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On the Use of Field RR Lyrae as Galactic Probes -- VIII. Early Formation of the Galactic Spheroid

Fuente: arXiv

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Main Authors:	Bono, G., Braga, V. F., Fabrizio, M., Tantalo, M., Baeza-Villagra, K., Crestani, J., D'Orazi, V., Dall'Ora, M., Di Criscienzo, M., Fiorentino, G., Gholami, M., Marengo, M., Martínez-Vázquez, C. E., Monelli, M., Mullen, J. P., Nunnari, A., Pipwala, V. D., Prudil, Z., Sneden, C., Altavilla, G., Bergemann, M., Topcu, G. Böcek, Buonanno, R., Calamida, A., Carretta, E., Ceci, G., Chaboyer, B., Correnti, M., da Silva, R., Ferraro, I., Gómez, F. A., Iannicola, G., Kudritzki, R. -P., Kunder, A., Kwak, S., Marconi, M., Marinoni, S., Matsunaga, N., Matteucci, F., Monachesi, A., Musella, I., Ovando, M. G. Navarro, Preston, G. W., Ripepi, V., Salaris, M., Sánchez-Benavente, M., Spitoni, E., Stetson, P. B., Thévenin, F., Thompson, I. B., Tissera, P. B., Tsujimoto, T., Valenti, E., Vivas, A. K., Walker, A. R., Zoccali, M., Zocchi, A.
Format:	Preprint
Published:	2026
Subjects:	Astrophysics of Galaxies
Online Access:	Acceder al recurso
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author	Bono, G. Braga, V. F. Fabrizio, M. Tantalo, M. Baeza-Villagra, K. Crestani, J. D'Orazi, V. Dall'Ora, M. Di Criscienzo, M. Fiorentino, G. Gholami, M. Marengo, M. Martínez-Vázquez, C. E. Monelli, M. Mullen, J. P. Nunnari, A. Pipwala, V. D. Prudil, Z. Sneden, C. Altavilla, G. Bergemann, M. Topcu, G. Böcek Buonanno, R. Calamida, A. Carretta, E. Ceci, G. Chaboyer, B. Correnti, M. da Silva, R. Ferraro, I. Gómez, F. A. Iannicola, G. Kudritzki, R. -P. Kunder, A. Kwak, S. Marconi, M. Marinoni, S. Matsunaga, N. Matteucci, F. Monachesi, A. Musella, I. Ovando, M. G. Navarro Preston, G. W. Ripepi, V. Salaris, M. Sánchez-Benavente, M. Spitoni, E. Stetson, P. B. Thévenin, F. Thompson, I. B. Tissera, P. B. Tsujimoto, T. Valenti, E. Vivas, A. K. Walker, A. R. Zoccali, M. Zocchi, A.
author_facet	Bono, G. Braga, V. F. Fabrizio, M. Tantalo, M. Baeza-Villagra, K. Crestani, J. D'Orazi, V. Dall'Ora, M. Di Criscienzo, M. Fiorentino, G. Gholami, M. Marengo, M. Martínez-Vázquez, C. E. Monelli, M. Mullen, J. P. Nunnari, A. Pipwala, V. D. Prudil, Z. Sneden, C. Altavilla, G. Bergemann, M. Topcu, G. Böcek Buonanno, R. Calamida, A. Carretta, E. Ceci, G. Chaboyer, B. Correnti, M. da Silva, R. Ferraro, I. Gómez, F. A. Iannicola, G. Kudritzki, R. -P. Kunder, A. Kwak, S. Marconi, M. Marinoni, S. Matsunaga, N. Matteucci, F. Monachesi, A. Musella, I. Ovando, M. G. Navarro Preston, G. W. Ripepi, V. Salaris, M. Sánchez-Benavente, M. Spitoni, E. Stetson, P. B. Thévenin, F. Thompson, I. B. Tissera, P. B. Tsujimoto, T. Valenti, E. Vivas, A. K. Walker, A. R. Zoccali, M. Zocchi, A.
contents	We introduce a new photometric catalog of RR Lyrae variables (RRLs, $\sim$300,000) mainly based on data available in public datasets. We also present the largest and most homogeneous spectroscopic dataset of RRLs and Blue Horizontal Branch [BHB] stars ever collected. This includes radial velocity measurements ($\sim$16,000) and iron abundances ($Δ$S method for 8,140 RRLs, plus 547 from literature). Elemental abundances based on high-resolution spectra are provided for 487 RRLs and 64 BHB stars. We identified candidate RRLs associated to the main Galactic components and their iron distribution function (IDF) becomes more metal-rich when moving from the Halo ([Fe/H]=-1.56) to the Thick (TCD; [Fe/H]=-1.47) and Thin (TND; [Fe/H]=-0.73) disk. Furthermore, Halo RRLs and RRLs in retrograde orbits are $α$-enhanced ([$α$/Fe]=0.27, $σ$=0.18), while TCD RRLs are either $α$-enhanced ([Fe/H]$\le$-1.0) or $α$-poor ([Fe/H]$>$-1.0), and TND RRLs are mainly $α$-poor ([$α$/Fe]=-0.01, $σ$=0.20). We also identified RRLs associated to the main stellar streams (Gaia-Sausage-Enceladus [GSE]; Sequoia, Helmi, Sagittarius) and we found that their IDFs are quite similar to Halo RRLs. However, GSE RRLs lack the metal-poor/metal-rich tails and their $α$-element distribution is quite compact. The iron radial gradient in Galactocentric distance for TND, TCD and Halo RRLs is negative and it decreases from -0.026, to -0.010, and to -0.002 dex/kpc. The iron radial gradient based on dry Halo (Halo without substructures) RRLs is, within the errors, equal to the global Halo. We also found a strong similarity between iron and [$α$/Fe] radial gradients of Milky Way RRLs and M31 globular clusters throughout the full range of galactocentric distances covered by the two samples.
format	Preprint
id	arxiv_https___arxiv_org_abs_2601_16523
institution	arXiv
publishDate	2026
record_format	arxiv
spellingShingle	On the Use of Field RR Lyrae as Galactic Probes -- VIII. Early Formation of the Galactic Spheroid Bono, G. Braga, V. F. Fabrizio, M. Tantalo, M. Baeza-Villagra, K. Crestani, J. D'Orazi, V. Dall'Ora, M. Di Criscienzo, M. Fiorentino, G. Gholami, M. Marengo, M. Martínez-Vázquez, C. E. Monelli, M. Mullen, J. P. Nunnari, A. Pipwala, V. D. Prudil, Z. Sneden, C. Altavilla, G. Bergemann, M. Topcu, G. Böcek Buonanno, R. Calamida, A. Carretta, E. Ceci, G. Chaboyer, B. Correnti, M. da Silva, R. Ferraro, I. Gómez, F. A. Iannicola, G. Kudritzki, R. -P. Kunder, A. Kwak, S. Marconi, M. Marinoni, S. Matsunaga, N. Matteucci, F. Monachesi, A. Musella, I. Ovando, M. G. Navarro Preston, G. W. Ripepi, V. Salaris, M. Sánchez-Benavente, M. Spitoni, E. Stetson, P. B. Thévenin, F. Thompson, I. B. Tissera, P. B. Tsujimoto, T. Valenti, E. Vivas, A. K. Walker, A. R. Zoccali, M. Zocchi, A. Astrophysics of Galaxies We introduce a new photometric catalog of RR Lyrae variables (RRLs, $\sim$300,000) mainly based on data available in public datasets. We also present the largest and most homogeneous spectroscopic dataset of RRLs and Blue Horizontal Branch [BHB] stars ever collected. This includes radial velocity measurements ($\sim$16,000) and iron abundances ($Δ$S method for 8,140 RRLs, plus 547 from literature). Elemental abundances based on high-resolution spectra are provided for 487 RRLs and 64 BHB stars. We identified candidate RRLs associated to the main Galactic components and their iron distribution function (IDF) becomes more metal-rich when moving from the Halo ([Fe/H]=-1.56) to the Thick (TCD; [Fe/H]=-1.47) and Thin (TND; [Fe/H]=-0.73) disk. Furthermore, Halo RRLs and RRLs in retrograde orbits are $α$-enhanced ([$α$/Fe]=0.27, $σ$=0.18), while TCD RRLs are either $α$-enhanced ([Fe/H]$\le$-1.0) or $α$-poor ([Fe/H]$>$-1.0), and TND RRLs are mainly $α$-poor ([$α$/Fe]=-0.01, $σ$=0.20). We also identified RRLs associated to the main stellar streams (Gaia-Sausage-Enceladus [GSE]; Sequoia, Helmi, Sagittarius) and we found that their IDFs are quite similar to Halo RRLs. However, GSE RRLs lack the metal-poor/metal-rich tails and their $α$-element distribution is quite compact. The iron radial gradient in Galactocentric distance for TND, TCD and Halo RRLs is negative and it decreases from -0.026, to -0.010, and to -0.002 dex/kpc. The iron radial gradient based on dry Halo (Halo without substructures) RRLs is, within the errors, equal to the global Halo. We also found a strong similarity between iron and [$α$/Fe] radial gradients of Milky Way RRLs and M31 globular clusters throughout the full range of galactocentric distances covered by the two samples.
title	On the Use of Field RR Lyrae as Galactic Probes -- VIII. Early Formation of the Galactic Spheroid
topic	Astrophysics of Galaxies
url	https://arxiv.org/abs/2601.16523