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L. E. Strubbe, K. Sheth, N. Z. Scoville (Caltech), M. W. Regan (STScI)
How does galaxy morphology change as a function of redshift? This fundamental question is the focal point of many observational studies, particularly those with datasets such as the Hubble Deep Fields. In order to draw meaningful conclusions from these observations, it is critical to understand instrumental and observational effects on the observed morphology of galaxies. To this end, we have developed an IDL code that transforms nearby galaxy images to high redshifts; our routine allows for different cosmologies, and includes bandshifting, rebinning, cosmological dimming and noise addition to simulate the appearance of nearby galaxies in the Hubble Deep Fields. Our code, which will be made publicly available, is applicable to a wide variety of morphological studies. One example, presented here, is the change in the appearance of the Hubble sequence as a function of redshift. We are also using the code to study the bar fraction in a control sample of nearby galaxies for comparison to the bar fraction in the NICMOS Deep Field (see talk by Sheth et al.).
This work was partially funded by grant HST-AR-09552.01-A provided by NASA through a grant from the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Incorporated, under NASA contract NAS5-26555, and the Flintridge Foundation grant towards the Summer Undergraduate Research Fellowship program at Caltech.
The author(s) of this abstract have provided an email address for comments about the abstract: les@astro.caltech.edu
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Bulletin of the American Astronomical Society, 34, #4
© 2002. The American Astronomical Soceity.