Globular Cluster Distances from RR Lyrae Stars

Cacciari, C.; Clementini, G.

doi:10.1007/978-3-540-39882-0_6

Cited by 105 publications

(55 citation statements)

References 55 publications

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“…Note that, if we assume a difference in distance between Reticulum and the LMC center of ∆µ = 0.08 (Walker, 1992), then the true distance to LMC becomes (DM ) J,0 = 18.43 ± 0.06 and (DM ) K,0 = 18.47 ± 0.07, respectively. Both values are in good agreement with the distance modulus of LMC evaluated by Cacciari & Clementini (2003), namely µ = 18.48±0.05, obtained by averaging different absolute magnitude determinations for RR Lyrae stars.…”

Section: −0734 Log L/lsupporting

confidence: 87%

Near-Infrared photometry of the LMC cluster Reticulum

Dall’Ora

Bono

Storm

et al. 2004

International Astronomical Union Colloquium

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Abstract. We present near-infrared (JKs) time series data of the Large Magellanic Cloud (LMC) cluster Reticulum. The observing strategy and data reduction (DAOPHOTII/ALLFRAME) allowed us to reach a photometry accuracy of the order of 0.02 mag at limiting magnitudes typical of RR Lyrae stars. We are interested in Reticulum, since it hosts a sizable sample of RR Lyrae (32), and therefore the use of the K-band Period-Luminosity-Metallicity (P LZK ) relation will allow us to supply an accurate LMC distance evaluation. The main advantages in using this method is that it is marginally affected by off-ZAHB evolutionary effects and by reddening corrections. As a preliminary but robust result we find a true distance in good agreement with the LMC Cepheid distance scale, i.e. µ = 18.47 ± 0.07 mag.

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Section: −0734 Log L/lsupporting

confidence: 87%

Near-Infrared photometry of the LMC cluster Reticulum

Dall’Ora

Bono

Storm

et al. 2004

International Astronomical Union Colloquium

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“…The most widely used methods include the Baade-Wesselink (B-W) analysis of field RR Lyraes, statistical and trigonometric parallaxes of RR Lyrae and BHB field stars, GC distance determination via main-sequence fitting and hence luminosities for RR Lyrae and BHB members. We refer the interested reader to Cacciari & Clementini (2003) for a review.…”

Section: The Assumed Metallicitymentioning

confidence: 99%

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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“…STEP ( (1) This distance modulus was derived using values from Clementini et al (2003) for V (RR) and the reddening, and the assumption of MV = 0.59 ± 0.03 mag for the absolute visual magnitude of RR Lyrae stars at metal abundance [Fe/H] = − 1.5 (Cacciari & Clementini 2003).…”

Section: The New Surveysmentioning

confidence: 99%

Pulsating variable stars in the Magellanic Clouds

Clementini

2008

Proc. IAU

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Abstract. Pulsating variable stars can be powerful tools to study the structure, formation and evolution of galaxies. I discuss the role that the Magellanic Clouds' pulsating variables play in our understanding of the whole Magellanic System, in light of results on pulsating variables produced by extensive observing campaigns like the MACHO and OGLE microlensing surveys. In this context, I also briefly outline the promise of new surveys and astrometric missions which will target the Clouds in the near future.

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Globular Cluster Distances from RR Lyrae Stars

Cited by 105 publications

References 55 publications

Near-Infrared photometry of the LMC cluster Reticulum

Near-Infrared photometry of the LMC cluster Reticulum

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

Pulsating variable stars in the Magellanic Clouds

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