The Updated BaSTI Stellar Evolution Models and Isochrones. I. Solar-scaled Calculations

Hidalgo, Sebastián L.; Pietrinferni, A.; Cassisi, S.; Salaris, Maurizio; Mucciarelli, A.; Savino, A.; Aparicio, A.; Aguirre, V. Silva; Verma, Kuldeep Chand

doi:10.3847/1538-4357/aab158

Cited by 293 publications

(267 citation statements)

References 154 publications

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“…We fit each entire CMD with five different stellar evolution libraries: Dartmouth (Dotter et al 2008), Padova (Girardi et al 2010), PARSEC (Bressan et al 2012), MIST (Choi et al 2016), and BaSTI (Hidalgo et al 2018). We find that for all CMDs analyzed in this paper the BaSTI 2018 models provide the best overall fits in terms of visual inspection of the residuals and through comparison of likelihood ratios between models.…”

Section: Methodsmentioning

confidence: 85%

Comparing the Quenching Times of Faint M31 and Milky Way Satellite Galaxies

Weisz

Martín

Dolphin

et al. 2019

ApJL

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We present the star formation histories (SFHs) of 20 faint M31 satellites (−12 M V −6) that were measured by modeling sub-horizontal branch (HB) depth color-magnitude diagrams constructed from Hubble Space Telescope (HST) imaging. Reinforcing previous results, we find that virtually all galaxies quenched between 3 and 9 Gyr ago, independent of luminosity, with a notable concentration 3 − 6 Gyr ago. This is in contrast to the Milky Way (MW) satellites, which are generally either faint with ancient quenching times or luminous with recent (<3 Gyr) quenching times. We suggest that systematic differences in the quenching times of M31 and MW satellites may be a reflection of the varying accretion histories of M31 and the MW. This result implies that the formation histories of low-mass satellites may not be broadly representative of low-mass galaxies in general. Among the M31 satellite population we identify two distinct groups based on their SFHs: one with exponentially declining SFHs (τ ∼ 2 Gyr) and one with rising SFHs with abrupt quenching. We speculate how these two groups could be related to scenarios for a recent major merger involving M31. The Cycle 27 HST Treasury survey of M31 satellites will provide well-constrained ancient SFHs to go along with the quenching times we measure here. The discovery and characterization of M31 satellites with M V −6 would help quantify the relative contributions of reionization and environment to quenching of the lowest-mass satellites.

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Section: Methodsmentioning

confidence: 85%

Comparing the Quenching Times of Faint M31 and Milky Way Satellite Galaxies

Weisz

Martín

Dolphin

et al. 2019

ApJL

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“…Much of this discrepancy is driven by differences in the isochronal ages, which is likely attributable to differences between the MIST stellar evolution models and those used in the AMP analysis: a combination of the Aarhus stellar evolution code (ASTEC Christensen-Dalsgaard 2008a) and the adiabatic pulsation code (ADIPLS Christensen-Dalsgaard 2008b). We compared non-rotating, Solar-metallicity MIST isochrones for middle-aged stars with Solar-metallicity BaSTI isochrones (Pietrinferni et al 2004;Hidalgo et al 2018) and found that, for stars between 4 and 8 Gyrs, in the same effective temperature range as the asteroseismic stars, the age discrepancy between the two sets of models can be as large as 1-2 billion years. The MIST isochrones lie above the BaSTI isochrones on the HR diagram, leading to a systematic underprediction of ages.…”

Section: Test 3: Kepler Asteroseismic Starsmentioning

confidence: 99%

Toward Precise Stellar Ages: Combining Isochrone Fitting with Empirical Gyrochronology

et al. 2019

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We present a new age-dating technique that combines gyrochronology with isochrone fitting to infer ages for FGKM main-sequence and subgiant field stars. Gyrochronology and isochrone fitting are each capable of providing relatively precise ages for field stars in certain areas of the Hertzsprung-Russell diagram: gyrochronology works optimally for cool main-sequence stars, and isochrone fitting can provide precise ages for stars near the main-sequence turnoff. Combined, these two age-dating techniques can provide precise and accurate ages for a broader range of stellar masses and evolutionary stages than either method used in isolation. We demonstrate that the position of a star on the Hertzsprung-Russell or color-magnitude diagram can be combined with its rotation period to infer a precise age via both isochrone fitting and gyrochronology simultaneously. We show that incorporating rotation periods with 5% uncertainties into stellar evolution models improves age precision for FGK stars on the main sequence, and can, on average, provide age estimates up to three times more precise than isochrone fitting alone. In addition, we provide a new gyrochronology -2relation, calibrated to the Praesepe cluster and the Sun, that includes a variance model to capture the rotational behavior of stars whose rotation periods do not lengthen with the square-root of time, and parts of the Hertzsprung-Russell diagram where gyrochronology has not been calibrated. This publication is accompanied by an open source Python package, stardate, for inferring the ages of main-sequence and subgiant FGKM stars from rotation periods, spectroscopic parameters and/or apparent magnitudes and parallaxes.

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“…Although the BaSTI theoretical library has been recently updated (Hidalgo et al 2018), we chose to use the original models computed with the "canonical" set-up. This is because the new BaSTI release is still limited to the scaled-solar chemical abundance mixture, while α-enhanced tracks, more appropriate to model Tucana's old population, are currently being calculated (Hidalgo et al, in prep.).…”

Section: Interpreting the Hb Of Tucanamentioning

confidence: 99%

The HST/ACS star formation history of the Tucana dwarf spheroidal galaxy: clues from the horizontal branch

Savino

Tolstoy

Salaris

et al. 2019

A&A

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We report a new star formation history for the Tucana dwarf spheroidal galaxy, obtained from a new look at a deep HST/ACS colourmagnitude diagram. We combined information from the main sequence turn-off and the horizontal branch to resolve the ancient star formation rates on a finer temporal scale than previously possible. We show that Tucana experienced three major phases of star formation, two very close together at ancient times and the last one ending between 6 and 8 Gyr ago. We show that the three discrete clumps of stars on the horizontal branch are linked to the distinct episodes of star formation in Tucana. The spatial distribution of the clumps reveals that each generation of stars presents a higher concentration than the previous one. The simultaneous modelling of the horizontal branch and the main sequence turn-off also allows us to measure the amount of mass lost by red giant branch stars in Tucana with unprecedented precision, confirming dwarf spheroidals to be excellent laboratories to study the advanced evolution of low-mass stars.

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The Updated BaSTI Stellar Evolution Models and Isochrones. I. Solar-scaled Calculations

Cited by 293 publications

References 154 publications

Comparing the Quenching Times of Faint M31 and Milky Way Satellite Galaxies

Comparing the Quenching Times of Faint M31 and Milky Way Satellite Galaxies

Toward Precise Stellar Ages: Combining Isochrone Fitting with Empirical Gyrochronology

The HST/ACS star formation history of the Tucana dwarf spheroidal galaxy: clues from the horizontal branch

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