... boundary

This image includes the most luminous source inside the D₂₅ ellipse, located at RA  $(2000) = 13^{\rm h}37^{\rm m}19\hbox{$.\!\!^{\prime\prime}$ }{8}$, Dec  $(2000) = -29^{\circ}53\hbox{$^\prime$ }49\hbox{$^{\prime\prime}$ }$, i.e., $\approx4\hbox{$.\mkern-4mu^\prime$ }{6}$ south-east of the nucleus. It has a net count rate of 0.048 cts s^-1 and a luminosity  $\approx10^{39}$ erg s^-1. However, it is located in chip S2 (just outside the S3 chip boundary), and therefore is not discussed in this paper. See Soria & Wu (2002).

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... parameter

We were also aware of the time-dependent degradation of the ACIS Quantum Efficiency at soft energies. However, we checked that this effect is still negligible for our 2000 April observation.

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... identification

After completing our spectral analysis, the Chandra ACIS data of a short (good time interval of 6.4 ks) observation of M 83 from 2001 April have become available in the public archive. A quick-look analysis of the new dataset suggests that the flux of source No. 8 has increased by a factor of 2. If this is confirmed, the SNR identification becomes less likely, and the thermal plasma is more likely to be ionized by an accreting XRB. A detailed comparison of all the sources' fluxes and colors in the two observations, and between the ROSAT and Chandra observations, is beyond the scope of this paper.

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... galaxy

http://cfa-www.harvard.edu/cfa/ps/lists/Supernovae.html

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... coordinates

http://nedwww.ipac.caltech.edu/

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... absorption

For an operative way of identifying and classifying soft and supersoft sources in Chandra ACIS observations, see Di Stefano & Kong (2003).

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