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<ri:Resource created="2021-12-15T12:51:49Z" 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>Archival Keck HIRES spectra analyzed with The Cannon</title><shortName>J/ApJ/898/119</shortName><identifier>ivo://CDS.VizieR/J/ApJ/898/119</identifier><altIdentifier>doi:10.26093/cds/vizier.18980119</altIdentifier><curation><publisher ivo-id="ivo://CDS">CDS</publisher><creator><name>Rice M.</name></creator><creator><name>Brewer J.M.</name></creator><date role="Updated">2023-03-06T08:11:56Z</date><date role="Created">2021-12-15T12:51:49Z</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>spectroscopy</subject><subject>astronomical-models</subject><subject>chemical-abundances</subject><subject>effective-temperature</subject><description>To accurately interpret the observed properties of exoplanets, it is necessary to first obtain a detailed understanding of host star properties. However, physical models that analyze stellar properties on a per-star basis can become computationally intractable for sufficiently large samples. Furthermore, these models are limited by the wavelength coverage of available spectra. We combine previously derived spectral properties from the Spectroscopic Properties of Cool Stars (SPOCS) catalog with generative modeling using The Cannon to produce a model capable of deriving stellar parameters (logg, Teff, and vsini) and 15 elemental abundances (C, N, O, Na, Mg, Al, Si, Ca, Ti, V, Cr, Mn, Fe, Ni, and Y) for stellar spectra observed with Keck Observatory's High Resolution Echelle Spectrometer (HIRES). We demonstrate the high accuracy and precision of our model, which takes just ~3s to classify each star, through cross-validation with pre-labeled spectra from the SPOCS sample. Our trained model, which takes continuum-normalized template spectra as its inputs, is publicly available at http://github.com/malenarice/keckspec. Finally, we interpolate our spectra and employ the same modeling scheme to recover labels for 477 stars using archival stellar spectra obtained prior to Keck's 2004 detector upgrade, demonstrating that our interpolated model can successfully predict stellar labels for different spectrographs that have (1) sufficiently similar systematics and (2) a wavelength range that substantially overlaps with that of the post-2004 HIRES spectra.</description><source format="bibcode">2020ApJ...898..119R</source><referenceURL>https://cdsarc.cds.unistra.fr/viz-bin/cat/J/ApJ/898/119</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/ApJ/622/1102">J/ApJ/622/1102 : The planet-metallicity correlation. (Fischer+, 2005)</relatedResource><relatedResource ivo-id="ivo://CDS.VizieR/J/ApJS/159/141">J/ApJS/159/141 : Spectroscopic properties of cool stars. I. (Valenti+, 2005)</relatedResource><relatedResource ivo-id="ivo://CDS.VizieR/J/A+A/497/497">J/A+A/497/497 : Physical parameters from JHK flux (Gonzalez-Hernandez+, 2009)</relatedResource><relatedResource ivo-id="ivo://CDS.VizieR/J/A+A/512/A54">J/A+A/512/A54 : Teff and Fbol from Infrared Flux Method (Casagrande+, 2010)</relatedResource><relatedResource ivo-id="ivo://CDS.VizieR/J/AJ/148/54">J/AJ/148/54 : The Hypatia Catalog ((Hinkel+, 2014)</relatedResource><relatedResource ivo-id="ivo://CDS.VizieR/J/ApJ/808/16">J/ApJ/808/16 : Cannon: a new approach to determine abundances (Ness+, 2015)</relatedResource><relatedResource ivo-id="ivo://CDS.VizieR/J/ApJS/225/32">J/ApJS/225/32 : Extended abundance analysis of cool stars (Brewer+, 2016)</relatedResource><relatedResource ivo-id="ivo://CDS.VizieR/J/ApJ/823/114">J/ApJ/823/114 : The Cannon: a new approach to determine masses (Ness+, 2016)</relatedResource><relatedResource ivo-id="ivo://CDS.VizieR/J/AJ/153/208">J/AJ/153/208 : LCES HIRES/Keck RVel Exoplanet Survey (Butler+, 2017)</relatedResource><relatedResource ivo-id="ivo://CDS.VizieR/J/ApJ/836/5">J/ApJ/836/5 : Abundances of LAMOST giants from APOGEE DR12 (Ho+, 2017)</relatedResource><relatedResource ivo-id="ivo://CDS.VizieR/J/ApJ/836/77">J/ApJ/836/77 : A library of high-S/N opt. spectra of FGKM stars (Yee+, 2017)</relatedResource><relatedResource ivo-id="ivo://CDS.VizieR/J/ApJS/237/38">J/ApJS/237/38 : Extended abundance analysis of KOIs (Brewer+, 2018)</relatedResource><relatedResource ivo-id="ivo://CDS.VizieR/J/MNRAS/478/4513">J/MNRAS/478/4513 : GALAH Survey DR2 (Buder+, 2018)</relatedResource><relatedResource ivo-id="ivo://CDS.VizieR/J/AJ/159/187">J/AJ/159/187 : RVs with the EXPRES spectrograph: 51Peg (Petersburg+, 2020)</relatedResource></relationship></content><rights>https://cds.unistra.fr/vizier-org/licences_vizier.html</rights><capability><interface xsi:type="vr:WebBrowser"><accessURL 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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>Teff</name><description>[4408/6797] Effective temperature</description><unit>K</unit><ucd>phys.temperature.effective</ucd><dataType xsi:type="vs:VOTableType">float</dataType></column><column><name>logg</name><description>[2.83/4.77] Log gravity</description><unit>log(cm.s**-2)</unit><ucd>phys.gravity</ucd><dataType xsi:type="vs:VOTableType">float</dataType></column><column><name>vsini</name><description>[-6.1/29.7] Line-of-sight velocity</description><unit>km/s</unit><ucd>phys.veloc</ucd><dataType xsi:type="vs:VOTableType">float</dataType></column><column><name>C/H</name><description>[-0.67/0.53] Abundance of C relative to H</description><ucd>phys.abund</ucd><dataType xsi:type="vs:VOTableType">float</dataType></column><column><name>N/H</name><description>[-1.08/0.58] Abundance of N relative to H</description><ucd>phys.abund</ucd><dataType xsi:type="vs:VOTableType">float</dataType></column><column><name>O/H</name><description>[-0.42/0.47] Abundance of O relative to H</description><ucd>phys.abund</ucd><dataType xsi:type="vs:VOTableType">float</dataType></column><column><name>Na/H</name><description>[-1.08/0.58] Abundance of Na relative to H</description><ucd>phys.abund</ucd><dataType xsi:type="vs:VOTableType">float</dataType></column><column><name>Mg/H</name><description>[-0.78/0.31] Abundance of Mg relative to H</description><ucd>phys.abund</ucd><dataType xsi:type="vs:VOTableType">float</dataType></column><column><name>Al/H</name><description>[-0.92/0.8] Abundance of Al relative to H</description><ucd>phys.abund</ucd><dataType xsi:type="vs:VOTableType">float</dataType></column><column><name>Si/H</name><description>[-0.76/0.39] Abundance of Si relative to H</description><ucd>phys.abund</ucd><dataType xsi:type="vs:VOTableType">float</dataType></column><column><name>Ca/H</name><description>[-0.84/0.41] Abundance of Ca relative to H</description><ucd>phys.abund</ucd><dataType xsi:type="vs:VOTableType">float</dataType></column><column><name>Ti/H</name><description>[-0.77/0.37] Abundance of Ti relative to H</description><ucd>phys.abund</ucd><dataType xsi:type="vs:VOTableType">float</dataType></column><column><name>V/H</name><description>[-0.85/0.32] Abundance of V relative to H</description><ucd>phys.abund</ucd><dataType xsi:type="vs:VOTableType">float</dataType></column><column><name>Cr/H</name><description>[-1.11/0.39] Abundance of Cr relative to H</description><ucd>phys.abund</ucd><dataType xsi:type="vs:VOTableType">float</dataType></column><column><name>Mn/H</name><description>[-1.41/0.54] Abundance of Mn relative to H</description><ucd>phys.abund</ucd><dataType xsi:type="vs:VOTableType">float</dataType></column><column><name>Fe/H</name><description>[-1.02/0.4] Abundance of Fe relative to H</description><ucd>phys.abund.Fe</ucd><dataType xsi:type="vs:VOTableType">float</dataType></column><column><name>Ni/H</name><description>[-1/0.45] Abundance of Ni relative to H</description><ucd>phys.abund</ucd><dataType xsi:type="vs:VOTableType">float</dataType></column><column><name>Y/H</name><description>[-0.9/0.67] Abundance of Y relative to H</description><ucd>phys.abund.Y</ucd><dataType xsi:type="vs:VOTableType">float</dataType></column><column><name>Flag</name><description>Reliability flag (1)</description><ucd>meta.code.error</ucd><dataType xsi:type="vs:VOTableType" arraysize="1*">char</dataType></column><column><name>SPOCS</name><description>Display data from SPOCS, Paper I (Valenti+, 2005, J/ApJS/159/141)</description><ucd>meta.ref.url</ucd><dataType xsi:type="vs:VOTableType">int</dataType><flag>nullable</flag></column><column><name>_RA</name><description>Right Ascension (J2000) from SIMBAD (not part of the original data)</description><unit>deg</unit><ucd>pos.eq.ra;meta.main</ucd></column><column><name>_DE</name><description>Declination (J2000) from SIMBAD (not part of the original data)</description><unit>deg</unit><ucd>pos.eq.dec;meta.main</ucd></column></table></schema></tableset></ri:Resource>