A distance to the galaxy NGC4258 from observations of Cepheid variable stars

Eyal Maoz (), Jeffrey A. Newman, Laura Ferrarese, Peter B. Stetson, Stephen E. Zepf, Marc Davis, Wendy L. Freedman and Barry F. Madore
Additional contact information
Eyal Maoz: NASA Ames Research Center
Jeffrey A. Newman: University of California
Laura Ferrarese: California Institute of Technology
Peter B. Stetson: Dominion Astrophysical Observatory
Stephen E. Zepf: PO Box 208101, Yale University
Marc Davis: University of California
Wendy L. Freedman: Observatories of the Carnegie Institution of Washington
Barry F. Madore: Observatories of the Carnegie Institution of Washington

Nature, 1999, vol. 401, issue 6751, 351-354

Abstract: Abstract Cepheid variable stars pulsate in a way that is correlated with their intrinsic luminosity, making them useful as ‘standard candles’ for determining distances to galaxies; the potential systematic uncertainties in the resulting distances have been estimated1 to be only 8–10%. They have played a crucial role in establishing the extragalactic distance scale and hence the value of the Hubble constant. Here we report observations of Cepheids in the nearby galaxy NGC4258; the distance calculated from the Cepheids is 8.1 ± 0.4 Mpc, where the uncertainty does not include possible systematic errors. There is an independently determined geometric distance to this galaxy of 7.2 ± 0.5 Mpc, based on the observed proper motions of water masers orbiting the central black hole2; the distances differ by 1.3σ. If the maser-based distance is adopted and the Cepheid distance scale revised accordingly, the derived value of the Hubble constant would increase by 12 ± 9%, while the expansion age of the Universe would decrease by the same amount.

Date: 1999
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DOI: 10.1038/43838

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