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<ri:Resource created="2026-01-09T16:24:32Z" status="active" updated="2026-07-02T11:45:31Z" 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 Baryonic Tully-Fisher Relation. II.</title><shortName>J/AJ/169/186</shortName><identifier>ivo://CDS.VizieR/J/AJ/169/186</identifier><altIdentifier>doi:10.26093/cds/vizier/be-59-5t</altIdentifier><curation><publisher ivo-id="ivo://CDS">CDS</publisher><creator><name>Duey F.</name></creator><creator><name>Schombert J.</name></creator><creator><name>McGaugh S.</name></creator><creator><name>Lelli F.</name></creator><date role="Updated">2026-07-02T11:45:31Z</date><date role="Created">2026-01-09T16:24:32Z</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>galaxies</subject><subject>infrared-photometry</subject><subject>visible-astronomy</subject><description>We present new color-U* (mass-to-light ratio) models to convert Wide-field Infrared Survey Explorer W1 fluxes into stellar masses. We outline a range of possible star formation histories and chemical evolution scenarios to explore the confidence limits of stellar population models on the value of U*. We conclude that the greatest uncertainties (around 0.1dex in U*) occur for the bluest galaxies with the strongest variation in recent star formation. For high-mass galaxies, the greatest uncertainty arises from the proper treatment of bulge-disk separation in which to apply different U* relations appropriate for those differing underlying stellar populations. We compare our deduced stellar masses with those deduced from Spitzer Space Telescope 3.6{mu}m fluxes and stellar mass estimates in the literature using optical photometry and different U* modeling. We find the correspondence to be excellent, arguing that rest-frame near-IR photometry is still more advantageous than other wavelengths.</description><source format="bibcode">2025AJ....169..186D</source><referenceURL>https://cdsarc.cds.unistra.fr/viz-bin/cat/J/AJ/169/186</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/II/311">II/311 : WISE All-Sky Data Release (Cutri+ 2012)</relatedResource><relatedResource ivo-id="ivo://CDS.VizieR/II/328">II/328 : AllWISE Data Release (Cutri+ 2013)</relatedResource><relatedResource ivo-id="ivo://CDS.VizieR/V/139">V/139 : The SDSS Photometric Cat., Release 9 (Adelman-McCarthy+, 2012)</relatedResource><relatedResource ivo-id="ivo://CDS.VizieR/V/147">V/147 : The SDSS Photometric Catalogue, Release 12 (Alam+, 2015)</relatedResource><relatedResource ivo-id="ivo://CDS.VizieR/J/ApJS/116/1">J/ApJS/116/1 : Old Stellar Populations. 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