2011
DOI: 10.1051/0004-6361/201117626
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Galactic distributions of carbon- and oxygen-rich AGB stars revealed by the AKARI mid-infrared all-sky survey

Abstract: Context. The environmental conditions for asympotic giant branch (AGB) stars to reach the carbon-rich (C-rich) phase are important to understand the evolutionary process of AGB stars. The difference between the spatial distributions of C-rich and oxygen-rich (O-rich) AGB stars is essential for the study of the Galactic structure and the chemical evolution of the interstellar medium. Aims. We quantitatively investigate the spatial distributions of C-rich and O-rich AGB stars in our Galaxy. We discuss the differ… Show more

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Cited by 42 publications
(64 citation statements)
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“…However, the JHK colours of mass-losing O-rich stars are very similar to those of C-stars and these will dominate in the higher metallicity Galactic bulge. Ojha et al (2007) have questioned the Cole & Weinberg interpretation of the 2MASS colours and Ishihara et al (2011) show, from a study of stars with both 2MASS and Akari photometry, that the majority of AGB stars in the direction of the Galactic centre are O-rich. This is confirmed by Uttenthaler et al (2015).…”
Section: Mira Variablesmentioning
confidence: 99%
“…However, the JHK colours of mass-losing O-rich stars are very similar to those of C-stars and these will dominate in the higher metallicity Galactic bulge. Ojha et al (2007) have questioned the Cole & Weinberg interpretation of the 2MASS colours and Ishihara et al (2011) show, from a study of stars with both 2MASS and Akari photometry, that the majority of AGB stars in the direction of the Galactic centre are O-rich. This is confirmed by Uttenthaler et al (2015).…”
Section: Mira Variablesmentioning
confidence: 99%
“…The maximum amplitude is used to limit the number of heavily reddened C-rich Miras in our sample, which have on average larger amplitudes than O-rich Miras with the same period range. While C-rich Miras with low reddening track the O-rich Mira PLR, heavily-reddened C-rich Miras fall below the PLR and would bias our fit (Ishihara et al 2011;Whitelock et al 2003). From our simulations, we find that our amplitudes are well-recovered, with the mean amplitude of the input and recovered Miras within a few 0.01 mag of each other.…”
Section: Recovery Of Mira Parametersmentioning
confidence: 97%
“…Alternative diagnostics in selecting O-rich and C-rich from photometry have been explored. Ishihara et al (2011) and Matsunaga et al (2017) have used color-color diagrams of J − K s and AKARI colors to select C-rich stars in the Bulge, and have shown this to be an improvement over the use of single 2MASS color. Lebzelter et al (2018) of 2MASS magnitudes defined as…”
Section: Determining Carbon-and Oxygen-rich Typesmentioning
confidence: 99%