UVES analysis of red giants in the bulge globular cluster NGC 6522

Barbuy, B.; Cantelli, E.; Muniz, L.; Souza, Stefano O.; Chiappini, Cristina; Hirschi, Raphaël; Cescutti, G.; Pignatari, M.; Ortolani, S.; Kerber, L. O.; Maia, F. F. S.; Bica, E.; Depagne, É.

doi:10.1051/0004-6361/202140815

Cited by 12 publications

(11 citation statements)

References 115 publications

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“…Cristallo et al 2015). This same conclusion was reached by Barbuy et al (2009Barbuy et al ( , 2014Barbuy et al ( , 2021b regarding the globular cluster NGC 6522, but here, since all the present sample stars are enhanced in Ce, all of them would have to be binaries with an AGB companion. Therefore the spinstars seem to be a more plausible explanation.…”

Section: Discussionsupporting

confidence: 83%

Abundance analysis of APOGEE spectra for 58 metal-poor stars from the bulge spheroid

Razera

Barbuy

Moura

et al. 2022

Monthly Notices of the Royal Astronomical Society

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The central part of the Galaxy host a multitude of stellar populations, including the spheroidal bulge stars, stars moved to the bulge through secular evolution of the bar, inner halo, inner thick disk, inner thin disk, as well as debris from past accretion events. We identified a sample of 58 candidate stars belonging to the stellar population of the spheroidal bulge, and analyse their abundances. The present calculations of Mg, Ca, and Si lines are in agreement with the APOGEE-ASPCAP abundances, whereas abundances of C, N, O, and Ce are re-examined. We find normal α-element enhancements in oxygen, similar to magnesium, Si, and Ca abundances, which are typical of other bulge stars surveyed in the optical in Baade’s Window. The enhancement of [O/Fe] in these stars suggests that they do not belong to accreted debris. No spread in N abundances is found, and none of the sample stars is N-rich, indicating that these stars are not second generation stars originated in globular clusters. Ce instead is enhanced in the sample stars, which points to an s-process origin such as due to enrichment from early generations of massive fast rotating stars, the so-called spinstars.

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Section: Discussionsupporting

confidence: 83%

Abundance analysis of APOGEE spectra for 58 metal-poor stars from the bulge spheroid

Razera

Barbuy

Moura

et al. 2022

Monthly Notices of the Royal Astronomical Society

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“…These are examples of the wide gamut of highly reddened GCs examined so far towards the bulge area (see Saracino et al 2015;Schiavon et al 2017;Barbuy et al 2018aBarbuy et al ,b, 2021Fernández-Trincado et al 2019, 2021dKunder & Butler 2020;Kunder et al 2021;Geisler et al 2021;Alonso-García et al 2021, for other cases).…”

Section: Introductionmentioning

confidence: 91%

APOGEE-2S view of the globular cluster Patchick 125 (Gran 3)

Fernández-Trincado

Minniti

Garro

et al. 2022

A&A

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We present detailed elemental abundances, radial velocity, and orbital elements for Patchick 125, a recently discovered metal-poor globular cluster (GC) in the direction of the Galactic bulge. Near-infrared high-resolution (R ∼ 22 500) spectra of two members were obtained during the second phase of the Apache Point Observatory Galactic Evolution Experiment at Las Campanas Observatory as part of the sixteenth Data Release (DR 16) of the Sloan Digital Sky Survey. We investigated elemental abundances for four chemical species, including α- (Mg, Si), Fe-peak (Fe), and odd-Z (Al) elements. We find a metallicity covering the range from [Fe/H] = −1.69 to −1.72, suggesting that Patchick 125 likely exhibits a mean metallicity ⟨[Fe/H]⟩ ∼ −1.7, which represents a significant increase in metallicity for this cluster compared to previous low-resolution spectroscopic analyses. We also found a mean radial velocity of 95.9 km s−1, which is ∼21.6 km s−1 higher than reported in the literature. The observed stars exhibit an α-enrichment ([Mg/Fe] ≲ 0.20, and [Si/Fe] ≲ +0.30) that follows the typical trend of metal-poor GCs. The aluminum abundance ratios for the present two member stars are enhanced in [Al/Fe] ≳ +0.58, which is a typical enrichment characteristic of the so-called ‘second-generation’ of stars in GCs at similar metallicity. This supports the possible presence of the multiple-population phenomenon in Patchick 125, as well as its genuine GC nature. Further, Patchick 125 shows a low-energy, low-eccentric (< 0.4) and retrograde orbit captured by the inner Galaxy, near the edge of the bulge. We confirm that Patchick 125 is a genuine metal-poor GC, which is currently trapped in the vicinity of the Milky Way bulge.

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“…In addition, UKS 1, a heavily reddened GC, with E(B−V)∼2.62, was recently classified as a fossil relic of the bulge based on its chemodynamics properties (Fernández-Trincado et al 2020). These are examples of the wide gamut of highly reddened GCs examined so far towards the bulge area (see Saracino et al 2015;Schiavon et al 2017;Barbuy et al 2018a;Fernández-Trincado et al 2019Barbuy et al 2018bBarbuy et al , 2021Kunder & Butler 2020;Kunder et al 2021;Geisler et al 2021;Fernández-Trincado et al 2021e;Alonso-García et al 2021, for other cases).…”

Section: Introductionmentioning

confidence: 99%

APOGEE-2S view of the globular cluster Patchick 125 (Gran 3). New metallicity and elemental abundances from high-resolution spectroscopy

Fernández-Trincado,

Minniti,

Garro

et al. 2021

Preprint

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We present detailed elemental abundances, radial velocity, and orbital elements for Patchick 125, a recently discovered metal-poor globular cluster (GC) in the direction of the Galactic bulge. Near-infrared high-resolution (R ∼ 22, 500) spectra of two members were obtained during the second phase of the Apache Point Observatory Galactic Evolution Experiment at Las Campanas Observatory as part of the sixteenth Data Release (DR 16) of the Sloan Digital Sky Survey. We investigated elemental abundances for four chemical species, including α-(Mg, Si), Fe-peak (Fe), and odd-Z (Al) elements. We find a metallicity covering the range from [Fe/H] = −1.69 to −1.72, suggesting that Patchick 125 likely exhibits a mean metallicity [Fe/H] ∼ −1.7, which represents a significant increase in metallicity for this cluster compared to previous low-resolution spectroscopic analyses. We also found a mean radial velocity of 95.9 km s −1 , which is ∼21.6 km s −1 higher than reported in the literature. The observed stars exhibit an α-enrichment ([Mg/Fe] +0.20, and [Si/Fe] +0.30) that follows the typical trend of metal-poor GCs. The aluminum abundance ratios for the present two member stars are enhanced in [Al/Fe] +0.58, which is a typical enrichment characteristic of the so-called 'second-generation' of stars in GCs at similar metallicity. This supports the possible presence of the multiple-population phenomenon in Patchick 125, as well as its genuine GC nature. Further, Patchick 125 shows a low-energy, low-eccentric (< 0.4) and retrograde orbit captured by the inner Galaxy, near the edge of the bulge. We confirm that Patchick 125 is a genuine metal-poor GC, which is currently trapped in the vicinity of the Milky Way bulge.

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UVES analysis of red giants in the bulge globular cluster NGC 6522

Cited by 12 publications

References 115 publications

Abundance analysis of APOGEE spectra for 58 metal-poor stars from the bulge spheroid

Abundance analysis of APOGEE spectra for 58 metal-poor stars from the bulge spheroid

APOGEE-2S view of the globular cluster Patchick 125 (Gran 3)

APOGEE-2S view of the globular cluster Patchick 125 (Gran 3). New metallicity and elemental abundances from high-resolution spectroscopy

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