Period-luminosity-metallicity relations, pulsation modes, absolute magnitudes, and distances for population 2 variable stars

Nemec, J. M.; Nemec, A.; Lutz, T. E.

doi:10.1086/117062

Cited by 182 publications

(232 citation statements)

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“…Several authors (e.g., Jones et al 1992;Carney et al 1992;Skillen et al 1993;Nemec et al 1994;Frolov & Samus 1998) have previously calibrated the PLK relation on the basis of Article published by EDP Sciences observations of Galactic globular clusters and field RR Lyrae stars in our Galaxy. Such studies are summarized in Table 2 of Sollima et al (2006b), who also analyzed 538 RR Lyrae variables in 16 globular clusters using infrared (K-band) photometry and derived a PLK relation based on purely observational constraints.…”

Section: Introductionmentioning

confidence: 99%

Properties of RR Lyrae stars in the inner regions of the Large Magellanic Cloud

Borissova¹,

Rejkuba²,

Minniti

et al. 2009

A&A

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Context. RR Lyrae variable stars are the primary Population II distance indicator. Likewise, the Large Magellanic Cloud (LMC) constitutes a key step in the extragalactic distance scale. Aims. By combining near-IR photometry and spectroscopically measured metallicities for a homogeneous sample of 50 RR Lyr stars in the LMC, we investigate the metallicity dependence of the period-luminosity relation in the near-infrared (IR), use the newly derived relations to re-derive the distance to the LMC, and compare the distance moduli obtained from RR Lyr and red clump stars. Methods. This paper presents new (single-epoch) J-band and (multi-epoch) K s -band photometry of RR Lyr stars in 7 different LMC fields, observed with the near-IR camera SOFI at ESO's New Technology Telescope. Additional K s -band data for another two LMC fields were taken with the ISPI infrared array at CTIO's Blanco 4m telescope. The near-IR photometry was cross-correlated with the MACHO and OGLE databases, resulting in a catalog of 62 RR Lyr stars with BVRI JK s photometry. A subsample of 50 stars also has spectroscopically measured metallicities. Results. In the deep JK color-magnitude diagrams of 7 fields, red giant branch, red clump and RR Lyr stars are detected. The majority of RR Lyr stars are located within the instability strip with near-IR colors between 0.14 ≤ (J − K s ) 0 < 0.32. The period-luminosity relation only has a very mild dependence on metallicity in the K band, consistent with no dependence: M Ks = 2.11(±0.17) log P + 0.05(±0.07) [Fe/H] − 1.05. In the J band the currently available data do not allow firm conclusions regarding the metallicity dependence of the period-luminosity relation. Conclusions. The distance modulus of the LMC, derived using our near-IR period-luminosity-metallicity relation for RR Lyr stars, is (m − M) 0 = 18.53 ± 0.13, in very good agreement with the distance modulus from the red clump stars, 18.46 ± 0.07. However, LMC modulus derived from the RR Lyrae stars depends on the parallax of the star RR Lyrae.

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Section: Introductionmentioning

confidence: 99%

Properties of RR Lyrae stars in the inner regions of the Large Magellanic Cloud

Borissova¹,

Rejkuba²,

Minniti

et al. 2009

A&A

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“…The connection between these stars and the bluestraggler phenomenon has been analysed by different authors. A number of reviews are also available in the bibliography (Nemec et al, 1994;McNamara, 1995McNamara, , 1997.…”

Section: Discussionmentioning

confidence: 99%

SX Phe Variables in Globular Clusters

Rodrı́guez

López-González

2002

International Astronomical Union Colloquium

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Abstract.We have compiled an extensive and up-dated list of SX Phetype pulsators in globular clusters. In addition, SX Phe variables discovered in the Carina dwarf galaxy and other ones probably belonging to the Sagittarius dwarf galaxy are included. This catalogue is intended to be an up-dated list of all the SX Phe stars, in globular clusters and galaxies, known until now. The stars and their most significant parameters are listed together with references to studies of individual stars and notes for a number of variables. In addition, the references on the discovery for each variable and sources for photometry are also listed. Some relevant distributions are also analysed. The analysis of metal abundances and mean periods shows that both parameters are correlated in the sense that the periods of the variables are longer as the metallicity of the stellar system is higher.

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“…Unlike relations given by Nemec et al (1994), this relation has no metallicity term; any such term is likely to be quite small, however, because of the relation between the period and [Fe/H]. McNamara's relation (eq.…”

Section: The Relation Of Gsc 2985-01044 To Other D Scuti Starsmentioning

confidence: 94%

The δ Scuti Star GSC 2985‐01044

Kinman¹

1998

PUBL ASTRON SOC PAC

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ABSTRACT. GSC 2985-01044 is a d Scuti star with a period of 0.0933584 days and a V-magnitude range of 11.85-12.05; its light curve is slightly variable. The location, space motion, and other properties of this star indicate that it is a higher amplitude d Scuti star (or "dwarf Cepheid") that is a member of the old disk population. The problem of determining the local space densities of the various populations of the higher amplitude d Scuti stars is discussed.

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Period-luminosity-metallicity relations, pulsation modes, absolute magnitudes, and distances for population 2 variable stars

Cited by 182 publications

References 0 publications

Properties of RR Lyrae stars in the inner regions of the Large Magellanic Cloud

Properties of RR Lyrae stars in the inner regions of the Large Magellanic Cloud

SX Phe Variables in Globular Clusters

The δ Scuti Star GSC 2985‐01044

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