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VV 114

The two galaxies in VV 114 are sufficiently extended that a mosaic of two images was required to cover them both using the NIC2 camera. These galaxies present a remarkable contrast from the visual to near-infrared (cf. Knop et al. 1994; Doyon et al. 1995) - the eastern galaxy which is very insignificant in the visual becomes the dominant source in the near-infrared in terms of surface brightness. The western galaxy has a great number of luminous star forming regions in an arm running between the two galaxies and to its south. This positioning of the young clusters in the overlap region of the two galaxies is similar to that seen in NGC 6090. In the mm-wave CO line (Yun, Scoville & Knop 1995) and 850 µm continuum (Frayer et al. 1999), the major concentration of emission actually lies between the two galaxies . In the eastern galaxy, there are two 2 µm peaks, the brightest being that to the SW where the reddening is also greatest. A more detailed discussion of this galaxy is provided in Scoville et al. (1999a).

VV 114

Shaded contour plots of the extinction corrected 2.2 µm emission are shown together with the 1.1 µm (upper left) observed emission. In both panels, the contours and shading are logarithmic with the contours spaced by factors 21/2. (The level values are the same as for the figure above). The arcsec displacements in RA and DEC, given along the borders are measured from the 2.2 µm in all frames. At the upper left, a length bar is drawn. For the ratio image, both the 2.2 and 1.1 µm images were smoothed with the same adaptive smoothing and then smoothed with a Gaussian FWHM = 0.2" in calculating the 2.2 µm opacity from Eq. 3 (see text). In cases where a strong point-source or variable background contaminated the 2.2 µm image, the extinction corrected image was derived for 1.6 µm. For the galaxies with strong point-sources, the PSF was fit to the source and then subtracted and replaced by a Gaussian with the proper integrated flux (see text - NGC 7469, IRAS 08572+3915, IRAS 05189-2524, PKS 1345+12, IRAS 07598+6508, Mrk 1014 and 3C48).

VV114

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