The Dust Budget of the Small Magellanic Cloud: Are Asymptotic Giant Branch Stars the Primary Dust Source at Low Metallicity?

Boyer, Martha L.; Srinivasan, S.; Riebel, D.; McDonald, Iain; Loon, Jacco Th. van; Clayton, Geoffrey C.; Gordon, K. D.; Meixner, M.; Sargent, Benjamin; Sloan, G. C.

doi:10.1088/0004-637x/748/1/40

Cited by 140 publications

(218 citation statements)

References 73 publications

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“…A number of recent studies have estimated the global dust production rate by evolved stars based on the SAGE-LMC program summarised in Table 1. Srinivasan et al (2009), Boyer et al (2012 and Riebel et al (2012) used the same data set based on SAGE-LMC point sources complemented by optical photometry from the Magellanic Clouds Photometric Survey (MCPS; Harris & Zaritsky 2009) and near-IR photometry from the Two Micron All Sky Survey (Skrutskie et al 2006) or the InfraRed Survey Facility (Kato et al 2007). The differences in their derived DPR arise from various source classifications and approaches outlined below.…”

Section: Observational Studies Of Dust Input From Agb Stars In the Lmcmentioning

confidence: 99%

“…During recent years IR dust emission from stellar sources in the LMC has been extensively studied in a number of surveys (e.g., Cioni et al 2000;Egan et al 2001;Meixner et al 2006;Skrutskie et al 2006;Ita et al 2008;Blum et al 2006). These studies have permitted, for the first time, measurements of the dust production rate (DPR) by stars for the entire galaxy (Matsuura et al 2009;Srinivasan et al 2009;Boyer et al 2012;Riebel et al 2012). This can be used to test and constrain models of dust evolution at the present time.…”

Section: Introductionmentioning

confidence: 99%

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Dust input from AGB stars in the Large Magellanic Cloud

Zhukovska

Henning

2013

A&A

112

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Aims. The dust-forming population of AGB stars and their input to the interstellar dust budget of the Large Magellanic Cloud (LMC) are studied with evolutionary dust models with the main goals (1) to investigate how the amount and composition of dust from AGB stars vary over the galactic history; (2) to characterise the mass and metallicity distribution of the present population of AGB stars; (3) to quantify the contribution of AGB stars of different mass and metallicity to the present stardust population in the interstellar medium (ISM). Methods. We used models of the stardust lifecycle in the ISM developed and tested for the solar neighbourhood. The first global spatially resolved reconstruction of the star formation history of the LMC from the Magellanic Clouds Photometric Survey was employed to calculate the stellar populations in the LMC. Results. The dust input from AGB stars is dominated by carbon grains from stars with masses 4 M almost during the entire history of the LMC. The production of silicate, silicon carbide, and iron dust is delayed until the ISM is enriched to about half the present metallicity in the LMC. For the first time, theoretically calculated dust production rates of AGB stars are compared with those derived from infrared observations of AGB stars for the entire galaxy. We find good agreement within scatter of various observational estimates. We show that the majority of silicate and iron grains in the present stardust population originate from a small population of intermediate-mass stars consisting of only 4% of the total number of stars, whereas in the solar neighbourhood they originate from low-mass stars. With models of the lifecycle of stardust grains in the ISM we confirm the strong discrepancy between dust input from stars and the existing interstellar dust mass in the LMC reported previously.

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Section: Observational Studies Of Dust Input From Agb Stars In the Lmcmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

Dust input from AGB stars in the Large Magellanic Cloud

Zhukovska

Henning

2013

A&A

112

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“…The silicate emission feature, low dust continuum, and relatively low luminosity (compared to RSGs) in the planetary nebula NGC 6804 suggests that source #12 may be a planetary nebula around an O-star (Bilikova et al 2012;Weidmann & Gamen 2011), or a dusty WR star. The shallow long-wavelength spectral energy distribution (SED) is also reminiscent of extreme-AGB stars, which are usually carbon-rich (see Boyer et al 2012, and references therein).…”

Section: A94 Page 8 Of 13mentioning

confidence: 99%

“…For metallicities as low as 1/200 Z , stars might take as short as 100 Myr to evolve from the zero-age main sequence to the AGB (Ventura et al 2002;Herwig 2004). Boyer et al (2012) found that AGBs produce most of the dust from cool evolved stars in the metal-poor Small Magellanic Cloud (SMC, 0.2 Z ), but they argue that other dust sources, such as growth from existing grains, are necessary to explain the total dust mass budget. Alternatively, it is largely debated whether cosmic dust abundance can be reconciled with Appendix A is available in electronic form at http://www.aanda.org SN dust (e.g., Li et al 2008;Maiolino et al 2004), as measurements of the dust produced by a single SN vary dramatically (10 −3 M up to 0.5 M ; e.g., Stanimirovic et al 2005;Matsuura et al 2011).…”

Section: Introductionmentioning

confidence: 99%

Oxygen-rich dust production in IC 10

Lebouteiller¹,

Sloan²,

Groenewegen³

et al. 2012

A&A

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Context. We report the detection of oxygen-rich circumstellar envelopes in stars of the nearby (700 kpc) starburst galaxy IC 10. The star-formation history and the chemical environment of this galaxy make it an ideal target to observe dust production by massive stars in a metal-poor environment. Aims. The goal of this study is to identify oxygen-rich stars in IC 10 and to constrain their nature between asymptotic giant branch stars (AGBs), red supergiants (RSGs), and other bright infrared sources. We examine the mass-loss rates of the stars and compare to results obtained for the Magellanic Clouds. Our objectives are to (1) assess whether RSGs can be significant dust producers in IC 10, and (2), solve the discrepancy between the star-formation history of IC 10 and the relatively low number of RSGs detected in the optical. Methods. We search for silicate dust in emission by using the spectral map observed with the Infrared Spectrograph on board the Spitzer Space Telescope. The optical (UBVRI) and infrared (JHK, Spitzer/IRAC and Spitzer/MIPS) photometry are used to assert the membership of the stars to IC 10 and distinguish between AGBs and RSGs. Radiative models are used to infer mass-loss rates and stellar luminosities. Results. The luminosity and colors of at least 9 silicate emission sources are consistent with stars within IC 10. Furthermore, the photometry of 2 of these sources is consistent with RSGs. We derive dust mass-loss rates similar to the values found in the Magellanic Clouds. Accounting for the sample completeness, RSGs are not important contributors to the dust mass budget in IC 10.

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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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The Dust Budget of the Small Magellanic Cloud: Are Asymptotic Giant Branch Stars the Primary Dust Source at Low Metallicity?

Cited by 140 publications

References 73 publications

Dust input from AGB stars in the Large Magellanic Cloud

Dust input from AGB stars in the Large Magellanic Cloud

Oxygen-rich dust production in IC 10

Planetary nebulae in the Small Magellanic Cloud

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