Induced star formation and morphological evolution in very high redshift radio galaxies

Details Induced star formation and morphological evolution in very high redshift radio galaxies Induced star formation and morphological evolution in very high redshift radio galaxies

1998-09-15

arxiv.org/abs/astro-ph/9809186v1

Astronomy and Astrophysics

Astrophysics

10 Pages, including 4 PostScript figures (2 in color); to appear in the proceedings of "The Most Distant Radiogalaxies", Amste

Scientific paper

Near-infrared, sub-arcsecond seeing images obtained with the W. M. Keck I Telescope of show strong evolution at rest--frame optical} wavelengths in the morphologies of high redshift radio galaxies (HzRGs) with 1.93, to much more compact and symmetrical shapes at z<3. The linear sizes (~10 kpc) and luminosities (M_B~-20 to -22) of the individual components in the z>3 HzRGs are similar to the total sizes and luminosities of normal, radio--quiet, star forming galaxies seen at z=3--4. `R'-band, 0.1 arcsec resolution images with the Hubble Space Telescope of one of these HzRGs, 4C41.17 at z=3.800, show that at rest--frame UV wavelengths the galaxy morphology breaks up in even smaller, ~1 kpc--sized components embedded in a large halo of low surface brightness emission. The brightest UV emission is from a radio--aligned, edge-brightened feature (4C41.17-North) downstream from a bright radio knot. A narrow--band Lyman-alpha image, also obtained with HST, shows an arc--shaped Lyman-alpha feature at this same location, suggestive of a strong jet/cloud collision. Deep spectropolarimetric observations with the W. M. Keck II Telescope of 4C41.17 show that the radio--aligned UV continuum is unpolarized. (abridged)

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