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Issue A&A
Volume 435, Number 2, May IV 2005
Page(s) 437 - 447
Section Extragalactic astronomy
DOI http://dx.doi.org/10.1051/0004-6361:20042535



A&A 435, 437-447 (2005)
DOI: 10.1051/0004-6361:20042535

The $\mathsf{\Sigma}$ - D relation for supernova remnants in nearby galaxies

D. Urosevic1, 2, T. G. Pannuti3, N. Duric4, 5 and A. Theodorou4

1  Department of Astronomy, Faculty of Mathematics, University of Belgrade, Studentski trg 16, PO 550, 11000 Belgrade, Serbia and Montenegro
2  Isaac Newton Institute of Chile, Yugoslavia Branch, Yugoslavia
    e-mail: dejanu@matf.bg.ac.yu
3  Spitzer Science Center, Jet Propulsion Laboratory/California Institute of Technology, Mailstop 220-6, Pasadena, CA 91125, USA
4  Institute for Astrophysics, Department of Physics and Astronomy, University of New Mexico, 800 Yale Blvd., N.E., Albuquerque, NM 87131, USA
5  Karmanos Cancer Institute, Department of Radiation Oncology, Wayne State University, 4100 John R Street, Detroit, MI 48201, USA

(Received 14 December 2004 / Accepted 20 December 2004)

Abstract
This paper examines relations between the radio surface brightness $\Sigma$ and the diameter D (also known as $\Sigma-D$ relations) for a sample of extragalactic supernova remnants (SNRs) as constructed from a combination of published data and data from our own surveys. Our sample of extragalactic SNRs is the largest ever devised for the purpose of analyzing $\Sigma-D$ relations. The main results of this paper may be summarized as follows: (i) the empirical relations for SNRs in 10 of the 11 nearby galaxies studied have the approximately trivial $\Sigma\propto D^{-2}$ form, therefore limiting their interpretation as physically meaningful relations. In addition, these relations are subject to selection effects rendering them even less useful. Further Monte Carlo simulations suggest that the effect of survey sensitivity has the opposite effect of volume selection (e.g. Malmquist bias, a volume selection effect that shapes the Galactic sample) by tending to flatten the slopes toward a trivial relation. In this case, the true slopes may be steeper than the observed slopes; (ii) compact M 82 SNRs appear to follow a uniquely different $\Sigma-D$ relation in comparison to the larger, older SNRs in the other 10 galaxies. Monte Carlo simulations suggest that the probability of this difference arising by chance is $\approx$1% to 10%, depending on what is assumed regarding the underlying SNR population; (iii) three candidate hypernova remnants were identified in our sample of 11 nearby galaxies.


Key words: ISM: supernova remnants -- methods: statistical -- radio continuum: galaxies

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