... LMC

Tables 1 and 3 are only available in electronic form at the CDS via anonymous ftp to cdsarc.u-strasbg.fr (130.79.128.5) or via http://cdsweb.u-strasbg.fr/cgi-bin/qcat?J/A+A/388/100

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... HP99

It is a new supersoft source RX J0529.4-6713 at the southern boundary of the supergiant shell LMC 4. This source is very close to another source RX J0529.7-6713 which is contained in the HP99 catalog. Due to the closeness of both sources (the other source has been classified as an AGN) the source detection algorithm may have excluded this source. Spectral fitting using a blackbody spectral shape gives a temperature of 40 eV and a luminosity of $\sim$ $2\times 10^{36}\ {\rm erg}\ {\rm s^{-1}}$ if a galactic absorbing column density of $5.6\times 10^{20}\ {\rm cm^{-2}}$ and a LMC column density of $4.7\times 10^{20}\ {\rm cm^{-2}}$ is used. The spectrum is consistent with such absorption which is in favor for a supersoft source in the LMC, the southern region of LMC 4. The source appears to be variable in time. The large luminosity of the source would argue against a conventional CV nature of the source as for CVs luminosities do not exceed $\sim$ $10^{33}\ {\rm erg}\ {\rm s^{-1}}$. It thus could be a white dwarf with steady nuclear burning. Inside the 11$\arcsec$ error circle no optical counterpart is seen in digital sky survey images (blue and red plates). There are 2 to 3 optical stellar objects at the periphery of the error circle.

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... expressed

Equation (3) has been derived assuming conservation of angular momentum during the encounter of the LMC and the SMC. As a result the SMC disk was spun up to a higher angular velocity than the LMC disk (but see Maragoudaki et al. 2001). This resulted in a more efficient star formation burst in the SMC compared to the LMC. The history of the interaction, i.e. the state of the system prior to the encounter, and the distance of both galaxies during the encounter do not enter into this consideration. Only the ratio of the star formation rates induced by the encounter of both galaxies is given. Only under the assumption that the encounter was close enough to enhance the star formation rate efficiently Eq. (3) may be of relevance for the consideration of the total star formation rate during the encounter. Different values have been derived from N-body and SPH simulations of such a galaxy-galaxy encounter for the distance of closest approach, 7 kpc (GSF94, GN96), and 20 kpc (Li & Thronson 1999), respectively. Any determination of the absolute value of the induced star formation rate depends on the specific assumptions made about the history of this galaxy encounter.

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... observations

The center of the merged observation is RA 05$^{\rm h}$29$^{\rm m}$00$^{\rm s}$, Dec $-66^{\rm o}$03$\arcmin$04$\arcsec$.

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