The Potential Importance of Binary Evolution in Ultraviolet-Optical Spectral Fitting of Early-Type Galaxies

Li, Zhongmu; Mao, Caiyan; Chen, Li; Zhang, Qian; Li, Maocai

doi:10.1088/0004-637x/776/1/37

Cited by 20 publications

(14 citation statements)

References 75 publications

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“…Evolution in close binaries is a channel for formation of a significant fraction of them, since RLOF is able to remove hydrogen envelopes from much lower-mass stars than stellar wind. As WR-stars are important contributors to the UV-light of the galaxies (as well as their lower-mass counterparts — hot subdwarfs), this points to the necessity of including binary evolution effects in the spectrophotometric-population-synthesis models, see, e.g., [419]. …”

Section: Evolutionary Scenario For Compact Binaries With Neutron Starmentioning

confidence: 99%

The Evolution of Compact Binary Star Systems

Постнов

Yungelson

2014

Living Rev. Relativ.

461

382

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We review the formation and evolution of compact binary stars consisting of white dwarfs (WDs), neutron stars (NSs), and black holes (BHs). Mergings of compact-star binaries are expected to be the most important sources for forthcoming gravitational-wave (GW) astronomy. In the first part of the review, we discuss observational manifestations of close binaries with NS and/or BH components and their merger rate, crucial points in the formation and evolution of compact stars in binary systems, including the treatment of the natal kicks, which NSs and BHs acquire during the core collapse of massive stars and the common envelope phase of binary evolution, which are most relevant to the merging rates of NS-NS, NS-BH and BH-BH binaries. The second part of the review is devoted mainly to the formation and evolution of binary WDs and their observational manifestations, including their role as progenitors of cosmologically-important thermonuclear SN Ia. We also consider AM CVn-stars, which are thought to be the best verification binary GW sources for future low-frequency GW space interferometers.

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Section: Evolutionary Scenario For Compact Binaries With Neutron Starmentioning

confidence: 99%

The Evolution of Compact Binary Star Systems

Постнов

Yungelson

2014

Living Rev. Relativ.

461

382

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“…First, despite its (well-deserved) status as a founding stone of modern astrophysics, stellar evolution is still an open business. Rotation in massive stars (Levesque et al 2012), rapid phases during the post-main-sequence evolution of intermediate-mass stars (Maraston 2005), and binarity (Li et al 2013) are examples of phenomena that affect the radiative output of stellar populations, but are still at the forefront of research, and thus prone to uncertainties. A practical example of how incomplete treatment of evolutionary phases affects spectral synthesis analysis is discussed by Koleva et al (2008), Cid Fernandes &Ocvirk (2010).…”

Section: Uncertainties Associated To Evolutionary Synthesis Models: Amentioning

confidence: 99%

Resolving galaxies in time and space

Fernandes

Delgado

García-Benito

et al. 2014

A&A

137

127

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Aims. In a companion paper we have presented many products derived from the application of the spectral synthesis code  to datacubes from the CALIFA survey, including 2D maps of stellar population properties (such as mean ages, mass, and extinction) and 1D averages in the temporal and spatial dimensions. Our goal here is to assess the uncertainties in these products. Methods. Uncertainties associated to noise and spectral shape calibration errors in the data and to the synthesis method were investigated by means of a suite of simulations, perturbing spectra and processing them through our analysis pipelines. The simulations used 1638 CALIFA spectra for NGC 2916, with perturbation amplitudes gauged in terms of the expected errors. A separate study was conducted to assess uncertainties related to the choice of evolutionary synthesis models, the key ingredient in the translation of spectroscopic information into stellar population properties. We compare the results obtained with three different sets of models: the traditional Bruzual & Charlot models, a preliminary update of them, and a combination of spectra derived from the Granada and MILES models. About 10 5 spectra from over 100 CALIFA galaxies were used in this comparison. Results. Noise and shape-related errors at the level expected for CALIFA propagate to uncertainties of 0.10−0.15 dex in stellar masses, mean ages, and metallicities. Uncertainties in A V increase from 0.06 mag for random noise to 0.16 mag for spectral shape errors. Higher-order products such as star formation histories are more uncertain than global properties, but still relatively stable. Owing to the large number statistics of datacubes, spatial averaging reduces uncertainties while preserving information on the history and structure of stellar populations. Radial profiles of global properties, and star formation histories averaged over different regions are much more stable than those obtained for individual spaxels. Uncertainties related to the choice of base models are larger than those associated with data and method. Except for metallicities, which come out very different when fits are performed with the Bruzual & Charlot models, differences in mean age, mass, and metallicity are of the order of 0.15 to 0.25 dex, and 0.1 mag for A V . Spectral residuals are of the order of 1% on average, but with systematic features of up to 4% amplitude. We discuss the origin of these features, most of which are present in both in CALIFA and SDSS spectra.

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“…A more precise measure of the oldest stellar population age might also be a useful discriminant between the He enriched models and alternative binary star evolution models, as the hot stars produced in the latter case need not be extremely old(Han et al 2007;Li et al 2013). …”

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confidence: 99%

Galaxy And Mass Assembly (GAMA): Defining passive galaxy samples and searching for the UV upturn

Phillipps

Ali

Bremer

et al. 2019

Monthly Notices of the Royal Astronomical Society

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We use data from the GAMA and GALEX surveys to demonstrate that the UV upturn, an unexpected excess of ultraviolet flux from a hot stellar component, seen in the spectra of many early-type galaxies, arises from processes internal to individual galaxies with no measurable influence from the galaxies’ larger environment. We first define a clean sample of passive galaxies without a significant contribution to their UV flux from low-level star formation. We confirm that galaxies with the optical colours of red sequence galaxies often have signs of residual star formation, which, without other information, would prevent a convincing demonstration of the presence of UV upturns. However, by including (NUV−u) and WISE (W2–W3) colours, and FUV data where it exists, we can convincingly constrain samples to be composed of non-star-forming objects. Using such a sample, we examine GALEX photometry of low-redshift GAMA galaxies in a range of low-density environments, from groups to the general field, searching for UV upturns. We find a wide range of (NUV−r) colours, entirely consistent with the range seen – and attributed to the UV upturn – in low-redshift red sequence cluster galaxies. The range of colours is independent of group multiplicity or velocity dispersion, with isolated passive galaxies just as likely to have blue UV-to-optical colours, implying significant upturn components, as those in richer groups and in the previous data on clusters. This is supported by equivalent results for (FUV−r) colours which are clear indicators of upturn components.

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The Potential Importance of Binary Evolution in Ultraviolet-Optical Spectral Fitting of Early-Type Galaxies

Cited by 20 publications

References 75 publications

The Evolution of Compact Binary Star Systems

The Evolution of Compact Binary Star Systems

Resolving galaxies in time and space

Galaxy And Mass Assembly (GAMA): Defining passive galaxy samples and searching for the UV upturn

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