J/MNRAS/477/4187ivo://CDS.VizieR/J/MNRAS/477/4187doi:10.26093/cds/vizier.74774187CDSHaghi H.Khodadadi A.Ghari A.Hasani Zonoozi A.Kroupa P.2024-08-18T20:19:19Z2021-08-20T14:07:40ZCDS support team

CDS, Observatoire de Strasbourg, 11 rue de l'Universite, F-67000 Strasbourg, France

cds-question@unistra.frgalaxiesgalaxy-classification-systemsMass models of a sample of 171 low- and high-surface brightness galaxies are presented in the context of the cold dark matter (CDM) theory using the NFW dark matter halo density distribution to extract a new concentration-viral mass relation (c-M_vir_). The rotation curves (RCs) are calculated from the total baryonic matter based on the 3.6{mu}m-band surface photometry, the observed distribution of neutral hydrogen, and the dark halo, in which the three adjustable parameters are the stellar mass-to-light ratio, halo concentration, and virial mass. Although accounting for a NFW dark halo profile can explain RC observations, the implied c-M_vir_ relation from RC analysis strongly disagrees with that resulting from different cosmological simulations. Also, the M/L-colour correlation of the studied galaxies is inconsistent with that expected from stellar population synthesis models with different stellar initial mass functions. Moreover, we show that the best-fitting stellar M/L ratios of 51 galaxies (30 per cent of our sample) have unphysically negative values in the framework of the {Lambda}CDM theory. This can be interpreted as a serious crisis for this theory. This suggests either that the commonly used NFW halo profile, which is a natural result of {Lambda}CDM cosmological structure formation, is not an appropriate profile for the dark haloes of galaxies, or, new dark matter physics or alternative gravity models are needed to explain the rotational velocities of disc galaxies.2018MNRAS.477.4187Hhttps://cdsarc.cds.unistra.fr/viz-bin/cat/J/MNRAS/477/4187CatalogResearchIsServedByTAP VizieR generic servicerelated-toJ/AJ/152/157 : Mass models for 175 disk galaxies with SPARC (Lelli+, 2016)https://cds.unistra.fr/vizier-org/licences_vizier.htmlhttps://vizier.cds.unistra.fr/viz-bin/VizieR-2?-source=J/MNRAS/477/4187https://vizier.iucaa.in/viz-bin/VizieR-2?-source=J/MNRAS/477/4187http://vizieridia.saao.ac.za/viz-bin/VizieR-2?-source=J/MNRAS/477/4187https://vizier.cds.unistra.fr/viz-bin/votable?-source=J/MNRAS/477/4187https://vizier.iucaa.in/viz-bin/votable?-source=J/MNRAS/477/4187http://vizieridia.saao.ac.za/viz-bin/votable?-source=J/MNRAS/477/4187GETtext/xml+votablehttps://tapvizier.cds.unistra.fr/TAPVizieR/tapOpticaldefaultJ/MNRAS/477/4187/table1The results for RC fits with assuming NFW halo profilesSimbadNameSimbad column added by the CDSmeta.idcharE_cError on c (upper value)stat.error;stat.maxfloatrecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintGalaxyGalaxy namemeta.id;meta.maincharType[0/11] Morphological typesrc.morph.typeintL[3.6]luminosity of the galaxy in the 3.6um band1e+09solLumphys.luminosityfloate_L[3.6]rms uncertainty on L[3.6]1e+09solLumstat.errorfloatReffEffective radius at [3.6] the radius at which half of the total light of the galaxy is emitted)kpcphys.size.radiusfloatRdiscExponential disc radiuskpcphys.size.radiusfloatMgasTotal gaseous mass1e+09solMassphys.massfloatB-V? B-V colour indexmagphot.color;em.opt.B;em.opt.VfloatnullableM*/L[3.6]Best-fitting stellar mass-to-light ratio in the 3.6 micron band for discsphys.composition.massLightRatiofloatE_M*/L[3.6]Error on M*/L[3.6] (upper value)stat.error;stat.maxfloate_M*/L[3.6]? Error on M*/L[3.6] (lower value)stat.errorfloatnullableMvirVirial mass of the halo (best-fitting parameters for the NFW dark-halo profile)1e+10solMassphys.massdoublee_MvirError on Mvir (upper value)1e+10solMassstat.errordoubleE_Mvir? Error on Mvir (lower value)1e+10solMassstat.error;stat.maxdoublenullablecConcentration parameter (best-fitting parameters for the NFW dark-halo profile)stat.paramfloate_c? Error on c (lower value)stat.errorfloatnullablechi2Reduced chi^2^stat.fit.chi2float