CUSANO, FELICEFELICECUSANOMoretti, Maria IdaMaria IdaMorettiCLEMENTINI, GisellaGisellaCLEMENTINIRIPEPI, VincenzoVincenzoRIPEPIMARCONI, MarcellaMarcellaMARCONICioni, M. -R. L.M. -R. L.CioniRUBELE, STEFANOSTEFANORUBELEGarofalo, A.A.Garofalode Grijs, R.R.de GrijsGroenewegen, M. A. T.M. A. T.GroenewegenOliveira, J. M.J. M.OliveiraSubramanian, S.S.SubramanianSun, N. -C.N. -C.Sunvan Loon, J. Th.J. Th.van Loon2022-03-252022-03-2520210035-8711http://hdl.handle.net/20.500.12386/31905We present results from an analysis of $\sim$ 29,000 RR Lyrae stars located in the Large Magellanic Cloud (LMC). For these objects, near-infrared time-series photometry from the VISTA survey of the Magellanic Clouds system (VMC) and optical data from the OGLE (Optical Gravitational Lensing Experiment) IV survey and the Gaia Data Release 2 catalogue of confirmed RR Lyrae stars were exploited. Using VMC and OGLE IV magnitudes we derived period-luminosity (PL), period-luminosity-metallicity (PLZ), period-Wesenheit (PW) and period-Wesenheit-metallicity (PWZ) relations in all available bands. More that ~7,000 RR Lyrae were discarded from the analysis because they appear to be overluminous with respect to the PL relations. The $PL_{K_{\mathrm{s}}}$ relation was used to derive individual distance to $\sim 22,000$ RR Lyrae stars, and study the three-dimensional structure of the LMC. The distribution of the LMC RR Lyrae stars is ellipsoidal with the three axis $S_1$=6.5 kpc, $S_2$=4.6 kpc and $S_3$=3.7 kpc, inclination i=$22\pm4^{\circ }$ relative to the plane of the sky and position angle of the line of nodes $\theta=167\pm7^{\circ }$ (measured from north to east). The north-eastern part of the ellipsoid is closer to us and no particular associated substructures are detected as well as any metallicity gradient.STAMPAenArticle10.1093/mnras/stab9012-s2.0-85107829982http://arxiv.org/abs/2103.15492v1https://academic.oup.com/mnras/article-abstract/504/1/1/6206842?redirectedFrom=fulltext&login=falseFIS/05 - ASTRONOMIA E ASTROFISICA