Metal-poor type II cepheids with periods less than three days

V. Kovtyukh, G. Wallerstein, I. Yegorova, S. Andrievsky, S. Korotin, I. Saviane, S. Belik, C. E. Davis, E. M. Farrell

Resultado de la investigación: Article

2 Citas (Scopus)

Resumen

We have analyzed 10 high-resolution spectra of Type II Cepheids with periods less than 3 days. We find that they clearly separate into two groups: those with near or slightly below solar metallicities, and those with [Fe/H] between −1.5 and −2.0. While the former are usually called BLHer stars, we suggest that the latter be called UYEri stars. The UYEri subclass appears to be similar to the short period variables in globular clusters of the Galactic Halo. Globular clusters with [Fe/H] > −1.0 almost never have Type II Cepheids.

Idioma originalEnglish
Número de artículo054201
PublicaciónPublications of the Astronomical Society of the Pacific
Volumen130
N.º987
DOI
EstadoPublished - 1 may 2018

Huella dactilar

globular clusters
stars
galactic halos
metal
metals
metallicity
high resolution

ASJC Scopus subject areas

  • Astronomy and Astrophysics
  • Space and Planetary Science

Citar esto

Kovtyukh, V., Wallerstein, G., Yegorova, I., Andrievsky, S., Korotin, S., Saviane, I., ... Farrell, E. M. (2018). Metal-poor type II cepheids with periods less than three days. Publications of the Astronomical Society of the Pacific, 130(987), [054201]. https://doi.org/10.1088/1538-3873/aaacf7
Kovtyukh, V. ; Wallerstein, G. ; Yegorova, I. ; Andrievsky, S. ; Korotin, S. ; Saviane, I. ; Belik, S. ; Davis, C. E. ; Farrell, E. M. / Metal-poor type II cepheids with periods less than three days. En: Publications of the Astronomical Society of the Pacific. 2018 ; Vol. 130, N.º 987.
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Kovtyukh, V, Wallerstein, G, Yegorova, I, Andrievsky, S, Korotin, S, Saviane, I, Belik, S, Davis, CE & Farrell, EM 2018, 'Metal-poor type II cepheids with periods less than three days', Publications of the Astronomical Society of the Pacific, vol. 130, n.º 987, 054201. https://doi.org/10.1088/1538-3873/aaacf7

Metal-poor type II cepheids with periods less than three days. / Kovtyukh, V.; Wallerstein, G.; Yegorova, I.; Andrievsky, S.; Korotin, S.; Saviane, I.; Belik, S.; Davis, C. E.; Farrell, E. M.

En: Publications of the Astronomical Society of the Pacific, Vol. 130, N.º 987, 054201, 01.05.2018.

Resultado de la investigación: Article

TY - JOUR

T1 - Metal-poor type II cepheids with periods less than three days

AU - Kovtyukh, V.

AU - Wallerstein, G.

AU - Yegorova, I.

AU - Andrievsky, S.

AU - Korotin, S.

AU - Saviane, I.

AU - Belik, S.

AU - Davis, C. E.

AU - Farrell, E. M.

PY - 2018/5/1

Y1 - 2018/5/1

N2 - We have analyzed 10 high-resolution spectra of Type II Cepheids with periods less than 3 days. We find that they clearly separate into two groups: those with near or slightly below solar metallicities, and those with [Fe/H] between −1.5 and −2.0. While the former are usually called BLHer stars, we suggest that the latter be called UYEri stars. The UYEri subclass appears to be similar to the short period variables in globular clusters of the Galactic Halo. Globular clusters with [Fe/H] > −1.0 almost never have Type II Cepheids.

AB - We have analyzed 10 high-resolution spectra of Type II Cepheids with periods less than 3 days. We find that they clearly separate into two groups: those with near or slightly below solar metallicities, and those with [Fe/H] between −1.5 and −2.0. While the former are usually called BLHer stars, we suggest that the latter be called UYEri stars. The UYEri subclass appears to be similar to the short period variables in globular clusters of the Galactic Halo. Globular clusters with [Fe/H] > −1.0 almost never have Type II Cepheids.

KW - Globular clusters: general

KW - Stars: abundances

KW - Stars: variable: cepheids

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U2 - 10.1088/1538-3873/aaacf7

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JO - Publications of the Astronomical Society of the Pacific

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Kovtyukh V, Wallerstein G, Yegorova I, Andrievsky S, Korotin S, Saviane I y otros. Metal-poor type II cepheids with periods less than three days. Publications of the Astronomical Society of the Pacific. 2018 may 1;130(987). 054201. https://doi.org/10.1088/1538-3873/aaacf7