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II.</title><shortName>J/A+A/577/A81</shortName><identifier>ivo://CDS.VizieR/J/A+A/577/A81</identifier><altIdentifier>doi:10.26093/cds/vizier.35770081</altIdentifier><curation><publisher ivo-id="ivo://CDS">CDS</publisher><creator><name>Fernandez-Alvar E.</name></creator><creator><name>Allende Prieto C.</name></creator><creator><name>Schlesinger K.J.</name></creator><creator><name>Beers T.C.,Robin A.C.</name></creator><creator><name>Schneider D.P.</name></creator><creator><name>Lee Y.S.</name></creator><creator><name>Bizyaev D.</name></creator><creator><name>Ebelke G.,Malanushenko E.</name></creator><creator><name>Malanushenko V.</name></creator><creator><name>Oravetz D.</name></creator><creator><name>Pan K.</name></creator><creator><name>Simmons A.</name></creator><date role="Updated">2017-10-09T13:34:25Z</date><date role="Created">2015-05-07T08:17:21Z</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>halo-stars</subject><subject>stellar-distance</subject><subject>metallicity</subject><description>We analyze a sample of 3942 low-resolution (R~2000) optical spectra from the Sloan Digital Sky Survey (SDSS), focusing on stars with effective temperatures 5800&lt;Teff&lt;6300K, and distances from the Milky Way plane in excess of 5kpc, and determine their abundances of Fe, Ca, and Mg. This work follows the same methodology as in the previous paper in this series, deriving atmospheric parameters by chi^2^ minimization, but we now obtain the abundances of individual elements by fitting their associated spectral lines. Distances are calculated from absolute magnitudes obtained by a statistical comparison of our stellar parameters with stellar-evolution models. The observations reveal a decrease in the abundances of iron, calcium and magnesium at large distances from the Galactic center. The median abundances for the halo stars analyzed are fairly constant up to a Galactocentric distance r~20kpc, rapidly decrease between r~20 and r~40kpc, and flatten out to significantly lower values at larger distances, consistent with previous studies. In addition, we examine the Ca/Fe and Mg/Fe ratios as a function of Fe/H and Galactocentric distance. Our results show that the most distant parts of the halo show a steeper variation of the Ca/Fe and Mg/Fe with iron. We found that at the range -1.6&lt;[Fe/H]&lt;-0.4 the Ca/Fe ratio decreases with distance, in agreement with earlier results based on local stars. However, the opposite trend is apparent for Mg/Fe. Our conclusion that the outer regions of the halo are more metal-poor than the inner regions, based on in-situ observations of distant stars, is in concert with recent results based on inferences from the kinematics of more local stars, and with predictions of recent galaxy formation simulations for galaxies similar to the Milky Way.</description><source format="bibcode">2015A&amp;A...577A..81F</source><referenceURL>https://cdsarc.cds.unistra.fr/viz-bin/cat/J/A+A/577/A81</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/568/A7">J/A+A/568/A7 : Model SDSS colors for 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Should Not be used for identification.</description><ucd>meta.record</ucd><dataType xsi:type="vs:VOTableType">int</dataType></column><column><name>T</name><description>Simbad column added by the CDS</description><ucd>meta.id;meta.dataset</ucd><dataType xsi:type="vs:VOTableType" arraysize="1*">char</dataType></column><column><name>PMF</name><description>Plate-mjd-fiber identification</description><ucd>meta.id</ucd><dataType xsi:type="vs:VOTableType" arraysize="15*">char</dataType></column><column><name>Teff</name><description>[5800/6300] Effective temperature</description><unit>K</unit><ucd>phys.temperature.effective</ucd><dataType xsi:type="vs:VOTableType">int</dataType></column><column><name>e_Teff</name><description>[8/122] Effective temperature error</description><unit>K</unit><ucd>stat.error;phys.temperature.effective</ucd><dataType xsi:type="vs:VOTableType">int</dataType></column><column><name>logg</name><description>[2.5/4.4] log_10_ of the surface gravity</description><unit>log(cm.s**-2)</unit><ucd>phys.gravity</ucd><dataType xsi:type="vs:VOTableType">float</dataType></column><column><name>e_logg</name><description>[0.05/1] log_10_ of the surface gravity error</description><unit>log(cm.s**-2)</unit><ucd>stat.error</ucd><dataType xsi:type="vs:VOTableType">float</dataType></column><column><name>[Fe/H]</name><description>i[-3.7/0.5] Iron abundance</description><unit>log(Sun)</unit><ucd>phys.abund</ucd><dataType xsi:type="vs:VOTableType">float</dataType></column><column><name>e_[Fe/H]</name><description>[0.05/0.5] Iron abundance error</description><unit>log(Sun)</unit><ucd>stat.error;phys.abund.Fe</ucd><dataType xsi:type="vs:VOTableType">float</dataType></column><column><name>[Ca/H]</name><description>[-4.3/-0.2]? Calcium abundance</description><unit>log(Sun)</unit><ucd>phys.abund</ucd><dataType xsi:type="vs:VOTableType">float</dataType><flag>nullable</flag></column><column><name>e_[Ca/H]</name><description>[0.01/0.4]? Calcium abundance error</description><unit>log(Sun)</unit><ucd>stat.error;phys.abund</ucd><dataType xsi:type="vs:VOTableType">float</dataType><flag>nullable</flag></column><column><name>[Mg/H]</name><description>[-3.6/-0]? Magnesium abundance</description><unit>log(Sun)</unit><ucd>phys.abund</ucd><dataType xsi:type="vs:VOTableType">float</dataType><flag>nullable</flag></column><column><name>e_[Mg/H]</name><description>[0.04/0.5]? Magnesium abundance error</description><unit>log(Sun)</unit><ucd>stat.error;phys.abund</ucd><dataType xsi:type="vs:VOTableType">float</dataType><flag>nullable</flag></column><column><name>dsun</name><description>[5/127] Distance from the sun</description><unit>kpc</unit><ucd>pos.distance;pos.heliocentric</ucd><dataType xsi:type="vs:VOTableType">float</dataType></column><column><name>e_dsun</name><description>[0.2/1.5] Distance from the sun error</description><unit>kpc</unit><ucd>stat.error</ucd><dataType xsi:type="vs:VOTableType">float</dataType></column><column><name>r</name><description>[5.7/132] Distance from the Galaxy center</description><unit>kpc</unit><ucd>pos.distance;pos.galactocentric</ucd><dataType xsi:type="vs:VOTableType">float</dataType></column><column><name>Z</name><description>[-76./103] Distance from the galactic plane</description><unit>kpc</unit><ucd>pos.cartesian.z;pos.galactic</ucd><dataType xsi:type="vs:VOTableType">float</dataType></column><column><name>Sp</name><description>Interactive spectrum from SDSS</description><ucd>meta.ref.url</ucd><dataType xsi:type="vs:VOTableType" arraysize="*">char</dataType></column><column><name>_RA</name><description>Simbad column added by the CDS</description><unit>deg</unit><ucd>pos.eq.ra;meta.main</ucd><flag>nullable</flag></column><column><name>_DE</name><description>Simbad column added by the CDS</description><unit>deg</unit><ucd>pos.eq.dec;meta.main</ucd><flag>nullable</flag></column></table></schema></tableset></ri:Resource>