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Encyclopedia > De Vaucouleurs

Gérard Henri de Vaucouleurs (April 25, 1918–October 7, 1995) was a French-American astronomer.


He had an early interest in amateur astronomy and received his undergraduate degree in 1939 at the Sorbonne in Paris. After military service in World War II, he resumed his pursuit of astronomy.


Fluent in English, he spent 1949–1951 in England and 1951–1957 in Australia, the latter at Mount Stromlo Observatory. In 1960 he was appointed to the University of Texas, where he spent the rest of his career.


He specialized in the study of galaxies and was co-author of the Third Reference Catalogue of Bright Galaxies.


The de Vaucouleurs modified Hubble sequence is a widely used variant of the standard Hubble sequence

Contents
1 See also
2 External links

2.1 Obituaries
2.2 Other resources

See also

External links

  • Biography (http://www.nap.edu/html/biomems/gvaucouleurs.html)

Obituaries

Other resources


  Results from FactBites:
 
Gérard de Vaucouleurs - Wikipedia, the free encyclopedia (178 words)
Gérard Henri de Vaucouleurs (April 25, 1918–October 7, 1995) was a French-American astronomer.
The de Vaucouleurs modified Hubble sequence is a widely used variant of the standard Hubble sequence.
De Vaucouleurs was awarded the Henry Norris Russell Lectureship by the American Astronomical Society in 1988.
Gérard de Vaucouleurs, April 25, 1918–October 7, 1995 | By E. Margaret Burbidge | Biographical Memoirs (3095 words)
De Vaucouleurs returned to Le Houga in July 1941, and without abandoning his lifelong interest in Mars he turned his attention to the measurement of close double stars, variable stars, and the brightness variations of the asteroid Eros.
De Vaucouleurs continued his association with the Péridier Observatory in Le Houga, applying the research done for his thesis to light scattering in the Earth's atmosphere.
Therefore, it was natural that de Vaucouleurs should look at Frank Kerr's map of 21-cm velocity residuals across the Large Magellanic Cloud, and he was able to recognize the presence of a typical rotation pattern for a disk galaxy.
  More results at FactBites »


 

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