Other
Scientific paper
May 2010
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2010aas...21641702e&link_type=abstract
American Astronomical Society, AAS Meeting #216, #417.02; Bulletin of the American Astronomical Society, Vol. 41, p.828
Other
Scientific paper
Selection effects from bandshifting, angular resolution limitations, surface brightness dimming, and intergalactic absorption skew our view of high redshift galaxies so that we primarily see those that are extremely bright, massive, and star-bursting. Bandshifting shows a galaxy in its restframe NUV or FUV at z>1, and also biases the determination of age from BViz colors to lower values. The rapid increase in resolvable physical size with redshift for z<1 causes a bias to larger clumps and larger galaxies at higher z in this range. Surface brightness dimming causes galaxies and clumps with normal star formation rates to drop below the Ultra Deep Field (UDF) noise by redshift z 2. Intergalactic absorption further decreases the brightness of galaxies by factors of a few at this z. These effects combine to make the average star formation rate in an observable clump increase as (1+z)8 for z<1. None of these selection effects directly causes the clump mass to increase with redshift in clumpy galaxies, however. Clumps are well separated from each other and they show up over a wide range of wavelengths. The increase in clump mass with redshift is mostly from an increase in observable galaxy mass. This is because there is a nearly constant ratio of clump mass to galaxy luminosity and the primary selection effect is for bright galaxies, considering that the intrinsic surface brightness for anything observable increases sharply with z. Redshifted versions of local grand design, multiple arm, and flocculent spiral galaxies, along with dwarf irregulars and interacting galaxies, will be shown to indicate which features are observable at high redshift.
Elmegreen Bruce
Elmegreen Debra Meloy
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