Old Stellar Populations. VI. Absorption‐Line Spectra of Galaxy Nuclei and Globular Clusters

Trager, S. C.; Worthey, Guy; Faber, S. M.; Burstein, David; González, J. Jesús

doi:10.1086/313099

Cited by 647 publications

(1,122 citation statements)

References 73 publications

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“…However, as pointed out by Roediger et al (2014), the lack of any correlation between [Mg/Fe] and [Ca/Fe] in GGCs seems to suggest that, while both are indeed α-elements, they are possibly produced in different nucleosynthetic sites. Interestingly, [Ca/Fe] does not seem to directly track [Mg/Fe] in massive galaxies (e.g., Vazdekis et al 1997;Trager et al 1998;Cenarro et al 2003;Thomas et al 2003;Conroy 2013).…”

Section: Galactic Globular Clustersmentioning

confidence: 99%

“…In fact, one of the most important results has been the finding that massive early-type galaxies (ETGs) show an overabundance of [Mg/Fe] (e.g., Peletier 1989;Worthey, Faber & González 1992). Such departure from the solar abundance pattern is generally attributed to short formation time-scales (<1 Gyr) for the bulk of their stellar populations (see the reviews of e.g., Trager et al 1998Trager et al , 2000Renzini 2006;Conroy 2013, and references therein). The Magnesium, an α-element, is ejected into the ISM by type-II supernovae resulting from massive stars on time-scales of ∼10 Myr, whereas most of the iron is released on time-scales of ∼1 Gyr, when SNIa explosions of intermediate-mass stars in binary systems occur.…”

Section: Introductionmentioning

confidence: 99%

“…It is becoming common practice to use these model SEDs with newly developed algorithms that aim at constraining and recovering the SFH by means of full spectrum-fitting approach (e.g., Panter, Heavens & Jimenez 2003, Cid Fernandes et al 2005Ocvirk et al 2006a,b;Chilingarian et al 2007;Koleva et al 2009;Tojeiro et al 2011). This method represents an alternative to the more classical approach of fitting a selected number of linestrength indices (e.g., Trager et al 1998). Furthermore these model SEDs have been used in a variety of applications.…”

Section: Introductionmentioning

confidence: 99%

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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

343

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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Section: Galactic Globular Clustersmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

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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

343

394

View full text Add to dashboard Cite

show abstract

“…To quantify peculiarities of the absorption-line index distributions in the center of NGC 3607, we have calculated azimuthally averaged radial profiles of the indices and have compared them to the 'zerodimensional' and one-dimensional spectral data published earlier by Proctor (2002), Trager et al (1998), and Fisher, Franx, & Illingworth (1996) (Fig. 16).…”

Section: Ngc 3608mentioning

confidence: 99%

Leo II Group: decoupled cores of NGC 3607 and NGC3608

Afanasiev

Сильченко

2007

Astronomical & Astrophysical Transactions

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The kinematics, structure, and stellar population properties in the centers of two brightest early-type galaxies of the Leo II group, NGC 3607 and NGC 3608, are studied by means of integral-field spectroscopy. The kinematically distinct areas in the centers of these galaxies, with radii of 6 ′′ and 5 ′′ respectively, are found also to be chemically distinct. These stellar structures are characterized by enhanced magnesiumline strength in the integrated spectra. However, we have not found any mean stellar age differences between the decoupled cores and their outskirts. Analysis of twodimensional line-of-sight velocity fields reveals systematic turns of kinematical major axes near the nuclei of both galaxies; in NGC 3608 the ionized gas rotates in the orthogonal plane with respect to the stellar component rotation. By taking into account some morphological features, we conclude that both NGC 3607 and NGC 3608 have large triaxial stellar spheroids. We argue that the magnesium-enhanced cores are not circumnuclear disks; instead they resemble rather compact triaxial structures which may be a cause of formation of polar disks around them -a gaseous one in NGC 3608 and a stellar-gaseous one in NGC 3607. In the latter galaxy the star formation is perhaps still proceeding over the polar disk.

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“…For completeness, it has to be mentioned that there exist further more sophisticated stellar population analysis techniques. Depending on the expected complexity of the stellar population mix, one can analyse the data by comparing line ratios, e.g., Lick indices (Worthey et al (1994), Trager et al (1998)), or by comparing with model spectra as calculated with stellar synthesis models. In principle, with the latter method it is possible to reconstruct the full star formation history.…”

Section: Far Infraredmentioning

confidence: 99%

The Structure and Interaction History of Moderate Luminosity Mergers

Hüttemeister¹,

Manthey²

2006

Proc. IAU

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Interaction and merging are the two most important driving forces of galaxy evolution. In contrast to the well studied major mergers of two large gas-rich disk galaxies, which may lead to Ultraluminous Infrared Galaxies (ULIRGs, LFIR>1012 L⊙), mergers between galaxies of unequal mass or a spiral and an elliptical (S+E mergers) are still poorly understood. These moderate luminosity mergers typically have LFIR > 1011 L⊙. Here, we present the results of our multiwavelength study of a sample of such kind of mergers, including interferometric HI and single-dish CO observations, optical and near-infrared imaging as well as optical spectroscopy.

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Old Stellar Populations. VI. Absorption‐Line Spectra of Galaxy Nuclei and Globular Clusters

Cited by 647 publications

References 73 publications

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

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

Leo II Group: decoupled cores of NGC 3607 and NGC3608

The Structure and Interaction History of Moderate Luminosity Mergers

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