PI: Tuan Do, UCLA, email@example.com
Address: Department of Physics and Astronomy, 8371 Math Sciences, Los Angeles, CA, 90095-1562 USA
CoI: Jonelle Walsh, Texas A&M U.
CoI: Aaron Barth, UC Irvine
CoI: Anil Seth, University of Utah
CoI: Remco van den Bosch, Max Planck Institut fur Astrophysik
CoI: Dan Carson, UC Irvine
Title: Constraining the formation of the nuclear star cluster in IC 342 with NIFS
Abstract: Nuclear star clusters (NSCs) are ubiquitous at the centers of galaxies like the Milky Way or those of lower mass. While these massive star clusters are known to follow similar galaxy scaling relationships such as M-sigma, like supermassive black holes, much is still unknown about their origin and role in galaxy formation. One prominent theory for the origin of NSCs is through the accumulation of star clusters at the center. The galaxy IC 342 provides may lend support for this theory with the existence of two young massive star clusters close to its central nuclear cluster, much like the clusters at the center of the Milky Way. In order to reach the center of IC 342, there are only a limited range orbits that are allowed -- these clusters must have radial velocities significantly below the maximum circular velocity at their postion. Therefore, we propose to measure the radial velocities of these two clusters with NIFS and LGS AO in order to determine if they can contribute to the mass of the NSC before they are disrupted by galactic tides. We also propose to measure the black hole mass in the IC 342 NSC with NIFS. This will help us understand the nature of the co-existence of supermassive black holes and NSCs as well as populate the scarce number of galaxies with black hole mass $<10^6$ $M_sun$ in galaxy scaling relationships.
Program Type: Standard/Extragalactic
Run 1 (2016B): GEM-NQ/NIFS -- 2hrs band 2 (GN-2016B-Q-38)
National Optical Astronomy Observatory, 950 North Cherry Avenue, P.O. Box 26732, Tucson, Arizona 85726, Phone: (520) 318-8000, Fax: (520) 318-8360