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<ri:Resource created="2022-12-16T13:51:47Z" 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>VLBA obs. of masers in the Scutum Spiral Arm</title><shortName>J/ApJS/262/42</shortName><identifier>ivo://CDS.VizieR/J/ApJS/262/42</identifier><altIdentifier>doi:10.26093/cds/vizier.22620042</altIdentifier><curation><publisher ivo-id="ivo://CDS">CDS</publisher><creator><name>Li J.J.</name></creator><creator><name>Immer K.</name></creator><creator><name>Reid M.J.</name></creator><creator><name>Sanna A.</name></creator><creator><name>Rygl K.L.J.</name></creator><creator><name>Xu Y.</name></creator><creator><name>Zhang B.,Brunthaler A.</name></creator><creator><name>Menten K.M.</name></creator><date role="Updated">2023-01-16T09:03:39Z</date><date role="Created">2022-12-16T13:51:47Z</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>star-forming-regions</subject><subject>astrophysical-masers</subject><subject>radio-astronomy</subject><subject>milky-way-galaxy</subject><subject>visible-astronomy</subject><subject>trigonometric-parallax</subject><subject>proper-motions</subject><subject>radio-sources</subject><description>As part of the Bar and Spiral Structure Legacy (BeSSeL) Survey, we have used the Very Long Baseline Array (VLBA) to measure 16 trigonometric parallaxes and proper motions of molecular masers associated with 14 high-mass star-forming regions in the Scutum arm in the first quadrant of the Milky Way. This increases the number of maser sources with accurate distances in this arm to 42. The Scutum arm can now be traced over a length of ~8kpc and spanning ~100{deg} of Galactic azimuth. We find that the large inward peculiar motions noted by Immer+ (2019A&amp;A...632A.123I) are concentrated near the end of the Galactic bar, while away from the bar modest peculiar motions more typical of spiral arms are seen, strengthening the suggestion that the large motions are induced by the bar.</description><source format="bibcode">2022ApJS..262...42L</source><referenceURL>https://cdsarc.cds.unistra.fr/viz-bin/cat/J/ApJS/262/42</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/126/2562">J/AJ/126/2562 : Second VLBA calibrator survey: VCS2 (Fomalont+, 2003)</relatedResource><relatedResource ivo-id="ivo://CDS.VizieR/J/AJ/129/1163">J/AJ/129/1163 : Third VLBA calibrator survey: VCS3 (Petrov+, 2005)</relatedResource><relatedResource ivo-id="ivo://CDS.VizieR/J/ApJS/166/526">J/ApJS/166/526 : Compact extragalactic radio sources (Xu+, 2006)</relatedResource><relatedResource ivo-id="ivo://CDS.VizieR/J/ApJS/194/25">J/ApJS/194/25 : VLBA calibrator search for the BeSSeL survey (Immer+, 2011)</relatedResource><relatedResource ivo-id="ivo://CDS.VizieR/J/ApJ/783/130">J/ApJ/783/130 : Parallaxes of high mass star forming regions (Reid+, 2014)</relatedResource><relatedResource ivo-id="ivo://CDS.VizieR/J/ApJ/885/131">J/ApJ/885/131 : ~200 high-mass SFR plx &amp; 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