http://arxiv.org/abs/1807.02986
Lenticular galaxies are generally thought to have descended from spirals via morphological transformation, although recent numerical simulations have shown that minor or even major merger can also lead to an S0-like remnant. These mechanisms, however, are active in a dense environment such as a group or a cluster of galaxies – making it harder to explain the remarkable fraction of S0s found in the field. Here, we propose a new mechanism to form such lenticular galaxies. We show that an isolated cold disk settled into rotational equilibrium becomes violently unstable – leading to fragmentation and formation of stellar clumps that, in turn, not only grow the bulge, but also increase the stellar disk velocity dispersion optimally in less than a billion year. Subsequently, the galaxy evolves passively without any conspicuous spiral structure. The final galaxy models resemble remarkably well the morphology and stellar kinematics of the present-day S0s observed by the Planetary Nebulae spectrograph. Our findings suggest a natural link between the high-redshift clumpy progenitors to the present-day S0 galaxies.
K. Saha and A. Cortesi
Tue, 10 Jul 18
26/79
Comments: 5 pages, 5 figures, Accepted for publication in ApJ Letters
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