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(Referência obtida automaticamente do Web of Science, por meio da informação sobre o financiamento pela FAPESP e o número do processo correspondente, incluída na publicação pelos autores.)

CAPOS: The bulge Cluster APOgee Survey II. The intriguing ``Sequoia{''} globular cluster FSR 1758

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Autor(es):
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Romero-Colmenares, Maria [1, 2] ; Fernandez-Trincado, Jose G. [1, 3] ; Geisler, Doug [4, 5, 6] ; Souza, Stefano O. [7] ; Villanova, Sandro [4] ; Longa-Pena, Penelope [2] ; Minniti, Dante [8, 9] ; Beers, Timothy C. [10, 11] ; Moni Bidin, Cristian [3] ; Perez-Villegas, Angeles [12] ; Moreno, Edmundo [13] ; Garro, Elisa R. [9] ; Baeza, Ian [4] ; Henao, Lady [4] ; Barbuy, Beatriz [7] ; Alonso-Garcia, Javier [2, 14] ; Cohen, Roger E. [15] ; Lane, Richard R. [1, 16] ; Munoz, Cesar [5, 6]
Número total de Autores: 19
Afiliação do(s) autor(es):
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[1] Univ Atacama, Inst Astron & Ciencias Planetarias, Copayapu 485, Copiapo - Chile
[2] Univ Antofagasta, Ctr Astron CITEVA, Antofagasta 601 - Chile
[3] Univ Catolica Norte, Inst Astron, Av Angamos 0610, Antofagasta - Chile
[4] Univ Concepcion, Dept Astron, Casilla 160-C, Concepcion - Chile
[5] Univ La Serena, Inst Invest Multidisciplinario Ciencia & Tecnol, Benavente 980, La Serena - Chile
[6] Univ La Serena, Dept Astron, La Serena 1700000 - Chile
[7] Univ Sao Paulo, IAG, Cidade Univ, Rua Matao 1226, BR-05508900 Sao Paulo - Brazil
[8] Vatican Observ, I-00120 Vatican City - Vatican
[9] Univ Andres Bello, Fac Ciencias Exactas, Dept Cs Fis, Av Fernandez Concha 700, Santiago - Chile
[10] Univ Notre Dame, Dept Phys, Notre Dame, IN 46556 - USA
[11] Univ Notre Dame, JINA Ctr Evolut Elements, Notre Dame, IN 46556 - USA
[12] Univ Nacl Autonoma Mexico, Inst Astron, Apdo Postal 106, Ensenada 22800, Baja California - Mexico
[13] Univ Nacl Autonoma Mexico, Inst Astron, Apdo Postal 70264, Mexico City 04510, DF - Mexico
[14] Millennium Inst Astrophys, Nuncio Monsenor Sotero Sanz 100, Of 104, Santiago - Chile
[15] Space Telescope Sci Inst, 3700 San Martin Dr, Baltimore, MD 21218 - USA
[16] Univ Bernardo O Higgins, Ctr Invest Astron, Ave Viel 1497, Santiago - Chile
Número total de Afiliações: 16
Tipo de documento: Artigo Científico
Fonte: Astronomy & Astrophysics; v. 652, AUG 27 2021.
Citações Web of Science: 1
Resumo

We present results from a study of 15 red giant members of the intermediate-metallicity globular cluster (GC) FSR 1758 using high-resolution, near-infrared spectra collected with the Apache Point Observatory Galactic Evolution Experiment II survey (APOGEE-2) that were obtained as part of CAPOS (the bulge Cluster APOgee Survey). Since its very recent discovery as a massive GC in the bulge region, evoking the name Sequoia, this has been an intriguing object with a highly debated origin, and initially led to the suggestion of a purported progenitor dwarf galaxy of the same name. In this work, we use new spectroscopic and astrometric data to provide additional clues as to the nature of FSR 1758. Our study confirms the GC nature of FSR 1758, and as such we report the existence of the characteristic N-C anticorrelation and Al-N correlation for the first time. We thereby reveal the existence of the multiple-population phenomenon, similar to that observed in virtually all GCs. Furthermore, the presence of a population with strongly enriched aluminum makes it unlikely that FSR 1758 is the remnant nucleus of a dwarf galaxy because Al-enhanced stars are uncommon in dwarf galaxies. We find that FSR 1758 is slightly more metal rich than previously reported in the literature; this source has a mean metallicity {[}Fe/H] between -1.43 to -1.36, depending on the adopted atmospheric parameters and a scatter within observational error, again pointing to its GC nature. Overall, the alpha-enrichment (greater than or similar to + 0.3 dex), Fe-peak (Fe, Ni), light (C, N), and odd-Z (Al) elements follow the trend of intermediate-metallicity GCs. Isochrone fitting in the Gaia bands yields an estimated age of similar to 11.6 Gyr. We used the exquisite kinematic data, including our CAPOS radial velocities and Gaia eDR3 proper motions, to constrain the N-body density profile of FSR 1758, and found that it is as massive (similar to 2.9 +/- 0.6 x 10(5) M-circle dot) as NGC 6752. We confirm a retrograde and eccentric orbit for FSR 1758. A new examination of its dynamical properties with the GravPot16 model favors an association with the Gaia-Enceladus-Sausage accretion event. Thus, paradoxically, the cluster that gave rise to the name of the Sequoia dwarf galaxy does not appear to belong to this specific merging event. (AU)

Processo FAPESP: 18/22044-3 - Aglomerados globulares do bojo: relíquias da formação e evolução da galáxia
Beneficiário:Stefano Oliveira de Souza
Modalidade de apoio: Bolsas no Brasil - Doutorado Direto