Volume 388, Number 2, June III 2002
|Page(s)||477 - 482|
|Section||Cosmology (including clusters of galaxies)|
|Published online||31 May 2002|
Variable stars in nearby galaxies*
VI. Frequency-period distribution of Cepheids in IC 1613 and other galaxies of the Local Group
Osservatorio Astronomico di Brera, Via E. Bianchi 46, 23807 Merate, Italy
Corresponding author: E. Antonello, email@example.com
Accepted: 29 March 2002
The frequency–period distribution and other properties of Cepheids in IC 1613 are discussed and compared with those of stars in our Galaxy (Milky Way), LMC, SMC, M 31 and M 33. Taking into account the observational limitations and related incompleteness, it is concluded that the frequency–period distribution of Cepheids in IC 1613 is similar to that of SMC; we suspect that a much larger number of stars exist in IC 1613 with a period of less than 2 d that have not yet been detected. A discussion of the deficiency of fundamental mode Cepheids with periods in the range 8–10 d in the Milky Way, M 31 and M 33 is reported. The present data are not sufficient to verify if this is produced by a real bimodal frequency–period distribution or whether depends on the lack of pulsating stars in such a period range due to pulsational stability reasons. Some arguments are presented in favor of a bimodal distribution that is a function of the average metallicity. The Milky Way, M 31 and M 33 have the two maxima located at the same periods, about 5 and 13 d, respectively. A comment on very long period Cepheids is also given.
Key words: stars: oscillations / stars: variables: Cepheids / galaxies: individual: IC 1613 / galaxies: Local Group / galaxies: stellar content
© ESO, 2002
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