Bibcode
Ramos Almeida, C.; Pérez García, A. M.; Acosta-Pulido, J. A.; Rodríguez Espinosa, J. M.
Referencia bibliográfica
The Astronomical Journal, Volume 135, Issue 4, pp. 1657 (2008).
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4
2008
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Descripción
In our original paper (Section 4.4) we compared the ratios of hard X-ray
to nuclear mid-infrared emission for Seyfert 1 and 2 (Sy1 and Sy2)
nuclei, finding that both distributions appear significatively different
according to the Kolmogorov-Smirnov test. We have detected a mistake in
the computation of the X-ray luminosities (the lack of a 4π factor).
Additionally, for two galaxies, the nuclear mid-infrared fluxes used
within calculations are slightly different from the correct values which
are reported in Table 3 of the original version. These mistakes affect
the mentioned ratios of hard X-ray to nuclear mid-infrared emission,
although they do not alter the result concerning the distributions,
being statistically different. The correct values of these ratios are
langlog(L X intr/L MIR)rang = -0.21
± 0.33 for the Seyfert 1 galaxies, and langlog(L X
intr/L MIR)rang = 0.17 ± 0.62 for the type
2 nuclei. Figure 8 has been updated with the newly computed values. We
have also corrected the X-axis with respect to the original figure,
which is now ν L ν. We have performed again Spearman's
rank correlation test, finding that the correlation is significant when
all galaxies and types 1 and 2 are considered separately. It is
worthwhile to note that here we have excluded from the analysis two
Seyfert 2 galaxies (NGC 1386 and NGC 7674) due to their extremely low
hard X-ray luminosities, consistent with being optically thick sources.
Recently, Horst et al. (2008) have estimated an intrinsic X-ray
luminosity for NGC 7674 of log L X intr = 44.56
erg s-1, in contrast to the non-absorption-corrected value
reported by Lutz et al. (2004) (log LX obs = 41.91
erg s-1). Such a difference of about 2.5 dex corroborates our
decision of not including these galaxies.
In a recent work, Horst et al. (2008) have argued that our luminosity
ratios are ~8 larger than what they have found for their well-resolved
objects, claiming that our nuclear data are heavily contaminated by
nuclear star formation. Our new values are now of the same order of
magnitude than theirs, even smaller for the case of Seyfert 2 galaxies.
Therefore, we believe that despite the limited resolution of ISOCAM
images, our nuclear fluxes are representative of the torus emission, and
the contamination by circumnuclear star formation, although present, is
not dominant.
There is a typographical mistake in Table 3 for the point-spread
function (PSF) flux in the LW7 filter corresponding to the galaxy
ESO144-G55; the correct value is 84.2 ± 2.44 mJy.
Based on observations with the Infrared Space Observatory, an ESA
project with instruments funded by ESA member states (especially the PI
countries: France, Germany, the Netherlands, and the United Kingdom) and
with the participation of ISAS and NASA.