Erratum: “Surveying the Agents of Galaxy Evolution in the Tidally Stripped, Low-Metallicity Small Magellanic Cloud (Sage-Smc). Ii. Cool Evolved Stars” (2011, Aj, 142, 103)

Boyer, Martha L.; Srinivasan, S.; Loon, Jacco Th. van; McDonald, Iain; Meixner, Margaret; Zaritsky, Dennis; Kemper, F.; Babler, B.; Block, M.; Bracker, S.; Engelbracht, C. W.; Hora, J. L.; Indebetouw, R.; Meade, M. R.; Misselt, K. A.; Robitaille, Thomas; Sewiło, M.; Shiao, Bernie; Whitney, B. A.

doi:10.1088/0004-6256/143/5/127

Cited by 67 publications

(228 citation statements)

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“…However, there are a couple of points that we have to take into account. First, stars labelled as RSGs in Boyer et al (2011) extend down to m K S = 12.5, a magnitude that translates to M K S ∼ −6.5 at the distance of the SMC, hardly compatible with what is expected for this population (see e.g. Elias et al 1985).…”

Section: Completeness Of the Samplementioning

confidence: 84%

“…8. At face value, this plot seems to indicate that we are missing a large fraction of the potential RSGs: of more than 3000 putative candidates flagged by Boyer et al (2011) in the SMC, we have only observed around 200. However, there are a couple of points that we have to take into account.…”

Section: Completeness Of the Samplementioning

confidence: 88%

“…We can check this by comparing our a priori photometric selection with other similar programs. Of those available, the most complete and deep is Boyer et al (2011), with the added advantage that their classification is based on the NIR and MIR photometry of their sources.…”

Section: Completeness Of the Samplementioning

confidence: 99%

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A new survey of cool supergiants in the Magellanic Clouds

González-Fernández

Dorda

Negueruela

et al. 2015

A&A

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Aims. In this study we conduct a pilot program aimed at the red supergiant population of the Magellanic Clouds. We intend to extend the current known sample to the unexplored low end of the brightness distribution of these stars, building a more representative dataset with which to extrapolate their behaviour to other Galactic and extra-galactic environments. Methods. We select candidates using only near infrared photometry, and with medium resolution multi-object spectroscopy, we perform spectral classification and derive their line-of-sight velocities, confirming the nature of the candidates and their membership in the clouds. Results. Around two hundred new red supergiants have been detected, hinting at a yet to be observed large population. Using nearand mid-infrared photometry we study the brightness distribution of these stars, the onset of mass-loss, and the effect of dust in their atmospheres. Based on this sample, new a priori classification criteria are investigated, combining mid-and near-infrared photometry to improve the observational efficiency of similar programs to this.

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Section: Completeness Of the Samplementioning

confidence: 84%

Section: Completeness Of the Samplementioning

confidence: 88%

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A new survey of cool supergiants in the Magellanic Clouds

González-Fernández

Dorda

Negueruela

et al. 2015

A&A

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“…Vijh et al 2009;Boyer et al 2011) follow the scheme introduced by Blum et al (2006) to divide the found AGB objects into three distinct classes tagged "O-rich", "C-rich", and "Extreme". Recently, efforts were made to interpret the SEDs of these objects (defined by photometry compiled from various catalogues; cf.…”

Section: Extremely Reddened C Starsmentioning

confidence: 99%

Synthetic photometry for carbon-rich giants

Nowotny¹,

Aringer²,

Höfner

et al. 2013

A&A

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Late-type giant stars in the evolutionary stage of the asymptotic giant branch increasingly lose mass via comparatively slow but dense stellar winds. Not only do these evolved red giants contribute in this way to the enrichment of the surrounding interstellar medium, but the outflows also have a substantial influence on the spectro-photometric appearance of such objects. In the case of carbon-rich atmospheric chemistries, the developing cool circumstellar envelopes contain dust grains mainly composed of amorphous carbon. With increasing mass-loss rates, this leads to more and more pronounced circumstellar reddening. With the help of model calculations we aim at reproducing the observational photometric findings for a large sample of well-characterised galactic C-type Mira variables losing mass at different rates. We used dynamic model atmospheres, describing the outer layers of C-rich Miras, which are severly affected by dynamic effects. Based on the resulting structures and under the assumptions of chemical equilibrium as well as LTE, we computed synthetic spectra and synthetic broad-band photometry (Johnson-Cousins-Glass BVRIJHKL M). A set of five representative models with different stellar parameters describes a sequence from less to more evolved objects with steadily increasing mass-loss rates. This allowed us to study the significant influence of circumstellar dust on the spectral energy distributions and the (amplitudes of) lightcurves in different filters. We tested the photometric properties (mean NIR magnitudes, colours, and amplitudes) and other characteristics of the models (mass-loss rates, periods, and bolometric corrections) by comparing these with the corresponding observational data adopted from the literature. Using different kinds of diagrams we illustrate where the models are located in a supposed evolutionary sequence defined by observed C-type Mira samples. Based on comparisons of galactic targets with empirical relations derived for C stars in the Large Magellanic Cloud we discuss the relevance of metallicity and excess carbon (C-O) for the development of dust-driven winds. Having investigated the dynamic model atmospheres from different (mainly photometric) perspectives, we conclude that our modelling approach (meaning the combination of numerical method and a suitable choice of model parameters) is able to describe C-rich long-period variables over a wide range of mass-loss rates, i.e., from moderately pulsating objects without any dusty wind to highly dust-enshrouded Carbon Miras. Thus, we can trace the observed sequence of C-type Miras, which is mainly determined by the mass loss.

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“…For example, such comparisons have allowed primarily to estimate the extension of the third dredge-up (hereinafter TDU), i.e. the inwards penetration of the bottom of the convective envelope in the phase following each thermal pulse (Izzard et al 2004;Girardi & Marigo 2007;Groenewegen et al 2007;Riebel et al 2010Riebel et al , 2012Srinivasan et al 2009Srinivasan et al , 2011Boyer et al 2011Boyer et al , 2012. More recent studies were focused on the dust production by AGB stars in the MC and the characterisation of the most obscured sources (Dell'Agli et al 2014, 2015aVentura et al 2015.…”

Section: Introductionmentioning

confidence: 99%

Planetary nebulae in the Small Magellanic Cloud

Ventura

Stanghellini

Criscienzo

et al. 2016

Mon. Not. R. Astron. Soc.

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We analyse the planetary nebulae (PNe) population of the Small Magellanic Cloud (SMC), based on evolutionary models of stars with metallicities in the range 10 −3 ≤ Z ≤ 4 × 10 −3 and mass 0.9 M < M < 8 M , evolved through the asymptotic giant branch (AGB) phase. The models used account for dust formation in the circumstellar envelope. To characterise the PNe sample of the SMC, we compare the observed abundances of the various species with the final chemical composition of the AGB models: this study allows us to identify the progenitors of the PNe observed, in terms of mass and chemical composition. According to our interpretation, most of the PNe descend from low-mass (M < 2M ) stars, which become carbon rich, after experiencing repeated third dredge-up episodes, during the AGB phase. A fraction of the PNe showing the signature of advanced CNO processing are interpreted as the progeny of massive AGB stars, with mass above ∼ 6M , undergoing strong hot bottom burning. The differences with the chemical composition of the PNe population of the Large Magellanic Cloud (LMC) is explained on the basis of the diverse star formation history and age-metallicity relation of the two galaxies. The implications of the present study for some still highly debated points regarding the AGB evolution are also commented.

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Erratum: “Surveying the Agents of Galaxy Evolution in the Tidally Stripped, Low-Metallicity Small Magellanic Cloud (Sage-Smc). Ii. Cool Evolved Stars” (2011, Aj, 142, 103)

Cited by 67 publications

References 0 publications

A new survey of cool supergiants in the Magellanic Clouds

A new survey of cool supergiants in the Magellanic Clouds

Synthetic photometry for carbon-rich giants

Planetary nebulae in the Small Magellanic Cloud

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