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<ri:Resource created="2026-02-18T08:01:33Z" status="active" updated="2026-03-02T06:25:50Z" 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>Molecular gas associated with HII regions</title><shortName>J/A+A/706/A280</shortName><identifier>ivo://CDS.VizieR/J/A+A/706/A280</identifier><curation><publisher ivo-id="ivo://CDS">CDS</publisher><creator><name>Khan S.</name></creator><creator><name>Jacob A.M.</name></creator><creator><name>Rugel M.R.</name></creator><creator><name>Urquhart J.S.</name></creator><creator><name>Neupane S.</name></creator><creator><name>Wyrowski F.,Brunthaler A.</name></creator><creator><name>Pandian J.D.</name></creator><creator><name>Gong Y.</name></creator><creator><name>Barlach Christensen I.</name></creator><creator><name>Menten K.M.</name></creator><date role="Updated">2026-03-02T06:25:50Z</date><date role="Created">2026-02-18T08:01:33Z</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>milky-way-galaxy</subject><subject>h-ii-regions</subject><subject>radio-continuum-emission</subject><subject>spectroscopy</subject><description>Massive stars strongly impact their natal environments and influence subsequent star formation through feedback mechanisms including shocks, outflows and radiation. HII regions are key laboratories for studying this impact. To understand such feedback, it is crucial to characterize the physical conditions of the dense molecular gas in which these regions are embedded. We aim to constrain the kinetic temperature and H_2_ volume density of massive star-forming clumps associated with HII regions using multiple p-H_2_CO transitions. The non-LTE analysis yielded kinetic temperatures (Tkin) ranging from 33.7K to 265K and H_2_ densities (n(H_2_)) between 0.8x10^4^ to 1.05x10^7^cm^-3^, providing a detailed characterization of the dense molecular gas contained in these clumps. We observed the JKaKc transitions of p-H_2_CO (within its J=3-2 and 4-3 states) with the Atacama Pathfinder EXperiment (APEX) 12m submillimeter telescope, using the nFLASH230 and SEPIA345 receivers toward a sample of 61 HII regions. We derived spectral line parameters via multicomponent Gaussian fitting, which was then used to constrain the physical conditions determined using PyRADEX, a non-local thermodynamic equilibrium (LTE) radiative transfer code in combination with Markov chain Monte Carlo analysis. The non-LTE analysis yielded kinetic temperatures (Tkin) ranging from 33.7K to 265K and H_2_ densities (n(H_2_)) between 0.8x10^4^ and 1.05x10^7^cm^-3^, providing a detailed characterization of the dense -olecular gas contained in these clumps. In addition to the p-H_2_CO emission arising from the targeted clump, a large fraction (57%) of the sources exhibited multiple p-H_2_CO components, with the secondary components being characterized by a higher Tkin and broader line widths. Investigation of the nature of the secondary component revealed its association with supersonic nonthermal motions and turbulent gas. When comparing the physical properties of the molecular gas and dust components with those of the ionized gas, we found that parameters directly linked to the central high-mass star, such as bolometric luminosity (Lbol) and Lyman continuum photon rate (NLyc), show stronger and more systematic correlations. These findings emphasize the role of the central star in governing the interplay between the molecular and ionized gas. In our sample of HII regions, the pressure of the neutral gas systematically exceeds that of the ionized gas. This suggests that the surrounding neutral molecular medium can hinder or slow down the expansion of HII regions due to its higher pressure. However, given the limited spatial resolution, a definitive conclusion on the role of molecular gas in confining HII regions cannot be made until high resolution observations are obtained.</description><source format="bibcode">2026A&amp;A...706A.280K</source><referenceURL>https://cdsarc.cds.unistra.fr/viz-bin/cat/J/A+A/706/A280</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/565/A75">J/A+A/565/A75 : ATLASGAL: dust condensations in Galactic plane</relatedResource><relatedResource ivo-id="ivo://CDS.VizieR/J/A+A/611/A6">J/A+A/611/A6 : ATLASGAL massive clumps H_2_CO data (Tang+, 2018)</relatedResource><relatedResource ivo-id="ivo://CDS.VizieR/J/MNRAS/473/1059">J/MNRAS/473/1059 : Complete sample of Galactic clump properties</relatedResource><relatedResource ivo-id="ivo://CDS.VizieR/J/A+A/627/A175">J/A+A/627/A175 : GLOSTAR. Radio Source Catalogue I (Medina+, 2019)</relatedResource><relatedResource ivo-id="ivo://CDS.VizieR/J/MNRAS/510/3389">J/MNRAS/510/3389 : High-mass star formation evolutionary trends</relatedResource><relatedResource ivo-id="ivo://CDS.VizieR/J/A+A/689/A196">J/A+A/689/A196 : GLOSTAR GPS. Radio source catalog (Medina+, 2024)</relatedResource><relatedResource ivo-id="ivo://CDS.VizieR/J/A+A/689/A81">J/A+A/689/A81 : GLOSTAR GPS. X. 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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>All</name><description>Display data for all the tables</description><ucd>meta.ref.url</ucd><dataType xsi:type="vs:VOTableType" arraysize="*">char</dataType></column><column><name>GLOSTAR</name><description>Name of the HII region in the GLOSTAR RRL catalog (G1)</description><ucd>meta.id;meta.main</ucd><dataType xsi:type="vs:VOTableType" arraysize="14*">char</dataType></column><column><name>ATLASGAL</name><description>Name of the associated ATLASGAL clump</description><ucd>meta.id</ucd><dataType xsi:type="vs:VOTableType" arraysize="18*">char</dataType></column><column><name>component</name><description>Secondary component name (G2)</description><ucd>meta.code.multip</ucd><dataType xsi:type="vs:VOTableType" arraysize="1*">char</dataType></column><column><name>Tkin</name><description>? Non-LTE Kinetic temperature</description><unit>K</unit><ucd>phys.temperature</ucd><dataType xsi:type="vs:VOTableType">float</dataType><flag>nullable</flag></column><column><name>E_Tkin</name><description>? Upper error in the non-LTE Kinetic temperature</description><unit>K</unit><ucd>stat.error;stat.max</ucd><dataType xsi:type="vs:VOTableType">float</dataType><flag>nullable</flag></column><column><name>e_Tkin</name><description>? Lower error in the non-LTE Kinetic temperature</description><unit>K</unit><ucd>stat.error</ucd><dataType xsi:type="vs:VOTableType">float</dataType><flag>nullable</flag></column><column><name>lognH2</name><description>? Log of H_2_ density</description><unit>log(cm**-3)</unit><ucd>phys.density</ucd><dataType xsi:type="vs:VOTableType">float</dataType><flag>nullable</flag></column><column><name>E_lognH2</name><description>? Log of upper error in the H_2_ density</description><unit>log(cm**-3)</unit><ucd>stat.error;stat.max</ucd><dataType xsi:type="vs:VOTableType">float</dataType><flag>nullable</flag></column><column><name>e_lognH2</name><description>? Log of lower error in the H_2_ density</description><unit>log(cm**-3)</unit><ucd>stat.error</ucd><dataType xsi:type="vs:VOTableType">float</dataType><flag>nullable</flag></column><column><name>logNH2CO</name><description>? Log of para-H_2_CO column density</description><unit>log(cm**-2)</unit><ucd>phys.columnDensity</ucd><dataType xsi:type="vs:VOTableType">float</dataType><flag>nullable</flag></column><column><name>E_logNH2CO</name><description>? Log of upper error in the para-H_2_CO column density</description><unit>log(cm**-2)</unit><ucd>stat.error;stat.max</ucd><dataType xsi:type="vs:VOTableType">float</dataType><flag>nullable</flag></column><column><name>e_logNH2CO</name><description>? Log of lower error in the para-H_2_CO column density</description><unit>log(cm**-2)</unit><ucd>stat.error</ucd><dataType xsi:type="vs:VOTableType">float</dataType><flag>nullable</flag></column><column><name>logXH2CO</name><description>? Log of fractional abundance of para-H_2_CO</description><ucd>phys.abund</ucd><dataType xsi:type="vs:VOTableType">float</dataType><flag>nullable</flag></column><column><name>logNH2</name><description>? Log of H_2_ column density</description><unit>log(cm**-2)</unit><ucd>phys.columnDensity</ucd><dataType xsi:type="vs:VOTableType">float</dataType><flag>nullable</flag></column></table></schema></tableset></ri:Resource>