Browsing by Author "Ripepi, Vincenzo"

Now showing 1 - 3 of 3
  • Thumbnail Image
    Item
    Discovery of Tidal RR Lyrae Stars in the Bulge Globular Cluster M62
    (2018) Minniti, D.; Fernandez-Trincado, Jose G.; Ripepi, Vincenzo; Alonso-Garcia, Javier; Contreras Ramos, Rodrigo Andrés; Marconi, Marcella
  • No Thumbnail Available
    Item
    Looking for the Building Blocks of the Galactic Halo: Variable stars in the Fornax, Bootes I, Canes Venatici II Dwarfs and in NGC2419
    (2009) Greco, Claudia; Clementini, Gisella; Held, Enrico E.; Poretti, Ennio; Catelan, Márcio; Federici, Luciana; Gullieuszik, Marco; Maio, Marcella; Ripepi, Vincenzo; Dall'Ora, Massimo; di Fabrizio, Luca; Kinemuchi, Karen; di Criscienzo, Marcella; Marconi, Marcella; Musella, Ilaria; Rest, Armin; de Lee, Nathan; Pritzl, Barton J.; Smith, Horace
    Looking for the building blocks of the Galactic Halo we have investigated and compared the properties of the RR Lyrae stars in a number of different stellar systems inside and outside the Milky Way.
  • No Thumbnail Available
    Item
    The RR Lyrae projected density distribution from the Galactic centre to the halo
    (2021) Gabriela Navarro, Maria; Minniti, Dante; Capuzzo-Dolcetta, Roberto; Alonso-Garcia, Javier; Contreras Ramos, Rodrigo; Majaess, Daniel; Ripepi, Vincenzo
    The projected density distribution of type ab RR Lyrae (RRab) stars was characterised from the innermost regions of the Milky Way to the halo, with the aim of placing constraints on the Galaxy's evolution. The compiled sample (N-RRab=64 850) stems from fundamental mode RR Lyrae variables identified by the VVV, OGLE, and Gaia surveys. The distribution is well fitted by three power laws over three radial intervals. In the innermost region (R<2.2) the distribution follows Sigma (RRab[1])proportional to R-0.94 +/- 0.051, while in the external region the distribution adheres to Sigma (RRab[2])proportional to R-1.50 +/- 0.019 for 2.2 degrees< R< 8.0 degrees and Sigma (RRab[3])proportional to R-2.43 +/- 0.043 for 8.0 degrees< R<30.0 degrees. Conversely, the cumulative distribution of red clump (RC) giants exhibits a more concentrated distribution in the mean, but in the central R<2.2 the RRab population is more peaked, whereas globular clusters (GCs) follow a density power law (Sigma (GCs)proportional to R-1.59 +/- 0.060 for R<30.0) similar to that of RRab stars, especially when considering a more metal-poor subsample ([Fe/H] < -1.1 dex). The main conclusion emerging from the analysis is that the RRab distribution favours the star cluster infall and merger scenario for creating an important fraction (> 18%) of the central Galactic region. The radii containing half of the populations (half populations radii) are R-H RRab=6.8 degrees (0.99 kpc), R-H RC=4.2 degrees (0.61 kpc), and R-H GCs=11.9 degrees (1.75 kpc) for the RRab stars, RC giants, and GCs, respectively. Finally, merely similar to 1% of the stars have been actually discovered in the innermost region (R< 35 pc) out of the expected (based on our considerations) total number of RRab therein: N1562. That deficit will be substantially ameliorated with future space missions like the Nancy Grace Roman Space Telescope (formerly WFIRST).