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Advances in Astronomy
Volume 2017 (2017), Article ID 8416945, 8 pages
https://doi.org/10.1155/2017/8416945
Research Article

Star Formation Law at Sub-kpc Scale in the Elliptical Galaxy Centaurus A as Seen by ALMA

1Physics Department, Faculty of Science, University of Malaya, 50603 Kuala Lumpur, Malaysia
2Physics Department, Faculty of Science, AL-Nahrain University, Baghdad 10072, Iraq
3Graduate Institute of Astronomy, National Central University, Chung-Li 32054, Taiwan

Correspondence should be addressed to Jazeel H. Azeez; moc.oohay@niessuhleezaj

Received 28 January 2017; Accepted 19 April 2017; Published 13 June 2017

Academic Editor: Dean Hines

Copyright © 2017 Jazeel H. Azeez et al. This is an open access article distributed under the Creative Commons Attribution License, which permits unrestricted use, distribution, and reproduction in any medium, provided the original work is properly cited.

Abstract

We present an extensive analysis of the relationship between star formation rate surface density () and molecular gas surface density () at sub-kpc scale in the elliptical galaxy Centaurus A (also known as NGC 5128) at the distance 3.8 Mpc. 12CO ( = 2-1) data from Atacama Large Millimetre/Sub-Millimetre Array SV data with very high resolution (2.9′′, 0.84′′), as well as 24 μm data from the Spitzer Space Telescope, were used. This is one of the first studies of the SF law on Centaurus A at this very high spatial resolution. The results showed a breakdown in star formation law with a index relating and at 185 pc. A significant correlation exists between surface densities of molecular gas and SFR with very long depletion time (68 Gy). In addition we examined the spatially resolved relationship between velocity dispersion and star formation rate surface density for the outer disk of this galaxy and we found that the average velocity dispersion is equal to 11.78 km/s. The velocity dispersion of the molecular ISM for the outer disk is found to follow a power relation with the star formation rate surface density , where β is the slope from the ordinary least square fitting. The value of β is about and is the power law index of the star formation law.