Jeremy Mould

Jeremy R. Mould (born 31 July 1949, Bristol) is an Australian astronomer currently at the Centre for Astrophysics and Supercomputing at Swinburne University of Technology. Mould was previously Director of the Research School of Astronomy and Astrophysics at the Australian National University and the American National Optical Astronomy Observatory. He is an Honorary Professorial Fellow, at the University of Melbourne.

He emigrated to Australia in 1963. He graduated from the University of Melbourne, and Australian National University with a PhD. He was research fellow at Kitt Peak National Observatory, and professor at the California Institute of Technology.

Mould's work at Caltech during the early 1980s aimed to determine both the size and the age of the Universe by identifying and calibrating Standard Candles, that is, very bright stars whose Absolute Magnitude can be accurately measured when near the Earth, with more distant examples being identified by their color, spectrum, or in the case of Cepheid Variables, the period of oscillation of their brightness. Other important work included the measurement of luminous evolved red giants in star clusters of the Magellanic Clouds, which he did in collaboration with Marc Aaronson. Also in collaboration with Marc Aaronson and John Huchra, Mould undertook measurements of the Hubble Constant that would eventually extend to the use of the Hubble Space Telescope and the WFPC2 camera to study Cepheid variables and use them as standard candles. Mould was on the science team for the WFPC2 camera that helped to restore the Hubble Space Telescope's image quality, correcting spherical aberration in the primary mirror.

In collaboration with Gary DaCosta and Michael David Crawford, Mould prepared Hertzsprung Russell Diagrams of Large Magellanic Cloud and Small Magellanic Cloud Globular Clusters to determine their age, with the resulting Standard Candle being the brightest star in each cluster, with that star's absolute luminosity being derivable from its distance, with the B-R Color of the brightest cluster's star being used to determine the ages of more distant clusters by the colors of their brightest stars.

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