Classical Cepheids, what else?

Abstract

We present new and independent estimates of the distances to the Magellanic Clouds (MCs) using near-infrared (NIR) and optical--NIR period--Wesenheit (PW) relations. The slopes of the PW relations are, within the dispersion, linear over the entire period range and independent of metal content. The absolute zero points were fixed using Galactic Cepheids with distances based on the infrared surface-brightness method. The true distance modulus we found for the Large Magellanic Cloud---$(m-M{)}_0=18.48\pm 0.01\pm 0.10$ mag---and the Small Magellanic Cloud---$(m-M{)}_0=18.94\pm 0.01\pm 0.10$ mag---agree quite well with similar distance determinations based on robust distance indicators. We also briefly discuss the evolutionary and pulsation properties of MC Cepheids.

References in corpus (6)

• A new Cepheid distance to the maser-host galaxy NGC 4258 and its implications for the Hubble Constant
• The influence of chemical composition on the properties of Cepheid stars. II-The iron content
• A new calibration of Galactic Cepheid Period-Luminosity relations from B to K bands, and a comparison to LMC PL relations
• New Optical Reddening Maps of the Large and Small Magellanic Clouds
• Galactic abundance gradients from Cepheids : On the iron abundance gradient around 10-12 kpc
• The VMC Survey. V. First results for Classical Cepheids

Cited by in corpus (2)

• On the effect of rotation on populations of classical Cepheids I. Predictions at solar metallicity
• Anchors for the Cosmic Distance Scale: the Cepheid QZ Normae in the Open Cluster NGC 6067