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<ri:Resource created="2016-06-03T07:28:22Z" 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>ATLASGAL dense filamentary structures</title><shortName>J/A+A/591/A5</shortName><identifier>ivo://CDS.VizieR/J/A+A/591/A5</identifier><altIdentifier>doi:10.26093/cds/vizier.35910005</altIdentifier><curation><publisher ivo-id="ivo://CDS">CDS</publisher><creator><name>Li G.-X.</name></creator><creator><name>Urquhart J.S.</name></creator><creator><name>Leurini S.</name></creator><creator><name>Csengeri T.</name></creator><creator><name>Wyrowski F.,Menten K.M.</name></creator><creator><name>Schuller F.</name></creator><date role="Updated">2017-07-03T14:25:38Z</date><date role="Created">2016-06-03T07:28:22Z</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>surveys</subject><subject>interstellar-medium</subject><subject>galaxy-classification-systems</subject><description>We study the properties of filamentary structures from the ATLASGAL survey. We use the DisPerSE algorithm to identify spatially coherent structures located across the inner-Galaxy (300&lt;l&lt;60 and |b|&lt;1.5). We have determined distances, masses and physical sizes for 241 of the filamentary structures. We find a median distance of 3.8kpc, a mean mass of a few 10^3^M_{sun}_, a mean length of ~6pc and a mass-to-length ratio of (M/L)~200-2000M_sun/pc. We also find that these filamentary structures are tightly correlated with the spiral arms in longitude and velocity, and that their semi-major axis is preferentially aligned parallel to the Galactic mid-plane and therefore with the direction of large-scale Galactic magnetic field. We find many examples where the dense filaments identified in ATLASGAL are associated with larger scale filamentary structures (~100pc), and argue that this is likely to be common, and as such these may indicate a connection between large-scale Galactic dynamics and star formation. We have produced a large and Galaxy-wide catalogue of dense filamentary structures that are representative of a particular size and mass range not previously well studied in the literature. Analyses of the properties and distribution of these filaments reveals that they are correlated with the spiral arms and make a significant contribution to star formation in the Galaxy. Massive star formation is ongoing within ~20% of the filaments and is strongly correlated with the filaments with the largest mass-to- length ratios. The luminosity of the embedded sources has a similar distribution to the Galactic-wide samples of young massive stars and can therefore be considered to be representative.</description><source format="bibcode">2016A&amp;A...591A...5L</source><referenceURL>https://cdsarc.cds.unistra.fr/viz-bin/cat/J/A+A/591/A5</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/540/A113">J/A+A/540/A113 : Starless clumps in ATLASGAL (Tackenberg+, 2012)</relatedResource><relatedResource ivo-id="ivo://CDS.VizieR/J/A+A/544/A146">J/A+A/544/A146 : ATLASGAL cold high-mass clumps with NH_3_ (Wienen+, 2012)</relatedResource><relatedResource ivo-id="ivo://CDS.VizieR/J/A+A/549/A45">J/A+A/549/A45 : ATLASGAL Compact Source Catalog: 330&lt;l&lt;21 (Contreras+, 2013)</relatedResource><relatedResource ivo-id="ivo://CDS.VizieR/J/MNRAS/431/1752">J/MNRAS/431/1752 : ATLASGAL 6.7GHz methanol masers (Urquhart+, 2013)</relatedResource><relatedResource ivo-id="ivo://CDS.VizieR/J/MNRAS/435/400">J/MNRAS/435/400 : ATLASGAL Properties of compact HII regions (Urquhart+, 2013)</relatedResource><relatedResource ivo-id="ivo://CDS.VizieR/J/MNRAS/443/1555">J/MNRAS/443/1555 : ATLASGAL massive star forming clumps sample (Urquhart+ 2014)</relatedResource><relatedResource ivo-id="ivo://CDS.VizieR/J/A+A/565/A75">J/A+A/565/A75 : ATLASGAL Dust condensations in Galactic plane</relatedResource><relatedResource ivo-id="ivo://CDS.VizieR/J/A+A/568/A41">J/A+A/568/A41 : ATLASGAL Compact Source Catalog: 280&lt;l&lt;60 (Urquhart+, 2014)</relatedResource><relatedResource ivo-id="ivo://CDS.VizieR/J/A+A/570/A65">J/A+A/570/A65 : ATLASGAL massive clumps CO depletion (Giannetti+, 2014)</relatedResource><relatedResource ivo-id="ivo://CDS.VizieR/J/A+A/579/A91">J/A+A/579/A91 : ATLASGAL inner Galaxy massive cold dust clumps</relatedResource><relatedResource ivo-id="ivo://CDS.VizieR/J/A+A/581/A74">J/A+A/581/A74 : Molecular clouds as viewed by ATLASGAL (Abreu-Vicente+ 2015)</relatedResource><relatedResource ivo-id="ivo://CDS.VizieR/J/A+A/586/A149">J/A+A/586/A149 : SiO in ATLASGAL-selected massive clumps (Csengeri+, 2016)</relatedResource></relationship></content><rights>https://cds.unistra.fr/vizier-org/licences_vizier.html</rights><capability><interface xsi:type="vr:WebBrowser"><accessURL use="full">https://vizier.cds.unistra.fr/viz-bin/VizieR-2?-source=J/A+A/591/A5</accessURL><mirrorURL title="VizieR at IUCAA: Pune, India">https://vizier.iucaa.in/viz-bin/VizieR-2?-source=J/A+A/591/A5</mirrorURL><mirrorURL title="VizieR at SAAO: SAAO, South 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