Chitre, A and Jog, CJ (2002) Luminosity profiles of advanced mergers of galaxies using 2MASS data. In: Astronomy & Astrophysics, 338 (2). pp. 407-424.
aa_338-2_2002.pdf - Published Version
A sample of 27 disturbed galaxies that show signs of interaction but have a single nucleus were selected from the Arp and the Arp-Madore catalogues. For these, the Ks band images from the Two Micron All Sky Survey (2MASS) are analysed to obtain their radial luminosity pro�les and other structural parameters. We �nd that in spite of their similar optical appearance, the sample galaxies vary in their dynamical properties, and fall into two distinct classes. The �rst class consists of galaxies which can be described by a single r1=4 law and the second class consists of galaxies that show an outer exponential disk. A few galaxies that have disturbed pro�les cannot be �t into either of the above classes. However, all the galaxies are similar in all other parameters such as the far-infrared colours, the molecular hydrogen content and the central velocity dispersion. Thus, the dynamical parameters of these sets seem to be determined by the ratio of the initial masses of the colliding galaxies. We propose that the galaxies in the �rst class result from a merger of spiral galaxies of equal masses whereas the second class of galaxies results from a merger of unequal mass galaxies. The few objects that do not fall into either category show a disturbed luminosity pro�le and a wandering centre, which is indicative of these being unrelaxed mergers. Of the 27 galaxies in our sample, 9 show elliptical-like pro�les and 13 show an outer exponential. Interestingly, Arp 224, the second oldest merger remnant of the Toomre sequence shows an exponential disk in the outer parts.
|Item Type:||Journal Article|
|Additional Information:||Copyright © ESO|
|Keywords:||galaxies:kinematics and dynamics -- galaxies:evolution -- galaxies:interactions -- galaxies:photometry -- galaxies: structure|
|Department/Centre:||Division of Physical & Mathematical Sciences > Physics|
|Date Deposited:||20 Sep 2011 05:56|
|Last Modified:||20 Sep 2011 06:00|
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