Population Gradients in Local Group Dwarf Spheroidals

Details Population Gradients in Local Group Dwarf Spheroidals Population Gradients in Local Group Dwarf Spheroidals

2001-09-07

arxiv.org/abs/astro-ph/0109121v1

Astron.J.122:3092,2001

Astronomy and Astrophysics

Astrophysics

accepted for publication in AJ; 25 pages; 11 images in jpeg and png format

Scientific paper

10.1086/324232

We present a systematic and homogeneous analysis of population gradients for the Local Group dwarf spheroidals (dSphs) Carina, Sculptor, Sextans, Tucana, Andromeda I-III, V, and VI. For all of the Milky Way companions studied here we find significant population gradients. The same is true for the remote dSph Tucana located at the outskirts of the LG. Among the M 31 dSph companions only Andromeda I and VI show obvious gradients. In all cases where a HB morphology gradient is visible, the red HB stars are more centrally concentrated. The occurence of a HB morphological gradient shows a correlation with a morphology gradient in the red giant branch. It seems likely that metallicity is the driver of the gradients in Sextans, Sculptor, Tucana, and Andromeda VI, while age is an important factor in Carina. We find no evidence that the vicinity of a nearby massive spiral galaxy influences the formation of the population gradients.

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