The RR Lyrae Period‐Luminosity Relation. I. Theoretical Calibration

Catelan, M.; Pritzl, B. J.; Smith, Horace A.

doi:10.1086/422916

Cited by 291 publications

(513 citation statements)

References 24 publications

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“…and both the metal-rich and metal-poor extremes are represented by only two stars. Although our results are very similar to those obtained by Bono et al (2003), Catelan et al (2004), and Sollima et al (2008), we cannot reach firm conclusions concerning the metallicity dependence of the period-luminosity relation in the J band based solely on these data. Therefore, to increase the sample size, we added the Sollima et al (2006a) dataset for ω Cen (Fig.…”

Section: Period-[fe/h] Relationssupporting

confidence: 54%

“…To evaluate the latter, we proceeded as follows: The theoretical value of the blue edge of the RR Lyrae instability strip is located near T eff = 7200 K, whereas the red edge is near 6100 K (e.g., Smith 1995;Catelan 2004, and references therein). To transform these temperature values into near-IR colors, we can use the model calculations from Catelan et al (2004), where the RR Lyrae period-luminosity relation was studied using synthetic horizontal branch models. The corresponding relationship between near-IR temperatures and colors, as implied by those models, is given in Fig.…”

Section: Mean J and K S Magnitudes And Error Analysismentioning

confidence: 99%

“…Accordingly, considerable attention has been devoted to this subject over the past several years, with several papers recently published on its accurate determination, by both empirical and theoretical approaches (e.g., Del Principe et al 2006;Solima et al 2006Solima et al , 2008Feast et al 2008;Pietrzyński et al 2008;Szewczyk et al 2008). From the theoretical point of view, its properties have been investigated by Bono et al (2001Bono et al ( , 2003, Cassisi et al (2004), and Catelan et al (2004).…”

Section: Introductionmentioning

confidence: 99%

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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: Period-[fe/h] Relationssupporting

confidence: 54%

Section: Mean J and K S Magnitudes And Error Analysismentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

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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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“…Both studies found that the metalpoor part of this relation was less steep (nearly flat according to McNamara) than the metal-rich part. Alternatively, a quadratic relation between M V (ZAHB) and metallicity was supported by several HB stellar evolution models (Dorman 1992;Cassisi et al 1999;VandenBerg et al 2000;Catelan et al 2004;Pietrinferni et al 2006) and pulsation models (Bono et al 2007), and was confirmed by empirical HB data for 61 Galactic GCs (Ferraro et al 1999).…”

Section: From Evolution and Pulsation Modelsmentioning

confidence: 78%

The horizontal branch luminosity vs. metallicity in M 31 globular clusters

Federici

Cacciari

Bellazzini

et al. 2012

A&A

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Context. Thanks to the outstanding capabilites of the HS T , our current knowledge about the M31 globular clusters (GCs) is similar to our knowledge of the Milky Way GCs in the 1960s-1970s, which set the basis for studying the halo and galaxy formation using these objects as tracers, and established their importance in defining the cosmic distance scale. Aims. We intend to derive a new calibration of the M V (HB)-[Fe/H] relation by exploiting the large photometric database of old GCs in M31 in the HS T archive. Methods. We collected the BVI data for 48 old GCs in M31 and analysed them by applying the same methods and procedures to all objects. We obtained a set of homogeneous colour-magnitude diagrams (CMDs) that were best-fitted with the fiducial CMD ridge lines of selected Milky Way template GCs. Reddening, metallicity, Horizontal Branch (HB) luminosity and distance were determined self-consistently for each cluster. Results. There are three main results of this study: i) the relation M V (HB)=0.25(±0.02)[Fe/H]+0.89(±0.03), which is obtained from the above parameters and is calibrated on the distances of the template Galactic GCs; ii) the distance modulus to M31 of (m-M) 0 =24.42±0.06 mag, obtained by normalising this relation at the reference value of [Fe/H]=-1.5 to a similar relation using V 0 (HB). This is the first determination of the distance to M31 based on the characteristics of its GC system which is calibrated on Galactic GCs; iii) the distance to the Large Magellanic Cloud (LMC), which is estimated to be 18.54±0.07 mag as a consequence of the previous results. These values agree excellently with the most recent estimate based on HS T parallaxes of Galactic Cepheid and RR Lyrae stars, as well as with recent methods.

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“…RR Lyrae stars make useful distance indicators because of the existence of an absolute magnitude-metallicity relation in the V band: (Sandage 1981a,b) and of a period-luminosity-metallicity relation in the K band: P L K Z (Longmore et al 1986, Bono et al 2003, Catelan et al 2004, Sollima et al 2008, and references therein).…”

Section: V − [Fe/h] and P L K Z Relations Of Rr Lyrae Starsmentioning

confidence: 99%