Astronomy and Astrophysics – Astronomy
Scientific paper
Dec 1992
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1992aas...181.3508h&link_type=abstract
American Astronomical Society, 181st AAS Meeting, #35.08; Bulletin of the American Astronomical Society, Vol. 24, p.1173
Astronomy and Astrophysics
Astronomy
Scientific paper
Based on optical spectroscopy, multicolor broad-band optical imaging, and narrow-band Hα imaging, it is claimed that the unusual spectral energy distribution of 60 microns Peakers is attributed to dust that is more centrally concentrated and exposed to a more intense radiation field than in randomly selected IRAS galaxies. Due to the central dust shroud, the morphology of the circumnuclear regions of 60 microns Peakers is virtually unknown at optical wavelengths. Since dust extinction in the near-infrared (NIR) is much lower than in the optical (AK ~ 0.1 times AV), a program of high resolution (0.6 arcsec/pixel) NIR (J, H, K) imaging at UKIRT was undertaken for roughly half of the sample ( ~ 30), in order to investigate the circumnuclear regions of 60 microns Peakers. Central structure has been uncovered in many 60 microns Peakers, including the discovery of previously undetected double nuclei in the centers of three amorphous galaxies (IRAS 05189, 06488 08014) and a third nucleus in the well studied ``double-nucleus" galaxy Mrk 463. All of these closely separated nuclei were detected on K-band images only, which is undoubtedly due to Brgamma emission and to reduced extinction. From the frequency and projected separations of multiple nuclei in the sample, it is estimated that the timescale of the 60 microns Peaker phase is ~ 10(8) yrs. The detection of multiple nuclei in a significant fraction of the amorphous galaxies and the short lifetime of the 60 microns Peaker phase strongly supports the claim that these are galaxies in a rapid phase of evolution following an interaction/merger event. A quantitative analysis of the NIR morphology (eg. surface brightness profiles, effective radii, axial ratios) is presented and compared with the optical (B, R) morphology.
de Robertis Michael M.
Heisler Charlene Anne
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