Obscured AGB Stars in the LMC

Loon, Jacco Th. van; Zijlstra, A. A.; Whitelock, Patricia; Groenewegen, M. A. T.; Loup, C.; Hekkert, P. te Lintel; Trams, N. R.; Waters, L. B. F. M.

doi:10.1007/978-94-011-5076-7_67

Cited by 29 publications

(40 citation statements)

References 7 publications

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“…We found that the LMC Miras clustered in two regions in the observed color-color diagram as shown in Figure 4. Most O-rich Miras (blue circles) are centered at [0.345 ±0.005 , 0.780 ±0.006 ], although we note that our sample does not contain some previously-known O-rich LMC Miras that are very red (van Loon et al 1998;Whitelock et al 2003). The C-rich Miras (red pluses) are located along a narrow strip.…”

Section: Color Excesses Of Mirasmentioning

confidence: 88%

Large Magellanic Cloud Near-infrared Synoptic Survey. V. Period–Luminosity Relations of Miras

Yuan¹,

Macri²,

He³

et al. 2017

101

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We study the near-infrared properties of 690 Mira candidates in the central region of the Large Magellanic Cloud, based on time-series observations at JHK s . We use densely-sampled I-band observations from the OGLE project to generate template light curves in the near infrared and derive robust mean magnitudes at those wavelengths. We obtain near-infrared Period-Luminosity relations for Oxygen-rich Miras with a scatter as low as 0.12 mag at K s . We study the Period-Luminosity-Color relations and the color excesses of Carbon-rich Miras, which show evidence for a substantially different reddening law.

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Section: Color Excesses Of Mirasmentioning

confidence: 88%

Large Magellanic Cloud Near-infrared Synoptic Survey. V. Period–Luminosity Relations of Miras

Yuan¹,

Macri²,

He³

et al. 2017

101

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“…IRAS-selected oxygen-rich AGB stars (Fouque et al 1992;Guglielmo et al 1993) derived by van Loon et al (1998). The offset could be due to the H band water absorption bands (Frogel & Whitford 1987;Glass et al 1995) that are found to be strong in LAV stars.…”

Section: Colour-colour Diagram Of Mira Starsmentioning

confidence: 99%

86 GHz SiO maser survey of late-type stars in the inner Galaxy

Messineo

Habing

Menten

et al. 2005

A&A

127

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Abstract. We have determined extinction corrections for a sample of 441 late-type stars in the inner Galaxy, which we previously searched for SiO maser emission, using the 2MASS near-infrared photometry of the surrounding stars. From this, the near-infrared extinction law is found to be approximated by a power law A λ ∝ λ −1.9±0.1 . Near-and mid-infrared colour-colour properties of known Mira stars are reviewed. From the distribution of the dereddened infrared colours of the SiO target stars we infer mass-loss rates between 10 −7 and 10 −5 M yr −1 .

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“…We complement our sample with objects from van Loon et al (1998) and Trams et al (1999) A further 34 IRAS-detected objects with spectral subclassification are available from Loup et al (1997;their …”

Section: Additional Samplesmentioning

confidence: 99%

An empirical formula for the mass-loss rates of dust-enshrouded red supergiants and oxygen-rich Asymptotic Giant Branch stars

Loon¹,

Cioni

Zijlstra

et al. 2005

A&A

382

359

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Abstract. We present an empirical determination of the mass-loss rate as a function of stellar luminosity and effective temperature, for oxygen-rich dust-enshrouded Asymptotic Giant Branch stars and red supergiants. To this aim we obtained optical spectra of a sample of dust-enshrouded red giants in the Large Magellanic Cloud, which we complemented with spectroscopic and infrared photometric data from the literature. Two of these turned out to be hot emission-line stars, of which one is a definite B[e] star. The mass-loss rates were measured through modelling of the spectral energy distributions. We thus obtain the massloss rate formula logṀ = −5.65 + 1.05 log(L/10 000 L ) − 6.3 log(T eff /3500 K), valid for dust-enshrouded red supergiants and oxygen-rich AGB stars. Despite the low metallicity of the LMC, both AGB stars and red supergiants are found at late spectral types. A comparison with galactic AGB stars and red supergiants shows excellent agreement between the mass-loss rate as predicted by our formula and that derived from the 60 µm flux density for dust-enshrouded objects, but not for optically bright objects. We discuss the possible implications of this for the mass-loss mechanism.

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Obscured AGB Stars in the LMC

Cited by 29 publications

References 7 publications

Large Magellanic Cloud Near-infrared Synoptic Survey. V. Period–Luminosity Relations of Miras

Large Magellanic Cloud Near-infrared Synoptic Survey. V. Period–Luminosity Relations of Miras

86 GHz SiO maser survey of late-type stars in the inner Galaxy

An empirical formula for the mass-loss rates of dust-enshrouded red supergiants and oxygen-rich Asymptotic Giant Branch stars

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