@article{AndersKhalatyanQueirozetal.2022,
  author    = {Anders, Friedrich and Khalatyan, Arman and Queiroz, Anna B. A. and Chiappini, Cristina and Ard{\`e}vol, Judith and Casamiquela, Laia and Figueras, Francesca and Jim{\´e}nez-Arranz, {\´O}scar and Jordi, Carme and Monguio, Maria and Romero-G{\´o}mez, Merce and Altamirano, Diego and Antoja, Teresa and Assaad, R. and Cantat-Gaudin, Tristan and Castro-Ginard, Alfred and Enke, Harry and Girardi, L{\´e}o and Guiglion, Guillaume and Khan, Saniya and Luri, Xavier and Miglio, Andrea and Minchev, Ivan and Ramos, Pau and Santiago, Basillio Xavier and Steinmetz, Matthias},
  title     = {Photo-astrometric distances, extinctions, and astrophysical parameters for Gaia EDR3 stars brighter than G=18.5},
  series = {Astronomy and astrophysics},
  volume    = {658},
  journal   = {Astronomy and astrophysics},
  publisher = {EDP Sciences},
  address   = {Les Ulis},
  issn      = {0004-6361},
  doi       = {10.1051/0004-6361/202142369},
  pages     = {27},
  year      = {2022},
  abstract  = {We present a catalogue of 362 million stellar parameters, distances, and extinctions derived from Gaia's Early Data Release (EDR3) cross-matched with the photometric catalogues of Pan-STARRS1, SkyMapper, 2MASS, and All WISE. The higher precision of the Gaia EDR3 data, combined with the broad wavelength coverage of the additional photometric surveys and the new stellar-density priors of the StarHorse code, allows us to substantially improve the accuracy and precision over previous photo-astrometric stellar-parameter estimates. At magnitude G = 14 (17), our typical precisions amount to 3\% (15\%) in distance, 0.13 mag (0.15 mag) in V-band extinction, and 140 K (180 K) in effective temperature. Our results are validated by comparisons with open clusters, as well as with asteroseismic and spectroscopic measurements, indicating systematic errors smaller than the nominal uncertainties for the vast majority of objects. We also provide distance- and extinction-corrected colour-magnitude diagrams, extinction maps, and extensive stellar density maps that reveal detailed substructures in the Milky Way and beyond. The new density maps now probe a much greater volume, extending to regions beyond the Galactic bar and to Local Group galaxies, with a larger total number density. We publish our results through an ADQL query interface (gaia . aip . de) as well as via tables containing approximations of the full posterior distributions. Our multi-wavelength approach and the deep magnitude limit render our results useful also beyond the next Gaia release, DR3.},
  language  = {en}
}
@article{MuravevaPalmerClementinietal.2015,
  author    = {Muraveva, Tatiana and Palmer, Max and Clementini, Gisella and Luri, Xavier and Cioni, Maria-Rosa L. and Moretti, Maria Ida and Marconi, Marcella and Ripepi, Vincenzo and Rubele, Stefano},
  title     = {New near-infrared period-luminosity-metallicity relations for RR lyrae stars and the outlock for GAIA},
  series = {The astrophysical journal : an international review of spectroscopy and astronomical physics},
  volume    = {807},
  journal   = {The astrophysical journal : an international review of spectroscopy and astronomical physics},
  number    = {2},
  publisher = {IOP Publ. Ltd.},
  address   = {Bristol},
  issn      = {0004-637X},
  doi       = {10.1088/0004-637X/807/2/127},
  pages     = {17},
  year      = {2015},
  abstract  = {We present results of the analysis of 70 RR Lyrae stars located in the bar of the Large Magellanic Cloud (LMC). Combining the spectroscopically determined metallicity of these stars from the literature with precise periods from the OGLE III catalog and multi-epoch K-s photometry from the VISTA survey of the Magellanic Clouds system, we derive a new near-infrared period-luminosity-metallicity (PLKsZ) relation for RR Lyrae variables. In order to fit the relation we use a fitting method developed specifically for this study. The zero-point of the relation is estimated two different ways: by assuming the value of the distance to the LMC and by using Hubble Space Telescope parallaxes of five RR Lyrae stars in the Milky Way (MW). The difference in distance moduli derived by applying these two approaches is similar to 0.2 mag. To investigate this point further we derive the PL(Ks)Z relation based on 23 MW RR Lyrae stars that had been analyzed in Baade-Wesselink studies. We compared the derived PL(Ks)Z relations for RR Lyrae stars in the MW and LMC. Slopes and zero-points are different, but still consistent within the errors. The shallow slope of the metallicity term is confirmed by both LMC and MW variables. The astrometric space mission Gaia is expected to provide a huge contribution to the determination of the RR Lyrae PL(Ks)Z relation; however, calculating an absolute magnitude from the trigonometric parallax of each star and fitting a PL(Ks)Z relation directly to period and absolute magnitude leads to biased results. We present a tool to achieve an unbiased solution by modeling the data and inferring the slope and zero-point of the relation via statistical methods.},
  language  = {en}
}