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<ri:Resource created="2016-03-03T08:50:27Z" status="active" updated="2025-06-13T15:25:00Z" 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>Low-luminosity type-1 QSO sample. V.</title><shortName>J/A+A/587/A138</shortName><identifier>ivo://CDS.VizieR/J/A+A/587/A138</identifier><altIdentifier>doi:10.26093/cds/vizier.35870138</altIdentifier><curation><publisher ivo-id="ivo://CDS">CDS</publisher><creator><name>Busch G.</name></creator><creator><name>Fazeli N.</name></creator><creator><name>Eckart A.</name></creator><creator><name>Valencia-S. M.</name></creator><creator><name>Smajic S.</name></creator><creator><name>Moser L.,Scharwaechter J.</name></creator><creator><name>Dierkes J.</name></creator><creator><name>Fischer S.</name></creator><date role="Updated">2016-03-03T07:57:11Z</date><date role="Created">2016-03-03T08:50:27Z</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>active-galactic-nuclei</subject><subject>seyfert-galaxies</subject><subject>infrared-astronomy</subject><subject>spectroscopy</subject><description>We present near-infrared (NIR) H+K-band long-slit spectra of eleven galaxies that were obtained with SOFI at the NTT (ESO). The galaxies are chosen from the low-luminosity type-1 quasi-stellar object (LLQSO) sample, which comprises the 99 closest (z&lt;=0.06) QSOs from the Hamburg/ESO survey for bright UV-excess QSOs. These objects are ideal targets to study the gap between local Seyfert galaxies and high-redshift quasars because they show much stronger AGN activity than local objects, but are still close enough for a detailed structural analysis. We fit hydrogen recombination, molecular hydrogen, and [FeII] lines after carefully subtracting the continuum emission. From the broad Pa{alpha} components, we estimated black hole masses and enlarged the sample of LLQSOs that deviate from the MBH-Lbulge relations of inactive galaxies from 12 to 16 objects. All objects show emission from hot dust (T~1200K) as well as stellar contribution. However, the respective fractions vary strongly among the objects. More than half of the objects show H_2_ emission lines, which indicate a large reservoir of molecular gas that is needed to feed the AGN and star formation. In the NIR diagnostic diagram all objects lie in the location of AGN-dominated objects. However, most of the objects show indications of star formation activity, suggesting that their offset location with respect to MBH-Lbulge relations of inactive galaxies may be a consequence of overluminous bulges.</description><source format="bibcode">2016A&amp;A...587A.138B</source><referenceURL>https://cdsarc.cds.unistra.fr/viz-bin/cat/J/A+A/587/A138</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/561/A140">J/A+A/561/A140 : Low-luminosity type-1 QSO sample. I. (Busch+, 2014)</relatedResource><relatedResource ivo-id="ivo://CDS.VizieR/J/A+A/580/A113">J/A+A/580/A113 : Low-luminosity type-1 QSO sample. III. 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