sMILES SSPs: a library of semi-empirical MILES stellar population models with variable [α/Fe] abundances

Knowles, Adam Thomas; Sansom, A. E.; Vazdekis, Alexandre; Prieto, C. Allende

doi:10.1093/mnras/stad1647

Monthly Notices of the Royal Astronomical Society

2023

DOI: 10.1093/mnras/stad1647

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sMILES SSPs: a library of semi-empirical MILES stellar population models with variable [α/Fe] abundances

Adam Thomas Knowles

A. E. Sansom

Alexandre Vazdekis

et al.

Abstract: We present a new library of semi-empirical stellar population models that are based on the empirical MILES and semi-empirical sMILES stellar libraries. The models span a large range of age and metallicity, in addition to an [α/Fe] coverage from −0.2 to +0.6 dex, at MILES resolution (FWHM = $2.5\,$ Å) and wavelength coverage ($3540.5-7409.6\,$ Å). These models are aimed at exploring abundance ratios in the integrated light from stellar populations in star clusters and galaxies. Our approach is to build SSPs fr… Show more

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Cited by 4 publications

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Ages, metallicity, and α-enhancement of the globular cluster populations in NGC 3311

Grasser,

Arnaboldi,

Barbosa

et al. 2024

A&A

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We aim to investigate the stellar population properties, ages, and metal content of the globular clusters (GCs) in NGC 3311, the central galaxy of the Hydra I cluster, to better constrain its evolution history. We used integral-field spectroscopic data from the Multi-Unit Spectroscopic Explorer (MUSE) to identify 680 sources in the central region of NGC 3311 and extract their 1D spectra. An analysis of these sources in terms of morphologies, radial velocities, and emission lines allowed us to narrow down our selection to $49$ bona fide GC candidates. We split these candidates into two groups depending on their projected distance to the galaxy center ($R$), namely inner ($R 20"$) and outer ($R>20''$) GCs. We stacked the extracted 1D spectra of the inner and outer GC populations to increase the signal-to-noise ratios (S/Ns) of the resulting spectra and hence allow full-spectrum fitting. In addition, we also created a stacked spectrum of all GCs in NGC 3311 and one of the two most central GC candidates. Using the code pPXF we performed a stellar population analysis on the four stacked 1D spectra, obtaining mass-weighted integrated ages, metallicities, and $ alpha/$Fe abundances. All GCs are old, with ages $ Gyr, and they have super-solar metallicities. Looking at the color distribution, we find that the inner ones tend to be redder and more metal rich than the outer ones. This is consistent with the two-phase formation scenario. Looking at the full-spectral fitting results, at face value the outer GCs have a larger alpha/$Fe ratio, which is in line with what is found for the stars that dominate the surface brightness profile at the same radii. However, the values for outer and inner GCs are consistent within the uncertainties. Interestingly, the stacked spectrum of the two most central GCs appears to have the highest metallicity and $ alpha/$Fe although with larger uncertainties. They might be associated with the core progenitor of NGC 3311. The careful analysis of the MUSE-extracted 1D spectra for compact sources in the center of NGC 3311 and its halo indicate that a significant fraction (28<!PCT!>) do display emission lines. Once they are removed, the selected bona fide GC candidates are old ($ 13.5$ Gyr) and have super-solar metallicities (slightly larger in the center) and alpha/$Fe (slightly larger for the outer GCs). Stellar population analyses of the extracted spectra do not support the presence of an intermediate (a few Gigayears) GC population in the central 40 arcsec (10 kpc) radius of NGC 3311.

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Ages, metallicity, and α-enhancement of the globular cluster populations in NGC 3311

Grasser,

Arnaboldi,

Barbosa

et al. 2024

A&A

View full text Add to dashboard Cite

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Radial gradients of CO absorptions and abundance ratios in the bulge of M31

La Barbera,

Vazdekis,

Pasquali

et al. 2024

A&A

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We present new H- and K-band spectroscopy for the bulge of M31, taken with the LUCI spectrograph at the Large Binocular Telescope (LBT). We studied radial trends of CO absorption features (namely and ) in the bulge of M31, out to a galactocentric distance of $ 380$ pc). We find that most COs do not exhibit a strong radial gradient, despite the strong metallicity gradient inferred from the optical spectral range, except for showing a steep increase in the center. We compared the observed line strengths to predictions of different state-of-the-art stellar population models, including an updated version of EMILES models, which also uses the extended IRTF spectral library. The observed COs are close to models' predictions, but in some models they turn out to be underestimated. We find that the lack of radial gradients is due to the combination of increasing CO strength with metallicity and C abundance, and decreasing CO strength with IMF slope and O abundance. We speculate that the steep gradient of might be due to Na overabundance. Remarkably, we were able to fit, at the same time, optical indices and all the NIR COs (except for CO1.68) leaving abundance ratios (i.e. and ) as free-fitting parameters, imposing age and metallicity constraints from the optical spectral range with no significant contribution from intermediate-age populations ($ 1$ Gyr-old). For the majority of the bulge, we find 0.15$ dex larger than (by $ 0.1$ dex), and C abundance consistent with that of Mg. In the central (few arcsec) region, we still find an enhancement of O and Mg, but significantly lower . We find that the COs' line strengths of the bulge are significantly lower than those of massive galaxies, possibly because of a difference in carbon abundance, as well as, to some extent, total metallicity.

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INSPIRE: INvestigating Stellar Population In RElics – V. A catalogue of ultra-compact massive galaxies outside the local Universe and their degree of relicness

Spiniello,

D’Ago,

Coccato

et al. 2023

Monthly Notices of the Royal Astronomical Society

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This paper presents the third data release of the INvestigating Stellar Population In RElics (INSPIRE) project, comprising 52 ultra-compact massive galaxies (UCMGs) observed with the X-Shooter spectrograph. We measure integrated stellar velocity dispersion, [Mg/Fe] abundances, ages, and metallicities for all the INSPIRE objects. We thus infer star formation histories and confirm the existence of a degree of relicness (DoR), defined in terms of the fraction of stellar mass formed by z = 2, the time at which a galaxy has assembled 75 per cent of its mass, and the final assembly time. Objects with a high DoR assembled their stellar mass at early epochs, while low-DoR objects show a non-negligible fraction of later formed populations and hence a spread in ages and metallicities. A higher DoR correlates with larger [Mg/Fe], supersolar metallicity, and larger velocity dispersion values. The 52 UMCGs span a large range of DoR from 0.83 to 0.06, with 38 of them having formed more than 75 per cent of their mass by z = 2. Of these, nine are extreme relics (DoR>0.7), since they formed the totality ($\gt 99~{{\ \rm per\ cent}}$) of their stellar mass by redshift z = 2. The remaining 14 UCMGs cannot be considered relics, as they are characterized by more extended star formation histories. With INSPIRE we built the first sizeable sample of relics outside the local Universe, up to z ∼ 0.4, increasing the number of confirmed relics by a factor of >10, and opening up an important window to explain the mass assembly of massive galaxies in the high-z Universe.

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sMILES SSPs: a library of semi-empirical MILES stellar population models with variable [α/Fe] abundances

Cited by 4 publications

References 80 publications

Ages, metallicity, and α-enhancement of the globular cluster populations in NGC 3311

Ages, metallicity, and α-enhancement of the globular cluster populations in NGC 3311

Radial gradients of CO absorptions and abundance ratios in the bulge of M31

INSPIRE: INvestigating Stellar Population In RElics – V. A catalogue of ultra-compact massive galaxies outside the local Universe and their degree of relicness

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