offset. In stars with [Fe/H]&gt;-1.0, the [P/Fe] ratio decreases toward the solar value with increasing metallicity, in agreement with previous observational studies. In stars with [Fe/H]&lt;-1.0, $&lt;[P/Fe]$&gt;=+0.04+/-0.10, which overlaps with the [P/Fe] ratios found in several high-redshift damped Lyman-{alpha} systems. This behavior hints at a primary origin in massive stars.</description><source format="bibcode">2014ApJ...797...69R</source><referenceURL>https://cdsarc.cds.unistra.fr/viz-bin/cat/J/ApJ/797/69</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/A+A/275/101">J/A+A/275/101 : Chemical evolution of the gal. disk I. 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