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<ri:Resource created="2021-12-31T10:09:33Z" 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>Morphological properties of galaxies</title><shortName>J/MNRAS/479/4136</shortName><identifier>ivo://CDS.VizieR/J/MNRAS/479/4136</identifier><altIdentifier>doi:10.26093/cds/vizier.74794136</altIdentifier><curation><publisher ivo-id="ivo://CDS">CDS</publisher><creator><name>Karachentsev I.D.</name></creator><creator><name>Kaisina E.I.</name></creator><creator><name>Makarov D.I.</name></creator><date role="Updated">2024-08-18T20:20:44Z</date><date role="Created">2021-12-31T10:09:33Z</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>galaxies</subject><subject>photometry</subject><subject>visible-astronomy</subject><description>We consider an all-sky sample of 1029 Local Volume (LV) galaxies situated within a distance of 11 Mpc. Majority of them have precise distances and estimates of hydrogen mass fraction and star-formation rate derived from far-ultraviolet or H{alpha} fluxes. To describe an environment, we attribute two dimensionless values: the density contrast created by the most significant neighbour and the local density contrast produced by all neighbours within a separation of 1Mpc. The hydrogen mass fraction exhibits a weak effect of HI deficiency being the most pronounced for irregular dwarf galaxies. The specific star formation rate (sSFR) is more sensitive to the environment than the hydrogen mass fraction. Almost all (99 per cent) LV galaxies have their sSFRs below -9.4dex (yr^-1^). We notice that irregular dwarfs as well as late-type bulgeless galaxies are capable of reproducing their stellar mass with the observed sSFR over the cosmic time. Thus, the transformation of gas into stars in dIrs and spiral discs is rather sluggish unlike that in E, S0, dSph galaxies, whose star formation history has been stormy and short. The SFR(H{alpha})-to-SFR(FUV) scatter ratio increases from Sc, Sd, Sm galaxies towards BCD, Im, Ir types which favours the idea of bursty star formations in low-mass galaxies. However, this bursty activity is caused rather by internal processes than by an external tidal action. A fraction of quenched E, S0, dSph galaxies increases from ~5 per cent in the field up to ~50 per cent in the densest regions.</description><source format="bibcode">2018MNRAS.479.4136K</source><referenceURL>https://cdsarc.cds.unistra.fr/viz-bin/cat/J/MNRAS/479/4136</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></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/MNRAS/479/4136</accessURL><mirrorURL title="VizieR at IUCAA: Pune, 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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>Name</name><description>Galaxy name in well-known catalogs</description><ucd>meta.id;meta.main</ucd><dataType xsi:type="vs:VOTableType" arraysize="24*">char</dataType></column><column><name>RAJ2000</name><description>Right ascension (J2000)</description><ucd>pos.eq.ra;meta.main</ucd></column><column><name>DEJ2000</name><description>Declination (J2000)</description><ucd>pos.eq.dec;meta.main</ucd></column><column><name>T</name><description>? Morphological type in de Vaucouleurs scale</description><ucd>src.morph.type</ucd><dataType xsi:type="vs:VOTableType">int</dataType><flag>nullable</flag></column><column><name>D</name><description>Distance</description><unit>Mpc</unit><ucd>pos.distance</ucd><dataType xsi:type="vs:VOTableType">float</dataType></column><column><name>logM*</name><description>? 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Average B-band surface brightness</description><unit>mag.arcsec**-2</unit><ucd>phot.mag.sb</ucd><dataType xsi:type="vs:VOTableType">float</dataType><flag>nullable</flag></column><column><name>theta1</name><description>Dimensionless parameters characterizing the local density contrast</description><ucd>stat.fit.param</ucd><dataType xsi:type="vs:VOTableType">float</dataType></column><column><name>thetaj</name><description>? Dimensionless parameters characterizing the local density contrast</description><ucd>stat.fit.param</ucd><dataType xsi:type="vs:VOTableType">float</dataType><flag>nullable</flag></column></table></schema></tableset></ri:Resource>