AGB stars in the Magellanic Clouds I: The C/M ratio

M-R.L. Cioni; H.J. Habing

doi:10.1051/0004-6361:20030226

AGB stars in the Magellanic Clouds I: The C/M ratio

M-R.L. Cioni, H.J. Habing

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Abstract

Regions of different metallicity have been identified in the Magellanic Clouds by using the ratio between Asymptotic Giant Branch stars of spectral type C and M. In the Large Magellanic Cloud the ratio appears to decrease radially while in the Small Magellanic Cloud (SMC) there is no clear trend, reflecting either the large extension of the SMC along the line of sight or a more complex star formation history. The distribution of the C/M ratio is clumpy and corresponds to a spread in [Fe/H] of 0.75 dex in both Clouds. There is an indication of increasing C/M ratio, thus decreasing metallicity, towards the Bridge region connecting the two Clouds.

Original language	English
Pages (from-to)	133-140
Journal	Astronomy and Astrophysics
Volume	402
Issue number	1
DOIs	https://doi.org/10.1051/0004-6361:20030226
Publication status	Published - 2003

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title = "AGB stars in the Magellanic Clouds I: The C/M ratio",

abstract = "Regions of different metallicity have been identified in the Magellanic Clouds by using the ratio between Asymptotic Giant Branch stars of spectral type C and M. In the Large Magellanic Cloud the ratio appears to decrease radially while in the Small Magellanic Cloud (SMC) there is no clear trend, reflecting either the large extension of the SMC along the line of sight or a more complex star formation history. The distribution of the C/M ratio is clumpy and corresponds to a spread in [Fe/H] of 0.75 dex in both Clouds. There is an indication of increasing C/M ratio, thus decreasing metallicity, towards the Bridge region connecting the two Clouds.",

author = "M-R.L. Cioni and H.J. Habing",

note = "Original article can be found at: http://www.aanda.org/ Copyright The European Southern Observatory",

year = "2003",

doi = "10.1051/0004-6361:20030226",

language = "English",

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journal = "Astronomy and Astrophysics",

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T1 - AGB stars in the Magellanic Clouds I: The C/M ratio

AU - Cioni, M-R.L.

AU - Habing, H.J.

N1 - Original article can be found at: http://www.aanda.org/ Copyright The European Southern Observatory

PY - 2003

Y1 - 2003

N2 - Regions of different metallicity have been identified in the Magellanic Clouds by using the ratio between Asymptotic Giant Branch stars of spectral type C and M. In the Large Magellanic Cloud the ratio appears to decrease radially while in the Small Magellanic Cloud (SMC) there is no clear trend, reflecting either the large extension of the SMC along the line of sight or a more complex star formation history. The distribution of the C/M ratio is clumpy and corresponds to a spread in [Fe/H] of 0.75 dex in both Clouds. There is an indication of increasing C/M ratio, thus decreasing metallicity, towards the Bridge region connecting the two Clouds.

AB - Regions of different metallicity have been identified in the Magellanic Clouds by using the ratio between Asymptotic Giant Branch stars of spectral type C and M. In the Large Magellanic Cloud the ratio appears to decrease radially while in the Small Magellanic Cloud (SMC) there is no clear trend, reflecting either the large extension of the SMC along the line of sight or a more complex star formation history. The distribution of the C/M ratio is clumpy and corresponds to a spread in [Fe/H] of 0.75 dex in both Clouds. There is an indication of increasing C/M ratio, thus decreasing metallicity, towards the Bridge region connecting the two Clouds.

U2 - 10.1051/0004-6361:20030226

DO - 10.1051/0004-6361:20030226

M3 - Article

SN - 0004-6361

VL - 402

SP - 133

EP - 140

JO - Astronomy and Astrophysics

JF - Astronomy and Astrophysics

IS - 1

ER -

AGB stars in the Magellanic Clouds I: The C/M ratio

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