MILES SSP Models

Vazdekis, Alexandre; Sánchez‐Blázquez, P.; Falcón-Barroso, J.; Cenarro, A. J.; Beasley, Michael A.; Cardiel, N.; Gorgas, J.; Peletier, Reynier F.

doi:10.1017/s174392131000253x

Cited by 223 publications

(409 citation statements)

References 24 publications

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“…The accuracy of the emission line flux measurements is ultimately tied to the accuracy with which we can fit and subtract the underlying stellar absorption features. The stellar at University of Durham on October 6, 2016 http://mnras.oxfordjournals.org/ Downloaded from continuum in each spectrum has been modelled using pPXF to fit a combination of simple stellar population models (SSP) from the MILES library (Vazdekis et al 2010) as well as an 8 th degree multiplicative polynomial to account for any residual flux calibration errors and the reddening effect of dust. Strong emission lines were masked during the fitting process and weaker emission lines were clipped by setting the clean keyword when invoking pPXF.…”

Section: Emission Line Fluxesmentioning

confidence: 99%

The SAMI Galaxy Survey: spatially resolving the environmental quenching of star formation in GAMA galaxies

Schaefer

Croom

Allen

et al. 2016

Mon. Not. R. Astron. Soc.

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We use data from the Sydney-AAO Multi-Object Integral Field Spectrograph (SAMI) Galaxy Survey and the Galaxy And Mass Assembly (GAMA) survey to investigate the spatially-resolved signatures of the environmental quenching of star formation in galaxies. Using dust-corrected measurements of the distribution of Hα emission we measure the radial profiles of star formation in a sample of 201 star-forming galaxies covering three orders of magnitude in stellar mass (M * ; 10 8.1 -10 10.95 M ) and in 5 th nearest neighbour local environment density (Σ 5 ; 10 −1.3 -10 2.1 Mpc −2 ). We show that star formation rate gradients in galaxies are steeper in dense (log 10 (Σ 5 /Mpc 2 ) > 0.5) environments by 0.58 ± 0.29 dex r e −1 in galaxies with stellar masses in the range 10 10 < M * /M < 10 11 and that this steepening is accompanied by a reduction in the integrated star formation rate. However, for any given stellar mass or environment density the star-formation morphology of galaxies shows large scatter. We also measure the degree to which the star formation is centrally concentrated using the unitless scaleradius ratio (r 50,Hα /r 50,cont ), which compares the extent of ongoing star formation to previous star formation. With this metric we find that the fraction of galaxies with centrally concentrated star formation increases with environment density, from ∼ 5 ± 4% in low-density environments (log 10 (Σ 5 /Mpc 2 ) < 0.0) to 30 ± 15% in the highest density environments (log 10 (Σ 5 /Mpc 2 ) > 1.0). These lines of evidence strongly suggest that with increasing local environment density the star formation in galaxies is suppressed, and that this starts in their outskirts such that quenching occurs in an outside-in fashion in dense environments and is not instantaneous.

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Section: Emission Line Fluxesmentioning

confidence: 99%

The SAMI Galaxy Survey: spatially resolving the environmental quenching of star formation in GAMA galaxies

Schaefer

Croom

Allen

et al. 2016

Mon. Not. R. Astron. Soc.

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“…We use the University of Lyon Spectroscopic analysis Software (ULySS) (Koleva et al 2009) to obtain a non-linear χ 2 -minimization against SSP (or a linear combination of more than one SSP) models convolved with the internal kinematics of the galaxy. We use two sets of high-resolution stellar population models, those of Vazdekis et al (2010) Emission lines (if present) are masked, as even weak emission lines can fill-in important absorption features like the Balmer lines and will lead to overestimated ages. The rest of the spectrum is then used to determine the best fit to the stellar population models.…”

Section: Stellar Populationsmentioning

confidence: 99%

“…metal-rich in general (see Loubser et al 2009 for stellar populations of nearby BCGs), and the measured metallicity is frequently limited by the upper limit of where the empirical stellar population models ([Fe/H] = 0.2 dex in Vazdekis/MILES models using solar-scaled Padova (Girardi et al 2000) isochrones) are considered reliable (Vazdekis et al 2010). As mentioned in section 3, we do not extrapolate by including corrections from computationally-derived model atmospheres, as this introduces uncertainty and will not influence the detection of a younger stellar component.…”

Section: Effect Of Uncertainty In the Imf And Metal Abundancesmentioning

confidence: 99%

The regulation of star formation in cool-core clusters: imprints on the stellar populations of brightest cluster galaxies

Loubser

Babul

Hoekstra

et al. 2015

Mon. Not. R. Astron. Soc.

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A fraction of brightest cluster galaxies (BCGs) shows bright emission in the UV and the blue part of the optical spectrum, which has been interpreted as evidence of recent star formation. Most of these results are based on the analysis of broadband photometric data. Here, we study the optical spectra of a sample of 19 BCGs hosted by X-ray luminous galaxy clusters at 0.15 < z < 0.3, a subset from the Canadian Cluster Comparison Project (CCCP) sample. We identify plausible star formation histories of the galaxies by fitting Simple Stellar Populations (SSPs) as well as composite populations, consisting of a young stellar component superimposed on an intermediate/old stellar component, to accurately constrain their star formation histories. We detect prominent young (∼ 200 Myr) stellar populations in 4 of the 19 galaxies. Of the four, the BCG in Abell 1835 shows remarkable A-type stellar features indicating a relatively large population of young stars, which is extremely unusual even amongst star forming BCGs. We constrain the mass contribution of these young components to the total stellar mass to be typically between 1% to 3%, but rising to 7% in Abell 1835. We find that the four of the BCGs with strong evidence for recent star formation (and only these four galaxies) are found within a projected distance of 5 kpc of their host cluster's X-ray peak, and the diffuse, X-ray gas surrounding the BCGs exhibit a ratio of the radiative cooling-to-free-fall time (t c /t ff ) of ≤ 10. These are also some of the clusters with the lowest central entropy. Our results are consistent with the predictions of the precipitation-driven star formation and AGN feedback model, in which the radiatively cooling diffuse gas is subject to local thermal instabilities once the instability parameter t c /t ff falls below ∼ 10, leading to the condensation and precipitation of cold gas. The number of galaxies in our sample where the host cluster satisfies all the criteria for recent and ongoing star formation is small, but their stellar populations suggest a timescale for star formation to restart of the order of ∼ 200 Myrs.

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“…We use the stellar population models of Vazdekis et al (2010), based on the MILES stellar library (Sánchez-Blázquez et al 2006), to estimate the ages and metallicities of galaxies in our sample. The Vazdekis et al (2010) We also considered the stellar population models of PEGASE-HR (Le Borgne et al 2004) coupled to the ELODIE (Prugniel et al 2007) stellar library.…”

Section: Stellar Population Modelsmentioning

confidence: 99%

“…The Vazdekis et al (2010) We also considered the stellar population models of PEGASE-HR (Le Borgne et al 2004) coupled to the ELODIE (Prugniel et al 2007) stellar library. These models are known for their high spectral resolution (0.55 Å) and for allowing the user to choose the initial mass function along with other physical ingredients.…”

Section: Stellar Population Modelsmentioning

confidence: 99%

The accretion histories of brightest cluster galaxies from their stellar population gradients

Oliva-Altamirano

Brough

Jimmy

et al. 2015

Monthly Notices of the Royal Astronomical Society

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We analyse the spatially-resolved stellar populations of 9 local (z < 0.1) Brightest Cluster Galaxies (BCGs) observed with VIMOS in IFU mode. Our sample is composed of 7 slowrotating and 2 fast-rotating BCGs. We do not find a connection between stellar kinematics and stellar populations in this small sample. The BCGs have shallow metallicity gradients (medianand a wide range of central ages (from 5 to 15 Gyr). We propose that the reason for this is diverse evolutionary paths in BCGs. 67 per cent of the sample (6/9) show ∼ 7 Gyr old central ages, which reflects an active accretion history, and 33 per cent of the sample (3/9) have central ages older than 11 Gyr, which suggest no star formation since z = 2. The BCGs show similar central stellar populations and stellar population gradients to early-type galaxies of similar mass (M dyn > 10 11.3 M ) from the ATLAS 3D survey (median [Z/H] = 0.04 ± 0.07, ∆[Z/H] = −0.19 ± 0.1). However, massive early-type galaxies from ATLAS 3D have consistently old ages (median Age = 12.0 ± 3.8 Gyr). We also analyse the close massive companion galaxies of two of the BCGs. These galaxies have similar stellar populations to their respective BCGs.

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MILES SSP Models

Cited by 223 publications

References 24 publications

The SAMI Galaxy Survey: spatially resolving the environmental quenching of star formation in GAMA galaxies

The SAMI Galaxy Survey: spatially resolving the environmental quenching of star formation in GAMA galaxies

The regulation of star formation in cool-core clusters: imprints on the stellar populations of brightest cluster galaxies

The accretion histories of brightest cluster galaxies from their stellar population gradients

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