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Hubble Space Telescope imaging of distant galaxies - 4C 41.17 at Z = 3.8
Miley, G. K.; Chambers, K. C.; van Breugel, W. J. M.; Macchetto, F.
AA(Leiden, Sterrewacht, Netherlands), AB(Hawaii Univ., Honolulu), AC(Lawrence Livermore National Lab., Livermore, CA), AD(Space Telescope Science Inst., Baltimore, MD)
Astrophysical Journal, Part 2 - Letters (ISSN 0004-637X), vol. 401, no. 2, p. L69-L73. (ApJL Homepage)
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NASA/STI Keywords:
Astrometry, Galactic Structure, Hubble Space Telescope, Radio Sources (Astronomy), Emission Spectra, Red Shift, Star Formation, Stellar Luminosity
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The Hubble Space Telescope has been used to image the continuum emission from 4C 41.17 at z = 3.8, the most distant galaxy known. The galaxy was detected with good signal-to-noise ratio and was spatially resolved at the 0.1 arcsec (440 pc) HST resolution. About 35 percent of this emission is in the form of a high brightness clumpy region extending by about 0.5 arcsec (1.7 kpc), whose morphology is remarkably similar to that of the radio components. A fainter more diffuse region of optical emission extends westward from the center of the nuclear complex for about 1.2 arcsec (5.3 kpc) out along the radio axis. The clumpiness of the optical emission and its close correspondence with the radio structure on the subkiloparsec scale is discussed in the light of current models for high-redshift galaxies. Our observations imply that the material in the center of this galaxy is clumpy on the subkiloparsec scale.

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