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Title:
Vacuum Ultraviolet Images of the Large Magellanic Cloud: Erratum
Authors:
Smith, Andrew M.; Cornett, Robert H.; Hill, Robert S.
Publication:
Astrophysical Journal v.355, p.746 (ApJ Homepage)
Publication Date:
06/1990
Origin:
APJ; KNUDSEN; NED
Astronomy Keywords:
ERRATA, ADDENDA
DOI:
10.1086/168808
Bibliographic Code:
1990ApJ...355..746S

Abstract

In the paper "Vacuum Ultraviolet Images of the Large Magellanic Cloud" by Andrew M. Smith, Robert H. Cornett, and Robert S. Hill (Ap. J., 320, 609 [1987]), an error was made in the dereddening formulae for vacuum ultraviolet (VUV) magnitudes on page 613. For 30 Dor dereddening, the formulae should be m_0(1500)_ = m_1500_ - 10.47 x E(B - V)_LMC_ - 8.05 x E(B - V)_Gal_, and m_0(1900)_ = m_1900_ - 8.87 x E(B - V)_LMC_ - 8.28 x E(B - V)_Gal_. For non-30 Dor dereddening, the formulae should be m_0(1500)_ = m_1500_ -8.72 x E(B - V)_LMC_ - 8.05 x E(B - V)_Gal_, and m_0(1900) = m_1900_ - 8.21 x E(B - V)_LMC_ - 8.28 x E(B - V)_Gal_. The ramifications of this error spread through several results. However, it must be noted that the overall effect is to make our original estimates of intrinsic VUV flux too low. As a result, our primary argument on energetics actually becomes stronger: there is ample energy flux in the southwestern Large Magellanic Cloud (LMC) to sustain into the next generation of stars the star-formation front visible in our VUV images. The three tables of observational results are replaced by the results given here in Table 1, in which intrinsic VUV fluxes are corrected (other quantities remain as they were). The discussion of Table 2 needs to be amended. This table compares ionizing fluxes computed by different methods for VUV sources (OB associations) that can be identified with 6 cm radio sources (H II regions). The aggregate ionizing fluxes for this set of objects derived from the two wavelength regimes are no longer so nearly equal as they were. However, as we pointed out, any such equality would be fortuitous, since the two derivations yield results differing by typically a factor of 2 for any given individual association. The discussion of Table 3 also needs to be amended. This table combines ionizing fluxes from OB associations (derived from VU photometry) with ionizing fluxes from 6 cm sources that do not coincide with any OB association. In this way, a total ionizing flux for the whole LMC is computed, as is a sub-total for the southwestern area where we find a large- scale star-formation front. The LMC total is now nearly identical to the "corrected" result of R. C. Kennicutt and P. W. Hodge (Ap. J., 306, 130 [1987]), so as to support their estimate of 1 mag of internal reddening for each H II region. On page 618, the total ionizing flux for VUV sources along and within the computed star-formation front should be 9 x 10^51^ photons s^-1^. The stellar winds have developed a total kinetic energy of ~ 4.6 x 10^53^ ergs over a period of 7.5 Myr. On page 613, the linear relations fitted to the plots in Figure 3 should be m_0(1900)_ = 0.85 x m_0(1500)_ + 1.1, and m_0(1500)_ = 2.9 x [m_0(1500)_-m_0(1900)_] +7.2, with a standard error of 1.5 in the ordinate of the second relation. The plots in Figure 3 would change only slightly, and so are no shown again here. Finally, on page 616 and in the legend to Figure 5, the elapsed time between plotted wave fronts should be 3 x 10^7^ yr. To summarize, our main inferences remain unchanged, as do our basic calibrated photometry results. The purpose of this erratum is to correct certain derived photometry results that may be useful to other investigators.

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