The RR Lyrae projected density distribution from the Galactic centre to the halo

¹ Departamento de Ciencias Físicas, Facultad de Ciencias Exactas, Universidad Andrés Bello, Av. Fernández Concha 700, Las Condes, Santiago, Chile
e-mail: mgnavarro@uc.cl
² Dipartimento di Fisica, Università degli Studi di Roma, “La Sapienza”, P.le Aldo Moro, 2, 00185 Rome, Italy
³ Millennium Institute of Astrophysics, Av. Vicuña Mackenna 4860, 782-0436 Santiago, Chile
⁴ Vatican Observatory, 00120 Vatican City State, Italy
⁵ Centro de Astronomía (CITEVA), Universidad de Antofagasta, Av. Angamos 601, Antofagasta, Chile
⁶ Instituto de Astrofísica, Pontificia Universidad Católica de Chile, Av. Vicuña Mackenna 4860, 782-0436 Macúl, Santiago, Chile
⁷ Mount Saint Vincent University, Halifax, Nova Scotia, Canada
⁸ Saint Mary’s University, Halifax, Nova Scotia, Canada
⁹ INAF-Osservatorio Astronomico di Capodimonte, Naples, Italy

Received: 21 May 2020
Accepted: 8 October 2020

Abstract

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 Σ_RRab[1] ∝ R^{−0.94 ± 0.051}, while in the external region the distribution adheres to Σ_RRab[2] ∝ R^{−1.50 ± 0.019} for 2.2° < R <  8.0° and Σ_RRab[3] ∝ R^{−2.43 ± 0.043} for 8.0° < R < 30.0°. 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 (Σ_GCs ∝ 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° (0.99 kpc), R_{H RC} = 4.2° (0.61 kpc), and R_{H GCs} = 11.9° (1.75 kpc) for the RRab stars, RC giants, and GCs, respectively. Finally, merely ∼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: N ∼ 1562. That deficit will be substantially ameliorated with future space missions like the Nancy Grace Roman Space Telescope (formerly WFIRST).