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This article is an erratum for: [this article]

Issue A&A
Volume 537, January 2012
Article Number C3
Number of page(s) 1
Section Interstellar and circumstellar matter
DOI http://dx.doi.org/10.1051/0004-6361/201116447e
Published online 12 January 2012

Erratum of: A&A 532, A152 (2011), DOI: 10.1051/0004-6361/201116447

1. [CII]/CO(1–0) intensity ratio

We made an error in the calculation of [C ii]/CO(1–0) intensity ratios presented in our recent publication (Mookerjea et al. 2011). We assumed a CO(2–1)/CO(1–0) intensity ratio of 0.8 on the K km s-1 scale (Gratier et al. 2010), but calculated the CO(1–0) intensities on the erg s-1 cm-2 sr-1 scale incorrectly. The resulting [C ii]/CO(1–0) ratios are too low by a factor 8.0. This affects Fig. 12 and one sentence of the last paragraph of the Discussion. The values used for the Hα peak position presented in Sect. 6, are correct as they were derived directly from observed CO(1–0) spectra. The corrected figure and text are given below.

thumbnail Fig. 12

Star formation rate (SFR) versus the [C ii]/CO(1–0) intensity ratio. Markers are the same as in Fig. 7.
Open with DEXTER

In BCLMP 302/M 33, we find that the [C ii]/CO(1–0) ratio varies between 103 and 7  ×  104 (Fig. 12), with the H ii region A shown by red markers having values in the range 6  ×  103 to 3 × 104. The spiral arm region B (green markers) exhibits values in the range 1  ×  103 to 4  ×  103, while region C (cyan markers), where CO has hardly been detected, shows higher values, between 6  ×  103 and 7  ×  104.

Figures 7 and 12 show values on a 12′′ grid, and not on a 6′′ grid as mentioned in the caption of Fig. 7 of the published paper.

References


© ESO, 2012

All Figures

thumbnail Fig. 12

Star formation rate (SFR) versus the [C ii]/CO(1–0) intensity ratio. Markers are the same as in Fig. 7.
Open with DEXTER
In the text

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