The Dartmouth Stellar Evolution Database

Dotter, Aaron; Chaboyer, Brian; Jevremović, D.; Kostov, Veselin B.; Baron, E.; Ferguson, Jason W.

doi:10.1086/589654

Cited by 1,712 publications

(2,286 citation statements)

References 63 publications

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“…The brightest objects at F606W = 22.5 - 23.5 represent the newly formed remnants of progenitor hydrogen--burning stars that just exhausted their nuclear fuel. The mass of the progenitor stars can be calculated accurately from stellar evolution models since the age of the population is well measured 9 . For Messier 4, this mass is M INITIAL = 0.802 (+0.007; --0.011) M SUN .…”

mentioning

confidence: 99%

The age of the Milky Way inner halo

Kalirai

2012

Nature

104

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The Milky Way galaxy is observed to have multiple components with distinct properties, such as the bulge, disk, and halo. Unraveling the assembly history of these populations provides a powerful test to the theory of galaxy formation and evolution, but is often restricted due to difficulties in measuring accurate stellar ages for low mass, hydrogen--burning stars. 1,2 Unlike these progenitors, the "cinders" of stellar evolution, white dwarf stars 3 , are remarkably

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mentioning

confidence: 99%

The age of the Milky Way inner halo

Kalirai

2012

Nature

104

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“…4, there is some disagreement between our own results and those of Pecaut, Mamajek, & Bubar (2012). However, we note that the use of Pecaut, Table 2. combination of empirical isochrones and the models of Dotter et al (2008) and found an age for USco of 11±1 Myr. As seen in Fig.…”

Section: Evolutionary Status Of the Investigated Starsmentioning

confidence: 99%

Keplerobservations of A–F pre-main-sequence stars in Upper Scorpius: discovery of six new δ Scuti and one γ Doradus stars

Ripepi¹,

Balona²,

Catanzaro³

et al. 2015

Mon. Not. R. Astron. Soc.

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We present light curves and periodograms for 27 stars in the young Upper Scorpius association (age=11 ± 1 Myr) obtained with the Kepler spacecraft. This association is only the second stellar grouping to host several pulsating pre-main sequence (PMS) stars which have been observed from space.From an analysis of the periodograms, we identify six δ Scuti variables and one γ Doradus star. These are most likely PMS stars or else very close to the zero-age main sequence. Four of the δ Scuti variables were observed in short-cadence mode, which allows us to resolve the entire frequency spectrum. For these four stars, we are able to infer some qualitative information concerning their ages. For the remaining two δ Scuti stars, only long-cadence data are available, which means that some of the frequencies are likely to be aliases. One of the stars appears to be a rotational variable in a hierarchical triple system. This is a particularly important object, as it allows the possibility of an accurate mass determination when radial velocity observations become available. We also report on new high-resolution echelle spectra obtained for some of the stars of our sample.

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“…7 A comparison among these population synthesis models and observations has been already performed by Noel et al (2013), and it was found that these models disagree -being in general too red -with the integrated colours of superclusters for ages between ∼ 10 8 and ∼ 10 9 years. than those of Pols et al (1995), which were implemented in Vazdekis et al (1996), and those of Dotter et al (2008) (see also An et al 2009). As their temperatures are higher the Padova00 VLM stars are brighter than the ones we employ here for the BASTI models (see figure 5 in Vazdekis et al 2012).…”

Section: Isochronesmentioning

confidence: 99%

Evolutionary stellar population synthesis with MILES – II. Scaled-solar and α-enhanced models

Vazdekis

Coelho

Cassisi

et al. 2015

Monthly Notices of the Royal Astronomical Society

332

394

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We present models that predict spectra of old-and intermediate-aged stellar populations at 2.51Å (FWHM) with varying [α/Fe] abundance. The models are based on the MILES library and on corrections from theoretical stellar spectra. The models employ recent [Mg/Fe] determinations for the MILES stars and BaSTI scaled-solar and α-enhanced isochrones. We compute models for a suite of IMF shapes and slopes, covering a wide age/metallicity range. Using BASTI, we also compute "base models" matching The Galactic abundance pattern. We confirm that the α-enhanced models show a flux excess with respect to the scaled-solar models blue-ward ∼4500Å, which increases with age and metallicity. We also confirm that both [MgFe] and [MgFe] ′ indices are [α/Fe]-insensitive. We show that the sensitivity of the higher order Balmer lines to [α/Fe] resides in their pseudo-continua, with narrower index definitions yielding lower sensitivity. We confirm that the α-enhanced models yield bluer (redder) colours in the blue (red) spectral range. To match optical colours of massive galaxies we require both α-enhancement and a bottom-heavy IMF. The comparison of Globular Cluster line-strengths with our predictions match the [Mg/Fe] determinations from their individual stars. We obtain good fits to both full spectra and indices of galaxies with varying [α/Fe]. Using thousands of SDSS galaxy spectra we obtain a linear relation between a proxy for the abundance,

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The Dartmouth Stellar Evolution Database

Cited by 1,712 publications

References 63 publications

The age of the Milky Way inner halo

The age of the Milky Way inner halo

Keplerobservations of A–F pre-main-sequence stars in Upper Scorpius: discovery of six new δ Scuti and one γ Doradus stars

Evolutionary stellar population synthesis with MILES – II. Scaled-solar and α-enhanced models

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