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Title:
Gasdynamics in NGC 5248: Fueling a Circumnuclear Starburst Ring of Super-Star Clusters
Authors:
Jogee, Shardha; Shlosman, Isaac; Laine, Seppo; Englmaier, Peter; Knapen, Johan H.; Scoville, Nick; Wilson, Christine D.
Affiliation:
AA(Division of Physics, Mathematics, and Astronomy, MS 105-24, California Institute of Technology, Pasadena, CA 91125; ), AB(JILA, University of Colorado, Campus Box 440, Boulder, CO 80309-0440 ), AC(Space Telescope Science Institute, 3700 San Martin Drive, Baltimore, MD 21218; ), AD(Max-Planck-Institut für extraterrestrische Physik, Postfach 1312, 85741 Garching, Germany; ), AE(Isaac Newton Group of Telescopes, Apartado 321, Santa Cruz de La Palma, Canary Islands E-38700, Spain; and Department of Physical Sciences, University of Hertfordshire, Hatfield, Herts AL10 9AB, UK; ), AF(Division of Physics, Mathematics, and Astronomy, MS 105-24, California Institute of Technology, Pasadena, CA 91125; ), AG(Department of Physics and Astronomy, McMaster University, Hamilton, ON L8S 4M1, Canada; )
Publication:
The Astrophysical Journal, Volume 575, Issue 1, pp. 156-177. (ApJ Homepage)
Publication Date:
08/2002
Origin:
UCP
ApJ Keywords:
Galaxies: Evolution, Galaxies: Individual: NGC Number: NGC 5248, Galaxies: ISM, Galaxies: Kinematics and Dynamics, Galaxies: Starburst, Galaxies: Structure
DOI:
10.1086/341196
Bibliographic Code:
2002ApJ...575..156J

Abstract

Through observations and modeling, we demonstrate how the recently discovered large-scale bar in NGC 5248 generates spiral structure that extends from 10 kpc down to 100 pc, fuels star formation on progressively smaller scales, and drives disk evolution. Deep inside the bar, two massive molecular spirals cover nearly 180° in azimuth, show streaming motions of 20-40 km s-1, and feed a starburst ring of super-star clusters at 375 pc. They also connect to two narrow K-band spirals that delineate the UV bright star clusters in the ring. The data suggest that the K-band spirals are young, and the starburst has been triggered by a bar-driven spiral density wave (SDW). The latter may even have propagated closer to the center where a second Hα ring and a dust spiral are found. The molecular and Hubble Space Telescope data support a scenario where stellar winds and supernovae efficiently clear out gas from dense star-forming regions on timescales less than a few Myr. We have investigated the properties of massive CO spirals within the framework of bar-driven SDWs, incorporating the effect of gas self-gravity. We find good agreement between the model predictions and the observed morphology, kinematics, and pitch angle of the spirals. This combination of observations and modeling provides the best evidence to date for a strong dynamical coupling between the nuclear region and the surrounding disk. It also confirms that a low central mass concentration, which may be common in late-type galaxies, is particularly favorable to the propagation of a bar-driven gaseous SDW deep into the central region of the galaxy, whereas a large central mass concentration favors other processes, such as the formation and decoupling of nuclear bars.
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