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

Vazdekis, Alexandre; Coelho, P.; Cassisi, S.; Ricciardelli, E.; Falcón-Barroso, J.; Sánchez‐Blázquez, P.; Barbera, F. La; Beasley, Michael A.; Pietrinferni, A.

doi:10.1093/mnras/stv151

Cited by 320 publications

(412 citation statements)

References 212 publications

(430 reference statements)

Supporting

Mentioning

394

Contrasting

Unclassified

Order By: Relevance

“…This is a hint that the star-formation timescale is shorter in the outer regions of discs. This result is promising but it should be tested against a larger sample of galaxy discs and when the new α-enhanced synthetic population models (Vazdekis et al 2015) will be released.…”

Section: Discussionmentioning

confidence: 96%

Study of the stellar population properties in the discs of ten spiral galaxies

Morelli¹,

Corsini²,

Pizzella³

et al. 2015

Mon. Not. R. Astron. Soc.

View full text Add to dashboard Cite

We investigated the properties of the stellar populations in the discs of a sample of ten spiral galaxies. Our analysis focused on the galaxy region where the disc contributes more than 95 per cent of total surface brightness in order to minimise the contamination of the bulge and bar.The luminosity-weighted age and metallicity were obtained by fitting the galaxy spectra with a linear combination of stellar population synthesis models, while the total overabundance of α-elements over iron was derived by measuring the line-strength indices.Most of the sample discs display a bimodal age distribution and they are characterised by a total [α/Fe] enhancement ranging from solar and supersolar. We interpreted the age bimodality as due to the simultaneous presence of both a young (Age 4 Gyr) and an old (Age > 4 Gyr) stellar population. The old stellar component usually dominates the disc surface brightness and its light contribution is almost constant within the observed radial range. For this reason, no age gradient is observed in half of the sample galaxies. The old component is slightly more metal poor than the young one. The metallicity gradient is negative and slightly positive in the old and young components, respectively.These results are in agreement with an inside-out scenario of disc formation and suggest a reduced impact of the radial migration on the stellar populations of the disc. The young component could be the result of a second burst of star formation in gas captured from the environment.

show abstract

Section: Discussionmentioning

confidence: 96%

Study of the stellar population properties in the discs of ten spiral galaxies

Morelli¹,

Corsini²,

Pizzella³

et al. 2015

Mon. Not. R. Astron. Soc.

View full text Add to dashboard Cite

show abstract

“…A full spectral fitting analysis was performed using the starlight code and a combination of composite stellar populations (CSP) spectra derived with the models of González Delgado et al (2005) and Vazdekis et al (2015). This base comprises 18 logarithmically spaced age bins centered at ages from 0.00245 to 11.50 Gyr, and 8 metallicities from log Z/Z = −2.28 to +0.40.…”

Section: Discussionmentioning

confidence: 99%

“…We shall say, for instance, that a stellar age of 4 Gyr corresponds to 4 Gyr in lookback time or z ∼ 0.4. 5 Due to limitations in the number of O and B stars in the MILES library (Sánchez-Blázquez et al 2006), the Vazdekis et al (2015) models are unsafe for t ≤ 63 Myr, and in particular for metallicities below half solar; further, BaSTI isochrones are not computed for ages younger than 10 Myr. In contrast, González Delgado et al (2005) are well optimized for young ages.…”

Section: A Note On Ages Lookback Times and Redshiftsmentioning

confidence: 99%

See 1 more Smart Citation

Spatially-resolved star formation histories of CALIFA galaxies

Delgado

Pérez

Fernandes

et al. 2017

A&A

View full text Add to dashboard Cite

This paper presents the spatially resolved star formation history (SFH) of nearby galaxies with the aim of furthering our understanding of the different processes involved in the formation and evolution of galaxies. To this end, we apply the fossil record method of stellar population synthesis to a rich and diverse data set of 436 galaxies observed with integral field spectroscopy in the CALIFA survey. The sample covers a wide range of Hubble types, with stellar masses ranging from M ∼ 10 9 to 7 × 10 11 M . Spectral synthesis techniques are applied to the datacubes to retrieve the spatially resolved time evolution of the star formation rate (SFR), its intensity (Σ SFR ), and other descriptors of the 2D-SFH in seven bins of galaxy morphology (E, S0, Sa, Sb, Sbc, Sc, and Sd), and five bins of stellar mass. Our main results are: (a) Galaxies form very fast independently of their current stellar mass, with the peak of star formation at high redshift (z > 2). Subsequent star formation is driven by M and morphology, with less massive and later type spirals showing more prolonged periods of star formation. (b) At any epoch in the past the SFR is proportional to M , with most massive galaxies having the highest absolute (but lowest specific) SFRs. (c) While nowadays Σ SFR is similar for all spirals, and significantly lower in early type galaxies (ETG), in the past Σ SFR scales well with morphology. The central regions of today's ETGs are where Σ SFR reached the highest values (> 10 3 M Gyr −1 pc −2 ), similar to those measured in high redshift star forming galaxies. (d) The evolution of Σ SFR in Sbc systems matches that of models for Milky-Way-like galaxies, suggesting that the formation of a thick disk may be a common phase in spirals at early epochs. (e) The SFR and Σ SFR in outer regions of E's and S0's show that they have undergone an extended phase of growth in mass between z = 2 and 0.4. The mass assembled in this phase is in agreement with the two-phase scenario proposed for the formation of ETG. (f) Evidence of an early and fast quenching is found only in the most massive (M > 2 × 10 11 M ) E galaxies of the sample, but not in spirals of similar mass, suggesting that halo-quenching is not the main mechanism for the shut down of star formation in galaxies. Less massive E and disk galaxies show more extended SFHs and a slow quenching. (g) Evidence of fast quenching is also found in the nuclei of ETG and early spirals, with SFR and Σ SFR indicating that they can be the relic of the "red nuggets" detected at high redshift.

show abstract

“…In extragalactic studies they are, for instance, at the heart of evolutionary stellar population synthesis models, i.e., the modeling of the spectral energy distribution (SED) emitted by evolving stellar populations (e.g., Leitherer et al 1999;Bruzual & Charlot 2003;Delgado et al 2005;Coelho et al 2007;Vazdekis et al 2015).…”

Section: Application In Stellar Population Synthesismentioning

confidence: 99%

A Grid of Synthetic Spectra for Hot DA White Dwarfs and Its Application in Stellar Population Synthesis

Levenhagen

Diaz

Coelho

et al. 2017

ApJS

View full text Add to dashboard Cite

In this work we present a grid of LTE and non-LTE synthetic spectra of hot DA white dwarfs (WDs). In addition to its usefulness for the determination of fundamental stellar parameters of isolated WDs and in binaries, this grid will be of interest for the construction of theoretical libraries for stellar studies from integrated light. The spectral grid covers both a wide temperature and gravity range, with 17,000 KT eff 100,000 K and 7.0 g log 9.5. The stellar models are built for pure hydrogen and the spectra cover a wavelength range from 900 Å to 2.5 μm. Additionally, we derive synthetic HST/ACS, HST/WFC3, Bessel UBVRI, and SDSS magnitudes. The grid was also used to model integrated spectral energy distributions of simple stellar populations and our modeling suggests that DAs might be detectable in ultraviolet bands for populations older than ∼8 Gyr.

show abstract

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

Cited by 320 publications

References 212 publications

Study of the stellar population properties in the discs of ten spiral galaxies

Study of the stellar population properties in the discs of ten spiral galaxies

Spatially-resolved star formation histories of CALIFA galaxies

A Grid of Synthetic Spectra for Hot DA White Dwarfs and Its Application in Stellar Population Synthesis

Contact Info

Product

Resources

About