UR: Self-Interacting Dark Matter Halos: To Collapse or to Not?

The Undergraduate Research series is where we feature the research that you’re doing. If you are an undergraduate that took part in an REU or similar astro research project and would like to share this on Astrobites, please check out our submission page for more details. We would also love to hear about your more general research experience!

Neev Shah

IISER Pune, India

This guest post was written by Neev Shah. Neev is a final year student studying Physics at IISER Pune. He worked on this project during his 3rd and 4th year under the supervision of Dr. Susmita Adhikari, and a paper in connection with this work is under review at MNRAS (and available on arXiv). His main interests are in gravitational wave astronomy and cosmology. He also likes to hike and explore new places.

The standard model of cosmology, ΛCDM, which assumes dark matter to be cold and interact only through gravity, has been excellent in explaining the large scale structure and evolution of the universe. However, at smaller scales, there exist tensions between observations and predictions from cosmological simulations.  Self-interacting dark matter (SIDM) is a popular alternative to the cold dark matter scenario, first proposed as a possible solution to resolve the small scale discrepancies. It allows for dark matter (DM) particles to interact with themselves through mechanisms other than just gravity. An interesting prediction of the SIDM hypothesis is that eventually there is a runaway collapse at the center of the dark matter halo, a process also known as “gravothermal catastrophe”. This can be accelerated by environmental effects, such as a subhalo orbiting inside a host dark matter halo.

Using Symphony, a suite of hundreds of zoom-in cosmological simulations of various host halos ranging from LMC-sized to as large as galaxy clusters, we aimed to find out what fraction of satellite subhalos would have collapsed  by today under the SIDM hypothesis. Since running multiple SIDM simulations is computationally expensive, we use a semi-analytic prescription to model the SIDM halo. A common approach is to treat the halo as a self-gravitating fluid, since SIDM allows for both gravitational interactions and collisions (like in a fluid!). We numerically evolved their density profiles to find out when the subhalos “collapsed”, which is the phase when the central density increases rapidly. We repeated this process for several different cross section models, varying the strength of the dark matter self interactions in the subhalo. We found that for reasonable models based on the current observational constraints on SIDM, at least 20% of the subhalo population collapses by the current time in low mass host environments such as the LMC (why its name should be changed), Milky Way and Group-sized hosts. We also studied certain other observable properties of the subhalos, such as their central densities and the inner slopes of their density profiles, and compared them to data from known dwarf spheroidal galaxies (dSph) orbiting the Milky Way. We found that the current data are consistent with these galaxies not exhibiting signs of significant core-collapse. However, this is not unexpected to occur even in the SIDM scenario, as not all halos reach the point of core collapse within the age of the universe.

A plot of the inner density profile slopes of subhalos for different models, with "Logarithmic slope at 1.5% r_vir" from -3.5 to 0.7 on the x-axis, and "Fraction of subhalos" from 0.00 to 0.25 on the y-axis. Two curves, colored blue and red and labeled "collapsing" and "cored", are shown. The blue "collapsing" curve, also labeled "YNY23" by the legend, peaks twice at slopes of -2.2 and -0.3, with a maximum subhalo fraction of approximately 0.085 and 0.13 respectively. The red "cored" curve, labeled "KTY16" in the legend, peaks once at a slope of around -0.3 with a maximum subhalo fraction of about 0.205. Black data points with horizontal error bars are plotted as well, and fall between slopes of -1.5 and -0.1, and subhalo fractions between 0.00 and 0.16. A gray shaded vertical bar falls between slopes of -1.5 and -1.3, and is labeled "NFW" in the legend.
Figure 1: The distribution of inner density profile slopes of the subhalo population in the Milky Way suite for 2 different SIDM cross section models. The black points are the data for dSph galaxies orbiting the Milky Way.

Astrobite edited by: Katherine Lee

Featured image credit: Wikimedia Commons

About Guest

This post was written by a guest author. If you're interested in writing a guest post for Astrobites, please contact us.

Discover more from astrobites

Subscribe to get the latest posts to your email.

Leave a Reply