摘要：The specific intensity (Eq. (5)) has not been correctly
evaluated 1 . This affects the computation of the flux den-
sities, whose correct trends are shown in the new ver-
sions of Figs. 3 and 4. We recovered the signal-to-noise
ratios (S/Ns) quoted in the paper by assuming a magnetic
Fig. 3. Radial flux density profiles for the starless core models described in Sect. 5.1 (upper row) and for B68 and FeSt 1-457 (lower row, see
Sect. 5.2). The observing frequency is shown in black at the top of each column, while numbers in the upper-right corner of each subplot represent
the radius-averaged S/N for the two values of κ (0.5 and 0.7 for models A, B, C, and B68, and 0.68 and 0.88 for FeSt 1-457, see Eq. (9)). Shaded
areas encompass the curves obtained with Eq. (9) by using the two values of κ (see Fig. 2 for colour-coding). The telescope beam is shown in the
leftmost column for models A, B, and C (dotted black line, 300 00 ), B68 (short-dashed black line, 330 00 ), and FeSt 1-457 (long-dashed black line,
284 00 ). Hatched areas display SKA sensitivities for one hour of integration at different frequencies. The two panels on the right side show the flux
density as a function of frequency. Empty (solid) circles refer to an S/N smaller (larger) than 3, respectively. The spectral index α is shown on the
right of each curve.
1
We thank Alexei Ivlev for pointing out this mistake.
field strength B 0 larger by a factor of 2.74−4.20, 2.02−2.72,
and 1.55−1.80 than originally assumed for models A, B, and C,
respectively(theloweranduppervaluescorrespondingtoκ=0.5
and κ=0.7, respectively). The conclusions of the paper are
unaffected.
关键词：enISM: cloudsISM: magnetic fieldscosmic rayserrataaddenda
