The Baade-Wesselink method and the distances to RR Lyrae stars. VII - The field stars SW Andromedae and DX Delphini and a comparison of recent Baade-Wesselink analyses

Jones, Rodney V.; Carney, Bruce W.; Storm, J.; Latham, David W.

doi:10.1086/171046

Cited by 101 publications

(137 citation statements)

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“…A great deal has been written about the virtue of utilizing the (V-K) index to infer the temperatures required for the B-W analysis (Liu and Janes, 1990;Jones et al 1992;Carney et al 1992;Femley 1993). In brief, the (V-K) index yields a smoother temperature variation, the phases of maximum angular diameter and maximum radius match, (V-K) has a longer wavelength baseline, is less sensitive to metallicity and gravity variations, is less sensitive to shockwave effects near maximum fight, and gives a better overall fit of the angular diameters versus phase curves.…”

Section: Discussionmentioning

confidence: 99%

The Absolute Magnitudes of the RR Lyrae Stars

McNamara¹

1997

PASP

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ABSTRACT. We present a new calibration of the relationship between the absolute magnitudes and metal abundances, [Fe/H], of RR Lyrae stars. Temperatures inferred from optical and near-infrared color indices and the new Kurucz models are utilized in conjunction with Baade-Wesselink solutions to derive absolute magnitudes. Temperatures inferred from the optical and near-infrared photometry are -200-300 K higher for the variables than those given from (V-K) color indices and the older Kurucz models. We find M v = 0.287[Fe/H]+ 0.964. This equation gives higher luminosities ( -0.2 mag) for the metal-poor variables than previous B-W calibrations. The RR Lyrae stars in the Large Magellanic Cloud in conjunction with our calibration yield a distance modulus of 18.53. Thus, the Cepheids and RR Lyrae stars give identical distance moduli at ^0.1 mag level. The repercussions of the higher temperatures and higher luminosities of RR Lyrae stars on the distances and ages of globular clusters, distance to the galactic center, the Hubble constant and age of the Universe, and the masses of RR Lyrae stars are discussed.

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Section: Discussionmentioning

confidence: 99%

The Absolute Magnitudes of the RR Lyrae Stars

McNamara¹

1997

PASP

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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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“…Distance estimates for globular clusters rely heavily on the absolute visual magnitudes of the cluster RR Lyr stars and the M^[Fe/H] relation [Cacciari et al 1989a,b;Sandage 1990;Liu and Janes 1990a,b;Jones et al 1992]. The question still remains, however, if this relation, determined from field RR Lyr stars, is truly representative for the stars found in globular clusters, or if the absolute magnitudes found for these stars are affected by evolutionary effects which are not taken into account in the M v -[Fe/H] relation.…”

Section: Introductionmentioning

confidence: 99%

Radial-velocity curves for RR Lyrae stars in the globular clusters M5 and M92 obtained using synthetic spectra cross-correlation templates

Storm

Carney

Latham

et al. 1992

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ABSTRACT. Radial-velocity curves are presented for the RR Lyrae stars VI and V3 in the lowmetallicity globular cluster M92 (NGC 6341) and V8 and V28 in the intermediate-metallicity globular cluster M5 (NGC 5904) based on between 50 and 90 observations per star. The radial velocities were derived by cross-correlating spectra obtained with the Multiple Mirror Telescope echelle spectrograph with synthetic templates calculated using Kurucz's model atmospheres (ATLAS8) and synthetic spectrum (SYNTHE) codes. The synthetic templates provide a better match to the observed spectra than the available observed templates, especially for the metal-poor stars, resulting in high-precision radialvelocities good to a few km s -1 in most cases. We find systemic velocities of -125.4, -122.6, +48.7, and +53.6 km s -1 for M92-V1, M92-V3, M5-V8, and M5-V28, respectively, in good agreement with previous determinations of cluster mean velocities.

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The Baade-Wesselink method and the distances to RR Lyrae stars. VII - The field stars SW Andromedae and DX Delphini and a comparison of recent Baade-Wesselink analyses

Cited by 101 publications

References 0 publications

The Absolute Magnitudes of the RR Lyrae Stars

The Absolute Magnitudes of the RR Lyrae Stars

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

Radial-velocity curves for RR Lyrae stars in the globular clusters M5 and M92 obtained using synthetic spectra cross-correlation templates

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