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<ri:Resource created="2010-03-26T13:19:12Z" 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>Bubbles in the galactic disk. II.</title><shortName>J/ApJ/670/428</shortName><identifier>ivo://CDS.VizieR/J/ApJ/670/428</identifier><altIdentifier>doi:10.26093/cds/vizier.16700428</altIdentifier><curation><publisher ivo-id="ivo://CDS">CDS</publisher><creator><name>Churchwell E.</name></creator><creator><name>Watson D.F.</name></creator><creator><name>Povich M.S.</name></creator><creator><name>Taylor M.G.</name></creator><creator><name>Babler B.L.,Meade M.R.</name></creator><creator><name>Benjamin R.A.</name></creator><creator><name>Indebetouw R.</name></creator><creator><name>Whitney B.A.</name></creator><date role="Updated">2017-06-30T05:48:32Z</date><date role="Created">2010-03-26T13:19:12Z</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>galaxy-planes</subject><subject>milky-way-galaxy</subject><subject>h-ii-regions</subject><subject>galaxy-classification-systems</subject><description>We report 269 mid-infrared bubbles within 10{deg} of the Galactic center from visual inspection of the Spitzer GLIMPSE II Legacy Science program images. The surface density of bubbles is ~5deg^-2^ or about 3 times that detected in longitudes |l|=10{deg}-65{deg}, because the inner 10{deg} of longitude were more thoroughly searched for small bubbles. There is a gradient in the number of bubbles with longitude with an increase of about a factor of 2 from 2{deg} to 10{deg}; this is probably the result of several factors, including decreasing diffuse background brightness, confusion, and opacity with longitude. Bubble eccentricities are typically between 0.6 and 0.8, and &gt;50% show evidence for blowouts, which we suggest result from local density fluctuations of the ISM and/or anisotropic stellar winds and radiation fields.</description><source format="bibcode">2007ApJ...670..428C</source><referenceURL>https://cdsarc.cds.unistra.fr/viz-bin/cat/J/ApJ/670/428</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/649/759">J/ApJ/649/759 : The bubbling galactic disk. 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