Statistics
Scientific paper
Aug 2000
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2000apj...539.1024c&link_type=abstract
The Astrophysical Journal, Volume 539, Issue 2, pp. 1024-1025.
Statistics
19
Scientific paper
In the paper ``The Scatter in the Relationship between Redshift and the Radio-to-Submillimeter Spectral Index'' by C. L. Carilli and Min S. Yun (ApJ, 530, 618 [2000]), the 350 GHz flux densities of four of the 17 galaxies were found to be low by a factor of 1.5-2 as a result of missing extended emission in the original U. Lisenfeld, K. G. Isaak, and R. Hills (MNRAS, 312, L433 [2000]) sample. These values were subsequently updated by Lisenfeld et al. after our paper went into press. We have corrected these values using the revised Lisenfeld et al. data, which agree (within the errors) with the data presented in L. Dunne, D. Clements, and S. Eales (MNRAS, in press [2000, astro-ph/0002436]). In addition, two of the radio flux densities have been adjusted to correct for confusing sources. In this erratum we present a revised Table 1, plus the revised model for the relationship between redshift, z, and α3501.4≡observed spectral index between 1.4 and 350 GHz (revised Fig. 3). The main change in the model has been an increase in α3501.4 by about 0.04 at all redshifts (e.g., from 0 to 0.04 at z=0, and from 1.10 to 1.14 at z=6). The rms scatter in α3501.4 remains roughly constant with redshift, ranging from +/-0.17 at z=0 to +/-0.14 at z=6. The changes in the model are insufficient to change the basic conclusions in Carilli & Yun (2000). In the revised Figure 3 we include the recent α3501.4-z model from Dunne et al. (2000), based on 104 low-redshift galaxies. The scatter in the Dunne et al. model is about +/-0.10 in α3501.4. While there is substantial overlap between the scatter ranges defined by the two distributions, the Dunne et al. model predicts systematically higher values of α3501.4 at a given redshift. For instance, at z=0 the Dunne et al. model predicts α3501.4=0.18+/-0.10, while the 17 galaxy model in the revised Figure 3 predicts α3501.4=0.04+/-0.17. This difference was pointed out by Dunne et al., based on the model in the original Figure 3 in Carilli & Yun (2000). They suggested that much of the difference might be due to the low submillimeter flux densities used for a few of the sources in the original model. The revised 17 galaxy model presented herein shows that about 30% of the difference can be explained by the errant data. If we also remove the two galaxies with evidence for a radio active galactic nucleus (Mrk 231 and NGC 6240), the z=0 value of α3501.4 rises to 0.08. The remaining difference could be due to the fact that most of the sources in our 17 galaxy sample are in the upper half of the luminosity distribution delineated by the 104 galaxies used by Dunne et al. (i.e., L1.4GHz>=5×1022 W Hz-1). Figure 3 in Dunne et al. shows a systematic decrease in α3501.4 with increasing radio luminosity (a fact also pointed out in Carilli & Yun 2000), from about +0.3 for galaxies with radio spectral luminosities at 1.4 GHz of about 3×1021 W Hz-1 to +0.05 for galaxies with radio luminosities of 3×1023 W Hz-1. On the other hand, the remaining difference is well within the scatters of the two distributions and could simply be due to limited statistics.
Carilli Chris L.
Yun Min. S.
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