A new method of determining distances to galaxies

Details A new method of determining distances to galaxies A new method of determining distances to galaxies

Feb 1977

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1977a%26a....54..661t&link_type=abstract

Astronomy and Astrophysics, vol. 54, no. 3, Feb. 1977, p. 661-673.

Astronomy and Astrophysics

Astrophysics

1240

Distance Measuring Equipment, H Lines, Luminous Intensity, Spectral Line Width, Spiral Galaxies, Telescopes, Astronomical Photometry, Calibrating, Galactic Clusters, Galactic Structure, Hubble Diagram, Synoptic Measurement

Scientific paper

It is proposed that for spiral galaxies there is a good correlation between the global neutral hydrogen line profile width, a distance-independent observable, and the absolute magnitude (or diameter). Such a relation is first sought in nearby calibration galaxies of the Local Group, the M 81 group, and the M 101 group, with well-determined distances, accurately known photometric properties, and accurately known global hydrogen profile width. On the basis of these calibration magnitude-global profile width and diameter-global profile width relationships, distances were derived for the Virgo cluster and the Ursa Major cluster. The distance moduli obtained are 30.6 m for the Virgo cluster and 30.5 m for the Ursa Major cluster. The result for the Virgo cluster suggests a Hubble constant of 80 km per sec per Mpc.

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