A Direct Distance to the LMC Cepheid HV 12198 from the Infrared Surface Brightness Technique

Abstract

We report on a first application of the infrared surface brightness technique on a Cepheid in the Large Magellanic Cloud, the variable HV 12198 in the young globular cluster NGC 1866. From this one star, we determine a distance modulus of 18.42 +- 0.10 (random and systematic uncertainty) to the cluster. When the results on further member Cepheids in NGC 1866 become available, we expect to derive the distance to the LMC with a +- 3-4 percent accuracy, including systematic errors, from this technique.

arXiv comment4 pages, 4 figures, accepted in ApJ Letters

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• The Hubble Constant
• Spectroscopic Survey of the Galaxy with Gaia II. The expected science yield from the Radial Velocity Spectrometer
• Calibration of the Barnes-Evans relation using interferometric observations of Cepheids
• The angular size of the Cepheid L Car: a comparison of the interferometric and surface brightness techniques
• The distance to the LMC cluster NGC 1866 and the surrounding field
• The Distance of the Large Magellanic Cloud Cluster NGC 1866
• The near-IR Surface Brightness Method applied to six Cepheids in the young LMC cluster NGC1866
• The distance to the LMC cluster NGC 1866; clues from the cluster Cepheid population
• Cepheid variables in the LMC cluster NGC 1866. I. New BVRI CCD photometry